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  1. toward star forming regions

    Directory of Open Access Journals (Sweden)

    Evan Jordan

    2008-01-01

    Full Text Available En este artículo se reportan observaciones de la línea J= 1 → 0 de 12CS en 20 regiones de formación estelar utilizando el telescopio Haystack de 37m del MIT. También se observaron tres regiones en la línea J= 1 → 0 de 13CS, y cinco regiones en la transición de 44 GHz de CH3OH (JK = 70 → 61 A+. Las emisiones de 13CS y CH3OH fueron detectadas en todas las regiones observadas, y la emisión de 12CS fue detectada en 19 de las 20 regiones, 11 de las cuales son nuevas detecciones. Se encontró una alta correlación entre el ancho de la línea de 12CS y la distancia a las regiones, lo que indica que la emisión de 12CS J= 1 → 0 podrá ser utilizada para estimar las distancias a regiones de formación estelar. Asimismo se reporta la detección de variabilidad de los máseres de CH3OH (44 GHz en la mayoría de las regiones observadas.

  2. Distances to star forming regions

    CERN Document Server

    Loinard, Laurent

    2014-01-01

    The determination of accurate distances to star-forming regions are discussed in the broader historical context of astronomical distance measurements. We summarize recent results for regions within 1 kpc and present perspectives for the near and more distance future.

  3. Spectroscopic studies of star forming regions

    OpenAIRE

    2006-01-01

    This paper reviews the results of studies of star forming regions, carried out at the Konkoly Observatory in the last two decades. The studies involved distance determination of star-forming dark clouds, search for candidate pre-main sequence stars, and determination of the masses and ages of the candidates by spectroscopic follow-up observations. The results expanded the list of the well-studied star forming regions in our galactic environment. Data obtained by this manner may be useful in a...

  4. The metallicity of circumnuclear star forming regions

    CERN Document Server

    Díaz, A I; Castellanos, M; Hägele, G F

    2006-01-01

    We present a spectrophotometric study of circumnuclear star forming regions (CNSFR) in the early type spiral galaxies: NGC 2903, NGC 3351 and NGC 3504, all of them of over solar metallicity according to standard empirical calibrations. A detailed determination of their abundances is made after careful subtraction of the very prominent underlying stellar absorption. It is found that most regions show the highest abundances in HII region-like objects. The relative N/O and S/O abundances are discussed. In is also shown that CNSFR, as a class, segregate from the disk HII region family, clustering around smaller ``softness parameter" -- \\eta' -- values, and therefore higher ionizing temperatures.

  5. Dynamical evolution of star forming regions

    CERN Document Server

    Parker, Richard J; Goodwin, Simon P; Meyer, Michael R

    2013-01-01

    We model the dynamical evolution of star forming regions with a wide range of initial properties. We follow the evolution of the regions' substructure using the Q-parameter, we search for dynamical mass segregation using the Lambda_MSR technique, and we also quantify the evolution of local density around stars as a function of mass using the Sigma_LDR method. The amount of dynamical mass segregation measured by Lambda_MSR is generally only significant for subvirial and virialised, substructured regions - which usually evolve to form bound clusters. The Sigma_LDR method shows that massive stars attain higher local densities than the median value in all regions, even those that are supervirial and evolve to form (unbound) associations. We also introduce the Q-Sigma_LDR plot, which describes the evolution of spatial structure as a function of mass-weighted local density in a star forming region. Initially dense (>1000 stars pc^{-2}), bound regions always have Q >1, Sigma_LDR > 2 after 5Myr, whereas dense unbound...

  6. Multiline Study of Galactic Star Forming Regions

    Science.gov (United States)

    Mookerjea, B.; Kramer, C.; Jakob, H.; Stutzki, J.

    We present first results of observations with SMART at KOSMA of selected Galactic star forming regions in mid-J (4-3) and (7-6) rotational transitions of CO and the two fine structure transitions of C I at 492 and 810 GHz. The aim of this study is to understand the interplay of the physical and chemical structure of the interstellar matter and the UV radiation field from the stars within the molecular clouds by observing the Photon Dominated Regions (PDRs). During this ongoing observational programme, regions around Orion BN/KL, W3, S106, S140 have been observed. Here we present the first results of observations of the W3 region (Jakob et al. 2002). These observations will be combined with existing observations of the emission due to low-J transitions of CO and other tracers of PDRs. The database of intensities of different lines from each of these regions will be used to derive a self-consistent interpretation using the PDR model developed by Störzer, Stutzki, & Sternberg (1996).

  7. Problems of regional innovation strategy forming

    Directory of Open Access Journals (Sweden)

    I. M. Golova

    2010-09-01

    Full Text Available The author considered problems and contradictions of modern innovation policy in Russia. It is shown, that at present time regions are removed from management of science-technical complex and spatial priorities are not produced. It is a serious factor of risk for conservation perspectives of innovation development for Russia. With taking into account of world experience main districts of rise effects regional police were formulated. It is underlined, that creation conditions for transformation of regional authorities in active subjects of innovation policy is necessary condition for building vital innovation system. It is shown, that state innovation policy must be constructed at combination of next principles: a support science-technical potential of regions — generators of innovation and creation conditions for its realization; b using of innovations for evening-out disproportions of social-economic development between regions; c widening powers and financial possibilities of regions at management of innovation climate. Methodical approaches for making effective mechanisms of management of innovation processes of territory are opened. Typology of Russian regions with high and middle degree of innovation climate is proposed, which takes level of science and innovation potential of territory and also degree of comfort of social-economic conditions for development of innovation activity are offered. Peculiarities of innovation strategy for different types of regions are defined. This typology may be used for substantiation spatial priorities of innovation strategy of Russia.

  8. Extreme Variables in Star Forming Regions

    Science.gov (United States)

    Contreras Peña, Carlos Eduardo

    2015-01-01

    in two multi-epoch infrared surveys: the UKIDSS Galactic Plane Survey (GPS) and the Vista Variables in the Via Lactea (VVV). In order to further investigate the nature of the selected variable stars, we use photometric information arising from public surveys at near- to far-infrared wavelengths. In addition we have performed spectroscopic and photometric follow-up for a large subset of the samples arising from GPS and VVV. We analyse the widely separated two-epoch K-band photometry in the 5th, 7th and 8th data releases of the UKIDSS Galactic Plane Survey. We find 71 stars with ΔK > 1 mag, including 2 previously known OH/IR stars and a Nova. Even though the mid-plane is mostly excluded from the dataset, we find the majority (66%) of our sample to be within known star forming regions (SFRs), with two large concentrations in the Serpens OB2 association (11 stars) and the Cygnus-X complex (27 stars). The analysis of the multi-epoch K-band photometry of 2010-2012 data from VVV covering the Galactic disc at |b| related to outbursts events cannot be confirmed from our data. Adding the GPS and VVV spectroscopic results, we find that between 6 and 14 objects are new additions to the FUor class from their close resemblance to the near-infrared spectra of FUors, and at least 23 more objects are new additions to the eruptive variable class. For most of these we are unable to classify them into any of the original definitions for this variable class. In any case, we are adding up to 37 new stars to the eruptive variable class which would double the current number of known objects. We note that most objects are found to be deeply embedded optically invisible stars, thus increasing the number of objects belonging to this subclass by a much larger factor. In general, objects in our samples which are found to be likely eruptive variable stars show a mixture of characteristics that can be attributed to both of the optically-defined classes. This agrees well with the recent

  9. Optical polarimetry of star-forming regions

    Energy Technology Data Exchange (ETDEWEB)

    Gledhill, T.M.

    1987-01-01

    The polarimetric investigation of nebulosity associated with loss-mass pre-main sequence (PMS) stellar objects is detailed. Three regions of on-going star formation are considered, specifically, the Haro 6-5 and the HL/XZ Tau systems - both associated with dark clouds in the Taurus complex - and the PV Cephei nebulosity near NGC7023. In each region the imaging observations suggest bipolarity in the optical structure of the nebulosity, and the polarimetric data are used to determine the locations of the illuminating sources. Evidence is found for the association of circumstellar discs of obscuration with the PMS objects Haro 6-5A (FS Tau), Haro 6-5B, HL Tau, and PV Cephei. In each case the polarimetric data suggest that the local magnetic field has played an important role in the evolution of the star and the circumstellar material. Examination of the source-region polarization maps suggests that at least one of the objects considered is surrounded by a dust grain-aligning magnetic field with a predominantly toroidal geometry in the plane of the circumstellar disc. Implications for current theories of outflow acceleration and cloud evolution are discussed.

  10. Nucleon Form Factors in the Space- and Timelike Regions

    CERN Document Server

    Hammer, H W

    2001-01-01

    Dispersion relations provide a powerful tool to describe the electromagnetic form factors of the nucleon both in the spacelike and timelike regions with constraints from unitarity and perturbative QCD. We give a brief introduction into dispersion theory for nucleon form factors and present results from a recent form factor analysis. Particular emphasis is given to the form factors in the timelike region. Furthermore, some recent results for the spacelike form factors at low momentum transfer from a ChPT calculation by Kubis and Meissner are discussed.

  11. Forming a Primordial Star in a Relic HII Region

    CERN Document Server

    O'Shea, B W; Whalen, D; Norman, M L; Shea, Brian W. O'; Abel, Tom; Whalen, Dan; Norman, Michael L.

    2005-01-01

    There has been considerable theoretical debate over whether photoionization and supernova feedback from the first Population III stars facilitate or suppress the formation of the next generation of stars. We present results from an Eulerian adaptive mesh refinement simulation demonstrating the formation of a primordial star within a region ionized by an earlier nearby star. Despite the higher temperatures of the ionized gas and its flow out of the dark matter potential wells, this second star formed within 23 million years of its neighbor's death. The enhanced electron fraction within the HII region catalyzes rapid molecular hydrogen formation that leads to faster cooling in the subsequent star forming halos than in the first halos. This ``second generation'' primordial protostar has a much lower accretion rate because, unlike the first protostar, it forms in a rotationally supported disk of approximately 10-100 solar masses. In contrast to unpreprocessed regions, such configurations may allow binaries or mul...

  12. Proton Form Factors Measurements in the Time-Like Region

    Energy Technology Data Exchange (ETDEWEB)

    Anulli, F.; /Frascati

    2007-10-22

    I present an overview of the measurement of the proton form factors in the time-like region. BABAR has recently measured with great accuracy the e{sup +}e{sup -} {yields} p{bar p} reaction from production threshold up to an energy of {approx} 4.5 GeV, finding evidence for a ratio of the electric to magnetic form factor greater than unity, contrary to expectation. In agreement with previous measurements, BABAR confirmed the steep rise of the magnetic form factor close to the p{bar p} mass threshold, suggesting the possible presence of an under-threshold N{bar N} vector state. These and other open questions related to the nucleon form factors both in the time-like and space-like region, wait for more data with different experimental techniques to be possibly solved.

  13. A kinematic study of the Lupus star-forming region

    Science.gov (United States)

    Galli, P. A. B.; Bertout, C.; Teixeira, R.; Ducourant, C.

    2014-10-01

    In this paper, we study the southern star-forming region located in Lupus that constitutes one of the richest associations of T Tauri stars. Based on the convergent point (CP) method combined with a k-NN analysis we identify 109 pre-main sequence stars in this region that define the Lupus association of comoving stars, and derive individual distances for all group members.

  14. Forming limits of nickel coating on right region

    Institute of Scientific and Technical Information of China (English)

    2007-01-01

    The forming limits of nickel coating on the right region were studied, so as to direct the preparation of the material and help the production of workpieces. The electrodeposited nickel coating was prepared on steel substrate to form advanced structures,and its plastic instability was investigated by the Swift Plastic Instability Theory. By using the compound law for laminated sheet metals, explicit equations for the calculation of the instable eigen values were deduced. The forming limit diagrams of the nickel coating on the right region were plotted. It is exhibited that the forming limit of the coating sheet is between the forming limits of the individual nickel coating and steel substrate. The forming limit of the nickel coating is not so good as that of the steel substrate, and the forming limit strain of the coating sheet tends to diminish with the increase of thickness of the coating. The greater the normal anisotropic coefficient of the materials is, the better the forming limit is.

  15. Organizational and legal aspects of regional transport cluster forming

    Directory of Open Access Journals (Sweden)

    V.V. Lyfar

    2014-06-01

    Full Text Available The aim of the article. The objective of the work is to define the organizational and legal aspects of transport cluster forming transport, in particular its maintenance, form and intercommunications of participants. The results of the analysis. In the article on the basis of comparative analysis of determination of clusters and interpretation of their essence by other scientists, authorial determination of transport cluster is given, its maintenance, structure and legal form, are also determined. In basis of transport cluster the forming of transport-logistic system lies, and the center of such cluster can be a transport-logistic center. The legal framework of creation of cluster can be an agreement about joint activity. At the same time a cluster can have organizational and legal registration as a contractual association of legal entities with preservation of their self-dependence and independence. Management of transport cluster forming must take place at the level of regional state administration on condition of support of branch organs of management and have a complex character. The offered structure of transport cluster includes three basic blocks: business, science, power. Between the blocks of cluster the high degree of co-ordination must be attained. The center of cluster mostly is formed by the few powerful transport companies of region, which constitute the «kernel». Round this kernel the significant amount of small and middle firms which also co-operate and compete between each other is concentrated. The enterprises of region or regions, uniting in a cluster, obtain the possibility to defend their interests more effectively at the level of local authorities and local self-government, and also to participate in the large investment projects. Ultimately transport cluster is determined as an integration form of menage which will allow uniting transport organizations and pointing all resources at development of a transport and logistic

  16. High Resolution CO Observations of Massive Star Forming Regions

    CERN Document Server

    Klaassen, P D; Keto, E R; Zhang, Q; Galván-Madrid, R; Liu, H-Y B

    2011-01-01

    Context. To further understand the processes involved in the formation of massive stars, we have undertaken a study of the gas dynamics surrounding three massive star forming regions. By observing the large scale structures at high resolution, we are able to determine properties such as driving source, and spatially resolve the bulk dynamical properties of the gas such as infall and outflow. Aims. With high resolution observations, we are able to determine which of the cores in a cluster forming massive stars is responsible for the large scale structures. Methods. We present CO observations of three massive star forming regions with known HII regions and show how the CO traces both infall and outflow. By combining data taken in two SMA configurations with JCMT observations, we are able to see large scale structures at high resolution. Results. We find large (0.26-0.40 pc), massive (2-3 M_sun) and energetic (13-17 \\times 10^44 erg) outflows emanating from the edges of two HII regions suggesting they are being ...

  17. Outflow and Accretion in Massive Star Forming Regions

    CERN Document Server

    Klaassen, P D

    2007-01-01

    In order to distinguish between the various components of massive star forming regions (i.e. infalling, outflowing and rotating gas structures) within our own Galaxy, we require high angular resolution observations which are sensitive to structures on all size scales. To this end, we present observations of the molecular and ionized gas towards massive star forming regions at 230 GHz from the SMA (with zero spacing from the JCMT) and at 22 and 23 GHz from the VLA at arcsecond or better resolution. These observations (of sources such as NGC7538, W51e2 and K3-50A) form an integral part of a multi-resolution study of the molecular and ionized gas dynamics of massive star forming regions (i.e. Klaassen & Wilson 2007). Through comparison of these observations with 3D radiative transfer models, we hope to be able to distinguish between various modes of massive star formation, such as ionized or halted accretion (i.e Keto 2003 or Klaassen et al. 2006 respectively).

  18. The IRAS 08589-4714 star-forming region

    CERN Document Server

    Saldaño, H P; Gómez, M; Cappa, C E; Duronea, N U; Rubio, M

    2016-01-01

    We present an analysis of the IRAS 08589-4714 star-forming region. This region harbors candidate young stellar objects identified in the WISE and Herschel images using color index criteria and spectral energy distributions (SEDs). The SEDs of some of the infrared sources and the 70 microns radial intensity profile of the brightest source (IRS 1) are modeled from Herschel fluxes using the one-dimensional radiative transfer DUSTY code. For these objects, we estimate the envelope masses, sizes, densities, and luminosities which suggest that they are very young, massive and luminous objects at early stages of the formation process. Color-color diagrams in the bands of WISE and 2MASS are used to identify potential young objects in the region. Those identified in the bands of WISE would be contaminated by the emission of PAHs. We use the emission distribution in the infrared at 70 and 160 microns, to estimate the dust temperature gradient. This suggests that the nearby massive star-forming region RCW 38, located ~ ...

  19. INFORMATIONAL-ANALYTIC MODEL OF REGIONAL PROJECT PORTFOLIO FORMING

    Directory of Open Access Journals (Sweden)

    I. A. Osaulenko

    2016-01-01

    Full Text Available The article is devoted to the problem of regional project portfolio management in context of interaction of the regional development’s motive forces interaction. The features of innovation development on the regional level and their influence on the portfolio forming process considered. An existing approaches for portfolio modelling and formal criterion of the projects selection analyzed. At the same time the organization of key subjects of regional development interaction described. The aim of the article is investigation of informational aspects of project selection in process of the main development’s motive forces interaction and analytic model of portfolio filling validation. At that an inclination of stakeholders to reach a consensus taking into account. The Triple Helix conception using for concrete definition of the functions of the regional development’s motive forces. Asserted, that any component of innovation triad «science–business–government» can be an initiator of regional project, but it need to support two another components. Non-power interaction theory using for investigation of subjects interrelations in process of joint activity proposed. One of the key concept of the theory is information distance. It characterizes inclination of the parties to reach a consensus based on statistics. Projections of information distance onto directions of development axes using for more accurate definition of mutual positions in the all lines of development proposed. Another important parameter of the model which has an influence on the project support is awareness of stakeholders about it. Formalized description of project in the form of fast set of parameters proposes to use for determination of the awareness. The weighting coefficients for each parameter by expert way. Simultaneously the precision of the each parameter setting for all presented projects determines. On the base of appointed values of information distances and

  20. Pluto's elongated dark regions formed by the Charon-forming giant impact

    Science.gov (United States)

    Genda, Hidenori; Sekine, Yusuhito; Kamata, Shunichi; Funatsu, Taro

    2017-04-01

    The New Horizons spacecraft has found elongated dark areas in the equatorial region of Pluto, which were informally called "the Whale" or Cthulhu Region (Stern et al. 2015). Here we examine the possibility that the dark areas on Pluto were formed by thermal alterations and polymerization of interstellar volatiles caused by a Charon-forming giant impact. Pluto is one of the largest Kuiper belt objects, which is highly likely to contain various interstellar volatiles, including aldehyde and ammonia. The previous study (Cordy et al. 2011) shows that these interstellar volatiles are thermally polymerized in solutions at high temperatures, forming complex insoluble organic solids. Given the satellite-to-planet mass ratio, the Pluto-Charon system is suggested to be of a giant impact origin (Canup 2005). Impact-induced heating on Pluto could have converted these volatile into complex organic matter in solution near the surface, which may explain the presence of dark areas in the equatorial region of Pluto. Here, we produce complex organic matter for various temperatures by thermal polymerization of formaldehyde and ammonia in solutions. By measuring the UV-VIS absorption spectra of the produced organic matter, we found that the color of the solution changes to be dark if the temerature is above 50 degree C for months or more. This duration corresponds to the cooling timescale of a water pond with 500-km thickness. By using SPH code (Genda et al. 2015), we carried out many simulations of a giant impact, and we found that a molten hot pond with > 500-km thickness is formed around the equatorial region of Pluto by a Charon-forming giant impact, if the water/rock mixing mass ratio is less than 1 or if the pre-impact interior temperature is 150 K. Both the dark equatorial region and a Charon-sized moon are formed when the pre-impact Pluto is undifferentiated. To keep a rock-rich Pluto undifferentiated at time of the giant impact, Pluto may have been formed >100 Myrs after CAIs

  1. Dynamical evolution of star forming regions - II. Basic kinematics

    CERN Document Server

    Parker, Richard J

    2016-01-01

    We follow the dynamical evolution of young star-forming regions with a wide range of initial conditions and examine how the radial velocity dispersion, $\\sigma$, evolves over time. We compare this velocity dispersion to the theoretically expected value for the velocity dispersion if a region were in virial equilibrium, $\\sigma_{\\rm vir}$ and thus assess the virial state ($\\sigma / \\sigma_{\\rm vir}$) of these systems. We find that in regions that are initially subvirial, or in global virial equilibrium but subvirial on local scales, the system relaxes to virial equilibrium within several million years, or roughly 25 - 50 crossing times, according to the measured virial ratio. However, the measured velocity dispersion, $\\sigma$, appears to be a bad diagnostic of the current virial state of these systems as it suggests that they become supervirial when compared to the velocity dispersion estimated from the virial mass, $\\sigma_{\\rm vir}$. We suggest that this discrepancy is caused by the fact that the regions ar...

  2. The chemistry of planet-forming regions is not interstellar

    CERN Document Server

    Pontoppidan, Klaus M

    2014-01-01

    Advances in infrared and submillimeter technology have allowed for detailed observations of the molecular content of the planet-forming regions of protoplanetary disks. In particular, disks around solar-type stars now have growing molecular inventories that can be directly compared with both prestellar chemistry and that inferred for the early solar nebula. The data directly address the old question whether the chemistry of planet-forming matter is similar or different and unique relative to the chemistry of dense clouds and protostellar envelopes. The answer to this question may have profound consequences for the structure and composition of planetary systems. The practical challenge is that observations of emission lines from disks do not easily translate into chemical concentrations. Here, we present a two-dimensional radiative transfer model of RNO 90, a classical protoplanetary disk around a solar-mass star, and retrieve the concentrations of dominant molecular carriers of carbon, oxygen and nitrogen in ...

  3. Locating Star-Forming Regions in Quasar Host Galaxies

    CERN Document Server

    Young, J E; Shemmer, O; Netzer, H; Gronwall, C; Lutz, Dieter; Ciardullo, R; Sturm, Eckhard

    2013-01-01

    We present a study of the morphology and intensity of star formation in the host galaxies of eight Palomar-Green quasars using observations with the Hubble Space Telescope. Our observations are motivated by recent evidence for a close relationship between black hole growth and the stellar mass evolution in its host galaxy. We use narrow-band [O II] $\\lambda$3727, H$\\beta$, [O III] $\\lambda$5007 and Pa$\\alpha$ images, taken with the WFPC2 and NICMOS instruments, to map the morphology of line-emitting regions, and, after extinction corrections, diagnose the excitation mechanism and infer star-formation rates. Significant challenges in this type of work are the separation of the quasar light from the stellar continuum and the quasar-excited gas from the star-forming regions. To this end, we present a novel technique for image decomposition and subtraction of quasar light. Our primary result is the detection of extended line-emitting regions with sizes ranging from 0.5 to 5 kpc and distributed symmetrically aroun...

  4. Scaling Relations of Star-Forming Regions: from kpc-size clumps to HII regions

    CERN Document Server

    Wisnioski, Emily; Blake, Chris; Poole, Gregory B; Green, Andrew W; Wyder, Ted; Martin, Chris

    2012-01-01

    We present the properties of 8 star-forming regions, or 'clumps,' in 3 galaxies at z~1.3 from the WiggleZ Dark Energy Survey, which are resolved with the OSIRIS integral field spectrograph. Within turbulent discs, \\sigma~90 km/s, clumps are measured with average sizes of 1.5 kpc and average Jeans masses of 4.2 x 10^9 \\Msolar, in total accounting for 20-30 per cent of the stellar mass of the discs. These findings lend observational support to models that predict larger clumps will form as a result of higher disc velocity dispersions driven-up by cosmological gas accretion. As a consequence of the changes in global environment, it may be predicted that star-forming regions at high redshift should not resemble star-forming regions locally. Yet despite the increased sizes and dispersions, clumps and HII regions are found to follow tight scaling relations over the range z=0-2 for size, velocity dispersion, luminosity, and mass when comparing >2000 HII regions locally and 30 clumps at z>1 (\\sigma \\propto r^{0.42+/-...

  5. VLBA Changes Picture of Famous Star-Forming Region

    Science.gov (United States)

    2007-10-01

    Using the supersharp radio "vision" of the National Science Foundation's Very Long Baseline Array (VLBA), astronomers have made the most precise measurement ever of the distance to a famous star-forming region. The measurement -- to the heavily studied Orion Nebula -- changes scientists' understanding of the characteristics of the young stars in the region. Parallax Diagram Trigonometric Parallax method determines distance to star by measuring its slight shift in apparent position as seen from opposite ends of Earth's orbit. CREDIT: Bill Saxton, NRAO/AUI/NSF Star Track Apparent track of star GMR A in the Orion Nebula Cluster, showing shift caused by Earth's orbital motion and star's movement in space. CREDIT: Sandstrom et al., NRAO/AUI/NSF Click on Images for Larger Files "This measurement is four times more precise than previous distance estimates. Because our measurement reduces the distance to this region, it tells us that the stars there are less bright than thought before, and changes the estimates of their ages," said Geoff Bower, an astronomer at the University of California at Berkeley. Bower, along with Karin Sandstrom, J.E.G. Peek, Alberto Bolatto and Richard Plambeck, all of Berkeley, published their findings in the October 10 edition of the Astrophysical Journal. The scientists determined the distance to a star called GMR A, one of a cluster of stars in the Orion Nebula, by measuring the slight shift in the star's apparent position in the sky caused by the Earth's motion around the Sun. Observing the star when the Earth is on opposite sides of its annual orbit allows astronomers to measure the angle of this small shift and thus provides a direct trigonometric calculation of its distance. "By using this technique, called parallax, we get a direct measurement that does not depend on various assumptions that are required to use less-direct methods," Bower said. "Only a telescope with the remarkable ability to see fine detail that is provided by the VLBA is

  6. [OI] disk emission in the Taurus star forming region

    CERN Document Server

    Aresu, G; Meijerink, R; Spaans, M; Vicente, S; Podio, L; Woitke, P; Menard, F; Thi, W -F; Gudel, M; Liebhart, A

    2014-01-01

    The structure of protoplanetary disks is thought to be linked to the temperature and chemistry of their dust and gas. Whether the disk is flat or flaring depends on the amount of radiation that it absorbs at a given radius, and on the efficiency with which this is converted into thermal energy. The understanding of these heating and cooling processes is crucial to provide a reliable disk structure for the interpretation of dust continuum emission and gas line fluxes. Especially in the upper layers of the disk, where gas and dust are thermally decoupled, the infrared line emission is strictly related to the gas heating/cooling processes. We aim to study the thermal properties of the disk in the oxygen line emission region, and to investigate the relative importance of X-ray (1-120 Angstrom) and far-UV radiation (FUV, 912-2070 Angstrom) for the heating balance there. We use [OI] 63 micron line fluxes observed in a sample of protoplanetary disks of the Taurus/Auriga star forming region and compare it to the mode...

  7. Locating star-forming regions in quasar host galaxies

    Science.gov (United States)

    Young, J. E.; Eracleous, M.; Shemmer, O.; Netzer, H.; Gronwall, C.; Lutz, Dieter; Ciardullo, R.; Sturm, Eckhard

    2014-02-01

    We present a study of the morphology and intensity of star formation in the host galaxies of eight Palomar-Green quasars using observations with the Hubble Space Telescope. Our observations are motivated by recent evidence for a close relationship between black hole growth and the stellar mass evolution in its host galaxy. We use narrow-band [O II]λ3727, Hβ, [O III]λ5007 and Paα images, taken with the Wide Field Planetary Camera 2 and NICMOS instruments, to map the morphology of line-emitting regions, and, after extinction corrections, diagnose the excitation mechanism and infer star-formation rates. Significant challenges in this type of work are the separation of the quasar light from the stellar continuum and the quasar-excited gas from the star-forming regions. To this end, we present a novel technique for image decomposition and subtraction of quasar light. Our primary result is the detection of extended line-emitting regions with sizes ranging from 0.5 to 5 kpc and distributed symmetrically around the nucleus, powered primarily by star formation. We determine star-formation rates of the order of a few tens of M⊙ yr-1. The host galaxies of our target quasars have stellar masses of the order of 1011 M⊙ and specific star-formation rates on a par with those of M82 and luminous infrared galaxies. As such they fall at the upper envelope or just above the star-formation mass sequence in the specific star formation versus stellar mass diagram. We see a clear trend of increasing star-formation rate with quasar luminosity, reinforcing the link between the growth of the stellar mass of the host and the black hole mass found by other authors.

  8. Water in star- and planet-forming regions.

    Science.gov (United States)

    Bergin, Edwin A; van Dishoeck, Ewine F

    2012-06-13

    In this paper, we discuss the astronomical search for water vapour in order to understand the disposition of water in all its phases throughout the processes of star and planet formation. Our ability to detect and study water vapour has recently received a tremendous boost with the successful launch and operation of the Herschel Space Observatory. Herschel spectroscopic detections of numerous transitions in a variety of astronomical objects, along with previous work by other space-based observatories, will be threaded throughout this paper. In particular, we present observations of water tracing the earliest stage of star birth where it is predominantly frozen as ice. When a star is born, the local energy release by radiation liberates ices in its surrounding envelope and powers energetic outflows that appear to be water factories. In these regions, water plays an important role in the gas physics. Finally, we end with an exploration of water in planet-forming discs surrounding young stars. The availability of accurate molecular data (frequencies, collisional rate coefficients and chemical reaction rates) is crucial to analyse the observations at each of these steps.

  9. Are Gamma-Ray Bursts in Star Forming Regions?

    CERN Document Server

    Paczynski, B

    1997-01-01

    The optical afterglow of the gamma-ray burst GRB 970508 (z = 0.835) was a few hundred times more luminous than any supernova. Therefore, a name `hypernova' is proposed for the whole GRB/afterglow event. There is tentative evidence that the GRBs: 970228, 970508, and 970828 were close to star forming regions. If this case is strengthened with future afterglows then the popular model in which GRBs are caused be merging neutron stars will have to be abandoned, and a model linking GRBs to cataclysmic deaths of massive stars will be favored. The presence of X-ray precursors, first detected with Ginga, is easier to understand within a framework of a `dirty' rather than a `clean' fireball. A very energetic explosion of a massive star is likely to create a dirty fireball, rather than a clean one. A specific speculative example of such an explosion is proposed, a microquasar. Its geometrical structure is similar to the `failed supernova' of Woosley (1993a): the inner core of a massive, rapidly rotating star collapses i...

  10. Methods of regional innovative clusters forming and development programs elaboration

    OpenAIRE

    Marchuk, Olha

    2013-01-01

    The aim of the article is to select programmes for the formation and development of innovative cluster structures. The analysis of the backgrounds of formation of innovative clusters was made in the regions of Ukraine. Two types of programmes were suggested for the implamentation of cluster policy at the regional level.

  11. Travel and urban form in the Greater Copenhagen region

    DEFF Research Database (Denmark)

    Nielsen, Thomas Alexander Sick

    and how much. Analysis of the stability of urban form correlates of travel over time has exploited the possibilities offered by the most recent and consistent data series produced by the Danish National Travel Survey. Data allows for a comparison of the urban form correlates of travel at the peak......Research into the associations between urban form and travel in the capital areal has focussed on subcenters and the stability of urban form correlates over time. A trend towards de-concentration and formation of subcenters in metropolitan areas has been acknowledged for decades. Studies have...... analyzed the new urban structure by identifying subcenters and their land value impacts. Others have focused on subcenters as a location attribute or ‘intervention’ that affects travel patterns and therefore may be employed in the context of urban and transportation demand management. The research has...

  12. Travel and urban form in the Greater Copenhagen region

    DEFF Research Database (Denmark)

    Nielsen, Thomas Alexander Sick

    of the economic upturn – with a later point in time where the financial crisis had radically changed the economic climate. It follows from the specificity of the historical events that an analysis of what happened to urban form and transport over the financial crisis is to be seen as a case study......Research into the associations between urban form and travel in the capital areal has focussed on subcenters and the stability of urban form correlates over time. A trend towards de-concentration and formation of subcenters in metropolitan areas has been acknowledged for decades. Studies have...... analyzed the new urban structure by identifying subcenters and their land value impacts. Others have focused on subcenters as a location attribute or ‘intervention’ that affects travel patterns and therefore may be employed in the context of urban and transportation demand management. The research has...

  13. Innovative forms of institutional structures in Russian regions

    OpenAIRE

    Larina Ekaterina

    2012-01-01

    The theme of scientific research is actual, now, as combines creation preconditions social – economic consortium between representatives of leading enterprises of region, young scientists and representatives of higher school, government, society. Working out of innovative approaches to formation scientifically – the educational center in system of preparation of scientific shots became result of scientific research.

  14. INNOVATIVE FORMS OF INSTITUTIONAL STRUCTURES IN RUSSIAN REGIONS

    Directory of Open Access Journals (Sweden)

    Larina Ekaterina

    2012-01-01

    Full Text Available The theme of scientific research is actual, now, as combines creation preconditions social – economic consortium between representatives of leading enterprises of region, young scientists and representatives of higher school, government, society. Working out of innovative approaches to formation scientifically – the educational center in system of preparation of scientific shots became result of scientific research.

  15. Molecular line tracers of high-mass star forming regions

    NARCIS (Netherlands)

    Nagy, Zsofia; Van der Tak, Floris; Ossenkopf, Volker; Bergin, Edwin; Black, John; Faure, Alexandre; Fuller, Gary; Gerin, Maryvonne; Goicoechea, Javier; Joblin, Christine; Le Bourlot, Jacques; Le Petit, Franck; Makai, Zoltan; Plume, Rene; Roellig, Markus; Spaans, Marco; Tolls, Volker

    2013-01-01

    High-mass stars influence their environment in different ways including feedback via their FUV radiation. The penetration of FUV photons into molecular clouds creates Photon Dominated Regions (PDRs) with different chemical layers where the mainly ionized medium changes into mainly molecular. Differe

  16. Star forming regions in gas-rich SO galaxies

    Science.gov (United States)

    Pogge, Richard W.; Eskridge, Paul B.

    1987-01-01

    The first results of an H alpha imaging survey of HI rich SO galaxies, which were searched for HII regions and other sources of emission, are presented. The charge coupled device H alpha interference filter images were made of 16 galaxies. Eight of these galaxies show evidence for on-going star formation, one has nuclear emission but no HII regions, and the remaining seven have no emissions detected within well defined upper limits. With the exception of one notably peculiar galaxy in which the emission from HII regions appears pervasive, the HII regions are either organized into inner-disk rings or randomly distributed throughout the disk. A few of these galaxies are found to be clearly not SO's; or peculiar objects atypical of the SO class. Using simple models star formation rates (SFRs) and gas depletion times from the observed H alpha fluxes were estimated. In general, the derived SFRs are much lower than those found in isolated field spiral galaxies and the corresponding gas depletion time scales are also longer.

  17. A submllimeter observation and study of star-forming regions

    Institute of Scientific and Technical Information of China (English)

    2002-01-01

    Using the 3-m radio telescope of KOSMA, we mapped 12CO (J = 3-2) lines for three molecular clouds, B35, S146 and TMC-2A. High-velocity molecular outflows are found in all these regions. The physical and dynamical parameters of the outflows are derived, and their shapes and driving sources are analyzed. Contour maps of center velocities show that the large scale systematic gradients exist in the three clouds. These observed motions are best explained by rotation after excluding the cause of outflows. Furthermore, in the core region of TMC-2A there is a velocity gradient in opposite direction from that of the large scale. It may be caused by magnetic braking. Finally, angular velocities of the clouds are calculated, and the effects of rotation against gravity and lowering the star-formation rate are also analyzed.

  18. The Young Cluster and Star Forming Region NGC 2264

    OpenAIRE

    Dahm, S. E.

    2008-01-01

    NGC 2264 is a young Galactic cluster and the dominant component of the Mon OB1 association lying approximately 760 pc distant within the local spiral arm. The cluster is hierarchically structured, with subclusters of suspected members spread across several parsecs. Associated with the cluster is an extensive molecular cloud complex spanning more than two degrees on the sky. Star formation is ongoing within the region as evidenced by the presence of numerous embedded clusters of protostars, mo...

  19. A new star-forming region in Canis Major

    CERN Document Server

    Magakian, T Yu; Bally, J

    2016-01-01

    A new southern star-formation region, located at an estimated distance of ~1.5 kpc in the Lynds 1664 dark cloud in Canis Major, is described. Lynds 1664 contains several compact star clusters, small stellar groups, and young stars associated with reflection nebulae. Narrow-band H{\\alpha} and [SII] images obtained with 4-m CTIO telescope reveal more than 20 new Herbig-Haro objects associated with several protostellar outflows.

  20. On the Form of the HII Region Luminosity Function

    CERN Document Server

    Oey, M S

    1997-01-01

    Observed variations in the HII region luminosity function (HII LF) seen in spiral arm vs. interarm regions, and different galactic Hubble type, can be explained simply by evolutionary effects and maximum number of ionizing stars per cluster. We present Monte Carlo simulations of the HII LF, drawing the number of ionizing stars N_* from a power-law distribution of constant slope, and the stellar masses from a Salpeter IMF with an upper-mass limit of 100 M_sol. We investigate the evolution of the HII LF, as determined by stellar main-sequence lifetimes and ionizing luminosities, for a single burst case and continuous creation of the nebular population. Shallower HII LF slopes measured for the arms of spiral galaxies can be explained as a composite slope, expected for a zero-age burst population, whereas the interarm regions tend to be dominated by evolved rich clusters described by a single, steeper slope. Steeper slopes in earlier-type galaxies can be explained simply by a lower maximum N_* cutoff found for th...

  1. The Embedded Massive Star Forming Region RCW 38

    CERN Document Server

    Wolk, Scott J; Vigil, Miquela

    2008-01-01

    RCW~38 is a uniquely young ($<$1 Myr), embedded ($A_V \\sim 10$) stellar cluster surrounding a pair of early O stars ($\\sim$O5.5) and is one of the few regions within 2 kpc other than Orion to contain over 1000 members. X-ray and deep near-infrared observations reveal a dense cluster with over 200 X-ray sources and 400 infrared sources embedded in a diffuse hot plasma within a 1 pc diameter. The central O star has evacuated its immediate surroundings of dust, creating a wind bubble $\\sim$0.1 pc in radius that is confined by the surrounding molecular cloud, as traced by millimeter continuum and molecular line emission. The interface between the bubble and cloud is a region of warm dust and ionized gas, which shows evidence for ongoing star formation. Extended warm dust is found throughout a 2--3 pc region and coincides with extended X-ray plasma. This is evidence that the influence of the massive stars reaches beyond the confines of the O star bubble. RCW~38 appears similar in structure to RCW~49 and M~20 bu...

  2. High resolution oh maser survey in star forming regions

    Directory of Open Access Journals (Sweden)

    A. E. Ruiz

    2006-01-01

    Full Text Available Presentamos los resultados de un rastreo de alta resoluci on de m aseres de OH en Regiones de Formaci on Estelar Gal actica con el prop osito de estudiar la emisi on m aser y establecer una lista de candidatos adecuados para realizar un seguimiento con instrumentos de mayor resoluci on. Se utiliz o el Very Long Baseline Array (VLBA para observar las transiciones del m aser de OH en 1665, 1667, 1612 y 1720 MHz dentro de 41 regiones. Estas son las primeras observaciones de alta resoluci on que se realizan en la mayor parte de las fuentes. Se detectaron 30 sitios de emisi on m aser en alguna o varias transiciones, con nuevas detecciones en 4 fuentes, y donde aproximadamente 40% de la muestra exhibe estructura muy compacta. Finalmente consideramos que el espectro observado en W75N muestra el estado inicial de una r afaga del m aser de OH en la l nea de 1665 MHz, la cual es la primera que se conoce

  3. Cosmic-Ray Injection from Star-Forming Regions.

    Science.gov (United States)

    Carlson, Eric; Profumo, Stefano; Linden, Tim

    2016-09-01

    At present, all physical models of diffuse Galactic γ-ray emission assume that the distribution of cosmic-ray sources traces the observed populations of either OB stars, pulsars, or supernova remnants. However, since H_{2}-rich regions host significant star formation and numerous supernova remnants, the morphology of observed H_{2} gas (as traced by CO line surveys) should also provide a physically motivated, high-resolution tracer for cosmic-ray injection. We assess the impact of utilizing H_{2} as a tracer for cosmic-ray injection on models of diffuse Galactic γ-ray emission. We employ state-of-the-art 3D particle diffusion and gas density models, along with a physical model for the star-formation rate based on global Schmidt laws. Allowing a fraction, f_{H_{2}}, of cosmic-ray sources to trace the observed H_{2} density, we find that a theoretically well-motivated value f_{H_{2}}∼0.20-0.25 (i) provides a significantly better global fit to the diffuse Galactic γ-ray sky and (ii) highly suppresses the intensity of the residual γ-ray emission from the Galactic center region. Specifically, in models utilizing our best global fit values of f_{H_{2}}∼0.20-0.25, the spectrum of the galactic center γ-ray excess is drastically affected, and the morphology of the excess becomes inconsistent with predictions for dark matter annihilation.

  4. Current correlators and form factors in the resonance region

    Energy Technology Data Exchange (ETDEWEB)

    Rosell, I. [Departamento de Ciencias Fisicas, Matematicas y de la Computacion, Universidad CEU Cardenal Herrera, c/Sant Bartomeu 55, E-46115 Alfara del Patriarca, Valencia (Spain); IFIC, Universitat de Valencia - CSIC, Apt. Correus 22085, E-46071 Valencia (Spain)

    2009-01-15

    Within Resonance Chiral Theory and in the context of QCD current correlators at next-to-leading order in 1/N{sub C}, we have analyzed the two-body form factors which include resonances as a final state. The short-distance constraints have been studied. One of the main motivations is the estimation of the chiral low-energy constants at subleading order, that is, keeping full control of the renormalization scale dependence. As an application we show the resonance estimation of some coupling, L{sub 10}{sup r}({mu}{sub 0})=(-4.4{+-}0.9).10{sup -3} and C{sub 87}{sup r}({mu}{sub 0})=(3.1{+-}1.1).10{sup -5}.

  5. Physical properties of star-forming regions across the Galaxy

    Science.gov (United States)

    Dunham, Miranda Kay

    2010-12-01

    The Bolocam Galactic Plane Survey (BGPS) has surveyed the northern Galactic plane at 1.1 mm and detected 8,358 sources. The BGPS catalog is large enough to characterize the properties of massive star formation in a statistically significant way. In this dissertation, I have conducted a survey of NH2 lines toward 771 BGPS sources located throughout the Galactic plane. The NH2 and 1.1 mm continuum observations together have allowed for complete characterization of the physical properties of these sources. I detected the NH2(1,1) line toward 408 BGPS sources in the inner Galaxy, allowing for determination of their kinematic distances. At distances less than roughly 1 kpc, the BGPS detects predominately cores which will form a single star or small multiple system, while at distances between 1 and 7 kpc the BGPS detects predominately clumps which will form entire stellar clusters. At distances greater than 7 kpc, the BGPS detects the large scale clouds which contain clumps and cores. I have correlated the BGPS catalog with mid-IR catalogs of massive young stellar objects (MYSOs), and found that 49% of the BGPS sources contain signs of active star formation. The masses, densities, H2 and NH2 column densities, gas kinetic temperatures, and NH2 velocity dispersions are higher in BGPS sources with associated mid-IR sources. I have also studied the physical properties of the BGPS sources as a function of Galactocentric radius, R[subscript Gal]. I find that the mean radius and mass decrease with increasing R[subscript Gal] but peak within the 5 kpc molecular ring where the gas kinetic temperature reaches a minimum. The fraction of BGPS sources with associated mid-IR sources decreases by 10% within the molecular ring. I postulate that these trends can be explained by an ambient gas density which decreases with R[subscript Gal], but peaks within the molecular ring. Similarly, the NH2 column density and abundance decrease by almost an order! of magnitude from the inner to outer

  6. Problems forming innovative-technological image of russian regions

    Directory of Open Access Journals (Sweden)

    Irina Markovna Golova

    2012-06-01

    Full Text Available In this paper, actual problems of innovative-technological image as a key element of the mechanism of the healing sources of socioeconomic development of the Russian regionsare considered. The author gives an assessment of the level of differentiation of subjects of the Russian Federation on the potential for innovative development. Trends in spatial transformations of thescientific and technical and innovation capacities of the country are analyzedand reasons of low innovational activity of Russian enterprises are disclosed. Basic conditions for the success of actions to create an attractive image of innovative-technological territory are formulated. Special attention is paid to the position of regions as participants in the innovational processes, creating preconditions for creativity, harmonization of spatial priorities of innovation, technological and socio-economic development, support for the development of new high-tech industries, improvement of inter-budgetary relations. There are proved priority areas of state policy to reduce barriers to the realization of an innovative paradigm for development of Russian society and effective inclusion of local communities in the implementation of innovative changes.

  7. Physical environment of massive star-forming region W42

    CERN Document Server

    Dewangan, L K; Ojha, D K; Anandarao, B G; Mallick, K K; Mayya, Y D

    2015-01-01

    We present an analysis of multi-wavelength observations from various datasets and Galactic plane surveys to study the star formation process in the W42 complex. A bipolar appearance of W42 complex is evident due to the ionizing feedback from the O5-O6 type star in a medium that is highly inhomogeneous. The VLT/NACO adaptive-optics K and L' images (resolutions ~0".2-0".1) resolved this ionizing source into multiple point-like sources below ~5000 AU scale. The position angle ~15 deg of W42 molecular cloud is consistent with the H-band starlight mean polarization angle which in turn is close to the Galactic magnetic field, suggesting the influence of Galactic field on the evolution of the W42 molecular cloud. Herschel sub-millimeter data analysis reveals three clumps located along the waist axis of the bipolar nebula, with the peak column densities of ~3-5 x10^{22} cm^{-2} corresponding to visual extinctions of AV ~32-53.5 mag. The Herschel temperature map traces a temperature gradient in W42, revealing regions ...

  8. Combining regional expertise to form a bereavement support alliance.

    Science.gov (United States)

    Friedrichs, Judy B; Kobler, Kathie; Roose, Rosmarie E; Meyer, Charlotte; Schmitz, Nancy; Kavanaugh, Karen

    2014-01-01

    Providing compassionate bereavement care for families experiencing perinatal loss is a standard of care in most healthcare organizations. In this article, we describe the development of The Alliance of Perinatal Bereavement Support Facilitators, begun over 25 years ago in Chicago by staff who identified the need to reach out to colleagues at other area institutions for advice and support in this work. This collaboration created a regional support network that has resulted in a long-lasting, active, sustainable organization of excellence focused on enhancing practice, education, and perinatal bereavement care. Alliance activities center around four main areas: education, networking/support, policy, and recognizing outstanding service to families. By continuing to draw upon the collective talent, wisdom, and expertise of its members, The Alliance still serves grieving families and provides mentoring for future interdisciplinary team members engaged in this work. The path taken to build this organization can be used by professionals in other specialties who are looking to create their own alliance infrastructure based on mutual benefit and interest.

  9. Stars and Star Clusters: A Look at Intermediate-Mass Star-Forming Regions

    Science.gov (United States)

    Lundquist, Michael J.; Kobulnicky, Henry A.; Lau, Ryan M.

    2017-01-01

    Star-forming regions hosting intermediate-mass stars straddle the boundary separating the the low- and high-mass regimes. These intermediate-mass star-forming regions can be used to probe this transition from low- to high-mass star formation. Our team has assembled an all-sky catalog of 616 candidate intermediate-mass star forming regions (IMSFRs) selected by IRAS colors and refined by visual inspection of WISE imagery. We present here two outer-Galaxy star-forming regions, IRAS22451+6154 and IRAS23448+6010, that despite having similar IRAS colors and mid-infrared morphologies, have vastly different stellar content. We combine Gemini and IRTF NIR spectroscopy with WIYN and SOFIA imaging for a thorough look at the stellar content of these two regions.

  10. MAJOR CHANNELS OF FORMING THE IMAGE OF A REGION ON THE INTERNET

    Directory of Open Access Journals (Sweden)

    Svetlana Lashova

    2015-01-01

    Full Text Available The article highlights the major channels of forming the image of a region on the Internet. The authors suppose that today the image of a region is formed as a certain communicative stream, with participation of both official and unofficial subjects of communication. The article analyzes such major channels of forming the image of a region on the Internet as blogs and social network. As stated by the authors, the abovementioned channels shape, firstly, the image which is expected by the people; secondly, the Internet forms the real but not the ideal (official image of the territory. In conclusion it is pointed out that the official image should be formed considering the positioning of a region in spontaneous communicative streams.

  11. Measuring Nearby Star Forming Regions with the VLBA: from the Distance to the Dynamics

    CERN Document Server

    Torres, Rosa M

    2010-01-01

    This thesis is part of a large ongoing effort to determine the distance and structure of all star-forming regions within several hundred parsecs of the Sun using radio-interferometric observations. The main goals of this thesis were: (1) Find the mean distance to the two best-studied nearby regions of low-mass star-formation (Taurus and Ophiuchus) with accuracies (a few percent or better) one to two orders of magnitude better than the present values, (2) Explore the structure and dynamics of these star-forming regions, and (3) Study the stars themselves.

  12. A Study on Karst Morphology Forms in Manjil Region of Gilan Province

    Directory of Open Access Journals (Sweden)

    Sina Hajati Ziabari

    2014-07-01

    Full Text Available The purpose of this study is The Study on Karst Morphology Forms in Manjil Region of Gilan Province. Due to geological features and quantity and type of rainfalls in Gilan Province and other effective factors on formation and development of Karst and Karst water resources, it is necessary to study karst morphology forms of this region. This study has studied Manjil region. It has first studied and identified karst forms of the region and then considered their formation in relation to the regional tectonic and creation of water potentials. Karst morphology forms of the region were identified and the cause of their creation was specified. Among them, Dorfak Mountain with an altitude of 2714 m in the south- central part of Gilan Province in Rudbar City near to Manjil can be mentioned as an example. Also Manjil Cheshmeh Bad Cave with an altitude of 1400 m above sea level is among other karst phenomena of the region and is regarded as the most important karst phenomenon in Asmari limestone.

  13. The H II Region/PDR Connection: Self-Consistent Calculations of Physical Conditions in Star-Forming Regions

    CERN Document Server

    Abel, N P; Shaw, G; Van Hoof, P A M

    2005-01-01

    We have performed a series of calculations designed to reproduce infrared diagnostics used to determine physical conditions in star forming regions. We self-consistently calculate the thermal and chemical structure of an H II region and photodissociation region (PDR) that are in pressure equilibrium. This differs from previous work, which used separate calculations for each gas phase. Our calculations span a wide range of stellar temperatures, gas densities, and ionization parameters. We describe improvements made to the spectral synthesis code Cloudy that made these calculations possible. These include the addition of a molecular network with ~1000 reactions involving 68 molecular species and improved treatment of the grain physics. Data from the Spitzer First Look Survey, along with other archives, are used to derive important physical characteristics of the H II region and PDR. These include stellar temperatures, electron densities, ionization parameters, UV radiation flux, and PDR density. Finally, we cal...

  14. Near-Infrared Circular Polarization Survey in Star-Forming Regions: Correlations and Trends

    CERN Document Server

    Kwon, Jungmi; Hough, James H; Kusakabe, Nobuhiko; Nagata, Tetsuya; Nakajima, Yasushi; Lucas, Phil W; Nagayama, Takahiro; Kandori, Ryo

    2014-01-01

    We have conducted a systematic near-infrared circular polarization (CP) survey in star-forming regions, covering high-mass, intermediate-mass, and low-mass young stellar objects. All the observations were made using the SIRPOL imaging polarimeter on the Infrared Survey Facility 1.4 m telescope at the South African Astronomical Observatory. We present the polarization properties of ten sub-regions in six star-forming regions. The polarization patterns, extents, and maximum degrees of linear and circular polarizations are used to determine the prevalence and origin of CP in the star-forming regions. Our results show that the CP pattern is quadrupolar in general, the CP regions are extensive, up to 0.65 pc, the CP degrees are high, up to 20 %, and the CP degrees decrease systematically from high- to low-mass young stellar objects. The results are consistent with dichroic extinction mechanisms generating the high degrees of CP in star forming regions.

  15. Commuting behaviour and urban form: a longitudinal study of a polycentric urban region in Denmark

    DEFF Research Database (Denmark)

    Grunfelder, Julien; Nielsen, Thomas Alexander Sick

    2012-01-01

    This paper is an empirical investigation of the relation between urban form and commuting behaviour in a polycentric urban region. It explores to what extent urban form and location variables help to explain commuting time, distance and mode based on an empirical case, East Jutland, which...... is a polycentric urban region in Denmark. Data from the National Transport Survey of Denmark were used for this quantitative analysis and two time periods were selected to highlight any potential changes over time. Empirical findings indicate that urban form and location variables help to explain the three...... selected aspects of commuting. However, urban form variables have greater explanatory power in explaining commuting modes than commuting time and commuting distance. No general trends in commuting were detectable from the data. Finally, the empirical findings revealed specificities of the case study...

  16. a Census of Medium-Mass Star-Forming Regions Within 1 KPC

    Science.gov (United States)

    Barnes, Peter J.; Myers, Philip C.; Burton, Michael G.

    We have used 13CO to associate kinematic distances for a sample of prospective medium-mass star-forming regions in the southern Milky Way. This complements the equivalent northern survey already completed and we present a valuable new source list for galactic star formation studies comprising dozens of previously unrecognised such regions. We also present preliminary results of maps of C18O CS and/or NH3 emission from these sources and analysis of these sources' spectral energy distributions.

  17. Looking for outflow and infall signatures in high mass star forming regions

    CERN Document Server

    Klaassen, P D; Beuther, H

    2011-01-01

    (Context) Many physical parameters change with time in star forming regions. Here we attempt to correlate changes in infall and outflow motions in high mass star forming regions with evolutionary stage using JCMT observations. (Aims) From a sample of 45 high mass star forming regions in three phases of evolution, we investigate the presence of established infall and outflow tracers to determine whether there are any trends attributable to the age of the source. (Methods) We obtained JCMT observations of HCO+/H13CO+ J=4-3 to trace large scale infall, and SiO J=8-7 to trace recent outflow activity. We compare the infall and outflow detections to the evolutionary stage of the host source (high mass protostellar objects, hypercompact HII regions and ultracompact HII regions). We also note that the integrated intensity of SiO varies with the full width at half maximum of the H13CO+. (Results) We find a surprising lack of SiO detections in the middle stage (Hypercompact HII regions), which may be due to an observat...

  18. YOUNG STELLAR OBJECTS IN THE MASSIVE STAR-FORMING REGION W49

    Energy Technology Data Exchange (ETDEWEB)

    Saral, G.; Hora, J. L.; Willis, S. E. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Koenig, X. P. [Yale University, Department of Astronomy, 208101, New Haven, CT 06520-8101 (United States); Gutermuth, R. A. [University of Massachusetts, Department of Astronomy, Amherst, MA 01003 (United States); Saygac, A. T., E-mail: gsaral@cfa.harvard.edu [Istanbul University, Faculty of Science, Astronomy and Space Sciences Department, Istanbul-Turkey (Turkey)

    2015-11-01

    We present the initial results of our investigation of the star-forming complex W49, one of the youngest and most luminous massive star-forming regions in our Galaxy. We used Spitzer/Infrared Array Camera (IRAC) data to investigate massive star formation with the primary objective of locating a representative set of protostars and the clusters of young stars that are forming around them. We present our source catalog with the mosaics from the IRAC data. In this study we used a combination of IRAC, MIPS, Two Micron All Sky Survey, and UKIRT Deep Infrared Sky Survey (UKIDSS) data to identify and classify the young stellar objects (YSOs). We identified 232 Class 0/I YSOs, 907 Class II YSOs, and 74 transition disk candidate objects using color–color and color–magnitude diagrams. In addition, to understand the evolution of star formation in W49, we analyzed the distribution of YSOs in the region to identify clusters using a minimal spanning tree method. The fraction of YSOs that belong to clusters with ≥7 members is found to be 52% for a cutoff distance of 96″, and the ratio of Class II/I objects is 2.1. We compared the W49 region to the G305 and G333 star-forming regions and concluded that W49 has the richest population, with seven subclusters of YSOs.

  19. Studying cooling mechanisms in the massive star forming region IRAS 12326-6245

    NARCIS (Netherlands)

    Dedes, C.; Herpin, F.; Chavarria, L.; Wampfler, S.; Wyrowski, F.; van der Tak, F.; Benz, A.; Bruderer, D.; Polehampton, E.; Melchior, M.

    2011-01-01

    The strong feedback processes of massive stars influence the surrounding ISM both locally and on large scales. An important question to be answered is the one of cooling and heating in massive star forming regions. There, heating is provided mostly by far-UV (FUV) and infra-red radiation. Cooling is

  20. Looking for phase-space structures in star-forming regions: an MST-based methodology

    Science.gov (United States)

    Alfaro, Emilio J.; González, Marta

    2016-03-01

    We present a method for analysing the phase space of star-forming regions. In particular we are searching for clumpy structures in the 3D sub-space formed by two position coordinates and radial velocity. The aim of the method is the detection of kinematic segregated radial velocity groups, that is, radial velocity intervals whose associated stars are spatially concentrated. To this end we define a kinematic segregation index, tilde{Λ }(RV), based on the Minimum Spanning Tree graph algorithm, which is estimated for a set of radial velocity intervals in the region. When tilde{Λ }(RV) is significantly greater than 1 we consider that this bin represents a grouping in the phase space. We split a star-forming region into radial velocity bins and calculate the kinematic segregation index for each bin, and then we obtain the spectrum of kinematic groupings, which enables a quick visualization of the kinematic behaviour of the region under study. We carried out numerical models of different configurations in the sub-space of the phase space formed by the coordinates and the that various case studies illustrate. The analysis of the test cases demonstrates the potential of the new methodology for detecting different kind of groupings in phase space.

  1. Hierarchical star formation in M33 : fundamental properties of the star-forming regions

    NARCIS (Netherlands)

    Bastian, N.; Ercolano, B.; Gieles, M.; Rosolowsky, E.; Scheepmaker, R.A.; Gutermuth, R.; Efremov, Y.

    2007-01-01

    Star formation within galaxies appears on multiple scales, from spiral structure, to OB associations, to individual star clusters, and often substructure within these clusters. This multitude of scales calls for objective methods to find and classify star-forming regions, regardless of spatial size.

  2. Wide-Field Infrared Survey Explorer Observations of the Evolution of Massive Star-Forming Regions

    Science.gov (United States)

    Koenig, X. P.; Leisawitz, D. T.; Benford, D. J.; Rebull, L. M.; Padgett, D. L.; Asslef, R. J.

    2012-01-01

    We present the results of a mid-infrared survey of II outer Galaxy massive star-forming regions and 3 open clusters with data from the Wide-field Infrared Survey Explorer (WISE). Using a newly developed photometric scheme to identify young stellar objects and exclude extragalactic contamination, we have studied the distribution of young stars within each region. These data tend to support the hypothesis that latter generations may be triggered by the interaction of winds and radiation from the first burst of massive star formation with the molecular cloud material leftover from that earlier generation of stars. We dub this process the "fireworks hypothesis" since star formation by this mechanism would proceed rapidly and resemble a burst of fireworks. We have also analyzed small cutout WISE images of the structures around the edges of these massive star-forming regions. We observe large (1-3 pc size) pillar and trunk-like structures of diffuse emission nebulosity tracing excited polycyclic aromatic hydrocarbon molecules and small dust grains at the perimeter of the massive star-forming regions. These structures contain small clusters of emerging Class I and Class II sources, but some are forming only a single to a few new stars.

  3. H{\\alpha} to FUV ratios in resolved star forming region populations of nearby spiral galaxies

    CERN Document Server

    Hermanowicz, Maciej T; Eldridge, John J

    2013-01-01

    We present a new study of H{\\alpha}/FUV flux ratios of star forming regions within a sample of nearby spiral galaxies. We search for evidence of the existence of a cluster mass dependent truncation in the underlying stellar initial mass function (IMF). We use an automated approach to identification of extended objects based on the SExtractor algorithm to catalogue resolved Hii regions within a set of nearby spiral galaxies. Corrections due to dust attenuation effects are applied to avoid artificially boosted H{\\alpha}/FUV values. We use the BPASS stellar population synthesis code of Eldridge & Stanway (2009) to create a benchmark population of star forming regions to act as a reference for our observations. Based on those models, we identify a zone of parameter space populated by regions that cannot be obtained with a cluster mass dependent truncation in the stellar IMF imposed. We find that the investigated galaxies display small subpopulations of star forming regions falling within our zone of interest,...

  4. The Incidence of Highly-Obscured Star-Forming Regions in SINGS Galaxies

    CERN Document Server

    Prescott, Moire K M; Bendo, George J; Buckalew, Brent A; Calzetti, Daniela; Engelbracht, Charles W; Gordon, Karl D; Hollenbach, David J; Lee, Janice C; Moustakas, John; Dale, Daniel A; Helou, George; Jarrett, Thomas H; Murphy, Eric J; Smith, John David T; Akiyama, Sanae; Sosey, Megan L; George J. Bendo Astrophysics Group, Imperial College

    2007-01-01

    Using the new capabilities of the Spitzer Space Telescope and extensive multiwavelength data from the Spitzer Infrared Nearby Galaxies Survey (SINGS), it is now possible to study the infrared properties of star formation in nearby galaxies down to scales equivalent to large HII regions. We are therefore able to determine what fraction of large, infrared-selected star-forming regions in normal galaxies are highly obscured and address how much of the star formation we miss by relying solely on the optical portion of the spectrum. Employing a new empirical method for deriving attenuations of infrared-selected star-forming regions we investigate the statistics of obscured star formation on 500pc scales in a sample of 38 nearby galaxies. We find that the median attenuation is 1.4 magnitudes in H-alpha and that there is no evidence for a substantial sub-population of uniformly highly-obscured star-forming regions. The regions in the highly-obscured tail of the attenuation distribution (A_H-alpha > 3) make up only ~...

  5. 13C Isotopic Fractionation of HC3N in Star-Forming Regions -Low-Mass Star Forming Region L1527 and High-Mass Star Forming Region G28.28-0.36-

    CERN Document Server

    Taniguchi, Kotomi; Ozeki, Hiroyuki

    2016-01-01

    We observed the J=9-8 and 10-9 rotational lines of three13C isotopologues of HC3N in L1527 and G28.28-0.36 with the 45-m radio telescope of the Nobeyama Radio Observatory in order to constrain the main formation mechanisms of HC3N in each source. The abundance ratios of the three 13C isotopologues of HC3N are found to be 0.9 (0.2) : 1.00 : 1.29 (0.19) (1sigma) and 1.0 (0.2) : 1.00 : 1.47 (0.17) (1sigma) for [H13CCCN]: [HC13CCN]: [HCC13CN] in L1527 and G28.28-0.36, respectively. We recognize a similar 13C isotopic fractionation pattern that the abundances of H13CCCN and HC13CCN are comparable, and HCC13CN is more abundant than the others. Based on the results, we discuss the main formation pathway of HC3N. The 13C isotopic fractionation pattern derived from our observations can be explained by the neutral-neutral reaction between C2H2 and CN in both the low-mass (L1527) and high-mass (28.28-0.36) star forming regions.

  6. Tomography of Galactic star-forming regions and spiral arms with the Square Kilometer Array

    CERN Document Server

    Loinard, Laurent; Hoare, Melvin; van Langevelde, Huib Jan; Ellingsen, Simon; Brunthaler, Andreas; Forbrich, Jan; Rygl, Kazi L J; Rodriguez, Luis F; Mioduszewski, Amy J; Torres-Lopez, Rosa M; Dzib, Sergio A; Ortiz-Leon, Gisela N; Bourke, Tyler L; Green, James A

    2014-01-01

    Very Long Baseline Interferometry (VLBI) at radio wavelengths can provide astrometry accurate to 10 micro-arcseconds or better (i.e. better than the target GAIA accuracy) without being limited by dust obscuration. This means that unlike GAIA, VLBI can be applied to star-forming regions independently of their internal and line-of-sight extinction. Low-mass young stellar objects (particularly T Tauri stars) are often non-thermal compact radio emitters, ideal for astrometric VLBI radio continuum experiments. Existing observations for nearby regions (e.g. Taurus, Ophiuchus, or Orion) demonstrate that VLBI astrometry of such active T Tauri stars enables the reconstruction of both the regions' 3D structure (through parallax measurements) and their internal kinematics (through proper motions, combined with radial velocities). The extraordinary sensitivity of the SKA telescope will enable similar "tomographic mappings" to be extended to regions located several kpc from Earth, in particular to nearby spiral arm segmen...

  7. The Gaia-ESO Survey: metallicity of the Chamaeleon I star forming region

    CERN Document Server

    Spina, L; Palla, F; Biazzo, K; Sacco, G G; Alfaro, E J; Franciosini, E; Magrini, L; Morbidelli, L; Frasca, A; Adibekyan, V; Delgado-Mena, E; Sousa, S G; Hernandez, J I Gonzalez; Montes, D; Tabernero, H; Tautvaisiene, G; Bonito, R; Lanzafame, A C; Gilmore, G; Jeffries, R D; Vallenari, A; Bensby, T; Bragaglia, A; Flaccomio, E; Korn, A J; Pancino, E; Recio-Blanco, A; Smiljanic, R; Bergemann, M; Costado, M T; Damiani, F; Hill, V; Hourihane, A; Jofre, P; de Laverny, P; Lardo, C; Masseron, T; Prisinzano, L; Worley, C C

    2014-01-01

    Context. Recent metallicity determinations in young open clusters and star-forming regions suggest that the latter may be characterized by a slightly lower metallicity than the Sun and older clusters in the solar vicinity. However, these results are based on small statistics and inhomogeneous analyses. The Gaia-ESO Survey is observing and homogeneously analyzing large samples of stars in several young clusters and star-forming regions, hence allowing us to further investigate this issue. Aims. We present a new metallicity determination of the Chamaeleon I star-forming region, based on the products distributed in the first internal release of the Gaia-ESO Survey. Methods. 48 candidate members of Chamaeleon I have been observed with the high-resolution spectrograph UVES. We use the surface gravity, lithium line equivalent width and position in the Hertzsprung-Russell diagram to confirm the cluster members and we use the iron abundance to derive the mean metallicity of the region. Results. Out of the 48 targets,...

  8. Looking for phase-space structures in star-forming regions: An MST-based methodology

    CERN Document Server

    Alfaro, Emilio J

    2015-01-01

    We present a method for analysing the phase space of star-forming regions. In particular we are searching for clumpy structures in the 3D subspace formed by two position coordinates and radial velocity. The aim of the method is the detection of kinematic segregated radial velocity groups, that is, radial velocity intervals whose associated stars are spatially concentrated. To this end we define a kinematic segregation index, $\\tilde{\\Lambda}$(RV), based on the Minimum Spanning Tree (MST) graph algorithm, which is estimated for a set of radial velocity intervals in the region. When $\\tilde{\\Lambda}$(RV) is significantly greater than 1 we consider that this bin represents a grouping in the phase space. We split a star-forming region into radial velocity bins and calculate the kinematic segregation index for each bin, and then we obtain the spectrum of kinematic groupings, which enables a quick visualization of the kinematic behaviour of the region under study. We carried out numerical models of different config...

  9. Phase-space structures and stellar populations in the star-forming region NGC~ 2264

    CERN Document Server

    Gonzalez, Marta

    2016-01-01

    In this work we analyse the structure of a subspace of the phase space of the star-forming region NGC~ 2264 using the Spectrum of Kinematic Groupings (SKG). We show that the SKG can be used to process a collection of star data to find substructure at different scales. We have found structure associated with the NGC~ 2264 region and also with the background area. In the NGC~ 2264 region, a hierarchical analysis shows substructure compatible with that found in previous specific studies of the area but with an objective, compact methodology that allows us to homogeneously compare the structure of different clusters and star-forming regions. Moreover, this structure is compatible with the different ages of the main NGC~ 2264 star-forming populations. The structure found in the field can be roughly associated with giant stars far in the background, dynamically decoupled from NGC~ 2264, which could be related either with the Outer Arm or Monoceros Ring. The results in this paper confirm the relationship between str...

  10. Phase-space structures and stellar populations in the star-forming region NGC 2264

    Science.gov (United States)

    González, Marta; Alfaro, Emilio J.

    2017-02-01

    In this work, we analyse the structure of a subspace of the phase space of the star-forming region NGC 2264 using the spectrum of kinematic groupings (SKG). We show that the SKG can be used to process a collection of star data to find substructure at different scales. We have found structure associated with the NGC 2264 region and also with the background area. In the NGC 2264 region, a hierarchical analysis shows substructure compatible with that found in previous specific studies of the area but with an objective, compact methodology that allows us to homogeneously compare the structure of different clusters and star-forming regions. Moreover, this structure is compatible with the different ages of the main NGC 2264 star-forming populations. The structure found in the field can be roughly associated with giant stars far in the background, dynamically decoupled from NGC 2264, which could be related either with the Outer Arm or Monoceros Ring. The results in this paper confirm the relationship between structure in the radial velocity phase-space subspace and different kinds of populations, defined by other variables not necessarily analysed with the SKG, such as age or distance, showing the importance of detecting phase-space substructure in order to trace stellar populations in the broadest sense of the word.

  11. Delineating Partnerships from other Forms of Collaboration in Regional Development Planning

    DEFF Research Database (Denmark)

    Larsen, Peter Wilgaard

    2016-01-01

    literature depicts similar difficulties in delineating partnerships from other collaboration models causing diversified messages about partnerships. In an attempt to invigorate the partnership literature by delineating partnerships from other forms of collaboration and thus progress the work and output...... to delineate partnerships from other forms of collaboration such as networks, clusters and governance-partnerships.......The idea of an all-encompassing partnership has vindicated all sorts of collaboration models to be articulated as partnerships although not occurring as ones, leaving practitioners and politicians of regional development planning with suboptimal ways of collaborating. Reviewing the partnership...

  12. The Connection Between Galaxy Environment and the Luminosity Function Slopes of Star-Forming Regions

    CERN Document Server

    Cook, David O; Lee, Janice C; Thilker, David; Calzetti, Daniela; Kennicutt, Robert C

    2016-01-01

    We present the first study of GALEX far ultra-violet (FUV) luminosity functions of individual star-forming regions within a sample of 258 nearby galaxies spanning a large range in total stellar mass and star formation properties. We identify ~65,000 star-forming regions (i.e., FUV sources), measure each galaxy's luminosity function, and characterize the relationships between the luminosity function slope (alpha) and several global galaxy properties. A final sample of 82 galaxies with reliable luminosity functions are used to define these relationships and represent the largest sample of galaxies with the largest range of galaxy properties used to study the connection between luminosity function properties and galaxy environment. We find that alpha correlates with global star formation properties, where galaxies with higher star formation rates and star formation rate densities (Sigma_SFR) tend to have flatter luminosity function slopes. In addition, we find that neither stochastic sampling of the luminosity f...

  13. Outflows in massive star forming regions: UV radiation and shocked cavity walls toward AFGL 2591

    Science.gov (United States)

    Doty, Steven; Rogers, Noah; Doty, Sandra; van der Tak, Floris; van Dishoeck, Ewine

    2015-08-01

    Outflows can play an important role in regulating the star formation process. These outflows have the potential to deposit significant energy to large distances from the protostar through material motion and shocks, as well as via radiation through the subsequent outflow cavity. Herschel observations of high-J CO lines toward massive star-forming regions such as AFGL 2591 show line strengths that appear to be inconsistent with a spherical envelope. Following recent work on low-mass star forming regions, we construct a model whereby the excited molecular line emission originates in a shocked + UV irradiated outflow cavity wall. The validity of the cavity wall model in this context is considered. The observational data are then used to constrain the model, including the type of shocks, and relative strength of shocks versus radiation.

  14. On the Onset of Secondary Stellar Generations in Giant Star Forming Regions and Massive Star Clusters

    CERN Document Server

    Palouš, Jan; Tenorio-Tagle, Guillermo

    2014-01-01

    Here we consider the strong evolution experienced by the matter reinserted by massive stars, both in giant star forming regions driven by a constant star formation rate, and in massive and coeval superstar clusters. In both cases we take into consideration the changes induced by stellar evolution on the number of massive stars, the number of ionizing photons and the integrated mechanical luminosity of the star forming regions. The latter is at all times compared with the critical luminosity that defines, for a given size, the lower mechanical luminosity limit above which the matter reinserted via strong winds and supernova explosions suffers frequent and recurrent thermal instabilities that reduce its temperature and pressure and inhibit its exit as part of a global wind. Instead, the unstable reinserted matter is compressed by the pervasive hot gas, and photoionization maintains its temperature at T $\\sim$ 10$^4$ K. As the evolution proceeds, more unstable matter accumulates and the unstable clumps grow in s...

  15. The connection between galaxy environment and the luminosity function slopes of star-forming regions

    Science.gov (United States)

    Cook, David O.; Dale, Daniel A.; Lee, Janice C.; Thilker, David; Calzetti, Daniela; Kennicutt, Robert C.

    2016-11-01

    We present the first study of GALEX far-ultraviolet (FUV) luminosity functions of individual star-forming regions within a sample of 258 nearby galaxies spanning a large range in total stellar mass and star formation properties. We identify ˜65 000 star-forming regions (i.e. FUV sources), measure each galaxy's luminosity function, and characterize the relationships between the luminosity function slope (α) and several global galaxy properties. A final sample of 82 galaxies with reliable luminosity functions are used to define these relationships and represent the largest sample of galaxies with the largest range of galaxy properties used to study the connection between luminosity function properties and galaxy environment. We find that α correlates with global star formation properties, where galaxies with higher star formation rates and star formation rate densities (ΣSFR) tend to have flatter luminosity function slopes. In addition, we find that neither stochastic sampling of the luminosity function in galaxies with low-number statistics nor the effects of blending due to distance can fully account for these trends. We hypothesize that the flatter slopes in high ΣSFR galaxies is due to higher gas densities and higher star formation efficiencies which result in proportionally greater numbers of bright star-forming regions. Finally, we create a composite luminosity function composed of star-forming regions from many galaxies and find a break in the luminosity function at brighter luminosities. However, we find that this break is an artefact of varying detection limits for galaxies at different distances.

  16. The Schmidt Law in Six Galactic Massive Star-forming Regions

    Science.gov (United States)

    Willis, S.; Guzman, A.; Marengo, M.; Smith, H. A.; Martínez-Galarza, J. R.; Allen, L.

    2015-08-01

    We present a census of young stars in five massive star-forming regions in the 4th Galactic quadrant, G305, G326-4, G326-6, G333 (RCW 106), and G351, and combine this census with an earlier census of young stars in NGC 6334. Each region was observed at J, H, and Ks with the NOAO Extremely Wide-Field Infrared Imager and combined with deep observations taken with the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope at the wavelengths 3.6 and 4.5 μm. We derived a five band point-source catalog containing >200,000 infrared sources in each region. We have identified a total of 2871 YSO candidates, 363 Class I YSOs, and 2508 Class II YSOs. We mapped the column density of each cloud using observations from Herschel between 160 and 500 μm and near-infrared extinction maps in order to determine the average gas surface density above AV > 2. We study the surface density of the YSOs and the star-formation rate as a function of the column density within each cloud and compare them to the results for nearby star-forming regions. We find a range in power-law indices across the clouds, with the dispersion in the local relations in an individual cloud much lower than the average over the six clouds. We find the average over the six clouds to be {{{Σ }}}{SFR}∼ {{{Σ }}}{gas}2.15+/- 0.41 and power-law exponents ranging from 1.77 to 2.86, similar to the values derived within nearby star-forming regions, including Taurus and Orion. The large dispersion in the power-law relations between individual Milky Way molecular clouds reinforces the idea that there is not a direct universal connection between Σgas and a cloud's observed star-formation rate.

  17. The First Detections of the Key Prebiotic Molecule PO in Star-forming Regions

    Science.gov (United States)

    Rivilla, V. M.; Fontani, F.; Beltrán, M. T.; Vasyunin, A.; Caselli, P.; Martín-Pintado, J.; Cesaroni, R.

    2016-08-01

    Phosphorus is a crucial element in biochemistry, in particular the P-O bond, which is key in the formation of the backbone of deoxyribonucleic acid. So far, PO has only been detected toward the envelope of evolved stars, but never toward star-forming regions. We report the first detection of PO toward two massive star-forming regions, W51 e1/e2 and W3(OH), using data from the IRAM 30 m telescope. PN has also been detected toward the two regions. The abundance ratio PO/PN is 1.8 and 3 for W51 and W3(OH), respectively. Our chemical model indicates that the two molecules are chemically related and are formed via gas-phase ion-molecule and neutral-neutral reactions during cold collapse. The molecules freeze out onto grains at the end of the collapse and desorb during the warm-up phase once the temperature reaches ˜35 K. Similar abundances of the two species are expected during a period of ˜5 × 104 yr at the early stages of the warm-up phase, when the temperature is in the range 35-90 K. The observed molecular abundances of 10-10 are predicted by the model if a relatively high initial abundance of 5 × 10-9 of depleted phosphorus is assumed.

  18. High Circular Polarization in the Star Forming Region NGC 6334: Implications

    Science.gov (United States)

    Ménard, François; Chrysostomou, A.; Gledhill, T.; Hough, J. H.; Bailey, J.

    The amino-acids which form the building blocks of biological proteins are all left-handed molecules. By contrast, when these molecules are made in the laboratory equal numbers of the right and left-handed versions are made. This homochirality found in biological material may then well be a prerequisite for the origin of life and a number of processes have been proposed to produce the required enantiomeric excess in prebiotic organic molecules. We report here on the detection of high degrees of circular polarisation in the star forming complex NGC 6334, in the constellation Scorpius. This important finding suggests the widespread nature of a potentially efficient process to produce biomolecules with large chiral excess, namely selective (asymmetric) photolysis by circularly polarised light. The mechanism, well known in the laboratory, was first suggested to take place in a star forming region by Bailey et al. (1998) (Science, 281, 672; and this conference), following our discovery of high degrees of near-infrared circular polarisation in the Orion molecular cloud, OMC-1. NGC 6334 is a giant HII region and molecular cloud similar to Orion. These two detections of large circular polarisation, among the small number of sources surveyed so far, lead us to suggest that selective photolysis by circular polarisation may be quite widespread in massive star formation regions.

  19. Properties of dense cores in clustered massive star-forming regions at high angular resolution

    CERN Document Server

    Sanchez-Monge, Alvaro; Fontani, Francesco; Busquet, Gemma; Juarez, Carmen; Estalella, Robert; Tan, Jonathan C; Sepulveda, Inma; Ho, Paul T P; Zhang, Qizhou; Kurtz, Stan

    2013-01-01

    We aim at characterising dense cores in the clustered environments associated with massive star-forming regions. For this, we present an uniform analysis of VLA NH3(1,1) and (2,2) observations towards a sample of 15 massive star-forming regions, where we identify a total of 73 cores, classify them as protostellar, quiescent starless, or perturbed starless, and derive some physical properties. The average sizes and ammonia column densities are 0.06 pc and 10^15 cm^-2, respectively, with no significant differences between the starless and protostellar cores, while the linewidth and rotational temperature of quiescent starless cores are smaller, 1.0 km/s and 16 K, than those of protostellar (1.8 km/s, 21 K), and perturbed starless (1.4 km/s, 19 K) cores. Such linewidths and temperatures for these quiescent starless cores in the surroundings of massive stars are still significantly larger than the typical values measured in starless cores of low-mass star-forming regions, implying an important non-thermal compone...

  20. Rehabilitation of urban identity of cities in the Banja Luka region through urban form regulation

    Directory of Open Access Journals (Sweden)

    Simonović Dijana

    2013-01-01

    Full Text Available This paper points to the possibility of codification of urban planning and application of physical regulation standards in urban form design to establish such instruments of guidance as will ensure the recognition, appreciation and development of local urban identity. The purpose of establishing general principles and making quality recommendations that would aim at urban form design regulation and be implemented as qualitative criteria and regulation standards is to propose a methodology for the rehabilitation of the City of Banja Luka’s identity applicable to similar cities in the region, with due adjustments to allow for contextual specificity, with the possibility of coordinated regional city development. The discontinuity in the urban development of Banja Luka and other cities in the region has jeopardised the inherent characteristics of their identities, resulting in reduced recognisability and impaired integrity. This study covers the period since the beginning of Banja Luka’s guided urban development (Austro-Hungarian administration, 1878, which should allow a review of its urban morphogenesis and an understanding of its key elements, as well as identification of the general principles and rules of urban form regulation as laid down in the local ordinance and planning legacy.

  1. First detections of the key prebiotic molecule PO in star-forming regions

    CERN Document Server

    Rivilla, V M; Beltrán, M T; Vasyunin, A; Caselli, P; Martín-Pintado, J; Cesaroni, R

    2016-01-01

    Phosphorus is a crucial element in biochemistry, especially the P-O bond, which is key for the formation of the backbone of the deoxyribonucleic acid. So far, PO has only been detected towards the envelope of evolved stars, and never towards star-forming regions. We report the first detection of PO towards two massive star-forming regions, W51 e1/e2 and W3(OH), using data from the IRAM 30m telescope. PN has also been detected towards the two regions. The abundance ratio PO/PN is 1.8 and 3 for W51 and W3(OH), respectively. Our chemical model indicates that the two molecules are chemically related and are formed via gas-phase ion-molecule and neutral-neutral reactions during the cold collapse. The molecules freeze out onto grains at the end of the collapse and desorb during the warm-up phase once the temperature reaches 35 K. Similar abundances of the two species are expected during a period of 5x10^{4} yr at the early stages of the warm-up phase, when the temperature is in the range 35-90 K. The observed molec...

  2. The Charon-forming giant impact as a source of Pluto's dark equatorial regions

    Science.gov (United States)

    Sekine, Yasuhito; Genda, Hidenori; Kamata, Shunichi; Funatsu, Taro

    2017-01-01

    Pluto exhibits complex regional diversity in its surface materials 1,2 . One of the most striking features is the dark reddish material, possibly organic matter, along Pluto's equator coexisting with the H2O-rich crust 2 . Little is known, however, about the surface process responsible for the dark equatorial regions. Here, we propose that Pluto's dark regions were formed through reactions in elongated pools of liquid water near the equator, generated by the giant impact that formed Charon 3-5 . Our laboratory experiments show that dark reddish organic matter, comparable to Pluto's dark materials, is produced through polymerization of simple organic compounds 6,7 that would have been present in proto-Pluto (for example, formaldehyde) by prolonged heating at temperatures ≥50 °C. Through hydrodynamic impact simulations, we demonstrate that an impactor, one-third the mass of Pluto, colliding with proto-Pluto—with an interior potential temperature of 150-200 K—could have generated both a Charon-sized satellite and high-temperature regions around Pluto's equator. We also propose that high-velocity giant impacts result in global or hemispherical darkening and reddening, suggesting that the colour variety of large Kuiper belt objects 8-12 could have been caused by frequent, stochastic giant impacts in a massive outer protoplanetary disk in the early Solar System 13-16 .

  3. Parsec-scale X-ray Flows in High-mass Star-forming Regions

    CERN Document Server

    Townsley, L K; Feigelson, E D; Garmire, G P

    2005-01-01

    The Chandra X-ray Observatory is providing remarkable new views of massive star-forming regions, revealing all stages in the life cycle of high-mass stars and their effects on their surroundings. We present a Chandra tour of several high-mass star-forming regions, highlighting physical processes that characterize the life of a cluster of high-mass stars, from deeply-embedded cores too young to have established an HII region to superbubbles so large that they shape our views of galaxies. Along the way we see that X-ray observations reveal hundreds of stellar sources powering great HII region complexes, suffused by both hard and soft diffuse X-ray structures caused by fast O-star winds thermalized in wind-wind collisions or by termination shocks against the surrounding media. Finally, we examine the effects of the deaths of high-mass stars that remained close to their birthplaces, exploding as supernovae within the superbubbles that these clusters created. We present new X-ray results on W51 IRS2E and 30 Doradu...

  4. Kinematic structure of massive star-forming regions - I. Accretion along filaments

    CERN Document Server

    Tackenberg, J; Henning, Th; Linz, H; Sakai, T; Ragan, S E; Krause, O; Nielbock, M; Hennemann, M; Pitann, J; Schmiedeke, A

    2014-01-01

    The mid- and far-infrared view on high-mass star formation, in particular with the results from the Herschel space observatory, has shed light on many aspects of massive star formation. However, these continuum studies lack kinematic information. We study the kinematics of the molecular gas in high-mass star-forming regions. We complemented the PACS and SPIRE far-infrared data of 16 high-mass star-forming regions from the Herschel key project EPoS with N2H+ molecular line data from the MOPRA and Nobeyama 45m telescope. Using the full N2H+ hyperfine structure, we produced column density, velocity, and linewidth maps. These were correlated with PACS 70micron images and PACS point sources. In addition, we searched for velocity gradients. For several regions, the data suggest that the linewidth on the scale of clumps is dominated by outflows or unresolved velocity gradients. IRDC18454 and G11.11 show two velocity components along several lines of sight. We find that all regions with a diameter larger than 1pc sho...

  5. Outflow and Infall in a Sample of Massive Star Forming Regions II: Large Scale Kinematics

    CERN Document Server

    Klaassen, P D

    2008-01-01

    We present maps of seven sources selected from Klaassen & Wilson (2007a) in SiO (J=8-7) and HCO$^+$ and H$^{13}$CO$^+$ (J=4-3) which were obtained using HARP-B on the James Clerk Maxwell Telescope. We find that four out of our seven sources have infall signatures based on their HCO$^+$ emission profiles. From our maps, we have determined the extent of both the outflowing and infalling regions towards these sources, and constrained the amount of infalling and outflowing mass as well as the mass infall rate for each massive star forming region. From our SiO observations, we estimate the source luminosity required to shock the surroundings of these massive star forming regions and find luminosities similar to those of the HII regions themselves. We find that the ratio between our infall and outflow masses is less than one, suggesting high mass entrainment rates in the molecular outflows. We also find that the large scale molecular infall rate towards G10.6-0.4 is comparable to the small scale molecular infal...

  6. Far and mid-infrared studies of star forming regions : Probing their thermal balance, chemistry and evolution

    NARCIS (Netherlands)

    Koumpia, Evgenia

    2016-01-01

    The goal of this thesis is to understand the physical and chemical processes that take place in regions forming stars, in particular during the early evolutionary stages of star formation. Why do we care about stars and star forming regions? Many elements on Earth were once formed in the heart of a

  7. Radio and infrared study of the star-forming region IRAS 20286+4105

    Science.gov (United States)

    Ramachandran, Varsha; Das, S. R.; Tej, A.; Vig, S.; Ghosh, S. K.; Ojha, D. K.

    2017-03-01

    In this paper, we present a multiwavelength investigation of the star-forming complex IRAS 20286+4105, located in the Cygnus X region. Near-infrared K-band data are used to revisit the cluster/stellar group identified in previous studies. Radio continuum observations at 610 and 1280 MHz show the presence of a H II region possibly powered by a star of spectral type B0-B0.5. The cometary morphology of the ionized region is explained by invoking the bow-shock model, where the likely association with a nearby supernova remnant is also explored. A compact radio knot with a non-thermal spectral index is detected towards the centre of the cloud. Mid-infrared data from the Spitzer Legacy Survey of the Cygnus X region show the presence of six Class I young stellar objects inside the cloud. Thermal dust emission in this complex is modelled using Herschel far-infrared data to generate dust temperature and column density maps. Herschel images also show the presence of two clumps in this region, the masses of which are estimated to be ∼175 and 30 M⊙. The mass-radius relation and the surface density of the clumps mean that they do not qualify as massive star-forming sites. An overall picture of a runaway star ionizing the cloud and a triggered population of intermediate-mass, Class I sources located towards the cloud centre emerges from this multiwavelength study. Variation in the dust emissivity spectral index is shown to exist in this region and is seen to have an inverse relation with the dust temperature.

  8. Millimetre spectral line mapping observations towards four massive star-forming H II regions

    Science.gov (United States)

    Li, Shanghuo; Wang, Junzhi; Zhang, Zhi-Yu; Fang, Min; Li, Juan; Zhang, Jiangshui; Fan, Junhui; Zhu, Qingfeng; Li, Fei

    2017-04-01

    We present spectral line mapping observations towards four massive star-forming regions - Cepheus A, DR21S, S76E and G34.26+0.15 - with the IRAM 30-m telescope at the 2 and 3 mm bands. In total, 396 spectral lines from 51 molecules, one helium recombination line, 10 hydrogen recombination lines and 16 unidentified lines were detected in these four sources. An emission line of nitrosyl cyanide (ONCN, 140, 14-130, 13) was detected in G34.26+0.15, as the first detection in massive star-forming regions. We found that c-C3H2 and NH2D show enhancement in shocked regions, as suggested by the evidence of SiO and/or SO emission. The column density and rotational temperature of CH3CN were estimated with the rotational diagram method for all four sources. Isotope abundance ratios of 12C/13C were derived using HC3N and its 13C isotopologue, which were around 40 in all four massive star-forming regions and slightly lower than the local interstellar value (∼65). The 14N/15N and 16O/18O abundance ratios in these sources were also derived using the double isotopic method, which were slightly lower than in the local interstellar medium. Except for Cep A, the 33S/34S ratios in the other three targets were derived, which were similar to that in the local interstellar medium. The column density ratios of N(DCN)/N(HCN) and N(DCO+)/N(HCO+) in these sources were more than two orders of magnitude higher than the elemental [D]/[H] ratio, which is 1.5 × 10-5. Our results show that the later stage sources, G34.26+0.15 in particular, present more molecular species than earlier stage sources. Evidence of shock activity is seen in all stages studied.

  9. Different Evolutionary Stages in the Massive Star Forming Region S255 Complex

    CERN Document Server

    Wang, Y; Bik, A; Vasyunina, T; Jiang, Z; Puga, E; Linz, H; Rodon, J A; Henning, Th; Tamura, M

    2010-01-01

    To understand evolutionary and environmental effects during the formation of high-mass stars, we observed three regions of massive star formation at different evolutionary stages that reside in the same natal molecular cloud. Methods. The three regions S255IR, S255N and S255S were observed at 1.3 mm with the Submillimeter Array (SMA) and followup short spacing information was obtained with the IRAM 30m telescope. Near infrared (NIR) H + K-band spectra and continuum observations were taken for S255IR with VLT-SINFONI to study the different stellar populations in this region. The combination of millimeter (mm) and near infrared data allow us to characterize different stellar populations within the young forming cluster in detail. While we find multiple mm continuum sources toward all regions, their outflow, disk and chemical properties vary considerably. The most evolved source S255IR exhibits a collimated bipolar outflow visible in CO and H2 emission, the outflows from the youngest region S255S are still small...

  10. Radio and infrared study of the star forming region IRAS 20286+4105

    CERN Document Server

    R, Varsha; Tej, A; Vig, S; Ghosh, S K; Ojha, D K

    2016-01-01

    A multi-wavelength investigation of the star forming complex IRAS 20286+4105, located in the Cygnus-X region, is presented here. Near-infrared K-band data is used to revisit the cluster / stellar group identified in previous studies. The radio continuum observations, at 610 and 1280 MHz show the presence of a HII region possibly powered by a star of spectral type B0 - B0.5. The cometary morphology of the ionized region is explained by invoking the bow-shock model where the likely association with a nearby supernova remnant is also explored. A compact radio knot with non-thermal spectral index is detected towards the centre of the cloud. Mid-infrared data from the Spitzer Legacy Survey of the Cygnus-X region show the presence of six Class I YSOs inside the cloud. Thermal dust emission in this complex is modelled using Herschel far-infrared data to generate dust temperature and column density maps. Herschel images also show the presence of two clumps in this region, the masses of which are estimated to be {\\sim...

  11. Neogene-Quaternary Volcanic forms in the Carpathian-Pannonian Region: a review

    Science.gov (United States)

    Lexa, Jaroslav; Seghedi, Ioan; Németh, Karoly; Szakács, Alexandru; Koneĉny, Vlastimil; Pécskay, Zoltan; Fülöp, Alexandrina; Kovacs, Marinel

    2010-09-01

    Neogene to Quaternary volcanic/magmatic activity in the Carpathian-Pannonian Region (CPR) occurred between 21 and 0.1 Ma with a distinct migration in time from west to east. It shows a diverse compositional variation in response to a complex interplay of subduction with rollback, back-arc extension, collision, slab break-off, delamination, strike-slip tectonics and microplate rotations, as well as in response to further evolution of magmas in the crustal environment by processes of differentiation, crustal contamination, anatexis and magma mixing. Since most of the primary volcanic forms have been affected by erosion, especially in areas of post-volcanic uplift, based on the level of erosion we distinguish: (1) areas eroded to the basement level, where paleovolcanic reconstruction is not possible; (2) deeply eroded volcanic forms with secondary morphology and possible paleovolcanic reconstruction; (3) eroded volcanic forms with remnants of original morphology preserved; and (4) the least eroded volcanic forms with original morphology quite well preserved. The large variety of volcanic forms present in the area can be grouped in a) monogenetic volcanoes and b) polygenetic volcanoes and their subsurface/intrusive counterparts that belong to various rock series found in the CPR such as calc-alkaline magmatic rock-types (felsic, intermediate and mafic varieties) and alkalic types including K-alkalic, shoshonitic, ultrapotassic and Na-alkalic. The following volcanic/subvolcanic forms have been identified: (i) domes, shield volcanoes, effusive cones, pyroclastic cones, stratovolcanoes and calderas with associated intrusive bodies for intermediate and basic calclkaline volcanism; (ii) domes, calderas and ignimbrite/ash-flow fields for felsic calc-alkaline volcanism and (iii) dome flows, shield volcanoes, maars, tuffcone/tuff-rings, scoria-cones with or without related lava flow/field and their erosional or subsurface forms (necks/ plugs, dykes, shallow intrusions

  12. Formation of ethylene glycol and other complex organic molecules in star-forming regions

    Science.gov (United States)

    Rivilla, V. M.; Beltrán, M. T.; Cesaroni, R.; Fontani, F.; Codella, C.; Zhang, Q.

    2017-02-01

    Context. The detection of complex organic molecules related with prebiotic chemistry in star-forming regions allows us to investigate how the basic building blocks of life are formed. Aims: Ethylene glycol (CH2OH)2 is the simplest sugar alcohol and the reduced alcohol of the simplest sugar glycoladehyde (CH2OHCHO). We study the molecular abundance and spatial distribution of (CH2OH)2, CH2OHCHO and other chemically related complex organic species (CH3OCHO, CH3OCH3, and C2H5OH) towards the chemically rich massive star-forming region G31.41+0.31. Methods: We analyzed multiple single-dish (Green Bank Telescope and IRAM 30 m) and interferometric (Submillimeter Array) spectra towards G31.41+0.31, covering a range of frequencies from 45 to 258 GHz. We fitted the observed spectra with a local thermodynamic equilibrium (LTE) synthetic spectra, and obtained excitation temperatures and column densities. We compared our findings in G31.41+0.31 with the results found in other environments, including low- and high-mass star-forming regions, quiescent clouds and comets. Results: We report for the first time the presence of the aGg' conformer of (CH2OH)2 towards G31.41+0.31, detecting more than 30 unblended lines. We also detected multiple transitions of other complex organic molecules such as CH2OHCHO, CH3OCHO, CH3OCH3, and C2H5OH. The high angular resolution images show that the (CH2OH)2 emission is very compact, peaking towards the maximum of the 1.3 mm continuum. These observations suggest that low abundance complex organic molecules, like (CH2OH)2 or CH2OHCHO, are good probes of the gas located closer to the forming stars. Our analysis confirms that (CH2OH)2 is more abundant than CH2OHCHO in G31.41+0.31, as previously observed in other interstellar regions. Comparing different star-forming regions we find evidence of an increase of the (CH2OH)2/CH2OHCHO abundance ratio with the luminosity of the source. The CH3OCH3/CH3OCHO and (CH2OH)2/C2H5OH ratios are nearly constant with

  13. An All-Sky Sample of Intermediate-Mass Star-Forming Regions

    CERN Document Server

    Lundquist, Michael J; Alexander, Michael J; Kerton, Charles R; Arvidsson, Kim

    2014-01-01

    We present an all-sky sample of 984 candidate intermediate-mass Galactic star-forming regions color-selected from the Infrared Astronomical Satellite (IRAS) Point Source Catalog and morphologically classify each object using mid-infrared Wide-field Infrared Survey Explorer (WISE) images. Of the 984 candidates, 616 are probable star-forming regions (62.6%), 128 are filamentary structures (13.0%), 39 are point-like objects of unknown nature (4.0%), and 201 are galaxies (20.4%). We conduct a study of four of these regions, IRAS 00259+5625, IRAS 00420+5530, IRAS 01080+5717, and IRAS 05380+2020, at Galactic latitudes |b| > 5 degrees using optical spectroscopy from the Wyoming Infrared Observatory along with near-infrared photometry from the Two-Micron All Sky Survey to investigate their stellar content. New optical spectra, color-magnitude diagrams, and color-color diagrams reveal their extinctions, spectrophotometric distances, and the presence of small stellar clusters containing 20-78 solar masses of stars. The...

  14. The distribution of water in the high-mass star-forming region NGC 6334I

    CERN Document Server

    Emprechtinger, M; Bell, T; Phillips, T G; Schilke, P; Comito, C; Rolffs, R; van der Tak, F; Ceccarelli, C; Aarts, H; Bacmann, A; Baudry, A; Benedettini, M; Bergin, E A; Blake, G; Boogert, A; Bottinelli, S; Cabrit, S; Caselli, P; Castets, A; Caux, E; Cernicharo, J; Codella, C; Coutens, A; Crimier, N; Demyk, K; Dominik, C; Encrenaz, P; Falgarone, E; Fuente, A; Gerin, M; Goldsmith, P; Helmich, F; Hennebelle, P; Henning, T; Herbst, E; Hily-Blant, P; Jacq, T; Kahane, C; Kama, M; Klotz, A; Kooi, J; Langer, W; Lefloch, B; Loose, A; Lord, S; Lorenzani, A; Maret, S; Melnick, G; Neufeld, D; Nisini, B; Ossenkopf, V; Pacheco, S; Pagani, L; Parise, B; Pearson, J; Risacher, C; Salez, M; Saraceno, P; Schuster, K; Stutzki, J; Tielens, X; van der Wiel, M; Vastel, C; Viti, S; Wakelam, V; Walters, A; Wyrowski, F; Yorke, H

    2010-01-01

    We present observations of twelve rotational transitions of H2O-16, H2O-18, and H2O-17 toward the massive star-forming region NGC 6334 I, carried out with Herschel/HIFI as part of the guaranteed time key program Chemical HErschel Surveys of Star forming regions (CHESS). We analyze these observations to obtain insights into physical processes in this region. We identify three main gas components (hot core, cold foreground, and outflow) in NGC 6334 I and derive the physical conditions in these components. The hot core, identified by the emission in highly excited lines, shows a high excitation temperature of 200 K, whereas water in the foreground component is predominantly in the ortho- and para- ground states. The abundance of water varies between 4 10^-5 (outflow) and 10^-8 (cold foreground gas). This variation is most likely due to the freeze-out of water molecules onto dust grains. The H2O-18/H2O-17 abundance ratio is 3.2, which is consistent with the O-18/O-17 ratio determined from CO isotopologues. The or...

  15. Neutral and Ionized Hydrides in Star-forming Regions -- Observations with Herschel/HIFI

    CERN Document Server

    Benz, Arnold O; van Dishoeck, Ewine F; Staeuber, Pascal; Wampfler, Susanne F

    2013-01-01

    The cosmic abundance of hydrides depends critically on high-energy UV, X-ray, and particle irradiation. Here we study hydrides in star-forming regions where irradiation by the young stellar object can be substantial, and density and temperature can be much enhanced over interstellar values. Lines of OH, CH, NH, SH and their ions OH+, CH+, NH+, SH+, H2O+, and H3O+ were observed in star-forming regions by the HIFI spectrometer onboard the Herschel Space Observatory. Molecular column densities are derived from observed ground-state lines, models, or rotational diagrams. We report here on two prototypical high-mass regions, AFGL 2591 and W3 IRS5, and compare them to chemical calculations making assumptions on the high-energy irradiation. A model assuming no ionizing protostellar emission is compared with (i) a model assuming strong protostellar X-ray emission and (ii) a two-dimensional (2D) model including emission in the far UV (FUV, 6 -- 13.6 eV) irradiating the outflow walls that separate the outflowing gas an...

  16. The protoplanetary disks in the nearby massive star forming region Cygnus OB2

    CERN Document Server

    Guarcello, M G; Wright, N J; Drew, J E; Gutermuth, R A; Hora, J L; Naylor, T; Aldcroft, T; Fruscione, A; Garcia-Alvarez, D; Kashyap, V L; King, R

    2013-01-01

    The formation of stars in massive clusters is one of the main modes of the star formation process. However, the study of massive star forming regions is hampered by their typically large distances to the Sun. One exception to this is the massive star forming region Cygnus OB2 in the Cygnus X region, at the distance of about 1400 pc. Cygnus OB2 hosts very rich populations of massive and low-mass stars, being the best target in our Galaxy to study the formation of stars, circumstellar disks, and planets in presence of massive stars. In this paper we combine a wide and deep set of photometric data, from the r band to 24 micron, in order to select the disk bearing population of stars in Cygnus OB2 and identify the class I, class II, and stars with transition and pre-transition disks. We selected 1843 sources with infrared excesses in an area of 1 degree x 1 degree centered on Cyg OB2 in several evolutionary stages: 8.4% class I, 13.1% flat-spectrum sources, 72.9% class II, 2.3% pre-transition disks, and 3.3% tran...

  17. A preliminary distance to W 75N in the Cygnus X star-forming region

    CERN Document Server

    Rygl, K L J; Menten, K M; Reid, M J; van Langevelde, H J; Honma, M; Torstensson, K J E; Fujisawa, K; Sanna, A

    2010-01-01

    Cygnus X is one of the closest giant molecular cloud complexes and therefore an extensively studied region of ongoing high mass star formation. However, the distance to this region has been a long-standing issue, since sources at galactic longitude of ~80 degrees could be in the Local Arm nearby (1-2 kpc), in the Perseus Arm at ~5 kpc, or even in the outer arm (~10 kpc). We use combined observations of the EVN plus two Japanese stations to measure very accurate parallaxes of methanol masers in five star-forming regions in Cygnus X to understand if they belong to one large star-forming complex or if they are separate entities located at different distances. Here we report our preliminary result for W75N based on six epochs of VLBI observations: we find that W75N is at a distance of 1.32^{+0.11}_{-0.09} kpc, which is significantly closer than the reported values in the literature (1.5-2 kpc).

  18. A spectral and photometric study of 102 star forming regions in seven spiral galaxies

    CERN Document Server

    Gusev, A S; Piskunov, A E; Kharchenko, N V; Bruevich, V V; Ezhkova, O V; Guslyakova, S A; Lang, V; Shimanovskaya, E V; Efremov, Yu N

    2016-01-01

    We present a study of complexes of young massive star clusters (YMCs), embedded in extragalactic giant HII regions, based on the coupling of spectroscopic with photometric and spectrophotometric observations of about 100 star forming regions in seven spiral galaxies (NGC 628, NGC 783, NGC 2336, NGC 6217, NGC 6946, NGC 7331, and NGC 7678). The complete observational database has been observed and accumulated within the framework of our comprehensive study of extragalactic star forming regions. The current paper presents the last part of either unpublished or refreshed photometric and spectrophotometric observations of the galaxies NGC 6217, NGC 6946, NGC 7331, and NGC 7678. We derive extinctions, chemical abundances, continuum and line emissions of ionised gas, ages and masses for cluster complexes. We find the young massive cluster complexes to have ages no greater than 10 Myr and masses between 10^4Msol and 10^7Msol, and the extinctions A(V) vary between ~ 0 and 3 mag, while the impact of the nebular emissio...

  19. Young Stellar Objects in the Massive Star Forming Region: W49

    CERN Document Server

    Saral, Gozde; Willis, Sarah E; Koenig, Xavier P; Gutermuth, Robert A; Saygac, A Talat

    2015-01-01

    We present the initial results of our investigation of the star-forming complex W49, one of the youngest and most luminous massive star forming regions in our Galaxy. We used Spitzer/Infrared Array Camera (IRAC) data to investigate massive star formation with the primary objective to locate a representative set of protostars and the clusters of young stars that are forming around them. We present our source catalog with the mosaics from the IRAC data. In this study we used a combination of IRAC, MIPS, Two Micron All Sky Survey (2MASS) and UKIRT Deep Infrared Sky Survey (UKIDSS) data to identify and classify the Young Stellar Objects (YSOs). We identified 232 Class 0/I YSOs, 907 Class II YSOs, and 74 transition disk candidate objects using color-color and color-magnitude diagrams. In addition, to understand the evolution of star formation in W49 we analysed the distribution of YSOs in the region to identify clusters using a minimal spanning tree method. The fraction of YSOs that belong to clusters with >7 memb...

  20. Functional characterization of the cardiac ryanodine receptor pore-forming region.

    Directory of Open Access Journals (Sweden)

    Joanne Euden

    Full Text Available Ryanodine receptors are homotetrameric intracellular calcium release channels. The efficiency of these channels is underpinned by exceptional rates of cation translocation through the open channel and this is achieved at the expense of the high degree of selectivity characteristic of many other types of channel. Crystallization of prokaryotic potassium channels has provided insights into the structures and mechanisms responsible for ion selection and movement in these channels, however no equivalent structural detail is currently available for ryanodine receptors. Nevertheless both molecular modeling and cryo-electron microscopy have identified the probable pore-forming region (PFR of the ryanodine receptor (RyR and suggest that this region contains structural elements equivalent to those of the PFRs of potassium-selective channels. The aim of the current study was to establish if the isolated putative cardiac RyR (RyR2 PFR could form a functional ion channel. We have expressed and purified the RyR2 PFR and shown that function is retained following reconstitution into planar phospholipid bilayers. Our data provide the first direct experimental evidence to support the proposal that the conduction pathway of RyR2 is formed by structural elements equivalent to those of the potassium channel PFR.

  1. Young Stellar Populations in MYStIX Star Forming Regions: Candidate Protostars

    CERN Document Server

    Romine, Gregory; Getman, Konstantin V; Kuhn, Michael A; Povich, Matthew S

    2016-01-01

    The Massive Young Star Forming Complex in Infrared and X-ray (MYStIX) project provides a new census on stellar members of massive star forming regions within 4 kpc. Here the MYStIX Infrared Excess catalog (MIRES) and Chandra-based X-ray photometric catalogs are mined to obtain high-quality samples of Class I protostars using criteria designed to reduce extragalactic and Galactic field star contamination. A total of 1,109 MYStIX Candidate Protostars (MCPs) are found in 14 star forming regions. Most are selected from protoplanetary disk infrared excess emission, but 20% are found from their ultrahard X-ray spectra from heavily absorbed magnetospheric flare emission. Two-thirds of the MCP sample is newly reported here. The resulting samples are strongly spatially associated with molecular cores and filaments on Herschel far-infrared maps. This spatial agreement and other evidence indicate that the MCP sample has high reliability with relatively few 'false positives' from contaminating populations. But the limite...

  2. ALMA maps the Star-Forming Regions in a Dense Gas Disk at z~3

    CERN Document Server

    Swinbank, Mark; Nightgale, James; Furlanetto, Christina; Smail, Ian; Cooray, Asantha; Dannerbauer, Helmut; Dunne, Loretta; Eales, Steve; Gavazzi, Raphael; Hunter, Todd; Ivison, Rob; Negrello, Mattia; Oteo, Ivan; Smit, Renske; van der Werf, Paul; Vlahakis, Catherine

    2015-01-01

    We exploit long-baseline ALMA sub-mm observations of the lensed star-forming galaxy SDP 81 at z=3.042 to investigate the properties of inter-stellar medium on scales of 50-100pc. The kinematics of the CO gas within this system are well described by a rotationally-supported disk with an inclination-corrected rotation speed, v=320+/-20km/s and a dynamical mass of M=(3.5+/-1.0)x10^10Mo within a radius of 1.5 kpc. The disk is gas rich and unstable, with a Toomre parameter, Q=0.30+/-0.10 and so should collapse in to star-forming regions with Jeans length L_J~130pc. We identify five star-forming regions within the ISM on these scales and show that their scaling relations between luminosity, line-widths and sizes are significantly offset from those typical of molecular clouds in local Galaxies (Larson's relations). These offsets are likely to be caused by the high external hydrostatic pressure for the interstellar medium (ISM), P/kB=(40+/-20)x10^7K/cm3, which is ~10,000x higher than the typical ISM pressure in the M...

  3. A kinematic analysis of the Giant star-forming Region of N11

    Science.gov (United States)

    Torres-Flores, Sergio; Barbá, Rodolfo; Maíz Apellániz, Jesús; Rubio, Mónica; Bosch, Guillermo

    2015-02-01

    In this work we present high resolution spectroscopic data of the giant star-forming region of N11, obtained with the GIRAFFE instrument at the Very Large Telescope. By using this data set, we find that most of the Hα emission lines profiles in this complex can be fitted by a single Gaussian, however, multiple emission line profiles can be observed in the central region of N11. By adding all the spectra, we derive the integrated Hα profile of this complex, which displays a width (σ) of about 12 km s-1 (corrected by instrumental and thermal width). We find that a single Gaussian fit on the integrated Hα profile leaves remaining wings, which can be fitted by a secondary broad Gaussian component. In addition, we find high velocity features, which spatially correlate with soft diffuse X-ray emission.

  4. Deep VLA observations of nearby star forming regions I: Barnard 59 and Lupus 1

    Science.gov (United States)

    Dzib, S. A.; Loinard, L.; Medina, S.-N. X.; Rodríguez, L. F.; Mioduszewski, A. J.; Torres, R. M.

    2016-10-01

    Barnard 59 and Lupus 1 are two nearby star-forming regions visible from the southern hemisphere. In this manuscript, we present deep (σ˜15 μJy) radio observations (ν=6 GHz) of these regions, and report the detection of a total of 114 sources. Thirteen of these sources are associated with known young stellar objects, nine in Barnard 59 and four in Lupus 1. The properties of the radio emission (spectral index and, in some cases, polarization) suggest a thermal origin for most young stellar objects. Only for two sources (Sz 65 and Sz 67) are there indications for a possible non-thermal origin. The remaining radio detections do not have counterparts at other wavelengths, and the number of sources detected per unit solid angle is in agreement with extragalactic number counts, suggesting that they are extragalactic sources.

  5. A kinematic analysis of the Giant star-forming Region of N11

    CERN Document Server

    Torres-Flores, S; Apellániz, J Maíz; Rubio, M; Bosch, G

    2015-01-01

    In this work we present high resolution spectroscopic data of the giant star-forming region of N11, obtained with the GIRAFFE instrument at the Very Large Telescope. By using this data set, we find that most of the H$\\alpha$ emission lines profiles in this complex can be fitted by a single Gaussian, however, multiple emission line profiles can be observed in the central region of N11. By adding all the spectra, we derive the integrated H$\\alpha$ profile of this complex, which displays a width ($\\sigma$) of about 12 km s$^{-1}$ (corrected by instrumental and thermal width). We find that a single Gaussian fit on the integrated H$\\alpha$ profile leaves remaining wings, which can be fitted by a secondary broad Gaussian component. In addition, we find high velocity features, which spatially correlate with soft diffuse X-ray emission.

  6. An accretion disks in the high-mass star forming region IRA 23151+5912

    Science.gov (United States)

    Migenes, Victor; Rodríguez-Esnard, T.; Trinidad, M. A.

    2014-01-01

    We present observations of radio continuum emission at 1.3 and 3.6 cm and H2O masers toward the high-mass star-forming regions IRA 23151+5912 carried out with the VLA-EVLA. We detected one continuum source at 1.3 cm and 13 water maser spots which are distributed in three groups aligned along the northeast-southwest direction. Our results suggest that the 1.3 cm emission is consistent with an HC HII region, probably with an embedded zero-age main sequence star of type B2. In particular, we find that this radio continuum source is probably associated with a circumstellar disk of about 68 AU, as traced by water masers. Furthermore, the masers of the second group are probably describing another circumstellar disk of about 86 AU, whose central protostar is still undetected. We discuss this results in the light of more recent high-resolution observations.

  7. Evidence of Evolution in the Dense Cores in Massive Star Forming Regions

    Institute of Scientific and Technical Information of China (English)

    Jian-Jun Zhou; Jarken Esimbek; Ji-Xian Sun; Bing-Gang Ju; Jing-Jiang Sun

    2005-01-01

    The excitation of H2O masers usually needs very high density gas,hence it can serve as a marker of dense gas in HⅡ region. We selected a sample of H2O maser sources from Plume et al. (four with, and four without detected CS(J = 7 - 6) emission), and observed them in 13CO(J=1-0) and C18O (J=1-0). C18O (J=1-0) emission was detected only in three of the sources with detected CS(J=7-6) emission. An analysis combined with some data in the literature suggests that these dense cores may be located at different evolutionary stages. Multi-line observation study may provide us clues on the evolution of massive star forming regions and the massive stars themselves.

  8. An X-ray Tour of Massive Star-forming Regions with Chandra

    CERN Document Server

    Townsley, L K

    2006-01-01

    The Chandra X-ray Observatory is providing fascinating new views of massive star-forming regions, revealing all stages in the life cycles of massive stars and their effects on their surroundings. I present a Chandra tour of some of the most famous of these regions: M17, NGC 3576, W3, Tr14 in Carina, and 30 Doradus. Chandra highlights the physical processes that characterize the lives of these clusters, from the ionizing sources of ultracompact HII regions (W3) to superbubbles so large that they shape our views of galaxies (30 Dor). X-ray observations usually reveal hundreds of pre-main sequence (lower-mass) stars accompanying the OB stars that power these great HII region complexes, although in one case (W3 North) this population is mysteriously absent. The most massive stars themselves are often anomalously hard X-ray emitters; this may be a new indicator of close binarity. These complexes are sometimes suffused by soft diffuse X-rays (M17, NGC 3576), signatures of multi-million-degree plasmas created by fas...

  9. Carbon gas in SMC low-metallicity star-forming regions

    CERN Document Server

    Requena-Torres, M A; Okada, Y; Guesten, R; Stutzki, J; Risacher, C; Simon, R; Zinnecker, H

    2016-01-01

    This paper presents [CII], [CI] and CO emission line maps of the star-forming regions N66, N25+N26, and N88 in the metal-poor Local Group dwarf galaxy SMC. The spatial and velocity structure of the large HII region N66 reveals an expanding ring of shocked molecular gas centered on the exciting star cluster NGC346, whereas a more distant dense molecular cloud is being eroded by UV radiation from the same cluster. In the N25+N26 and N88 maps, diffuse [CII] emission at a relatively low surface brightness extends well beyond the compact boundaries of the bright emission associated with the [CII] regions. In all regions, the distribution of this bright [CII] emission and the less prominent [CI] emission closely follows the outline of the CO complexes, but the intensity of the [CII] and [CI] emission is generally anticorrelated, which can be understood by the action of photodissociation and photoionization processes. Notwithstanding the overall similarity of CO and [CII] maps, the intensity ratio of these lines var...

  10. Far Infrared Mapping of Three Galactic Star Forming Regions: W3(OH), S209 & S187

    Indian Academy of Sciences (India)

    S. K. Ghosh; B. Mookerjea; T. N. Rengarajan; S. N. Tandon; R. P. Verma

    2001-06-01

    Three Galactic star forming regions associated with W3(OH), S209 and S187 have been simultaneously mapped in two trans-IRAS far infrared (FIR) bands centered at ∼ 140 and 200m using the TIFR 100 cm balloon borne FIR telescope. These maps showextended FIR emission with structures. The HIRES processed IRAS maps of these regions at 12, 25, 60 & 100 m have also been presented for comparison. Point-like sources have been extracted from the longest waveband TIFR maps and searched for associations in the other five bands. The diffuse emission from these regions have been quantified, which turns out to be a significant fraction of the total emission. The spatial distribution of cold dust (T < 30 K) for two of these sources (W3(OH) & S209), has been determined reliably from the maps in TIFR bands. The dust temperature and optical depth maps show complex morphology. In general the dust around S209 has been found to be warmer than that in W3(OH) region.

  11. A CATALOG OF METHANOL MASERS IN MASSIVE STAR-FORMING REGIONS. III. THE MOLECULAR OUTFLOW SAMPLE

    Energy Technology Data Exchange (ETDEWEB)

    Gómez-Ruiz, A. I. [Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis E. Erro 1, Tonantzintla, Puebla, C.P. 72840, México (Mexico); Kurtz, S. E.; Loinard, L. [Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Apartado Postal 3-72, Morelia 58089, México (Mexico); Araya, E. D. [Physics Department, Western Illinois University, 1 University Circle, Macomb, IL 61455 (United States); Hofner, P. [New Mexico Institute of Mining and Technology, Socorro, NM 87801 (United States)

    2016-02-15

    We present an interferometric survey of the 44 GHz class I methanol maser transition toward a sample of 69 sources consisting of high-mass protostellar object (HMPO) candidates and ultracompact (UC) H ii regions. We found a 38% detection rate (16 of 42) in the HMPO candidates and a 54% detection rate (13 of 24) for the regions with ionized gas. This result indicates that class I methanol maser emission is more common toward the more evolved young stellar objects of our sample. Comparing with similar interferometric data sets, our observations show narrower linewidths, likely due to our higher spatial resolution. Based on a comparison between molecular outflow tracers and the maser positions, we find several cases where the masers appear to be located at the outflow interface with the surrounding core. Unlike previous surveys, we also find several cases where the masers appear to be located close to the base of the molecular outflow, although we cannot discard projection effects. This and other surveys of class I methanol masers not only suggest that these masers may trace shocks at different stages, but also that they may even trace shocks arising from a number of different phenomena occurring in star-forming regions: young/old outflows, cloud–cloud collisions, expanding H ii regions, among others.

  12. A multiwavelength study of the star forming region IRAS 18544+0112

    CERN Document Server

    Ortega, M E; Cichowolski, S; Rubio, M; Castelletti, G; Dubner, G

    2009-01-01

    This work aims at investigating the molecular and infrared components in the massive young stellar object (MYSO) candidate IRAS 18544+0112. The purpose is to determine the nature and the origin of this infrared source. To analyze the molecular gas towards IRAS 18544+0112, we have carried out observations in a 90" x 90" region around l = 34.69, b = -0.65, using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12CO J=3-2, 13CO J=3-2, HCO+ J=4-3 and CS J=7-6 lines with an angular resolution of 22". The infrared emission in the area has been analyzed using 2MASS and Spitzer public data. From the molecular analysis, we find self-absorbed 12CO J=3-2 profiles, which are typical in star forming regions, but we do not find any evidence of outflow activity. Moreover, we do not detect either HCO+ J=4-3 or CS J=7-6 in the region, which are species normally enhanced in molecular outflows and high density envelopes. The 12CO J=3-2 emission profile suggests the presence of expanding gas in the region. The Spitze...

  13. Parsec-scale X-ray Flows in High-mass Star-forming Regions

    CERN Document Server

    Townsley, L K; Montmerle, T; Broos, P; Chu, Y H; Garmire, G; Getman, K

    2004-01-01

    We present Chandra/ACIS images of several high-mass star-forming regions. The massive stellar clusters powering these HII regions are resolved at the arcsecond level into hundreds of stellar sources, similar to those seen in closer young stellar clusters. However, we also detect diffuse X-ray emission on parsec scales that is spatially and spectrally distinct from the point source population. For nearby regions (e.g. M17 and Rosette) the emission is soft, with plasma temperatures less than 10 million degrees, in contrast to what is seen in more distant complexes (e.g. RCW49, W51). This extended emission most likely arises from the fast O-star winds thermalized either by wind-wind collisions or by a termination shock against the surrounding media. We have established that only a small portion of the wind energy and mass appears in the observed diffuse X-ray plasma; in the blister HII regions, we suspect that most of it flows without cooling into the low-density interstellar medium through blow-outs or fissures...

  14. Si and Fe depletion in Galactic star-forming regions observed by the Spitzer Space Telescope

    CERN Document Server

    Okada, Yoko; Miyata, Takashi; Okamoto, Yoshiko K; Sakon, Itsuki; Shibai, Hiroshi; Takahashi, Hidenori

    2008-01-01

    We report the results of the mid-infrared spectroscopy of 14 Galactic star-forming regions with the high-resolution modules of the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. We detected [SiII] 35um, [FeII] 26um, and [FeIII] 23um as well as [SIII] 33um and H2 S(0) 28um emission lines. Using the intensity of [NII] 122um or 205um and [OI] 146um or 63um reported by previous observations in four regions, we derived the ionic abundance Si+/N+ and Fe+/N+ in the ionized gas and Si+/O0 and Fe+/O0 in the photodissociation gas. For all the targets, we derived the ionic abundance of Si+/S2+ and Fe2+/S2+ for the ionized gas. Based on photodissociation and HII region models the gas-phase Si and Fe abundance are suggested to be 3-100% and <8% of the solar abundance, respectively, for the ionized gas and 16-100% and 2-22% of the solar abundance, respectively, for the photodissociation region gas. Since the [FeII] 26um and [FeIII] 23um emissions are weak, the high sensitivity of the IRS enables to de...

  15. Sulphur-bearing species in the star forming region L1689N

    CERN Document Server

    Wakelam, V; Ceccarelli, C; Le Floc'h, B; Caux, E; Pagani, L

    2004-01-01

    We report observations of the expected main S-bearing species (SO, SO2 and H2S) in the low-mass star forming region L1689N. We obtained large scale (~300''x200'') maps of several transitions from these molecules with the goal to study the sulphur chemistry, i.e. how the relative abundances change in the different physical conditions found in L1689N. We identified eight interesting regions, where we carried out a quantitative comparative study: the molecular cloud (as reference position), five shocked regions caused by the interaction of the molecular outflows with the cloud, and the two protostars IRAS16293-2422 and 16293E. In the cloud we carefully computed the gas temperature and density by means of a non-LTE LVG code, while in other regions we used previous results. We hence derived the column density of SO, SO2 and H2S, together with SiO and H2CO - which were observed previously - and their relevant abundance ratios. We find that SiO is the molecule that shows the largest abundance variations in the shock...

  16. Ultraluminous X-ray Source Correlations with Star-Forming Regions

    CERN Document Server

    Swartz, Douglas A; Soria, Roberto

    2009-01-01

    Maps of low-inclination nearby galaxies in Sloan Digitized Sky Survey u-g, g-r and r-i colors are used to determine whether Ultraluminous X-ray sources (ULXs) are predominantly associated with star-forming regions of their host galaxies. An empirical selection criterion is derived from colors of HII regions in M81 and M101 that differentiates between the young, blue stellar component and the older disk and bulge population. This criterion is applied to a sample of 58 galaxies of Hubble type S0 and later and verified through an application of Fisher's linear discriminant analysis. It is found that 60% (49%) of ULXs in optically-bright environments are within regions blueward of their host galaxy's HII regions compared to only 27% (0%) of a control sample according to the empirical (Fisher) criterion. This is an excess of 3-sigma above the 32% (27%) expected if the ULXs were randomly distributed within their galactic hosts. This indicates a ULX preference for young, approximately <10 Myr, OB associations. Ho...

  17. The electromagnetic form factors of the Λ in the timelike region

    Science.gov (United States)

    Haidenbauer, J.; Meißner, U.-G.

    2016-10-01

    The reaction e+e- → Λ bar Λ is investigated for energies close to the threshold. Specific emphasis is put on the role played by the interaction in the final Λ bar Λ system which is taken into account rigorously. For that interaction a variety of Λ bar Λ potential models is employed that have been constructed for the analysis of the reaction p bar p → Λ bar Λ in the past. The enhancement of the effective form factor for energies close to the Λ bar Λ threshold, seen in pertinent experiments, is reproduced. Predictions for the Λ electromagnetic form factors GM and GE in the timelike region and for spin-dependent observables such as spin-correlation parameters are presented.

  18. Diffuse Matter from Star Forming Regions to Active Galaxies A Volume Honouring John Dyson

    CERN Document Server

    Hartquist, T W

    2006-01-01

    John Dyson has contributed to the study of the hydrodynamic processes that govern a wide variety of astrophysical sources which he has helped explain. In this volume dedicated to him, introductory reviews to a number of the key processes and to the sources themselves are given by leading experts. The mechanisms in which the multi-component natures of media affect their dynamics receive particular attention, but the roles of hydromagnetic effects are also highlighted. The importance of cosmic ray moderation and mass transfer between different thermal phases for cosmic ray moderation and mass transfer between different thermal phases for the evolution of flows are amongst the topics treated. The main types of regions considered include those where stars form, the circumstellar environments of evolved stars, the larger scale interstellar structures caused by the mass loss of stars, and those where the lines of AGNs form. The reviews complement one another and together provide a coherent introduction to the astro...

  19. The electromagnetic form factors of the $\\Lambda$ in the timelike region

    CERN Document Server

    Haidenbauer, J

    2016-01-01

    The reaction $e^+e^- \\to \\bar \\Lambda \\Lambda$ is investigated for energies close to the threshold. Specific emphasis is put on the role played by the interaction in the final $\\bar \\Lambda \\Lambda$ system which is taken into account rigorously. For that interaction a variety of $\\bar \\Lambda \\Lambda$ potential models is employed that have been constructed for the analysis of the reaction $\\bar p p \\to \\bar \\Lambda \\Lambda$ in the past. The enhancement of the effective form factor for energies close to the $\\bar \\Lambda \\Lambda$ threshold, seen in pertinent experiments, is reproduced. Predictions for the $\\Lambda$ electromagnetic form factors $G_M$ and $G_E$ in the timelike region and for spin-dependent observables such as spin-correlation parameters are presented.

  20. Complex organic molecules toward low-mass and high-mass star forming regions

    Science.gov (United States)

    Favre, C.; Ceccarelli, C.; Lefloch, B.; Bergin, E.; Carvajal, M.; Brouillet, N.; Despois, D.; Jørgensen, J.; Kleiner, I.

    2016-12-01

    One of the most important questions in molecular astrophysics is how, when, and where complex organic molecules, COMs (≥ 6 atoms) are formed. In the Interstellar-Earth connection context, could this have a bearing on the origin of life on Earth? Formation mechanisms of COMs, which include potentially prebiotic molecules, are still debated and may include grain-mantle and/or gas-phase chemistry. Understanding the mechanisms that lead to the interstellar molecular complexification, along with the involved physicochemical processes, is mandatory to answer the above questions. In that context, active researches are ongoing in theory, laboratory experiment, chemical modeling and observations. Thanks to recent progress in radioastronomy instrumentation for both single-dish and millimeter array (e.g. Herschel, NOEMA, ALMA), new results have been obtained. I will review some notable results on the detection of COMs, including prebiotic molecules, towards star forming regions.

  1. Desert Pavement Process and Form: Modes and Scales of Landscape Stability and Instability in Arid Regions

    Science.gov (United States)

    Wells, Stephen G.; McFadden, Leslie D.; McDonald, Eric V.; Eppes, Martha C.; Young, Michael H.; Wood, Yvonne A.

    2014-05-01

    Desert pavements are recognized in arid landscapes around the world, developing via diminution of constructional/depositional landform relief and creating a 1-2 stone thick armor over a "stone free" layer. Surface exposure dating demonstrates that clasts forming the desert pavements are maintained at the land surface over hundreds of thousands of years, as aeolian fines are deposited on the land surface, transported into the underlying parent material and incorporated into accretionary soil horizons (e.g., the stone free or vesicular [Av] horizon). This surface armor provides long-term stability over extensive regions of the landscape. Over shorter time periods and at the landform-element scale, dynamic surficial processes (i.e., weathering, runoff) continue to modify the pavement form. Clast size reduction in comparison to underlying parent material, along with armoring and packing of clasts in pavements contribute to their persistence, and studies of crack orientations in pavement clasts indicate physical weathering and diminution of particle size are driven by diurnal solar insolation. Over geologic time, cracks form and propagate from tensile stresses related to temporal and spatial gradients in temperature that evolve and rotate in alignment with the sun's rays. Observed multimodal nature of crack orientations appear related to seasonally varying, latitude-dependent temperature fields resulting from solar angle and weather conditions. Surface properties and their underlying soil profiles vary across pavement surfaces, forming a landscape mosaic and controlling surface hydrology, ecosystem function and the ultimate life-cycle of arid landscapes. In areas of well-developed pavements, surface infiltration and soluble salt concentrations indicate that saturated hydraulic conductivity of Av horizons decline on progressively older alluvial fan surfaces. Field observations and measurements from well-developed desert pavement surfaces landforms also yield

  2. Kinematic Distances of Pre-main Sequence Stars in the Lupus Star-Forming Region

    Science.gov (United States)

    Galli, P. A. B.; Teixeira, R.; Ducourant, C.; Bertout, C.

    2014-06-01

    The problem of the determination of distances has always played a central role in astronomy. However, little recent progress has been made in the distance determination of faint young stellar objects such as pre-main sequence (PMS) stars. Many of the PMS stars were neither observed by the Hipparcos satellite due to their magnitude nor have any trigonometric parallax measured from the ground due to their distance. Here we investigate the kinematic properties of the Lupus moving group with the primary objective of deriving individual parallaxes for each group member of this star-forming region.

  3. A Survey of Large Molecules of Biological Interest toward Selected High Mass Star Forming Regions

    Science.gov (United States)

    Remijan, A.; Shiao, Y.-S.; Friedel, D. N.; Meier, D. S.; Snyder, L. E.

    2004-01-01

    We have surveyed three high mass Galactic star forming regions for interstellar methanol (CH3OH), formic acid (HCOOH), acetic acid (CH3COOH), methyl formate (HCOOCH3), methyl cyanide (CH3CN), and ethyl cyanide (CH3CH2CN) with the BIMA Array. From our observations, we have detected two new sources of interstellar HCOOH toward the hot core regions G19.61-0.23 and W75N. We have also made the first detections of CH3CH2CN and HCOOCH3 toward G19.61-0.23. The relative HCOOH/HCOOCH3 abundance ratio toward G19.61-0.23 is 0.18 which is comparable to the abundance ratios found by Liu and colleagues toward Sgr B2(N-LMH), Orion and W51(approximately 0.10). We have made the first detection of HCOOCH3 toward W75N. The relative HCOOH/HCOOCH3 abundance ratio toward W75N is 0.26 which is more than twice as large as the abundance ratios found by Liu and colleagues. Furthermore, the hot core regions around W75N show a chemical differentiation between the O and N cores similar to what is seen toward the Orion Hot Core and Compact Ridge and W3(OH) and W3(H2O). It is also apparent from our observations that the high mass star forming region G45.47+0.05 does not contain any compact hot molecular core and as a consequence its chemistry may be similar to cold dark clouds. Finally, the formation of CH3COOH appears to favor HMCs with well mixed N and O, despite the fact that CH3COOH does not contain a N atom. If proved to be true, this is an important constraint on CH3COOH formation and possibly other structurally similar biomolecules.

  4. An all-sky sample of intermediate-mass star-forming regions

    Energy Technology Data Exchange (ETDEWEB)

    Lundquist, Michael J.; Kobulnicky, Henry A.; Alexander, Michael J. [Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071 (United States); Kerton, Charles R. [Department of Physics and Astronomy, Iowa State University, Ames, IA 50011 (United States); Arvidsson, Kim [Trull School of Sciences and Mathematics, Schreiner University, 2100 Memorial Boulevard, Kerrville, TX 78028 (United States)

    2014-04-01

    We present an all-sky sample of 984 candidate intermediate-mass Galactic star-forming regions that are color selected from the Infrared Astronomical Satellite (IRAS) Point Source Catalog and morphologically classify each object using mid-infrared Wide-field Infrared Survey Explorer (WISE) images. Of the 984 candidates, 616 are probable star-forming regions (62.6%), 128 are filamentary structures (13.0%), 39 are point-like objects of unknown nature (4.0%), and 201 are galaxies (20.4%). We conduct a study of four of these regions, IRAS 00259+5625, IRAS 00420+5530, IRAS 01080+5717, and IRAS 05380+2020, at Galactic latitudes |b| > 5° using optical spectroscopy from the Wyoming Infrared Observatory, along with near-infrared photometry from the Two-Micron All Sky Survey, to investigate their stellar content. New optical spectra, color-magnitude diagrams, and color-color diagrams reveal their extinctions, spectrophotometric distances, and the presence of small stellar clusters containing 20-78 M {sub ☉} of stars. These low-mass diffuse star clusters contain ∼65-250 stars for a typical initial mass function, including one or more mid-B stars as their most massive constituents. Using infrared spectral energy distributions we identify young stellar objects near each region and assign probable masses and evolutionary stages to the protostars. The total infrared luminosity lies in the range 190-960 L {sub ☉}, consistent with the sum of the luminosities of the individually identified young stellar objects.

  5. Iron meteorites as remnants of planetesimals formed in the terrestrial planet region.

    Science.gov (United States)

    Bottke, William F; Nesvorný, David; Grimm, Robert E; Morbidelli, Alessandro; O'Brien, David P

    2006-02-16

    Iron meteorites are core fragments from differentiated and subsequently disrupted planetesimals. The parent bodies are usually assumed to have formed in the main asteroid belt, which is the source of most meteorites. Observational evidence, however, does not indicate that differentiated bodies or their fragments were ever common there. This view is also difficult to reconcile with the fact that the parent bodies of iron meteorites were as small as 20 km in diameter and that they formed 1-2 Myr earlier than the parent bodies of the ordinary chondrites. Here we show that the iron-meteorite parent bodies most probably formed in the terrestrial planet region. Fast accretion times there allowed small planetesimals to melt early in Solar System history by the decay of short-lived radionuclides (such as 26Al, 60Fe). The protoplanets emerging from this population not only induced collisional evolution among the remaining planetesimals but also scattered some of the survivors into the main belt, where they stayed for billions of years before escaping via a combination of collisions, Yarkovsky thermal forces, and resonances. We predict that some asteroids are main-belt interlopers (such as (4) Vesta). A select few may even be remnants of the long-lost precursor material that formed the Earth.

  6. Sulphur abundance determinations in star-forming regions-I: Ionization Correction Factor

    CERN Document Server

    Dors, O L; Hagele, G F; Cardaci, M V; Krabbe, A C

    2016-01-01

    In the present work we used a grid of photoionization models combined with stellar population synthesis models to derive reliable Ionization Correction Factors (ICFs) for the sulphur in star-forming regions. These models cover a large range of nebular parameters and yielding ionic abundances in consonance with those derived through optical and infrared observational data of star-forming regions. From our theoretical ICFs, we suggested an {\\alpha} value of 3.27 in the classical Stasinska formulae. We compared the total sulphur abundance in the gas phase of a large sample of objects by using our Theoretical ICF and other approaches. In average, the differences between the determinations via the use of the different ICFs considered are similar to the uncertainties in the S/H estimations. Nevertheless, we noted that for some objects it could reach up to about 0.3 dex for the low metallicity regime. Despite of the large scatter of the points, we found a trend of S/O ratio to decrease with the metallicity, independ...

  7. A kinematic study and membership analysis of the Lupus star-forming region

    CERN Document Server

    Galli, P A B; Teixeira, R; Ducourant, C

    2013-01-01

    This paper is dedicated to investigating the kinematic properties of the Lupus moving group of young stars with the primary objective of deriving individual parallaxes for each group member. We identify those stars in the Lupus star-forming region that define the comoving association of young stars by utilizing our new and improved convergent point search method that allows us to derive the precise position of the convergent point of the comoving association from the stars' proper motions. We used published proper motion catalogs and searched the literature for radial velocities, which are needed to compute individual parallaxes. We supplemented the radial velocity data with new measurements from spectroscopic observations performed with the FEROS spectrograph mounted on the MPG/ESO 2.2m telescope at La Silla. We identify a comoving group with 109 pre-main sequence stars and candidates that define the kinematic properties of the Lupus low-mass star-forming region. We derive individual parallaxes for stars wit...

  8. Fluctuations and Shape of Cooperative Rearranging Regions in Glass-Forming Liquids

    Science.gov (United States)

    Biroli, Giulio; Cammarota, Chiara

    2017-01-01

    We develop a theory of amorphous interfaces in glass-forming liquids. We show that the statistical properties of these surfaces, which separate regions characterized by different amorphous arrangements of particles, coincide with the ones of domain walls in the random field Ising model. A major consequence of our results is that supercooled liquids are characterized by two different static lengths: the point-to-set ξPS , which is a measure of the spatial extent of cooperative rearranging regions, and the wandering length ξ⊥, which is related to the fluctuations of their shape. We find that ξ⊥ grows when approaching the glass transition but slower than ξPS. The wandering length increases as sc-1 /2, where sc is the configurational entropy. Our results strengthen the relationship with the random field Ising model found in recent works. They are in agreement with previous numerical studies of amorphous interfaces and provide a theoretical framework for explaining numerical and experimental findings on pinned particle systems and static lengths in glass-forming liquids.

  9. H2D+ in the high mass star-forming Region Cygnus-X

    CERN Document Server

    Pillai, Thushara; Kauffmann, Jens; Zhang, Qizhou; Thompson, Mark; Lis, Darek

    2012-01-01

    H2D+ is a primary ion which dominates the gas-phase chemistry of cold dense gas. Therefore it is hailed as a unique tool in probing the earliest, prestellar phase of star formation. Observationally, its abundance and distribution is however just beginning to be understood in low-mass prestellar and cluster-forming cores. In high mass star forming regions, H2D+ has been detected only in two cores, and its spatial distribution remains unknown. Here we present the first map of the 372 GHz ortho-H2D+ and N2H+ 4-3 transition in the DR21 filament of Cygnus-X with the JCMT, and N2D+ 3--2 and dust continuum with the SMA. We have discovered five very extended (<= 34000 AU diameter) weak structures in H2D+ in the vicinity of, but distinctly offset from embedded protostars. More surprisingly, the H2D+ peak is not associated with either a dust continuum or N2D+ peak. We have therefore uncovered extended massive cold dense gas that was undetected with previous molecular line and dust continuum surveys of the region. Th...

  10. Water in low-mass star-forming regions with Herschel: HIFI spectroscopy of NGC1333

    CERN Document Server

    Kristensen, L E; van Dishoeck, E F; Yıldız, U A; Doty, S D; Herczeg, G J; Liu, F -C; Parise, B; Jørgensen, J K; van Kempen, T A; Brinch, C; Wampfler, S F; Bruderer, S; Benz, A O; Hogerheijde, M R; Deul, E; Bachiller, R; Baudry, A; Benedettini, M; Bergin, E A; Bjerkeli, P; Blake, G A; Bontemps, S; Braine, J; Caselli, P; Cernicharo, J; Codella, C; Daniel, F; de Graauw, Th; di Giorgio, A M; Dominik, C; Encrenaz, P; Fich, M; Fuente, A; Giannini, T; Goicoechea, J R; Helmich, F; Herpin, F; Jacq, T; Johnstone, D; Kaufman, M J; Larsson, B; Lis, D; Liseau, R; Marseille, M; McCoey, C; Melnick, G; Neufeld, D; Nisini, B; Olberg, M; Pearson, J C; Plume, R; Risacher, C; Santiago-Garcia, J; Saraceno, P; Shipman, R; Tafalla, M; Tielens, A G G M; van der Tak, F; Wyrowski, F; Beintema, D; de Jonge, A; Dieleman, P; Ossenkopf, V; Roelfsema, P; Stutzki, J; Whyborn, N

    2010-01-01

    'Water In Star-forming regions with Herschel' (WISH) is a key programme dedicated to studying the role of water and related species during the star-formation process and constraining the physical and chemical properties of young stellar objects. The Heterodyne Instrument for the Far-Infrared (HIFI) on the Herschel Space Observatory observed three deeply embedded protostars in the low-mass star-forming region NGC1333 in several H2-16O, H2-18O, and CO transitions. Line profiles are resolved for five H16O transitions in each source, revealing them to be surprisingly complex. The line profiles are decomposed into broad (>20 km/s), medium-broad (~5-10 km/s), and narrow (20 km/s), indicating that its physical origin is the same as for the broad H2-16O component. In one of the sources, IRAS4A, an inverse P Cygni profile is observed, a clear sign of infall in the envelope. From the line profiles alone, it is clear that the bulk of emission arises from shocks, both on small (<1000 AU) and large scales along the out...

  11. X-ray and Radio Observations of the Massive Star Forming Region IRAS 20126+4104

    CERN Document Server

    Montes, Virginie A; Anderson, Crystal; Rosero, Viviana

    2015-01-01

    We present results of Chandra ACIS-I and Karl G. Jansky Very Large Array (VLA) 6 cm continuum observations of the IRAS 20126+4104 massive star forming region. We detect 150 X-ray sources within the 17 arcmin x 17 arcmin ACIS-I field, and a total of 13 radio sources within the 9'.2 primary beam at 4.9 GHz. Among these are the first 6 cm detections of the central sources reported by Hofner et al. (2007), namely I20N1, I20S, and I20var. A new variable radio sources is also reported. Searching the 2MASS archive we identified 88 NIR counterparts to the X-ray sources. Only 4 of the X-ray sources had 6 cm counterparts. Based on an NIR color-color analysis, and on the Besancon simulation of Galactic stellar populations (Robin et al. 2003), we estimate that about 90 X-ray sources are associated with this massive star forming region. We detect an increasing surface density of X-ray sources toward the massive protostar and infer the presence of a cluster of at least 46 YSOs within a distance of 1.2 pc from the massive p...

  12. Chemical Evolution in High-Mass Star-Forming Regions: Results from the MALT90 Survey

    CERN Document Server

    Hoq, Sadia; Foster, Jonathan B; Sanhueza, Patricio; Guzman, Andres; Whitaker, J Scott; Claysmith, Christopher; Rathborne, Jill M; Vasyunina, Tatiana; Vasyunin, Anton

    2013-01-01

    The chemical changes of high-mass star-forming regions provide a potential method for classifying their evolutionary stages and, ultimately, ages. In this study, we search for correlations between molecular abundances and the evolutionary stages of dense molecular clumps associated with high-mass star formation. We use the molecular line maps from Year 1 of the Millimetre Astronomy Legacy Team 90 GHz (MALT90) Survey. The survey mapped several hundred individual star-forming clumps chosen from the ATLASGAL survey to span the complete range of evolution, from prestellar to protostellar to H II regions. The evolutionary stage of each clump is classified using the Spitzer GLIMPSE/MIPSGAL mid-IR surveys. Where possible, we determine the dust temperatures and H2 column densities for each clump from Herschel Hi-GAL continuum data. From MALT90 data, we measure the integrated intensities of the N2H+, HCO+, HCN and HNC (1-0) lines, and derive the column densities and abundances of N2H+ and HCO+. The Herschel dust tempe...

  13. The molecular composition of the planet-forming regions of protoplanetary disks across the luminosity regime

    CERN Document Server

    Walsh, Catherine; van Dishoeck, Ewine F

    2015-01-01

    (Abridged) Near- to mid-IR observations of protoplanetary disks show that the inner regions (<10AU) are rich in small organic volatiles (e.g., C2H2 and HCN). Trends in the data suggest that disks around cooler stars (~3000K) are potentially more carbon- and molecule-rich than their hotter counterparts. Our aims are to explore the composition of the planet-forming region of disks around stars from M dwarf to Herbig Ae and compare with the observed trends. Models of the disk physical structure are coupled with a gas-grain chemical network to map the abundances in the planet-forming zone. N2 self shielding, X-ray-induced chemistry, and initial abundances, are investigated. The composition in the 'observable' atmosphere is compared with that in the midplane where the planet-building reservoir resides. M dwarf disk atmospheres are relatively more molecule rich than those for T Tauri or Herbig Ae disks. The weak far-UV flux helps retain this complexity which is enhanced by X-ray-induced ion-molecule chemistry. N...

  14. Zeeman effect in sulfur monoxide. A tool to probe magnetic fields in star forming regions

    Science.gov (United States)

    Cazzoli, Gabriele; Lattanzi, Valerio; Coriani, Sonia; Gauss, Jürgen; Codella, Claudio; Ramos, Andrés Asensio; Cernicharo, José; Puzzarini, Cristina

    2017-09-01

    Context. Magnetic fields play a fundamental role in star formation processes and the best method to evaluate their intensity is to measure the Zeeman effect of atomic and molecular lines. However, a direct measurement of the Zeeman spectral pattern from interstellar molecular species is challenging due to the high sensitivity and high spectral resolution required. So far, the Zeeman effect has been detected unambiguously in star forming regions for very few non-masing species, such as OH and CN. Aims: We decided to investigate the suitability of sulfur monoxide (SO), which is one of the most abundant species in star forming regions, for probing the intensity of magnetic fields via the Zeeman effect. Methods: We investigated the Zeeman effect for several rotational transitions of SO in the (sub-)mm spectral regions by using a frequency-modulated, computer-controlled spectrometer, and by applying a magnetic field parallel to the radiation propagation (i.e., perpendicular to the oscillating magnetic field of the radiation). To support the experimental determination of the g factors of SO, a systematic quantum-chemical investigation of these parameters for both SO and O2 has been carried out. Results: An effective experimental-computational strategy for providing accurate g factors as well as for identifying the rotational transitions showing the strongest Zeeman effect has been presented. Revised g factors have been obtained from a large number of SO rotational transitions between 86 and 389 GHz. In particular, the rotational transitions showing the largest Zeeman shifts are: N,J = 2, 2 ← 1, 1 (86.1 GHz), N,J = 4, 3 ← 3, 2 (159.0 GHz), N,J = 1, 1 ← 0, 1 (286.3 GHz), N,J = 2, 2 ← 1, 2 (309.5 GHz), and N,J = 2, 1 ← 1, 0 (329.4 GHz). Our investigation supports SO as a good candidate for probing magnetic fields in high-density star forming regions. The complete list of measured Zeeman components is only available at the CDS via anonymous ftp to http

  15. The Role of Grain Surface Reactions in the Chemistry of Star Forming Regions

    Science.gov (United States)

    Kress, M. E.; Tielens, A. G. G. M.; Roberge, W. G.

    1998-01-01

    The importance of reactions at the surfaces of dust grains has long been recognized to be one of the two main chemical processes that form molecules in cold, dark interstellar clouds where simple, saturated (fully-hydrogenated) molecules such as H2 water, methanol, H2CO, H2S, ammonia and CH4 are present in quantities far too high to be consistent with their extremely low gas phase formation rates. In cold dark regions of interstellar space, dust grains provide a substrate onto which gas-phase species can accrete and react. Grains provide a "third body" or a sink for the energy released in the exothermic reactions that form chemical bonds. In essence, the surfaces of dust grains open up alternative reaction pathways to form observed molecules whose abundances cannot be explained with gas-phase chemistry alone. This concept is taken one step further in this work: instead of merely acting as a substrate onto which radicals and molecules may physically adsorb, some grains may actively participate in the reaction itself, forming chemical bonds with the accreting species. Until recently, surface chemical reactions had not been thought to be important in warm circumstellar media because adspecies rapidly desorb from grains at very low temperatures; thus, the residence times of molecules and radicals on the surface of grains at all but the lowest temperatures are far too short to allow these reactions to occur. However, if the adspecies could adsorb more strongly, via a true chemical bond with surfaces of some dust grains, then grain surface reactions will play an important role in warm circumstellar regions as well. In this work, the surface-catalyzed reaction CO + 3 H2 yields CH4 + H2O is studied in the context that it may be very effective at converting the inorganic molecule CO into the simplest organic compound, methane. H2 and CO are the most abundant molecules in space, and the reaction converting them to methane, while kinetically inhibited in the gas phase under

  16. Star forming regions linked to RCW78 and the discovery of a new IR bubble

    CERN Document Server

    Cappa, C E; Romero, G A; Duronea, N U; Firpo, V

    2013-01-01

    With the aim of investigating the presence of molecular and dust clumps linked to two star forming regions identified in the expanding molecular envelope of the stellar wind bubble RCW78, we analyzed the distribution of the molecular gas and cold dust. To accomplish this study we performed dust continuum observations at 870 \\mu m and 13CO(2-1) line observations with the APEX telescope, using LABOCA and SHeFI-1 instruments, respectively, and analyzed Herschel images at 70, 160, 250, 350, and 500 \\mu m. These observations allowed us to identify cold dust clumps linked to region B (named the Southern clump) and region C (clumps 1 and 2) and an elongated Filament. Molecular gas was clearly detected linked to the Southern clump and the Filament. The velocity of the molecular gas is compatible with the location of the dense gas in the expanding envelope of RCW78. We estimate dust temperatures and total masses for the dust condensations from the emissions at different wavelengths in the far-IR and from the molecular...

  17. Density Profiles in Molecular Cloud Cores Associated with High-Mass Star-Forming Regions

    CERN Document Server

    Pirogov, Lev E

    2009-01-01

    Radial density profiles for the sample of dense cores associated with high-mass star-forming regions from southern hemisphere have been derived using the data of observations in continuum at 250 GHz. Radial density profiles for the inner regions of 16 cores (at distances $\\la 0.2-0.8$ pc from the center) are close on average to the $\\rho\\propto r^{-\\alpha}$ dependence, where $\\alpha=1.6\\pm 0.3$. In the outer regions density drops steeper. An analysis with various hydrostatic models showed that the modified Bonnor-Ebert model, which describes turbulent sphere confined by external pressure, is preferable compared with the logotrope and polytrope models practically in all cases. With a help of the Bonnor-Ebert model, estimates of central density in a core, non-thermal velocity dispersion and core size are obtained. The comparison of central densities with the densities derived earlier from the CS modeling reveals differences in several cases. The reasons of such differences are probably connected with the presen...

  18. Sejong open cluster survey (SOS) - V. The active star forming region Sh 2-255 -- 257

    CERN Document Server

    Lim, Beomdu; Hur, Hyeonoh; Lee, Byeong-Cheol; Bessell, Michael S; Kim, Jinyoung S; Lee, Kang Hwan; Park, Byeong-Gon; Jeong, Gwanghui

    2015-01-01

    There is much observational evidence that active star formation is taking place in the HII regions Sh 2-255 -- 257. We present a photometric study of this star forming region (SFR) using imaging data obtained in passbands from the optical to the mid-infrared in order to study the star formation process. A total of 218 members were identified using various selection criteria based on their observational properties. The SFR is reddened by at least E(B-V) = 0.8 mag, and the reddening law toward the region is normal (R_V = 3.1). From the zero-age main sequence fitting method it is confirmed that the SFR is 2.1 +/- 0.3 kpc from the Sun. The median age of the identified members is estimated to be about 1.3 Myr from comparison of the Hertzsprung-Russell diagram (HRD) with stellar evolutionary models. The initial mass function (IMF) is derived from the HRD and the near-infrared (J, J-H) color-magnitude diagram. The slope of the IMF is about Gamma = -1.6 +/- 0.1, which is slightly steeper than that of the Salpeter/Kro...

  19. Studying the kinematics of the giant star-forming region 30 Doradus. I. The data

    CERN Document Server

    Torres-Flores, S; Apellániz, J Maíz; Rubio, M; Bosch, G; Hénault-Brunet, V; Evans, C J

    2013-01-01

    We present high-quality VLT-FLAMES optical spectroscopy of the nebular gas in the giant star-forming region 30 Doradus. In this paper, the first of a series, we introduce our observations and discuss the main kinematic features of 30 Dor, as revealed by the spectroscopy of the ionized gas in the region. The primary data set consists of regular grid of nebular observations, which we used to produce a spectroscopic datacube of 30 Dor, centered on the massive star cluster R136 and covering a field-of-view of 10'x10'. The main emission lines present in the datacube are from Halpha and [NII]6548,6584. The Halpha emission-line profile varies across the region from simple single-peaked emission to complex, multiple-component profiles, suggesting that different physical mechanisms are acting on the excited gas. To analyse the gas kinematics we fit Gaussian profiles to the observed Halpha features. Unexpectedly, the narrowest Halpha profile in our sample lies close to the supernova remnant 30 Dor B. We present maps of...

  20. B- and A-Type Stars in the Taurus-Auriga Star Forming Region

    CERN Document Server

    Mooley, Kunal P; Rebull, Luisa M; Padgett, Deborah L; Knapp, Gillian R

    2013-01-01

    We describe the results of a search for early-type stars associated with the Taurus-Auriga molecular cloud complex, a diffuse nearby star-forming region noted as lacking young stars of intermediate and high mass. We investigate several sets of possible O, B and early A spectral class members. The first is a group of stars for which mid-infrared images show bright nebulae, all of which can be associated with stars of spectral type B. The second group consists of early-type stars compiled from (i) literature listings in SIMBAD; (ii) B stars with infrared excesses selected from the Spitzer Space Telescope survey of the Taurus cloud; (iii) magnitude- and color-selected point sources from the 2MASS; and (iv) spectroscopically identified early-type stars from the SDSS coverage of the Taurus region. We evaluated stars for membership in the Taurus-Auriga star formation region based on criteria involving: spectroscopic and parallactic distances, proper motions and radial velocities, and infrared excesses or line emiss...

  1. Infrared polarization images of star-forming regions. I - The ubiquity of bipolar structure

    Science.gov (United States)

    Tamura, M.; Gatley, Ian; Joyce, R. R.; Ueno, M.; Suto, H.; Sekiguchi, M.

    1991-01-01

    The inefficiency of the stellar formation process leads rather generally to high residual dust densities, and so to the existence of infrared reflection nebulosity (IRN), in regions of star formation. Polarization images of several star-forming regions with mass outflows (GSS 30, S255, GL 5180, GL 2591, GGD 27, and NGC 7538) presented here: (1) establish the universality of bipolarity and of shell or cavity structure in the IRN consistent with that of CO outflow; (2) identify the source of the mass outflow in each case; (3) show that the opening angle near this central source is large; and (4) demonstrate several instances of multiple shells, probably arising from episodic mass loss. Astrometry of 2.2-micron sources with arcsecond accuracy identifies the illuminating source of each IRN uniquely with a compact H II region or a bright IR source. The polarization images provide strong evidence for large-scale dust toroids around each of these sources. The density and mass of these disks are estimated from the extinction through the disk.

  2. An Ultraviolet Study of Star-Forming Regions in M31

    CERN Document Server

    Kang, Yongbeom; Rey, Soo-Chang

    2009-01-01

    We present a comprehensive study of star-forming (SF) regions in the nearest large spiral galaxy M31. We use GALEX far-UV (1344-1786 \\AA, FUV) and near-UV (1771-2831 \\AA, NUV) imaging to detect young massive stars and trace the recent star formation across the galaxy. The FUV and NUV flux measurements of the SF regions, combined with ground-based data for estimating the reddening by interstellar dust from the massive stars they contain, are used to derive their ages and masses. The GALEX imaging, combining deep sensitivity and entire coverage of the galaxy, provides a complete picture of the recent star formation in M31 and its variation with environment throughout the galaxy. The FUV and NUV measurements are sensitive to detect stellar populations younger than a few hundred Myrs. We detected 894 SF regions, with size > 1600 pc^{2} above an average FUV flux limit of ~ 26 ABmag arcsecond^{-2}, over the whole 26 kpc galaxy disk. We derive the star-formation history of M31 within this time span. The star formati...

  3. Self-similar fragmentation regulated by magnetic fields in a region forming massive stars

    Science.gov (United States)

    Li, Hua-Bai; Yuen, Ka Ho; Otto, Frank; Leung, Po Kin; Sridharan, T. K.; Zhang, Qizhou; Liu, Hauyu; Tang, Ya-Wen; Qiu, Keping

    2015-04-01

    Most molecular clouds are filamentary or elongated. For those forming low-mass stars (8 solar masses). But whether the core field morphologies are inherited from the intercloud medium or governed by cloud turbulence is unknown, as is the effect of magnetic fields on cloud fragmentation at scales of 10 to 0.1 parsecs. Here we report magnetic-field maps inferred from polarimetric observations of NGC 6334, a region forming massive stars, on the 100 to 0.01 parsec scale. NGC 6334 hosts young star-forming sites where fields are not severely affected by stellar feedback, and their directions do not change much over the entire scale range. This means that the fields are dynamically important. The ordered fields lead to a self-similar gas fragmentation: at all scales, there exist elongated gas structures nearly perpendicular to the fields. Many gas elongations have density peaks near the ends, which symmetrically pinch the fields. The field strength is proportional to the 0.4th power of the density, which is an indication of anisotropic gas contractions along the field. We conclude that magnetic fields have a crucial role in the fragmentation of NGC 6334.

  4. Variations in H2O+/H2O ratios toward massive star-forming regions

    CERN Document Server

    Wyrowski, F; Herpin, F; Baudry, A; Bontemps, S; Chavarria, L; Frieswijk, W; Jacq, T; Marseille, M; Shipman, R; van Dishoeck, E F; Benz, A O; Caselli, P; Hogerheijde, M R; Johnstone, D; Liseau, R; Bachiller, R; Benedettini, M; Bergin, E; Bjerkeli, P; Blake, G; Braine, J; Bruderer, S; Cernicharo, J; Codella, C; Daniel, F; di Giorgio, A M; Dominik, C; Doty, S D; Encrenaz, P; Fich, M; Fuente, A; Giannini, T; Goicoechea, J R; de Graauw, Th; Helmich, F; Herczeg, G J; Jørgensen, J K; Kristensen, L E; Larsson, B; Lis, D; McCoey, C; Melnick, G; Nisini, B; Olberg, M; Parise, B; Pearson, J C; Plume, R; Risacher, C; Santiago, J; Saraceno, P; Tafalla, M; van Kempen, T A; Visser, R; Wampfler, S; Yıldız, U A; Black, J H; Falgarone, E; Gerin, M; Roelfsema, P; Dieleman, P; Beintema, D; De Jonge, A; Whyborn, N; Stutzki, J; Ossenkopf, V

    2010-01-01

    Early results from the Herschel Space Observatory revealed the water cation H2O+ to be an abundant ingredient of the interstellar medium. Here we present new observations of the H2O and H2O+ lines at 1113.3 and 1115.2 GHz using the Herschel Space Observatory toward a sample of high-mass star-forming regions to observationally study the relation between H2O and H2O+ . Nine out of ten sources show absorption from H2O+ in a range of environments: the molecular clumps surrounding the forming and newly formed massive stars, bright high-velocity outflows associated with the massive protostars, and unrelated low-density clouds along the line of sight. Column densities per velocity component of H2 O+ are found in the range of 10^12 to a few 10^13 cm-2 . The highest N(H2O+) column densities are found in the outflows of the sources. The ratios of H2O+/H2O are determined in a range from 0.01 to a few and are found to differ strongly between the observed environments with much lower ratios in the massive (proto)cluster e...

  5. Fragmentation in the massive star-forming region IRAS 19410+2336

    Science.gov (United States)

    Rodón, J. A.; Beuther, H.; Schilke, P.

    2012-09-01

    Context. The core mass functions (CMFs) of low-mass star-forming regions are found to resemble the shape of the initial mass function (IMF). A similar result is observed for the dust clumps in high-mass star-forming regions, although on spatial scales of clusters that do not resolve the substructure that is found in these massive clumps. The region IRAS 19410+2336 is one exception, having been observed on spatial scales on the order of ~2500 AU, which are sufficient to resolve the clump substructure into individual cores. Aims: We investigate the protostellar content of IRAS 19410+2336 at high spatial resolution at 1.4 mm, determining the temperature structure of the region and deriving its CMF. Methods: The massive star-forming region IRAS 19410+2336 was mapped with the PdBI (BCD configurations) at 1.4 mm and 3 mm in the continuum and several transitions of formaldehyde (H2CO) and methyl cyanide (CH3CN). The H2CO transitions were also observed with the IRAM 30 m Telescope. Results: We detect 26 continuum sources at 1.4 mm with a spatial resolution as low as ~2200 AU, several of them with counterparts at near- and mid-infrared wavelengths, distributed in two (proto)clusters. With the PdBI CH3CN and PdBI/IRAM 30 m H2CO emission, we derive the temperature structure of the region, ranging from 35 K to 90 K. Using these temperatures, we calculate the core masses of the detected sources, ranging from ~0.7 M⊙ to ~8 M⊙. These masses are strongly affected by the spatial filtering of the interferometer, which removes a common envelope with ~90% of the single-dish flux. Considering only the detected dense cores and accounting for binning effects as well as cumulative distributions, we derive a CMF, with a power-law index β = -2.3 ± 0.2. We resolve the Jeans length of the (proto)clusters by one order of magnitude, and only find a small velocity dispersion between the different subsources. Conclusions: Since we cannot unambiguously differentiate between protostellar and

  6. The molecular composition of the planet-forming regions of protoplanetary disks across the luminosity regime

    Science.gov (United States)

    Walsh, Catherine; Nomura, Hideko; van Dishoeck, Ewine

    2015-10-01

    Context. Near- to mid-infrared observations of molecular emission from protoplanetary disks show that the inner regions are rich in small organic volatiles (e.g., C2H2 and HCN). Trends in the data suggest that disks around cooler stars (Teff ≈ 3000 K) are potentially (i) more carbon-rich; and (ii) more molecule-rich than their hotter counterparts (Teff ≳ 4000 K). Aims: We explore the chemical composition of the planet-forming region (gas-grain chemical network to map the molecular abundances in the planet-forming zone. The effects of (i) N2 self shielding; (ii) X-ray-induced chemistry; and (iii) initial abundances, are investigated. The chemical composition in the "observable" atmosphere is compared with that in the disk midplane where the bulk of the planet-building reservoir resides. Results: M dwarf disk atmospheres are relatively more molecule rich than those for T Tauri or Herbig Ae disks. The weak far-UV flux helps retain this complexity which is enhanced by X-ray-induced ion-molecule chemistry. N2 self shielding has only a small effect in the disk molecular layer and does not explain the higher C2H2/HCN ratios observed towards cooler stars. The models underproduce the OH/H2O column density ratios constrained in Herbig Ae disks, despite reproducing (within an order of magnitude) the absolute value for OH: the inclusion of self shielding for H2O photodissociation only increases this discrepancy. One possible explanation is the adopted disk structure. Alternatively, the "hot" H2O (T ≳ 300 K) chemistry may be more complex than assumed. The results for the atmosphere are independent of the assumed initial abundances; however, the composition of the disk midplane is sensitive to the initial main elemental reservoirs. The models show that the gas in the inner disk is generally more carbon rich than the midplane ices. This effect is most significant for disks around cooler stars. Furthermore, the atmospheric C/O ratio appears larger than it actually is when

  7. Distribution of water in the G327.3-0.6 massive star-forming region

    Science.gov (United States)

    Leurini, S.; Herpin, F.; van der Tak, F.; Wyrowski, F.; Herczeg, G. J.; van Dishoeck, E. F.

    2017-06-01

    Aims: Following our past study of the distribution of warm gas in the G327.3-0.6 massive star-forming region, we aim here at characterizing the large-scale distribution of water in this active region of massive star formation made of individual objects in different evolutionary phases. We investigate possible variations of the water abundance as a function of evolution. Methods: We present Herschel/PACS (4'× 4') continuum maps at 89 and179 μm encompassing the whole region (Hii region and the infrared dark cloud, IRDC) and an APEX/SABOCA (2'× 2') map at 350 μm of the IRDC. New spectral Herschel/HIFI maps toward the IRDC region covering the low-energy water lines at 987 and 1113 GHz (and their H218O counterparts) are also presented and combined with HIFI pointed observations toward the G327 hot core region. We infer the physical properties of the gas through optical depth analysis and radiative transfer modeling of the HIFI lines. Results: The distribution of the continuum emission at 89 and 179 μm follows the thermal continuum emission observed at longer wavelengths, with a peak at the position of the hot core and a secondary peak in the Hii region, and an arch-like layer of hot gas west of this Hii region. The same morphology is observed in the p-H2O 111-000 line, in absorption toward all submillimeter dust condensations. Optical depths of approximately 80 and 15 are estimated and correspond to column densities of 1015 and 2 × 1014 cm-2, respectively, for the hot core and IRDC position. These values indicate an abundance of water relative to H2 of 3 × 10-8 toward the hot core, while the abundance of water does not change along the IRDC with values close to some 10-8. Infall (over at least 20″) is detected toward the hot core position with a rate of 1-1.3 × 10-2M⊙ /yr, high enough to overcome the radiation pressure that is due to the stellar luminosity. The source structure of the hot core region appears complex, with a cold outer gas envelope in

  8. Insights from Synthetic Star-forming Regions: I. Reliable Mock Observations from SPH Simulations

    CERN Document Server

    Koepferl, Christine M; Dale, James E; Biscani, Francesco

    2016-01-01

    Through synthetic observations of a hydrodynamical simulation of an evolving star-forming region, we assess how the choice of observational techniques affects the measurements of properties which trace star formation. Testing and calibrating observational measurements requires synthetic observations which are as realistic as possible. In this part of the paper series (Paper I), we explore different techniques for how to map the distributions of densities and temperatures from the particle-based simulations onto a Voronoi mesh suitable for radiative transfer and consequently explore their accuracy. We further test different ways to set up the radiative transfer in order to produce realistic synthetic observations. We give a detailed description of all methods and ultimately recommend techniques. We have found that the flux around 20 microns is strongly overestimated when blindly coupling the dust radiative transfer temperature with the hydrodynamical gas temperature. We find that when instead assuming a consta...

  9. Detections of 2 cm formaldehyde emissions towards Galactic star-forming regions with 6 cm counterpart

    Science.gov (United States)

    Chen, Xi; Shen, Zhi-Qiang; Li, Xiao-Qiong; Yang, Kai; Li, Juan; Wang, Jun-Zhi; Wu, Ya-Jun; Zhao, Rong-Bin; Wang, Jin-Qing; Dong, Jian; Jiang, Dong-Rong; Li, Bin

    2017-01-01

    We report the detections of H2CO emission at the 2 cm transition towards Galactic star-forming regions with known 6 cm counterpart using the Shanghai Tianma Radio Telescope (TMRT). One significant detection (in NGC7538) and two possible detections (in G23.01-0.41 and G29.96-0.02) were made. Comparing with previous observations, we found that there is a time lag of appearance of 2 cm and 6 cm emissions detected in NGC7538, contradicting with the prediction of radiative pumping via radio continuum radiation. Combinations of the variability of 6 cm masers in NGC7538 suggest that collisional pumping via high-velocity shocks could better explain the 6 cm H2CO maser emission. Under this scheme, excitation of the 2 cm maser may require a higher collision energy compared to the 6 cm transition.

  10. Optical and mid-infrared neon abundance determinations in star-forming regions

    CERN Document Server

    Dors, Oli L; Cardaci, Monica V; Perez-Montero, Enrique; Krabbe, Angela C; Vilchez, Jose M; Sales, Dinalva A; Riffel, Rogerio; Riffel, Rogemar A

    2013-01-01

    We employed observational spectroscopic data of star-forming regions compiled from the literature and photoionization models to analyse the neon ionic abundances obtained using both optical and mid-infrared emission-lines. Comparing Ne++/H+ ionic abundances from distinct methods, we found that, in average, the abundances obtained via IR emission-lines are higher than those obtained via optical lines by a factor of 4. Photoionization models with abundance variations along the radius of the hypothetical nebula provide a possible explanation for a large part of the difference between ionic abundances via optical and infrared emission-lines. Ionization Correction Factor (ICF) for the neon is obtained from direct determinations of ionic fractions using infrared emission-lines. A constant Ne/O ratio (logNe/O \\approx -0.70) for a large range of metallicity, independently of the ICF used to compute the neon total abundance is derived.

  11. A Hubble View of Star Forming Regions in the Magellanic Clouds

    CERN Document Server

    Gouliermis, D A; Brandner, W; Rosa, M R; Dolphin, A E; Schmalzl, M; Hennekemper, E; Zinnecker, H; Panagia, N; Chu, Y -H; Brandl, B; Quanz, S P; Robberto, M; De Marchi, G; Gruendl, R A; Romaniello, M

    2007-01-01

    The Magellanic Clouds (MCs) offer an outstanding variety of young stellar associations, in which large samples of low-mass stars (with masses less than 1 solar mass) currently in the act of formation can be resolved and explored sufficiently with the Hubble Space Telescope. These pre-main sequence (PMS) stars provide a unique snapshot of the star formation process, as it is being recorded for the last 20 Myr, and they give important information on the low-mass Initial Mass Function (IMF) of their host environments. We present the latest results from observations with the Advanced Camera for Surveys (ACS) of such star-forming regions in the MCs, and discuss the importance of Hubble}for a comprehensive collection of substantial information on the most recent low-mass star formation and the low-mass IMF in the MCs.

  12. A kinematic study of the giant star-forming region 30 Doradus

    CERN Document Server

    Torres-Flores, Sergio; Apellániz, Jesús Maíz; Rubio, Mónica; Bosch, Guillermo

    2012-01-01

    We present, for the first time, an optical spectroscopic data cube of the giant star-forming region 30 Doradus, obtained with the GIRAFFE on the VLT at Paranal Observatory. The main emission lines present in this data cube correspond to H{\\alpha}, [NII] 6548 {\\AA} and [NII] 6584 {\\AA}. By using this data set, we found that H{\\alpha} presents from simple to multiple profiles, which suggests that different physical mechanisms act in different ways on the excited gas in 30 Doradus. We found, at least, three unclassified large expanding structures. These structures correlate with peaks in the X-ray distribution. Given the excellent signal-to-noise ratio and the large spatial coverage of this data cube, we have studied in detail the kinematics of 30 Doradus, showing the importance of the small scale phenomena on the integrated properties of 30 Doradus.

  13. Four Highly Luminous Massive Star Forming Regions in the Norma Spiral Arm II. Deep NIR imaging

    CERN Document Server

    Chavarria, L; Garay, G; Escala, A; Bronfman, L; Lizano, S

    2009-01-01

    We present sensitive NIR (J, H and K) imaging observations toward four luminous massive star forming regions in the Norma Spiral Arm: G324.201+0.119, G328.307+0.432, G329.337+0.147 and G330.949-0.174. We identify three clusters of young stellar objects (YSO) based on surface density diagnostics. We also find that sources detected only in the H and K-bands and with colors corresponding to spectral types earlier than B2, are likely YSOs. We analyze the spatial distribution of stars of different masses and find signatures in two clusters of primordial mass segregation which can't be explained as due to incompleteness effects. We show that dynamic interactions of cluster members with the dense gas from the parent core can explain the observed mass segregation, indicating that the gas plays an important role in the dynamics of young clusters.

  14. Chemical Evolution in High-mass Star-forming Regions: Results from the MALT90 Survey

    Science.gov (United States)

    Hoq, Sadia; Jackson, James M.; Foster, Jonathan B.; Sanhueza, Patricio; Guzmán, Andrés; Whitaker, J. Scott; Claysmith, Christopher; Rathborne, Jill M.; Vasyunina, Tatiana; Vasyunin, Anton

    2013-11-01

    The chemical changes of high-mass star-forming regions provide a potential method for classifying their evolutionary stages and, ultimately, ages. In this study, we search for correlations between molecular abundances and the evolutionary stages of dense molecular clumps associated with high-mass star formation. We use the molecular line maps from Year 1 of the Millimetre Astronomy Legacy Team 90 GHz (MALT90) Survey. The survey mapped several hundred individual star-forming clumps chosen from the ATLASGAL survey to span the complete range of evolution, from prestellar to protostellar to H II regions. The evolutionary stage of each clump is classified using the Spitzer GLIMPSE/MIPSGAL mid-IR surveys. Where possible, we determine the dust temperatures and H2 column densities for each clump from Herschel/Hi-GAL continuum data. From MALT90 data, we measure the integrated intensities of the N2H+, HCO+, HCN and HNC (1-0) lines, and derive the column densities and abundances of N2H+ and HCO+. The Herschel dust temperatures increase as a function of the IR-based Spitzer evolutionary classification scheme, with the youngest clumps being the coldest, which gives confidence that this classification method provides a reliable way to assign evolutionary stages to clumps. Both N2H+ and HCO+ abundances increase as a function of evolutionary stage, whereas the N2H+ (1-0) to HCO+ (1-0) integrated intensity ratios show no discernable trend. The HCN (1-0) to HNC(1-0) integrated intensity ratios show marginal evidence of an increase as the clumps evolve.

  15. Water in low-mass star-forming regions with Herschel

    DEFF Research Database (Denmark)

    Kristensen, L. E.; Visser, R.; Van Dishoeck, E. F.

    2010-01-01

    "Water In Star-forming regions with Herschel" (WISH) is a key programme dedicated to studying the role of water and related species during the star-formation process and constraining the physical and chemical properties of young stellar objects. The Heterodyne Instrument for the Far-Infrared (HIFI...... is observed, a clear sign of infall in the envelope. From the line profiles alone, it is clear that the bulk of emission arises from shocks, both on small (1000 AU) and large scales along the outflow cavity walls (∼10 000 AU). The H2O line profiles are compared to CO line profiles to constrain the H2O...... abundance as a function of velocity within these shocked regions. The H2O/CO abundance ratios are measured to be in the range of ∼0.1-1, corresponding to H2O abundances of ∼10-5-10-4 with respect to H 2. Approximately 5-10% of the gas is hot enough for all oxygen to be driven into water in warm post...

  16. The molecular environment of the Galactic star forming region G19.61-0.23

    CERN Document Server

    Santangelo, G; Leurini, S; Walmsley, C M; Cesaroni, R; Bronfman, L; Carey, S; Gregorini, L; Menten, K M; Molinari, S; Noriega-Crespo, A; Olmi, L; Schuller, F

    2010-01-01

    We present single-dish (sub)millimeter observations of gas and dust in the Galactic high-mass star-forming region G19.61-0.23, with the aim of studying the large-scale properties and physical conditions of the molecular gas across the region. The final aim is to compare the large-scale (about 100 pc) properties with the small-scale (about 3 pc) properties and to consider possible implications for extragalactic studies. We have mapped CO isotopologues in the J=1-0 transition using the FCRAO-14m telescope and the J=2-1 transition using the IRAM-30m telescope. We have also used data from the ATLASGAL survey and from the BU-FCRAO Galactic Ring Survey, as well as the Spitzer infrared Galactic plane surveys GLIMPSE and MIPSGAL to characterize the star-formation activity within the molecular clouds. We reveal a population of molecular clumps in the 13CO(1-0) emission. Our analysis of the 13CO suggests that the virial parameter (ratio of kinetic to gravitational energy) varies over an order of magnitude between clump...

  17. The SONYC survey: Towards a complete census of brown dwarfs in star forming regions

    CERN Document Server

    Muzic, K; Geers, V C; Jayawardhana, R; Tamura, M; Dawson, P; Ray, T P

    2013-01-01

    SONYC, short for "Substellar Objects in Nearby Young Clusters", is a survey program to provide a census of the substellar population in nearby star forming regions. We have conducted deep optical and near-infrared photometry in five young regions (NGC1333, rho Ophiuchi, Chamaeleon-I, Upper Sco, and Lupus-3), combined with proper motions, and followed by extensive spectroscopic campaigns with Subaru and VLT, in which we have obtained more than 700 spectra of candidate low-mass objects. We have identified and characterized more than 60 new substellar objects, among them a handful of objects with masses close to, or below the Deuterium burning limit. Through SONYC and surveys by other groups, the substellar IMF is now well characterized down to ~ 5 - 10 MJup, and we find that the ratio of the number of stars with respect to brown dwarfs lies between 2 and 6. A comprehensive survey of NGC 1333 reveals that, down to ~5MJup, free-floating objects with planetary masses are 20-50 times less numerous than stars, i.e. ...

  18. Modeling the water line emission from the high-mass star-forming region AFGL2591

    CERN Document Server

    Poelman, D R

    2007-01-01

    Context: observations of water lines are a sensitive probe of the geometry, dynamics and chemical structure of dense molecular gas. The launch of Herschel with on board HIFI and PACS allow to probe the behaviour of multiple water lines with unprecedented sensitivity and resolution. Aims: we investigate the diagnostic value of specific water transitions in high-mass star-forming regions. As a test case, we apply our models to the AFGL2591 region. Results: in general, for models with a constant water abundance, the ground state lines, i.e., 1_(10)-1_(01), 1_(11)-0_(00), and 2_(12)-1_(01), are predicted in absorption, all the others in emission. This behaviour changes for models with a water abundance jump profile in that the line profiles for jumps by a factor of ~10-100 are similar to the line shapes in the constant abundance models, whereas larger jumps lead to emission profiles. Asymmetric line profiles are found for models with a cavity outflow and depend on the inclination angle. Models with an outflow cav...

  19. An Infrared/X-ray Survey for New Members of the Taurus Star-Forming Region

    CERN Document Server

    Luhman, K L; Allen, P R; Cruz, K L

    2009-01-01

    We present the results of a search for new members of the Taurus star-forming region using data from the Spitzer Space Telescope and the XMM-Newton Observatory. We have obtained optical and near-infrared spectra of 44 sources that exhibit red Spitzer colors that are indicative of stars with circumstellar disks and 51 candidate young stars that were identified by Scelsi and coworkers using XMM-Newton. We also performed spectroscopy on four possible companions to members of Taurus that were reported by Kraus and Hillenbrand. Through these spectra, we have demonstrated the youth and membership of 41 sources, 10 of which were independently confirmed as young stars by Scelsi and coworkers. Five of the new Taurus members are likely to be brown dwarfs based on their late spectral types (>M6). One of the brown dwarfs has a spectral type of L0, making it the first known L-type member of Taurus and the least massive known member of the region (M=4-7 M_Jup). Another brown dwarf exhibits a flat infrared spectral energy d...

  20. The star forming region Monoceros R2 as a gamma-ray source

    CERN Document Server

    Martí, Josep; Muñoz-Arjonilla, Álvaro J; Sánchez-Ayaso, Estrella; Munar-Adrover, Pere; Sánchez-Sutil, Juan R; Romero, Gustavo E; Paredes, Josep M; Combi, Jorge A

    2013-01-01

    Context. After the release of the gamma-ray source catalog produced by the Fermi satellite during its first two years of operation, a significant fraction of sources still remain unassociated at lower energies. In addition to well-known high-energy emitters (pulsars, blazars, supernova remnants, etc.) theoretical expectations predict new classes of gamma-ray sources. In particular, gamma-ray emission could be associated with some of the early phases of stellar evolution, but this interesting possibility is still poorly understood. Aims. The aim of this paper is to assess the possibility of the Fermi gamma-ray source 2FGL J0607.5-0618c being associated with the massive star forming region Monoceros R2. Methods. A multi-wavelength analysis of the Monoceros R2 region is carried out using archival data at radio, infrared, X-ray, and gamma-ray wavelengths. The resulting observational properties are used to estimate the physical parameters needed to test the different physical scenarios. Results. We confirm the 2FG...

  1. On the kinematics of massive star forming regions: the case of IRAS 17233-3606

    CERN Document Server

    Leurini, S; Zapata, L; Beltran, M T; Schilke, P; Cesaroni, R

    2011-01-01

    Direct observations of accretion disks around high-mass young stellar objects would help to discriminate between different models of formation of massive stars. However, given the complexity of massive star forming regions, such studies are still limited in number. Additionally, there is still no general consensus on the molecular tracers to be used for such investigations. Because of its close distance and high luminosity, IRAS 17233-3606 is a potential good laboratory to search for traces of rotation in the inner gas around the protostar(s). Therefore, we selected the source for a detailed analysis of its molecular emission at 230 GHz with the SMA. We systematically investigated the velocity fields of transitions in the SMA spectra which are not affected by overlap with other transitions, and searched for coherent velocity gradients to compare them to the distribution of outflows in the region. Beside CO emission we also used high-angular H2 images to trace the outflow motions driven by the IRAS 17233-3606 ...

  2. Young open clusters in the galactic star forming region NGC 6357

    CERN Document Server

    Massi, Fabrizio; di Carlo, Elisa; Brand, Jan; Beltrán, Maria Teresa; Marconi, Gianni

    2014-01-01

    NGC6357 is an active star forming region with very young massive open clusters (OC). These clusters contain some of the most massive stars in the Galaxy and strongly interact with nearby giant molecular clouds (GMC). We study the young stellar populations of the region and of the OC Pismis24, focusing on their relationship with the nearby GMCs. We seek evidence of triggered star formation propagating from the clusters. We used new deep JHKs photometry, along with unpublished deep IRAC/Spitzer MIR photometry, complemented with optical HST/WFPC2 high spatial resolution photometry and X-ray Chandra observations, to constrain age, initial mass function, and star formation modes in progress. We carefully examine and discuss all sources of bias (saturation, confusion, different sensitivities, extinction). NGC6357 hosts three large young stellar clusters, of which Pismis24 is the most prominent. We found that Pismis24 is a very young (~1-3 Myr) OC with a Salpeter-like IMF and a few thousand members. A comparison bet...

  3. A very young star forming region detected by the ISOPHOT Serendipity Survey

    CERN Document Server

    Krause, O; Tóth, L V; Klaas, U; Haas, M; Stickel, M; Vavrek, R

    2003-01-01

    We present a multi-wavelength study of the star forming region ISOSS J 20298+3559, which was identified by a cross-correlation of cold compact sources from the 170 micron ISOPHOT Serendipity Survey (ISOSS) database coinciding with objects detected by the MSX, 2MASS and IRAS infrared surveys. ISOSS J 20298+3559 is associated with a massive dark cloud complex (M ~ 760 M$_{\\odot}$) and located in the Cygnus X giant molecular cloud. We derive a distance of 1800 pc on the basis of optical extinction data. The low average dust temperature (T ~ 16 K) and large mass (M ~ 120 M$_{\\odot}$) of the dense inner part of the cloud, which has not been dispersed, indicates a recent begin of star formation. The youth of the region is supported by the early evolutionary stage of several pre- and protostellar objects discovered across the regio n: I) Two candidate Class 0 objects with masses of 8 and 3.5 M$_{\\odot}$, II) a gravitationally bound, cold (T ~ 12 K) and dense (n(H$_{2}$) \\~ 2 x 10$^{5}$ cm$^{-3}$) cloud core with a m...

  4. Molecular Emission in Dense Massive Clumps from the Star-Forming Regions S231-S235

    CERN Document Server

    Ladeyschikov, D A; Tsivilev, A P; Sobolev, A M

    2016-01-01

    The article deals with observations of star-forming regions S231-S235 in 'quasi-thermal' lines of ammonia (NH$_3$), cyanoacetylene (HC$_3$N) and maser lines of methanol (CH$_3$OH) and water vapor (H$_2$O). S231-S235 regions is situated in the giant molecular cloud G174+2.5. We selected all massive molecular clumps in G174+2.5 using archive CO data. For the each clump we determined mass, size and CO column density. After that we performed observations of these clumps. We report about first detections of NH$_3$ and HC$_3$N lines toward the molecular clumps WB89 673 and WB89 668. This means that high-density gas is present there. Physical parameters of molecular gas in the clumps were estimated using the data on ammonia emission. We found that the gas temperature and the hydrogen number density are in the ranges 16-30 K and 2.8-7.2$\\times10^3$ cm$^{-3}$, respectively. The shock-tracing line of CH$_3$OH molecule at 36.2 GHz is newly detected toward WB89 673.

  5. Detection of Far-Infrared Features in Star-Forming Regions

    CERN Document Server

    Onaka, T; Onaka, Takashi; Okada, Yoko

    2003-01-01

    We report the detection of a feature at 65um and a broad feature around 100um in the far-infrared spectra of the diffuse emission from two active star-forming regions, the Carina nebula and Sharpless 171. The features are seen in the spectra over a wide area of the observed regions, indicating that the carriers are fairly ubiquitous species in the interstellar medium. A similar 65um feature has been detected in evolved stars and attributed to diopside, a Ca-bearing crystalline silicate. The present observations indicate the first detection of a crystalline silicate in the interstellar medium if this identification holds true also for the interstellar feature. A similar broad feature around 90um reported in the spectra of evolved stars has been attributed to calcite, a Ca-bearing carbonate mineral. The interstellar feature seems to be shifted to longer wavelengths and have a broader width although the precise estimate of the feature profile is difficult. As a carrier for the interstellar 100um feature, we inve...

  6. Water in massive star-forming regions: HIFI observations of W3 IRS5

    CERN Document Server

    Chavarria, L; Jacq, T; Braine, J; Bontemps, S; Baudry, A; Marseille, M; van der Tak, F; Pietropaoli, B; Wyrowski, F; Shipman, R; Frieswijk, W; van Dishoeck, E F; Cernicharo, J; Bachiller, R; Benedettini, M; Benz, A O; Bergin, E; Bjerkeli, P; Blake, G A; Bruderer, S; Caselli, P; Codella, C; Daniel, F; di Giorgio, A M; Dominik, C; Doty, S D; Encrenaz, P; Fich, M; Fuente, A; Giannini, T; Goicoechea, J R; de Graauw, Th; Hartogh, P; Helmich, F; Herczeg, G J; Hogerheijde, M R; Johnstone, D; Jørgensen, J K; Kristensen, L E; Larsson, B; Lis, D; Liseau, R; McCoey, C; Melnick, G; Nisini, B; Olberg, M; Parise, B; Pearson, J C; Plume, R; Risacher, C; Santiago-Garcia, J; Saraceno, P; Szczerba, J Stutzki R; Tafalla, M; Tielens, A; van Kempen, T A; Visser, R; Wampfler, S F; Willem, J; Yıldız, U A

    2010-01-01

    We present Herschel observations of the water molecule in the massive star-forming region W3 IRS5. The o-H17O 110-101, p-H18O 111-000, p-H2O 22 202-111, p-H2O 111-000, o-H2O 221-212, and o-H2O 212-101 lines, covering a frequency range from 552 up to 1669 GHz, have been detected at high spectral resolution with HIFI. The water lines in W3 IRS5 show well-defined high-velocity wings that indicate a clear contribution by outflows. Moreover, the systematically blue-shifted absorption in the H2O lines suggests expansion, presumably driven by the outflow. No infall signatures are detected. The p-H2O 111-000 and o-H2O 212-101 lines show absorption from the cold material (T ~ 10 K) in which the high-mass protostellar envelope is embedded. One-dimensional radiative transfer models are used to estimate water abundances and to further study the kinematics of the region. We show that the emission in the rare isotopologues comes directly from the inner parts of the envelope (T > 100 K) where water ices in the dust mantles ...

  7. Cluster approach to forming innovative model of developing mineral resources base of Russia’s regions

    Directory of Open Access Journals (Sweden)

    Andrey Gennad'evich Shelomentsev

    2012-03-01

    Full Text Available In this paper, the necessity of applying innovative model of developing mineral resources base of Russia’s regions and relevance of cluster approach for forming this model are proved. Components of process of clustering in the case of innovative developing mineral raw complex are proposed and analyzed: consolidation of socioeconomic potential of region, consolidation of potential of different branches of people’s activities, consolidation of processes of primary (wining sector in the single chain. In particular, the first component implies concentration of population in certain centers of gravitation. The second component implies consolidation of education, fundamental as well as applying science and production. The creating of administrative nets is necessary for that. For the realization of the first and the second components, the availability of clustering organization is necessary. The third component of process of clustering implies in prospect the adding of increasing amount of stages of product manufacturing. Eventually, the multi-stage structure of innovative process is analyzed.

  8. Fundamental properties of pre-main sequence stars in young, southern star forming regions: metallicities

    CERN Document Server

    James, D J; Santos, N C; Bouvier, J; James, David J.; Melo, Claudio; Santos, Nuno C.; Bouvier, Jerome

    2005-01-01

    Aims: The primary motivation for this project is to search for metal-rich star forming regions, in which, stars of super-solar metallicity will be created, as hopefully, will be extra-solar planets orbiting them ! Results: We find (pre-main sequence) model-dependent isochronal ages of the Lupus, Chamaeleon and CrA targets to be $9.1 \\pm 2.1$ Myr, $4.5 \\pm 1.6$ Myr and $9.0 \\pm 3.9$ Myr respectively. The majority of the stars have Li I 6707.8A equivalent widths similar to, or above those of, their similar mass Pleiades counterparts, confirming their youthfulness. Most stars are kinematic members, either single or binary, of their regions. We find a mean radial velocity for objects in the Lupus cloud to be ${\\bar {RV}}=+2.6 \\pm 1.8$ km s$^{-1}$, for the Chamaeleon I & II clouds, ${\\bar {RV}}=+12.8 \\pm 3.6$ km s$^{-1}$ whereas for the CrA cloud, we find ${\\bar {RV}}=-1.1 \\pm 0.5$ km s$^{-1}$. All stars are coronally and chromospherically active, exhibiting X-ray and H$\\alpha$ emission levels marginally less,...

  9. VLBA Survey of OH Masers in Star-Forming Regions II: Satellite Lines

    CERN Document Server

    Ruiz-Velasco, A E; Migenes, V; Wiggins, B K

    2016-01-01

    Using the Very Long Baseline Array (VLBA) we performed a high resolution OH maser survey in Galactic star-forming regions (SFRs). We observed all the ground state spectral lines: the main lines at 1665 and 1667 MHz and the satellite lines at 1612 and 1720 MHz. Due to the exceptionality of finding satellite lines in SFRs, we will focus our discussion on those lines. In our sample of 41 OH maser sources, five (12%) showed the 1612 MHz line and ten (24%) showed the 1720 MHz line, with only one source showing both lines. We find that 1720 MHz emission is correlated with the presence of HII regions, suggesting that this emission could be used to diagnose or trace high-mass star formation. We include an analysis of the possible mechanisms that could be causing this correlation as well as assessing the possible relationships between lines in our sample. In particular, the presence of magnetic fields seems to play an important role, as we found Zeeman splitting in four of our sources (W75 N, W3(OH), W51 and NGC 7538)...

  10. Outflow and Infall in a Sample of Massive Star Forming Regions

    CERN Document Server

    Klaassen, P D

    2007-01-01

    We present single pointing observations of SiO, HCO$^+$ and H$^{13}$CO$^+$ from the James Clerk Maxwell Telescope towards 23 massive star forming regions previously known to contain molecular outflows and ultracompact HII regions. We detected SiO towards 14 sources and suggest that the non-detections in the other nine sources could be due to those outflows being older and without ongoing shocks to replenish the SiO. We serendipitously detected SO$_2$ towards 17 sources in the same tuning as HCO$^+$. We detected HCO$^+$ towards all sources, and suggest that it is tracing infall in nine cases. For seven infall candidates, we estimate mass infall rates between 1$\\times10^{-2}$ and 2$\\times10^{-5}$ M$_{\\odot}$ yr$^{-1}$. Seven sources show both SiO detections (young outflows) and HCO$^+$ infall signatures. We also find that the abundance of H$^{13}$CO$^+$ tends to increase along with the abundance of SiO in sources for which we could determine abundances. We discuss these results with respect to current theories ...

  11. Kinematics of gas and stars in circumnuclear star-forming regions of early type spirals

    CERN Document Server

    Hagele, Guillermo F; Cardaci, Monica V; Terlevich, Elena; Terlevich, Roberto

    2008-01-01

    (Abbr.) We present high resolution (R~20000) spectra in the blue and the far red of cicumnuclear star-forming regions (CNSFRs) in three early type spirals (NGC3351, NGC2903 and NGC3310) which have allowed the study of the kinematics of stars and ionized gas in these structures and, for the first time, the derivation of their dynamical masses for the first two. In some cases these regions, about 100 to 150 pc in size, are seen to be composed of several individual star clusters with sizes between 1.5 and 4.9 pc estimated from Hubble Space Telescope (HST) images. The stellar dispersions have been obtained from the Calcium triplet (CaT) lines at $\\lambda\\lambda$ 8494,8542,8662 \\AA, while the gas velocity dispersions have been measured by Gaussian fits to the H$\\beta$ and [OIII] $\\lambda\\lambda$ 5007 \\AA lines on the high dispersion spectra. Values of the stellar velocity dispersions are between 30 and 68 km/s. We apply the virial theorem to estimate dynamical masses of the clusters, assuming that systems are grav...

  12. Properties of the ionized gas of circumnuclear star-forming regions in early type spirals

    CERN Document Server

    Diaz, Angeles I; Terlevich, Elena; Terlevich, Roberto

    2008-01-01

    (Abbr.) A study of cicumnuclear star-forming regions (CNSFRs) in several early type spirals has been made in order to investigate their main properties: stellar and gas kinematics, dynamical masses, ionising stellar masses, chemical abundances and other properties of the ionised gas. Both high resolution (R$ \\sim $20000) and moderate resolution (R ~ 5000) have been used. In some cases these regions, about 100 to 150 pc in size, are seen to be composed of several individual star clusters with sizes between 1.5 and 4.9 pc estimated from Hubble Space Telescope (HST) images. Stellar and gas velocity dispersions are found to differ by about 20 to 30 km/s with the H$\\beta$ emission lines being narrower than both the stellar lines and the [OIII] $\\lambda$ 5007 \\AA lines. The twice ionized oxygen, on the other hand, shows velocity dispersions comparable to those shown by stars. We have applied the virial theorem to estimate dynamical masses of the clusters, assuming that systems are gravitationally bounded and spheri...

  13. Cannibalization and Rebirth in the NGC5387 System. I. The Stellar Stream & Star Forming Region

    CERN Document Server

    Beaton, Rachael L; D'Onghia, Elena; Zibetti, Stefano; Gabany, R Jay; Johnson, Kelsey E; Majewski, Steven R; Blanton, Michael; Verbiscer, Anne

    2013-01-01

    We have identified a low surface brightness stellar stream from visual inspection of SDSS imaging for the edge-on, spiral galaxy NGC5387. A blue overdensity was also identified in SDSS coincident with the stream intersection with the NGC5387 disk. The overdensity was also detected in the GALEX Deep Imaging Survey and found to contribute 38% of the total FUV integrated flux from NGC5387, which suggests that the region is actively forming stars. Deeper imaging was acquired with the Vatican Advanced Technology Telescope (VATT) in the B, V, and R filters that confirmed the presence of both the stellar stream and the blue overdensity. Analysis of the VATT photometry indicates the stellar stream is red in color, B-V = 0.7, and has a stellar mass of 6x10^8 M$_{\\odot}$, which implies a merger ratio of 1:50. Assessment of the stream morphology suggests that the merger event has a circular radius, R~16 kpc, the stream formed in ~400 Myr, and the progenitor had a total mass of ~2x10 M$_{\\odot}$. Spectroscopy from LBT+MO...

  14. The formation of ethylene glycol and other complex organic molecules in star-forming regions

    CERN Document Server

    Rivilla, V M; Cesaroni, R; Fontani, F; Codella, C; Zhang, Q

    2016-01-01

    We study the molecular abundance and spatial distribution of the simplest sugar alcohol, ethylene glycol (EG), the simplest sugar glycoladehyde (GA), and other chemically related complex organic species towards the massive star-forming region G31.41+0.31. We have analyzed multiple single dish and interferometric data, and obtained excitation temperatures and column densities using an LTE analysis. We have reported for the first time the presence of EG towards G31.41+0.31, and we have also detected multiple transitions of other complex organic molecules such as GA, methyl formate (MF), dimethyl ether (DME) and ethanol (ET). The high angular resolution images show that the EG emission is very compact, peaking towards the maximum of the continuum. These observations suggest that low abundance complex organic molecules, like EG or GA, are good probes of the gas located closer to the forming stars. Our analysis confirms that EG is more abundant than GA in G31.41+0.31, as previously observed in other interstellar r...

  15. Circumnuclear star-forming regions in early type spiral galaxies: dynamical masses

    CERN Document Server

    Hagele, G F; Bosch, G L; Diaz, A I; Terlevich, E; Terlevich, R

    2012-01-01

    We present the measurements of gas and stellar velocity dispersions in 17 circumnuclear star-forming regions (CNSFRs) and the nuclei of three barred spiral galaxies: NGC2903, NGC3310 and NGC3351 from high dispersion spectra. The stellar dispersions have been obtained from the CaII triplet (CaT) lines at 8494, 8542, 8662A, while the gas velocity dispersions have been measured by Gaussian fits to the Hbeta and to the [OIII]5007A\\ lines. The CNSFRs, with sizes of about 100 to 150pc in diameter, are seen to be composed of several individual star clusters with sizes between 1.5 and 6.2pc on HST images. Using the stellar velocity dispersions, we have derived dynamical masses for the entire star-forming complexes and for the individual star clusters. Values of the stellar velocity dispersions are between 31 and 73 km/s. Dynamical masses for the whole CNSFRs are between 4.9x10^6 and 1.9x10^8 Mo and between 1.4x10^6 and 1.1x10^7 Mo for the individual star clusters. We have found indications for the presence of two dif...

  16. Evolution and excitation conditions of outflows in high-mass star-forming regions

    CERN Document Server

    Sanchez-Monge, A; Cesaroni, R; Walmsley, C M; Codella, C; Beltran, M T; Pestalozzi, M; Molinari, S

    2013-01-01

    Theoretical models suggest that massive stars form via disk-mediated accretion, with bipolar outflows playing a fundamental role. A recent study toward massive molecular outflows has revealed a decrease of the SiO line intensity as the object evolves. The present study aims at characterizing the variation of the molecular outflow properties with time, and at studying the SiO excitation conditions in outflows associated with massive YSOs. We used the IRAM30m telescope to map 14 massive star-forming regions in the SiO(2-1), SiO(5-4) and HCO+(1-0) outflow lines, and in several dense gas and hot core tracers. Hi-GAL data was used to improve the spectral energy distributions and the L/M ratio, which is believed to be a good indicator of the evolutionary stage of the YSO. We detect SiO and HCO+ outflow emission in all the sources, and bipolar structures in six of them. The outflow parameters are similar to those found toward other massive YSOs. We find an increase of the HCO+ outflow energetics as the object evolve...

  17. Chemical segregation toward massive hot cores: The AFGL2591 star forming region

    CERN Document Server

    Jimenez-Serra, I; Viti, S; Martin-Pintado, J; de Wit, W -J

    2012-01-01

    We present high angular resolution observations (0.5"x0.3") carried out with the Submillimeter Array (SMA) toward the AFGL2591 high-mass star forming region. Our SMA images reveal a clear chemical segregation within the AFGL2591 VLA 3 hot core, where different molecular species (Type I, II and III) appear distributed in three concentric shells. This is the first time that such a chemical segregation is ever reported at linear scales <3000 AU within a hot core. While Type I species (H2S and 13CS) peak at the AFGL2591 VLA 3 protostar, Type II molecules (HC3N, OCS, SO and SO2) show a double-peaked structure circumventing the continuum peak. Type III species, represented by CH3OH, form a ring-like structure surrounding the continuum emission. The excitation temperatures of SO2, HC3N and CH3OH (185+-11 K, 150+-20 K and 124+-12 K, respectively) show a temperature gradient within the AFGL2591 VLA 3 envelope, consistent with previous observations and modeling of the source. By combining the H2S, SO2 and CH3OH imag...

  18. Sejong Open Cluster Survey (SOS) - V. The Active Star Forming Region SH 2-255-257

    Science.gov (United States)

    Lim, Beomdu; Sung, Hwankyung; Hur, Hyeonoh; Lee, Byeong-Cheol; Bessell, Michael S.; Kim, Jinyoung S.; Lee, Kang Hwan; Park, Byeong-Gon; Jeong, Gwanghui

    2015-12-01

    There is much observational evidence that active star formation is taking place in the H II regions Sh 2-255-257. We present a photometric study of this star forming region (SFR) using imaging data obtained in passbands from the optical to the mid-infrared, in order to study the star formation process. A total of 218 members were identified using various selection criteria based on their observational properties. The SFR is reddened by at least E(B-V) = 0.8 mag, and the reddening law toward the region is normal (R_V = 3.1). From the zero-age main sequence fitting method it is confirmed that the SFR is 2.1 ± 0.3 kpc from the Sun. The median age of the identified members is estimated to be about 1.3 Myr from a comparison of the Hertzsprung-Russell diagram (HRD) with stellar evolutionary models. The initial mass function (IMF) is derived from the HRD and the near-infrared (J, J-H) color-magnitude diagram. The slope of the IMF is about Γ = -1.6 ± 0.1, which is slightly steeper than that of the Salpeter/Kroupa IMF. It implies that low-mass star formation is dominant in the SFR. The sum of the masses of all the identified members provides the lower limit of the cluster mass (169 M_{⊙}). We also analyzed the spectral energy distribution (SED) of pre-main sequence stars using the SED fitting tool of Robitaille et al., and confirm that there is a significant discrepancy between stellar mass and age obtained from two different methods based on the SED fitting tool and the HRD.

  19. B- and A-Type Stars in the Taurus-Auriga Star-Forming Region

    Science.gov (United States)

    Mooley, Kunal; Hillenbrand, Lynne; Rebull, Luisa; Padgett, Deborah; Knapp, Gillian

    2013-01-01

    We describe the results of a search for early-type stars associated with the Taurus-Auriga molecular cloud complex, a diffuse nearby star-forming region noted as lacking young stars of intermediate and high mass. We investigate several sets of possible O, B, and early A spectral class members. The first is a group of stars for which mid-infrared images show bright nebulae, all of which can be associated with stars of spectral-type B. The second group consists of early-type stars compiled from (1) literature listings in SIMBAD, (2) B stars with infrared excesses selected from the Spitzer Space Telescope survey of the Taurus cloud, (3) magnitude- and color-selected point sources from the Two Micron All Sky Survey, and (4) spectroscopically identified early-type stars from the Sloan Digital Sky Survey coverage of the Taurus region. We evaluated stars for membership in the Taurus-Auriga star formation region based on criteria involving: spectroscopic and parallactic distances, proper motions and radial velocities, and infrared excesses or line emission indicative of stellar youth. For selected objects, we also model the scattered and emitted radiation from reflection nebulosity and compare the results with the observed spectral energy distributions to further test the plausibility of physical association of the B stars with the Taurus cloud. This investigation newly identifies as probable Taurus members three B-type stars: HR 1445 (HD 28929), t Tau (HD 29763), 72 Tau (HD 28149), and two A-type stars: HD 31305 and HD 26212, thus doubling the number of stars A5 or earlier associated with the Taurus clouds. Several additional early-type sources including HD 29659 and HD 283815 meet some, but not all, of the membership criteria and therefore are plausible, though not secure, members.

  20. Escape of ionizing radiation from star-forming regions in Young galaxies

    DEFF Research Database (Denmark)

    Razoumov, A; Sommer-Larsen, Jesper

    2006-01-01

    Galaxies: Formation, Galaxies: Intergalactic Medium, ISM: H II Regions, Radiative Transfer Udgivelsesdato: Nov. 10......Galaxies: Formation, Galaxies: Intergalactic Medium, ISM: H II Regions, Radiative Transfer Udgivelsesdato: Nov. 10...

  1. A search for companions to brown dwarfs in the Taurus and Chamaeleon star-forming regions

    Energy Technology Data Exchange (ETDEWEB)

    Todorov, K. O.; Luhman, K. L. [Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802 (United States); Konopacky, Q. M. [Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94550 (United States); McLeod, K. K. [Whitin Observatory, Wellesley College, Wellesley, MA 02481 (United States); Apai, D.; Pascucci, I. [Department of Astronomy, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721 (United States); Ghez, A. M. [Division of Astronomy and Astrophysics, University of California, Los Angeles, CA 90095 (United States); Robberto, M., E-mail: todorovk@phys.ethz.ch [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)

    2014-06-10

    We have used WFPC2 on board the Hubble Space Telescope to obtain images of 47 members of the Taurus and Chamaeleon I star-forming regions that have spectral types of M6-L0 (M ∼ 0.01-0.1 M {sub ☉}). An additional late-type member of Taurus, FU Tau (M7.25+M9.25), was also observed with adaptive optics at Keck Observatory. In these images, we have identified promising candidate companions to 2MASS J04414489+2301513 (ρ = 0.''105/15 AU), 2MASS J04221332+1934392 (ρ = 0.''05/7 AU), and ISO 217 (ρ = 0.''03/5 AU). We reported the first candidate in a previous study, showing that it has a similar proper motion as the primary in images from WFPC2 and Gemini adaptive optics. We have collected an additional epoch of data with Gemini that further supports that result. By combining our survey with previous high-resolution imaging in Taurus, Chamaeleon I, and Upper Sco (τ ∼ 10 Myr), we measure binary fractions of 14/93 = 0.15{sub −0.03}{sup +0.05} for M4-M6 (M ∼ 0.1-0.3 M {sub ☉}) and 4/108 = 0.04{sub −0.01}{sup +0.03} for >M6 (M ≲ 0.1 M {sub ☉}) at separations of >10 AU. Given the youth and low density of these regions, the lower binary fraction at later types is probably primordial rather than due to dynamical interactions among association members. The widest low-mass binaries (>100 AU) also appear to be more common in Taurus and Chamaeleon I than in the field, which suggests that the widest low-mass binaries are disrupted by dynamical interactions at >10 Myr, or that field brown dwarfs have been born predominantly in denser clusters where wide systems are disrupted or inhibited from forming.

  2. HIGH-VELOCITY LINE FORMING REGIONS IN THE TYPE Ia SUPERNOVA 2009ig

    Energy Technology Data Exchange (ETDEWEB)

    Marion, G. H.; Foley, Ryan J.; Challis, Peter; Kirshner, Robert P. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Vinko, Jozsef; Wheeler, J. Craig; Silverman, Jeffrey M. [University of Texas at Austin, 1 University Station C1400, Austin, TX 78712-0259 (United States); Hsiao, Eric Y. [Carnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601 (Chile); Brown, Peter J. [George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A and M University, 4242 AMU, College Station, TX 77843 (United States); Filippenko, Alexei V. [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States); Garnavich, Peter [Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556 (United States); Landsman, Wayne B. [Adnet Systems, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Parrent, Jerod T. [Las Cumbres Observatory Global Telescope Network, Goleta, CA 93117 (United States); Pritchard, Tyler A.; Roming, Peter W. A. [Department of Astronomy and Astrophysics, Penn State University, 525 Davey Lab, University Park, PA 16802 (United States); Wang, Xiaofeng, E-mail: gmarion@cfa.harvard.edu [Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 1,00084 (China)

    2013-11-01

    We report measurements and analysis of high-velocity (HVF) (>20,000 km s{sup –1}) and photospheric absorption features in a series of spectra of the Type Ia supernova (SN) 2009ig obtained between –14 days and +13 days with respect to the time of maximum B-band luminosity (B-max). We identify lines of Si II, Si III, S II, Ca II, and Fe II that produce both HVF and photospheric-velocity (PVF) absorption features. SN 2009ig is unusual for the large number of lines with detectable HVF in the spectra, but the light-curve parameters correspond to a slightly overluminous but unexceptional SN Ia (M{sub B} = –19.46 mag and Δm{sub 15}(B) = 0.90 mag). Similarly, the Si II λ6355 velocity at the time of B-max is greater than 'normal' for an SN Ia, but it is not extreme (v{sub Si} = 13,400 km s{sup –1}). The –14 days and –13 days spectra clearly resolve HVF from Si II λ6355 as separate absorptions from a detached line forming region. At these very early phases, detached HVF are prevalent in all lines. From –12 days to –6 days, HVF and PVF are detected simultaneously, and the two line forming regions maintain a constant separation of about 8000 km s{sup –1}. After –6 days all absorption features are PVF. The observations of SN 2009ig provide a complete picture of the transition from HVF to PVF. Most SNe Ia show evidence for HVF from multiple lines in spectra obtained before –10 days, and we compare the spectra of SN 2009ig to observations of other SNe. We show that each of the unusual line profiles for Si II λ6355 found in early-time spectra of SNe Ia correlate to a specific phase in a common development sequence from HVF to PVF.

  3. Molecular Gas and Dust in the Massive Star Forming Region S 233 IR

    Institute of Scientific and Technical Information of China (English)

    Rui-Qing Mao; Qin Zeng

    2004-01-01

    The massive star forming region S 233 IR is observed in the molecular lines CO J = 2-1, 3-2, NH3 (1,1), (2,2) and the 870μm dust continuum. Four submillimeter continuum sources, labelled SMM 1-4, are revealed in the 870μm dust emission. The main core, SMM1, is found to be associated with a deeply embedded near infrared cluster in the northeast; while the weaker source SMM2 coincides with a more evolved cluster in the southwest. The best fit spectral energy distribution of SMM1 gives an emissivity ofβ = 1.6, and temperatures of 32 K and 92 K for the cold- and hot-dust components. An SMM1 core mass of 246 M⊙ and a total mass of 445 M⊙ are estimated from the 870 μm dust continuum emission.SMM1 is found to have a temperature gradient decreasing from inside out, indicative of the presence of interior heating sources. The total outflow gas mass as traced by the CO J - 3-2 emission is estimated to be 35 M⊙. Low velocity outflows are also found in the NH3 (1,1) emission. The non-thermal dominant NH3 line width as well as the substantial core mass suggest that the SMM1 core is a "turbulent,massive dense core", in the process of forming a group or a cluster of stars. The much higher star formation efficiency found in the southwest cluster supports the suggestion that this cluster is more evolved than the northeast one. Large near infrared photometric variations found in the source PCS-IR93, a previously found highly polarized nebulosity, indicate an underlying star showing the FU Orionis type of behavior.

  4. Trigonometric parallaxes to star-forming regions within 4 kpc of the galactic center

    Energy Technology Data Exchange (ETDEWEB)

    Sanna, A.; Menten, K. M.; Zhang, B.; Sato, M.; Brunthaler, A.; Immer, K. [Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn (Germany); Reid, M. J.; Dame, T. M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Moscadelli, L., E-mail: asanna@mpifr-bonn.mpg.de [INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze (Italy)

    2014-02-01

    We report four trigonometric parallaxes for high-mass star-forming regions within 4 kpc of the Galactic center. These measurements were made with the Very Long Baseline Array as part of the BeSSeL Survey. By associating these sources kinematically with large-scale features in CO and H I longitude-velocity diagrams, we begin to outline some major features of the inner Milky Way: the Connecting arm, the near and far 3 kpc arms, and the Norma arm. The Connecting arm in the first Galactic quadrant lies closer to the Galactic center than the far 3 kpc arm and is offset by the long-bar's major axis near its leading edge, supporting the presence of an inner Lindblad resonance. Assuming the 3 kpc arms are a continuous physical structure, the relative Galactocentric distance of its near and far sides suggests highly elliptical streamlines of gas around the bar(s) and a bar corotation radius, r {sub CR} ≳ 3.6 kpc. At a Galactic longitude near 10° and a heliocentric distance of about 5 kpc, the near 3 kpc arm and the Norma arm intersect on a face-on view of our Galaxy, while passing at different Galactic latitudes. We provide an accurate distance measurement to the W 31 star-forming complex of 4.95{sub −0.43}{sup +0.51} kpc from the Sun, which associates it with a bright CO feature belonging to the near 3 kpc arm.

  5. Trigonometric parallaxes of high mass star forming regions: the structure and kinematics of the Milky Way

    Energy Technology Data Exchange (ETDEWEB)

    Reid, M. J.; Dame, T. M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Menten, K. M.; Brunthaler, A.; Wu, Y.; Zhang, B.; Sanna, A.; Sato, M.; Choi, Y. K.; Immer, K. [Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn (Germany); Zheng, X. W. [Department of Astronomy, Nanjing University Nanjing 210093 (China); Xu, Y. [Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China); Hachisuka, K. [Shanghai Astronomical Observatory, 80 Nandan Rd., Shanghai (China); Moscadelli, L. [Arcetri Observatory, Firenze (Italy); Rygl, K. L. J. [European Space Agency (ESA-ESTEC), Keplerlaan 1, P.O. Box 299, 2200 AG, Noordwijk (Netherlands); Bartkiewicz, A. [Centre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun (Poland)

    2014-03-10

    Over 100 trigonometric parallaxes and proper motions for masers associated with young, high-mass stars have been measured with the Bar and Spiral Structure Legacy Survey, a Very Long Baseline Array key science project, the European VLBI Network, and the Japanese VLBI Exploration of Radio Astrometry project. These measurements provide strong evidence for the existence of spiral arms in the Milky Way, accurately locating many arm segments and yielding spiral pitch angles ranging from about 7° to 20°. The widths of spiral arms increase with distance from the Galactic center. Fitting axially symmetric models of the Milky Way with the three-dimensional position and velocity information and conservative priors for the solar and average source peculiar motions, we estimate the distance to the Galactic center, R {sub 0}, to be 8.34 ± 0.16 kpc, a circular rotation speed at the Sun, Θ{sub 0}, to be 240 ± 8 km s{sup –1}, and a rotation curve that is nearly flat (i.e., a slope of –0.2 ± 0.4 km s{sup –1} kpc{sup –1}) between Galactocentric radii of ≈5 and 16 kpc. Assuming a 'universal' spiral galaxy form for the rotation curve, we estimate the thin disk scale length to be 2.44 ± 0.16 kpc. With this large data set, the parameters R {sub 0} and Θ{sub 0} are no longer highly correlated and are relatively insensitive to different forms of the rotation curve. If one adopts a theoretically motivated prior that high-mass star forming regions are in nearly circular Galactic orbits, we estimate a global solar motion component in the direction of Galactic rotation, V {sub ☉} = 14.6 ± 5.0 km s{sup –1}. While Θ{sub 0} and V {sub ☉} are significantly correlated, the sum of these parameters is well constrained, Θ{sub 0} + V {sub ☉} = 255.2 ± 5.1 km s{sup –1}, as is the angular speed of the Sun in its orbit about the Galactic center, (Θ{sub 0} + V {sub ☉})/R {sub 0} = 30.57 ± 0.43 km s{sup –1} kpc{sup –1}. These parameters improve the accuracy

  6. An HST Imaging Survey of Low-Mass Stars in the Chamaeleon I Star Forming region

    CERN Document Server

    Robberto, M; Da Rio, N; Apai, D; Pascucci, I; Ricci, L; Goddi, C; Testi, L; Palla, F; Bacciotti, F

    2012-01-01

    We present new HST/WFPC2 observations of 20 fields centered around T Tauri stars in the Chamaeleon I star forming region. Images have been obtained in the F631N ([OI]6300A), F656N (Ha) and F673N ([SII]6716A+6731A) narrow-band filters, plus the Johnson V-band equivalent F547M filter. We detect 31 T Tauri stars falling within our fields. We discuss the optical morphology of 10 sources showing evidence of either binarity, circumstellar material, or mass loss. We supplement our photometry with a compilation of optical, infrared and sub-millimeter data from the literature, together with new sub-mm data for three objects, to build the Spectral Energy Distributions (SED) of 19 single sources. Using an SED model fitting tool, we self-consistently estimate a number of stellar and disk parameters, while mass accretion rates are directly derived from our Ha photometry. We find that bolometric luminosities derived from dereddened optical data tend to be underestimated in systems with high alpha(2-24} IR spectral index, s...

  7. H i-to-H2 Transition Layers in the Star-forming Region W43

    Science.gov (United States)

    Bialy, Shmuel; Bihr, Simon; Beuther, Henrik; Henning, Thomas; Sternberg, Amiel

    2017-02-01

    The process of atomic-to-molecular (H i-to-H2) gas conversion is fundamental for molecular-cloud formation and star formation. 21 cm observations of the star-forming region W43 revealed extremely high H i column densities, of 120–180 {M}ȯ {{pc}}-2, a factor of 10–20 larger than predicted by H i-to-H2 transition theories. We analyze the observed H i with a theoretical model of the H i-to-H2 transition, and show that the discrepancy between theory and observation cannot be explained by the intense radiation in W43, nor be explained by variations of the assumed volume density or H2 formation rate coefficient. We show that the large observed H i columns are naturally explained by several (9–22) H i-to-H2 transition layers, superimposed along the sightlines of W43. We discuss other possible interpretations such as a non-steady-state scenario and inefficient dust absorption. The case of W43 suggests that H i thresholds reported in extragalactic observations are probably not associated with a single H i-to-H2 transition, but are rather a result of several transition layers (clouds) along the sightlines, beam-diluted with diffuse intercloud gas.

  8. The very low-mass population of the Corona Australis and Chamaeleon II star forming regions

    CERN Document Server

    Martí-Bonmatí, L; Mundt, R; Mart\\'{\\i}, Bel\\'en L\\'opez; Eisl\\"offel, Jochen; Mundt, Reinhard

    2005-01-01

    We present the results of a deep optical survey in the Corona Australis and Chamaeleon II star forming regions. Our optical photometry is combined with available near- and mid-infrared photometry to identify very low-mass candidate members in these dark clouds. In our Chamaeleon II field, only one object exhibits clear H-alpha emission, but the discrepancy between its optical and near-infrared colours suggests that it might be a foreground star. We also identify two objects without H-alpha emission that could be planetary mass members of Chamaeleon II. In Corona Australis, we find ten stars and three brown dwarf candidates in the Coronet cluster. Five of our new members are identified with ISOCAM sources. Only two of them have a mid-infrared excess, indicating the presence of an accretion disk. On the other hand, one brown dwarf candidate has a faint close companion, seen only in our deepest I-band image. For many of the candidates in both clouds, membership could not be inferred from their H-alpha emission o...

  9. Extremely-bright submillimeter galaxies beyond the Lupus-I star-forming region

    CERN Document Server

    Tamura, Y; Shimajiri, Y; Tsukagoshi, T; Nakajima, Y; Oasa, Y; Wilner, D J; Chandler, C J; Saigo, K; Tomida, K; Yun, M S; Taniguchi, A; Kohno, K; Hatsukade, B; Aretxaga, I; Austermann, J E; Dickman, R; Ezawa, H; Goss, W M; Hayashi, M; Hughes, D H; Hiramatsu, M; Inutsuka, S; Ogasawara, R; Ohashi, N; Oshima, T; Scott, K S; Wilson, G W

    2015-01-01

    We report detections of two candidate distant submillimeter galaxies (SMGs), MM J154506.4$-$344318 and MM J154132.7$-$350320, which are discovered in the AzTEC/ASTE 1.1 mm survey toward the Lupus-I star-forming region. The two objects have 1.1 mm flux densities of 43.9 and 27.1 mJy, and have Herschel/SPIRE counterparts as well. The Submillimeter Array counterpart to the former SMG is identified at 890 $\\mu$m and 1.3 mm. Photometric redshift estimates using all available data from the mid-infrared to the radio suggest that the redshifts of the two SMGs are $z_{\\rm photo} \\simeq$ 4-5 and 3, respectively. Near-infrared objects are found very close to the SMGs and they are consistent with low-$z$ ellipticals, suggesting that the high apparent luminosities can be attributed to gravitational magnification. The cumulative number counts at $S_{\\rm 1.1mm} \\ge 25$ mJy, combined with other two 1.1-mm brightest sources, are $0.70 ^{+0.56}_{-0.34}$ deg$^{-2}$, which is consistent with a model prediction that accounts for ...

  10. Probing dynamical processes in the planet forming region with dust mineralogy

    CERN Document Server

    McClure, M K; Calvet, N; Adame, L; Espaillat, C; Watson, D M; Sargent, B; Forrest, W J; D'Alessio, P

    2012-01-01

    We present Herschel Space Observatory PACS spectra of GQ Lup, a protoplanetary disk in the Lupus star-forming region. Through SED fitting from 0.3{\\mu}m to 1.3mm, we construct a self-consistent model of this system's temperature and density structures, finding that although it is 3 Myr old, its dust has not settled to the midplane substantially. The disk has a radial gradient in both the silicate dust composition and grain size, with large amorphous grains in the upper layers of the inner disk and an enhancement of submicron, crystalline grains in the outer disk. We detect an excess of emission in the Herschel PACS B2A band near 63{\\mu}m and model it with a combination of {\\sim}15 to 70{\\mu}m crystalline water ice grains with a size distribution consistent with ice recondensation-enhanced grain growth and a mass fraction half of that of our solar system. The combination of crystalline water ice and silicates in the outer disk is suggestive of disk-wide heating events or planetesimal collisions. If confirmed, ...

  11. The Stellar Mass Distribution in the Giant Star Forming Region NGC 346

    CERN Document Server

    Sabbi, E; Nota, A; Tosi, M; Gallagher, J; Smith, L J; Angeretti, L; Meixner, M; Oey, M S; Walterbos, R; Pasquali, A

    2007-01-01

    Deep F555W and F814W Hubble Space Telescope ACS images are the basis for a study of the present day mass function (PDMF) of NGC346, the largest active star forming region in the Small Magellanic Cloud (SMC). We find a PDMF slope of Gamma=-1.43+/-0.18 in the mass range 0.8-60 Mo, in excellent agreement with the Salpeter Initial Mass Function (IMF) in the solar neighborhood. Caveats on the conversion of the PDMF to the IMF are discussed. The PDMF slope changes, as a function of the radial distance from the center of the NGC 346 star cluster, indicating a segregation of the most massive stars. This segregation is likely primordial considering the young age (~3 Myr) of NGC346, and its clumpy structure which suggests that the cluster has likely not had sufficient time to relax. Comparing our results for NGC346 with those derived for other star clusters in the SMC and the Milky Way (MW), we conclude that, while the star formation process might depend on the local cloud conditions, the IMF does not seem to be affect...

  12. YSOVAR: Mid-IR variability in the star forming region Lynds 1688

    CERN Document Server

    Günther, H M; Covey, K R; Hillenbrand, L A; Plavchan, P; Poppenhaeger, K; Rebull, L M; Stauffer, J R; Wolk, S J; Allen, L; Bayo, A; Gutermuth, R A; Hora, J L; Meng, H Y A; Morales-Calderon, M; Parks, J R; Song, Inseok

    2014-01-01

    The emission from young stellar objects (YSOs) in the mid-IR is dominated by the inner rim of their circumstellar disks. We present an IR-monitoring survey of about 800 objects in the direction of the Lynds 1688 (L1688) star forming region over four visibility windows spanning 1.6 years using the \\emph{Spitzer} space telescope in its warm mission phase. Among all lightcurves, 57 sources are cluster members identified based on their spectral-energy distribution and X-ray emission. Almost all cluster members show significant variability. The amplitude of the variability is larger in more embedded YSOs. Ten out of 57 cluster members have periodic variations in the lightcurves with periods typically between three and seven days, but even for those sources, significant variability in addition to the periodic signal can be seen. No period is stable over 1.6 years. Non-periodic lightcurves often still show a preferred timescale of variability which is longer for more embedded sources. About half of all sources exhib...

  13. Weak and Compact Radio Emission in Early High-Mass Star Forming Regions: I. VLA Observations

    CERN Document Server

    Rosero, V; Claussen, M; Kurtz, S; Cesaroni, R; Araya, E D; Carrasco-González, C; Rodríguez, L F; Menten, K M; Wyrowski, F; Loinard, L; Ellingsen, S P

    2016-01-01

    We present a high sensitivity radio continuum survey at 6 and 1.3$\\,$cm using the Karl G. Jansky Very Large Array towards a sample of 58 high-mass star forming regions. Our sample was chosen from dust clumps within infrared dark clouds with and without IR sources (CMC-IRs, CMCs, respectively), and hot molecular cores (HMCs), with no previous, or relatively weak radio continuum detection at the $1\\,$mJy level. Due to the improvement in the continuum sensitivity of the VLA, this survey achieved map rms levels of $\\sim$ 3-10 $\\mu$Jy beam$^{-1}$ at sub-arcsecond angular resolution. We extracted 70 centimeter continuum sources associated with 1.2$\\,$mm dust clumps. Most sources are weak, compact, and are prime candidates for high-mass protostars. Detection rates of radio sources associated with the mm dust clumps for CMCs, CMC-IRs and HMCs are 6$\\%$, 53$\\%$ and 100$\\%$, respectively. This result is consistent with increasing high-mass star formation activity from CMCs to HMCs. The radio sources located within HMCs...

  14. Phosphorus-bearing molecules in solar-type star forming regions: First PO detection

    CERN Document Server

    Lefloch, B; Viti, S; Jimenez-Serra, I; Codella, C; Podio, L; Ceccarelli, C; Mendoza, E; Lepine, J R D; Bachiller, R

    2016-01-01

    As part of the Large Program ASAI (Astrochemical Surveys At IRAM), we have used the IRAM 30m telescope to lead a systematic search for the emission of rotational transitions of P-bearing species between 80 and 350 GHz towards L1157-B1, a shock position in the solar-type star forming region L1157. We report the detection of several transitions of PN and, for the first time, of prebiotic molecule PO. None of these species are detected towards the driving protostar of the outflow L1157-mm. Analysis of the line profiles shows that PN arises from the outflow cavity, where SiO, a strong shock tracer, is produced. Radiative transfer analysis yields an abundance of 2.5e-9 and 0.9e-9 for PO and PN, respectively. These results imply a strong depletion (approx 100) of Phosphorus in the quiescent cloud gas. Shock modelling shows that atomic N plays a major role in the chemistry of PO and PN. The relative abundance of PO and PN brings constraints both on the duration of the pre-shock phase, which has to be about 1 Myr, an...

  15. Extreme Infrared Variables from UKIDSS - I. A Concentration in Star Forming Regions

    CERN Document Server

    Peña, C Contreras; Froebrich, D; Kumar, M S N; Goldstein, J; Drew, J E; Adamson, A; Davis, C J; Barentsen, G; Wright, N J

    2014-01-01

    We present initial results of the first panoramic search for high-amplitude near-infrared variability in the Galactic Plane. We analyse the widely separated two-epoch K-band photometry in the 5th and 7th data releases of the UKIDSS Galactic Plane Survey. We find 45 stars with \\Delta K > 1 mag, including 2 previously known OH/IR stars and a Nova. Even though the mid-plane is not yet included in the dataset, we find the majority (66%) of our sample to be within known star forming regions (SFRs), with two large concentrations in the Serpens OB2 association (11 stars) and the Cygnus-X complex (12 stars). Sources in SFRs show spectral energy distributions (SEDs) that support classification as Young Stellar Objects (YSOs). This indicates that YSOs dominate the Galactic population of high amplitude infrared variable stars at low luminosities and therefore likely dominate the total high amplitude population. Spectroscopic follow up of the DR5 sample shows at least four stars with clear characteristics of eruptive pre...

  16. Water maser kinematics in massive star-forming regions: Cepheus A and W75N

    CERN Document Server

    Torrelles, J M; Curiel, S; Gómez, J F; Anglada, G; Estalella, R

    2012-01-01

    VLBI multi-epoch water maser observations are a powerful tool to study the dense, warm shocked gas very close to massive protostars. The very high-angular resolution of these observations allow us to measure the proper motions of the masers in a few weeks, and together with the radial velocity, to determine their full kinematics. In this paper we present a summary of the main observational results obtained toward the massive star-forming regions of Cepheus A and W75N, among them: (i) the identification of different centers of high-mass star formation activity at scales of 100 AU; (ii) the discovery of new phenomena associated with the early stages of high-mass protostellar evolution (e.g., isotropic gas ejections); and (iii) the identification of the simultaneous presence of a wide-angle outflow and a highly collimated jet in the massive object Cep A HW2, similar to what is observed in some low-mass protostars. Some of the implications of these results in the study of high-mass star formation are discussed.

  17. YSOVAR: Mid-infrared variability in the star-forming region Lynds 1688

    Energy Technology Data Exchange (ETDEWEB)

    Günther, H. M.; Poppenhaeger, K.; Wolk, S. J.; Hora, J. L. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Cody, A. M. [Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125 (United States); Covey, K. R. [Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001 (United States); Hillenbrand, L. A. [Department of Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States); Plavchan, P. [NASA Exoplanet Science Institute, California Institute of Technology, 770 South Wilson Avenue, Pasadena, CA 91125 (United States); Rebull, L. M.; Stauffer, J. R. [Spitzer Science Center/Caltech, 1200 East California Boulevard, Pasadena, CA 91125 (United States); Allen, L. [National Optical Astronomy Observatories, Tucson, AZ 85719 (United States); Bayo, A. [Max Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg (Germany); Gutermuth, R. A. [Department of Astronomy, University of Massachusetts, Amherst, MA 01003 (United States); Meng, H. Y. A. [Infrared Processing and Analysis Center, California Institute of Technology, MC 100-22, 770 South Wilson Avenue, Pasadena, CA 91125 (United States); Morales-Calderón, M. [Centro de Astrobiología (INTA-CSIC), ESAC Campus, P.O. Box 78, E-28691 Villanueva de la Canada (Spain); Parks, J. R. [Department of Physics and Astronomy, Georgia State University, 25 Park Place South, Atlanta, GA 30303 (United States); Song, Inseok, E-mail: hguenther@cfa.harvard.edu [Physics and Astronomy Department, University of Georgia, Athens, GA 30602-2451 (United States)

    2014-12-01

    The emission from young stellar objects (YSOs) in the mid-infrared (mid-IR) is dominated by the inner rim of their circumstellar disks. We present IR data from the Young Stellar Object VARiability (YSOVAR) survey of ∼800 objects in the direction of the Lynds 1688 (L1688) star-forming region over four visibility windows spanning 1.6 yr using the Spitzer Space Telescope in its warm mission phase. Among all light curves, 57 sources are cluster members identified based on their spectral energy distribution and X-ray emission. Almost all cluster members show significant variability. The amplitude of the variability is larger in more embedded YSOs. Ten out of 57 cluster members have periodic variations in the light curves with periods typically between three and seven days, but even for those sources, significant variability in addition to the periodic signal can be seen. No period is stable over 1.6 yr. Nonperiodic light curves often still show a preferred timescale of variability that is longer for more embedded sources. About half of all sources exhibit redder colors in a fainter state. This is compatible with time-variable absorption toward the YSO. The other half becomes bluer when fainter. These colors can only be explained with significant changes in the structure of the inner disk. No relation between mid-IR variability and stellar effective temperature or X-ray spectrum is found.

  18. Trigonometric parallaxes to star-forming regions within 4 kpc of the galactic center

    CERN Document Server

    Sanna, A; Menten, K M; Dame, T M; Zhang, B; Sato, M; Brunthaler, A; Moscadelli, L; Immer, K

    2013-01-01

    We report four trigonometric parallaxes for high-mass star-forming regions within 4 kpc of the Galactic center. These measurements were made with the VLBA as part of the BeSSeL Survey. By associating these sources kinematically with large-scale features in CO and HI longitude-velocity diagrams, we begin to outline some major features of the inner Milky Way: the Connecting arm, the near and far 3 kpc arms, and the Norma arm. The Connecting arm in the first Galactic quadrant lies closer to the Galactic center than the far 3 kpc arm and is offset by the long-bar's major axis near its leading edge, supporting the presence of an inner Lindblad resonance. Assuming the 3 kpc arms are a continuous physical structure, the relative Galactocentric distance of its near and far sides suggests highly elliptical streamlines of gas around the bar(s) and a bar corotation radius, r_CR > 3.6 kpc. At a Galactic longitude near 10{\\deg} and a heliocentric distance of about 5 kpc, the near 3 kpc arm and the Norma arm intersect on a...

  19. Externally heated protostellar cores in the Ophiuchus star-forming region

    CERN Document Server

    Lindberg, Johan E; Jørgensen, Jes K; Cordiner, Martin A; Bjerkeli, Per

    2016-01-01

    We present APEX 218 GHz observations of molecular emission in a complete sample of embedded protostars in the Ophiuchus star-forming region. To study the physical properties of the cores, we calculate H$_2$CO and c-C$_3$H$_2$ rotational temperatures, both of which are good tracers of the kinetic temperature of the molecular gas. We find that the H$_2$CO temperatures range between 16 K and 124 K, with the highest H$_2$CO temperatures toward the hot corino source IRAS 16293-2422 (69-124 K) and the sources in the $\\rho$ Oph A cloud (23-49 K) located close to the luminous Herbig Be star S 1, which externally irradiates the $\\rho$ Oph A cores. On the other hand, the c-C$_3$H$_2$ rotational temperature is consistently low (7-17 K) in all sources. Our results indicate that the c-C$_3$H$_2$ emission is primarily tracing more shielded parts of the envelope whereas the H$_2$CO emission (at the angular scale of the APEX beam; 3600 au in Ophiuchus) mainly traces the outer irradiated envelopes, apart from in IRAS 16293-24...

  20. Spitzer Infrared Spectrograph survey of young stars in the Chamaeleon I star-forming region

    CERN Document Server

    Manoj, P; Furlan, E; McClure, M K; Luhman, K L; Watson, D M; Espaillat, C; Calvet, N; Najita, J R; D'Alessio, P; Adame, L; Sargent, B A; Forrest, W J; Bohac, C; Green, J D; Arnold, L A

    2011-01-01

    We present 5 to 36 micron mid-infrared spectra of 82 young stars in the ~2 Myr old Chamaeleon I star-forming region, obtained with the Spitzer Infrared Spectrograph (IRS). We have classified these objects into various evolutionary classes based on their spectral energy distributions and the spectral features seen in the IRS spectra. We have analyzed the mid-IR spectra of Class II objects in Chamaeleon I in detail, in order to study the vertical and radial structure of the protoplanetary disks surrounding these stars. We find evidence for substantial dust settling in most protoplanetary disks in Chamaeleon I. We have identified several disks with altered radial structures in Chamaeleon I, among them transitional disk candidates which have holes or gaps in their disks. Analysis of the silicate emission features in the IRS spectra of Class II objects in Chamaeleon I shows that the dust grains in these disks have undergone significant processing (grain growth and crystallization). However, disks with radial holes...

  1. CO observations of massive star forming regions at different evolutionary phases

    Institute of Scientific and Technical Information of China (English)

    CHEN; Xi; XU; Ye; SHEN; Zhiqiang; LI; Jingjing

    2006-01-01

    The 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) emissions in 9 massive star forming regions, which are believed to be at different stages of massive star formation,were mapped with the 13.7 m millimeter wave telescope at Qinghai Station of Purple Mountain Observatory. Of the observed 9 sources, 13CO cores were detected in seven of them, and C18O cores in five of them. And only two sources associated with C18O cores and H2O masers showed the extended structures and strong outflows. This is the first detection of outflow associated with IRAS 22566+5828 in the observing field of S152/S153.The physical parameters of cores and outflows for these sources, derived from Local Thermal Equilibrium (LTE) analysis, are presented. These observing results suggest that the C18O cores will only appear when the gas density is high enough and the probability to have an outflow is very high when the clumps show the C18O and H2O maser simultaneously.

  2. MULTIPLICITY, DISKS, AND JETS IN THE NGC 2071 STAR-FORMING REGION

    Energy Technology Data Exchange (ETDEWEB)

    Carrasco-Gonzalez, Carlos [Max-Planck-Institut fuer Radioastronomie (MPIfR), Auf dem Huegel 69, 53121 Bonn (Germany); Osorio, Mayra; Anglada, Guillem; Gomez, Jose F. [Instituto de Astrofisica de Andalucia, CSIC, Camino Bajo de Huetor 50, E-18008 Granada (Spain); D' Alessio, Paola; Rodriguez, Luis F. [Centro de Radioastronomia y Astrofisica UNAM, Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacan (Mexico); Torrelles, Jose M., E-mail: carrasco@mpifr-bonn.mpg.de [Instituto de Ciencias del Espacio (CSIC)-UB/IEEC, Universitat de Barcelona, Marti i Franques 1, E-08028 Barcelona (Spain)

    2012-02-10

    We present centimeter (cm) and millimeter (mm) observations of the NGC 2071 star-forming region performed with the Very Large Array (VLA) and Combined Array for Research in Millimeter-wave Astronomy (CARMA). We detected counterparts at 3.6 cm and 3 mm for the previously known sources IRS 1, IRS 2, IRS 3, and VLA 1. All these sources show spectral energy distributions (SEDs) dominated by free-free thermal emission at cm wavelengths and thermal dust emission at mm wavelengths, suggesting that all of them are associated with young stellar objects (YSOs). IRS 1 shows a complex morphology at 3.6 cm, with changes in the direction of its elongation. We discuss two possible explanations to this morphology: the result of changes in the direction of a jet due to interactions with a dense ambient medium, or that we are actually observing the superposition of two jets arising from two components of a binary system. Higher angular resolution observations at 1.3 cm support the second possibility, since a double source is inferred at this wavelength. IRS 3 shows a clear jet-like morphology at 3.6 cm. Over a timespan of four years, we observed changes in the morphology of this source that we interpret as due to ejection of ionized material in a jet. The emission at 3 mm of IRS 3 is angularly resolved, with a deconvolved size (FWHM) of {approx}120 AU, and seems to be tracing a dusty circumstellar disk perpendicular to the radio jet. An irradiated accretion disk model around an intermediate-mass YSO can account for the observed SED and spatial intensity profile at 3 mm, supporting this interpretation.

  3. Multi-wavelength, Multi-scale Observations of Outflows in Star-Forming Regions

    Science.gov (United States)

    Plunkett, Adele Laurie Dennis

    During the early stages of star formation, an embedded protostar accretes mass and simultaneously expels mass and angular momentum in the form of a bipolar outflow. In the common case of clustered star formation, outflows likely impact their surrounding environment and influence subsequent star formation. Numerical simulations have shown that outflows can sustain turbulence and maintain a cluster in quasi-equilibrium; alternatively, it was proposed that outflows may trigger rather than regulate or inhibit star formation. Observations of outflows and their impact on clusters are challenging because they must probe spatial scales over several orders of magnitude --- from the size of a core (a few hundred AU, or N ~ 10-3 pc) to a cluster (a few pc) --- and previous works generally focused on one scale or the other. This thesis incorporates high-resolution, high-sensitivity interferometry observations (with millimeter/sub-millimeter wavelengths) complemented by observations obtained using single dish telescopes in order to assess molecular outflow properties and their cumulative impact in two young protostellar clusters: Serpens South and NGC 1333. Based on these case studies, I develop an evolutionary scenario for clustered star formation spanning the ages of the two clusters, about 0.1 - 1 Myr. Within this scenario, outflows in both Serpens South and NGC 1333 provide sufficient energy to sustain turbulence early in the protocluster formation process. In neither cluster do outflows provide enough energy to counter the gravitational potential energy and disrupt the entire cluster. However, most of the mass in outflows in both clusters have velocities greater than the escape velocity, and therefore the relative importance of outflow-driven turbulence compared with gravitational potential likely changes with time as ambient gas escapes. We estimate that enough gas mass will escape via outflows in Serpens South so that it will come to resemble NGC 1333 in terms of its

  4. A Multi-line Study of Atomic Carbon and Carbon Monoxide in the Galactic Star- forming Region W3

    Science.gov (United States)

    Jakob, H.; Kramer, C.; Mookerjea, B.; Jeyakumar, S.; Stutzki, J.

    We present results from simultaneous observations of the fine structure line emissions of neutral carbon (C I) at 492 and 809 GHz from selected Galactic star forming regions. These observations include the first results using the the newly installed SMART (SubmilliMeter Array Receiver at Two wavelengths) on KOSMA. The regions observed were selected in order to cover a range of strengths of the incident UV radiation from the exciting star/stars and also densities of the interstellar medium. Extended maps of C I emission from massive star forming regions including W3, S106 and Orion BN/KL have been observed. Simultaneous observation of the two C I lines ensures better relative calibration. The results from these observations will be combined with observed intensities of low-J and mid-J CO and C+ lines and analyzed using radiation transfer based models for Photon Dominated Regions (PDRs).

  5. Analysis of nucleon electromagnetic form factors from light-front holographic QCD: The spacelike region

    Science.gov (United States)

    Sufian, Raza Sabbir; de Téramond, Guy F.; Brodsky, Stanley J.; Deur, Alexandre; Dosch, Hans Günter

    2017-01-01

    We present a comprehensive analysis of the spacelike nucleon electromagnetic form factors and their flavor decomposition within the framework of light-front (LF) holographic QCD (LFHQCD) We show that the inclusion of the higher Fock components |q q q q q ¯ ⟩ has a significant effect on the spin-flip elastic Pauli form factor and almost zero effect on the spin-conserving Dirac form factor. We present light-front holographic QCD results for the proton and neutron form factors at any momentum transfer range, including asymptotic predictions, and show that our results agree with the available experimental data with high accuracy. In order to correctly describe the Pauli form factor we need an admixture of a five quark state of about 30% in the proton and about 40% in the neutron. We also extract the nucleon charge and magnetic radii and perform a flavor decomposition of the nucleon electromagnetic form factors. The free parameters needed to describe the experimental nucleon form factors are very few: two parameters for the probabilities of higher Fock states for the spin-flip form factor and a phenomenological parameter r , required to account for possible SU(6) spin-flavor symmetry breaking effects in the neutron, whereas the Pauli form factors are normalized to the experimental values of the anomalous magnetic moments. The covariant spin structure for the Dirac and Pauli nucleon form factors prescribed by AdS5 semiclassical gravity incorporates the correct twist scaling behavior from hard scattering and also leads to vector dominance at low energy.

  6. The Sagittarius B2 star-forming region - Subarcsecond radio spectral line and continuum observations

    Energy Technology Data Exchange (ETDEWEB)

    Gaume, R.A.; Claussen, M.J. (E. O. Hulburt Center for Space Research, Washington, DC (USA))

    1990-03-01

    Results are reported of a subarcsecond spatial resolution RF line and continuum study of the Sgr B2 region, observed at the frequency of the 76-alpha hydrogen recombination line and at the (J,K = 3,2) transition of NH3. Also reported are new observations of the ground-state OH main line masers toward Sgr B2 in both left and right circular polarization. The continuum images showed no less than 19 separate H II regions in the Sgr B2 complex. Ammonia emission was observed in the Sgr B2 K and F regions. The emission toward K was found near the K1, K2, and K3 regions. The NH3 emission and absorption toward the F region, along with the OH maser emission, delineate a rotating disk or torus of molecular material surrounding the Sgr B2 F complex of H II regions. The mass interior to the NH3 and OH emission regions was calculated to be on the order of 1400 solar masses. 38 refs.

  7. Changes to urban form and commuting patterns: trends in two Danish city regions

    DEFF Research Database (Denmark)

    Nielsen, Thomas Alexander Sick

    2015-01-01

    towards more balanced development. The increasing size of the main node in the PUR is the only deviation from the general trend. The general tendency towards a more polycentric regional structure was most marked in changing interaction and commuting patterns. Inter-urban commuting increased, while intra......-urban commuting decreased, leading to dispersion of commuters and a rapid increase in commuting across the region. Commuting distances were shortest in the polycentric region, but it also had the highest growth rates. In both regions, the balancing trend leads to a dispersal of commuting demand over...... an increasingly complex web of origins and destination nodes. This tendency compels us to question whether people’s choice of residence is becoming increasingly irrelevant to their place of work. In relation to polycentricity and sustainability, this calls into question the degree to which proximity can...

  8. METHODS OF DETERMINATION OF POTENTIAL AREAS OF FORMING SOCIO-ECONOMIC INNOVATIVE CLUSTERS IN THE REGION

    Directory of Open Access Journals (Sweden)

    Oleg A. Donichev

    2013-01-01

    Full Text Available The article describes the main problems of formation of innovation clusters in the regions, the role and the importance of government in these issues. The characteristics of the main socio-economic and innovative performances of the region are analyzed to determine its potential for creating innovative economic cluster. The methods for detecting possible potential areas of formation of such cluster are developed.

  9. Observations of Galactic star-forming regions with the Cosmic Background Imager at 31 GHz

    CERN Document Server

    Demetroullas, Constantinos; Stamadianos, Dimitrios; Harper, Stuart; Cleary, Kieran; Jones, Mike; Pearson, Tim; Readhead, Anthony; Taylor, Angela

    2015-01-01

    Studies of the diffuse Galactic radio emission are interesting both for better understanding the physical conditions in our Galaxy and for minimising the contamination in cosmological measurements. Motivated by this we present Cosmic Background Imager 31 GHz observations of the Galactic regions NGC 6357, NGC 6334, W51 and W40 at $\\sim$4$'$.5 resolution and conduct an investigation of the spectral emission process in the regions at 4$'$.5 and 1$^{\\circ}$ resolution. We find that most of the emission in the regions is due to optically thin free-free. For 2 sub-regions of NGC 6334 and for a sub-region of W51 though, at 4$'$.5 resolution and at 31 GHz we detect less emission than expected from extrapolation of radio data at lower frequencies assuming a spectral index of $-$0.12 for optically thin free-free emission, at 3.3$\\sigma$, 3.7$\\sigma$ and 6.5$\\sigma$ respectively. We also detect excess emission in a sub-region of NCG 6334 at 6.4$\\sigma$, after ruling out any possible contribution from Ultra Compact HII (...

  10. Testing the universality of star formation - II. Comparing separation distributions of nearby star-forming regions and the field

    CERN Document Server

    King, Robert R; Parker, Richard J; Patience, Jenny

    2012-01-01

    We have measured the multiplicity fractions and separation distributions of seven young star-forming regions using a uniform sample of young binaries. Both the multiplicity fractions and separation distributions are similar in the different regions. A tentative decline in the multiplicity fraction with increasing stellar density is apparent, even for binary systems with separations too close (19-100au) to have been dynamically processed. The separation distributions in the different regions are statistically indistinguishable over most separation ranges, and the regions with higher densities do not exhibit a lower proportion of wide (300-620au) relative to close (62-300au) binaries as might be expected from the preferential destruction of wider pairs. Only the closest (19-100au) separation range, which would be unaffected by dynamical processing, shows a possible difference in separation distributions between different regions. The combined set of young binaries, however, shows a distinct difference when comp...

  11. An Extensive, Sensitive Search for SiO Masers in High- and Intermediate-Mass Star-Forming Regions

    CERN Document Server

    Zapata, Luis A; Reid, Mark; Beuther, Henrik

    2008-01-01

    We present sensitive Very Large Array observations with an angular resolution of a few arcseconds of the $J= 1 - 0$ line of SiO in the $v$=1 and 2 vibrationally excited states toward a sample of 60 Galactic regions in which stars of high or intermediate mass are currently forming and/or have recently formed. We report the detection of SiO maser emission in \\textit{both} vibrationally excited transitions toward only three very luminous regions: Orion-KL, W51N and Sgr B2(M). Toward all three, SiO maser emission had previously been reported, in Orion-KL in both lines, in W51N only in the $v=2$ line and in Sgr B2(M) only in the $v=1$ line. Our work confirms that SiO maser emission in star-forming regions is a rare phenomenon, indeed, that requires special, probably extreme, physical and chemical conditions not commonly found. In addition to this SiO maser survey, we also present images of the simultaneously observed 7 mm continuum emission from a subset of our sample of star-forming regions where such emission wa...

  12. Investigation on the geographical distribution and life form of plant species in sub alpine zone Karsanak region, Shahrekord

    Directory of Open Access Journals (Sweden)

    Jahanbakhsh Pairanj

    2011-09-01

    Full Text Available This study was carried out in rangelands of Karsanak, Chaharmahal and Bakhtiari province, which is regarded as one of the rich rangelands. Phytogeographically, this region is located in Irano-Turanian (zone of sub alpine. Endemic and rare plants were identified and geographical distribution and life form of identified plant species were investigated as well. Overall, 100 species from 17 families were identified from which 20 percent of identified species was endemic element of Irano-Turanian region. Results indicated that 75.7 percent of identified plants belonged to the Irano-Turanian and only 3 and 2 percent belonged to Euro-Siberian and Mediterranean regions respectively. The reason of high percentage of Irano-Turanian elements is probably the long distance of this region from other regions. Similarities of Irano-Turanian and Mediterranean were included 6.1 percent of identified plants and Irano-Turanian and Euro-Siberian included 2 percent. Results of life forms showed hemichryptophytes including 60 percent of life forms which indicate the cold and mountainous weather.

  13. The growth of the central region by acquisition of counter-rotating gas in star-forming galaxies

    CERN Document Server

    Chen, Yan-Mei; Tremonti, Christy A; Bershady, Matt; Merrifield, Michael; Emsellem, Eric; Jin, Yi-Fei; Huang, Song; Fu, Hai; Wake, David A; Bundy, Kevin; Stark, David; Lin, Lihwai; Argudo-Fernandez, Maria; Bergmann, Thaisa Storchi; Bizyaev, Dmitry; Brownstein, Joel; Bureau, Martin; Chisholm, John; Drory, Niv; Guo, Qi; Hao, Lei; Hu, Jian; Li, Cheng; Li, Ran; Lopes, Alexandre Roman; Pan, Kai-Ke; Riffel, Rogemar A; Thomas, Daniel; Wang, Lan; Westfall, Kyle; Yan, Ren-Bin

    2016-01-01

    Galaxies grow through both internal and external processes. In about 10% of nearby red galaxies with little star formation, gas and stars are counter-rotating, demonstrating the importance of external gas acquisition in these galaxies. However, systematic studies of such phenomena in blue, star-forming galaxies are rare, leaving uncertain the role of external gas acquisition in driving evolution of blue galaxies. Based on new measurements with integral field spectroscopy of a large representative galaxy sample, we find an appreciable fraction of counter-rotators among blue galaxies (9 out of 489 galaxies). The central regions of blue counter-rotators show younger stellar populations and more intense, ongoing star formation than their outer parts, indicating ongoing growth of the central regions. The result offers observational evidence that the acquisition of external gas in blue galaxies is possible; the interaction with pre-existing gas funnels the gas into nuclear regions (< 1 kpc) to form new stars.

  14. Hyperon elastic electromagnetic form factors in the space-like momentum region

    Energy Technology Data Exchange (ETDEWEB)

    Sanchis-Alepuz, Helios [Justus-Liebig-Universitaet Giessen, Institut fuer Theoretische Physik, Giessen (Germany); Karl-Franzens-Universitaet Graz, Institut fuer Physik, Graz (Austria); Fischer, Christian S. [Justus-Liebig-Universitaet Giessen, Institut fuer Theoretische Physik, Giessen (Germany)

    2016-02-15

    We present a calculation of the electric and magnetic form factors of ground-state octet and decuplet baryons including strange quarks. We work with a combination of Dyson-Schwinger equations for the quark propagator and covariant Bethe-Salpeter equations describing baryons as bound states of three (non-perturbative) quarks. Our form factors for the octet baryons are in good agreement with corresponding lattice data at finite Q{sup 2}; deviations in some isospin channels for the magnetic moments can be explained by missing meson cloud effects. At larger Q{sup 2} our quark core calculation has predictive power for both, the octet and decuplet baryons. (orig.)

  15. A multiwavelength study of the star forming H II region Sh2-82

    CERN Document Server

    Wang, Nai-Ping Yu Jun-Jie

    2016-01-01

    Based on a multiwavelength study, the interstellar medium and young stellar objects (YSOs) around the HII region Sh2-82 have been analyzed. Two molecular clumps were found from the archival data of the Galactic Ring Survey, and using the Two Micron All-Sky Survey catalog, we found two corresponding young clusters embedded in the molecular clumps. The very good relations between CO emission, infrared shells and YSOs suggest that it is probably a triggered star formation region from the expansion of Sh2-82. We further used the data from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire from Spitzer to study the YSOs within the two clumps, confirming star formation in this region. By spectral energy distribution fits to each YSO candidate with infrared excess, we derived the slope of the initial mass function. Finally, comparing the HII region's dynamical age and the fragmentation time of the molecular shell, we discard the "collect and collapse" process as being the triggering mechanism for YSO forma...

  16. Near-Infrared Imaging Polarimetry of S106 Cluster-Forming Region with SIRPOL

    CERN Document Server

    Saito, Hiro; Kandori, Ryo; Kusakabe, Nobuhiko; Hashimoto, Jun; Nakajima, Yasushi; Sato, Yaeko; Nagata, Tetsuya; Nagayama, Takahiro; Kato, Daisuke

    2008-01-01

    We present the results of wide-field JHKs polarimetry toward the HII region S106 using the IRSF (Infrared Survey Facility) telescope. Our polarimetry data revealed an extended (up to ~ 5') polarized nebula over S106. We confirmed the position of the illuminating source of most of the nebula as consistent with S106 IRS4 through an analysis of polarization vectors. The bright portion of the polarized intensity is consistent with the red wing component of the molecular gas. Diffuse polarized intensity emission is distributed along the north--south molecular gas lanes. We found the interaction region between the radiation from S106 IRS4 and the dense gas. In addition, we also discovered two small polarization nebulae, SIRN1 and SIRN2, associated with a young stellar objects (YSO). Aperture polarimetry of point-like sources in this region was carried out for the first time. The regional magnetic field structures were derived using point-like source aperture polarimetry, and the magnetic field structure position an...

  17. Teoretical and practical problems of territorial branding at the example of Sumy region brend forming

    Directory of Open Access Journals (Sweden)

    M.Yu. Karpischenko

    2011-12-01

    Full Text Available Actual theoretical and practical problems of territorial branding have seen in this article. There are historical formation analysis of territorial branding have examined as an independent area of marketing and has presented new conception of Sumy Region brand formation.

  18. 76 FR 22675 - Proposed Information Collection; Comment Request; Pacific Islands Region Permit Family of Forms

    Science.gov (United States)

    2011-04-22

    ...) Pacific Islands Region (PIR) manages the U.S. Fisheries of the Exclusive Economic Zone (EEZ) in the...: Regular submission. Affected Public: Business or other for-profit organizations; individuals or households... on: (a) Whether the proposed collection of information is necessary for the proper performance of...

  19. Water emission from the high-mass star-forming region IRAS 17233-3606

    NARCIS (Netherlands)

    Leurini, S.; Gusdorf, A.; Wyrowski, F.; Codella, C.; Csengeri, T.; van der Tak, F.; Beuther, H.; Flower, D. R.; Comito, C.; Schilke, P.

    2014-01-01

    We investigate the physical and chemical processes at work during the formation of a massive protostar based on the observation of water in an outflow from a very young object previously detected in H2 and SiO in the IRAS 17233-3606 region. We estimated the abundance of water to understand its chemi

  20. A multiwavelength study of the star forming H Ⅱ region Sh2-82

    Institute of Scientific and Technical Information of China (English)

    Nai-Ping Yu; Jun-Jie Wang

    2012-01-01

    Based on a multiwavelength study,the interstellar medium and young stellar objects (YSOs) around the H Ⅱ region Sh2-82 have been analyzed.Two molecular clumps were found from the archival data of the Galactic Ring Survey,and using the Two Micron All-Sky Survey catalog,we found two corresponding young clusters embedded in the molecular clumps.The very good relations between CO emission,infrared shells and YSOs suggest that it is probably a triggered star formation region from the expansion of Sh2-82.We further used the data from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire from Spitzer to study the YSOs within the two clumps,confirming star formation in this region.By spectral energy distribution fits to each YSO candidate with infrared excess,we derived the slope of the initial mass function.Finally,comparing the H Ⅱ region's dynamical age and the fragmentation time of the molecular shell,we discard the "collect and collapse" process as being the triggering mechanism for YSO formation.Sh2-82 can be a mixture of other processes such as radiative-driven implosion and/or collisions with pre-existing clumps.

  1. 77 FR 67792 - Proposed Information Collection; Comment Request; Northeast Region Permit Family of Forms

    Science.gov (United States)

    2012-11-14

    ... extension of a current information collection. Under the Magnuson-Stevens Fishery Conservation and... electronic vessel monitoring system (VMS) to declare their intent to fish before starting a particular trip... signed paper form sent in the mail. VMS Requirements Vessels with VMS requirements are required to...

  2. Distribution of various forms of Cd, Pb and Cu in the Wadge Bank region (Arabian Sea)

    Digital Repository Service at National Institute of Oceanography (India)

    George, M.D.

    Labile, nonlabile and particulate forms of Cd,Pb and Cu were determined in 29 water samples collected from a depth of 5 m, from the Wadge Bank area. Labile Cd varied from 0.1 to 0.2 mu g.l-1 while nonlabile fraction was in the range 0.1 to 0.3 mu gl...

  3. Velocity Field Statistics in Star-Forming Regions, 1 Centroid Velocity Observations

    CERN Document Server

    Miesch, M S; Bally, J

    1998-01-01

    The probability density functions (pdfs) of molecular line centroid velocity fluctuations and fluctuation differences at different spatial lags are estimated for several nearby molecular clouds with active internal star formation. The data consist of over 75,000 $^{13}$CO line profiles divided among twelve spatially and/or kinematically distinct regions. Although three regions (all in Mon R2) appear nearly Gaussian, the others show strong evidence for non-Gaussian, often nearly exponential, centroid velocity pdfs, possibly with power law contributions in the far tails. Evidence for nearly exponential centroid pdfs in the neutral HI component of the ISM is also presented, based on older optical and radio observations. These results are in striking contrast to pdfs found in isotropic incompressible turbulence experiments and simulations. Furthermore, no evidence is found for the scaling of difference pdf kurtosis with Reynolds number which is seen in incompressible turbulence, and the spatial distribution of hi...

  4. Spitzer IRAC Color Diagnostics for Extended Emission in Star Forming Regions

    CERN Document Server

    Ybarra, Jason E; Román-Zúñiga, Carlos G; Lada, Elizabeth A

    2014-01-01

    The infrared data from the Spitzer Space Telescope has provided an invaluable tool for identifying physical processes in star formation. In this study we calculate the IRAC color space of UV fluorescent molecular hydrogen (H$_2$) and Polycyclic Aromatic Hydrocarbon (PAH) emission in photodissociation regions (PDRs) using the Cloudy code with PAH opacities from Draine & Li 2007. We create a set of color diagnostics that can be applied to study the structure of PDRs and to distinguish between FUV excited and shock excited H$_2$ emission. To test this method we apply these diagnostics to Spitzer IRAC data of NGC 2316. Our analysis of the structure of the PDR is consistent with previous studies of the region. In addition to UV excited emission, we identify shocked gas that may be part of an outflow originating from the cluster.

  5. FAMILY AND YOUTH POLICY AS REGULATION FORMS REPRODUCTION OF THE POPULATION OF REGION

    Directory of Open Access Journals (Sweden)

    R.I. Akyulov

    2009-12-01

    Full Text Available In article the problem of formation of a regional family, youth policy is considered, necessity of regulation of processes of reproduction of the population, especially, in the conditions of the proceeding demographic crisis assuming presence of is standard-legal base, corresponding to the decision of problems of demographic development of region is proved. Results of the spent sociological interrogations on problems of family-marriage, reproductive behaviour of youth, and also the relation of the population of younger age groups to the state measures, the young families directed on support, birth rate increase are analyzed. The series of measures for increase family-marriage, reproductive, socio-labor activity of the population and, first of all, youth is offered.

  6. Molecular gas in the star-forming region IRAS 08589-4714

    Science.gov (United States)

    Saldaño, Hugo P.; Vásquez, J.; Cappa, C. E.; Gómez, M.; Duronea, N.; Rubio, M.

    2016-10-01

    Aims: We present an analysis of the region IRAS 08589-4714 with the aim of characterizing the molecular environment. Methods: We observed the 12CO(3 -2), 13CO(3 -2), C18O(3 -2), HCO+(3 -2), and HCN(3 -2) molecular lines in a region of 150''× 150'', centered on the IRAS source, to analyze the distribution and characteristics of the molecular gas linked to the IRAS source. Results: The molecular gas distribution reveals a molecular clump that is coincident with IRAS 08589-4714 and with a dust clump detected at 1.2 mm. The molecular clump is 0.45 pc in radius and its mass and H2 volume density are 310 M⊙ and 1.2 × 104 cm-3, respectively. Two overdensities were identified within the clump in HCN(3-2) and HCO+(3-2) lines. A comparison of the LTE and virial masses suggests that the clump is collapsing in regions that harbor young stellar objects. An analysis of the molecular lines suggests that they are driving molecular outflows. Final reduced APEX data are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/594/A115

  7. Chandra Study of the Cepheus B Star Forming Region: Stellar Populations and the Initial Mass Function

    CERN Document Server

    Getman, K V; Feigelson, E D; Garmire, G; Townsley, L; Tsujimoto, M; Broos, Patrick; Feigelson, Eric D.; Garmire, Gordon; Getman, Konstantin V.; Townsley, Leisa; Tsujimoto, Masahiro

    2006-01-01

    Cepheus B (Cep B) molecular cloud and a portion of the nearby Cep OB3b OB association, one of the most active regions of star formation within 1 kpc, has been observed with the ACIS detector on board the Chandra X-ray Observatory. We detect 431 X-ray sources, of which 89% are confidently identified as clustered pre-main sequence stars. Two main results are obtained. First, we provide the best census to date for the stellar population of the region. We identify many members of two rich stellar clusters: the lightly obscured Cep OB3b association, and the deeply embedded cluster in Cep B whose existence was previously traced only by a handful of radio sources and T Tauri stars. Second, we find a discrepancy between the X-ray Luminosity Functions of the Cep OB3b and the Orion Nebula Cluster. This may be due to different Initial Mass Functions of two regions (excess of ~0.3 solar mass stars), or different age distributions. Several other results are obtained. A diffuse X-ray component seen in the field is attribut...

  8. Molecular gas in the star-forming region IRAS 08589-4714

    CERN Document Server

    Saldaño, Hugo P; Cappa, C E; Gómez, M; Duronea, N U; Rubio, M

    2016-01-01

    We present an analysis of the region IRAS 08589-4714 with the aim of characterizing the molecular environment. We observed the CO(3-2), ^{13}CO(3-2), C^{18}O(3-2), HCO+(3-2), and HCN(3-2) molecular lines in a region of 150" x 150", centered on the IRAS source, to analyze the distribution and characteristics of the molecular gas linked to the IRAS source. The molecular gas distribution reveals a molecular clump that is coincident with IRAS 08589-4714 and with a dust clump detected at 1.2 mm. The molecular clump is 0.45 pc in radius and its mass and H_2 volume density are 310 Mo and 1.2 x 10^4 cm^{-3}, respectively. Two overdensities were identified within the clump in HCN and HCO lines. A comparison of the LTE and virial masses suggests that the clump is collapsing in regions that harbor young stellar objects. An analysis of the molecular lines suggests that they are driving molecular outflows.

  9. Geological characteristics and ore-forming process of the gold deposits in the western Qinling region, China

    Science.gov (United States)

    Liu, Jiajun; Liu, Chonghao; Carranza, Emmanuel John M.; Li, Yujie; Mao, Zhihao; Wang, Jianping; Wang, Yinhong; Zhang, Jing; Zhai, Degao; Zhang, Huafeng; Shan, Liang; Zhu, Laimin; Lu, Rukui

    2015-05-01

    The western Qinling, belonging to the western part of the Qinling-Dabie-Sulu orogen between the North China Block and South China Block, is one of the most important gold regions in China. Isotopic dates suggest that the Mesozoic granitoids in the western Qinling region emplaced during the Middle-Late Triassic, and the deposits formed during the Late Triassic. Almost all gold deposits in the western Qinling region are classified as orogenic, Carlin-type, and Carlin-like gold deposits, and they are the products of Qinling Orogenesis caused by the final collision between the North China Block and the South China Block. The early subduction of the Mian-Lue oceanic crust and the latter collision between South Qinling Terrane and the South China Block along the Mian-Lue suture generated lithosphere-scale thermal anomalies to drive orogen-scale hydrothermal systems. The collision-related magmatism also provided heat source for regional ore-forming fluids in the Carlin-like gold deposits. Orogenic gold deposits such as Huachanggou, Liziyuan, and Baguamiao lie between the Shang-Dan and Mian-Lue sutures and are confined to WNW-trending brittle-ductile shear zones in Devonian and Carboniferous greenschist-facies metasedimentary rocks that were highly-deformed and regionally-metamorphosed. These deposits are typical orogenic gold deposits and formed within a Late Triassic age. The deposits show a close relationship between Au and Ag. Ores contain mainly microscopic gold, and minor electrum and visible gold, along with pyrite. The ore-forming fluids were main metamorphic fluids. Intensive tectonic movements caused by orogenesis created fluid-migrating channels for precipitation locations. Although some orogenic gold deposits occur adjacent to granitoids, mineralization is not synchronous with magmatism; that is, the granitoids have no genetic relations to orogenic gold deposits. As ore-forming fluids converged into dilated fractures during the extension stage of orogenesis

  10. Implications of the recent high statistics determination of the pion electromagnetic form factor in the timelike region

    Science.gov (United States)

    Ananthanarayan, B.; Caprini, Irinel; Imsong, I. Sentitemsu

    2011-05-01

    The recently evaluated two-pion contribution to the muon g-2 and the phase of the pion electromagnetic form factor in the elastic region, known from ππ scattering by Fermi-Watson theorem, are exploited by analytic techniques for finding correlations between the coefficients of the Taylor expansion at t=0 and the values of the form factor at several points in the spacelike region. We do not use specific parametrizations, and the results are fully independent of the unknown phase in the inelastic region. Using for instance, from recent determinations, ⟨rπ2⟩=(0.435±0.005)fm2 and F(-1.6GeV2)=0.243-0.014+0.022, we obtain the allowed ranges 3.75GeV-4≲c≲3.98GeV-4 and 9.91GeV-6≲d≲10.46GeV-6 for the curvature and the next Taylor coefficient, with a strong correlation between them. We also predict a large region in the complex plane where the form factor cannot have zeros.

  11. Implications of the recent high statistics determination of the pion electromagnetic form factor in the timelike region

    CERN Document Server

    Ananthanarayan, B; Imsong, I Sentitemsu

    2011-01-01

    The recently evaluated two-pion contribution to the muon g-2 and the phase of the pion electromagnetic form factor in the elastic region, known from \\pi\\pi scattering by Fermi-Watson theorem, are exploited by analytic techniques for finding correlations between the coefficients of the Taylor expansion at t=0 and the values of the form factor at several points in the spacelike region. We do not use specific parametrizations and the results are fully independent of the unknown phase in the inelastic region. Using for instance, from recent determinations, = (0.435 \\pm 0.005) fm^2 and F(-1.6 GeV^2)=0.243^{+0.022}_{-0.014}, we obtain the allowed ranges 3.75 GeV^{-4}\\lesssim c \\lesssim 3.98 GeV^{-4} and 9.91 GeV^{-6}\\lesssim d \\lesssim 10.46 GeV^{-6} for the curvature and the next Taylor coefficient, with a strong correlation between them. We also predict a large region in the complex plane where the form factor can not have zeros.

  12. «Goroda-bliznecy»: novaja forma prigranichnogo sotrudnichestva v Baltijskom regione? [Twin cities: a new form of cross-border cooperation in the Baltic Sea Region?

    Directory of Open Access Journals (Sweden)

    Anishenko Anatoly

    2012-01-01

    Full Text Available The paper demonstrates the first attempt in Russian political studies to conduct a comprehensive analysis of the “twin city” movement as a form of cross-border cooperation in the Baltic region. This phenomenon emerged as a result of a global tendency towards more active involvement of municipal units in international cooperation, on the one hand, and aspirations of frontier cities and towns in the Baltic region to solve common problems together, on the other hand. This work is based on a comparative analysis method and a case study methodology. The authors consider four examples (city pairs: Tornio — Haparanda, Valga — Valka, Narva — Ivangorod and Imatra — Svetogorsk. The article specifies the terminological framework used in this field of research. The authors analyse achievements and failures of this type of international inter-municipal cooperation and emphasise that for twin cities it served not only as a means of survival in the difficult situation of the 1990s, but also as an experimental ground for new forms of crossborder cooperation. The authors arrive at the conclusion that this model proves to be promising for further development of integration processes in the Baltic region. This practice can be applied by Russian municipal, regional and federal authorities in promotion of cross-border cooperation not only in the Baltic region, but also in other regions of the country. Thus, influenced by the successful experience of Baltic frontier cities and towns, the Russian city of Nikel and the Norwegian city of Kirkenes decided to adopt this model for further development of their cooperation.

  13. Uncovering the monster stars in W49: the most luminous star-forming region in the Milky Way

    Science.gov (United States)

    Wu, Shiwei; Bik, Arjan; Henning, Thomas; Pasquali, Anna; Brandner, Wolfgang; Stolte, Andrea

    2015-08-01

    As a part of the LOBSTAR project (Luci OBservations of STARburst regions), which aims at understanding the stellar content of some of the most massive star-forming regions, we present our result on the high-mass stellar content of W49. K-band spectra of the candidate massive stars from VLT/ISAAC and LBT/LUCI provide us with reliable spectral types of dozens of massive stars in this HII region.The first results show that this region hosts several of the most massive stars in our galaxy. Two most brightest stars, one in the core of the central cluster and one in W49 South, were identified as very massive stars (M > 100 M⊙). Their K-band spectra exhibit strong stellar wind features, and they are classified as O2-3.5If* supergiant stars. After comparison to the Geneva evolutionary models, the mass range of W49nr1 was estimated to be between 100 M⊙ and 180 M⊙. Additionally we find 12 O stars with spectral types between O7V and O3V and masses from 25 M⊙ to 125 M⊙, respectively.These results allow us to derive the fundamental parameters of the cluster (mass, age) as well as the total energy output in the form of ionising photons. This will enable us to study the feedback effects of this extreme star forming region in great detail. To our surprise, two young stellar objects with infrared excess feature showing CO emission lines in their spectra are identified. This suggests that circumstellar disks can survive even in this extreme environment. Finally the spatial distribution of the massive stars is analysed to discuss the star formation history and identify potential runaway stars. The extreme properties of this region makes it a good template for more extreme star formation outside our galaxy.

  14. STAR FORMING REGIONS TOWARDS STELLAR WIND BUBBLES: RCW 52 AND RCW 78

    Directory of Open Access Journals (Sweden)

    C. E. Cappa

    2011-01-01

    Full Text Available Hemos llevado a cabo observaciones de la emisión en el continuo infrarrojo en 870 uÊm y de la línea molecular 13CO(2-1 hacia regiones de formación estelar en las burbujas interestelares RCW52 and RCW78 utilizando el telescopio APEX. Las observaciones moleculares revelaron los densos grumos en los que están embebidos los candidatos a objetos estelares jóvenes, mientras que las observaciones de continuo en el infrarrojo nos permitieron detectar el polvo frío asociado.

  15. [Gamma]-ray emission form regions of star formation theory and observations with the MAGIC telescope /

    OpenAIRE

    Domingo Santamaría, Eva

    2006-01-01

    Consultable des del TDX Títol obtingut de la portada digitalitzada Es el propósito de esta tesis estudiar la posibilidad de que regiones con importante actividad en formación estelar sean fuentes de rayos gamma para los actuales y futuros detectores, ya sean detectores de rayos gamma con base en satélites como telescopios Cherenkov situados en la superficie terrestre. Tras una evaluación fenomenológica positiva de que la emisión de rayos gamma procedente de galaxias con elevada activida...

  16. Normal mode analyses of methyl palmitate all-trans and disordered forms in wagging progressive region.

    Science.gov (United States)

    Ishioka, Tsutomu; Yan, Wenhong; Strauss, Herbert L; Snyder, Robert G

    2003-03-01

    Normal mode analyses are made for methyl palmitate molecule having all-trans or conformational disorders around the ester head group, in order to explain characteristic observed frequency shifts in the wagging progressive region between all-trans and disorder chains in triglyceride molecules. It was found that one gauche conformation at C(alpha)-C(beta) position and 90 degrees rotation of the ester head group in an alkyl chain produce frequency shifts for twisting mode as observed. For wagging modes, contamination of the disorders around the head group makes assignments change and apparent frequency shifts occur.

  17. TADPOL: A 1.3 mm Survey of Dust Polarization in Star-forming Cores and Regions

    OpenAIRE

    Hull, Charles L. H.; Plambeck, Richard L.; Kwon, Woojin; Bower, Geoffrey C.; Carpenter, John M.; Crutcher, Richard M.; Fiege, Jason D.; Franzmann, Erica; Hakobian, Nicholas S.; Heiles, Carl; Houde, Martin; Hughes, A. Meredith; Lamb, James W.; Looney, Leslie W.; Marrone, Daniel P.

    2014-01-01

    We present λ 1.3 mm Combined Array for Research in Millimeter-wave Astronomy observations of dust polarization toward 30 star-forming cores and eight star-forming regions from the TADPOL survey. We show maps of all sources, and compare the ~2".5 resolution TADPOL maps with ~20" resolution polarization maps from single-dish submillimeter telescopes. Here we do not attempt to interpret the detailed B-field morphology of each object. Rather, we use average B-field orientations to derive conclusi...

  18. Final-state interaction correction to the electromagnetic nucleon form factors in the time-like region

    Energy Technology Data Exchange (ETDEWEB)

    Van de Wiele, Jacques; Ong, Saro [Universite de Paris-Sud, Institut de Physique Nucleaire d' Orsay (UMR 8608), IN2P3-CNRS, Orsay Cedex (France)

    2015-10-15

    We study the strong energy dependence of the proton electromagnetic form factors in the time-like region, taking into account the one-pion-exchange final-state interaction in a covariant way. This effect is quantified in terms of the corrected Dirac F{sub 1} and Pauli F{sub 2} form factors and in the commonly used electric G{sub E} and magnetic G{sub M} ones. Our results on the ratio G{sub E} /G{sub M} depend only on the values of two free parameters and allow significant comparisons with the BaBar data. (orig.)

  19. 15N Fractionation in Star-Forming Regions and Solar System Objects

    Science.gov (United States)

    Wirstrom, Eva; Milam, Stefanie; Adande, GIlles; Charnley, Steven; Cordiner, Martin

    2015-01-01

    A central issue for understanding the formation and evolution of matter in the early Solar System is the relationship between the chemical composition of star-forming interstellar clouds and that of primitive Solar System materials. The pristinemolecular content of comets, interplanetary dust particles and carbonaceous chondrites show significant bulk nitrogen isotopic fractionation relative to the solar value, 14N15N 440. In addition, high spatial resolution measurements in primitive materials locally show even more extreme enhancements of 14N15N 100.

  20. Protoplanetary Disk Evolution around the Triggered Star Forming Region Cepheus B

    CERN Document Server

    Getman, Konstantin V; Luhman, Kevin L; Sicilia-Aguilar, Aurora; Wang, Junfeng; Garmire, Gordon P

    2009-01-01

    The Cepheus B (CepB) molecular cloud and a portion of the nearby CepOB3b OB association, one of the most active regions of star formation within 1 kpc, have been observed with the IRAC detector on board the Spitzer Space Telescope. The goals are to study protoplanetary disk evolution and processes of sequential triggered star formation in the region. Out of ~400 pre-main sequence (PMS) stars selected with an earlier Chandra X-ray Observatory observation, 95% are identified with mid-infrared sources and most of these are classified as diskless or disk-bearing stars. The discovery of the additional >200 IR-excess low-mass members gives a combined Chandra+Spitzer PMS sample complete down to 0.5 Mo outside of the cloud, and somewhat above 1 Mo in the cloud. Analyses of the nearly disk-unbiased combined Chandra+Spitzer selected stellar sample give several results. Our major finding is a spatio-temporal gradient of young stars from the hot molecular core towards the primary ionizing O star HD 217086. This strongly ...

  1. Interaction between the Supernova Remnant HB 3 and the Nearby Star-Forming Region W3

    CERN Document Server

    Zhou, Xin; Fang, Min; Su, Yang; Sun, Yan; Chen, Yang

    2016-01-01

    We performed millimeter observations in CO lines toward the supernova remnant (SNR) HB 3. Substantial molecular gas around -45 km s^-1 is detected in the conjunction region between the SNR HB 3 and the nearby W3 complex. This molecular gas is distributed along the radio continuum shell of the remnant. Furthermore, the shocked molecular gas indicated by line wing broadening features is also distributed along the radio shell and inside it. By both morphological correspondence and dynamical evidence, we confirm that the SNR HB 3 is interacting with the -45 km s^-1 molecular cloud (MC), in essence, with the nearby H II region/MC complex W3. The red-shifted line wing broadening features indicate that the remnant is located at the nearside of the MC. With this association, we could place the remnant at the same distance as the W3/W4 complex, which is 1.95 +- 0.04 kpc. The spatial distribution of aggregated young stellar object candidates (YSOc) shows a correlation to the shocked molecular strip associated with the ...

  2. A Catalog of Methanol Masers in Massive Star-forming Regions. III. The Molecular Outflow Sample

    CERN Document Server

    Gómez-Ruiz, A I; Araya, E D; Hofner, P; Loinard, L

    2016-01-01

    We present an interferometric survey of the 44 GHz class I methanol maser transition toward a sample of 69 sources consisting of High Mass Protostellar Object candidates and Ultracompact (UC) H II regions. We found a 38% detection rate (16 of 42) in the HMPO candidates and a 54% detection rate (13 of 24) for the regions with ionized gas. This result indicates that class I methanol maser emission is more common toward more evolved young stellar objects of our sample. Comparing with similar interferometric data sets, our observations show narrower linewidths, likely due to our higher spatial resolution. Based on a comparison between molecular outflow tracers and the maser positions, we find several cases where the masers appear to be located at the outflow interface with the surrounding core. Unlike previous surveys, we also find several cases where the masers appear to be located close to the base of the molecular outflow, although we can not discard projection effects. This and other surveys of class I methan...

  3. Digitisation Project Planning in the Maribor City Library as a Form of Regional Cross Institutional Cooperation

    Directory of Open Access Journals (Sweden)

    Nina Hriberšek Vuk

    2013-09-01

    Full Text Available EXTENDED ABSTRACT:More and more Slovenian public libraries have been facing the question of selection criteria for digitisation of library materials as well as the issue of financial resources, copyright permission and the promotion of digitised materials. Libraries having long tradition of collecting valuable local history resources are more convinced about the selection criteria. Digitisation is, in spite of being expensive, time consuming and labour intensive, an easy method to enable quick access to library materials, to promote and preserve library collections. The mission of the central regional public library (cofinanced by the Ministry of Culture is not only to coordinate the collection, cataloguing and storage of local history resources but also to coordinate local history digital projects. Due to historical circumstances, the local history resources were first collected by the Maribor University Library. It is only in the recent past that the Maribor City Library has started to systematically collect these materials. Due to this fact, the Maribor City Library does not hold an extensive collection of rare and valuable local history items. It was initially faced with the problem of selection criteria for digitisation. However, it soon succeeded to establish the strategy to promote the local history collections in the region, regardless of their location. Thus the library started to cooperate with different regional institutions and the first partner projects were designed. In the year 2007 the library collaborated with the elementary school at Lovrenc na Pohorju and decided to digitise research papers of ex-pupils of the school. The first part of the project was accomplished in 2007 when 72 research papers were digitised, in the next two years their number was increased as the second part of the project was concluded. The papers were published on the KAMRA portal and the project was promoted at the summer annual meeting at Lovrenc na

  4. Cloud Structure of Galactic OB Cluster Forming Regions from Combining Ground and Space Based Bolometric Observations

    CERN Document Server

    Lin, Yuxin; Li, Di; Zhang, Zhiyu; Ginsburg, Adam; Pineda, Jaime E; Qian, Lei; Galván-Madrid, Roberto; McLeod, Anna Faye; Rosolowsky, Erik; Dale, James E; Immer, Katharina; Koch, Eric; Longmore, Steve; Walker, Daniel; Testi, Leonardo

    2016-01-01

    We have developed an iterative procedure to systematically combine the millimeter and submillimeter images of OB cluster-forming molecular clouds, which were taken by ground based (CSO, JCMT, APEX, IRAM-30m) and space telescopes (Herschel, Planck). For the seven luminous ($L$$>$10$^{6}$ $L_{\\odot}$) Galactic OB cluster-forming molecular clouds selected for our analyses, namely W49A, W43-Main, W43-South, W33, G10.6-0.4, G10.2-0.3, G10.3-0.1, we have performed single-component, modified black-body fits to each pixel of the combined (sub)millimeter images, and the Herschel PACS and SPIRE images at shorter wavelengths. The $\\sim$10$"$ resolution dust column density and temperature maps of these sources revealed dramatically different morphologies, indicating very different modes of OB cluster-formation, or parent molecular cloud structures in different evolutionary stages. The molecular clouds W49A, W33, and G10.6-0.4 show centrally concentrated massive molecular clumps that are connected with approximately radia...

  5. Photodissociation of organic molecules in star-forming regions. II. Acetic acid

    Science.gov (United States)

    Pilling, S.; Santos, A. C. F.; Boechat-Roberty, H. M.

    2006-04-01

    Fragments from organic molecule dissociation (such as reactive ions and radicals) can form interstellar complex molecules like amino acids. The goal of this work is to experimentally study photoionization and photodissociation processes of acetic acid (CH3COOH), a glycine (NH2CH2COOH) precursor molecule, by soft X-ray photons. The measurements were taken at the Brazilian Synchrotron Light Laboratory (LNLS), employing soft X-ray photons from a toroidal grating monochromator (TGM) beamline (100-310 eV). Mass spectra were obtained using the photoelectron photoion coincidence (PEPICO) method. Kinetic energy distribution and abundances for each ionic fragment have been obtained from the analysis of the corresponding peak shapes in the mass spectra. Absolute photoionization and photodissociation cross sections were also determined. We have found, among the channels leading to ionization, that only 4-6% of CH3COOH survive the strong ionization field. CH3CO^+, COOH+ and CH3+ ions are the main fragments, and the presence of the former may indicate that the production-destruction process of acetic acid in hot molecular cores (HMCs) could decrease the H2O abundance since the net result of this process converts H2O into OH + H^+. The COOH+ ion plays an important role in ion-molecule reactions to form large biomolecules like glycine.

  6. CIRCUMNUCLEAR STAR-FORMING REGIONS IN EARLY TYPE SPIRAL GALAXIES: DYNAMICAL MASSES

    Directory of Open Access Journals (Sweden)

    G. F. Hägele

    2014-01-01

    Full Text Available Presentamos medidas de la dispersi ́on de velocidades en 17 regiones de formaci ́on es telar circunnucleares (CNS- FRs y los n ́ucleos de tres galaxias espirales barradas: NGC2903, NGC33 10 y NGC3351 a partir de espectros de alta dispersi ́on. Las dispersiones estelares han sido obtenidas de las l ́ıneas del triplete de CaII (CaT a λλ 8494, 8542, 8662 ̊ A, mientras que las dispersiones de velocidades del gas han sido medidas mediante ajus tes gaussianos a las l ́ıneas de H β λ 4861 ̊ A y de [OIII] λ 5007 ̊ A. Las CNSFRs, con tama ̃nos de alrededor de 100 a 150pc en di ́ametro, parecen estar compuestas por varios c ́umulos estelares indiv iduales con tama ̃nos entre 1.5 y 6.2pc medidos sobre im ́agenes del Telescopio Espacial Hubble (HST. Utilizando las di spersiones de velocidades estelares, hemos derivado las masas din ́amicas para los complejos de formaci ́o n estelar completos y para los c ́umulos estelares individuales. Los valores de la dispersi ́on de velocidades estel ares est ́an entre 31 y 73kms − 1 . Las masas din ́amicas para las CNSFRs completas est ́an entre 4 . 9 × 10 6 y 1 . 9 × 10 8 M ⊙ y entre 1 . 4 × 10 6 y 1 . 1 × 10 7 M ⊙ para los c ́umulos estelares individuales. Hemos encontrado indicaciones de la presencia de do s componentes cinem ́aticas diferentes en el gas ionizado de las regiones. La componente es trecha proporcionada por el ajuste de dos-componentes gausianas, parece tener un valor relativamente cons tante para todas las CNSFRs estudiadas, con los valores estimados muy pr ́oximos a 25kms − 1 . Esta componente estrecha podr ́ıa identificarse con gas ionizado en un disco rotante, mientras que las estrellas y l a fracci ́on de gas (responsable de la componente ancha relacionadas con las regiones de formaci ́on estelar, esta r ́ıan mayormente soportadas por presi ́on din ́amica.

  7. Properties of the high-mass star forming region IRAS 22475+5939

    Institute of Scientific and Technical Information of China (English)

    Xiao-Lan Liu; Jun-Jie Wang

    2012-01-01

    IRAS 22475+5939 has been well studied by previous astronomers,but we can still discover new characteristics about it,using the first observations of the lines from CO J=2-1,13CO J=2-1 and 13CO J=3-2 by the KOSMA 3m telescope.The mapping of the intensity ratio of 13CO J=3-2 and 13CO J=2-1 shows that the distribution of the temperature has two peaks,neither of which coincide with the IRAS 22475+5939 source or the center of the HII region,but rather are located at the edge of the HII region.Overlays of the Spitzer IRAC 8 μm with CO contours indicate that they are associated with each other and that the strongest polycyclic aromatic hydrocarbon(PAH)emission is at the IRAS 22475+5939 source position.The IRAS LRS spectrum at 7 μm 23 μm and the PHT-s spectrum at 2 μm ~ 12 μm of the IRAS 22475+5939 source also exhibit strong PAH emission characteristics in the main PAH bands.The diversity of the PAH family should be responsible for the plateaus in the PAH emission in the PHT-s and IRAS-LRS spectra.Analysis and modeling in the infrared bands suggest that IRAS 22475+5939 is more likely to be a class I young stellar object.Where this is the case,the star is likely to have a temperature of Teff~ 9995.8K,mass ~ 15.34M⊙,luminosity ~ 1.54 × 104 L⊙ and age ~ 1.54 × 104 yr.The model shows that circumstellar disc emission is important for wavelengths between 1 and 10 μm,otherwise,the envelope fluctuates for A > 10μm.Bipolar outflow is confirmed in the molecular cloud,and the excited star of the HII region could be the driving source of the outflow.High resolution is required for better results.

  8. Near-Infrared Observations of the Massive Star Forming Region IRAS 23151+5912

    Institute of Scientific and Technical Information of China (English)

    Xue-Peng Chen; Yong-Qiang Yao

    2004-01-01

    Near-infrared images and K-band spectroscopy of the massive starforming region IRAS 23151+5912 are presented.The JHK' images reveal an embedded infrared cluster associated with infrared nebula,and the H2(2.12μm)narrowband image provides for the first time evidence of outflow activity associated with the cluster.That the cluster is young can be shown by the high percentage of infrared excess sources and the outflow activity.We suggest an age of the cluster of ~ 106 yr.Eight young stars are found in the bright nebular core around IRAS 23151+5912.By the color-magnitude diagrams of the cluster,we found five high-mass YSOs and four intermediate-mass YSOs in the cluster.Eight H2 emission features are discovered in the region with a scattered and non-axisymmetric distribution,indicating the existence of multiple outflows driven by the cluster.Diffuse H2 emission detected to the north and to the west of the cluster may result from UV leakage of the cluster.Brγ,H2,and CIV emission lines are found in the K-band spectrum of the brightest source,NIRS 19,indicating the presence of envelope,stellar wind,and shock in the circumstellar environment.We have estimated an O7-O9spectral type for the central massive YSO(20 ~ 30M⊙),with an age of less than 1×106 yr.

  9. Photodissociation of organic molecules in star-forming regions II: Acetic acid

    CERN Document Server

    Pilling, S; Boechat-Roberty, H M

    2006-01-01

    Fragments from organic molecule dissociation (such as reactive ions and radicals) can form interstellar complex molecules like amino acids. The goal of this work is to experimentally study photoionization and photodissociation processes of acetic acid (CH$_3$COOH), a glycine (NH$_2$CH$_2$COOH) precursor molecule, by soft X-ray photons. The measurements were taken at the Brazilian Synchrotron Light Laboratory (LNLS), employing soft X-ray photons from a toroidal grating monochromator (TGM) beamline (100 - 310 eV). Mass spectra were obtained using the photoelectron photoion coincidence (PEPICO) method. Kinetic energy distribution and abundances for each ionic fragment have been obtained from the analysis of the corresponding peak shapes in the mass spectra. Absolute photoionization and photodissociation cross sections were also determined. We have found, among the channels leading to ionization, that only 4-6% of CH$_3$COOH survive the strong ionization field. CH$_3$CO$^+$, COOH$^+$ and CH$_3^+$ ions are the mai...

  10. A new sympatric region for distinct karyotypic forms of Hoplias malabaricus (Pisces, Erythrinidae

    Directory of Open Access Journals (Sweden)

    G. G. Born

    Full Text Available Specimens of Hoplias malabaricus from Lagoa Carioca, an isolated lake of the Rio Doce State Park (state of Minas Gerais, Brazil, were cytogenetically studied. The diploid number was found to be constant, i.e., 2n = 42 chromosomes, although two karyotypic forms were found: karyotype A, characterized by 22M + 20SM chromosomes, observed only in a male specimen, and karyotype B, characterized by 24M + 16SM + 2ST and 24M + 17SM + 1ST chromosomes in female and male specimens, respectively. This sex difference found in karyotype B is related to an XX/XY sex chromosome system. Another female specimen of H. malabaricus, also carrying karyotype A, had previously been found in the same lake. The available data indicate that two sympatric cytotypes of H. malabaricus exist in the Lagoa Carioca, with cytotype A occurring at a lower frequency and differing from cytotype B by undifferentiated sex chromosomes.

  11. The Comparison of Physical Properties Derived from Gas and Dust in a Massive Star-Forming Region

    CERN Document Server

    Battersby, Cara; Dunham, Miranda; Ginsburg, Adam; Longmore, Steve; Darling, Jeremy

    2014-01-01

    We explore the relationship between gas and dust in massive star-forming regions by comparing physical properties derived from each. We compare the temperatures and column densities in a massive star-forming Infrared Dark Cloud (IRDC, G32.02+0.05), which shows a range of evolutionary states, from quiescent to active. The gas properties were derived using radiative transfer modeling of the (1,1), (2,2), and (4,4) transitions of NH3 on the Karl G. Jansky Very Large Array (VLA), while the dust temperatures and column densities were calculated using cirrus-subtracted, modified blackbody fits to Herschel data. We compare the derived column densities to calculate an NH3 abundance, 4.6 x 10^-8. In the coldest star-forming region, we find that the measured dust temperatures are lower than the measured gas temperatures (mean and standard deviations T_dust ~ 11.6 +/- 0.2 K vs. T_gas ~ 15.2 +/- 1.5 K), which may indicate that the gas and dust are not well-coupled in the youngest regions (~0.5 Myr) or that these observat...

  12. Forming and development of the regional innovational structures as the new paradigm of cooperation between educational institutions and business

    Directory of Open Access Journals (Sweden)

    Pavlo Dudkin

    2013-11-01

    Full Text Available . This article deals with the important scientific-practical problem – justification theoretic-methodological and applied basics of creation and development of regional start-up centers as the innovative form cooperation between educational institutions and business. Meaning of the state innovative policy has been determined, and its realization mechanisms have been analyzed; problems of institutional, legislative and resource supply of the system "education-science-production" activity have been identified. Authors characterize features of innovative structures development and define the place of regional start-up centers within it. Necessity of development of special financial, material-technical and informational support mechanisms of innovational and entrepreneurial activities have been justified. New approaches to cooperation between educational institutions and business have been proposed; which are based on the "hatching" mechanism and promotion of innovations. It is proven that regional start-up centers are convenient to create on the ground of leading educational establishments which have innovations production and commercialization as one of their activity directions. Necessity of functioning of regional university start-up centers have been justified to become a new form of innovational and investment infrastructure, special areas which allow to coordinate demands of innovations producers and entrepreneurship subjects, unite interests of education, science, state and business.

  13. The infield varietu of available forms in the forest-steppe of western part Central Chernozemic region

    Science.gov (United States)

    Belik, Anton; Devyatova, Tatiana; Bozhko, Svetlana; Gorbunova, Yulia

    2016-04-01

    The infield varietu of available forms in the forest-steppe of western part Central Chernozemic region The Central Chernozemic region of Russia has been a region with a strong agricultural industry and determines the food security of the state by most part. The soil cover of the region is represented mainly by chernozems and is favorable for the cultivation of major crops and produce high crop yields. However, the high development of agriculture in the territory of Central Chernozemic region are led to the development of agrogenic degradation processes which impacts on the growth of the soil cover complexity and contrast, and as a consequence a significant infield variety of soil fertility and yields of major crops. In this regard, very promising direction in CChR is the development and practical application technologies of precision agriculture, which implies the spatial variety of soil fertility analysis within specific fields and work areas, especially the content of available forms of nutrients. The aim of our research was a study of the agro-ecological characteristics of the spatial variety of the content by available forms to plants of major nutrients in representative areas of sloping agricultural landscapes with forest-steppe chernozems in the western part of Central Chernozemic region of Russia. The research of infield variety by content of available forms of major nutrients are carried in the fields of Russian Research Institute of Agriculture and Protect the Soil from Erosion experimental and industrial farm in Medvensky district of Kursk region. The area characterized by a complex organization of relief. The soil cover is represented by full-profile typical (conventional and carbonate), leached chernozems. The growth of contrast of the soil cover are largely determined by the appearance of eroded soils of these analogues, as well as zoogenic dug and accumulative soils All of the studied areas with the forest-steppe chernozems were characterized by

  14. Complex Chemistry in Star-Forming Regions: An Expanded Gas-Grain Warm-up Chemical Model

    CERN Document Server

    Garrod, Robin T; Herbst, Eric

    2008-01-01

    Gas-phase processes were long thought to be the key formation mechanisms for complex organic molecules in star-forming regions. However, recent experimental and theoretical evidence has cast doubt on the efficiency of such processes. Grain-surface chemistry is frequently invoked as a solution, but until now there have been no quantitative models taking into account both the high degree of chemical complexity and the evolving physical conditions of star-forming regions. Here, we introduce a new gas-grain chemical network, wherein a wide array of complex species may be formed by reactions involving radicals. The radicals we consider (H, OH, CO, HCO, CH3, CH3O, CH2OH, NH and NH2) are produced primarily by cosmic ray-induced photodissociation of the granular ices formed during the colder, earlier stages of evolution. The gradual warm-up of the hot core is crucial to the formation of complex molecules, allowing the more strongly-bound radicals to become mobile on grain surfaces. This type of chemistry is capable o...

  15. Water maser variability over 20 years in a large sample of star-forming regions: the complete database

    Science.gov (United States)

    Felli, M.; Brand, J.; Cesaroni, R.; Codella, C.; Comoretto, G.; Di Franco, S.; Massi, F.; Moscadelli, L.; Nesti, R.; Olmi, L.; Palagi, F.; Panella, D.; Valdettaro, R.

    2007-12-01

    Context: Water vapor emission at 22 GHz from masers associated with star-forming regions is highly variable. Aims: We present a database of up to 20 years of monitoring of a sample of 43 masers within star-forming regions. The sample covers a large range of luminosities of the associated IRAS source and is representative of the entire population of H2O masers of this type. The database forms a good starting point for any further study of H2O maser variability. Methods: The observations were obtained with the Medicina 32-m radiotelescope, at a rate of 4-5 observations per year. Results: To provide a database that can be easily accessed through the web, we give for each source: plots of the calibrated spectra, the velocity-time-flux density plot, the light curve of the integrated flux, the lower and upper envelopes of the maser emission, the mean spectrum, and the rate of the maser occurrence as a function of velocity. Figures for just one source are given in the text for representative purposes. Figures for all the sources are given in electronic form the appendix. A discussion of the main properties of the H2O variability in our sample will be presented in a forthcoming paper. Based on observations with the Medicina radiotelescope operated by INAF - Istituto di Radioastronomia.

  16. Star-forming regions and the metallicity gradients in the tidal tails: The case of NGC 92

    CERN Document Server

    Torres-Flores, Sergio; de Oliveira, Claudia Mendes; de Mello, Duilia; Amram, Philippe; Plana, Henri

    2013-01-01

    We present new Gemini/GMOS spectroscopic and archival imaging data of the interacting galaxy NGC 92, which is part of a compact group and displays an extended tidal tail. We have studied the physical properties of 20 star-forming complexes in this system. We found that the star-forming regions located in the tidal tail of NGC 92 have ages younger than 8 Myr, which suggests that these objects were formed in situ. The spectroscopic data reveals that these regions have slightly sub-solar metallicities, suggesting that they were formed from pre-enriched material. Using the oxygen abundances derived for each system, we found that the extended tidal tail of NGC 92 has a flat metallicity distribution. Although this scenario is consistent with N-body simulations of interacting systems, where there is gas mixing triggered by the interaction, archival Halpha Fabry-Perot data cubes of NGC 92 have not shown a velocity gradient along the tail of this galaxy, which under certain assumptions could be interpreted as a lack o...

  17. Massive envelopes and filaments in the NGC 3603 star forming region

    CERN Document Server

    Hummel, C A; Galvan-Madrid, R; Koribalski, B S

    2015-01-01

    The formation of massive stars and their arrival on the zero-age main-sequence occurs hidden behind dense clouds of gas and dust. In the giant Hii region NGC 3603, the radiation of a young cluster of OB stars has dispersed dust and gas in its vicinity. At a projected distance of 2:5 pc from the cluster, a bright mid-infrared (mid-IR) source (IRS 9A) had been identified as a massive young stellar object (MYSO), located on the side of a molecular clump (MM2) of gas facing the cluster. We investigated the physical conditions in MM2, based on APEX sub-mm observations using the SABOCA and SHFI instruments, and archival ATCA 3 mm continuum and CS spectral line data. We resolved MM2 into several compact cores, one of them closely associated with IRS 9A. These are likely infrared dark clouds as they do not show the typical hot-core emission lines and are mostly opaque against the mid-IR background. The compact cores have masses of up to several hundred times the solar mass and gas temperatures of about 50 K, without ...

  18. The depletion of water during dispersal of planet-forming disk regions

    CERN Document Server

    Banzatti, A; Salyk, C; Herczeg, G; van Dishoeck, E F; Blake, G A

    2016-01-01

    We present a new velocity-resolved survey of 2.9 $\\mu$m spectra of hot H$_2$O and OH gas emission from protoplanetary disks, obtained with CRIRES at the VLT ($\\Delta v \\sim$ 3 km s$^{-1}$). With the addition of archival Spitzer-IRS spectra, this is the most comprehensive spectral dataset of water vapor emission from disks ever assembled. We provide line fluxes at 2.9-33 $\\mu$m that probe from disk radii of $\\sim0.05$ au out to the region across the water snow line. With a combined dataset for 55 disks, we find a new correlation between H$_2$O line fluxes and the radius of CO gas emission as measured in velocity-resolved 4.7 $\\mu$m spectra (R$_{\\rm co}$), which probes molecular gaps in inner disks. We find that H$_2$O emission disappears from 2.9 $\\mu$m (hotter water) to 33 $\\mu$m (colder water) as R$_{\\rm co}$ increases and expands out to the snow line radius. These results suggest that the infrared water spectrum is a tracer of inside-out water depletion within the snow line. It also helps clarifying an unso...

  19. Interferometric Mapping of Magnetic Fields in Star-forming Regions II. NGC2024 FIR5

    CERN Document Server

    Lai, S P; Girart, J M; Rao, R; Lai, Shih-Ping; Crutcher, Richard M.; Girart, Jose M.; Rao, Ramprasad

    2001-01-01

    We present the first interferometric polarization maps of the NGC2024 FIR5 molecular core obtained with the BIMA array at approximately 2 arcsec resolution. We measure an average position angle of -60+-6 degrees in the main core of FIR5 and 54+-9 degrees in the eastern wing of FIR5. The morphology of the polarization angles in the main core of FIR5 suggests that the field lines are parabolic with a symmetry axis approximately parallel to the major axis of the putative disk in FIR5, which is consistent with the theoretical scenario that the gravitational collapse pulled the field lines into an hour-glass shape. The polarization percentage decreases toward regions with high intensity and close to the center of the core, suggesting that the dust alignment efficiency may decrease at high density. The plane-of-sky field strength can be estimated with the modified Chandrasekhar-Fermi formula, and the small dispersion of the polarization angles in FIR5 suggests that the magnetic field is strong ($\\gtrsim$ 2mG) and p...

  20. Tracing the potential planet-forming regions around seven pre-main-sequence stars

    CERN Document Server

    Schegerer, A A; Hummel, C A; Quanz, S P; Richichi, A

    2009-01-01

    We investigate the nature of the innermost regions of seven circumstellar disks around pre-main-sequence stars. Our object sample contains disks apparently at various stages of their evolution. Both single stars and spatially resolved binaries are considered. In particular, we search for inner disk gaps as proposed for several young stellar objects. When analyzing the underlying dust population in the atmosphere of circumstellar disks, the shape of the 10um feature is investigated. We performed interferometric observations in N band 8-13um with MIDI using baseline lengths of between 54m and 127m. The data analysis is based on radiative-transfer simulations using the Monte Carlo code MC3D by modeling simultaneously the SED, N band spectra, and interferometric visibilities. Correlated and uncorrelated N band spectra are compared to investigate the radial distribution of the dust composition of the disk atmosphere. Spatially resolved mid-infrared emission was detected in all objects. For four objects, the observ...

  1. The molecular environment of the massive star forming region NGC 2024: Multi CO transition analysis

    CERN Document Server

    Emprechtinger, M; Simon, R; Wieching, G; Volgenau, N H; Bielau, F; Graf, U U; Guesten, R; Honingh, C E; Jacobs, K; Rabanus, D; Stutzki, J; Wyrowski, F

    2009-01-01

    NGC 2024, a sites of massive star formation, have complex internal structures caused by cal heating by young stars, outflows, and stellar winds. These complex cloud structures lead to intricate emission line shapes. The goal of this paper is to show that the complex line shapes of 12 CO lines in NGC 2024 can be explained consistently with a model, whose temperature and velocity structure are based on the well-established scenario of a PDR and the Blister model. We present velocity-resolved spectra of seven CO lines ranging from J=3 to J=13, and we combined these data with CO high-frequency data from the ISO satellite. We find that the bulk of the molecular cloud associated with NGC 2024 consists of warm (75 K) and dense (9e5 cm-3) gas. An additional hot (~ 300 K) component, located at the interface of the HII region and the molecular cloud, is needed to explain the emission of the high-J CO lines. Deep absorption notches indicate that very cold material (20 K) exists in front of the warm material, too. A temp...

  2. Entrainment Mechanisms for Outflows in the L1551 Star-Forming Region

    CERN Document Server

    Stojimirovi'c, I; Snell, R L; Bally, J; Stojimirovi\\'c, Irena; Narayanan, Gopal; Snell, Ronald L.; Bally, John

    2006-01-01

    We present high sensitivity 12/13CO(1-0) molecular line maps covering the full extent of the parsec scale L1551 molecular outflow, including the redshifted east-west (EW) flow. We also present 12CO(3-2) data that extends over a good fraction of the area mapped in the 1-0 transition. We compare the molecular data to widefield, narrow-band optical emission in H$\\alpha$. While there are multiple outflows in the L1551 cloud, the main outflow is oriented at 50\\arcdeg position angle and appears to be driven by embedded source(s) in the central IRS 5 region. The 3-2 data indicate that there may be molecular emission associated with the L1551 NE jet, within the redshifted lobe of main outflow. We have also better defined the previously known EW flow and believe we have identified its blueshifted counterpart. We further speculate that the origin of the EW outflow lies near HH 102. We use velocity dependent opacity correction to estimate the mass and the energy of the outflow. The resulting mass spectral indices from o...

  3. Star forming activity in the H II regions associated with IRAS 17160-3707 complex

    CERN Document Server

    Nandakumar, G; Vig, S; Tej, A; Ghosh, S K; Ojha, D K

    2016-01-01

    We present a multiwavelength investigation of star formation activity towards the southern H II regions associated with IRAS 17160-3707, located at a distance of 6.2 kpc with a bolometric luminosity of 830000 Lsun.The ionised gas distribution and dust clumps in the parental molecular cloud are examined in detail using measurements at infrared, submillimeter and radio wavelengths.The radio continuum images at 1280 and 610 MHz obtained using Giant Metrewave Radio Telescope reveal the presence of multiple compact sources as well as nebulous emission.At submillimeter wavelengths, we identify seven dust clumps and estimate their physical properties like temperature: 24 - 30 K, mass: 300 - 4800 Msun and luminosity: 900 - 31700 Lsun using modified blackbody fits to the spectral energy distributions between 70 and 870 um.We find 24 young stellar objects in the mid-infrared, with few of them coincident with the compact radio sources.The spectral energy distributions of young stellar objects have been fitted by the Rob...

  4. The RMS Survey: Ammonia and water maser analysis of massive star forming regions

    CERN Document Server

    Urquhart, J S; Figura, C C; Moore, T J T; Lumsden, S L; Hoare, M G; Oudmaijer, R D; Mottram, J C; Davies, B; Dunham, M K

    2011-01-01

    The Red MSX Source (RMS) survey has identified a sample of ~1200 massive young stellar objects (MYSOs), compact and ultra compact HII regions from a sample of ~2000 MSX and 2MASS colour selected sources. We have used the 100 m Green Bank telescope to search for 22-24 GHz water maser and ammonia (1,1), (2,2) and (3,3) emission towards ~600 RMS sources located within the northern Galactic plane. We have identified 308 H2O masers which corresponds to an overall detection rate of ~50%. Abridged: We detect ammonia emission towards 479 of these massive young stars, which corresponds to ~80%. Ammonia is an excellent probe of high density gas allowing us to measure key parameters such as gas temperatures, opacities, and column densities, as well as providing an insight into the gas kinematics. The average kinetic temperature, FWHM line width and total NH3 column density for the sample are approximately 22 K, 2 km/s and 2x10^{15} cm^{-2}, respectively. We find that the NH3 (1,1) line width and kinetic temperature are ...

  5. SiO outflows in high-mass star forming regions: A potential chemical clock?

    CERN Document Server

    López-Sepulcre, A; Cesaroni, R; Codella, C; Schuller, F; Bronfman, L; Carey, S J; Menten, K M; Molinari, S; Noriega-Crespo, A

    2010-01-01

    Some theoretical models propose that O-B stars form via accretion, in a similar fashion to low-mass stars. Jet-driven molecular outflows play an important role in this scenario, and their study can help to understand the process of high-mass star formation and the different evolutionary phases involved. Observations towards low-mass protostars so far favour an evolutionary picture in which jets are always associated with Class 0 objects while more evolved Class I/II objects show less evidence of powerful jets. The present study aims at checking whether an analogous picture can be found in the high-mass case. The IRAM 30-m telescope (Spain) has been used to perform single-pointing SiO(2-1) and (3-2) observations towards a sample of 57 high-mass molecular clumps in different evolutionary stages. Continuum data at different wavelengths, from mid-IR to 1.2 mm, have been gathered to build the spectral energy distributions of all the clumps and estimate their bolometric luminosities. SiO emission at high velocities...

  6. THE EFFECTS OF EPISODIC STAR FORMATION ON THE FUV-NUV COLORS OF STAR FORMING REGIONS IN OUTER DISKS

    Energy Technology Data Exchange (ETDEWEB)

    Barnes, Kate L.; Van Zee, Liese [Department of Astronomy, Indiana University, Bloomington, IN 47405 (United States); Dowell, Jayce D., E-mail: barneskl@astro.indiana.edu, E-mail: vanzee@astro.indiana.edu, E-mail: jdowell@unm.edu [Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131 (United States)

    2013-09-20

    We run stellar population synthesis models to examine the effects of a recently episodic star formation history (SFH) on UV and Hα colors of star forming regions. Specifically, the SFHs we use are an episodic sampling of an exponentially declining star formation rate (SFR; τ model) and are intended to simulate the SFHs in the outer disks of spiral galaxies. To enable comparison between our models and observational studies of star forming regions in outer disks, we include in our models sensitivity limits that are based on recent deep UV and Hα observations in the literature. We find significant dispersion in the FUV-NUV colors of simulated star forming regions with frequencies of star formation episodes of 1 × 10{sup –8} to 4 × 10{sup –9} yr{sup –1}. The dispersion in UV colors is similar to that found in the outer disk of nearby spiral galaxies. As expected, we also find large variations in L{sub H{sub α}}/L{sub FUV}. We interpret our models within the context of inside-out disk growth, and find that a radially increasing τ and decreasing metallicity with an increasing radius will only produce modest FUV-NUV color gradients, which are significantly smaller than what is found for some nearby spiral galaxies. However, including moderate extinction gradients with our models can better match the observations with steeper UV color gradients. We estimate that the SFR at which the number of stars emitting FUV light becomes stochastic is ∼2 × 10{sup –6} M{sub ☉} yr{sup –1}, which is substantially lower than the SFR of many star forming regions in outer disks. Therefore, we conclude that stochasticity in the upper end of the initial mass function is not likely to be the dominant cause of dispersion in the FUV-NUV colors of star forming regions in outer disks. Finally, we note that if outer disks have had an episodic SFH similar to that used in this study, this should be taken into account when estimating gas depletion timescales and modeling chemical

  7. Asymmetric introgression between sympatric molestus and pipiens forms of Culex pipiens (Diptera: Culicidae in the Comporta region, Portugal

    Directory of Open Access Journals (Sweden)

    Côrte-Real Ana R

    2009-11-01

    Full Text Available Abstract Background Culex pipiens L. is the most widespread mosquito vector in temperate regions. This species consists of two forms, denoted molestus and pipiens, that exhibit important behavioural and physiological differences. The evolutionary relationships and taxonomic status of these forms remain unclear. In northern European latitudes molestus and pipiens populations occupy different habitats (underground vs. aboveground, a separation that most likely promotes genetic isolation between forms. However, the same does not hold in southern Europe where both forms occur aboveground in sympatry. In these southern habitats, the extent of hybridisation and its impact on the extent of genetic divergence between forms under sympatric conditions has not been clarified. For this purpose, we have used phenotypic and genetic data to characterise Cx. pipiens collected aboveground in Portugal. Our aims were to determine levels of genetic differentiation and the degree of hybridisation between forms occurring in sympatry, and to relate these with both evolutionary and epidemiological tenets of this biological group. Results Autogeny and stenogamy was evaluated in the F1 progeny of 145 individual Cx. pipiens females. Bayesian clustering analysis based on the genotypes of 13 microsatellites revealed two distinct genetic clusters that were highly correlated with the alternative traits that define pipiens and molestus. Admixture analysis yielded hybrid rate estimates of 8-10%. Higher proportions of admixture were observed in pipiens individuals suggesting that more molestus genes are being introgressed into the pipiens form than the opposite. Conclusion Both physiological/behavioural and genetic data provide evidence for the sympatric occurrence of molestus and pipiens forms of Cx. pipiens in the study area. In spite of the significant genetic differentiation between forms, hybridisation occurs at considerable levels. The observed pattern of asymmetric

  8. An infrared-submillimeter study of star-forming regions selected by the ISOSS 170um survey

    CERN Document Server

    Hennemann, M; Krause, O; Lemke, D

    2008-01-01

    Using the ISOPHOT Serendipity Survey (ISOSS) at 170um a sample of galactic star-forming regions exhibiting very cold dust temperatures ( 100 M_sun) has been established. We characterise the star-forming content of five regions that were selected as potential sites for early stage high-mass star formation using SCUBA (JCMT) and Spitzer observations. In every region we identify one to four submillimeter clumps with projected sizes between 0.1 and 0.4 pc. The dust temperatures range from 11.6 to 21.3 K and the estimated clump masses are 2 to 166 M_sun. Towards the majority of submillimeter peaks we find point sources in the near- to mid-infrared. Most are interpreted as low-mass young stellar objects but we also detect very red sources. They probably represent very young and deeply embedded protostars that continue to accrete clump material and may reach higher masses. Several candidate intermediate-mass proto- or pre-main-sequence stars embedded in the clumps are identified. A subset of four clumps may be massi...

  9. The interrelationship of dune forming processes and the occurrence of wetlands and peatbogs in the Holy Cross Mountains Region

    Science.gov (United States)

    Jaskowski, B.

    2003-04-01

    Dunes of the Holy Cross Mts. Region were formed, like those in other regions of Poland, in the Late Vistulian and were transformed during the different Holocene periods. Numerous factors were influential in the distribution of dunes in the Holy Cross Mts. Region such as relief, drainage pattern, distribution and thickness of deposits susceptible to eolian processes, depth of groundwater level and density of plants. In a number places the phenomena of encroaching complexes dunes, eolian cover sands in river valleys and the damming up of riverflows were observed. In newly created water reservoirs and wetlands organic sediments were deposited. These phenomena crated a modification in drainage pattern. Detailed investigations have determined that the phenomena are related to neotectonic activity of a basement complex. Dunes encroachment in river valleys causing damming of flow happened to occur on lines runnig transverse to the tectonic elevations. In the light of radiocarbon dating the organic sediments of the water reservoirs and wetlands were formed in the Late Vistulian period.

  10. Insights from Synthetic Star-forming Regions - III. Calibration of Measurement Techniques of Star-formation Rates

    CERN Document Server

    Koepferl, Christine M; Dale, James E

    2016-01-01

    Through an extensive set of realistic synthetic observations (produced in Paper I), we assess in this part of the paper series (Paper III) how the choice of observational techniques affects the measurement of star-formation rates (SFRs) in star-forming regions. We test the accuracy of commonly used techniques and construct new methods to extract the SFR, so that these findings can be applied to measure the SFR in real regions throughout the Milky Way. We investigate diffuse infrared SFR tracers such as those using 24 {\\mu}m, 70 {\\mu}m and total infrared emission, which have been previously calibrated for global galaxy scales. We set up a toy model of a galaxy and show that the infrared emission is consistent with the intrinsic SFR using extra-galactic calibrated laws (although the consistency does not prove their reliability). For local scales, we show that these techniques produce completely unreliable results for single star-forming regions, which are governed by different characteristic timescales. We show...

  11. Magnetized Converging Flows toward the Hot Core in the Intermediate/High-mass Star-forming Region NGC 6334 V

    Science.gov (United States)

    Juárez, Carmen; Girart, Josep M.; Zamora-Avilés, Manuel; Tang, Ya-Wen; Koch, Patrick M.; Liu, Hauyu Baobab; Palau, Aina; Ballesteros-Paredes, Javier; Zhang, Qizhou; Qiu, Keping

    2017-07-01

    We present Submillimeter Array (SMA) observations at 345 GHz toward the intermediate/high-mass cluster-forming region NGC 6334 V. From the dust emission we spatially resolve three dense condensations, the brightest one presenting the typical chemistry of a hot core. The magnetic field (derived from the dust polarized emission) shows a bimodal converging pattern toward the hot core. The molecular emission traces two filamentary structures at two different velocities, separated by 2 km s-1, converging to the hot core and following the magnetic field distribution. We compare the velocity field and the magnetic field derived from the SMA observations with magnetohydrodynamic simulations of star-forming regions dominated by gravity. This comparison allows us to show how the gas falls in from the larger-scale extended dense core (˜0.1 pc) of NGC 6334 V toward the higher-density hot core region (˜0.02 pc) through two distinctive converging flows dragging the magnetic field, whose strength seems to have been overcome by gravity.

  12. Sulfur-Bearing Molecules In Massive Star-Forming Regions: Observations Of OCS, CS, H2S and SO

    CERN Document Server

    Li, Juan; Zhu, Qingfeng; Zhang, Jiangshui; Li, Di

    2015-01-01

    We studied sulfur chemistry of massive star-forming regions through single-dish submillimeter spectroscopy. OCS, O13CS, 13CS, H2S and SO transitions were observed toward a sample of massive star-forming regions with embedded UCH II or CH II regions. These sources could be divided into H II-hot core and H II-only sources based on their CH3CN emission. Our results show that the OCS line of thirteen sources is optically thick, with optical depth ranging from 5 to 16. Column densities of these molecules were computed under LTE conditions. CS column densities were also derived using its optically thin isotopologue 13CS. H2S is likely to be the most abundant gas-phase sulfuretted molecules in hot assive cores. Both the column density and abundance of sulfur-bearing molecules decrease significantly from H II-hot core to H II-only sources. Ages derived from hot core models appear to be consistent with star-formation theories, suggesting that abundance ratios of [CS]/[SO], [SO]/[OCS] and [OCS]/[CS] could be used as ch...

  13. Water maser variability over 20 years in a large sample of star-forming regions: the complete database

    CERN Document Server

    Felli, M; Cesaroni, R; Codella, C; Comoretto, G; Di Franco, S; Massi, F; Moscadelli, L; Nesti, R; Olmi, L; Palagi, F; Panella, D; Valdettaro, R

    2007-01-01

    Context. Water vapor emission at 22 GHz from masers associated with star-forming regions is highly variable. Aims. We present a database of up to 20 years of monitoring of a sample of 43 masers within star-forming regions. The sample covers a large range of luminosities of the associated IRAS source and is representative of the entire population of H2O masers of this type. The database forms a good starting point for any further study of H2O maser variability. Methods. The observations were obtained with the Medicina 32-m radiotelescope, at a rate of 4-5 observations per year. Results. To provide a database that can be easily accessed through the web, we give for each source: plots of the calibrated spectra, the velocity-time-flux density plot, the light curve of the integrated flux, the lower and upper envelopes of the maser emission, the mean spectrum, and the rate of the maser occurrence as a function of velocity. Figures for just one source are given in the text for representative purposes. Figures for al...

  14. Radio and infrared recombination studies of the southern massive star-forming region G333.6-0.2

    CERN Document Server

    Fujiyoshi, T; Caswell, J L; Moore, T J T; Lumsden, S L; Aitken, D K; Roche, P F; Fujiyoshi, Takuya; Smith, Craig H.; Caswell, James L.; Moore, Toby J. T.; Lumsden, Stuart L.; Aitken, David K.; Roche, Patrick F.

    2006-01-01

    We present high spatial resolution radio and near-infrared hydrogen recombination line observations of the southern massive star-forming region G333.6-0.2. The 3.4-cm continuum peak is found slightly offset from the infrared source. The H90alpha spectra show for the first time a double peak profile at some positions. The complex velocity structure may be accounted for by champagne outflows, which may also explain the offset between the radio and infrared sources. The 2.17-um Brackett gamma image and H90alpha map are combined to construct an extinction map which shows a trend probably set by the blister nature of the HII region. The total number of Lyman continuum photons in the central 50-arcsec is estimated to be equivalent to that emitted by up to 19 O7V stars.

  15. Irradiated shocks in the W28 A2 massive star-forming region: a site for cosmic rays acceleration?

    CERN Document Server

    Gusdorf, A; Gerin, M; Guesten, R

    2015-01-01

    The formation of massive stars play a crucial role in galaxies from numerous points of view. The protostar generates a strong ultraviolet radiation field that ionizes its surroundings, and it drives powerful shock waves in the neighbouring medium in the form of jets and bipolar outflows, whose structure can be partially organized by local, strong magnetic field. Such an ejection activity locally modifies the interstellar chemistry, contributing to the cycle of matter. It also significantly participates to the energetic balance of galaxies. In the latter stages of massive star formation, the protostar is surrounded by an ultra-compact HII region, and irradiates its bipolar outflows, where an intrinsically strong magnetic field structure is associated to the generally high densities. In the HII region, or in the bipolar outflows, the question of in situ cosmic rays acceleration can then be raised by the simultaneous presence of strong magnetic fields, significant ionization of the matter, and mechanical energy ...

  16. H II regions, infrared dark molecular clouds and the local geometry of the Milky Way's nuclear star-forming ring

    CERN Document Server

    Liszt, H S

    2009-01-01

    To interpret the galactic center H II region complexes as constituents of a barred galaxy's nuclear star-forming ring, we compare 18cm VLA radiocontinuumm, $8-22\\mu$ MSX IR and 2.6mm BTL and ARO12m CO emission in the inner few hundred pc. Galactic center H II regions are comparable in their IR appearance, luminosity and SED to M17 or N!0, but the IR light distribution is strongly modified by extinction at 8-22$\\mu$, locally and overall. In Sgr B2 at $l > 0.6$\\degr strong radio H II regions are invisible in the IR. In two favorable cases, extinction from individual galactic center molecular clouds is shown to have $\\tau \\ga 1$ at 8-22$\\mu$ independent of wavelength. The gas kinematics are mostly rotational but with systematic $\\pm 30-50$ \\kms non-circular motion. Sgr B and C both show the same shell and high-velocity cap structure. The H II regions lie in a slightly-inclined ring of radius $\\approx$ 180 pc (1.2\\degr) whose near side appears at higher latitude and lower velocity and contains Sgr B. Sgr C is on ...

  17. Nearby supernova host galaxies from the CALIFA Survey: I. Sample, data analysis, and correlation to star-forming regions

    CERN Document Server

    Galbany, L; Mourão, A M; Rodrigues, M; Flores, H; García-Benito, R; Mast, D; Mendoza, M A; Sánchez, S F; Badenes, C; Barrera-Ballesteros, J; Bland-Hawthorn, J; Falcón-Barroso, J; García-Lorenzo, B; Gomes, J M; Delgado, R M González; Kehrig, C; Lyubenova, M; López-Sánchez, A R; de Lorenzo-Cáceres, A; Marino, R A; Meidt, S; Mollá, M; Papaderos, P; Pérez-Torres, M A; Rosales-Ortega, F F; van de Ven, G

    2014-01-01

    [Abridged] We use optical IFS of nearby SN host galaxies provided by the CALIFA Survey with the goal of finding correlations in the environmental parameters at the location of different SN types. We recover the sequence in association of different SN types to the star-forming regions by using several indicators of the ongoing and recent SF related to both the ionized gas and the stellar populations. While the total ongoing SF is on average the same for the three SN types, SNe Ibc/IIb tend to happen closer to star-forming regions and occur in higher SF density locations compared to SNe II and SNe~Ia, the latter showing the weakest correlation. SNe~Ia host galaxies have on average masses that are $\\sim$0.3-0.8~dex higher than CC SNe hosts due to a larger fraction of old stellar populations in the SNe~Ia hosts. Using the recent SN~Ia delay-time distribution and the SFHs of the galaxies, we show that the SN~Ia hosts in our sample should presently produce a factor 2 more SNe~Ia than the CC~SN hosts. Since both typ...

  18. X-RAY AND RADIO OBSERVATIONS OF THE MASSIVE STAR-FORMING REGION IRAS 20126+4104

    Energy Technology Data Exchange (ETDEWEB)

    Montes, V. A.; Hofner, P.; Anderson, C.; Rosero, V. [Physics Department, New Mexico Tech, 801 Leroy Place, Socorro, NM 87801 (United States)

    2015-08-15

    We present results from Chandra ACIS-I and Karl G. Jansky Very Large Array 6 cm continuum observations of the IRAS 20126+4104 massive star-forming region. We detect 150 X-ray sources within the 17′ × 17′ ACIS-I field, and a total of 13 radio sources within the 9.′2 primary beam at 4.9 GHz. Among these observtions are the first 6 cm detections of the central sources reported by Hofner et al., namely, I20N1, I20S, and I20var. A new variable radio source is also reported. Searching the 2MASS archive, we identified 88 near-infrared (NIR) counterparts to the X-ray sources. Only four of the X-ray sources had 6 cm counterparts. Based on an NIR color–color analysis and on the Besançon simulation of Galactic stellar populations, we estimate that approximately 80 X-ray sources are associated with this massive star-forming region. We detect an increasing surface density of X-ray sources toward the massive protostar and infer the presence of a cluster of at least 43 young stellar objects within a distance of 1.2 pc from the massive protostar.

  19. Four highly luminous massive star forming regions in the Norma Spiral Arm.: I. Molecular gas and dust observations

    CERN Document Server

    Garay, Guido; Bronfman, Leonardo; May, Jorge; Chavarria, Luis; Nyman, Lars-Ake

    2009-01-01

    We report molecular line and dust continuum observations, made with the SEST telescope, towards four young high-mass star forming regions associated with highly luminous (L> 6x10^5 Lsun) IRAS sources (15290-5546, 15502-5302, 15567-5236 and 16060-5146). Molecular emission was mapped in lines of CS (J=2-1, 3-2 and 5-4), SiO (J=2-1 and 3-2), CH3OH (Jk=3k-2k and 2k-1k), and C34S (J=3-2). In addition, single spectra at the peak position were taken in the CO, 13CO and C18O (J=1-0) lines. We find that the luminous star forming regions are associated with molecular gas and dust structures with radii of typically 0.5 pc, masses of ~5x10^3 Msun, column densities of ~5x10^{23} cm^{-2}, molecular hydrogen densities of typically ~2x10^5 cm^{-3} and dust temperatures of ~40 K. The 1.2 mm dust continuum observations further indicate that the cores are centrally condensed, having radial density profiles with power-law indices in the range 1.6-1.9. We find that under these conditions dynamical friction by the gas plays an imp...

  20. Multidimensional Chemical Modeling of Young Stellar Objects. II. Irradiated Outflow Walls in a High-Mass Star-Forming Region

    Science.gov (United States)

    Bruderer, S.; Benz, A. O.; Doty, S. D.; van Dishoeck, E. F.; Bourke, T. L.

    2009-07-01

    Observations of the high-mass star-forming region AFGL 2591 reveal a large abundance of CO+, a molecule known to be enhanced by far-ultraviolet (FUV) and X-ray irradiation. In chemical models assuming a spherically symmetric envelope, the volume of gas irradiated by protostellar FUV radiation is very small due to the high extinction by dust. The abundance of CO+ is thus underpredicted by orders of magnitude. In a more realistic model, FUV photons can escape through an outflow region and irradiate gas at the border to the envelope. Thus, we introduce the first two-dimensional axisymmetric chemical model of the envelope of a high-mass star-forming region to explain the CO+ observations as a prototypical FUV tracer. The model assumes an axisymmetric power-law density structure with a cavity due to the outflow. The local FUV flux is calculated by a Monte Carlo radiative transfer code taking scattering on dust into account. A grid of precalculated chemical abundances, introduced in the first part of this series of papers, is used to quickly interpolate chemical abundances. This approach allows us to calculate the temperature structure of the FUV-heated outflow walls self-consistently with the chemistry. Synthetic maps of the line flux are calculated using a raytracer code. Single-dish and interferometric observations are simulated and the model results are compared to published and new JCMT and Submillimeter Array (SMA) observations. The two-dimensional model of AFGL 2591 is able to reproduce the JCMT single-dish observations and also explains the nondetection by the SMA. We conclude that the observed CO+ line flux and its narrow width can be interpreted by emission from the warm and dense outflow walls irradiated by protostellar FUV radiation.

  1. Pre-main sequence accretion in the low metallicity Galactic star-forming region Sh 2-284

    CERN Document Server

    Kalari, V M

    2014-01-01

    We present optical spectra of pre-main sequence (PMS) candidates around the H$\\alpha$ region taken with the Southern African Large Telescope, SALT, in the low metallicity ($Z$) Galactic region Sh 2-284, which includes the open cluster Dolidze 25 with an atypical low metallicity of $Z$ $\\sim$ 1/5 $Z_{\\odot}$. It has been suggested on the basis of both theory and observations that PMS mass-accretion rates, $\\dot M_{\\rm{acc}}$, are a function of $Z$. We present the first sample of spectroscopic estimates of mass-accretion rates for PMS stars in any low-$Z$ star-forming region. Our data-set was enlarged with literature data of H$\\alpha$ emission in intermediate-resolution R-band spectroscopy. Our total sample includes 24 objects spanning a mass range between 1 - 2 $M_{\\odot}$ and with a median age of approximately 3.5 Myr. The vast majority (21 out of 24) show evidence for a circumstellar disk on the basis of 2MASS and Spitzer infrared photometry. We find $\\dot M_{\\rm{acc}}$ in the 1 - 2 $M_{\\odot}$ interval to d...

  2. The BLAST View of the Star Forming Region in Aquila (ell=45deg,b=0deg)

    CERN Document Server

    Rivera-Ingraham, Alana; Bock, James J; Chapin, Edward L; Devlin, Mark J; Dicker, Simon R; Griffin, Matthew; Gundersen, Joshua O; Halpern, Mark; Hargrave, Peter C; Hughes, David H; Klein, Jeff; Marsden, Gaelen; Martin, Peter G; Mauskopf, Philip; Netterfield, Calvin B; Olmi, Luca; Patanchon, Guillaume; Rex, Marie; Scott, Douglas; Semisch, Christopher; Truch, Matthew D P; Tucker, Carole; Tucker, Gregory S; Viero, Marco P; Wiebe, Donald V

    2010-01-01

    We have carried out the first general submillimeter analysis of the field towards GRSMC 45.46+0.05, a massive star forming region in Aquila. The deconvolved 6 deg^2 (3\\degree X 2\\degree) maps provided by BLAST in 2005 at 250, 350, and 500 micron were used to perform a preliminary characterization of the clump population previously investigated in the infrared, radio, and molecular maps. Interferometric CORNISH data at 4.8 GHz have also been used to characterize the Ultracompact HII regions (UCHIIRs) within the main clumps. By means of the BLAST maps we have produced an initial census of the submillimeter structures that will be observed by Herschel, several of which are known Infrared Dark Clouds (IRDCs). Our spectral energy distributions of the main clumps in the field, located at ~7 kpc, reveal an active population with temperatures of T~35-40 K and masses of ~10^3 Msun for a dust emissivity index beta=1.5. The clump evolutionary stages range from evolved sources, with extended HII regions and prominent IR ...

  3. Infrared and radio study of star forming regions associated with IRAS 19111+1048 and IRAS 19110+1045

    CERN Document Server

    Vig, S; Kulkarni, V K; Ojha, D K; Verma, R P

    2006-01-01

    A multiwavelength study of the star forming regions associated with IRAS 19111+1048 and IRAS 19110+1045 has been carried out. These have been simultaneously mapped in two far infrared bands at lambda_eff ~ 130 and 200 micron with ~1' angular resolution using the TIFR 1-m balloon borne telescope. The radio emission from the ionised gas of these regions has been imaged at 1280, 610 and 325 MHz using the Giant Metrewave Radio Telescope, India. A total of 20 compact radio sources have been detected from the high resolution radio map of IRAS 19111+1048 at 1280 MHz. Assuming these sources to represent exciting zero age main sequence (ZAMS) stars, the initial mass function is found to be quite steep, with the power law index of 5.3+-0.5 for the mass range 14 < m/M_sun < 33. The spectral types of the ZAMS stars inferred independently from the radio and NIR measurements match very well for a good fraction of the radio sources having NIR counterparts. For IRAS 19110+1045 region, seven radio sources have been dete...

  4. Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

    CERN Document Server

    Okada, Yoko; Murakami, Noriko; Ootsubo, Takafumi; Takahashi, Hidenori; Yasuda, Akiko; Ishihara, Daisuke; Kaneda, Hidehiro; Kataza, Hirokazu; Nakagawa, Takao; Onaka, Takashi

    2009-01-01

    We investigate the structure of the interstellar medium (ISM) and identify the location of possible embedded excitation sources from far-infrared (FIR) line and mid-infrared continuum emission maps. We carried out imaging spectroscopic observations of four giant Galactic star-forming regions with the Fourier Transform Spectrometer (FTS) onboard AKARI. We obtained [OIII] 88 micron and [CII] 158 micron line intensity maps of all the regions: G3.270-0.101, G333.6-0.2, NGC3603, and M17. For G3.270-0.101, we obtained high-spatial-resolution [OIII] 88 micron line-emission maps and a FIR continuum map for the first time, which imply that [OIII] 88 micron emission identifies the excitation sources more clearly than the radio continuum emission. In G333.6-0.2, we found a local [OIII] 88 micron emission peak, which is indicative of an excitation source. This is supported by the 18 micron continuum emission, which is considered to trace the hot dust distribution. For all regions, the [CII] 158 micron emission is distrib...

  5. HH 223: a parsec-scale H2 outflow in the star-forming region L723

    CERN Document Server

    Lopez, R; Gomez, G; Estalella, R; Carrasco-Gonzalez, C

    2010-01-01

    The dark cloud Lynds 723 (L723) is a low-mass star-forming region where one of the few known cases of a quadrupolar CO outflow has been reported. Two recent works have found that the radio continuum source VLA 2, towards the centre of the CO outflow, is actually a multiple system of young stellar objects (YSOs). Several line-emission nebulae that lie projected on the east-west CO outflow were detected in narrow-band Halpha and [SII] images. The spectra of the knots are characteristic of shock-excited gas (Herbig-Haro spectra), with supersonic blueshifted velocities, which suggests an optical outflow also powered by the VLA 2 YSO system of L723. We imaged a field of ~5' X 5' centred on HH 223, which includes the whole region of the quadrupolar CO outflow with nir narrow-band filters . The H2 line-emission structures appear distributed over a region of 5.5' (0.5 pc for a distance of 300 pc) at both sides of the VLA 2 YSO system, with an S-shape morphology, and are projected onto the east-west CO outflow. Most o...

  6. First evidence for molecular interfaces between outflows and ambient cloud in high-mass star forming regions?

    CERN Document Server

    Codella, C; Viti, S; Williams, D A

    2006-01-01

    We present new observations of the CepA-East region of massive star formation and describe an extended and dynamically distinct feature not previously recognised. This feature is present in emission from H2CS, OCS, CH3OH, and HDO at -5.5 km/s, but is not traced by conventional tracers of star forming regions H2S, SO2, SO, CS. The feature is extended up to at least 0.1 pc. We show that the feature is neither a hot core nor a shocked outflow. However, the chemistry of the feature is consistent with predictions of a model of an eroding interface between a fast wind and a dense core; mixing between the two media occurs in the interface on a timescale of 10-50 years. If these observations are confirmed by detailed maps and by detections in species also predicted to be abundant (e.g. HCO+, H2CO, and NH3) this feature would be the first detection of such an interface in regions of massive star formation. An important implication of the model is that a significant reservoir of sulfur in grain mantles is required to b...

  7. A microscopic investigation of the transition form factor in the region of collective multipole excitations of stable and unstable nuclei

    Energy Technology Data Exchange (ETDEWEB)

    Papakonstantinou, P. [Technische Univ. Darmstadt (Germany). Inst. fuer Kernphysik]|[Athens Univ. (Greece). Physics Dept., Nuclear and Particle Physics Section; Mavrommatis, E. [Athens Univ. (Greece). Physics Dept., Nuclear and Particle Physics Section; Wambach, J.; Ponomarev, V.Y. [Technische Univ. Darmstadt (Germany). Inst. fuer Kernphysik

    2004-12-20

    We have used a self-consistent Skyrme-Hartree-Fock plus continuum-RPA model to study the low-multipole response of stable and neutron/proton-rich Ni and Sn isotopes. We focus on the momentum-transfer dependence of the strength distribution, as it provides information on the structure of excited nuclear states and in particular on the variations of the transition form factor (TFF) with the energy. Our results show, among other things, that the TFF may show significant energy dependence in the region of the isoscalar giant monopole resonance and that the TFF corresponding to the threshold strength in the case of neutron-rich nuclei is different compared to the one corresponding to the respective giant resonance. Perspectives are given for more detailed future investigations. (orig.)

  8. Age gradients in the stellar populations of massive star forming regions based on a new stellar chronometer

    Energy Technology Data Exchange (ETDEWEB)

    Getman, Konstantin V.; Feigelson, Eric D.; Kuhn, Michael A.; Broos, Patrick S.; Townsley, Leisa K.; Luhman, Kevin L. [Department of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802 (United States); Naylor, Tim [School of Physics and Astronomy, University of Exeter, Stocker Road, Exeter, EX4 4QL (United Kingdom); Povich, Matthew S. [Department of Physics and Astronomy, California State Polytechnic University, 3801 West Temple Avenue, Pomona, CA 91768 (United States); Garmire, Gordon P. [Huntingdon Institute for X-ray Astronomy, LLC, 10677 Franks Road, Huntingdon, PA 16652 (United States)

    2014-06-01

    A major impediment to understanding star formation in massive star-forming regions (MSFRs) is the absence of a reliable stellar chronometer to unravel their complex star formation histories. We present a new estimation of stellar ages using a new method that employs near-infrared (NIR) and X-ray photometry, Age {sub JX} . Stellar masses are derived from X-ray luminosities using the L{sub X} -M relation from the Taurus cloud. J-band luminosities are compared to mass-dependent pre-main-sequence (PMS) evolutionary models to estimate ages. Age {sub JX} is sensitive to a wide range of evolutionary stages, from disk-bearing stars embedded in a cloud to widely dispersed older PMS stars. The Massive Young Star-Forming Complex Study in Infrared and X-ray (MYStIX) project characterizes 20 OB-dominated MSFRs using X-ray, mid-infrared, and NIR catalogs. The Age {sub JX} method has been applied to 5525 out of 31,784 MYStIX Probable Complex Members. We provide a homogeneous set of median ages for over 100 subclusters in 15 MSFRs; median subcluster ages range between 0.5 Myr and 5 Myr. The important science result is the discovery of age gradients across MYStIX regions. The wide MSFR age distribution appears as spatially segregated structures with different ages. The Age {sub JX} ages are youngest in obscured locations in molecular clouds, intermediate in revealed stellar clusters, and oldest in distributed populations. The NIR color index J – H, a surrogate measure of extinction, can serve as an approximate age predictor for young embedded clusters.

  9. On the onset of secondary stellar generations in giant star-forming regions and massive star clusters

    Energy Technology Data Exchange (ETDEWEB)

    Palouš, J.; Wünsch, R. [Astronomical Institute, Academy of Sciences of the Czech Republic, Boční II 1401, 14131 Prague (Czech Republic); Tenorio-Tagle, G. [Instituto Nacional de Astrofísica Optica y Electrónica, AP 51, 72000 Puebla (Mexico)

    2014-09-10

    Here we consider the strong evolution experienced by the matter reinserted by massive stars, both in giant star-forming regions driven by a constant star formation rate and in massive and coeval superstar clusters. In both cases we take into consideration the changes induced by stellar evolution on the number of massive stars, the number of ionizing photons, and the integrated mechanical luminosity of the star-forming regions. The latter is at all times compared with the critical luminosity that defines, for a given size, the lower mechanical luminosity limit above which the matter reinserted via strong winds and supernova explosions suffers frequent and recurrent thermal instabilities that reduce its temperature and pressure and inhibit its exit as part of a global wind. Instead, the unstable reinserted matter is compressed by the pervasive hot gas, and photoionization maintains its temperature at T ∼ 10{sup 4} K. As the evolution proceeds, more unstable matter accumulates and the unstable clumps grow in size. Here we evaluate the possible self-shielding of thermally unstable clumps against the UV radiation field. Self-shielding allows for a further compression of the reinserted matter, which rapidly develops a high-density neutral core able to absorb in its outer skin the incoming UV radiation. Under such conditions the cold (T ∼ 10 K) neutral cores soon surpass the Jeans limit and become gravitationally unstable, creating a new stellar generation with the matter reinserted by former massive stars. We present the results of several calculations of this positive star formation feedback scenario promoted by strong radiative cooling and mass loading.

  10. Challenging shock models with SOFIA OH observations in the high-mass star-forming region Cepheus A

    CERN Document Server

    Gusdorf, A; Menten, K M; Flower, D R; Forets, G Pineau des; Codella, C; Csengeri, T; Gomez-Ruiz, A I; Heyminck, S; Jacobs, K; Kristensen, L E; Leurini, S; Requena-Torres, M A; Wampfler, S F; Wiesemeyer, H; Wyrowski, F

    2015-01-01

    OH is a key molecule in H2O chemistry, a valuable tool for probing physical conditions, and an important contributor to the cooling of shock regions. OH participates in the re-distribution of energy from the protostar towards the surrounding ISM. Our aim is to assess the origin of the OH emission from the Cepheus A massive star-forming region and to constrain the physical conditions prevailing in the emitting gas. We thus want to probe the processes at work during the formation of massive stars. We present spectrally resolved observations of OH towards the outflows of Cepheus A with the GREAT spectrometer onboard the SOFIA telescope. Three triplets were observed at 1834.7 GHz, 1837.8 GHz, and 2514.3 GHz (163.4, 163.1, and 119.2 microns), at angular resolutions of 16.3", 16.3", and 11.9", respectively. We present the CO (16-15) spectrum at the same position. We compared the integrated intensities in the redshifted wings to shock models. The two triplets near 163 microns are detected in emission with blending h...

  11. Dense gas and exciting sources of the molecular outflow in the AFGL 437 star-forming region

    CERN Document Server

    Manjarrez, G; de Gregorio-Monsalvo, I

    2011-01-01

    We present Very Large Array (VLA) high resolution observations of the NH3(1,1) and NH3(2,2) molecular transitions towards the high mass star forming region AFGL 437. Our aim was to investigate if the poorly collimated CO molecular outflow previously detected in the region is the result of a projection effect, with no intrinsic bipolarity, as suggested by Gomez et al. We complemented our observations with radio continuum archived data from the VLA at 2 and 3.6 cm, and with unpublished public data at 450 {\\mu}m taken with Submillimetre Common-User Bolometer Array at the James Clerk Maxwell Telescope. Ammonia emission was found mainly in three clumps located at the south and east of the position of the compact infrared cluster of AFGL 437, where the CO outflow seemed to have its origin. One of the NH3(1,1) clumps coincides with the maximum of NH3(2,2) and with a local peak of emission at 450 {\\mu}m. A near infrared source (s11) is also found at that position. Our continuum map at 2 cm shows extended elongated em...

  12. Disk-outflow models as applied to high mass star forming regions through methanol and water maser observations

    CERN Document Server

    Farmer, Hontas

    2013-01-01

    As the recent publication by Breen et al (2013) found Class II methanol masers are exclusively associated with high mass star forming regions. Based on the positions of the Class I and II methanol and H$_{2}$O masers, UC H II regions and 4.5 $\\mu$m infrared sources, and the center velocities ($v_{\\text{LSR}}$) of the Class I methanol and H$_{2}$O masers, compared to the $v_{\\text{LSR}}$ of the Class II methanol masers, we propose three disk-outflow models that may be traced by methanol masers. In all three models, we have located the Class II methanol maser near the protostar, and the Class I methanol maser in the outflow, as is known from observations during the last twenty years. In our first model, the H$_{2}$O masers trace the linear extent of the outflow. In our second model, the H$_{2}$O masers are located in a circumstellar disk. In our third model, the H$_{2}$O masers are located in one or more outflows near the terminating shock where the outflow impacts the ambient interstellar medium. Together, the...

  13. Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4

    CERN Document Server

    Hagele, Guillermo F; Perez-Montero, Enrique; Diaz, Angeles I; Cardaci, Monica V; Firpo, Veronica; Terlevich, Elena; Terlevich, Roberto

    2011-01-01

    We analyze high signal-to-noise spectrophotometric observations acquired simultaneously with TWIN, a double-arm spectrograph, from 3400 to 10400 \\AA of three star-forming regions in the HII galaxy SDSS J165712.75+321141.4. We have measured four line temperatures: Te([OIII]), Te([SIII]), Te([OII]), and Te([SII]), with high precision, rms errors of order 2%, 5%, 6% and 6%, respectively, for the brightest region, and slightly worse for the other two. The temperature measurements allowed the direct derivation of ionic abundances of oxygen, sulphur, nitrogen, neon and argon. We have computed CLOUDY tailor-made models which reproduce the O2+ measured thermal and ionic structures within the errors in the three knots, with deviations of only 0.1 dex in the case of O+ and S2+ ionic abundances. In the case of the electron temperature and the ionic abundances of S+/H+, we find major discrepancies which could be consequence of the presence of colder diffuse gas. The star formation history derived using STARLIGHT shows a ...

  14. The structure and early evolution of massive star forming regions - Substructure in the infrared dark cloud SDC13

    CERN Document Server

    McGuire, Catherine; Peretto, Nicolas; Zhang, Qizhou; Traficante, Alessio; Avison, Adam; Jimenez-Serra, Izaskun

    2016-01-01

    Investigations into the substructure of massive star forming regions are essential for understanding the observed relationships between core mass distributions and mass distributions in stellar clusters, differentiating between proposed mechanisms of massive star formation. We study the substructure in the two largest fragments (i.e. cores) MM1 and MM2, in the infrared dark cloud complex SDC13. As MM1 appears to be in a later stage of evolution than MM2, comparing their substructure provides an insight in to the early evolution of massive clumps. We report the results of high resolution SMA dust continuum observations towards MM1 and MM2. Combining these data with Herschel observations, we carry out RADMC-3D radiative transfer modelling to characterise the observed substructure. SMA continuum data indicates 4 sub-fragments in the SDC13 region. The nature of the second brightest sub-fragment (B) is uncertain as it does not appear as prominent at the lower MAMBO resolution or at radio wavelengths. Statistical a...

  15. CHESS, Chemical Herschel surveys of star forming regions:Peering into the protostellar shock L1157-B1

    CERN Document Server

    Lefloch, B; Codella, C; Melnick, G; Cernicharo, J; Caux, E; Benedettini, M; Boogert, A; Caselli, P; Ceccarelli, C; Gueth, F; Hily-Blant, P; Lorenzani, A; Neufeld, D; Nisini, B; Pacheco, S; Pagani, L; Pardo, J R; Parise, B; Salez, M; Schuster, K; Viti, S; Bacmann, A; Baudry, A; Bell, T; Bergin, E A; Blake, G; Bottinelli, S; Castets, A; Comito, C; Coutens, A; Crimier, N; Dominik, C; Demyk, K; Encrenaz, P; Falgarone, E; Fuente, A; Gerin, M; Goldsmith, P; Helmich, F; Hennebelle, P; Henning, T; Herbst, E; Jacq, T; Kahane, C; Kama, M; Klotz, A; Langer, W; Lis, D; Lord, S; Maret, S; Pearson, J; Phillips, T; Saraceno, P; Schilke, P; Tielens, X; van der Tak, F; van der Wiel, M; Vastel, C; Wakelam, V; Walters, A; Wyrowski, F; Yorke, H; Bachiller, R; Borys, C; De Lange, G; Delorme, Y; Kramer, C; Larsson, B; Lai, R; Maiwald, F W; Martin-Pintado, J; Mehdi, I; Ossenkopf, V; Siegel, P; Stutzki, J; Wunsch, J H

    2010-01-01

    The outflow driven by the low-mass class 0 protostar L1157 is the prototype of the so-called chemically active outflows. The bright bowshock B1 in the southern outflow lobe is a privileged testbed of magneto-hydrodynamical (MHD) shock models, for which dynamical and chemical processes are strongly interdependent. We present the first results of the unbiased spectral survey of the L1157-B1 bowshock, obtained in the framework of the key program "Chemical Herschel Surveys of Star Forming Regions" (CHESS). The main aim is to trace the warm and chemically enriched gas and to infer the excitation conditions in the shock region. The CO 5-4 and H2O lines have been detected at high-spectral resolution in the unbiased spectral survey of the HIFI-Band 1b spectral window (555-636 GHz), presented by Codella et al. in this volume. Complementary ground-based observations in the submm window help establish the origin of the emission detected in the main-beam of HIFI, and the physical conditions in the shock.}{Both lines exhi...

  16. Microstructure and kinematics of H2O masers in the massive star forming region IRAS 06061+2151

    CERN Document Server

    Motogi, K; Sorai, K; Habe, A; Honma, M; Imai, H; Yamauchi, A; Kobayashi, H; Fujisawa, K; Omodaka, T; Takaba, H; Shibata, K M; Minamidani, T; Wakamatsu, K; Sudou, H; Kawai, E; Koyama, Y

    2008-01-01

    We have made multi-epoch VLBI observations of H2O maser emission in the massive star forming region IRAS 06061+2151 with the Japanese VLBI network (JVN) from 2005 May to 2007 October. The detected maser features are distributed within an 1\\arcsec$\\times$1\\arcsec (2000 au$\\times$2000 au at the source position) around the ultra-compact H {\\small\\bf II} region seen in radio continuum emission. Their bipolar morphology and expanding motion traced through their relative proper motions indicate that they are excited by an energetic bipolar outflow. Our three-dimensional model fitting has shown that the maser kinematical structure in IRAS 06061+2151 is able to be explained by a biconical outflow with a large opening angle ($>$ 50\\degr). The position angle of the flow major axis coincides very well with that of the large scale jet seen in 2.1$\\:\\mu\\rmn{m}$ hydrogen emission. This maser geometry indicates the existence of dual structures composed of a collimated jet and a less collimated massive molecular flow. We hav...

  17. The Star-Forming Region NGC 346 in the Small Magellanic Cloud with Hubble Space Telescope ACS Observations I. Photometry

    CERN Document Server

    Gouliermis, D A; Brandne, W; Henning, T; Henning, Th.

    2006-01-01

    We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V ~ 11 to V ~ 28 mag, including all stellar types from the most massive young stars to faint lower main sequence and pre-main sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: The stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete st...

  18. The change in the chemical form of copper in fly ash in a suitable temperature region for de novo synthesis

    Energy Technology Data Exchange (ETDEWEB)

    Takaoka, M.; Shiono, A.; Nishimura, K.; Takeda, N.; Oshita, K.; Matsumoto, T.; Harada, H. [Kyoto Univ. (Japan). Dept. of Urban and Environ. Eng.; Yamamoto, T. [Tokyo Inst. of Tech., Yokohama (Japan). Chemical Resources Lab.; Uruga, T. [JASRI, Hyogo (Japan); Tanaka, T. [Kyoto Univ. (Japan). Dept. of Molecular Eng.

    2004-09-15

    Copper chloride as an important catalyst generates many polychlorinated dibenzo-p-dioxins and dibenzofurans (PCDD/DFs) and related compounds in heat experiments involving model fly ash. We investigated the chemical forms of copper in actual fly ash before heating experiments and discuss the relationship that we discovered between the copper species Cu(OH){sub 2}, CuO, and Cu(OH){sub 2}.CuCO{sub 3}.H{sub 2}O and the formation of chlorinated aromatics in actual fly ash using X-ray absorption near-edge spectroscopy (XANES). Other results using model fly ash differ from ours. The thermal stabilities of these compounds are not high, so these compounds might not exist in fly ash in the temperature region suitable for de novo synthesis. Therefore, we conducted in situ XANES experiments using actual fly ash and two models of fly ash to understand the behavior of copper in fly ash in the temperature region suitable for de novo synthesis.

  19. Integral Field Spectroscopy of Local LCBGs: NGC 7673, a case study. Physical properties of star-forming regions

    CERN Document Server

    Castillo-Morales, A; Pérez-Gallego, J; Guzmán, R; Muñoz-Mateos, J C; Zamorano, J; Sánchez, S F

    2010-01-01

    Physical properties of the star-forming regions in the local Luminous Compact Blue Galaxy NGC 7673 are studied in detail using 3D spectroscopic data taken with the PPAK IFU at the 3.5-m telescope in CAHA. We derive integrated and spatially resolved properties such as extinction, star formation rate and metallicity for this galaxy. Our data show an extinction map with maximum values located at the position of the main clumps of star formation showing small spatial variations (E(B-V)_{t}=0.12-0.21 mag). We derive a H\\alpha-based SFR for this galaxy of 6.2 \\pm 0.8 M_{\\odot}/yr in agreement with the SFR derived from infrared and radio continuum fluxes. The star formation is located mainly in clumps A, B, C and F. Different properties measured in clump B makes this region peculiar. We find the highest H\\alpha luminosity with a SFR surface density of 0.5 M_{\\odot}yr^{-1}kpc^{-2} in this clump. In our previous work, the kinematic analysis for this galaxy shows an asymmetrical ionized gas velocity field with a kinema...

  20. Probing the Microscopic with the Macroscopic: from Properties of Star Cluster Systems to Properties of Cluster-Forming Regions

    Science.gov (United States)

    Parmentier, G.

    To understand how systems of star clusters have reached their presently observed properties constitutes a powerful probe into the physics of cluster formation, without needing to resort to high spatial resolution observations of individual cluster-forming regions (CFRg) in distant galaxies. In this contribution I focus on the mass-radius relation of CFRgs, how it can be uncovered by studying the gas expulsion phase of forming star clusters, and what the implications are. I demonstrate that, through the tidal field impact upon exposed star clusters, the CFRg mass-radius relation rules cluster infant weight-loss in dependence of cluster mass. The observational constraint of a time-invariant slope for the power-law young cluster mass function is robustly satisfied by CFRgs with a constant mean volume density. In contrast, a constant mean surface density would be conducive to the preferential destruction of high-mass clusters. A purely dynamical line-of-reasoning leads therefore to a conclusion consistent with star formation a process driven by a volume density threshold. Developing this concept further, properties of molecular clumps and CFRgs naturally get dissociated. This allows to understand: (i) why the star cluster mass function is steeper than the molecular cloud/clump mass function; (ii) the presence of a massive star formation limit in the mass-size space of molecular structures.

  1. Precision Measurements of the Proton Electromagnetic Form Factors in the Time-Like Region and Vector Meson Spectroscopy

    CERN Multimedia

    2002-01-01

    The aim of this experiment is to measure with precision the electromagnetic form factors of the proton in the time-like region via the reaction: .ce @*p @A e|+e|- with antiprotons of momenta between 0 and 2 GeV/c. Up to @= 800 MeV/c, a continuous energy scan in @= 2 MeV (@]s) bins will be performed. The form factor !G(E)! and !G(M)! will be determined separately since large statistics can be collected with LEAR antiproton beams, so that angular distributions can be obtained at many momenta.\\\\ \\\\ In addition, e|+e|- pairs produced via the reaction: .ce @*p @A V|0 + neutrals, .ce !@A e|+e|- where the antiprotons are at rest, will be detected allowing the vector meson mass spectrum between @= 1 GeV and @= 1.7 GeV to be obtained with high statistics and in one run. \\\\ \\\\ The proposed apparatus consists of a central detector, surrounded by a gas Cerenkov counter, wire chambers, hodoscopes, and an electromagnetic calorimeter. The central detector consists of several layers of proportional chambers around a liquid-h...

  2. The Star Formation in Radio Survey: GBT 33 GHz Observations of Nearby Galaxy Nuclei and Extranuclear Star-Forming Regions

    CERN Document Server

    Murphy, E J; Mason, B S; Condon, J J; Schinnerer, E; Aniano, G; Armus, L; Helou, G; Turner, J L; Jarrett, T H

    2012-01-01

    We present 33\\,GHz photometry of 103 galaxy nuclei and extranuclear star-forming complexes taken with the Green Bank Telescope (GBT) as part of the Star Formation in Radio Survey (SFRS). Among the sources without evidence for an AGN, and also having lower frequency radio data, we find a median thermal fraction at 33GHz of ~76% with a dispersion of ~24%. For all sources resolved on scales 90%. This suggests that the rest-frame 33GHz emission provides a sensitive measure of the ionizing photon rate from young star-forming regions, thus making it a robust star formation rate indicator. Taking the 33GHz star formation rates as a reference, we investigate other empirical calibrations relying on different combinations of warm 24\\mu m dust, total infrared (IR; 8-1000\\mu m), H\\alpha\\ line, and far-UV continuum emission. The recipes derived here generally agree with others found in the literature, albeit with a large dispersion that most likely stems from a combination of effects. Comparing the 33GHz to total IR flux ...

  3. Water in star-forming regions with Herschel: highly excited molecular emission from the NGC 1333 IRAS 4B outflow

    CERN Document Server

    Herczeg, Gregory J; Bruderer, Simon; Kristensen, Lars E; van Dishoeck, Ewine F; Jørgensen, Jes K; Visser, Ruud; Wampfler, Susanne F; Bergin, Edwin A; Yildiz, Umut A; Pontoppidan, Klaus M; Gracia-Carpio, Javier

    2011-01-01

    During the embedded phase of pre-main sequence stellar evolution, a disk forms from the dense envelope while an accretion-driven outflow carves out a cavity within the envelope. Highly excited H2O emission in spatially unresolved Spitzer/IRS spectra of a low-mass Class 0 object, NGC 1333 IRAS 4B, has previously been attributed to the envelope-disk accretion shock but could instead be produced in an outflow. As part of the survey of low-mass sources in the Water in Star Forming Regions with Herschel (WISH-LM) program, we used Herschel/PACS to obtain a far-IR spectrum and several Nyquist-sampled spectral images with to determine the origin of excited H2O emission from NGC 1333 IRAS 4B. The spectrum has high signal-to-noise in a rich forest of H2O, CO, and OH lines, providing a near-complete census of far-IR molecular emission from a Class 0 protostar. The excitation diagrams for the three molecules all require fits with two excitation temperatures, indicating the presence of two physical components. The highly ...

  4. TADPOL: A 1.3 mm Survey of Dust Polarization in Star-forming Cores and Regions

    CERN Document Server

    Hull, Charles L H; Kwon, Woojin; Bower, Geoffrey C; Carpenter, John M; Crutcher, Richard M; Fiege, Jason D; Franzmann, Erica; Hakobian, Nicholas S; Heiles, Carl; Houde, Martin; Hughes, A Meredith; Lamb, James W; Looney, Leslie W; Marrone, Daniel P; Matthews, Brenda C; Pillai, Thushara; Pound, Marc W; Rahman, Nurur; Sandell, Göran; Stephens, Ian W; Tobin, John J; Vaillancourt, John E; Volgenau, N H; Wright, Melvyn C H

    2013-01-01

    We present results of 1.3 mm dust polarization observations toward 29 star-forming cores and 8 high-mass star-forming regions, mapped with ~2.5'' resolution at CARMA as part of the TADPOL survey. We discuss three main findings in this work: (1) A subset of the sources have consistent magnetic field orientations between the large scales measured by single-dish submillimeter telescopes (with ~20'' resolution) and the small scales measured by CARMA. Those same sources also tend to have higher fractional polarizations than the sources with inconsistent large-to-small-scale fields, possibly because there is less twisting of the B-fields to reduce the polarization fraction. This suggests that in at least some sources, the B-fields play a role in regulating the infall of material over many orders of magnitude, all the way down to ~1000AU protostellar envelope scales. (2) Even in the sources with consistent large-to-small-scale field orientations, the magnetic fields in the cores are misaligned with outflows from the...

  5. A Hi-GAL study of the high-mass star-forming region G29.96-0.02

    CERN Document Server

    Beltran, M T; Cesaroni, R; Schisano, E; Elia, D; Molinari, S; Di Giorgio, A M; Kirk, J M; Mottram, J C; Pestalozzi, M; Testi, L; Thompson, M A

    2013-01-01

    Context. G29.96-0.02 is a high-mass star-forming cloud observed at 70, 160, 250, 350, and 500 microns as part of the Herschel survey of the Galactic Plane during the Science Demonstration Phase. Aims. We wish to conduct a far-infrared study of the sources associated with this star-forming region by estimating their physical properties and evolutionary stage, and investigating the clump mass function, the star formation efficiency and rate in the cloud. Methods. We have identified the Hi-GAL sources associated with the cloud, searched for possible counterparts at centimeter and infrared wavelengths, fitted their spectral energy distribution and estimated their physical parameters. Results. A total of 198 sources have been detected in all 5 Hi-GAL bands, 117 of which are associated with 24 microns emission and 87 of which are not associated with 24 microns emission. We called the former sources 24 microns-bright and the latter ones 24 microns-dark. The [70-160] color of the 24 microns-dark sources is smaller th...

  6. Age Gradients in the Stellar Populations of Massive Star Forming Regions Based on a New Stellar Chronometer

    CERN Document Server

    Getman, Konstantin V; Kuhn, Michael A; Broos, Patrick S; Townsley, Leisa K; Naylor, Tim; Povich, Matthew S; Luhman, Kevin L; Garmire, Gordon P

    2014-01-01

    A major impediment to understanding star formation in massive star forming regions (MSFRs) is the absence of a reliable stellar chronometer to unravel their complex star formation histories. We present a new estimation of stellar ages using a new method that employs near-infrared (NIR) and X-ray photometry, AgeJX. Stellar masses are derived from X-ray luminosities using the Lx - Mass relation from the Taurus cloud. J-band luminosities are compared to mass-dependent pre-main-sequence evolutionary models to estimate ages. AgeJX is sensitive to a wide range of evolutionary stages, from disk-bearing stars embedded in a cloud to widely dispersed older pre-main sequence stars. The MYStIX (Massive Young Star-Forming Complex Study in Infrared and X-ray) project characterizes 20 OB-dominated MSFRs using X-ray, mid-infrared, and NIR catalogs. The AgeJX method has been applied to 5525 out of 31,784 MYStIX Probable Complex Members. We provide a homogeneous set of median ages for over a hundred subclusters in 15 MSFRs; me...

  7. A GALEX-BASED SEARCH FOR THE SPARSE YOUNG STELLAR POPULATION IN THE TAURUS-AURIGAE STAR FORMING REGION

    Energy Technology Data Exchange (ETDEWEB)

    Gómez de Castro, Ana I.; Lopez-Santiago, Javier; López-Martínez, Fatima; Sánchez, Néstor; Sestito, Paola; Gestoso, Javier Yañez [AEGORA Research Group, Universidad Complutense de Madrid, Plaza de Ciencias 3, E-28040 Madrid (Spain); De Castro, Elisa; Cornide, Manuel [Fac. de CC. Físicas, Universidad Complutense de Madrid, Plaza de Ciencias 1, E-28040 Madrid (Spain)

    2015-02-01

    In this work, we identify 63 bona fide new candidates to T Tauri stars (TTSs) in the Taurus-Auriga region, using its ultraviolet excess as our baseline. The initial data set was defined from the GALEX all sky survey (AIS). The GALEX satellite obtained images in the near-ultraviolet (NUV) and far-ultraviolet (FUV) bands where TTSs show a prominent excess compared with main-sequence or giants stars. GALEX AIS surveyed the Taurus-Auriga molecular complex, as well as a fraction of the California Nebula and the Perseus complex; bright sources and dark clouds were avoided. The properties of TTSs in the ultraviolet (GALEX), optical (UCAC4), and infrared (2MASS) have been defined using the TTSs observed with the International Ultraviolet Explorer reference sample. The candidates were identified by means of a mixed ultraviolet-optical-infrared excess set of colors; we found that the FUV-NUV versus J–K color-color diagram is ideally suited for this purpose. From an initial sample of 163,313 bona fide NUV sources, a final list of 63 new candidates to TTSs in the region was produced. The search procedure has been validated by its ability to detect all known TTSs in the area surveyed: 31 TTSs. Also, we show that the weak-lined TTSs are located in a well-defined stripe in the FUV-NUV versus J–K diagram. Moreover, in this work, we provide a list of TTSs photometric standards for future GALEX-based studies of the young stellar population in star forming regions.

  8. The effects of density-dependent form factors for (e, e'p) reaction in quasi-elastic region

    Energy Technology Data Exchange (ETDEWEB)

    Kim, K.S. [Korea Aerospace University, School of Liberal Arts and Science, Goyang (Korea, Republic of); Cheoun, Myung-Ki [Soongsil University, Department of Physics, Seoul (Korea, Republic of); Kim, Hungchong [Kookmin University, Department of General Education, Seoul (Korea, Republic of); So, W.Y. [Kangwon National University at Dogye, Department of Radiological Science, Samcheok (Korea, Republic of)

    2016-04-15

    Within the framework of a relativistic single particle model, the effects of density-dependent electromagnetic form factors on the exclusive (e, e'p) reaction are investigated in the quasi-elastic region. The density-dependent electromagnetic form factors are generated from a quark-meson coupling model and used to calculate the cross sections in two different densities, either at the normal density of ρ{sub 0} ∝ 0.15 fm{sup -3} or at the lower density, 0.5ρ{sub 0}. Then these cross sections are analyzed in the two different kinematics: One is that the momentum of the outgoing nucleon is along the momentum transfer. The other is that the angle between the momentum of the outgoing nucleon and the momentum transfer is varied at fixed magnitude of the momentum of the outgoing nucleon. Our theoretical differential reduced cross sections are compared with the NIKHEF data for the {sup 208}Pb(e, e'p) reaction, which is related to the probability that a bound nucleon from a given orbit can be knocked-out of the nucleus. The effects of the density-dependent form factors increase the differential cross sections for both knocked-out proton and neutron by an amount of a few percent. Moreover they are shown to be almost the same within only a few percent, i.e., nearly independent of the shell location of knockout nucleons. These results are quite consistent with the characteristics of double magic nuclei which have relatively sharp smearing in the density distribution. (orig.)

  9. Prevention of liver fibrosis by triple helix-forming oligodeoxyribonucleotides targeted to the promoter region of type I collagen gene.

    Science.gov (United States)

    Koilan, Subramaniyan; Hamilton, David; Baburyan, Narina; Padala, Mythili K; Weber, Karl T; Guntaka, Ramareddy V

    2010-10-01

    Hepatic fibrosis leading to cirrhosis remains a global health problem. The most common etiologies are alcoholism and viral infections. Liver fibrosis is associated with major changes in both quantity and composition of extracellular matix and leads to disorganization of the liver architecture and irreversible damage to the liver function. As of now there is no effective therapy to control fibrosis. The end product of fibrosis is abnormal synthesis and accumulation of type I collagen in the extracellular matrix, which is produced by activated stellate or Ito cells in the damaged liver. Therefore, inhibition of transcription of type I collagen should in principle inhibit its production and accumulation in liver. Normally, DNA exists in a duplex form. However, under some circumstances, DNA can assume triple helical (triplex) structures. Intermolecular triplexes, formed by the addition of a sequence-specific third strand to the major groove of the duplex DNA, have the potential to serve as selective gene regulators. Earlier, we demonstrated efficient triplex formation between the exogenously added triplex-forming oligodeoxyribonucleotides (TFOs) and a specific sequence in the promoter region of the COL1A1 gene. In this study we used a rat model of liver fibrosis, induced by dimethylnitrosamine, to test whether these TFOs prevent liver fibrosis. Our results indicate that both the 25-mer and 18-mer TFOs, specific for the upstream nucleotide sequence from -141 to -165 (relative to the transcription start site) in the 5' end of collagen gene promoter, effectively prevented accumulation of liver collagen and fibrosis. We also observed improvement in liver function tests. However, mutations in the TFO that eliminated formation of triplexes are ineffective in preventing fibrosis. We believe that these TFOs can be used as potential antifibrotic therapeutic molecules.

  10. Cannibalization and Rebirth in the NGC 5387 System. I. The Stellar Stream and Star-forming Region

    Science.gov (United States)

    Beaton, Rachael L.; Martínez-Delgado, David; Majewski, Steven R.; D'Onghia, Elena; Zibetti, Stefano; Gabany, R. Jay; Johnson, Kelsey E.; Blanton, Michael; Verbiscer, Anne

    2014-08-01

    We have identified a low surface brightness stellar stream from visual inspection of Sloan Digital Sky Survey (SDSS) imaging for the edge-on, spiral galaxy NGC 5387. An optically blue overdensity coincident with the stream intersection with the NGC 5387 disk was also identified in SDSS and in the Galaxy Evolution Explorer Deep Imaging Survey contributing 38% of the total far-UV integrated flux from NGC 5387. Deeper optical imaging was acquired with the Vatican Advanced Technology Telescope that confirmed the presence of both features. The stellar stream is red in color, (B - V) = 0.7, has a stellar mass of 6 × 108 M ⊙, which implies a 1:50 merger ratio, has a circular radius, R circ ~ 11.7 kpc, formed in ~240 Myr, and the progenitor had a total mass of ~4 × 1010 M ⊙. Spectroscopy from LBT+MODS1 was used to determine that the blue overdensity is at the same redshift as NGC 5387, consists of young stellar populations (~10 Myr), is metal-poor (12 + log (O/H) = 8.03), and is forming stars at an enhanced rate (~1-3 M ⊙ yr-1). The most likely interpretations are that the blue overdensity is (1) a region of enhanced star formation in the outer disk of NGC 5387 induced by the minor accretion event or (2) the progenitor of the stellar stream experiencing enhanced star formation. Additional exploration of these scenarios is presented in a companion paper. Based on observations with the VATT: the Alice P. Lennon Telescope and the Thomas J. Bannan Astrophysics Facility.

  11. TADPOL: A 1.3 mm SURVEY OF DUST POLARIZATION IN STAR-FORMING CORES AND REGIONS

    Energy Technology Data Exchange (ETDEWEB)

    Hull, Charles L. H.; Plambeck, Richard L.; Bower, Geoffrey C.; Heiles, Carl [Astronomy Department and Radio Astronomy Laboratory, University of California, Berkeley, CA 94720-3411 (United States); Kwon, Woojin [SRON Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen (Netherlands); Carpenter, John M.; Lamb, James W.; Pillai, Thushara [Department of Astronomy, California Institute of Technology, 1200 E. California Blvd., MC 249-17, Pasadena, CA 91125 (United States); Crutcher, Richard M.; Hakobian, Nicholas S.; Looney, Leslie W. [Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W Green Street, Urbana, IL 61801 (United States); Fiege, Jason D.; Franzmann, Erica [Department of Physics and Astronomy, University of Manitoba, Winnipeg, MB, R3T 2N2 (Canada); Houde, Martin [Department of Physics and Astronomy, University of Western Ontario, London, ON, N6A 3K7 (Canada); Hughes, A. Meredith [Van Vleck Observatory, Astronomy Department, Wesleyan University, 96 Foss Hill Drive, Middletown, CT 06459 (United States); Marrone, Daniel P. [Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States); Matthews, Brenda C. [Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Rd., Victoria, BC, V8P 5C2 (Canada); Pound, Marc W. [Astronomy Department and Laboratory for Millimeter-wave Astronomy, University of Maryland, College Park, MD 20742 (United States); Rahman, Nurur [Physics Department, University of Johannesburg, C1-Lab 140, P.O. Box 524, Auckland Park 2006 (South Africa); Sandell, Göran, E-mail: chat@astro.berkeley.edu [SOFIA Science Center, Universities Space Research Association, NASA Ames Research Center, Moffett Field, CA 94035 (United States); and others

    2014-07-01

    We present λ 1.3 mm Combined Array for Research in Millimeter-wave Astronomy observations of dust polarization toward 30 star-forming cores and eight star-forming regions from the TADPOL survey. We show maps of all sources, and compare the ∼2.''5 resolution TADPOL maps with ∼20'' resolution polarization maps from single-dish submillimeter telescopes. Here we do not attempt to interpret the detailed B-field morphology of each object. Rather, we use average B-field orientations to derive conclusions in a statistical sense from the ensemble of sources, bearing in mind that these average orientations can be quite uncertain. We discuss three main findings. (1) A subset of the sources have consistent magnetic field (B-field) orientations between large (∼20'') and small (∼2.''5) scales. Those same sources also tend to have higher fractional polarizations than the sources with inconsistent large-to-small-scale fields. We interpret this to mean that in at least some cases B-fields play a role in regulating the infall of material all the way down to the ∼1000 AU scales of protostellar envelopes. (2) Outflows appear to be randomly aligned with B-fields; although, in sources with low polarization fractions there is a hint that outflows are preferentially perpendicular to small-scale B-fields, which suggests that in these sources the fields have been wrapped up by envelope rotation. (3) Finally, even at ∼2.''5 resolution we see the so-called polarization hole effect, where the fractional polarization drops significantly near the total intensity peak. All data are publicly available in the electronic edition of this article.

  12. Investigation of OH and H2O masers in the star-forming region G 188.946+0.886

    Science.gov (United States)

    Ashimbaeva, N. T.; Colom, P.; Lekht, E. E.; Pashchenko, M. I.; Rudnitskii, G. M.; Tolmachev, A. M.

    2016-10-01

    We present the results of our observations of the maser radio emission source G188.946+0.886 in hydroxyl (OH) molecular lines with the radio telescope of the Nançay Observatory (France) and in the H2O line at λ = 1.35 cm with the RT-22 radio telescope at the Pushchino Observatory (Russia). An emission feature in the 1720-MHz satellite line of the OH ground state has been detected for the first time. The radial velocity of the feature, V LSR = 3.6 km s-1, has a "blue" shift relative to the range of emission velocities in the main 1665- and 1667-MHz OH lines, which is 8-11 km s-1. This suggests a probable connection of the observed feature in the 1720-MHz line with the "blue" wing of the bipolar outflow observed in this region in the CO line. We have estimated the magnetic field strength for three features (0.90 and 0.8 mG for 1665 MHz and 0.25 mG for 1720 MHz) from the Zeeman splitting in the 1665- and 1720-MHz lines. No emission and (or) absorption has been detected in the other 1612-MHz satellite OH line. Three cycles of H2O maser activity have been revealed. The variability is quasi-periodic in pattern. There is a general tendency for the maser activity to decrease. Some clusters of H2O maser spots can form organized structures, for example, chains and other forms.

  13. Cannibalization and rebirth in the NGC 5387 system. I. The stellar stream and star-forming region

    Energy Technology Data Exchange (ETDEWEB)

    Beaton, Rachael L.; Majewski, Steven R.; Johnson, Kelsey E.; Verbiscer, Anne [Department of Astronomy, University of Virginia, Charlottesville, VA 22904 (United States); Martínez-Delgado, David [Max Planck Institut fur Astronomie, D-69117 Heidelberg (Germany); D' Onghia, Elena [Department of Astronomy, University of Wisconsin-Madison, Madison, WI 53706 (United States); Zibetti, Stefano [INAF-Osservatorio Astrofisico di Arcetri, I-50125 Firenze (Italy); Gabany, R. Jay [Black Bird II Observatory, Alder Springs, CA 93602 (United States); Blanton, Michael, E-mail: rbeaton@virginia.edu [Department of Physics, New York University, New York, NY 10003 (United States)

    2014-08-01

    We have identified a low surface brightness stellar stream from visual inspection of Sloan Digital Sky Survey (SDSS) imaging for the edge-on, spiral galaxy NGC 5387. An optically blue overdensity coincident with the stream intersection with the NGC 5387 disk was also identified in SDSS and in the Galaxy Evolution Explorer Deep Imaging Survey contributing 38% of the total far-UV integrated flux from NGC 5387. Deeper optical imaging was acquired with the Vatican Advanced Technology Telescope that confirmed the presence of both features. The stellar stream is red in color, (B – V) = 0.7, has a stellar mass of 6 × 10{sup 8} M{sub ☉}, which implies a 1:50 merger ratio, has a circular radius, R{sub circ} ∼ 11.7 kpc, formed in ∼240 Myr, and the progenitor had a total mass of ∼4 × 10{sup 10} M{sub ☉}. Spectroscopy from LBT+MODS1 was used to determine that the blue overdensity is at the same redshift as NGC 5387, consists of young stellar populations (∼10 Myr), is metal-poor (12 + log (O/H) = 8.03), and is forming stars at an enhanced rate (∼1-3 M{sub ☉} yr{sup –1}). The most likely interpretations are that the blue overdensity is (1) a region of enhanced star formation in the outer disk of NGC 5387 induced by the minor accretion event or (2) the progenitor of the stellar stream experiencing enhanced star formation. Additional exploration of these scenarios is presented in a companion paper.

  14. Challenging shock models with SOFIA OH observations in the high-mass star-forming region Cepheus A

    Science.gov (United States)

    Gusdorf, A.; Güsten, R.; Menten, K. M.; Flower, D. R.; Pineau des Forêts, G.; Codella, C.; Csengeri, T.; Gómez-Ruiz, A. I.; Heyminck, S.; Jacobs, K.; Kristensen, L. E.; Leurini, S.; Requena-Torres, M. A.; Wampfler, S. F.; Wiesemeyer, H.; Wyrowski, F.

    2016-01-01

    Context. OH is a key molecule in H2O chemistry, a valuable tool for probing physical conditions, and an important contributor to the cooling of shock regions around high-mass protostars. OH participates in the re-distribution of energy from the protostar towards the surrounding Interstellar Medium. Aims: Our aim is to assess the origin of the OH emission from the Cepheus A massive star-forming region and to constrain the physical conditions prevailing in the emitting gas. We thus want to probe the processes at work during the formation of massive stars. Methods: We present spectrally resolved observations of OH towards the protostellar outflows region of Cepheus A with the GREAT spectrometer onboard the Stratospheric Observatory for Infrared Astronomy (SOFIA) telescope. Three triplets were observed at 1834.7 GHz, 1837.8 GHz, and 2514.3 GHz (163.4 μm, 163.1 μm between the 2Π1/2 J = 1/2 states, and 119.2 μm, a ground transition between the 2Π3/2 J = 3/2 states), at angular resolutions of 16.̋3, 16.̋3, and 11.̋9, respectively. We also present the CO (16-15) spectrum at the same position. We compared the integrated intensities in the redshifted wings to the results of shock models. Results: The two OH triplets near 163 μm are detected in emission, but with blending hyperfine structure unresolved. Their profiles and that of CO (16-15) can be fitted by a combination of two or three Gaussians. The observed 119.2 μm triplet is seen in absorption, since its blending hyperfine structure is unresolved, but with three line-of-sight components and a blueshifted emission wing consistent with that of the other lines. The OH line wings are similar to those of CO, suggesting that they emanate from the same shocked structure. Conclusions: Under this common origin assumption, the observations fall within the model predictions and within the range of use of our model only if we consider that four shock structures are caught in our beam. Overall, our comparisons suggest that

  15. c-Myc quadruplex-forming sequence Pu-27 induces extensive damage in both telomeric and nontelomeric regions of DNA.

    Science.gov (United States)

    Islam, Md Ashraful; Thomas, Shelia D; Murty, Vundavalli V; Sedoris, Kara J; Miller, Donald M

    2014-03-21

    Quadruplex-forming DNA sequences are present throughout the eukaryotic genome, including in telomeric DNA. We have shown that the c-Myc promoter quadruplex-forming sequence Pu-27 selectively kills transformed cells (Sedoris, K. C., Thomas, S. D., Clarkson, C. R., Muench, D., Islam, A., Singh, R., and Miller, D. M. (2012) Genomic c-Myc quadruplex DNA selectively kills leukemia. Mol. Cancer Ther. 11, 66-76). In this study, we show that Pu-27 induces profound DNA damage, resulting in striking chromosomal abnormalities in the form of chromatid or chromosomal breaks, radial formation, and telomeric DNA loss, which induces γ-H2AX in U937 cells. Pu-27 down-regulates telomeric shelterin proteins, DNA damage response mediators (RAD17 and RAD50), double-stranded break repair molecule 53BP1, G2 checkpoint regulators (CHK1 and CHK2), and anti-apoptosis gene survivin. Interestingly, there are no changes of DNA repair molecules H2AX, BRCA1, and the telomere maintenance gene, hTERT. ΔB-U937, where U937 cells stably transfected with deleted basic domain of TRF2 is partially sensitive to Pu-27 but exhibits no changes in expression of shelterin proteins. However, there is an up-regulation of CHK1, CHK2, H2AX, BRCA1, and survivin. Telomere dysfunction-induced foci assay revealed co-association of TRF1with γ-H2AX in ATM deficient cells, which are differentially sensitive to Pu-27 than ATM proficient cells. Alt (alternating lengthening of telomere) cells are relatively resistant to Pu-27, but there are no significant changes of telomerase activity in both Alt and non-Alt cells. Lastly, we show that this Pu-27-mediated sensitivity is p53-independent. The data therefore support two conclusions. First, Pu-27 induces DNA damage within both telomeric and nontelomeric regions of the genome. Second, Pu-27-mediated telomeric damage is due, at least in part, to compromise of the telomeric shelterin protein complex.

  16. A Study of the Distribution of Star-Forming Regions in Luminous Infrared Galaxies by Means of H$\\alpha$ Imaging Observations

    CERN Document Server

    Hattori, T; Ohtani, H; Sugai, H; Ishigaki, T; Sasaki, M; Hayashi, T; Ozaki, S; Ishii, M; Kawai, A

    2003-01-01

    We performed H-alpha imaging observations of 22 luminous infrared galaxies to investigate how the distribution of star-forming regions in these galaxies is related to galaxy interactions. Based on correlation diagrams between H-alpha flux and continuum emission for individual galaxies, a sequence for the distribution of star-forming regions was found: very compact (~100 pc) nuclear starbursts with almost no star-forming activity in the outer regions (type 1), dominant nuclear starbursts 1 kpc in size and a significant contribution from the outer regions (type 3), and extended starbursts with relatively faint nuclei (type 4). These classes of star-forming region were found to be strongly related to global star-forming properties such as star-formation efficiency, far-infrared color, and dust extinction. There was a clear tendency for the objects with more compact distributions of star-forming regions to show a higher star-formation efficiency and hotter far-infrared color. An appreciable fraction of the sampl...

  17. Community-led local development approach principles implementation when forming a regional local development projects support system in Ukraine

    Directory of Open Access Journals (Sweden)

    Y. G. Udod

    2017-03-01

    Full Text Available The article contains a brief description of the Community-led local development approach (local development under the leadership of the community, CLLD and the main purpose of its use in the European Union. The study indicated periods of the major initiatives to support local development in EU. Moreover the article posted CLLD approach principles’ evolution and the basic principles of the LEADER method and its application in CLLD, which can be applied in Ukraine. Subject to the provisions of the European Economic and Social Committee (EESC for further CLLD-approach distribution the five trends were identified that must be considered when forming a Regional local development projects support system in Ukraine: Multi-fund financing; Unification; Networking and collaboration; Extending the approach; Simplifying the process. The characteristic of the present phase of CLLD-approach, in particular, of the European Network for Rural Development (ENRD, which attaches great importance to the dissemination of the most effective CLLD practices and establish partnerships between communities and territories where the approach is implemented. The study found out the relationship between Community-led local development and Community-driven development (CDD supported by the World Bank.

  18. Trigonometric Distance and Proper Motion of IRAS 20056+3350: Massive Star Forming Region on the Solar Circle

    CERN Document Server

    Burns, Ross A; Handa, Toshihiro; Omodaka, Toshihiro; Nakagawa, Akiharu; Nakanishi, Hiroyuki; Hayashi, Masahiko; Shizugami, Makoto

    2014-01-01

    We report our measurement of the trigonometric distance and proper motion IRAS 20056+3350, obtained from the annual parallax of H2O masers. Our distance of D = 4.69 +0.65-0.51 kpc, which is more than two times larger than the near kinematic distance adopted in the literature, places IRAS 20056+3350 at the leading tip of the Local arm, and proximal to the Solar circle. Using our distance we re-evaluate past observations to reveal IRAS 20056+3350 as a site of massive star formation at a young stage of evolution. This result is consistent with the spectral energy distribution of the source evaluated with published photometric data from UKIDSS, WISE, AKARI, IRAS and sub-millimetre continuum. Both analytical approaches reveal the luminosity of the region to be 2.4 x 10^4 Lo, and suggest that IRAS 20056+3350 is forming an embedded star of 16 Mo. We estimated the proper motion of IRAS 20056+3350 to be ($\\mu_{\\alpha}\\cos\\delta$, $\\mu_{\\delta}$) = ($-2.62\\pm0.33$, $-5.65\\pm0.52$) mas yr$^{-1}$ from the group motion of...

  19. Deconvolution of Images from BLAST 2005: Insight into the K3-50 and IC 5146 Star-Forming Regions

    CERN Document Server

    Roy, Arabindo; Bock, James J; Brunt, Christopher M; Chapin, Edward L; Devlin, Mark J; Dicker, Simon R; France, Kevin; Gibb, Andrew G; Griffin, Matthew; Gundersen, Joshua O; Halpern, Mark; Hargrave, Peter C; Hughes, David H; Klein, Jeff; Marsden, Gaelen; Martin, Peter G; Mauskopf, Philip; Netterfield, Calvin B; Olmi, Luca; Patanchon, Guillaume; Rex, Marie; Scott, Douglas; Semisch, Christopher; Truch, Matthew D P; Tucker, Carole; Tucker, Gregory S; Viero, Marco P; Wiebe, Donald V

    2010-01-01

    We present an implementation of the iterative flux-conserving Lucy-Richardson (L-R) deconvolution method of image restoration for maps produced by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST). We have analyzed its performance and convergence extensively through simulations and cross-correlations of the deconvolved images with available highresolution maps. We present new science results from two BLAST surveys, in the Galactic regions K3-50 and IC 5146, further demonstrating the benefits of performing this deconvolution. We have resolved three clumps within a radius of 4.'5 inside the star-forming molecular cloud containing K3-50. Combining the well-resolved dust emission map with available multi-wavelength data, we have constrained the Spectral Energy Distributions (SEDs) of five clumps to obtain masses (M), bolometric luminosities (L), and dust temperatures (T). The L-M diagram has been used as a diagnostic tool to estimate the evolutionary stages of the clumps. There are close relationsh...

  20. Emergence of recombinant forms in geographic regions with co-circulating HIV subtypes in the dynamic HIV-1 epidemic

    Energy Technology Data Exchange (ETDEWEB)

    Zhang, Ming [Los Alamos National Laboratory; Letiner, Thomas K [Los Alamos National Laboratory; Korber, Bette T [Los Alamos National Laboratory; Foley, Brian [Los Alamos National Laboratory

    2009-01-01

    We have reexamined the subtype designations of {approx}10,000 subtype A, B, C, G, and AG, BC, BF recombinant sequences, and compared the results of the new analysis with their published designations. Intersubtype recombinants dominate HIV epidemics in three different geographical regions. The circulating recombinant from (CRF) CRF02-AG, common in West Central Africa, appears to result from a recombination event that occurred early in the divergence between subtypes A and G, although additional more recent recombination events may have contributed to the breakpoint pattern in this recombinant lineage as well. The Chinese recombinant epidemic strains CRF07 and CRF08, in contrast, result from recent recombinations between more contemporary strains. Nevertheless, CRF07 and CRF08 contributed to many subsequent recombination events. The BF recombinant epidemics in two HIV-1 epicenters in South America are not independent and BF epidemics in South America have an unusually high fraction of unique recombinant forms (URFs) that have each been found only once and carry distinctive breakpoints. Taken together, these analyses reveal a complex and dynamic picture of the current HIV-1 epidemic, and suggest a means of grouping and tracking relationships between viruses through preservation of shared breakpints.

  1. A Survey for New Members of the Taurus Star-Forming Region with the Sloan Digital Sky Survey

    CERN Document Server

    Luhman, K L; Shukla, S J; Loutrel, N P

    2016-01-01

    Previous studies have found that ~1 deg2 fields surrounding the stellar aggregates in the Taurus star-forming region exhibit a surplus of solar-mass stars relative to denser clusters like IC~348 and the Orion Nebula Cluster. To test whether this difference reflects mass segregation in Taurus or a variation in the IMF, we have performed a survey for members of Taurus across a large field (~40 deg2) that was imaged by the Sloan Digital Sky Survey (SDSS). We obtained optical and near-infrared spectra of candidate members identified with those images and the Two Micron All Sky Survey, as well as miscellaneous candidates that were selected with several other diagnostics of membership. We have classified 22 of the candidates as new members of Taurus, which includes one of the coolest known members (M9.75). Our updated census of members within the SDSS field shows a surplus of solar-mass stars relative to clusters, although it is less pronounced than in the smaller fields towards the stellar aggregates that were sur...

  2. Fundamental stellar parameters for selected T-Tauri stars in the Chamaeleon and Rho Ophiuchus star-forming regions

    CERN Document Server

    James, David; Richert, Alexander; Cargile, Phillip; Santo, Nuno; Melo, Claudio; Bouvier, Jerome

    2016-01-01

    We present the results of an optical photometry and high-resolution spectroscopy campaign for a modest sample of X-ray selected stars in the Chamaeleon and Rho Ophiuchus star forming regions. With R~50000 optical spectra, we establish kinematic membership of the parent association and confirm stellar youth for each star in our sample. With the acquisition of new standardized BVIc photometry, in concert with near-infrared data from the literature, we derive age and mass from stellar positions in model-dependent Hertzsprung-Russell diagrams. We compare isochronal ages derived using colour-dependent extinction values finding that, within error bars, ages are the same irrespective of whether E(B-V), E(V-Ic), E(J-H) or E(H-K) is used to establish extinction, although model ages tend to be marginally younger for redder Ecolour values. For Cham I and Eta Cham members we derive ages of ~ 25 Myr post-T Tauri star population. In Rho Ophiuchus, most stars in our sample have isochronal ages 5) in the 2MASS colour colour ...

  3. Direct imaging of extra-solar planets in star forming regions: Lessons learned from a false positive around IM Lup

    CERN Document Server

    Mawet, Dimitri; Riaud, Pierre; Surdej, Jean; Montagnier, Guillaume; Ducourant, Christine; Augereau, Jean-Charles; Rottinger, Sarah; Girard, Julien; Krist, John; Stapelfeldt, Karl

    2012-01-01

    Most exoplanet imagers consist of ground-based adaptive optics coronagraphic cameras which are currently limited in contrast, sensitivity and astrometric precision, but advantageously observe in the near-IR (1- 5{\\mu}m). Because of these practical limitations, our current observational aim at detecting and characterizing planets puts heavy constraints on target selection, observing strategies, data reduction, and follow-up. Most surveys so far have thus targeted young systems (1-100Myr) to catch the putative remnant thermal radiation of giant planets, which peaks in the near-IR. They also favor systems in the solar neighborhood (d<80pc), which eases angular resolution requirements but also ensures a good knowledge of the distance and proper motion, which are critical to secure the planet status, and enable subsequent characterization. Because of their youth, it is very tempting to target the nearby star forming regions, which are typically twice as far as the bulk of objects usually combed for planets by d...

  4. A structural model of the pore-forming region of the skeletal muscle ryanodine receptor (RyR1.

    Directory of Open Access Journals (Sweden)

    Srinivas Ramachandran

    2009-04-01

    Full Text Available Ryanodine receptors (RyRs are ion channels that regulate muscle contraction by releasing calcium ions from intracellular stores into the cytoplasm. Mutations in skeletal muscle RyR (RyR1 give rise to congenital diseases such as central core disease. The absence of high-resolution structures of RyR1 has limited our understanding of channel function and disease mechanisms at the molecular level. Here, we report a structural model of the pore-forming region of RyR1. Molecular dynamics simulations show high ion binding to putative pore residues D4899, E4900, D4938, and D4945, which are experimentally known to be critical for channel conductance and selectivity. We also observe preferential localization of Ca(2+ over K(+ in the selectivity filter of RyR1. Simulations of RyR1-D4899Q mutant show a loss of preference to Ca(2+ in the selectivity filter as seen experimentally. Electrophysiological experiments on a central core disease mutant, RyR1-G4898R, show constitutively open channels that conduct K(+ but not Ca(2+. Our simulations with G4898R likewise show a decrease in the preference of Ca(2+ over K(+ in the selectivity filter. Together, the computational and experimental results shed light on ion conductance and selectivity of RyR1 at an atomistic level.

  5. Far-infrared molecular lines from Low- to High-Mass Star Forming Regions observed with Herschel

    CERN Document Server

    Karska, A; Bruderer, S; Goicoechea, J R; Herczeg, G J; van Dishoeck, E F; José-García, I San; Contursi, A; Feuchtgruber, H; Fedele, D; Baudry, A; Braine, J; Chavarría, L; Cernicharo, J; van der Tak, F F S; Wyrowski, F

    2013-01-01

    (Abridged) We study the response of the gas to energetic processes associated with high-mass star formation and compare it with studies on low- and intermediate-mass young stellar objects (YSOs) using the same methods. The far-IR line emission and absorption of CO, H$_2$O, OH, and [OI] reveals the excitation and the relative contribution of different species to the gas cooling budget. Herschel-PACS spectra covering 55-190 um are analyzed for ten high-mass star forming regions of various luminosities and evolutionary stages at spatial scales of ~10^4 AU. Radiative transfer models are used to determine the contribution of the envelope to the far-IR CO emission. The close environments of high-mass YSOs show strong far-IR emission from molecules, atoms, and ions. Water is detected in all 10 objects even up to high excitation lines. CO lines from J=14-13 up to typically 29-28 show a single temperature component, Trot~300 K. Typical H$_2$O temperatures are Trot~250 K, while OH has Trot~80 K. Far-IR line cooling is ...

  6. 12 GHz methanol maser outflow from the massive star-forming region: G35.20-0.74

    Institute of Scientific and Technical Information of China (English)

    Qing-Zeng Yan; Bo Zhang; Zheng-Hong Tang; Xing-Wu Zheng

    2013-01-01

    We report the internal proper motions of 12 GHz methanol masers in massive star-forming region G35.20-0.74 observed with the Very Long Baseline Array (VLBA) at four epochs spanning about 1.5 yr.Two groups of maser features were detected,groups A and B,and the latter that had a V-shaped spatial distribution is likely tracing the north outflow in G35.20-0.74.We present a three-dimensional model for the kinematics of these masers,by assuming the interstellar medium was blown by the stellar wind from the driving source (G35.2N) of the outflow.Adopting a position angle of ~ 81° for the main axis of the outflow from previous studies,we estimate an inclination of 35° ± 5.5°,a velocity of 8.1 ± 0.7 km s-1 for the stellar wind along the main axis and an expansion speed gradient of 0.05 ± 0.016 km s-1 AU-1.From the model,we derive the age of the north outflow in G35.20-0.74 to be ~ 1.6 × 104 yr.

  7. The Massive Star Forming Region Cygnus OB2. II. Integrated Stellar Properties and the Star Formation History

    CERN Document Server

    Wright, Nicholas J; Drew, Janet E; Vink, Jorick S

    2010-01-01

    Cygnus OB2 is the nearest example of a massive star forming region, containing over 50 O-type stars and hundreds of B-type stars. We have analysed the properties of young stars in two fields in Cyg OB2 using the recently published deep catalogue of Chandra X-ray point sources with complementary optical and near-IR photometry. Our sample is complete to 1 Msun (excluding A and B-type stars that do not emit X-rays), making this the deepest study of the stellar properties and star formation history in Cyg OB2 to date. From Siess et al. (2000) isochrone fits to the near-IR color-magnitude diagram, we derive ages of 3.5 (+0.75/-1.0) and 5.25 (+1.5/-1.0) Myrs for sources in the two fields, both with considerable spreads around the pre-MS isochrones. The presence of a stellar population somewhat older than the present-day O-type stars, also fits in with the low fraction of sources with inner circumstellar disks (as traced by the K-band excess) that we find to be very low, but appropriate for a population of age ~5 My...

  8. The James Clerk Maxwell Telescope Legacy Survey of Nearby Star-forming Regions in the Gould Belt

    CERN Document Server

    Ward-Thompson, D; Hatchell, J; Hogerheijde, M R; Bastien, P; Basu, S; Bonnell, I; Bowey, J; Brunt, C; Buckle, J; Butner, H; Cavanagh, B; Chrysostomou, A; Curtis, E; Davis, C J; Dent, W R F; van Dishoeck, E; Edmunds, M G; Fich, M; Fiege, J; Fissel, L; Friberg, P; Friesen, R; Frieswijk, W; Fuller, G A; Gosling, A; Graves, S; Greaves, J S; Helmich, F; Hills, R E; Holland, W S; Houde, M; Jayawardhana, R; Johnstone, D; Joncas, G; Kirk, H; Kirk, J M; Knee, L B G; Matthews, B; Matthews, H; Matzner, C; Moriarty-Schieven, G H; Naylor, D; Nutter, D; Padman, R; Plume, R; Rawlings, J M C; Redman, R O; Reid, M; Richer, J S; Shipman, R; Simpson, R J; Spaans, M; Stamatellos, D; Tsanis, Y; Viti, S; Weferling, B; White, G J; Whitworth, A P; Wouterloot, J; Yates, J; Zhu, M

    2007-01-01

    This paper describes a James Clerk Maxwell Telescope (JCMT) legacy survey that has been awarded roughly 500 hrs of observing time to be carried out from 2007 to 2009. In this survey we will map with SCUBA-2 (Submillimetre Common User Bolometer Array 2) almost all of the well-known low-mass and intermediate-mass star-forming regions within 0.5 kpc that are accessible from the JCMT. Most of these locations are associated with the Gould Belt. From these observations we will produce a flux-limited snapshot of star formation near the Sun, providing a legacy of images, as well as point-source and extended-source catalogues, over almost 700 square degrees of sky. The resulting images will yield the first catalogue of prestellar and protostellar sources selected by submillimetre continuum emission, and should increase the number of known sources by more than an order of magnitude. We will also obtain CO maps with the array receiver HARP (Heterodyne Array Receiver Programme), in three CO isotopologues, of a large typi...

  9. Peering into the Giant Planet Forming Region of the TW Hydrae Disk with the Gemini Planet Imager

    CERN Document Server

    Rapson, Valerie A; Millar-Blanchaer, Maxwell A; Dong, Ruobing

    2015-01-01

    We present Gemini Planet Imager (GPI) adaptive optics near-infrared images of the giant planet-forming regions of the protoplanetary disk orbiting the nearby (D = 54 pc), pre-main sequence (classical T Tauri) star TW Hydrae. The GPI images, which were obtained in coronagraphic/polarimetric mode, exploit starlight scattered off small dust grains to elucidate the surface density structure of the TW Hya disk from 80 AU to within 10 AU of the star at 1.5 AU resolution. The GPI polarized intensity images unambiguously con?rm the presence of a gap in the radial surface brightness distribution of the inner disk. The gap is centered near 23 AU, with a width of 5 AU and a depth of 50%. In the context of recent simulations of giant planet formation in gaseous, dusty disks orbiting pre-main sequence stars, these results indicate that at least one young planet with a mass 0.2 M_J could be present in the TW Hya disk at an orbital semi-major axis similar to that of Uranus. If this (proto)planet is actively accreting gas fr...

  10. H2O maser motions and the distance of the star forming region G192.16-3.84

    CERN Document Server

    Shiozaki, Satoshi; Tafoya, Daniel; Omodaka, Toshihiro; Hirota, Tomoya; Honma, Mareki; Matsui, Makoto; Ueno, Yuji

    2011-01-01

    We present the results of astrometic observations of H2O masers associated with the star forming region G192.16-3.84 with the VLBI Exploration of Radio Astrometry (VERA). The H2O masers seem to be associated with two young stellar objects (YSOs) separated by \\sim1200 AU as reported in previous observations. In the present observations, we successfully detected an annual parallax of 0.66 \\pm 0.04 mas for the H2 O masers, which corresponds to a distance to G192.16-3.84 of D = 1.52 \\pm 0.08 kpc from the Sun. The determined distance is shorter than the estimated kinematic distance. Using the annual parallax distance and the estimated parameters of the millimeter continuum emission, we estimate the mass of the disk plus circumstellar cloud in the southern young stellar object to be 10.0+4.3M\\cdot. We also estimate the galactocentric distance and the peculiar motion -3.6 of G192.16-3.84, relative to a circular Galactic rotation: R\\star = 9.99 \\pm 0.08 kpc, Z\\star = -0.10 \\pm 0.01 kpc, and (U\\star,V\\star,W\\star)=(-2...

  11. a Search for Interstellar Carbon-Chain Alcohol HC4OH in the Star Forming Region L1527

    Science.gov (United States)

    Araki, Mitsunori; Takano, Shuro; Koshikawa, Hiromichi Yamabe Naohiro; Tsukiyama, Koichi; Nakane, Aya; Okabatyashi, Toshiaki; Kunimatsu, Arisa; Kuze, Nobuhiko

    2011-06-01

    We have made a sensitive search for the rotational transitions of carbon-chain alcohol HC_4OH with the frequency ragne from 21.2 to 46.7 GHz in the star forming region L1527 in Taurus with rich carbon-chain chemistry. The incentive of this observation was a laboratory detection of HC_4OH by the microwave spectroscopy. Despite achieving an rms of several mK in antenna temperature by the 45m telescope at Nobeyama Radio Observatory, the searche for HC_4OH was negative, leading to a 5 sigma upper limit corresponding to the column density of 4 × 1012 Cm-2 based on the excitation temperature of 12.3 K. The upper limit indicates that the [HC_4-OH]/[HC_4-CN] ratio is less than 1.0. The ratio suggests that the cyanide species with carbon-chain structure is dominant in comparison with the hydroxyl one in L1527, which can be the opposite case of saturated compounds, e.g. CH_3OH and CH_3CN, in hot cores and dark clouds.

  12. A Multi-Wavelength High Resolution Study of the S255 Star Forming Region. General structure and kinematics

    CERN Document Server

    Zinchenko, I; Su, Y -N; Kurtz, S; Ojha, D K; Samal, M R; Ghosh, S K

    2012-01-01

    We present observational data for two main components (S255IR and S255N) of the S255 high mass star forming region in continuum and molecular lines obtained at 1.3 mm and 1.1 mm with the SMA, at 1.3 cm with the VLA and at 23 and 50 cm with the GMRT. The angular resolution was from ~ 2" to ~ 5" for all instruments. With the SMA we detected a total of about 50 spectral lines of 20 different molecules (including isotopologues). About half of the lines and half of the species (in particular N2H+, SiO, C34S, DCN, DNC, DCO+, HC3N, H2CO, H2CS, SO2) have not been previously reported in S255IR and partly in S255N at high angular resolution. Our data reveal several new clumps in the S255IR and S255N areas by their millimeter wave continuum emission. Masses of these clumps are estimated at a few solar masses. The line widths greatly exceed expected thermal widths. These clumps have practically no association with NIR or radio continuum sources, implying a very early stage of evolution. At the same time, our SiO data ind...

  13. A biochemically distinct form of cytochrome oxidase (COX) deficiency in the Saguenay-Lac-Saint-Jean region of Quebec.

    Science.gov (United States)

    Merante, F; Petrova-Benedict, R; MacKay, N; Mitchell, G; Lambert, M; Morin, C; De Braekeleer, M; Laframboise, R; Gagné, R; Robinson, B H

    1993-08-01

    We report the results of biochemical and molecular investigations on a group of patients from the Saguenay-Lac-Saint-Jean region of Quebec who have an unusual form of cytochrome oxidase deficiency and Leigh disease. This group can be distinguished from the classical presentation of cytochrome oxidase deficiency with Leigh disease, by the severity of the biochemical defect in different tissues. The activity in skin fibroblasts, amniocytes, and skeletal muscle of cytochrome oxidase is 50% of normal, while in kidney and heart it is close to normal values. Brain and liver, on the other hand, have very low activities. The defect in activity appears to result from a failure of assembly of the cytochrome oxidase complex in liver, but levels of mRNA for both mitochondrially encoded and nuclear-encoded subunits in liver and skin fibroblasts were found to be the same as those in controls. The cDNA sequence of the liver-specific cytochrome oxidase subunits VIa and VIIa were determined in samples from patient liver and skin fibroblasts and showed normal coding sequence.

  14. Water vapor in high-mass star-forming regions and PDRs : Tracing the dynamics and chemistry with Herschel/HIFI

    NARCIS (Netherlands)

    Choi, Yunhee

    2015-01-01

    Massive stars play a major role in the interstellar energy budget and the shaping of the galactic environment. The water molecule is thought to be a sensitive tracer of physical conditions in star-forming regions because of its large abundance variations between hot and cold regions. Herschel/HIFI

  15. HH 223: a parsec-scale H2 outflow in the star-forming region L723

    Science.gov (United States)

    López, R.; Acosta-Pulido, J. A.; Gómez, G.; Estalella, R.; Carrasco-González, C.

    2010-11-01

    Context. The dark cloud Lynds 723 (L723) is a low-mass star-forming region where one of the few known cases of a quadrupolar CO outflow has been reported. Two recent works have found that the radio continuum source VLA 2, towards the centre of the CO outflow, is actually a multiple system of young stellar objects (YSOs). Several line-emission nebulae that lie projected on the east-west CO outflow were detected in narrow-band Hα and [S ii] images. The spectra of the knots are characteristic of shock-excited gas (Herbig-Haro spectra), with supersonic blueshifted velocities, which suggests an optical outflow also powered by the VLA 2 YSO system of L723. Aims: Our aim is to study L723 in the near-infrared and look for line-emission nebulae associated with the optical and CO outflows. Methods: We imaged a field of ~5' × 5' centred on HH 223, which includes the whole region of the quadrupolar CO outflow with narrow-band filters centred on the [Fe ii] 1.644 μm and H2 2.122 μm lines, together with off-line Hc and Kc filters. The [Fe ii] and H2 line-emission structures were identified after extracting the continuum contribution, if any. Their positions were determined from an accurate astrometry of the images. Results: The H2 line-emission structures appear distributed over a region of 5.5 arcmin (~0.5 pc for a distance of 300 pc) at both sides of the VLA 2 YSO system, with an S-shape morphology, and are projected onto the east-west CO outflow. Most of them were resolved in smaller knotty substructures. The [Fe ii] emission only appears associated with HH 223. An additional nebular emission from the continuum in Hc and Kc appears associated with HH 223-K1, the structure closest to the VLA 2 YSO system, and could be tracing the cavity walls. Conclusions: We propose that the H2 structures form part of a large-scale near-infrared outflow, which is also associated with the VLA 2 YSO system. The current data do not allow us to discern which of the YSOs of VLA 2 is powering

  16. Star-forming Activity in the H II Regions Associated with the IRAS 17160–3707 Complex

    Science.gov (United States)

    Nandakumar, G.; Veena, V. S.; Vig, S.; Tej, A.; Ghosh, S. K.; Ojha, D. K.

    2016-11-01

    We present a multiwavelength investigation of star formation activity toward the southern H ii regions associated with IRAS 17160–3707, located at a distance of 6.2 kpc with a bolometric luminosity of 8.3 × 105 L ⊙. The ionized gas distribution and dust clumps in the parental molecular cloud are examined in detail using measurements at infrared, submillimeter and radio wavelengths. The radio continuum images at 1280 and 610 MHz obtained using the Giant Metrewave Radio Telescope reveal the presence of multiple compact sources as well as nebulous emission. At submillimeter wavelengths, we identify seven dust clumps and estimate their physical properties such as temperature: 24–30 K, mass: 300–4800 M ⊙ and luminosity: 9–317 × 102 L ⊙ using modified blackbody fits to the spectral energy distributions (SEDs) between 70 and 870 μm. We find 24 young stellar objects (YSOs) in the mid-infrared, with a few of them coincident with the compact radio sources. The SEDs of the YSOs have been fitted by the Robitaille models and the results indicate that those having radio compact sources as counterparts host massive objects in early evolutionary stages with best fit age ≤0.2 Myr. We compare the relative evolutionary stages of clumps using various signposts such as masers, ionized gas, presence of YSOs and infrared nebulosity, and find six massive star-forming clumps and one quiescent clump. Of the former, five are in a relatively advanced stage and one in an earlier stage.

  17. Trigonometric distance and proper motion of IRAS 20056+3350: a massive star-forming region on the solar circle

    Energy Technology Data Exchange (ETDEWEB)

    Burns, Ross A.; Handa, Toshihiro; Omodaka, Toshihiro; Nakagawa, Akiharu; Nakanishi, Hiroyuki [Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Kôrimoto, Kagoshima, Kagoshima 890-0065 (Japan); Nagayama, Takumi [Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Hayashi, Masahiko [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Shizugami, Makoto, E-mail: RossBurns88@MilkyWay.sci.Kagoshima-u.ac.jp [Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-12 Hoshi-ga-oka, Mizusawa-ku, Oshu, Iwate 023-0861 (Japan)

    2014-12-10

    We report our measurement of the trigonometric distance and proper motion of IRAS 20056+3350, obtained from the annual parallax of H{sub 2}O masers. Our distance of D=4.69{sub −0.51}{sup +0.65} kpc, which is 2.8 times larger than the near kinematic distance adopted in the literature, places IRAS 20056+3350 at the leading tip of the Local arm and proximal to the solar circle. Using our distance, we reevaluate past observations to reveal IRAS 20056+3350 as a site of massive star formation at a young stage of evolution. This result is consistent with the spectral energy distribution of the source evaluated with published photometric data from UKIDSS, WISE, AKARI, IRAS, and the submillimeter continuum. Both analytical approaches reveal the luminosity of the region to be 2.4 × 10{sup 4} L {sub ☉}, and suggest that IRAS 20056+3350 is forming an embedded star of ≥16 M {sub ☉}. We estimated the proper motion of IRAS 20056+3350 to be (μ{sub α}cos δ, μ{sub δ}) = (–2.62 ± 0.33, –5.65 ± 0.52) mas yr{sup –1} from the group motion of H{sub 2}O masers, and use our results to estimate the angular velocity of Galactic rotation at the Galactocentric distance of the Sun, Ω{sub 0} = 29.75 ± 2.29 km s{sup –1} kpc{sup –1}, which is consistent with the values obtained for other tangent point and solar circle objects.

  18. Fundamental stellar parameters for selected T-Tauri stars in the Chamaeleon and Rho Ophiuchus star-forming regions

    Science.gov (United States)

    James, D. J.; Aarnio, A. N.; Richert, A. J. W.; Cargile, P. A.; Santos, N. C.; Melo, C. H. F.; Bouvier, J.

    2016-06-01

    We present the results of an optical photometry and high-resolution spectroscopy campaign for a modest sample of X-ray selected stars in the Chamaeleon and Rho Ophiuchus star-forming regions. With R˜ 50 000 optical spectra, we establish kinematic membership of the parent association and confirm stellar youth for each star in our sample. With the acquisition of new standardized BVIc photometry, in concert with near-infrared data from the literature, we derive age and mass from stellar positions in model-dependent Hertzsprung-Russell diagrams. We compare isochronal ages derived using colour-dependent extinction values finding that, within error bars, ages are the same irrespective of whether E(B - V), E(V - Ic), E(J - H) or E(H - K) is used to establish extinction, although model ages tend to be marginally younger for redder Ecolour values. For Cham I and η Cham members, we derive ages of ≲5-6 Myr, whereas our three η Cha candidates are more consistent with a ≳25 Myr post-T Tauri star population. In Rho Ophiuchus, most stars in our sample have isochronal ages 5) in the Two Micron All Sky Survey colour-colour diagram, however in terms of Hα emission, all stars except RXJ1625.6-2613 are consistent with being weak-lined T-Tauri stars. Spectral energy distributions (SEDs) over the range ≃4000 Å <λ < 1000 μm, show that only one Chamaeleon star (RXJ1112.7 -7637) and three Rho Ophiuchus stars (ROXR1 13, RXJ1625.6-2613 & RXJ1627.1-2419) reveal substantial departures from a bare photosphere.

  19. An HST Imaging Survey of Low-mass Stars in the Chamaeleon I Star-forming Region

    Science.gov (United States)

    Robberto, M.; Spina, L.; Da Rio, N.; Apai, D.; Pascucci, I.; Ricci, L.; Goddi, C.; Testi, L.; Palla, F.; Bacciotti, F.

    2012-09-01

    We present new Hubble Space Telescope/WFPC2 observations of 20 fields centered around T Tauri stars in the Chamaeleon I star-forming region. Images have been obtained in the F631N ([O I] λ6300), F656N (Hα), and F673N ([S II] λλ6716, 6731) narrow-band filters, plus the Johnson V-band equivalent F547M filter. We detect 31 T Tauri stars falling within our fields. We discuss the optical morphology of 10 sources showing evidence of either binarity, circumstellar material, or mass loss. We supplement our photometry with a compilation of optical, infrared, and submillimeter (sub-mm) data from the literature, together with new sub-mm data for three objects, to build the spectral energy distributions (SEDs) of 19 single sources. Using an SED model fitting tool, we self-consistently estimate a number of stellar and disk parameters, while mass accretion rates are directly derived from our Hα photometry. We find that bolometric luminosities derived from dereddened optical data tend to be underestimated in systems with high α2-24 IR spectral index, suggesting that disks seen nearly edge-on may occasionally be interpreted as low-luminosity (and therefore more evolved) sources. On the other hand, the same α2-24 IR spectral index, a tracer of the amount of dust in the warmer layers of the circumstellar disks, and the mass accretion rate appear to decay with the isochronal stellar age, suggesting that the observed age spread (sime 0.5-5 Myr) within the cluster is real. Our sample contains a few outliers that may have dissipated their circumstellar disks on a shorter timescale.

  20. A Survey for New Members of the Taurus Star-forming Region with the Sloan Digital Sky Survey

    Science.gov (United States)

    Luhman, K. L.; Mamajek, E. E.; Shukla, S. J.; Loutrel, N. P.

    2017-01-01

    Previous studies have found that ∼1 deg2 fields surrounding the stellar aggregates in the Taurus star-forming region exhibit a surplus of solar-mass stars relative to denser clusters like IC 348 and the Orion Nebula Cluster. To test whether this difference reflects mass segregation in Taurus or a variation in the initial mass function, we have performed a survey for members of Taurus across a large field (∼40 deg2) that was imaged by the Sloan Digital Sky Survey (SDSS). We obtained optical and near-infrared spectra of candidate members identified with those images and the Two Micron All Sky Survey, as well as miscellaneous candidates that were selected with several other diagnostics of membership. We have classified 22 of the candidates as new members of Taurus, which includes one of the coolest known members (M9.75). Our updated census of members within the SDSS field shows a surplus of solar-mass stars relative to clusters, although it is less pronounced than in the smaller fields toward the stellar aggregates that were surveyed for previously measured mass functions in Taurus. In addition to spectra of our new members, we include in our study near-IR spectra of roughly half of the known members of Taurus, which are used to refine their spectral types and extinctions. We also present an updated set of near-IR standard spectra for classifying young stars and brown dwarfs at M and L types. Based on observations performed with the Sloan Digital Sky Survey, Hobby-Eberly Telescope, NASA Infrared Telescope Facility, Gemini Observatory, and Canada–France–Hawaii Telescope.

  1. THE IMPORTANCE OF THE MAGNETIC FIELD FROM AN SMA-CSO-COMBINED SAMPLE OF STAR-FORMING REGIONS

    Energy Technology Data Exchange (ETDEWEB)

    Koch, Patrick M.; Tang, Ya-Wen; Ho, Paul T. P.; Chen, Huei-Ru Vivien; Liu, Hau-Yu Baobab; Yen, Hsi-Wei; Lai, Shih-Ping [Academia Sinica, Institute of Astronomy and Astrophysics, Taipei, Taiwan (China); Zhang, Qizhou; Chen, How-Huan; Ching, Tao-Chung [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Girart, Josep M. [Institut de Ciències de l' Espai, CSIC-IEEC, Campus UAB, Facultat de Ciències, C5p 2, 08193 Bellaterra, Catalonia (Spain); Frau, Pau [Observatorio Astronómico Nacional, Alfonso XII, 3 E-28014 Madrid (Spain); Li, Hua-Bai [Department of Physics, The Chinese University of Hong Kong (Hong Kong); Li, Zhi-Yun [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904 (United States); Padovani, Marco [Laboratoire Univers et Particules de Montpellier, UMR 5299 du CNRS, Université de Montpellier II, place E. Bataillon, cc072, F-34095 Montpellier (France); Qiu, Keping [School of Astronomy and Space Science, Nanjing University, 22 Hankou Road, Nanjiing 210093 (China); Rao, Ramprasad, E-mail: pmkoch@asiaa.sinica.edu.tw [Academia Sinica, Institute of Astronomy and Astrophysics, 645 N. Aohoku Place, Hilo, HI 96720 (United States)

    2014-12-20

    Submillimeter dust polarization measurements of a sample of 50 star-forming regions, observed with the Submillimeter Array (SMA) and the Caltech Submillimeter Observatory (CSO) covering parsec-scale clouds to milliparsec-scale cores, are analyzed in order to quantify the magnetic field importance. The magnetic field misalignment δ—the local angle between magnetic field and dust emission gradient—is found to be a prime observable, revealing distinct distributions for sources where the magnetic field is preferentially aligned with or perpendicular to the source minor axis. Source-averaged misalignment angles (|δ|) fall into systematically different ranges, reflecting the different source-magnetic field configurations. Possible bimodal (|δ|) distributions are found for the separate SMA and CSO samples. Combining both samples broadens the distribution with a wide maximum peak at small (|δ|) values. Assuming the 50 sources to be representative, the prevailing source-magnetic field configuration is one that statistically prefers small magnetic field misalignments |δ|. When interpreting |δ| together with a magnetohydrodynamics force equation, as developed in the framework of the polarization-intensity gradient method, a sample-based log-linear scaling fits the magnetic field tension-to-gravity force ratio (Σ {sub B}) versus (|δ|) with (Σ {sub B}) = 0.116 · exp (0.047 · (|δ|)) ± 0.20 (mean error), providing a way to estimate the relative importance of the magnetic field, only based on measurable field misalignments |δ|. The force ratio Σ {sub B} discriminates systems that are collapsible on average ((Σ {sub B}) < 1) from other molecular clouds where the magnetic field still provides enough resistance against gravitational collapse ((Σ {sub B}) > 1). The sample-wide trend shows a transition around (|δ|) ≈ 45°. Defining an effective gravitational force ∼1 – (Σ {sub B}), the average magnetic-field-reduced star formation efficiency is at least a

  2. Physical and chemical variations within the W3 star-forming region. II. The 345 GHz spectral line survey.

    Science.gov (United States)

    Helmich, F. P.; van Dishoeck, E. F.

    1997-08-01

    Results are presented of the 345 GHz spectral survey toward three sources in the W3 Giant Molecular Cloud: W3 IRS4, W3 IRS5 and W3(H_2O). Nearly 90% of the atmospheric window between 334 and 365 GHz has been scanned using the James Clerk Maxwell Telescope down to a noise level of ~80 mK per resolution element. These observations are complemented by a large amount of data in the 230 GHz atmospheric window. From this data set physical conditions and beam-averaged column densities are derived for more than 14 chemically different species (over 24 different isotopes). The physical parameters derived in Paper I (\\cite[Helmich et al. 1994]{ref36}) are confirmed by the analysis of the excitation of other species, although there is evidence that the silicon- and sulfur-bearing molecules exist in a somewhat denser and warmer environment. The densities are high, >= 10^6 cm^{-3}, in the three sources and the kinetic temperatures for the bulk of the gas range from 55 K for IRS4 to 220 K for W3(H_2O). The chemical differences between the three sources are very striking: silicon- and sulfur-bearing molecules such as SiO and SO_2 are prominent toward IRS5, whereas organic molecules like CH_3OH, CH_3OCH_3 and CH_3OCHO are at least an order of magnitude more abundant toward W3(H_2O). Vibrationally excited molecules are also detected toward this source. Only simple molecules are found toward IRS4. The data provide constraints on the amount of deuterium fractionation and the ionization fraction in the observed regions as well. These chemical characteristics are discussed in the context of an evolutionary sequence, in which IRS5 is the youngest, W3(H_2O) somewhat older and IRS4, although still enigmatic, the oldest. The James Clerk Maxwell Telescope is operated by the The Joint Astronomy Centre on behalf of the Particle Physics and Astronomy Research Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada

  3. Search for OB stars running away from young star clusters. II. The NGC 6357 star-forming region

    Science.gov (United States)

    Gvaramadze, V. V.; Kniazev, A. Y.; Kroupa, P.; Oh, S.

    2011-11-01

    Dynamical few-body encounters in the dense cores of young massive star clusters are responsible for the loss of a significant fraction of their massive stellar content. Some of the escaping (runaway) stars move through the ambient medium supersonically and can be revealed via detection of their bow shocks (visible in the infrared, optical or radio). In this paper, which is the second of a series of papers devoted to the search for OB stars running away from young ( ≲ several Myr) Galactic clusters and OB associations, we present the results of the search for bow shocks around the star-forming region NGC 6357. Using the archival data of the Midcourse Space Experiment (MSX) satellite and the Spitzer Space Telescope, and the preliminary data release of the Wide-Field Infrared Survey Explorer (WISE), we discovered seven bow shocks, whose geometry is consistent with the possibility that they are generated by stars expelled from the young (~1-2 Myr) star clusters, Pismis 24 and AH03 J1725-34.4, associated with NGC 6357. Two of the seven bow shocks are driven by the already known OB stars, HD 319881 and [N78] 34. Follow-up spectroscopy of three other bow-shock-producing stars showed that they are massive (O-type) stars as well, while the 2MASS photometry of the remaining two stars suggests that they could be B0 V stars, provided that both are located at the same distance as NGC 6357. Detection of numerous massive stars ejected from the very young clusters is consistent with the theoretical expectation that star clusters can effectively lose massive stars at the very beginning of their dynamical evolution (long before the second mechanism for production of runaway stars, based on a supernova explosion in a massive tight binary system, begins to operate) and lends strong support to the idea that probably all field OB stars have been dynamically ejected from their birth clusters. A by-product of our search for bow shocks around NGC 6357 is the detection of three circular

  4. A new species of habitat-forming Suberites (Porifera, Demospongiae, Suberitida) in the Benguela upwelling region (South Africa).

    Science.gov (United States)

    Samaai, Toufiek; Maduray, Seshnee; Janson, Liesl; Gibbons, Mark J; Ngwakum, Benedicta; Teske, Peter R

    2017-04-12

    S. dandelenae sp. nov. is described from the west coast of South Africa and occurs at depths of 80-500 m among unconsolidated sediments. Specimens can reach 40 cm in length and in some areas off South Africa, up to 18 tons/km2 can be collected in a single demersal trawl. Morphologically, the sponge is straw yellow, massive with rounded lobes and has a velvety surface: it is characterized by subradiate, irregular reticulation of bundles of tylostyles and tylostrongyles. Specimens of S. dandelenae sp. nov. have three size classes of tylostyles with the largest tylostyle lengths being 516 μm (441-614 μm), medium tylostyle lengths being 352 μm (307-422 μm) and the shortest tylostyle lengths being 215 μm (153-288 μm). Apart from the presence of tylostyles, some specimens of S. dandelenae sp. nov. also possess centrotylostongyles/oxeas, tylostrongyles and microacanthostrongyles spicules. We have used morphological characters to distinguish this species and a molecular marker (cox1) to conform that all specimens are the same species. At the spicular level, S. dandelenae sp. nov. is characterized by a complex of spicule types that vary with specimen size. Following a histological investigation and re-description of the holotypes of S. ficus (Johnston, 1842) and S. tylobtusus Lévi, 1958, and comparisons with S. carnosus (Johnston, 1842), S. stilensis Burton, 1933, and other Suberites species described from the African region, it is clear that the new species is different in spicule morphology, spicule size and external morphology. For example, microacanthostrongyles are not present in S. tylobtusus and S. carnosus, whilst S. ficus possesses a second, non-spinose category of microstrongyles. Suberites tylobtusus has tylostyles that are sometimes polytylote, with heads either well formed, pear shaped or reduced, in only one size catogory. The 'tylobtuse' condition of the tylostyles is also different to the kidney-shaped and centrotylostrongyles found in S. dandelenae

  5. Analysis of Nucleon Electromagnetic Form Factors from Light-Front Holographic QCD : The Space-Like Region

    CERN Document Server

    Sufian, Raza Sabbir; Brodsky, Stanley J; Deur, Alexandre; Dosch, Hans Günter

    2016-01-01

    We present a comprehensive analysis of the nucleon electromagnetic form factors and their flavor decomposition within the framework of light-front holographic QCD. We show that the inclusion of the higher Fock components $|qqqq\\bar{q}>$ has a significant effect on the spin-flip elastic Pauli form factor and almost zero effect on the spin-conserving Dirac form factor. We present light-front holographic QCD predictions of proton and neutron form factors in the momentum transfer range of $0\\leq Q^2 \\leq 20\\, \\text{GeV}^2$ and show that these predictions agree with the available experimental data with high accuracy. In order to correctly describe the Pauli form factor we need an admixture of a five quark state of about 30$\\%$ in the proton and about 40$\\%$ in the neutron. We also extract the nucleon charge and magnetic radii and perform a flavor decomposition of the nucleon electromagnetic form factors. The number of free parameters needed to describe the experimental nucleon form factors in the space-like domain...

  6. Forms of occurrence and genesis of toxic elements in host rocks of coal mining areas of tectonic structures Luhansk region

    OpenAIRE

    Udalov I.V.

    2013-01-01

    The state ofthe problem of accumulationof industrialwaste on the territoryof Ukraineand the Donbass. Indicated bythe presence of raremetalsin the wasteof coal mining.Identifiedforms of presenceof toxic elementsin the hostrocks of thetectonic structures ofcoalLugansk region.Definedgenesisof toxic elementsin the hostrocks of thetectonic structures ofcoalLugansk region.Described in detailthe genesisof mercury(Hg).Found thatarock-formingelementsofpotentiallytoxic elementsincludevanadium(V)and chr...

  7. Extended High Circular Polarization in the Orion Massive Star Forming Region: Implications for the Origin of Homochirality in the Solar System

    CERN Document Server

    Fukue, Tsubasa; Kandori, Ryo; Kusakabe, Nobuhiko; Hough, James H; Bailey, Jeremy; Whittet, Douglas C B; Lucas, Philip W; Nakajima, Yasushi; Hashimoto, Jun

    2010-01-01

    We present a wide-field (~6'x6') and deep near-infrared (Ks band: 2.14 micro m) circular polarization image in the Orion nebula, where massive stars and many low-mass stars are forming. Our results reveal that a high circular polarization region is spatially extended (~0.4 pc) around the massive star-forming region, the BN/KL nebula. However, other regions, including the linearly polarized Orion bar, show no significant circular polarization. Most of the low-mass young stars do not show detectable extended structure in either linear or circular polarization, in contrast to the BN/KL nebula. If our solar system formed in a massive star-forming region and was irradiated by net circularly polarized radiation, then enantiomeric excesses could have been induced, through asymmetric photochemistry, in the parent bodies of the meteorites and subsequently delivered to Earth. These could then have played a role in the development of biological homochirality on Earth.

  8. Extended high circular polarization in the Orion massive star forming region: implications for the origin of homochirality in the solar system.

    Science.gov (United States)

    Fukue, Tsubasa; Tamura, Motohide; Kandori, Ryo; Kusakabe, Nobuhiko; Hough, James H; Bailey, Jeremy; Whittet, Douglas C B; Lucas, Philip W; Nakajima, Yasushi; Hashimoto, Jun

    2010-06-01

    We present a wide-field (approximately 6' x 6') and deep near-infrared (K(s) band: 2.14 mum) circular polarization image in the Orion nebula, where massive stars and many low-mass stars are forming. Our results reveal that a high circular polarization region is spatially extended (approximately 0.4 pc) around the massive star-forming region, the BN/KL nebula. However, other regions, including the linearly polarized Orion bar, show no significant circular polarization. Most of the low-mass young stars do not show detectable extended structure in either linear or circular polarization, in contrast to the BN/KL nebula. If our solar system formed in a massive star-forming region and was irradiated by net circularly polarized radiation, then enantiomeric excesses could have been induced, through asymmetric photochemistry, in the parent bodies of the meteorites and subsequently delivered to Earth. These could then have played a role in the development of biological homochirality on Earth.

  9. The Abundance, Ortho/Para Ratio, and Deuteration of Water in the High-mass Star-forming Region NGC 6334 I

    NARCIS (Netherlands)

    Emprechtinger, M.; Lis, D. C.; Rolffs, R.; Schilke, P.; Monje, R. R.; Comito, C.; Ceccarelli, C.; Neufeld, D. A.; van der Tak, F. F. S.

    2013-01-01

    We present Herschel/HIFI observations of 30 transitions of water isotopologues toward the high-mass star-forming region NGC 6334 I. The line profiles of (H2O)-O-16, (H2O)-O-17, (H2O)-O-18, and HDO show a complex pattern of emission and absorption components associated with the embedded hot cores, a

  10. CH+(1-0) and 13CH+(1-0) absorption lines in the direction of massive star-forming regions

    NARCIS (Netherlands)

    Falgarone, E.; Godard, B.; Cernicharo, J.; de Luca, M.; Gerin, M.; Phillips, T. G.; Black, J. H.; Lis, D. C.; Bell, T. A.; Boulanger, F.; Coutens, A.; Dartois, E.; Encrenaz, P.; Giesen, T.; Goicoechea, J. R.; Goldsmith, P. F.; Gupta, H.; Gry, C.; Hennebelle, P.; Herbst, E.; Hily-Blant, P.; Joblin, C.; Kaźmierczak, M.; Kołos, R.; Krełowski, J.; Martin-Pintado, J.; Monje, R.; Mookerjea, B.; Neufeld, D. A.; Perault, M.; Pearson, J. C.; Persson, C.; Plume, R.; Salez, M.; Schmidt, M.; Sonnentrucker, P.; Stutzki, J.; Teyssier, D.; Vastel, C.; Yu, S.; Menten, K.; Geballe, T. R.; Schlemmer, S.; Shipman, R.; Tielens, A. G. G. M.; Philipp, S.; Cros, A.; Zmuidzinas, J.; Samoska, L. A.; Klein, K.; Lorenzani, A.; Szczerba, R.; Péron, I.; Cais, P.; Gaufre, P.; Ravera, L.; Morris, P.; Lord, S.; Planesas, P.

    2010-01-01

    We report the detection of the ground-state rotational transition of the methylidyne cation CH+ and its isotopologue 13CH+ toward the remote massive star-forming regions W33A, W49N, and W51 with the HIFI instrument onboard the Herschel satellite. Both lines are seen only in absorption against the du

  11. The Schmidt-Kennicutt Law of Matched-Age Star Forming Regions; Pa-alpha Observations of the Early-Phase Interacting Galaxy Taffy I

    CERN Document Server

    Komugi, S; Motohara, K; Takagi, T; Iono, D; Kaneko, H; Ueda, J; Saitoh, T R; Kato, N; Konishi, M; Koshida, S; Morokuma, T; Takahashi, H; Tanabe, T; Yoshii, Y

    2012-01-01

    In order to test a recent hypothesis that the dispersion in the Schmidt-Kennicutt law arises from variations in the evolutionary stage of star forming molecular clouds, we compared molecular gas and recent star formation in an early-phase merger galaxy pair, Taffy I (UGC\\ 12915/UGC\\ 12914, VV\\ 254) which went through a direct collision 20 Myr ago and whose star forming regions are expected to have similar ages. Narrow-band Pa-alpha image is obtained using the ANIR near-infrared camera on the mini-TAO 1m telescope. The image enables us to derive accurate star formation rates within the galaxy directly. The total star formation rate, 22.2 M_sun/yr, was found to be much higher than previous estimates. Ages of individual star forming blobs estimated from equivalent widths indicate that most star forming regions are ~7 Myr old, except for a giant HII region at the bridge which is much younger. Comparison between star formation rates and molecular gas masses for the regions with the same age exhibits a surprisingly...

  12. Detection of interstellar oxidaniumyl : Abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334

    NARCIS (Netherlands)

    Ossenkopf, V.; Mueller, H. S. P.; Lis, D. C.; Schilke, P.; Bell, T. A.; Bruderer, S.; Bergin, E.; Ceccarelli, C.; Comito, C.; Stutzki, J.; Bacman, A.; Baudry, A.; Benz, A. O.; Benedettini, M.; Berne, O.; Blake, G.; Boogert, A.; Bottinelli, S.; Boulanger, F.; Cabrit, S.; Caselli, P.; Caux, E.; Cernicharo, J.; Codella, C.; Coutens, A.; Crimier, N.; Crockett, N. R.; Daniel, F.; Demyk, K.; Dieleman, P.; Dominik, C.; Dubernet, M. L.; Emprechtinger, M.; Encrenaz, P.; Falgarone, E.; France, K.; Fuente, A.; Gerin, M.; Giesen, T. F.; di Giorgio, A. M.; Goicoechea, J. R.; Goldsmith, P. F.; Guesten, R.; Harris, A.; Helmich, F.; Herbst, E.; Hily-Blant, P.; Jacobs, K.; Jacq, T.; Joblin, Ch.; Johnstone, D.; Kahane, C.; Kama, M.; Klein, T.; Klotz, A.; Kramer, C.; Langer, W.; Lefloch, B.; Leinz, C.; Lorenzani, A.; Lord, S. D.; Maret, S.; Martin, P. G.; Martin-Pintado, J.; McCoey, C.; Melchior, M.; Melnick, G. J.; Menten, K. M.; Mookerjea, B.; Morris, P.; Murphy, J. A.; Neufeld, D. A.; Nisini, B.; Pacheco, S.; Pagani, L.; Parise, B.; Pearson, J. C.; Perault, M.; Phillips, T. G.; Plume, R.; Quin, S. -L.; Rizzo, R.; Roellig, M.; Salez, M.; Saraceno, P.; Schlemmer, S.; Simon, R.; Schuster, K.; van der Tak, F. F. S.; Tielens, A. G. G. M.; Teyssier, D.; Trappe, N.; Vastel, C.; Viti, S.; Wakelam, V.; Walters, A.; Wang, S.; Whyborn, N.; van der Wiel, M.; Yorke, H. W.; Yu, S.; Zmuidzinas, J.

    2010-01-01

    Aims. We identify a prominent absorption feature at 1115 GHz, detected in first HIFI spectra towards high-mass star-forming regions, and interpret its astrophysical origin. Methods. The characteristic hyperfine pattern of the H2O+ ground-state rotational transition, and the lack of other known

  13. Herschel/HIFI observations of high-J CO lines in the NGC 1333 low-mass star-forming region

    DEFF Research Database (Denmark)

    Yildiz, U. A.; van Dishoeck, E. F.; Kristensen, L. E.

    2010-01-01

    Herschel/HIFI observations of high-J lines (up to Ju = 10) of 12CO, 13CO and C18O are presented toward three deeply embedded low-mass protostars, NGC 1333 IRAS 2A, IRAS 4A, and IRAS 4B, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. The spectrally-resolved...

  14. The Abundance, Ortho/Para Ratio, and Deuteration of Water in the High-mass Star-forming Region NGC 6334 I

    NARCIS (Netherlands)

    Emprechtinger, M.; Lis, D. C.; Rolffs, R.; Schilke, P.; Monje, R. R.; Comito, C.; Ceccarelli, C.; Neufeld, D. A.; van der Tak, F. F. S.

    2013-01-01

    We present Herschel/HIFI observations of 30 transitions of water isotopologues toward the high-mass star-forming region NGC 6334 I. The line profiles of H16 2O, H17 2O, H18 2O, and HDO show a complex pattern of emission and absorption components associated with the embedded hot cores, a lower-densit

  15. The Abundance, Ortho/Para Ratio, and Deuteration of Water in the High-mass Star-forming Region NGC 6334 I

    NARCIS (Netherlands)

    Emprechtinger, M.; Lis, D. C.; Rolffs, R.; Schilke, P.; Monje, R. R.; Comito, C.; Ceccarelli, C.; Neufeld, D. A.; van der Tak, F. F. S.

    2013-01-01

    We present Herschel/HIFI observations of 30 transitions of water isotopologues toward the high-mass star-forming region NGC 6334 I. The line profiles of (H2O)-O-16, (H2O)-O-17, (H2O)-O-18, and HDO show a complex pattern of emission and absorption components associated with the embedded hot cores, a

  16. The CHESS spectral survey of star forming regions : Peering into the protostellar shock L1157-B1. I. Shock chemical complexity

    NARCIS (Netherlands)

    Codella, C.; Lefloch, B.; Ceccarelli, C.; Cernicharo, J.; Caux, E.; Lorenzani, A.; Viti, S.; Hily-Blant, P.; Parise, B.; Maret, S.; Nisini, B.; Caselli, P.; Cabrit, S.; Pagani, L.; Benedettini, M.; Boogert, A.; Gueth, F.; Melnick, G.; Neufeld, D.; Pacheco, S.; Salez, M.; Schuster, K.; Bacmann, A.; Baudry, A.; Bell, T.; Bergin, E. A.; Blake, G.; Bottinelli, S.; Castets, A.; Comito, C.; Coutens, A.; Crimier, N.; Dominik, C.; Demyk, K.; Encrenaz, P.; Falgarone, E.; Fuente, A.; Gerin, M.; Goldsmith, P.; Helmich, F.; Hennebelle, P.; Henning, Th; Herbst, E.; Jacq, T.; Kahane, C.; Kama, M.; Klotz, A.; Langer, W.; Lis, D.; Lord, S.; Pearson, J.; Phillips, T.; Saraceno, P.; Schilke, P.; Tielens, X.; van der Tak, F.; van der Wiel, M.; Vastel, C.; Wakelam, V.; Walters, A.; Wyrowski, F.; Yorke, H.; Borys, C.; Delorme, Y.; Kramer, C.; Larsson, B.; Mehdi, I.; Ossenkopf, V.; Stutzki, J.

    2010-01-01

    We present the first results of the unbiased survey of the L1157-B1 bow shock, obtained with HIFI in the framework of the key program Chemical HErschel Survey of Star forming regions (CHESS). The L1157 outflow is driven by a low-mass Class 0 protostar and is considered the prototype

  17. Water in star-forming regions with Herschel (WISH) : II. Evolution of 557 GHz 1(10)-1(01) emission in low-mass protostars

    NARCIS (Netherlands)

    Kristensen, L. E.; van Dishoeck, E. F.; Bergin, E. A.; Visser, R.; Yildiz, U. A.; Jose-Garcia, I. San; Jorgensen, J. K.; Herczeg, G. J.; Johnstone, D.; Wampfler, S. F.; Benz, A. O.; Bruderer, S.; Cabrit, S.; Caselli, P.; Doty, S. D.; Harsono, D.; Herpin, F.; Hogerheijde, M. R.; Karska, A.; van Kempen, T. A.; Liseau, R.; Nisini, B.; Tafalla, M.; van der Tak, F.; Wyrowski, F.

    2012-01-01

    Context. Water is a key tracer of dynamics and chemistry in low-mass star-forming regions, but spectrally resolved observations have so far been limited in sensitivity and angular resolution, and only data from the brightest low-mass protostars have been published. Aims. The first systematic survey

  18. 2MASS wide field extinction maps: IV. The Orion, Mon R2, Rosette, and Canis Major star forming regions

    OpenAIRE

    Lombardi, M.; Alves,J.; Lada, C. J.

    2011-01-01

    We present a near-infrared extinction map of a large region (approximately 2200 deg^2) covering the Orion, the Monoceros R2, the Rosette, and the Canis Major molecular clouds. We used robust and optimal methods to map the dust column density in the near-infrared (NICER and NICEST) towards ~19 million stars of the Two Micron All Sky Survey (2MASS) point source catalog. Over the relevant regions of the field, we reached a 1-sigma error of 0.03 mag in the K-band extinction with a resolution of 3...

  19. New SIO Masers in Star Forming Regions W:51 IRS:2 and SAGITTARIUS-B2 MD:5

    Science.gov (United States)

    Hasegawa, T.; Morita, K.; Okumura, S.; Kaifu, N.; Suzuki, H.; Ohishi, M.; Hayashi, M.; Ukita, N.

    The maser emission of the 43 GHz SiO J = 1-0 transitions in two regions of active star formation, W51 IRS2 and Sgr B2 MD5, have been detected using the 45 m telescope at Nobeyama. The SiO masers coincide in position with strong H2O masers in each region within a positional uncertainty of 5arcsec. If the masers radiate isotropically, the power radiated from W51 IRS2 and Sgr B2 MD5 in the masing 43 GHz SiO lines are comparable to that from the maser in Orion-KL.

  20. Modeling the physical structure of star-forming regions with LIME, a 3D radiative transfer code

    Science.gov (United States)

    Quénard, D.; Bottinelli, S.; Caux, E.

    2016-05-01

    The ability to predict line emission is crucial in order to make a comparison with observations. From LTE to full radiative transfer codes, the goal is always to derive the most accurately possible the physical properties of the source. Non-LTE calculations can be very time consuming but are needed in most of the cases since many studied regions are far from LTE.

  1. Indocyanine Green Angiographic and Multifocal Electroretinographic Features in the Diffuse and Regional Form of Bietti′s Crystalline Retinopathy

    Institute of Scientific and Technical Information of China (English)

    Libin Jiang; Feng Wen; Lezheng Wu; Hong Yan; Shixing Hu

    2002-01-01

    Prpose: To observe different features of indocyanine green angiography(ICGA) andtifocal electroretinography (ERG) in the diffuse and regional type of Bieti′sc stalline retinopathy (BCR). Thods: ICGA and the multifocal ERG were performed in two cases of the diffuse andregional type of BCR respectively. These data were compared with fluoresceinangiography (FA), standard Ganzfeld ERG, and visual field testing. Results: In the regional case, ICGA revealed reduced perfusion of the choroidalcirculation in the early phase and multiple hypofluorescent spots in the posterior pole in the late phase, due to choriocapillaris filling defect; the extent of choroiocapillaris losswas shown in early phase of ICGA and there were multifocal hyperfluorescent dotssurrounding hypofluorescent spots in late phase in the diffuse case. The multifocal ERGshowed that the central responses were markedly depressed, corresponding to the visualfield defects, while the findings of Ganzfeld ERG were normal in the regional BCR;however, both the multifocal ERG and Ganzfeld ERG were severely subnormal in thediffuse case.Conclusions: The features of ICGA and multifocal ERG are different between the diffuseand regional BCR. In the meantime, the two tools are also useful to differentiate the typeand assess the extentof evolution in BCR.

  2. Quadruplex forming promoter region of c-myc oncogene as a potential target for a telomerase inhibitory plant alkaloid, chelerythrine.

    Science.gov (United States)

    Ghosh, Saptaparni; Dasgupta, Dipak

    2015-03-27

    Guanine rich sequences present in the promoter region of oncogenes could fold into G-quadruplexes and modulate transcription. Equilibrium between folding and unfolding of the quadruplexes in these regions play important role in disease processes. We have studied the effect of a putative anticancer agent chelerythrine on G-rich NHE III1 present in the promoter region of c-myc oncogene. We have demonstrated the ability of chelerythrine, a telomerase inhibitor, to block the hybridization of Pu27 with its complementary strand via folding it into a quadruplex structure. Calorimetry shows that the association of Pu27 with chelerythrine is primarily enthalpy driven with high binding affinity (∼10(5) M(-1)). The association does not lead to any major structural perturbation of Pu27. The resulting 2:1 complex has enhanced stability as compared to free Pu27. Another notable feature is that the presence of molecular crowding agent like ficoll 70 does not change the mode of recognition though the binding affinity decreases. We suggest that the anticancer activity of chelerythrine could be ascribed to its ability to stabilize the quadruplex structure in the c-myc promoter region thereby downregulating its transcription. Copyright © 2015 Elsevier Inc. All rights reserved.

  3. Which visual functions depend on intermediate visual regions? Insights from a case of developmental visual form agnosia.

    Science.gov (United States)

    Gilaie-Dotan, Sharon

    2016-03-01

    A key question in visual neuroscience is the causal link between specific brain areas and perceptual functions; which regions are necessary for which visual functions? While the contribution of primary visual cortex and high-level visual regions to visual perception has been extensively investigated, the contribution of intermediate visual areas (e.g. V2/V3) to visual processes remains unclear. Here I review more than 20 visual functions (early, mid, and high-level) of LG, a developmental visual agnosic and prosopagnosic young adult, whose intermediate visual regions function in a significantly abnormal fashion as revealed through extensive fMRI and ERP investigations. While expectedly, some of LG's visual functions are significantly impaired, some of his visual functions are surprisingly normal (e.g. stereopsis, color, reading, biological motion). During the period of eight-year testing described here, LG trained on a perceptual learning paradigm that was successful in improving some but not all of his visual functions. Following LG's visual performance and taking into account additional findings in the field, I propose a framework for how different visual areas contribute to different visual functions, with an emphasis on intermediate visual regions. Thus, although rewiring and plasticity in the brain can occur during development to overcome and compensate for hindering developmental factors, LG's case seems to indicate that some visual functions are much less dependent on strict hierarchical flow than others, and can develop normally in spite of abnormal mid-level visual areas, thereby probably less dependent on intermediate visual regions. Copyright © 2015 Elsevier Ltd. All rights reserved.

  4. 2MASS wide field extinction maps: IV. The Orion, Mon R2, Rosette, and Canis Major star forming regions

    CERN Document Server

    Lombardi, Marco; lada, Charles

    2011-01-01

    We present a near-infrared extinction map of a large region (approximately 2200 deg^2) covering the Orion, the Monoceros R2, the Rosette, and the Canis Major molecular clouds. We used robust and optimal methods to map the dust column density in the near-infrared (NICER and NICEST) towards ~19 million stars of the Two Micron All Sky Survey (2MASS) point source catalog. Over the relevant regions of the field, we reached a 1-sigma error of 0.03 mag in the K-band extinction with a resolution of 3 arcmin. We measured the cloud distances by comparing the observed density of foreground stars with the prediction of galactic models, thus obtaining d_{Orion A} = (371 +/- 10) pc, d_{Orion B} = (398 +/- 12) pc, $d_{Mon R2} = (905 +/- 37) pc, $d_{Rosette} = (1330 +/- 48) pc, and $d_{CMa} = (1150 +/- 64) pc, values that compare very well with independent estimates.

  5. Fragmentation and dynamical collapse of the starless high-mass star-forming region IRDC18310-4

    CERN Document Server

    Beuther, H; Tackenberg, J; Henning, Th; Krause, O; Ragan, S; Nielbock, M; Launhardt, R; Bihr, S; Schmiedeke, A; Smith, R; Sakai, T

    2013-01-01

    Aims: We study the fragmentation and dynamical properties of a massive starless gas clump at the onset of high-mass star formation. Methods: Based on Herschel continuum data we identify a massive gas clump that remains far-infrared dark up to 100mum wavelengths. The fragmentation and dynamical properties are investigated by means of Plateau de Bure Interferometer and Nobeyama 45m single-dish spectral line and continuum observations. Results: The massive gas reservoir fragments at spatial scales of ~18000AU in four cores. Comparing the spatial extent of this high-mass region with intermediate- to low-mass starless cores from the literature, we find that linear sizes do not vary significantly over the whole mass regime. However, the high-mass regions squeeze much more gas into these similar volumes and hence have orders of magnitude larger densities. The fragmentation properties of the presented low-to high-mass regions are consistent with gravitational instable Jeans fragmentation. Furthermore, we find multipl...

  6. Influence of university network structures on forming the network environment of regional economy (on the example of national research universities of Tatarstan Republic

    Directory of Open Access Journals (Sweden)

    Darya-Anna Alekseevna Kaibiyainen

    2015-03-01

    Full Text Available Objective to elaborate theoretical and applied aspects of the processes of forming the new network institutional environment of the Russian regional economy under the influence of the developing integral educational network structures basing on the study of the experience of national research universities of Tatarstan Republic Methods general scientific logical methods of analysis and synthesis induction and deduction scientific abstraction as well as the method of systemicfunctional analysis. Results the practical examples are revealed and analyzed of introducing the new network integral principles into the functioning of national research universities which have a real economic effect and influencing such indicators of regional economy as the growth of employment reduction of unemployment etc. Scientific novelty problems of network structures development in the Russian education have not been thoroughly studied yet. The article analyzes the experience reveals and describes the methods and techniques of forming the network educational structures in the functioning of national research universities in Tatarstan Republic Practical value the author shows the ability of network university structures not only to play a significant role forming the new institutional environment of the regional economy but also to influence the macro and microeconomic indicators of development of the region and the country. nbsp

  7. Farm level survey of spore-forming bacteria on four dairy farms in the Waikato region of New Zealand.

    Science.gov (United States)

    Gupta, Tanushree B; Brightwell, Gale

    2017-03-03

    The aim of our study was to determine the occurrence and diversity of economically important spore-forming bacteria in New Zealand dairy farm systems. Farm dairy effluent (FDE) collected from Waikato dairy farms were tested for the presence of spore-forming bacteria, using a new culture-based methodology followed by genomic analysis. An enrichment step in which samples were inoculated in cooked meat glucose starch broth under anaerobic conditions, aided in the differential isolation of Bacillus and Clostridium species. Furthermore, the use of molecular methods such as ERIC genotyping, 16S rRNA gene sequence analysis identified different spore-forming bacteria present in FDE. C. sporogenes signature PCR gave further information on the phylogenetic relationship of the different Clostridium spp. isolated in this study. In total 19 Bacillus spp., 5 Paenibacillus spp. and 17 Clostridium spp. were isolated from farm dairy effluent. Sequence types similar to economically important food spoilage bacteria viz: C. butyricum, C. sporogenes and members of the Paenibacillus Genus were isolated from all four farms, whereas, sequence types similar to potential toxigenic, B. cereus, C. perfringens, C. butyricum, and C. botulinum were found on at least three of the farms. Sampling of farm dairy effluent provides a good indicator of farm level prevalence of bacterial load as it is used to irrigate dairy pasture in New Zealand. This study highlights the presence of various spore-forming bacteria in dairy waste water and indicates the implementation of good hygienic farm practices and dairy waste effluent management.

  8. Trigonometric Parallaxes of Massive Star-Forming Regions: VII. G9.62+0.20 and the Expanding 3 KPC-ARM

    CERN Document Server

    Sanna, A; Moscadelli, L; Dame, T M; Menten, K M; Brunthaler, A; Zheng, X W; Xu, Y

    2009-01-01

    We report a trigonometric parallax of 12 GHz methanol masers associated with the massive star forming region G9.62+0.20, corresponding to a distance of 5.2+-0.6 kpc. With a local standard of rest velocity of about 2 km/s, the region's kinematic distances of 0.5 and 16 kpc differ greatly from the distance derived here. Our measurement of the peculiar motion of the star forming region shows a very large deviation from a circular Galactic orbit: 41 km/s radially outward from the Galactic center and 60 km/s counter to Galactic rotation. The combination of its radial velocity and distance places G9.62+0.20 in the inner region of the Galaxy close to the Expanding Near 3 kpc-Arm, where the bulge/bar potential has strong gravitational influence. We also map the distribution of 12 GHz methanol masers, locate them with respect to a hypercompact H II region, and compare our data with the periodic flare phenomenon reported previously for this source.

  9. The Herschel M33 extended survey (HerM33es): PACS spectroscopy of the star forming region BCLMP 302

    CERN Document Server

    Mookerjea, B; Buchbender, C; Boquien, M; Verley, S; Relano, M; Quintana-Lacaci, G; Aalto, S; Braine, J; Calzetti, D; Combes, F; Garcia-Burillo, S; Gratier, P; Henkel, C; Israel, F; Lord, S; Nikola, T; Roellig, M; Stacey, G; Tabatabaei, F S; van der Tak, F; van der Werf, P

    2011-01-01

    Context: The emission line of [CII] at 158 micron is one of the strongest cooling lines of the interstellar medium (ISM) in galaxies. Aims: Disentangling the relative contributions of the different ISM phases to [CII] emission, is a major topic of the HerM33es program, a Herschel key project to study the ISM in the nearby spiral galaxy M33. Methods: Using PACS, we have mapped the emission of [CII] 158 micron, [OI] 63 micron, and other FIR lines in a 2'x2' region of the northern spiral arm of M33, centered on the HII region BCLMP302. At the peak of H-alpha emission, we have observed in addition a velocity resolved [CII] spectrum using HIFI. We use scatterplots to compare these data with PACS 160 micron continuum maps, and with maps of CO and HI data, at a common resolution of 12 arcsec or 50 pc. Maps of H-alpha and 24 micron emission observed with Spitzer are used to estimate the SFR. We have created maps of the [CII] and [OI] 63 micron emission and detected [NII] 122 micron and NIII 57 micron at individual po...

  10. CHARACTERIZING THE EMBEDDED YOUNG STELLAR OBJECTS IN THE GALACTIC STAR-FORMING REGION IRAS 18236-1205

    Directory of Open Access Journals (Sweden)

    R. Retes

    2011-01-01

    Full Text Available Presentamos un estudio multibanda de candidatos a objetos jóvenes estelares (YSOs embebidos en la nube molecular galáctica asociada con la fuente IRAS 18236-1205. Para identificar y clasificar a los YSOs embebidos en la nube molecular se usan los datos de 2MASS, Spitzer/IRAC, Spitzer/MIPS a 24 ¿Êm y gas molecular 13CO(J=1-0. Se encuentran dos regiones con formación estelar activa, una localizada en la región central de la nube molecular asociada con la posición de la fuente IRAS y otra al Norte-Oeste de la fuente IRAS. Estas regiones están asociadas a su vez con nubes infrarrojas oscuras (IRDCs y muestran una fenomenología que está de acuerdo con la fase temprana denominada "Hot Molecular Core", del proceso de la formación estelar de alta masa.

  11. Tethered domains and flexible regions in tRNase Z(L, the long form of tRNase Z.

    Directory of Open Access Journals (Sweden)

    Christopher Wilson

    Full Text Available tRNase Z, a member of the metallo-β-lactamase family, endonucleolytically removes the pre-tRNA 3' trailer in a step central to tRNA maturation. The short form (tRNase Z(S is the only one found in bacteria and archaebacteria and is also present in some eukaryotes. The homologous long form (tRNase Z(L, exclusively found in eukaryotes, consists of related amino- and carboxy-domains, suggesting that tRNase Z(L arose from a tandem duplication of tRNase Z(S followed by interdependent divergence of the domains. X-ray crystallographic structures of tRNase Z(S reveal a flexible arm (FA extruded from the body of tRNase Z remote from the active site that binds tRNA far from the scissile bond. No tRNase Z(L structures have been solved; alternative biophysical studies are therefore needed to illuminate its functional characteristics. Structural analyses of tRNase Z(L performed by limited proteolysis, two dimensional gel electrophoresis and mass spectrometry establish stability of the amino and carboxy domains and flexibility of the FA and inter-domain tether, with implications for tRNase Z(L function.

  12. Phylogenetic relationships of intraspecific forms of the house mouse Mus musculus: Analysis of variability of the control region (D-loop) of mitochondrial DNA.

    Science.gov (United States)

    Maltsev, A N; Stakheev, V V; Bogdanov, A S; Fomina, E S; Kotenkova, E V

    2015-11-01

    Analysis of the control region of mitochondrial DNA (mtDNA) or D-loop of 96 house mice (Mus musculus) from Russia, Moldova, Armenia, Azerbaijan, Kazakhstan, and Turkmenistan has been used to reconstruct the phylogenetic relationships and phylogeographic patterns of intraspecific forms. New data on the phylogenetic structure of the house mouse are presented. Three phylogroups can be reliably distinguished in the eastern part of the M. musculus species range, the first one mainly comprising the haplotypes of mice from Transcaucasia (Armenia); the second one, the haplotypes of mice from Kazakhstan; and the third one, the haplotypes of mice from Siberia and some other regions. The morphological subspecies M. m. wagneri and M. m. gansuensis have proved to be genetically heterogeneous and did not form discrete phylogroups in the phylogenetic tree.

  13. Cloud Structure of Galactic OB Cluster-forming Regions from Combining Ground- and Space-based Bolometric Observations

    Science.gov (United States)

    Lin, Yuxin; Liu, Hauyu Baobab; Li, Di; Zhang, Zhi-Yu; Ginsburg, Adam; Pineda, Jaime E.; Qian, Lei; Galván-Madrid, Roberto; McLeod, Anna Faye; Rosolowsky, Erik; Dale, James E.; Immer, Katharina; Koch, Eric; Longmore, Steve; Walker, Daniel; Testi, Leonardo

    2016-09-01

    We have developed an iterative procedure to systematically combine the millimeter and submillimeter images of OB cluster-forming molecular clouds, which were taken by ground-based (CSO, JCMT, APEX, and IRAM-30 m) and space telescopes (Herschel and Planck). For the seven luminous (L\\gt {10}6 L ⊙) Galactic OB cluster-forming molecular clouds selected for our analyses, namely W49A, W43-Main, W43-South, W33, G10.6-0.4, G10.2-0.3, and G10.3-0.1, we have performed single-component, modified blackbody fits to each pixel of the combined (sub)millimeter images, and the Herschel PACS and SPIRE images at shorter wavelengths. The ˜10″ resolution dust column density and temperature maps of these sources revealed dramatically different morphologies, indicating very different modes of OB cluster-formation, or parent molecular cloud structures in different evolutionary stages. The molecular clouds W49A, W33, and G10.6-0.4 show centrally concentrated massive molecular clumps that are connected with approximately radially orientated molecular gas filaments. The W43-Main and W43-South molecular cloud complexes, which are located at the intersection of the Galactic near 3 kpc (or Scutum) arm and the Galactic bar, show a widely scattered distribution of dense molecular clumps/cores over the observed ˜10 pc spatial scale. The relatively evolved sources G10.2-0.3 and G10.3-0.1 appear to be affected by stellar feedback, and show a complicated cloud morphology embedded with abundant dense molecular clumps/cores. We find that with the high angular resolution we achieved, our visual classification of cloud morphology can be linked to the systematically derived statistical quantities (i.e., the enclosed mass profile, the column density probability distribution function (N-PDF), the two-point correlation function of column density, and the probability distribution function of clump/core separations). In particular, the massive molecular gas clumps located at the center of G10.6-0.4 and

  14. Analysis of MOST light curves of five young stars in Taurus-Auriga and Lupus~3 Star Forming Regions

    CERN Document Server

    Siwak, Michal; Matthews, Jaymie M; Kuschnig, Rainer; Guenther, David B; Moffat, Anthony F J; Sasselov, Dimitar; Weiss, Werner W

    2011-01-01

    Continuous photometric observations of five young stars obtained by the MOST satellite in 2009 and 2010 in the Taurus and Lupus star formation regions are presented. Using light curve modelling under the assumption of internal invariability of spots, we obtained small values of the solar-type differential-rotation parameter (k=0.0005-0.009) for three spotted weak-line T Tau stars, V410 Tau, V987 Tau and Lupus 3-14; for another spotted WTTS, Lupus 3-48, the data are consistent with a rigidly rotating surface (k=0). Three flares of similar rise (4 min 30 sec) and decay (1 h 45 min) times were detected in the light curve of Lupus 3-14. The brightness of the classical T Tau star RY Tau continuously decreased over 3 weeks of its observations with a variable modulation not showing any obvious periodic signal.

  15. Introduction of the flora, life forms and chorology of plants of some regions in western Chabahar (Sistan and Baluchestan Province

    Directory of Open Access Journals (Sweden)

    Somayeh Salimi

    2014-12-01

    Full Text Available This study focused on Zarabad, Cheraghabad and Nogombecom plants of sub-basin watershed city of Chabahar, Iran. The studied flora included 78 species which belonged to 66 genera and 29 families. Poaceae with 16 genera and 19 species, Asteraceae with 7 genera and 8 species, Chenopodiaceae with 5 genera and 4 species, Papilionaceae, with 5 genera and 6 species, constituted the largest plant families respectively. The largest genera of the region were: Salsola, Heliotropium and Plantago, respectively. 42% of the flora belonged to Nobo-Sindian elements, 35%to Irano-Turanian, 18%were bioregional elements and 5% of the species were cosmopolitan. Flora of the studied area, included therophytes (56%, chamaephytes (15%, phanerophytes (14%, geophytes (12% and hemicryptophytes (3%.

  16. Comparing the model forms estimating generalised diameter-height relationships in Tecomella undulata plantations in hot arid region of India

    Institute of Scientific and Technical Information of China (English)

    Vindhya Prasad Tewari

    2007-01-01

    Four generalised diameter-height equations were developed and compared for pure and even-aged stands of Tecomella undulata in hot arid region of Rajasthan State in India. The data used to fit the equations consisted of 1 540 diameter-height observations collected from the plots laid out in uniformly stocked stands of varying age and density. The performance of four equations was tested by non-linear least squares regression and evaluated using different statistical criteria. Finally, these equations, with the same values of coefficients obtained during the fitting phase, were validated by an independent data set consisting of 854 diameter-height observations. Overall, equation (4) (Hui and Gadow function) was found to perform best for both the fitting data set as well as validation data set.

  17. Water deuterium fractionation in the high-mass star-forming region G34.26+0.15 based on Herschel/HIFI data

    DEFF Research Database (Denmark)

    Coutens, Audrey; Vastel, C.; Hincelin, U.;

    2014-01-01

    Understanding water deuterium fractionation is important for constraining the mechanisms of water formation in interstellar clouds. Observations of HDO and H_2^{18}O transitions were carried out towards the high-mass star-forming region G34.26+0.15 with the Heterodyne Instrument for the Far-Infrared...... to an age of ˜105 yr after the infrared dark cloud stage....

  18. Limits to diffusive O2 transport: flow, form, and function in nudibranch egg masses from temperate and polar regions.

    Directory of Open Access Journals (Sweden)

    Amy L Moran

    Full Text Available BACKGROUND: Many aquatic animals enclose embryos in gelatinous masses, and these embryos rely on diffusion to supply oxygen. Mass structure plays an important role in limiting or facilitating O2 supply, but external factors such as temperature and photosynthesis can play important roles as well. Other external factors are less well understood. METHODOLOGY/PRINCIPAL FINDINGS: We first explored the effects of water flow on O2 levels inside nudibranch embryo masses and compared the effects of flow on masses from temperate and polar regions. Water flow (still vs. vigorously bubbled had a strong effect on central O2 levels in all masses; in still water, masses were considerably more hypoxic than in bubbled water. This effect was stronger in temperate than in polar masses, likely due to the increased metabolic demand and O2 consumption of temperate masses. Second, we made what are to our knowledge the first measurements of O2 in invertebrate masses in the field. Consistent with laboratory experiments, O2 in Antarctic masses was high in masses in situ, suggesting that boundary-layer effects do not substantially limit O2 supply to polar embryos in the field. CONCLUSIONS/SIGNIFICANCE: All else being equal, boundary layers are more likely to depress O2 in masses in temperate or tropical regions; thus, selection on parents to choose high-flow sites for mass deposition is likely greater in warm water. Because of the large number of variables affecting diffusive O2 supply to embryos in their natural environment, field observations are necessary to test hypotheses generated from laboratory experiments and mathematical modeling.

  19. Limits to diffusive O2 transport: flow, form, and function in nudibranch egg masses from temperate and polar regions.

    Science.gov (United States)

    Moran, Amy L; Woods, H Arthur

    2010-08-11

    Many aquatic animals enclose embryos in gelatinous masses, and these embryos rely on diffusion to supply oxygen. Mass structure plays an important role in limiting or facilitating O2 supply, but external factors such as temperature and photosynthesis can play important roles as well. Other external factors are less well understood. We first explored the effects of water flow on O2 levels inside nudibranch embryo masses and compared the effects of flow on masses from temperate and polar regions. Water flow (still vs. vigorously bubbled) had a strong effect on central O2 levels in all masses; in still water, masses were considerably more hypoxic than in bubbled water. This effect was stronger in temperate than in polar masses, likely due to the increased metabolic demand and O2 consumption of temperate masses. Second, we made what are to our knowledge the first measurements of O2 in invertebrate masses in the field. Consistent with laboratory experiments, O2 in Antarctic masses was high in masses in situ, suggesting that boundary-layer effects do not substantially limit O2 supply to polar embryos in the field. All else being equal, boundary layers are more likely to depress O2 in masses in temperate or tropical regions; thus, selection on parents to choose high-flow sites for mass deposition is likely greater in warm water. Because of the large number of variables affecting diffusive O2 supply to embryos in their natural environment, field observations are necessary to test hypotheses generated from laboratory experiments and mathematical modeling.

  20. Measurement of the pion form factor at BESIII in the rho-peak region relevant for (g — 2)μ

    Science.gov (United States)

    Redmer, C. F.; BESIII Collaboration

    2016-11-01

    Measurements of hadronic cross sections in e+e- collisions are an important input for the Standard Model calculations of the hadronic contribution to the anomalous magnetic moment of the muon, (g — 2)μ. We present a new measurement of the cross section e+e- → π+π-, the pion form factor, which dominates the hadronic contribution. Using the method of initial state radiation, 2.93 fb-1 of data taken with the BESIII detector at the ψ (3770) peak have been evaluated to determine the cross section in the energy range between 600 and 900 MeV with a systematic uncertainty of 0.9%. The new BESIII data are compared to previous measurements by KLOE and BaBar, and their impact on (g — 2)μ is discussed.

  1. The Features of Forming and Using the Finansial and Material Resources of Socially Oriented Non-Profit Organizations of Volgograd Region

    Directory of Open Access Journals (Sweden)

    Oleynik Olga Stepanovna

    2014-12-01

    Full Text Available The article deals with the problem of interaction of regional authorities and the institute of socially oriented non-profit organizations that carry out the activity aimed at solving social problems, the development of civil society in Russia. The forms and activities of socially oriented non-profit organizations are systematically presented. The authors reveal the directions and tools for supporting the activities of socially oriented non-profit organizations by public authorities and local self-government bodies. The authors aimed at fixing the peculiarities of organization and conduct of statistical observation over the activity of socially-oriented organizations in Volgograd region. The organizational events were arranged. They were necessary for the conduct of qualitative statistical analysis of the activity of socially oriented organizations. For the first time the official data on the activity of socially oriented non-profit organizations in Volgograd region, including the information on formation and use of money and other property, was received as a result of the statistical observation. The authors focus on the analysis of the sources of money and other property, reveal the composition of income in non-profit organizations of various organizational and legal forms. The forms of work in socially oriented non-profit organizations of Volgograd region and its results as of 2013 are thoroughly studied. The conducted statistical analysis showed that the significant public sector has been established in the region. It provides the necessary public social services, financial or social assistance to the most vulnerable members of society.

  2. Insights from Synthetic Star-forming Regions: II. Verifying Dust Surface Density, Dust Temperature & Gas Mass Measurements with Modified Blackbody Fitting

    CERN Document Server

    Koepferl, Christine M; Dale, James E

    2016-01-01

    We use a large data-set of realistic synthetic observations (PaperI) to assess how observational techniques affect the measurement of physical properties of star-forming regions. In this paper (PaperII), we explore the reliability of the measured total gas mass, dust surface density and dust temperature maps derived from modified blackbody fitting of synthetic Herschel observations. We found from our pixel-by-pixel analysis of the measured dust surface density and dust temperature a worrisome error spread especially close to star-formation sites and low-density regions, where for those "contaminated" pixels the surface densities can be under/overestimated by up to three orders of magnitude. In light of this, we recommend to treat the pixel-based results from this technique with caution in regions with active star formation. In regions of high background typical in the inner Galactic plane, we are not able to recover reliable surface density maps of individual synthetic regions, since low-mass regions are lost...

  3. A UKIDSS-based search for low-mass stars and small stellar clumps in off-cloud parts of young star-forming regions* **

    Directory of Open Access Journals (Sweden)

    Barrado y Navascués D.

    2011-07-01

    Full Text Available The form and universality of the mass function of young and nearby star-forming regions is still under debate. Its relation to the stellar density, its mass peak and the dependency on most recent models shows significant differencies for the various regions and remains unclear up to date. We aim to get a more complete census of two of such regions. We investigate yet unexplored areas of Orion and Taurus-Auriga, observed by the UKIDSS survey. In the latter, we search for low-mass stars via photometric and proper motion criteria and signs for variability. In Orion, we search for small stellar clumps via nearest-neighbor methods. Highlights in Taurus would be the finding of the missing low-mass stars and the detection of a young cluster T dwarf. In Orion, we discovered small stellar associations of its OB1b and OB1c populations. Combined with what is known in literature, we will provide by this investigations a general picture of the results of the star-forming processes in large areas of Taurus and Orion and probe the most recent models.

  4. A quality check of the $AKARI$ mid-infrared all-sky diffuse map toward the massive star-forming regions NGC 6334 and NGC 6357

    CERN Document Server

    Sano, Hidetoshi; Kondo, Toru; Nakamichi, Keichiro; Yamagishi, Mitsuyoshi; Ishihara, Daisuke; Oyabu, Shinki; Kaneda, Hidehiro; Tachihara, Kengo; Fukui, Yasuo

    2016-01-01

    We present a comparative study of CO and polycyclic aromatic hydrocarbon (PAH) emission toward a region including the massive star-forming regions of NGC 6334 and NGC 6357. We use the NANTEN $^{12}$CO($J$ = 1--0) data and the $AKARI$ 9 $\\mu$m All-Sky diffuse map in order to evaluate the calibration accuracy of the $AKARI$ data. We confirm that the overall CO distribution shows a good spatial correspondence with the PAH emission, and their intensities exhibit a good power-law correlation with a spatial resolution down to 4$'$ over the region of 10$^\\circ$$\\times$10$^\\circ$. We also reveal poorer correlation for small scale structures between the two quantities toward NGC 6357, due to strong UV radiation from local sources. Larger scatter in the correlation toward NGC 6357 indicates higher ionization degree and/or PAH excitation than that of NGC 6334.

  5. The Precise Radio Observation of the 13C Isotopic Fractionation for Carbon Chain Molecule HC3N in the Low-Mass Star Forming Region L1527

    Science.gov (United States)

    Araki, Mitsunori; Takano, Shuro; Sakai, Nami; Yamamoto, Satoshi; Oyama, Takahiro; Kuze, Nobuhiko; Tsukiyama, Koichi

    2016-06-01

    We observed the three 13C isotopic species of HC3N with the high signal-to-noise ratios in L1527 using Green Bank 100 m telescope and Nobeyama 45 m telescope to explore the production scheme of HC3N, where L1527 is the low-mass star forming region in the phase of a warm carbon chain chemistry region. The spectral lines of the J = 5--4, 9--8, 10--9, and 12--11 transitions in the 44-109 GHz region were used to measure isotopic ratios. The abundance of HCCCN was determined from the line intensities of the two weak hyperfine components of the J = 5-4 transition. The isotopic ratios were precisely determined to be 1.00 : 1.01 : 1.35 : 86.4 for [H13CCCN] : [HC13CCN] : [HCC13CN] : [HCCCN]. It was found that the abundance of H13CCCN is equal to that of HC13CCN, and it was implied that HC3N is mainly formed by the reaction schemes via C2H2 and C2H2+ in L1527. This would suggest a universality of dicarbide chemistry producing HC3N irrespective of evolutional phases from a starless dark cloud to a warm carbon chain chemistry region. Sakai, N., Sakai, T., Hirota, T., & Yamamoto, S. 2008, ApJ, 672, 371 Takano, S., Masuda, A., Hirahara, Y., et al. 1998, A&A, 329, 1156

  6. Short forms of the Utrecht-Management of Identity Commitments Scale (U-MICS) with the domains of job, romantic relationship, and region.

    Science.gov (United States)

    Schubach, Elisabeth; Zimmermann, Julia; Noack, Peter; Neyer, Franz J

    2017-01-01

    The U-MICS is a self-report questionnaire designed to assess the identity dimensions from a domain-specific perspective. The present study reports on the development of a short-form version for the domains of job and romantic relationship in young adults from Germany and extends this scale to include the domain of region (nSample1 = 95, 84% female, mean age 22.45 years; nSample2 = 1,795, 71% female, mean age 24.53 years). We found the short form to possess adequate psychometric properties and to demonstrate a factor structure congruent to the long-form version. Regarding validity, the small correlations across domains within dimensions support a domain-specific approach to identity. The associations between the different identity domains with personality traits are similar, indicating a consistent pattern of convergent validity for all domains. We conclude that "region" provides a valuable complement to the established domains that can all be reliably assessed with the U-MICS-Short Form. Copyright © 2016 The Foundation for Professionals in Services for Adolescents. Published by Elsevier Ltd. All rights reserved.

  7. Radiative transfer models of mid-infrared H2O lines in the Planet-forming Region of Circumstellar Disks

    CERN Document Server

    Meijerink, R; Blake, G A; Poelman, D R; Dullemond, C P

    2009-01-01

    The study of warm molecular gas in the inner regions of protoplanetary disks is of key importance for the study of planet formation and especially for the transport of H2O and organic molecules to the surfaces of rocky planets/satellites. Recent Spitzer observations have shown that the mid-infrared spectra of protoplanetary disks are covered in emission lines due to water and other molecules. Here, we present a non-LTE 2D radiative transfer model of water lines in the 10-36 mum range that can be used to constrain the abundance structure of water vapor, given an observed spectrum, and show that an assumption of local thermodynamic equilibrium (LTE) does not accurately estimate the physical conditions of the water vapor emission zones. By applying the model to published Spitzer spectra we find that: 1) most water lines are subthermally excited, 2) the gas-to-dust ratio must be one to two orders of magnitude higher than the canonical interstellar medium ratio of 100-200, and 3) the gas temperature must be higher...

  8. X-Ray Emission from Young Stars in the Massive Star Forming Region IRAS 20126+4104

    CERN Document Server

    Anderson, Crystal Nicole; Shepherd, Debra; Creech-Eakman, Michelle

    2011-01-01

    We present a $40\\,$ks Chandra observation of the IRAS$\\,$20126+4104 core region. In the inner $6^{\\prime\\prime}$ two X-ray sources were detected, which are coincident with the radio jet source I20S and the variable radio source I20Var. No X-ray emission was detected from the nearby massive protostar I20N. The spectra of both detected sources are hard and highly absorbed, with no emission below $3\\,$keV. For I20S, the measured $0.5-8\\,$keV count rate was $4.3\\,$cts$\\,$ks$^{-1}$. The X-ray spectrum was fit with an absorbed 1T APEC model with an energy of kT$\\,=10\\,$keV and an absorbing column of N$_H = 1.2\\times 10^{23}\\,$cm$^{-2}$. An unabsorbed X-ray luminosity of about $1.4\\times 10^{32}\\,$erg$\\,$s$^{-1}$ was estimated. The spectrum shows broad line emission between 6.4 and 6.7\\, keV, indicative of emission from both neutral and highly ionized iron. The X-ray lightcurve indicates that I20S is marginally variable; however, no flare emission was observed. The variable radio source I20Var was detected with a co...

  9. Magnetic Field Structures in Star Forming Regions: Mid-Infrared Imaging Polarimetry of K3-50

    CERN Document Server

    Barnes, Peter; Telesco, Charles; Tanakul, Nahathai; Mariñas, Naibí; Wright, Chris; Packham, Chris; Pantin, Eric; Roche, Patrick; Hough, James

    2015-01-01

    We report new imaging polarimetry observations of the Galactic compact HII region K3-50 using CanariCam at the Gran Telescopio Canarias. We use a standard polarimetric analysis technique, first outlined by Aitken, to decompose the observed polarisation images centred at 8.7, 10.3, and 12.5 $\\mu$m into the emissive and absorptive components from silicate grains that are aligned with the local magnetic field. These components reveal the spatially-resolved magnetic field structures across the mid-infrared emission area of K3-50. We examine these structures and show that they are consistent with previously observed features and physical models of K3-50, such as the molecular torus and the ionised outflow. We propose a 3D geometry for all the structures seen at different wavelengths. We also compute relevant physical quantities in order to estimate the associated magnetic field strengths that would be implied under various physical assumptions. We compare these results with MHD simulations of protostar formation t...

  10. The coal-forming plants of the upper part of the Lower Cretaceous Starosuchan Formation (Partizansk Basin, South Primorye region)

    Science.gov (United States)

    Bugdaeva, E. V.; Markevich, V. S.; Volynets, E. B.

    2014-05-01

    The plant remains and palynological assemblages are studied in detail in the section of the coal-bearing upper part of the Aptian Starosuchan Formation near the village of Molchanovka (Partizansk Basin, South Primorye region). On the basis of the light and electron microscopic study of the disperse cuticles, it was established that the coals are mostly composed of remains of taxodialean Elatides asiatica (Yok.) Krassil., subordinate Miroviaceae, rare ginkgoalean Pseudotorellia sp., and bennettite Nilssoniopteris rithidorachis (Krysht.) Krassil. The spores Gleicheniidites and pollen Taxodiaceaepollenites are dominant in the palynospectrum of the coal interlayer. It was found that dominant taxodialeans and gleicheniaceous ferns with less abundant Miroviaceae, ginkgoaleans, and rare bennettites occurred in the Aptian swamp communities of the Partizansk basin. Shoots and leaves of Elatides asiatica, fronds of Birisia onychioides (Vassil. et K.-M.) Samyl., are dominant in the burials of plants from the clastic rocks. The fragments of leaves of Nilssoniopteris, scale-leaved conifers, and Ginkgo ex gr. adiantoides are rare. The disperse cuticle of these layers mostly includes Pseudotorellia sp.; however, its remains in burials were not found. The spores Laevigatosporites are dominant in the palynospectra from the clastic interlayers. Ginkgocycadophytus and taxa close to Pinaceae are plentiful among the pollen of gymnosperms.

  11. L1157-B1, a factory of complex organic molecules in a solar-type star-forming region

    Science.gov (United States)

    Lefloch, Bertrand; Ceccarelli, C.; Codella, C.; Favre, C.; Podio, L.; Vastel, C.; Viti, S.; Bachiller, R.

    2017-07-01

    We report on a systematic search for oxygen-bearing complex organic molecules (COMs) in the solar-like protostellar shock region L1157-B1, as part of the IRAM Large Program 'Astrochemical Surveys At IRAM'. Several COMs are unambiguously detected, some for the first time, such as ketene H2CCO, dimethyl ether (CH3OCH3) and glycolaldehyde (HCOCH2OH), and others firmly confirmed, such as formic acid (HCOOH) and ethanol (C2H5OH). Thanks to the high sensitivity of the observations and full coverage of the 1, 2 and 3 mm wavelength bands, we detected numerous (˜10-125) lines from each of the detected species. Based on a simple rotational diagram analysis, we derive the excitation conditions and the column densities of the detected COMs. Combining our new results with those previously obtained towards other protostellar objects, we found a good correlation between ethanol, methanol and glycolaldehyde. We discuss the implications of these results on the possible formation routes of ethanol and glycolaldehyde.

  12. A GALEX based search for the sparse young stellar population in the Taurus-Aurigae star forming region

    CERN Document Server

    de Castro, Ana I Gomez; López-Martínez, Fátima; Sánchez, Néstor; Sestito, Paola; de Castro, Elisa; Cornide, Manuel; Gestoso, Javier Yañez

    2014-01-01

    In this work, we identify 63 bona fide new candidates to T Tauri stars (TTSs) in the Taurus-Auriga region using as baseline its ultraviolet excess. The initial data set has been defined from the GALEX all sky survey (AIS). The GALEX satellite obtained images in the near ultraviolet (NUV) and far ultraviolet (FUV) bands where the TTSs show a prominent excess, compared with main sequence or giants stars. GALEX AIS surveyed the Taurus-Auriga molecular complex, as well as, a fraction of the California Nebula and the Perseus complex; bright sources and the dark clouds themselves are avoided. The properties of the TTSs in the ultraviolet (GALEX), optical (UCAC4) and infrared (2MASS) have been defined using as qualification sample the TTSs observed with the International Ultraviolet Explorer. The candidates have been identified by means of a mixed ultraviolet-optical-infrared excess set of colors; it is found that the color-color diagram FUV-NUV versus J-K is ideally suited for this purpose. From an initial sample o...

  13. [Topsoil phosphorus forms and availability of different soil and water conservation plantations in typical black soil region, northeast China].

    Science.gov (United States)

    Yang, Xiao-Yan; Fan, Rui-Ying; Wang, En-Heng; Xia, Xiang-You; Chen, Xiang-Wei

    2014-06-01

    Aiming to understand soil phosphorus status of plantations in typical black soil region of Northeast China, the topsoil (0-10 cm) phosphorus fractionations and its availability were examined in four soil and water conservation plantations dominantly composed of Larix gmelini, Fraxinus mandshurica, Pinus sylvestris var. mongolica and Populus nigra var. italica x P. cathayan, respectively. The results showed that total P, Olsen-P and the concentration of different P fractionations in F. mandshurica and P. nigra var. italica x P. cathayan plantations were significantly higher than that of the other two coniferous plantations. Organic P was the major fractionation in the four plantations' topsoil, and sodium hydroxide extractable organic P (NaOH-Po ) representing moderately labile organic phosphorus was predominant, which accounted for 58.9% of total P. The contents of H2O-Pi and NaHCO3-P which were more labile to plant were lower, only accounting for 1.2% and 6.6% of total P, respectively. Except for NaHCO3-Po, all the other P fractions of four plantations correlated with each other, and they also had significant correlations with soil organic matter, total P, Olsen-P. Compared with the coniferous plantations, the broadleaf plantations presented higher availability of phosphorus.

  14. Trypanosoma cruzi: identification of a surface antigen restricted to the flagellar region of the infective form of the parasite.

    Science.gov (United States)

    Saborio, J L; Wrightsman, R A; Kazuko, S G; Granger, B S; Manning, J E

    1990-05-01

    A hybridoma cell line was derived from spleen cells of B6D2 mice infected with the Peru strain of Trypanosoma cruzi. The monoclonal antibody produced by this hybridoma, designated mAb20H1, reacts exclusively with molecular components of trypomastigotes, the infective form of the parasite. The results of indirect immunofluorescence and of immunoelectron microscopy with gold-tagged antibodies indicate that the 20H1 antigen is restricted to the surface of the part of the flagellum in contact with the cell body and to the surface of the cell body in the immediate vicinity of this organelle. Western blot analysis showed that the 20H1 antigen consists of four to five different molecules with sizes between 34 and 41 kDa, and that these molecules are glycoproteins with affinity for concanavalin A. In other strains of T. cruzi, mAb20H1 reacts with glycoproteins with apparent sizes that range between 37 and 43 kDa in the CL, Esmeraldo and Y strains, and between 41 and 45 kDa in the Silvio strain.

  15. PTF10iya: A short-lived, luminous flare from the nuclear region of a star-forming galaxy

    CERN Document Server

    Cenko, S Bradley; Kulkarni, S R; Strubbe, Linda E; Miller, Adam A; Butler, Nathaniel R; Quimby, Robert M; Gal-Yam, Avishay; Ofek, Eran O; Quataert, Eliot; Bildsten, Lars; Poznanski, Dovi; Perley, Daniel A; Morgan, Adam N; Filippenko, Alexei V; Arcavi, Iair; Ben-Ami, Sagi; Cucchiara, Antonio; Fassnacht, Christopher D; Green, Yoav; Hook, Isobel M; Howell, D Andrew; Lagattuta, David J; Law, Nicholas M; Kasliwal, Mansi M; Nugent, Peter E; Silverman, Jeffrey M; Sullivan, Mark; Tendulkar, Shriharsh P; Yaron, Ofer

    2011-01-01

    We present the discovery and characterisation of PTF10iya, a short-lived (dt ~ 10 d, with an optical decay rate of ~ 0.3 mag per d), luminous (M_g ~ -21 mag) transient source found by the Palomar Transient Factory. The ultraviolet/optical spectral energy distribution is reasonably well fit by a blackbody with T ~ 1-2 x 10^4 K and peak bolometric luminosity L_BB ~ 10^44 -10^45 erg per s (depending on the details of the extinction correction). A comparable amount of energy is radiated in the X-ray band that appears to result from a distinct physical process. The location of PTF10iya is consistent with the nucleus of a star-forming galaxy (z = 0.22405 +/- 0.00006) to within 350 mas (99.7 per cent confidence radius), or a projected distance of less than 1.2 kpc. At first glance, these properties appear reminiscent of the characteristic "big blue bump" seen in the near-ultraviolet spectra of many active galactic nuclei (AGNs). However, emission-line diagnostics of the host galaxy, along with a historical light cur...

  16. VizieR Online Data Catalog: W3 star-forming region 345 GHz survey (Helmich+ 1997)

    Science.gov (United States)

    Helmich, F. P.; van Dishoeck, E. F.

    1997-07-01

    Results are presented of the 345 GHz spectral survey toward three sources in the W 3 Giant Molecular Cloud: W 3 IRS4, W 3 IRS5 and W 3(H2O). Nearly 90% of the atmospheric window between 334 and 365GHz has been scanned using the James Clerk Maxwell Telescope (JCMT) down to a noise level of ~80mK per resolution element. These observations are complemented by a large amount of data in the 230GHz atmospheric window. From this data set physical conditions and beam-averaged column densities are derived for more than 14 chemically different species (over 24 different isotopes). The physical parameters derived in Paper I (Helmich et al., 1994A&A...283..626H) are confirmed by the analysis of the excitation of other species, although there is evidence that the silicon- and sulfur-bearing molecules exist in a somewhat denser and warmer environment. The densities are high, >=106cm-3, in the three sources and the kinetic temperatures for the bulk of the gas range from 55K for IRS4 to 220K for W 3(H2O). The chemical differences between the three sources are very striking: silicon- and sulfur-bearing molecules such as SiO and SO2 are prominent toward IRS5, whereas organic molecules like CH3OH, CH3OCH3 and CH3OCHO are at least an order of magnitude more abundant toward W 3(H2O). Vibrationally excited molecules are also detected toward this source. Only simple molecules are found toward IRS4. The data provide constraints on the amount of deuterium fractionation and the ionization fraction in the observed regions as well. These chemical characteristics are discussed in the context of an evolutionary sequence, in which IRS5 is the youngest, W 3(H2O) somewhat older and IRS4, although still enigmatic, the oldest. (6 data files).

  17. Genetic characterization and phylogenetic relationships based on 18S rRNA and ITS1 region of small form of canine Babesia spp. from India.

    Science.gov (United States)

    Mandal, M; Banerjee, P S; Garg, Rajat; Ram, Hira; Kundu, K; Kumar, Saroj; Kumar, G V P P S Ravi

    2014-10-01

    Canine babesiosis is a vector borne disease caused by intra-erythrocytic apicomplexan parasites Babesia canis (large form) and Babesia gibsoni (small form), throughout the globe. Apart from few sporadic reports on the occurrence of B. gibsoni infection in dogs, no attempt has been made to characterize Babesia spp. of dogs in India. Fifteen canine blood samples, positive for small form of Babesia, collected from northern to eastern parts of India, were used for amplification of 18S rRNA gene (∼1665bp) of Babesia sp. and partial ITS1 region (∼254bp) of B. gibsoni Asian genotype. Cloning and sequencing of the amplified products of each sample was performed separately. Based on sequences and phylogenetic analysis of 18S rRNA and ITS1 sequences, 13 were considered to be B. gibsoni. These thirteen isolates shared high sequence identity with each other and with B. gibsoni Asian genotype. The other two isolates could not be assigned to any particular species because of the difference(s) in 18S rRNA sequence with B. gibsoni and closer identity with Babesiaoccultans and Babesiaorientalis. In the phylogenetic tree, all the isolates of B. gibsoni Asian genotype formed a separate major clade named as Babesia spp. sensu stricto clade with high bootstrap support. The two unnamed Babesia sp. (Malbazar and Ludhiana isolates) clustered close together with B. orientalis, Babesia sp. (Kashi 1 isolate) and B. occultans of bovines. It can be inferred from this study that 18S rRNA gene and ITS1 region are highly conserved among 13 B. gibsoni isolates from India. It is the maiden attempt of genetic characterization by sequencing of 18S rRNA gene and ITS1 region of B. gibsoni from India and is also the first record on the occurrence of an unknown Babesia sp. of dogs from south and south-east Asia.

  18. A hemicentric inversion in the maize line knobless Tama flint created two sites of centromeric elements and moved the kinetochore-forming region.

    Science.gov (United States)

    Lamb, Jonathan C; Meyer, Julie M; Birchler, James A

    2007-06-01

    A maize line, knobless Tama flint (KTF), was found to contain a version of chromosome 8 with two spatially distinct regions of centromeric elements, one at the original genetic position and the other at a novel location on the long arm. The new site of centromeric elements functions as the kinetochore-forming region resulting in a change of arm length ratio. Examination of fluorescence in situ hybridization markers on chromosome 8 revealed an inversion between the two centromere sites relative to standard maize lines, indicating that this chromosome 8 resulted from a hemicentric inversion with one breakpoint approximately 20 centi-McClintocks (cMc) on the long arm (20% of the total arm length from the centromere) and the other in the original cluster of centromere repeats. This inversion moved the kinetochore-forming region but left the remainder of the centromere repeats. In a hybrid between a standard line (Mo17) and KTF, both chromosome 8 homologues were completely synapsed at pachytene despite the inversion. Although the homologous centromeres were not paired, they were always correctly oriented at anaphase and migrated to opposite poles. Additionally, recombination on 8L was severely repressed in the hybrid.

  19. Detection of interstellar oxidaniumyl: abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334

    CERN Document Server

    Ossenkopf, V; Lis, D C; Schilke, P; Bell, T A; Bruderer, S; Bergin, E; Ceccarelli, C; Comito, C; Stutzki, J; Bacman, A; Baudry, A; Benz, A O; Benedettini, M; Berne, O; Blake, G; Boogert, A; Bottinelli, S; Boulanger, F; Cabrit, S; Caselli, P; Caux, E; Cernicharo, J; Codella, C; Coutens, A; Crimier, N; Crockett, N R; Daniel, F; Demyk, K; Dieleman, P; Dominik, C; Dubernet, M L; Emprechtinger, M; Encrenaz, P; Falgarone, E; France, K; Fuente, A; Gerin, M; Giesen, T F; di Giorgio, A M; Goicoechea, J R; Goldsmith, P F; Güsten, R; Harris, A; Helmich, F; Herbst, E; Hily-Blant, P; Jacobs, K; Jacq, T; Joblin, Ch; Johnstone, D; Kahane, C; Kama, M; Klein, T; Klotz, A; Kramer, C; Langer, W; Lefloch, B; Leinz, C; Lorenzani, A; Lord, S D; Maret, S; Martin, P G; Martin-Pintado, J; McCoey, C; Melchior, M; Melnick, G J; Menten, K M; Mookerjea, B; Morris, P; Murphy, J A; Neufeld, D A; Nisini, B; Pacheco, S; Pagani, L; Parise, B; Pearson, J C; Pérault, M; Phillips, T G; Plume, R; Quin, S -L; Rizzo, R; Röllig, M; Salez, M; Saraceno, P; Schlemmer, S; Simon, R; Schuster, K; van der Tak, F F S; Tielens, A G G M; Teyssier, D; Trappe, N; Vastel, C; Viti, S; Wakelam, V; Walters, A; Wang, S; Whyborn, N; van der Wiel, M; Yorke, H W; Yu, S; Zmuidzinas, J

    2010-01-01

    We identify a prominent absorption feature at 1115 GHz, detected in first HIFI spectra towards high-mass star-forming regions, and interpret its astrophysical origin. The characteristic hyperfine pattern of the H2O+ ground-state rotational transition, and the lack of other known low-energy transitions in this frequency range, identifies the feature as H2O+ absorption against the dust continuum background and allows us to derive the velocity profile of the absorbing gas. By comparing this velocity profile with velocity profiles of other tracers in the DR21 star-forming region, we constrain the frequency of the transition and the conditions for its formation. In DR21, the velocity distribution of H2O+ matches that of the [CII] line at 158\\mu\\m and of OH cm-wave absorption, both stemming from the hot and dense clump surfaces facing the HII-region and dynamically affected by the blister outflow. Diffuse foreground gas dominates the absorption towards Sgr B2. The integrated intensity of the absorption line allows ...

  20. Time evolution of the high temperature region formed by laser induced breakdown and of the development of the flame kernel in the constant volume combustion vessel

    Science.gov (United States)

    Hayashi, J.; Nakatsuka, N.; Morimoto, I.; Akamatsu, F.

    2017-02-01

    The lean combustion is one of the key techniques for the advanced internal combustion systems due to the requirement of the higher thermal efficiency. Since the successful ignition must be guaranteed even in the lean combustion, advanced ignition systems have been developed in this decade. Laser ignition is one of the advanced ignition systems which have the profits of the flexibility in the position and the timing of ignition. To develop this ignition system for the actual combustion system, it is required to reveal the underlying physics of the laser ignition. Particularly, the time evolution of high temperature region formed by laser induced breakdown should be discussed. In this study, therefore, the time evolution of the high temperature region formed by the laser induced breakdown and the development of flame kernel were observed by using high-speed imaging. The ignition trials of methane/air lean premixed mixture were carried out in the constant volume combustion vessel to obtain minimum laser pulse energy for ignition (MPE). Results showed that the light emission from plasma formed by laser induced breakdown remained at least in several tens nano-seconds. In addition, there were large differences between the breakdown threshold and the MPE, which meant that the breakdown threshold did not determine the minimum pulse energy for ignition.

  1. Interorganisational networking as the principal form of technological, innovative and research cooperation between Russia and the European Union in the Baltic region

    Directory of Open Access Journals (Sweden)

    Bolychev Oleg

    2013-11-01

    Full Text Available This article concerns the role that international cooperation in research, technology, and innovation plays in ensuring innovative development and producing an innovative model of the Russian economy. One of the key objectives of the country’s integration into international research, technological, and innovative space is the development of Russia-EU cooperation in the Baltic region. It is established that, with the development of integration connections and regionalization processes, interorganizational networking takes on special importance in the organization and development of the innovative space. The authors analyze the existing typologies of forms of cooperation in the field of research, technology, and innovation, within which cases of networking are identified. The article gives a definition of interorganizational networks in view of the spatial and structural components of networking. The authors introduce the notion of international interorganizational networks as a special form of international cooperation. A study into the spatial form of interorganizational networks helps explain the effect of different levels and types of economic integration. Key areas of research on international interorganizational networks are identified in view of the features of integration processes in the development of network processes and in the framework of network approach in general.

  2. Interorganisational networking as the principal form of technological, innovative and research cooperation between Russia and the European Union in the Baltic region

    Directory of Open Access Journals (Sweden)

    Bolychev Oleg

    2013-01-01

    Full Text Available This article concerns the role that international cooperation in research, technology, and innovation plays in ensuring innovative development and producing an innovative model of the Russian economy. One of the key objectives of the country’s integration into international research, technological, and innovative space is the development of Russia-EU cooperation in the Baltic region. It is established that, with the development of integration connections and regionalization processes, interorganizational networking takes on special importance in the organization and development of the innovative space. The authors analyze the existing typologies of forms of cooperation in the field of research, technology, and innovation, within which cases of networking are identified. The article gives a definition of interorganizational networks in view of the spatial and structural components of networking. The authors introduce the notion of international interorganizational networks as a special form of international cooperation. A study into the spatial form of interorganizational networks helps explain the effect of different levels and types of economic integration. Key areas of research on international interorganizational networks are identified in view of the features of integration processes in the development of network processes and in the framework of network approach in general.

  3. Mid-infrared diagnostics of starburst galaxies: clumpy, dense structures in star-forming regions in the Antennae (NGC 4038/4039)

    CERN Document Server

    Snijders, Leonie; van der Werf, Paul P

    2007-01-01

    Recently, mid-infrared instruments have become available on several large ground-based telescopes, resulting in data sets with unprecedented spatial resolution at these long wavelengths. In this paper we examine 'ground-based-only' diagnostics, which can be used in the study of star-forming regions in starburst galaxies. By combining output from the stellar population synthesis code Starburst 99 with the photoionization code Mappings, we model stellar clusters and their surrounding interstellar medium, focusing on the evolution of emission lines in the N- and Q-band atmospheric windows (8-13 and 16.5-24.5 micron respectively) and those in the near-infrared. We address the detailed sensitivity of various emission line diagnostics to stellar population age, metallicity, nebular density, and ionization parameter. Using our model results, we analyze observations of two stellar clusters in the overlap region of the Antennae galaxies obtained with VLT Imager and Spectrometer for mid Infrared (VISIR). We find eviden...

  4. Stripped gas as fuel for newly formed HII regions in the encounter between VCC1249 and M49: a unified picture from NGVS and GUViCS

    CERN Document Server

    Battaia, Fabrizio Arrigoni; Fumagalli, Michele; Boselli, Alessandro; Boissier, Samuel; Cortese, Luca; Heinis, Sebastien; Ferrarese, Laura; Côté, Patrick; Mihos, J Christopher; Cuillandre, Jean Charles; Duc, Pierre-Alain; Durrell, Patrick; Gwyn, Stephen; Jordán, Andrés; Liu, Chengze; Peng, Eric

    2012-01-01

    Context: We study the peculiar interacting galaxy system of VCC1249/M49 located in the core of the Virgo B subcluster. Owing to a recent interaction between the dwarf galaxy VCC1249 and the halo gas of the gE M49, neutral hydrogen has been displaced from the interstellar medium of this dwarf into the Virgo ICM. Observations also reveal multiple compact star-forming regions that are embedded in this HI cloud, with a projected separation up to 13 kpc from VCC1249 in the northwest direction. Aims: Motivated by recent NUV imaging from GUViCS of the VCC1249/M49 system that shows significant ongoing/recent star formation in the compact regions, we aim to constrain the origin of these outlying HII regions with a multi-wavelength approach. Methods: Using deep optical (u, g, i, z) imaging from NGVS and new Halpha imaging obtained at the San Pedro Martir observatory together with Keck long-slit spectroscopy, we characterize the SFR, ages, and metallicity of VCC1249 and its outlying compact regions. Moreover, we analyze...

  5. Revealing the "missing" low-mass stars in the S254-S258 star forming region by deep X-ray imaging

    CERN Document Server

    Mucciarelli, Paola; Zinnecker, Hans

    2011-01-01

    (abbreviated) In the central part of the S254-S258 star forming complex, a dense embedded cluster of very young stellar objects (S255-IR) is sandwiched between the two HII regions S255 and S257. This interesting configuration had led to different speculations such as dynamical ejection of the B-stars from the central cluster or triggered star formation in a cloud that was swept up in the collision zone between the two expanding HII regions. The presence or absence of low-mass stars associated with these B-stars can discriminate between the possible scenarios. We performed a deep Chandra X-ray observation of the S254-S258 region in order to efficiently discriminate young stars from the numerous older field stars in the area. We detected 364 X-ray point sources, providing a complete sample of all young stars in the observed region down to ~0.5 Msun. A clustering analysis identifies three significant clusters, containing 64 X-ray sources in total. After accounting for X-ray background contaminants, this implies ...

  6. WFCAM, Spitzer-IRAC and SCUBA observations of the massive star forming region DR21/W75: II. Stellar content and star formation

    CERN Document Server

    Kumar, M S N; Grave, J M C; Froebrich, B F D

    2006-01-01

    Wide field near-infrared observations and Spitzer Space Telescope IRAC observations of the DR21/W75 star formation regions are presented. The photometric data are used to analyse the extinction, stellar content and clustering in the entire region by using standard methods. A young stellar population is identified all over the observed field, which is found to be distributed in embedded clusters that are surrounded by a distributed halo population extending over a larger projected area. The Spitzer/IRAC data are used to compute a spectral index value, "alpha", for each YSO in the field. We use these data to separate pure photospheres from disk excess sources. We find a small fraction of sources with "alpha" in excess of 2 to 3 (plus a handful with "alpha"~4), which is much higher than the values found in the low mass star forming region IC348 ("alpha" < 2). The sources with high values of "alpha" spatially coincide with the densest regions of the filaments and also with the sites of massive star formation. ...

  7. Semiconductor systems utilizing materials that form rectifying junctions in both N and P-type doping regions, whether metallurgically or field induced, and methods of use

    Science.gov (United States)

    Welch, James D.

    2000-01-01

    Disclosed are semiconductor systems, such as integrated circuits utilizing Schotky barrier and/or diffused junction technology, which semiconductor systems incorporate material(s) that form rectifying junctions in both metallurgically and/or field induced N and P-type doping regions, and methods of their use. Disclosed are Schottky barrier based inverting and non-inverting gate voltage channel induced semiconductor single devices with operating characteristics similar to multiple device CMOS systems and which can be operated as modulators, N and P-channel MOSFETS and CMOS formed therefrom, and (MOS) gate voltage controlled rectification direction and gate voltage controlled switching devices, and use of such material(s) to block parasitic current flow pathways. Simple demonstrative five mask fabrication procedures for inverting and non-inverting gate voltage channel induced semiconductor single devices with operating characteristics similar to multiple device CMOS systems are also presented.

  8. A Pan-STARRS1 Proper-Motion Survey for Young Brown Dwarfs in the Taurus and the Upper Scorpius Star-Forming Regions

    Science.gov (United States)

    Zhang, Zhoujian; Liu, Michael C.; Best, William M. J.; Magnier, Eugene A.; Aller, Kimberly Mei

    2017-01-01

    Young brown dwarfs are of prime importance to investigate the universality of the initial mass function (IMF) and to understand the physical connections between substellar and planetary-mass objects. Pan-STARRS1 (PS1) 3π survey (δ ≥ -30○) is finished and has obtained stacked images reaching down to the planetary regime (≤ 13 MJup) in nearby star-forming regions, thus providing an innovative tool to search for brown dwarfs. Using photometry and astrometry from PS1, WISE, 2MASS and UKIDSS, we are performing the widest and deepest brown dwarf survey in Taurus (≈370 deg2, ˜1 Myr) and Upper Scorpius (USco, ≈450 deg2, ˜10 Myr), which are among the closest star-forming regions. Our work is the first to measure proper motions, a robust proxy of membership, for Taurus and USco brown dwarf candidates over such large area and long time baseline (˜13 yr by combining PS1 and 2MASS). Our spectroscopic follow-up has found the lowest-mass objects in both regions (Taurus: ≈ 6 MJup USco: ≈ 14 MJup), and has yielded a success rates of ≈ 80% and ≈ 90% in Taurus and USco, respectively, far better than any previous searches (≤ 50%). Our newly confirmed members have already added ≈ 60% more brown dwarfs in USco and more than doubled the number of L-type members (≤ 20 MJup) in both regions. Upon completion, our discoveries will be a significant addition to the substellar regimes of the Taurus and the USco IMF and will provide more benchmarks to investigate the compositions of substellar and planetary atmospheres.

  9. Teaching Form as Form

    DEFF Research Database (Denmark)

    Keiding, Tina Bering

    2012-01-01

    understanding of form per se, or, to use an expression from this text, of form as form. This challenge can be reduced to one question: how can design teaching support students in achieving not only the ability to recognize and describe different form-related concepts in existing design (i.e. analytical...... means that form serves both as the connective value and as the concept for reflection. In other words, form is observed as form, not anything else. The didactical challenge of teaching form as form is accentuated by students’ everyday-based pre-orientation towards function at the expense of form....... In general, students enter design education as far more skilled observers with regards to function than form. They are, in other words, predisposed to observe objects asking ‘what is?’, rather than ‘how is?’. This habit has not only cognitive implications. It is closely intertwined with a rudimentary...

  10. Teaching Form as Form

    DEFF Research Database (Denmark)

    Keiding, Tina Bering

    2012-01-01

    understanding of form per se, or, to use an expression from this text, of form as form. This challenge can be reduced to one question: how can design teaching support students in achieving not only the ability to recognize and describe different form-related concepts in existing design (i.e. analytical...... means that form serves both as the connective value and as the concept for reflection. In other words, form is observed as form, not anything else. The didactical challenge of teaching form as form is accentuated by students’ everyday-based pre-orientation towards function at the expense of form...... vocabulary of form. Even in cases in which teaching uses terms and phrases from everyday life (for instance, ‘intersection’), the meaning of the word cannot necessarily be transmitted directly from an ordinary vocabulary into a design context. And it is clearly a common issue for the contributions...

  11. 13C-methyl formate: observations of a sample of high mass star-forming regions including Orion-KL and spectroscopic characterization

    CERN Document Server

    Favre, Cecile; Field, David; Jorgensen, Jes; Bisschop, Suzanne; Brouillet, Nathalie; Despois, Didier; Baudry, Alain; Kleiner, Isabelle; Bergin, Edwin; Crockett, Nathan; Neill, Justin; Margules, Laurent; Huet, Therese; Demaison, Jean

    2014-01-01

    We have surveyed a sample of massive star-forming regions located over a range of distances from the Galactic centre for methyl formate, HCOOCH$_{3}$, and its isotopologues H$^{13}$COOCH$_{3}$ and HCOO$^{13}$CH$_{3}$. The observations were carried out with the APEX telescope in the frequency range 283.4--287.4~GHz. Based on the APEX observations, we report tentative detections of the $^{13}$C-methyl formate isotopologue HCOO$^{13}$CH$_{3}$ towards the following four massive star-forming regions: Sgr~B2(N-LMH), NGC~6334~IRS~1, W51 e2 and G19.61-0.23. In addition, we have used the 1~mm ALMA science verification observations of Orion-KL and confirm the detection of the $^{13}$C-methyl formate species in Orion-KL and image its spatial distribution. Our analysis shows that the $^{12}$C/$^{13}$C isotope ratio in methyl formate toward Orion-KL Compact Ridge and Hot Core-SW components (68.4$\\pm$10.1 and 71.4$\\pm$7.8, respectively) are, for both the $^{13}$C-methyl formate isotopologues, commensurate with the average ...

  12. [Variation of the mitochondrial DNA control region in the populations of southern form of Dolly Varden (Salvelinus malma krascheninnikovi) from Sakhalin].

    Science.gov (United States)

    Osinov, A G; Miuge, N S

    2008-12-01

    Analysis of a 551-bp segment of the mitochondrial DNA control region in 23 individuals from nine populations of Dolly Varden from Sakhalin and three individuals from the Shikaribetsu Lake (Hokkaido) revealed the presence of seven haplotypes of southern form, along with one haplotype of northern form of Dolly Varden. All seven haplotypes of southern Dolly Varden were earlier described in the populations from Hokkaido. Nested analysis of molecular variance (AMOVA) based on the haplotype frequencies, performed using literature data, suggested that, during the glacial epoch, there were three regional population groups of Dolly Varden (from eastern and western coasts of Sakhalin, and from Southern Primorye). Population groups from Sakhalin and Primorye were clearly separated. The differences between two Sakhalin population groups in the mtDNA haplotype frequencies were not statistically significant. However, relative to the earlier obtained data on microsatellite loci, these differences were statistically significant. For the populations of Sakhalin Dolly Varden, the data on mitochondrial and microsatellite DNA variation supplement each other.

  13. Trigonometric Parallaxes of Massive Star Forming Regions: V. G23.01-0.41 and G23.44-0.18

    CERN Document Server

    Brunthaler, A; Menten, K M; Zheng, X W; Moscadelli, L; Xu, Y

    2008-01-01

    We report trigonometric parallaxes for the massive star-forming regions G23.01-0.41 and G23.44-0.18, corresponding to distances of 4.59 [+0.38/-0.33] kpc and 5.88 [+1.37/-0.93] kpc, respectively. The distance to G23.01-0.41 is smaller than its near kinematic distance assuming a standard model of the Milky Way and less than half of its far kinematic distance, which has usually been assumed. This places it in the Crux-Scutum spiral arm. The distance to G23.44-0.18 is close to its near kinematic distance and most likely places it in the Norma spiral arm near the end of the Galactic bar. Combining the distance and proper motions with observed radial velocities gives the location and full space motion of the star forming regions. We find large deviations from circular Galactic orbits for these sources: both sources show peculiar motions of 20 to 30 km/s counter to Galactic rotation and toward the Galactic center. These large peculiar motions might be the result of gravitational perturbations from the Galactic bar.

  14. The Isotopic Composition of Noble Gases in Gold Deposits and the Source of Ore-Forming Materials in the Region of North Hebei,China

    Institute of Scientific and Technical Information of China (English)

    王宝德; 牛树银; 孙爱群; 李红阳

    2003-01-01

    The source of ore-forming materials has long been a controversial focus both in metallogenic theory and in ore-searching practice. This study deals with the helium and argon isotopic characteristics of pyrites from 11 gold deposits and some country rocks in the gold mineralizationconcentrated areas within the three mantle-branch structures in the region of North Hebei Province. It is indicated that 3He/4He ratios in the gold deposits are within the range of 0.93 × 10 -6-7.3×10-6,with an average of 3.55 × 10-6; R/Ra =0.66 -4.93,averaging 2.53;40Ar/39Ar ratios vary between 426 and 2073,with the average value of 40Ar being 8.32; and the average of 4He/40Ar ratios is 2.17. 3He/4He ratios in gneiss and granite in the periphery of the mining district are within the range of 0. 001 × 10 -6 _ 0. 55 × 10 -6,reflecting significant differences in their sources. 3 He and 4 He fall near the mantle,as is shown in the He concentration diagram. Studies have shown that the ore-forming materials in this region should come from the deep interior of the Earth. With the multi-stage evolution of mantle plume,ore-forming fluids in the deep interior were moving upwards to shallow levels (crust). Under such circumstances,there would be inevitably occur crust/mantle fluid mixing,so their noble gas isotopic characteristics are intermediate between the mantle and the crust.

  15. THE CLUSTERED NATURE OF STAR FORMATION. PRE-MAIN-SEQUENCE CLUSTERS IN THE STAR-FORMING REGION NGC 602/N90 IN THE SMALL MAGELLANIC CLOUD

    Energy Technology Data Exchange (ETDEWEB)

    Gouliermis, Dimitrios A.; Gennaro, Mario [Max Planck Institute for Astronomy, Koenigstuhl 17, 69117 Heidelberg (Germany); Schmeja, Stefan [Zentrum fuer Astronomie der Universitaet Heidelberg, Institut fuer Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg (Germany); Dolphin, Andrew E. [Raytheon Company, P.O. Box 11337, Tucson, AZ 85734 (United States); Tognelli, Emanuele; Prada Moroni, Pier Giorgio [Dipartimento di Fisica ' Enrico Fermi' , Universita di Pisa, largo Pontecorvo 3, Pisa I-56127 (Italy)

    2012-03-20

    Located at the tip of the wing of the Small Magellanic Cloud (SMC), the star-forming region NGC 602/N90 is characterized by the H II nebular ring N90 and the young cluster of pre-main-sequence (PMS) and early-type main-sequence stars NGC 602, located in the central area of the ring. We present a thorough cluster analysis of the stellar sample identified with Hubble Space Telescope/Advanced Camera for Surveys in the region. We show that apart from the central cluster low-mass PMS stars are congregated in 13 additional small, compact sub-clusters at the periphery of NGC 602, identified in terms of their higher stellar density with respect to the average background density derived from star counts. We find that the spatial distribution of the PMS stars is bimodal, with an unusually large fraction ({approx}60%) of the total population being clustered, while the remaining is diffusely distributed in the intercluster area, covering the whole central part of the region. From the corresponding color-magnitude diagrams we disentangle an age difference of {approx}2.5 Myr between NGC 602 and the compact sub-clusters, which appear younger, on the basis of comparison of the brighter PMS stars with evolutionary models, which we accurately calculated for the metal abundance of the SMC. The diffuse PMS population appears to host stars as old as those in NGC 602. Almost all detected PMS sub-clusters appear to be centrally concentrated. When the complete PMS stellar sample, including both clustered and diffused stars, is considered in our cluster analysis, it appears as a single centrally concentrated stellar agglomeration, covering the whole central area of the region. Considering also the hot massive stars of the system, we find evidence that this agglomeration is hierarchically structured. Based on our findings, we propose a scenario according to which the region NGC 602/N90 experiences an active clustered star formation for the last {approx}5 Myr. The central cluster NGC 602 was

  16. The chemical composition of the Orion star-forming region. III. C, N, Ne, Mg and Fe abundances in B-type stars revisited

    CERN Document Server

    Nieva, Maria-Fernanda

    2011-01-01

    Early B-type stars are invaluable indicators for elemental abundances of their birth environments. In contrast to the surrounding neutral interstellar matter (ISM) and HII regions their chemical composition is unaffected by depletion onto dust grains and by the derivation of different abundances from recombination and collisional lines. In combination with ISM or nebular gas-phase abundances they facilitate the dust-phase composition to be constrained. Precise abundances of C, N, Mg, Ne, Fe in early B-type stars in the Orion star-forming region are determined in order to: a) review previous determinations using a self-consistent quantitative spectral analysis based on modern stellar atmospheres and recently updated model atoms, b) complement results found in Paper I for oxygen and silicon, c) establish an accurate and reliable set of stellar metal abundances to constrain the dust-phase composition of the Orion HII region in Paper II of the series. A detailed, self-consistent spectroscopic study of a sample of...

  17. Accurate positions of SiO masers in active star-forming regions - Orion-KL, W51-IRS2, and Sagittarius-B2 MD5

    Science.gov (United States)

    Morita, Koh-Ichiro; Hasegawa, Tetsuo; Ukita, Nobuharu; Okumura, Sachiko K.; Ishiguro, Masato

    1992-08-01

    Accurate positional measurements of SiO J = 1-0 masers in active star-forming regions, Orion-KL, W51-IRS2, and Sgr-B2 MD5, were made with the Nobeyama Millimeter Array. Absolute positional accuracies of 0.12-0.6 arcsec were achieved. The SiO maser in W51-IRS2 is located within 0.4 arcsec (0.5 x 10 exp 17 cm at the distance of W51-IRS2) of the strongest H2O masers. In Sgr-B2 MD5, the SiO maser coincides with the strongest H2O masers, most of the strong OH masers, and the peak of radio continuum emission from the ultracompact H II region within 0.7 arcsec (0.8 x 10 exp 17 cm at the distance of Sgr-B2). Peaks of the emission from hot NH3 were found to exist within about 1 arcsec of the SiO masers in both regions. The precise positional coincidence confirms our former conclusion that the SiO masers in W51-IRS2 and Sgr-B2 MD5 are actually associated with the ongoing activity of star formation, as is the case of Orion-KL.

  18. Characterization and expression of multiple alternatively spliced transcripts of the Goodpasture antigen gene region. Goodpasture antibodies recognize recombinant proteins representing the autoantigen and one of its alternative forms.

    Science.gov (United States)

    Penadés, J R; Bernal, D; Revert, F; Johansson, C; Fresquet, V J; Cervera, J; Wieslander, J; Quinones, S; Saus, J

    1995-05-01

    Collagen IV, the major component of basement membranes, is composed of six distinct alpha chains (alpha 1-alpha 6). Atypically among the collagen IV genes, the exons encoding the carboxyl-terminal region of the human alpha 3(IV) chain undergo alternative splicing. This region has been designated as the Goodpasture antigen because of its reactivity in the kidney and lung with the pathogenic autoantibodies causing Goodpasture syndrome. The data presented in this report demonstrate that, in human kidney, the gene region encompassing the Goodpasture antigen generates at least six alternatively spliced transcripts predicting five distinct proteins that differ in their carboxyl-terminus and retain, except in one case, the exon that harbors the characteristic amino-terminus of the antigen. Goodpasture antibodies specifically recognize recombinant proteins representing the antigen and the alternative form that retains the amino-half of the antigen, suggesting that this moiety could be involved in the in vivo binding of the pathogenic antibodies. Furthermore, the sera of control individuals contain autoantibodies against the antigen that can be differentiated from those causing the syndrome based on their specific reactivities, suggesting that the binding of the pathogenic autoantibodies to a specific determinant likely trigger a distinct and unique cascade of events causing the disease.

  19. Immune complexes in chronic Chagas disease patients are formed by exovesicles from Trypanosoma cruzi carrying the conserved MASP N-terminal region

    Science.gov (United States)

    Díaz Lozano, Isabel María; de Pablos, Luis Miguel; Longhi, Silvia Andrea; Zago, María Paola; Schijman, Alejandro Gabriel; Osuna, Antonio

    2017-03-01

    The exovesicles (EVs) are involved in pathologic host-parasite immune associations and have been recently used as biomarkers for diagnosis of infectious diseases. The release of EVs by Trypanosoma cruzi, the causative agent of Chagas disease, has recently been described, with different protein cargoes including the MASP multigene family of proteins MASPs are specific to this parasite and characterized by a conserved C-terminal (C-term) region and an N-terminal codifying for a signal peptide (SP). In this investigation, we identified immature MASP proteins containing the MASP SP in EVs secreted by the infective forms of the parasite. Those EVs are responsible for the formation of immune complexes (ICs) containing anti-MASP SP IgGs in patients with different (cardiac, digestive and asymptomatic) chronic Chagas disease manifestations. Moreover, purified EVs as well as the MASP SP inhibit the action of the complement system and also show a significant association with the humoral response in patients with digestive pathologies. These findings reveal a new route for the secretion of MASP proteins in T. cruzi, which uses EVs as vehicles for immature and misfolded proteins, forming circulating immune complexes. Such complexes could be used in the prognosis of digestive pathologies of clinical forms of Chagas disease.

  20. Discontinuous drainage systems formed by highland precipitation and ground-water outflow in the Navua Valles and southwest Hadriacus Mons regions, Mars

    Science.gov (United States)

    Hargitai, H. I.; Gulick, V. C.; Glines, N. H.

    2017-09-01

    The Navua Valles are systems of paleodrainages located north of Dao Vallis, which empty into Hellas Planitia, the largest impact basin on Mars. In this study, we mapped and characterized the Navua Valles Region's individual drainage systems, including drainages along the southwestern flank of Hadriacus Mons, and one valley network from the same source as Navua Valles but flowing in the opposite direction. The major drainage systems share morphological characteristics common to both outflow channels and valley networks. The slopes in this region are dissected by two major Navua drainage systems (here Navua A* and B*) and several shorter, sub-parallel valleys formed on the highest gradient (approximately 20 m/km [1.15°]) slopes, at the lowest part of Hellas Basin's rim. The two major drainage systems originate in the highlands, and empty into the basin. Our mapping suggests that water in Navua Valles reached the basin floor in a complicated descent and included several episodes of surface ponding, surface runoff, infiltration, subsurface flow and subsequent outflow. The most prominent channel system, Navua A, forms a repetitive sequence of deep incision into bedrock, followed by a transition into broad channels in erodible materials, and then into unconfined deposits. This successive erosion-transport-deposition sequence continues to repeat along the valley's entire length forming a discontinuous pattern that is consistent with classical fluvial process models. The channels cut into volcanic plains likely emplaced from the formation of Tyrrhenus and Hadriacus Montes. The dendritic source valleys of Navua A originate from the rim of a highland crater while the rest of this subsystem consists of a single, discontinuous channel which is consistent with a single water source zone that likely supplied water for all channels downslope. These drainages may have formed as discontinuous channels, revealing the potential existence of subsurface drainage pathways located

  1. A locus for the nystagmus-associated form of episodic ataxia maps to an 11-cM region on chromosome 19p

    Energy Technology Data Exchange (ETDEWEB)

    Kramer, P.L.; Gancher, S.T.; Nutt, J.G. [Oregon Health Oregon Health Sciences Univ., Portland, OR (United States)] [and others

    1995-07-01

    Episodic ataxia (EA) is a rare neurological disorder characterized by attacks of generalized ataxia and near-normal neurological function between attacks. Most inherited cases are the result of an autosomal dominant condition with unknown neuropathology. It is heterogeneous and includes at least two distinct forms. In EA-1, attacks last minutes and interictal myokymia may be present. In EA-2, attacks may last hours and interictal nystagmus may occur. We reported linkage in four EA-1 families to chromosome 12p13 and identified mutations in these families in a potassium channel gene, KCNA1. Recently, we reported linkage in two EA-2 families to a 30-cM region on chromosome 19p. This report is based on members of the same two families and one additional kindred. 18 refs., 1 fig., 1 tab.

  2. THE ABUNDANCE, ORTHO/PARA RATIO, AND DEUTERATION OF WATER IN THE HIGH-MASS STAR-FORMING REGION NGC 6334 I

    Energy Technology Data Exchange (ETDEWEB)

    Emprechtinger, M.; Lis, D. C.; Monje, R. R. [California Institute of Technology, Cahill Center for Astronomy and Astrophysics 301-17, Pasadena, CA 91125 (United States); Rolffs, R.; Schilke, P. [Physikalisches Institut, Universitaet zu Koeln, Zuelpicher Str. 77, D-50937 Koeln (Germany); Comito, C. [Max-Planck-Institut fuer Radioastronomie, Auf dem Huegel 69, D-53121 Bonn (Germany); Ceccarelli, C. [UJF-Grenoble 1/CNRS-INSU, Institut de Planetologie et d' Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble F-38041 (France); Neufeld, D. A. [Department of Physics and Astronomy Johns Hopkins University, Baltimore, MD 21218 (United States); Van der Tak, F. F. S., E-mail: dcl@caltech.edu [SRON Netherlands Institute for Space Research and Kapteyn Astronomical Institute, University of Groningen, Groningen (Netherlands)

    2013-03-01

    We present Herschel/HIFI observations of 30 transitions of water isotopologues toward the high-mass star-forming region NGC 6334 I. The line profiles of H{sup 16} {sub 2}O, H{sup 17} {sub 2}O, H{sup 18} {sub 2}O, and HDO show a complex pattern of emission and absorption components associated with the embedded hot cores, a lower-density envelope, two outflow components, and several foreground clouds, some associated with the NGC 6334 complex, others seen in projection against the strong continuum background of the source. Our analysis reveals an H{sub 2}O ortho/para ratio of 3 {+-} 0.5 in the foreground clouds, as well as the outflow. The water abundance varies from {approx}10{sup -8} in the foreground clouds and the outer envelope to {approx}10{sup -6} in the hot core. The hot core abundance is two orders of magnitude below the chemical model predictions for dense, warm gas, but within the range of values found in other Herschel/HIFI studies of hot cores and hot corinos. This may be related to the relatively low gas and dust temperature ({approx}100 K), or time-dependent effects, resulting in a significant fraction of water molecules still locked up in dust grain mantles. The HDO/H{sub 2}O ratio in NGC 6334 I, {approx}2 Multiplication-Sign 10{sup -4}, is also relatively low, but within the range found in other high-mass star-forming regions.

  3. The clustered nature of star formation. Pre--main-sequence clusters in the star-forming region NGC 602/N90 in the Small Magellanic Cloud

    CERN Document Server

    Gouliermis, Dimitrios A; Dolphin, Andrew E; Gennaro, Mario; Tognelli, Emanuele; Moroni, Pier Giorgio Prada

    2012-01-01

    Located at the tip of the wing of the Small Magellanic Cloud (SMC), the star-forming region NGC602/N90 is characterized by the HII nebular ring N90 and the young cluster of pre--main-sequence (PMS) and early-type main sequence stars NGC602. We present a thorough cluster analysis of the stellar sample identified with HST/ACS camera in the region. We show that apart from the central cluster, low-mass PMS stars are congregated in thirteen additional small compact sub-clusters at the periphery of NGC602. We find that the spatial distribution of the PMS stars is bimodal, with an unusually large fraction (~60%) of the total population being clustered, while the remaining is diffusely distributed in the inter-cluster area. From the corresponding color-magnitude diagrams we disentangle an age-difference of ~2.5Myr between NGC602 and the compact sub-clusters which appear younger. The diffuse PMS population appears to host stars as old as those in NGC602. Almost all detected PMS sub-clusters appear to be centrally conc...

  4. Z-DNA-forming sites identified by ChIP-Seq are associated with actively transcribed regions in the human genome

    Science.gov (United States)

    Shin, So-I.; Ham, Seokjin; Park, Jihwan; Seo, Seong Hye; Lim, Chae Hyun; Jeon, Hyeongrin; Huh, Jounghyun; Roh, Tae-Young

    2016-01-01

    Z-DNA, a left-handed double helical DNA is structurally different from the most abundant B-DNA. Z-DNA has been known to play a significant role in transcription and genome stability but the biological meaning and positions of Z-DNA-forming sites (ZFSs) in the human genome has not been fully explored. To obtain genome-wide map of ZFSs, Zaa with two Z-DNA-binding domains was used for ChIP-Seq analysis. A total of 391 ZFSs were found and their functions were examined in vivo. A large portion of ZFSs was enriched in the promoter regions and contain sequences with high potential to form Z-DNA. Genes containing ZFSs were occupied by RNA polymerase II at the promoters and showed high levels of expression. Moreover, ZFSs were significantly related to active histone marks such as H3K4me3 and H3K9ac. The association of Z-DNA with active transcription was confirmed by the reporter assay system. Overall, our results suggest that Z-DNA formation depends on chromatin structure as well as sequence composition, and is associated with active transcription in human cells. The global information about ZFSs positioning will provide a useful resource for further understanding of DNA structure-dependent transcriptional regulation. PMID:27374614

  5. Water in low-mass star-forming regions with Herschel (WISH-LM): High-velocity H2O bullets in L1448-MM observed with HIFI

    CERN Document Server

    Kristensen, L E; Tafalla, M; Bachiller, R; Nisini, B; Liseau, R; Yildiz, U A

    2011-01-01

    Herschel-HIFI observations of water in the low-mass star-forming object L1448-MM, known for its prominent outflow, are presented, as obtained within the `Water in star-forming regions with Herschel' (WISH) key programme. Six H2-16O lines are targeted and detected (E_up/k_B ~ 50-250 K), as is CO J= 10-9 (E_up/k_B ~ 305 K), and tentatively H2-18O 110-101 at 548 GHz. All lines show strong emission in the "bullets" at |v| > 50 km/s from the source velocity, in addition to a broad, central component and narrow absorption. The bullets are seen much more prominently in H$_2$O than in CO with respect to the central component, and show little variation with excitation in H2O profile shape. Excitation conditions in the bullets derived from CO lines imply a temperature >150 K and density >10^5 cm^-3, similar to that of the broad component. The H2O/CO abundance ratio is similar in the "bullets" and the broad component, ~ 0.05-1.0, in spite of their different origins in the molecular jet and the interaction between the ou...

  6. A dearth of short-period massive binaries in the young massive star forming region M 17. Evidence for a large orbital separation at birth?

    Science.gov (United States)

    Sana, H.; Ramírez-Tannus, M. C.; de Koter, A.; Kaper, L.; Tramper, F.; Bik, A.

    2017-03-01

    Aims: The formation of massive stars remains poorly understood and little is known about their birth multiplicity properties. Here, we aim to quantitatively investigate the strikingly low radial-velocity dispersion measured for a sample of 11 massive pre- and near-main-sequence stars (σ1D= 5.6 ± 0.2 km s-1) in the very young massive star forming region M 17, in order to obtain first constraints on the multiplicity properties of young massive stellar objects. Methods: We compute the radial-velocity dispersion of synthetic populations of massive stars for various multiplicity properties and we compare the obtained σ1D distributions to the observed value. We specifically investigate two scenarios: a low binary fraction and a dearth of short-period binary systems. Results: Simulated populations with low binary fractions () or with truncated period distributions (Pcutoff > 9 months) are able to reproduce the low σ1D observed within their 68%-confidence intervals. Furthermore, parent populations with fbin > 0.42 or Pcutoff star formation process. In the context of the second scenario, compact binaries must form later on, and the cut-off period may be related to physical length-scales representative of the bloated pre-main-sequence stellar radii or of their accretion disks. Conclusions: If the obtained constraints for the M 17's massive-star population are representative of the multiplicity properties of massive young stellar objects, our results may provide support to a massive star formation process in which binaries are initially formed at larger separations, then harden or migrate to produce the typical (untruncated) power-law period distribution observed in few Myr-old OB binaries.

  7. Infrared Study of the Southern Galactic Star-Forming Regions Associated with IRAS 10049-5657 and IRAS 10031-5632

    Science.gov (United States)

    Vig, S.; Ghosh, S. K.; Ojha, D. K.; Verma, R. P.

    2008-10-01

    We investigate the physical conditions of the interstellar medium and stellar components in the regions of the southern Galactic star-forming complexes associated with IRAS 10049-5657 and IRAS 10031-5632. These regions have been mapped simultaneously in two far-infrared bands (λeff ~ 150 and 210 μm), with ~1' angular resolution using the Tata Institute of Fundamental Research 1 m balloon-borne telescope. Spatial distribution of the temperature of cool dust and optical depth at 200 μm have been obtained taking advantage of the similar beams in the two bands. The HIRES processed Infrared Astronomical Satellite (IRAS) maps at 12, 25, 60, and 100 μm have been used for comparison. Using the Two Micron All Sky Survey near-infrared sources, we find the stellar populations of the embedded young clusters. A rich cluster of OB stars is seen in the IRAS 10049-5657 region. The fits to the stellar density radial profile of the cluster associated with IRAS 10049-5657 have been explored with the inverse radius profile as well as the King's profile; the cluster radius is ~2 pc. The source in the cluster closest to the IRAS peak is IRA-7, which lies above the zero-age main-sequence curve of spectral type O5 in the color-magnitude diagram. Unlike IRAS 10049-5657, a small cluster comprising a few deeply embedded sources is seen at the location of IRAS 10031-5632. Self-consistent radiative transfer modeling aimed at extracting important physical and geometrical details of the two IRAS sources shows that the best-fit models are in good agreement with the observed spectral energy distributions. The geometric details of the associated cloud and optical depths (τ100) have been estimated. A uniform density distribution of dust and gas is implied for both the sources. In addition, the infrared ionic fine-structure line emission from gas has been modeled for both the regions and compared with data from the IRAS low-resolution spectrometer. For IRAS 10049-5657, the observed and modeled

  8. {sup 13}C-METHYL FORMATE: OBSERVATIONS OF A SAMPLE OF HIGH-MASS STAR-FORMING REGIONS INCLUDING ORION-KL AND SPECTROSCOPIC CHARACTERIZATION

    Energy Technology Data Exchange (ETDEWEB)

    Favre, Cécile; Bergin, Edwin A.; Crockett, Nathan R.; Neill, Justin L. [Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109 (United States); Carvajal, Miguel [Dpto. Física Aplicada, Unidad Asociada CSIC, Facultad de Ciencias Experimentales, Universidad de Huelva, E-21071 Huelva (Spain); Field, David [Department of Physics and Astronomy, University of Aarhus, Ny Munkegade 120, DK-8000 Aarhus C (Denmark); Jørgensen, Jes K.; Bisschop, Suzanne E. [Centre for Star and Planet Formation, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø (Denmark); Brouillet, Nathalie; Despois, Didier; Baudry, Alain [Univ. Bordeaux, LAB, UMR 5804, F-33270, Floirac (France); Kleiner, Isabelle [Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), CNRS, UMR 7583, Université de Paris-Est et Paris Diderot, 61, Av. du Général de Gaulle, F-94010 Créteil Cedex (France); Margulès, Laurent; Huet, Thérèse R.; Demaison, Jean, E-mail: cfavre@umich.edu, E-mail: miguel.carvajal@dfa.uhu.es [Laboratoire de Physique des Lasers, Atomes et Molécules, UMR CNRS 8523, Université Lille I, F-59655 Villeneuve d' Ascq Cedex (France)

    2015-01-01

    We have surveyed a sample of massive star-forming regions located over a range of distances from the Galactic center for methyl formate, HCOOCH{sub 3}, and its isotopologues H{sup 13}COOCH{sub 3} and HCOO{sup 13}CH{sub 3}. The observations were carried out with the APEX telescope in the frequency range 283.4-287.4 GHz. Based on the APEX observations, we report tentative detections of the {sup 13}C-methyl formate isotopologue HCOO{sup 13}CH{sub 3} toward the following four massive star-forming regions: Sgr B2(N-LMH), NGC 6334 IRS 1, W51 e2, and G19.61-0.23. In addition, we have used the 1 mm ALMA science verification observations of Orion-KL and confirm the detection of the {sup 13}C-methyl formate species in Orion-KL and image its spatial distribution. Our analysis shows that the {sup 12}C/{sup 13}C isotope ratio in methyl formate toward the Orion-KL Compact Ridge and Hot Core-SW components (68.4 ± 10.1 and 71.4 ± 7.8, respectively) are, for both the {sup 13}C-methyl formate isotopologues, commensurate with the average {sup 12}C/{sup 13}C ratio of CO derived toward Orion-KL. Likewise, regarding the other sources, our results are consistent with the {sup 12}C/{sup 13}C in CO. We also report the spectroscopic characterization, which includes a complete partition function, of the complex H{sup 13}COOCH{sub 3} and HCOO{sup 13}CH{sub 3} species. New spectroscopic data for both isotopomers H{sup 13}COOCH{sub 3} and HCOO{sup 13}CH{sub 3}, presented in this study, have made it possible to measure this fundamentally important isotope ratio in a large organic molecule for the first time.

  9. Origin of spinel lamella and/or inclusions in olivine of harzburgite form the Pauza ultramafic rocks from the Kurdistan region, northeastern Iraq

    Science.gov (United States)

    Mohammad, Y.; Maekawa, H.; Karim, K.

    2009-04-01

    Exsolution lamellae and octahedral inclusions of chromian spinel occur in olivine of harzburgite of the Pauza ultramafic rocks, Kurdistan region, northeastern Iraq. The lamella is up to 80μm long and up to 50 μm wide. The lamellae and octahedral inclusions of chromian spinel are distributed heterogeneously in the host olivine crystal. They are depleted in Al2O3 relative to the subhedral spinel grains in the matrix and spinel lamella in orthopyroxene. Olivine (Fo92 - 93) with spinel lamellae occurs as fine-grained crystals around orthopyroxene, whereas olivine (Fo90-91) free from spinel is found in matrix. Based on back-scattered images analyses, enrichments of both Cr # and Fe+3 in the chromian spinel lamella in olivine (replacive olivine) relative to that in adjacent orthopyroxene. As well as the compositions of chromian spinel lamellae host olivine are more Mg-rich than the matrix olivine. Furthermore the restriction of olivine with spinel lamellae and octahedral inclusions on around orthopyroxene, and the similarity of spinel lamella orientations in both olivine and adjacent orthopyroxene. This study concludes that the spinel inclusions in olivine are remnant (inherited from former orthopyroxene) spinel exsolution lamella in orthopyroxene, that has been formed in upper mantle conditions ( T = 1200 °C, P = 2.5 GPa ). Replacive olivine are formed by reaction of ascending silica poor melt and orthopyroxene in harzburgite as pressure decrease the solubility of silica-rich phase (orthopyroxene) in the system increase, therefore ascending melt dissolve pyroxene with spinel exsolution lamella and precipitate replacive olivine with spinel inclusions. We can conclude that the olivines with spinel lamella are not necessary to be original and presenting ultrahigh-pressure and/or ultra deep-mantle conditions as previously concluded. It has been formed by melting of orthopyroxene (orthopyroxene with spinel exsolution lamella = olivine with spinel lamellae and octahedral

  10. A study on subarcsecond scales of the ammonia and continuum emission toward the G16.59-0.05 high-mass star-forming region

    CERN Document Server

    Moscadelli, L; Sánchez-Monge, Á; Goddi, C; Furuya, R S; Sanna, A; Pestalozzi, M

    2013-01-01

    We wish to investigate the structure, velocity field, and stellar content of the G16.59-0.05 high-mass star-forming region, where previous studies have established the presence of two almost perpendicular (NE-SW and SE-NW), massive outflows, and a rotating disk traced by methanol maser emission. We performed Very Large Array observations of the radio continuum and ammonia line emission, complemented by COMICS/Subaru and Hi-GAL/Herschel images in the mid- and far-infrared (IR). Our centimeter continuum maps reveal a collimated radio jet that is oriented E-W and centered on the methanol maser disk, placed at the SE border of a compact molecular core. The spectral index of the jet is negative, indicating non-thermal emission over most of the jet, except the peak close to the maser disk, where thermal free-free emission is observed. We find that the ammonia emission presents a bipolar structure consistent (on a smaller scale) in direction and velocity with that of the NE-SW bipolar outflow detected in previous CO...

  11. The Abundance, Ortho/Para Ratio, and Deuteration of Water in the High-Mass Star Forming Region NGC 6334 I

    CERN Document Server

    Emprechtinger, M; Rolffs, R; Schilke, P; Monje, R R; Comito, C; Ceccarelli, C; Neufeld, D A; van der Tak, F F S

    2012-01-01

    We present Herschel/HIFI observations of 30 transitions of water isotopologues toward the high-mass star forming region NGC 6334 I. The line profiles of H_2^{16}O, H_2^{17}O, H_2^{18}O, and HDO show a complex pattern of emission and absorption components associated with the embedded hot cores, a lower-density envelope, two outflow components, and several foreground clouds, some associated with the NGC 6334 complex, others seen in projection against the strong continuum background of the source. Our analysis reveals an H2O ortho/para ratio of 3 +/- 0.5 in the foreground clouds, as well as the outflow. The water abundance varies from ~10^{-8} in the foreground clouds and the outer envelope to ~10^{-6} in the hot core. The hot core abundance is two orders of magnitude below the chemical model predictions for dense, warm gas, but within the range of values found in other Herschel/HIFI studies of hot cores and hot corinos. This may be related to the relatively low gas and dust temperature (~100 K), or time depende...

  12. NEAR-INFRARED PERIODIC AND OTHER VARIABLE FIELD STARS IN THE FIELD OF THE CYGNUS OB7 STAR-FORMING REGION

    Energy Technology Data Exchange (ETDEWEB)

    Wolk, Scott J.; Rice, Thomas S. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Aspin, Colin A. [Institute for Astronomy, University of Hawaii at Manoa, 640 North Aohoku Place, Hilo, HI 96720 (United States)

    2013-04-15

    We present a subset of the results of a three-season, 124 night, near-infrared monitoring campaign of the dark clouds Lynds 1003 and Lynds 1004 in the Cygnus OB7 star-forming region. In this paper, we focus on the field star population. Using three seasons of UKIRT J, H, and K-band observations spanning 1.5 years, we obtained high-quality photometry on 9200 stars down to J = 17 mag, with photometric uncertainty better than 0.04 mag. After excluding known disk-bearing stars we identify 149 variables-1.6% of the sample. Of these, about 60 are strictly periodic, with periods predominantly <2 days. We conclude this group is dominated by eclipsing binaries. A few stars have long period signals of between 20 and 60 days. About 25 stars have weak modulated signals, but it was not clear if these were periodic. Some of the stars in this group may be diskless young stellar objects with relatively large variability due to cool starspots. The remaining {approx}60 stars showed variations which appear to be purely stochastic.

  13. Precise observations of the 12C/13C ratios of HC3N in the low-mass star-forming region L1527

    CERN Document Server

    Araki, Mitsunori; Sakai, Nami; Yamamoto, Satoshi; Oyama, Takahiro; Kuze, Nobuhiko; Tsukiyama, Koichi

    2016-01-01

    Using the Green Bank 100 m telescope and the Nobeyama 45 m telescope, we have observed the rotational emission lines of the three 13C isotopic species of HC3N in the 3 and 7 mm bands toward the low-mass star-forming region L1527 in order to explore their anomalous 12C/13C ratios. The column densities of the 13C isotopic species are derived from the intensities of the J = 5-4 lines observed at high signal-to-noise ratios. The abundance ratios are determined to be 1.00:1.01 +- 0.02:1.35 +- 0.03:86.4 +- 1.6 for [H13CCCN]:[HC13CCN]:[HCC13CN]:[HCCCN], where the errors represent one standard deviation. The ratios are very similar to those reported for the starless cloud, Taurus Molecular Cloud-1 Cyanopolyyne Peak (TMC-1 CP). These ratios cannot be explained by thermal equilibrium, but likely reflect the production pathways of this molecule. We have shown the equality of the abundances of H13CCCN and HC13CCN at a high-confidence level, which supports the production pathways of HC3N via C2H2 and C2H2+. The average 12...

  14. Inducible and targeted deletion of the ERK5 MAP kinase in adult neurogenic regions impairs adult neurogenesis in the olfactory bulb and several forms of olfactory behavior.

    Directory of Open Access Journals (Sweden)

    Yung-Wei Pan

    Full Text Available Although adult-born neurons in the subventricular zone (SVZ and olfactory bulb (OB have been extensively characterized at the cellular level, their functional impact on olfactory behavior is still highly controversial with many conflicting results reported in the literature. Furthermore, signaling mechanisms regulating adult SVZ/OB neurogenesis are not well defined. Here we report that inducible and targeted deletion of erk5, a MAP kinase selectively expressed in the adult neurogenic regions of the adult brain, impairs adult neurogenesis in the SVZ and OB of transgenic mice. Although erk5 deletion had no effect on olfactory discrimination among discrete odorants in the habituation/dishabituation assay, it reduced short-term olfactory memory as well as detection sensitivity to odorants and pheromones including those evoking aggression and fear. Furthermore, these mice show impaired acquisition of odor-cued associative olfactory learning, a novel phenotype that had not been previously linked to adult neurogenesis. These data suggest that ERK5 MAP kinase is a critical kinase signaling pathway regulating adult neurogenesis in the SVZ/OB, and provide strong evidence supporting a functional role for adult neurogenesis in several distinct forms of olfactory behavior.

  15. A Search for Interstellar Carbon Chain Alcohol HC4OH in Star-Forming Region L1527 and Dark Cloud TMC-1

    CERN Document Server

    Araki, Mitsunori; Yamabe, Hiromichi; Koshikawa, Naohiro; Tsukiyama, Koichi; Nakane, Aya; Okabayashi, Toshiaki; Kunimatsu, Arisa; Kuze, Nobuhiko

    2011-01-01

    We report a sensitive search for the rotational transitions of the carbon chain alcohol HC4OH in the frequency range of 21.2-46.7 GHz in the star-forming region L1527 and the dark cloud TMC-1. The motivation was laboratory detection of HC4OH by microwave spectroscopy. Despite achieving rms noise levels of several millikelvin in the antenna temperature using the 45 m telescope at Nobeyama Radio Observatory, the detection was not successful, leading to 3 sigma upper limits corresponding to the column densities of 2.0 \\times 1012 and 5.6 \\times 1012 cm-2 in L1527 and TMC-1, respectively. These upper limits indicate that [HC4OH]/[HC5N] ratios are less than 0.3 and 0.1 in L1527 and TMC-1, respectively, where HC5N is an HC4-chain cyanide and HC4OH is a hydroxide. These ratios suggest that the cyano carbon chain molecule dominates the hydroxyl carbon chain molecule in L1527 and TMC-1. This is contrary to the case of saturated compounds in hot cores, e.g., CH3OH and CH3CN, and can be a chemical feature of carbon chai...

  16. Outer Rotation Curve of the Galaxy with VERA II: Annual Parallax and Proper Motion of the Star-Forming Region IRAS21379+5106

    CERN Document Server

    Nakanishi, Hiroyuki; Kurayama, Tomoharu; Matsuo, Mitsuhiro; Imai, Hiroshi; Burns, Ross A; Ozawa, Takeaki; Honma, Mareki; Shibata, Katsunori; Kawaguchi, Noriyuki

    2015-01-01

    We conducted astrometric VLBI observations of water-vapor maser emission in the massive star forming region IRAS 21379+5106 to measure the annual parallax and proper motion, using VERA. The annual parallax was measured to be $0.262 \\pm 0.031$ mas corresponding to a trigonometric distance of $3.82^{+0.51}_{-0.41}$ kpc. The proper motion was $(\\mu_\\alpha\\cos{\\delta}, \\mu_\\delta)=(-2.74 \\pm 0.08, -2.87 \\pm 0.18)$ mas yr$^{-1}$. Using this result, the Galactic rotational velocity was estimated to be $V_\\theta=218\\pm 19$ km s$^{-1}$ at the Galactocentric distance $R=9.22\\pm0.43$ kpc, when we adopted the Galactic constants $R_0=8.05\\pm 0.45$ kpc and $V_0=238\\pm 14$ km s$^{-1}$. With newly determined distance, {the bolometric luminosity of the central young stellar object was re-evaluated to $(2.15\\pm 0.54)\\times 10^3 L_\\odot$, which corresponds to spectral type of} B2--B3. Maser features were found to be distributed along a straight line from south-west to north-east. In addition, a vector map of the internal motio...

  17. Physical and chemical differentiation of the luminous star-forming region W49A - Results from the JCMT Spectral Legacy Survey

    CERN Document Server

    Nagy, Z; Fuller, G A; Plume, R

    2015-01-01

    The massive and luminous star-forming region W49A is a well known Galactic candidate to probe the physical conditions and chemistry similar to those expected in external starburst galaxies. We aim to probe the physical and chemical structure of W49A on a spatial scale of ~0.8 pc based on the JCMT Spectral Legacy Survey, which covers the frequency range between 330 and 373 GHz. The wide 2x2 arcminutes field and the high spectral resolution of the HARP instrument on JCMT provides information on the spatial structure and kinematics of the cloud. For species where multiple transitions are available, we estimate excitation temperatures and column densities. We detected 255 transitions corresponding to 60 species in the 330-373 GHz range at the center position of W49A. Excitation conditions can be probed for 16 molecules. The chemical composition suggests the importance of shock-, PDR-, and hot core chemistry. Many molecular lines show a significant spatial extent across the maps including high density tracers (e.g...

  18. PARALLAXES FOR W49N AND G048.60+0.02: DISTANT STAR FORMING REGIONS IN THE PERSEUS SPIRAL ARM

    Energy Technology Data Exchange (ETDEWEB)

    Zhang, B.; Menten, K. M.; Brunthaler, A. [Max-Plank-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn (Germany); Reid, M. J.; Dame, T. M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Zheng, X. W. [Department of Astronomy, Nanjing University, Nanjing 210093 (China); Xu, Y. [Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China)

    2013-09-20

    We report trigonometric parallax measurements of 22 GHz H{sub 2}O masers in two massive star-forming regions from Very Long Baseline Array observations as part of the Bar and Spiral Structure Legacy Survey. The distances of 11.11{sup +0.79}{sub -0.69} kpc to W49N (G043.16+0.01) and 10.75{sup +0.61}{sub -0.55} kpc to G048.60+0.02 locate them in a distant section of the Perseus arm near the solar circle in the first Galactic quadrant. This allows us to locate accurately the inner portion of the Perseus arm for the first time. Combining the present results with sources measured in the outer portion of the arm in the second and third quadrants yields a global pitch angle of 9.°5 ± 1.°3 for the Perseus arm. We have found almost no H{sub 2}O maser sources in the Perseus arm for 50°

  19. EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions III. The flux-limited sample

    CERN Document Server

    Surcis, G; van Langevelde, H J; Kramer, B Hutawarakorn; Bartkiewicz, A; Blasi, M G

    2015-01-01

    Theoretical simulations and observations at different angular resolutions have shown that magnetic fields have a central role in massive star formation. Like in low-mass star formation, the magnetic field in massive young stellar objects can either be oriented along the outflow axis or randomly. Measuring the magnetic field at milliarcsecond resolution (10-100 au) around a substantial number of massive young stellar objects permits determining with a high statistical significance whether the direction of the magnetic field is correlated with the orientation of the outflow axis or not. In late 2012, we started a large VLBI campaign with the European VLBI Network to measure the linearly and circularly polarized emission of 6.7 GHz methanol masers around a sample of massive star-forming regions. This paper focuses on the first seven observed sources, G24.78+0.08, G25.65+1.05, G29.86-0.04, G35.03+0.35, G37.43+1.51, G174.20-0.08, and G213.70-12.6. For all these sources, molecular outflows have been detected in the...

  20. Herschel-HIFI observations of high-J CO lines in the NGC 1333 low-mass star-forming region

    CERN Document Server

    Yıldız, U A; Kristensen, L E; Visser, R; Jørgensen, J K; Herczeg, G J; van Kempen, T A; Hogerheijde, M R; Doty, S D; Benz, A O; Bruderer, S; Wampfler, S F; Deul, E; Bachiller, R; Baudry, A; Benedettini, M; Bergin, E; Bjerkeli, P; Blake, G A; Bontemps, S; Braine, J; Caselli, P; Cernicharo, J; Codella, C; Daniel, F; di Giorgio, A M; Dominik, C; Encrenaz, P; Fich, M; Fuente, A; Giannini, T; Goicoechea, J R; de Graauw, Th; Helmich, F; Herpin, F; Jacq, T; Johnstone, D; Larsson, B; Lis, D; Liseau, R; Liu, F -C; Marseille, M; McCoey, C; Melnick, G; Neufeld, D; Nisini, B; Olberg, M; Parise, B; Pearson, J C; Plume, R; Risacher, C; Santiago-Garcia, J; Saraceno, P; Shipman, R; Tafalla, M; Tielens, A G G M; van der Tak, F; Wyrowski, F; Dieleman, P; Jellema, W; Ossenkopf, V; Schieder, R; Stutzki, J; 10.1051/0004-6361/201015119

    2010-01-01

    Herschel-HIFI observations of high-J lines (up to J_u=10) of 12CO, 13CO and C18O are presented toward three deeply embedded low-mass protostars, NGC 1333 IRAS 2A, IRAS 4A, and IRAS 4B, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. The spectrally-resolved HIFI data are complemented by ground-based observations of lower-J CO and isotopologue lines. The 12CO 10-9 profiles are dominated by broad (FWHM 25-30 km s^-1) emission. Radiative transfer models are used to constrain the temperature of this shocked gas to 100-200 K. Several CO and 13CO line profiles also reveal a medium-broad component (FWHM 5-10 km s^-1), seen prominently in H2O lines. Column densities for both components are presented, providing a reference for determining abundances of other molecules in the same gas. The narrow C18O 9-8 lines probe the warmer part of the quiescent envelope. Their intensities require a jump in the CO abundance at an evaporation temperature around 25 K, thus providing new direct e...

  1. Gas and dust in the star-forming region rho Oph A: The dust opacity exponent beta and the gas-to-dust mass ratio g2d

    CERN Document Server

    Liseau, R; Lunttila, T; Olberg, M; Rydbeck, G; Bergman, P; Justtanont, K; Olofsson, G; de Vries, B L

    2015-01-01

    We aim at determining the spatial distribution of the gas and dust in star-forming regions and address their relative abundances in quantitative terms. We also examine the dust opacity exponent beta for spatial and/or temporal variations. Using mapping observations of the very dense rho Oph A core, we examined standard 1D and non-standard 3D methods to analyse data of far-infrared and submillimeter (submm) continuum radiation. The resulting dust surface density distribution can be compared to that of the gas. The latter was derived from the analysis of accompanying molecular line emission, observed with Herschel from space and with APEX from the ground. As a gas tracer we used N2H+, which is believed to be much less sensitive to freeze-out than CO and its isotopologues. Radiative transfer modelling of the N2H+(J=3-2) and (J=6-5) lines with their hyperfine structure explicitly taken into account provides solutions for the spatial distribution of the column density N(H2), hence the surface density distribution ...

  2. A Search for Interstellar Carbon-chain Alcohol HC4OH in Star-forming Region l1527 and Dark Cloud TMC-1

    Science.gov (United States)

    Araki, Mitsunori; Takano, Shuro; Yamabe, Hiromichi; Koshikawa, Naohiro; Tsukiyama, Koichi; Nakane, Aya; Okabayashi, Toshiaki; Kunimatsu, Arisa; Kuze, Nobuhiko

    2012-01-01

    We report a sensitive search for the rotational transitions of the carbon-chain alcohol HC4OH in the frequency range 21.2-46.7 GHz in the star-forming region L1527 and the dark cloud TMC-1. The motivation was laboratory detection of HC4OH by microwave spectroscopy. Despite achieving rms noise levels of several millikelvin in the antenna temperature using the 45 m telescope at Nobeyama Radio Observatory, the detection was not successful, leading to 3σ upper limits corresponding to the column densities of 2.0 × 1012 and 5.6 × 1012 cm-2 in L1527 and TMC-1, respectively. These upper limits indicate that [HC4OH]/[HC5N] ratios are less than 0.3 and 0.1 in L1527 and TMC-1, respectively, where HC5N is an HC4-chain cyanide and HC4OH is a hydroxide. These ratios suggest that the cyano carbon-chain molecule dominates the hydroxyl carbon-chain molecule in L1527 and TMC-1. This is contrary to the case of saturated compounds in hot cores, e.g., CH3OH and CH3CN, and can be a chemical feature of carbon-chain molecules in L1527 and TMC-1. In addition, the column densities of the "unsubstituted" carbon-chain molecule C4H and the sulfur-bearing molecules SO and HCS+ were determined from detected lines in L1527.

  3. Collaborative form(s)

    DEFF Research Database (Denmark)

    Gunn, Wendy

    Gunn asks us to consider beauty as collaborative forms of action generated by moving between design by means of anthropology and anthropology by means of design. Specifically, she gives focus to play-like reflexions on practices of designing energy products, systems and infrastructure. Design...

  4. Fungal specificity and selectivity for algae play a major role in determining lichen partnerships across diverse ecogeographic regions in the lichen-forming family Parmeliaceae (Ascomycota).

    Science.gov (United States)

    Leavitt, Steven D; Kraichak, Ekaphan; Nelsen, Matthew P; Altermann, Susanne; Divakar, Pradeep K; Alors, David; Esslinger, Theodore L; Crespo, Ana; Lumbsch, Thorsten

    2015-07-01

    Microbial symbionts are instrumental to the ecological and long-term evolutionary success of their hosts, and the central role of symbiotic interactions is increasingly recognized across the vast majority of life. Lichens provide an iconic group for investigating patterns in species interactions; however, relationships among lichen symbionts are often masked by uncertain species boundaries or an inability to reliably identify symbionts. The species-rich lichen-forming fungal family Parmeliaceae provides a diverse group for assessing patterns of interactions of algal symbionts, and our study addresses patterns of lichen symbiont interactions at the largest geographic and taxonomic scales attempted to date. We analysed a total of 2356 algal internal transcribed spacer (ITS) region sequences collected from lichens representing ten mycobiont genera in Parmeliaceae, two genera in Lecanoraceae and 26 cultured Trebouxia strains. Algal ITS sequences were grouped into operational taxonomic units (OTUs); we attempted to validate the evolutionary independence of a subset of the inferred OTUs using chloroplast and mitochondrial loci. We explored the patterns of symbiont interactions in these lichens based on ecogeographic distributions and mycobiont taxonomy. We found high levels of undescribed diversity in Trebouxia, broad distributions across distinct ecoregions for many photobiont OTUs and varying levels of mycobiont selectivity and specificity towards the photobiont. Based on these results, we conclude that fungal specificity and selectivity for algal partners play a major role in determining lichen partnerships, potentially superseding ecology, at least at the ecogeographic scale investigated here. To facilitate effective communication and consistency across future studies, we propose a provisional naming system for Trebouxia photobionts and provide representative sequences for each OTU circumscribed in this study.

  5. Polarization effects in the reaction e{sup +} + e{sup -} {yields} {rho}{sup +} + {rho}{sup -} and determination of the {rho}{sup -} meson form factors in the time-like region

    Energy Technology Data Exchange (ETDEWEB)

    Adamuscin, C. [Slovak Academy of Sciences, Dept. of Theoretical Physics, Bratislava (Slovakia); Gakh, G.I. [NSC Kharkov Physical Technical Institute, Kharkov (Ukraine); Tomasi-Gustafsson, E. [CEA Saclay, Dept. d' Astrophysique, de Physique des Particules, de Physique Nucleaire et de l' Instrumentation Associee (DAPNIA/SPhN), 91- Gif sur Yvette (France)

    2006-12-15

    The electron positron annihilation reaction into 4 pion production has been studied, through the channel e{sup +} + e{sup -} {yields} {rho}-bar + {rho}. The differential (and total) cross sections and various polarization observables for this reaction have been calculated in terms of the electromagnetic form factors of the corresponding {gamma}{sup *}{rho}{rho} current. The elements of the spin-density matrix of the {rho}-meson were also calculated. Numerical estimations have been done, with the help of phenomenological form factors obtained in the space-like region of the momentum transfer squared and analytically extended to the time-like region. (authors)

  6. Forming of the regional core transport network taking into account the allocation of alternative energy sources based on artificial intelligence methods

    Directory of Open Access Journals (Sweden)

    Marina ZHURAVSKAYA

    2014-12-01

    Full Text Available In the modern world the alternative energy sources, which considerably depend on a region, play more and more significant role. However, the transition of regions to new energy sources lead to the change of transport and logistic network configuration. The formation of optimal core transport network today is a guarantee of the successful economic development of a region tomorrow. The present article studies the issue of advanced core transport network development in a region based on the experience of European and Asian countries and the opportunity to adapt the best foreign experience to Russian conditions. On the basis of artificial intelligence methods for forest industry complex of Sverdlovskaya Oblast the algorithm of problem solution of an optimal logistic infrastructure allocation is offered and some results of a regional transport network are presented. These methods allowed to solve the set task in the conditions of information uncertainty. There are suggestions on the improvement of transport and logistic network in the territory of Sverdlovskaya Oblast. Traditionally the logistics of mineral fuel plays main role in regions development. Actually it is required to develop logistic strategic plans to be able to provide different possibilities of power-supply, flexible enough to change with the population density, transport infrastructure and demographics of different regions. The problem of logistic centers allocation was studied by many authors. The approach, offered by the authors of this paper is to solve the set of tasks by applying artificial intelligence methods, such as fuzzy set theory and genetic algorithms.

  7. Influence of the form of the magnetic axis on the regions of stability and their variations (1963); Influence de la forme de l'axe magnetique sur les plages de stabilite et leur variation (1963)

    Energy Technology Data Exchange (ETDEWEB)

    Mercier, C.; Tasso, H. [Commissariat a l' Energie Atomique, Fontenay-aux-Roses (France). Centre d' Etudes Nucleaires

    1963-07-01

    We study many cases of plane and twisted magnetic axis and we show for a set of regular magnetic axis tending to racetrack limit, the stability regions tend rapidly to the racetrack stability. But, for the case at two axis apparently not very far, we find that the corresponding regions of stability may be sometimes sensibly different. (authors) [French] Nous etudions plusieurs exemples d'axes magnetiques plans et gauches et montrons que pour une suite d'axes magnetiques qui converge vers une limite du type hippodrome, les plages de stabilite convergent rapidement vers la plage limite. Mais, si on prend deux axes apparemment peu eloignes, on trouve que les plages correspondantes peuvent etre parfois sensiblement differentes. (auteurs)

  8. Sequential Star Formation in RCW 34: A Spectroscopic Census of the Stellar Content of High-mass Star-forming Regions

    CERN Document Server

    Bik, A; Waters, L B F M; Horrobin, M; Henning, Th; Vasyunina, T; Beuther, H; Linz, H; Kaper, L; Ancker, M van den; Lenorzer, A; Churchwell, E; Kurtz, S; Kouwenhoven, M B N; Stolte, A; de Koter, A; Thi, W- F; Comeron, F; Waelkens, Ch

    2010-01-01

    We present VLT/SINFONI integral field spectroscopy of RCW 34 along with Spitzer/IRAC photometry of the surroundings. RCW 34 consists of three different regions. A large bubble has been detected on the IRAC images in which a cluster of intermediate- and low-mass class II objects is found. At the northern edge of this bubble, an HII region is located, ionized by 3 OB stars. Intermediate mass stars (2 - 3 Msun) are detected of G- and K- spectral type. These stars are still in the pre-main sequence (PMS) phase. North of the HII region, a photon-dominated region is present, marking the edge of a dense molecular cloud traced by H2 emission. Several class 0/I objects are associated with this cloud, indicating that star formation is still taking place. The distance to RCW 34 is revised to 2.5 +- 0.2 kpc and an age estimate of 2 - 1 Myrs is derived from the properties of the PMS stars inside the HII region. The most likely scenario for the formation of the three regions is that star formation propagates from South to ...

  9. Evaluating Form and Function of Regional Partnerships: Applying Social Network Analysis to the "Network for a Healthy California", 2001-2007

    Science.gov (United States)

    Gregson, Jennifer; Sowa, Marcy; Flynn, Heather Kohler

    2011-01-01

    Objective: To evaluate the partnership structure of the "Network for a Healthy California" ("Network"), a social marketing program, from 2001-2007, to determine if California's program was able to establish and maintain partnerships that (1) provided access to a local audience, (2) facilitated regional collaboration, (3)…

  10. Isolation and measurement of the features of arrays of cell aggregates formed by dielectrophoresis using the user-specified Multi Regions Masking (MRM) technique

    Energy Technology Data Exchange (ETDEWEB)

    Yusvana, Rama; Markx, Gerard H [School of Engineering and Physical Science, Department of Chemical Engineering, Heriot-Watt University, Riccarton Campus, Edinburgh - EH14 4AS (United Kingdom); Headon, Denis, E-mail: g.h.markx@hw.ac.u [Roslin Institute and Royal (Dick) School of Veterinary Studies, University of Edinburgh, Roslin, Midlothian, Edinburgh - EH25 9PS (United Kingdom)

    2009-08-01

    The use of dielectrophoresis for the construction of artificial skin tissue with skin cells in follicle-like 3D cell aggregates in well-defined patterns is demonstrated. To analyse the patterns produced and to study their development after their formation a Virtual Instrument (VI) system was developed using the LabVIEW IMAQ Vision Development Module. A series of programming functions (algorithms) was used to isolate the features on the image (in our case; the patterned aggregates) and separate them from all other unwanted regions on the image. The image was subsequently converted into a binary version, covering only the desired microarray regions which could then be analysed by computer for automatic object measurements. The analysis utilized the simple and easy-to-use User-Specified Multi-Regions Masking (MRM) technique, which allows one to concentrate the analysis on the desired regions specified in the mask. This simplified the algorithms for the analysis of images of cell arrays having similar geometrical properties. By having a collection of scripts containing masks of different patterns, it was possible to quickly and efficiently develop sets of custom virtual instruments for the offline or online analysis of images of cell arrays in the database.

  11. OH (1720 MHz) Masers: A Multiwavelength Study of the Interaction between the W51C Supernova Remnant and the W51B Star Forming Region

    CERN Document Server

    Brogan, C L; Hunter, T R; Richards, A M S; Chandler, C J; Lazendic, J S; Koo, B -C; Hoffman, I M; Claussen, M J

    2013-01-01

    We present a comprehensive view of the W51B HII region complex and the W51C supernova remnant (SNR) using new radio observations from the VLA, VLBA, MERLIN, JCMT, and CSO along with archival data from Spitzer, ROSAT, ASCA, and Chandra. Our VLA data include the first 400 cm (74 MHz) continuum image of W51 at high resolution (88 arcsec). The 400 cm image shows non-thermal emission surrounding the G49.2-0.3 HII region, and a compact source of non-thermal emission (W51B_NT) coincident with the previously-identified OH (1720 MHz) maser spots, non-thermal 21 and 90 cm emission, and a hard X-ray source. W51B_NT falls within the region of high likelihood for the position of TeV gamma-ray emission. Using the VLBA three OH (1720 MHz) maser spots are detected in the vicinity of W51B_NT with sizes of 60 to 300 AU and Zeeman effect magnetic field strengths of 1.5 to 2.2 mG. The multiwavelength data demonstrate that the northern end of the W51B HII region complex has been partly enveloped by the advancing W51C SNR and this...

  12. The GABA[subscript A] Receptor Agonist Muscimol Induces an Age- and Region-Dependent Form of Long-Term Depression in the Mouse Striatum

    Science.gov (United States)

    Zhang, Xiaoqun; Yao, Ning; Chergui, Karima

    2016-01-01

    Several forms of long-term depression (LTD) of glutamatergic synaptic transmission have been identified in the dorsal striatum and in the nucleus accumbens (NAc). Such experience-dependent synaptic plasticity might play important roles in reward-related learning. The GABA[subscript A] receptor agonist muscimol was recently found to trigger a…

  13. Urban Courtyard Housing Form as a Response to Human Need, Culture and Environment in Hot Climate Regions: Baghdad as a Case Study

    Directory of Open Access Journals (Sweden)

    Wezha Hawez Baiz

    2016-09-01

    Full Text Available Courtyard housing is an important dwelling type in human history. It was founded in many ancient histories of different countries and climate zones. Many factors influenced certain types and forms of urban courtyard houses in order to create better living environments. This study try to explore some criticize points about basic human needs of courtyards. Which it refers to environmental and social backgrounds during past times, which it selected to analyze two contemporary types of traditional sample work in Baghdad.Drawings and framework used to understand the ideology of courtyards as well as other factors related to territory, society, psychology, culture and environment. Religion and traditions of Baghdad have played a special role. Through time and across cultures, territorial and environmental factors were found to be highly relevant to almost all the courtyard-housing forms. This study might be helpful for architects where they undertake contemporary design works.

  14. The FMOS-COSMOS survey of star-forming galaxies at z~1.6. IV: Excitation state and chemical enrichment of HII regions

    CERN Document Server

    Kashino, D; Sanders, D; Kartaltepe, J S; Daddi, E; Renzini, A; Valentino, F; Rodighiero, G; Juneau, S; Kewley, L J; Zahid, H J; Arimoto, N; Nagao, T; Chu, J; Sugiyama, N; Civano, F; Ilbert, O; Kajisawa, M; Fevre, O Le; Maier, C; Onodera, M; Puglisi, A; Taniguchi, Y; COSMOS,

    2016-01-01

    We present results on the physical conditions of the interstellar medium of star-forming galaxies at 1.410^11Msun being well sampled. The excitation state and chemical enrichment of the ionized gas are investigated using diagnostic diagrams based on the ratios of emission line strengths, including Alpha, [NII]6584, [SII]6717,6731, Hbeta, and [OIII]5007. Our data confirm an offset of the star-forming sequence on the BPT diagram ([OIII]/Hbeta vs. [NII]/Halpha), primarily towards higher [OIII]/Hbeta, compared with local star-forming galaxies. Based on the [SII] ratio, we measure an electron density (n_e=222^{+172}_{-128} cm^-3), higher than that of local galaxies. Overall, these changes in emission-line properties are due to a higher ionization parameter in high redshift galaxies as demonstrated by a lower than expected [SII]/Halpha ratio and a comparison to theoretical models. These results likely rule out an offset in the BPT diagram caused by a harder radiation field or AGN as assessed with Chandra. Finally, ...

  15. [Content of natural uranium in the lichens and distribution of forms in the soil at the coastal area of Lakes Itkul and Sinara of Chelyabinsk region].

    Science.gov (United States)

    Polyudina, A L; Deryagin, V V; Levina, S G

    2014-01-01

    The distribution of natural uranium in soils superaquatic and transeluvial positions of the coastal landscape of lakes Itkul and Sinara, and liches on this site.The necessity of analysis of the content item in accordance with its form of occurrence in the natural environment. The peculiarities of the migration, accumulation and distribution of uranium in soils of the mountain areas of the watersheds of lakes Itkul and Sinara are found. Identified of specificity species lichens on the content of uranium in the substrate.

  16. FOSTER FAMILY AS A FORM OF UNITS FOR ORPHANS AND CHILDREN WITHOUT PARENTAL CARE (CASE STUDY OF SARATOV AND BELGOROD REGIONS

    Directory of Open Access Journals (Sweden)

    Oksana Vladimirovna Besschetnova

    2013-09-01

    Full Text Available This paper discusses the development and functioning of foster families, one of the priority interventions for children without parental care in Russia and abroad. The paper analyzes the current official statistics on the problem of child abandonment in Russia as a whole and in the Saratov and Belgorod regions of Russia in particular. The mechanism of social adaptation of children in foster care is based on the qualitative and quantitative methods (surveys and interviews of foster parents and foster children. The author identifies obstacles to the development of social institutions in the regions and the necessity of its active implementation in domestic social practices. The study found that foster care has been successful in areas where accepted legal basis allowed the recruiting, selecting candidates for adoptive parents, and foster care maintenance are carried out by social services. In addition, in order to reduce risk factors such as the secondary abandonment of foster children it is necessarily to increase assistance from the social guardianship bodies and professionals as well as building trusting parent-child relationships that use the democratic parenting style by foster parents.DOI: http://dx.doi.org/10.12731/2218-7405-2013-8-8

  17. Water emission from the high-mass star-forming region IRAS 17233-3606. High water abundances at high velocities

    CERN Document Server

    Leurini, S; Wyrowski, F; Codella, C; Csengeri, T; van der Tak, F; Beuther, H; Flower, D R; Comito, C; Schilke, P

    2014-01-01

    We investigate the physical and chemical processes at work during the formation of a massive protostar based on the observation of water in an outflow from a very young object previously detected in H2 and SiO in the IRAS 17233-3606 region. We estimated the abundance of water to understand its chemistry, and to constrain the mass of the emitting outflow. We present new observations of shocked water obtained with the HIFI receiver onboard Herschel. We detected water at high velocities in a range similar to SiO. We self-consistently fitted these observations along with previous SiO data through a state-of-the-art, one-dimensional, stationary C-shock model. We found that a single model can explain the SiO and H2O emission in the red and blue wings of the spectra. Remarkably, one common area, similar to that found for H2 emission, fits both the SiO and H2O emission regions. This shock model subsequently allowed us to assess the shocked water column density, N(H2O)=1.2x10^{18} cm^{-2}, mass, M(H2O)=12.5 M_earth, a...

  18. How regional museums form a museum cluster and forge its identity: Take7 Shanghai Science & Technology Museum as an example

    Institute of Scientific and Technical Information of China (English)

    2015-01-01

    At present, there are many cases of museum clusters around the world, such as Smithsonian Insti- tution, the Guggenheim Museums and Foundation, Science Museums Group, National Museum Liverpool and so on. Through the analysis, we found that they form clusters in different ways, but they are for the same pur- pose, which is to provide multiple services for the public from the different cultural environment, and to strengthen the local cultural expression and transmission. Shanghai Science & Technology Museum is a large-scale comprehensive museum which contains three venues: a science and technology museum, a natu- ral history museum and a planetarium. Through learns the experience of the international cases for museum clusters, also explore itself museum cluster road to meet the local cultural environment.

  19. Binding labour and capital: moral obligation and forms of regulation in a regional economy Ligando o trabalho e o capital: obrigação moral e formas de regulação numa economia regional

    Directory of Open Access Journals (Sweden)

    Susana Narotzky

    2006-11-01

    Full Text Available The article is a critique of models of successful economic development in Europe based on the "economic region" idea. These models stress the usefulness of embedding economic relations in the social fabric ("social capital". The ethnography reveals, however, a conflict-laden space where increased embeddedness produces increased tension within the family and the community. In this "modelic" regional economy in Southern Alicante (Spain, recent violent events have involved local actors in the shoe-wear industry, with resident Chinese entrepreneurs. I will show how this confrontation underlines the rise of local modalities of conflict that build upon the organic and culturally bounded elements of economic production that the model stresses: local homogeneity and common interest. The ethnographic evidence shows the complexity of a "regional economy" in a globalized context where appeals to the State to strengthen and enforce some regulations coexist with appeals to de-regulate other areas of the economy.Este artigo é uma crítica aos modelos de sucesso de desenvolvimento económico na Europa baseados na ideia de "região económica". Estes modelos acentuam a utilidade do encastramento das relações económicas no tecido social ("capital social". No entanto, a etnografia mostra-nos um espaço de conflito onde um crescente encastramento produz um aumento da tensão na família e na comunidade. Nesta economia regional "modelar" do sul de Alicante (Espanha, episódios recentes de violência envolveram actores locais da indústria do calçado com empresários chineses aí residentes. Mostrarei como este confronto ilustra o surgimento de modalidades locais de conflito que se exprimem na base dos elementos orgânicos e de enraizamento cultural da produção económica sublinhados pelo modelo: a homogeneidade local e o interesse comum. A investigação etnográfica mostra a complexidade da "economia regional" num contexto globalizado, onde apelos dirigidos

  20. Floodplain inundation response to climate, valley form, and flow regulation on a gravel-bed river in a Mediterranean-climate region

    Science.gov (United States)

    Cienciala, P.; Pasternack, G. B.

    2017-04-01

    Floodplain inundation regime defines hydrological connectivity between river channel and floodplain and thus strongly controls structure and function of these highly diverse and productive ecosystems. We combined an extensive LiDAR data set on topography and vegetation, long-term hydrological records, as well as the outputs of hydrological and two-dimensional hydraulic models to examine how floodplain inundation regimes in a dynamic, regulated, gravel-cobble river in a Mediterranean-climate region are controlled by reach-scale valley morphology, hydroclimatic conditions, and flow regulation. Estimated relative differences in the extent, duration, and cumulative duration of inundation events were often as large as an order of magnitude and generally greatest for large and long duration events. The relative impact of flow regulation was greatest under dry hydroclimatic conditions. Although the effects of hydroclimate and flow impairment are larger than that of valley floor topography, the latter controls sensitivity of floodplain hydroperiod to flow regime changes and should not be ignored. These quantitative estimates of the relative importance of factors that control floodplain processes in Mediterranean, semiarid rivers contributes to better understanding of hydrology and geomorphology of this important class of channels. We also discuss implications of our findings for processes that shape floodplain habitat for riparian vegetation and salmonid fish, especially in the context of ecological restoration.

  1. The extinction curves of star-forming regions from z=0.1 to 6.7 using GRB afterglow spectroscopy

    CERN Document Server

    Zafar, Tayyaba; Fynbo, Johan P U; Malesani, Daniele; Jakobsson, Pall; Postigo, Antonio de Ugarte

    2011-01-01

    GRB afterglows are well suited to extinction studies due to their brightness, simple power-law spectra and the occurrence of GRBs in distant star forming galaxies. In this paper we present results from the SED analysis of a sample of 41 GRB afterglows, from X-ray to NIR wavelengths. This is the largest sample of extinction curves outside the Local Group and, to date, the only extragalactic sample of absolute extinction curves based on spectroscopy. Visual extinction correlation with HI column density as well as total and gas-phase metal column density are examined. Approximately half the sample require a cooling break between the optical and X-ray regimes. The broken power-law SEDs show an average change in the spectral index of delta_beta=0.51 with a standard deviation of 0.02. This is consistent with the expectation from a simple synchrotron model. Of the sample, 63% are well described by the SMC-type extinction curve and have moderate or low extinction, with AV1.0. We find an anti-correlation between gas-t...

  2. Exploring the role of cognitive and structural forms of social capital in HIV/AIDS trends in the Kagera region of Tanzania - a grounded theory study.

    Science.gov (United States)

    Frumence, Gasto; Eriksson, Malin; Nystrom, Lennarth; Killewo, Japhet; Emmelin, Maria

    2011-04-01

    The article presents a synthesis of data from three village case studies focusing on how structural and cognitive social capital may have influenced the progression of the HIV epidemic in the Kagera region of Tanzania. Grounded theory was used to develop a theoretical model describing the possible links between structural and cognitive social capital and the impact on sexual health behaviours. Focus group discussions and key informant interviews were carried out to represent the range of experiences of existing social capital. Both structural and cognitive social capital were active avenues for community members to come together, empower each other, and develop norms, values, trust and reciprocal relations. This empowerment created an enabling environment in which members could adopt protective behaviours against HIV infection. On the one hand, we observed that involvement in formal and informal organisations resulted in a reduction of numbers of sexual partners, led people to demand abstinence from sexual relations until marriage, caused fewer opportunities for casual sex, and gave individuals the agency to demand the use of condoms. On the other hand, strict membership rules and regulations excluded some members, particularly excessive alcohol drinkers and debtors, from becoming members of the social groups, which increased their vulnerability in terms of exposure to HIV. Social gatherings (especially those organised during the night) were also found to increase youths' risk of HIV infection through instances of unsafe sex. We conclude that even though social capital may at times have negative effects on individuals' HIV-prevention efforts, this study provides initial evidence that social capital is largely protective through empowering vulnerable groups such as women and the poor to protect against HIV infection and by promoting protective sexual behaviours.

  3. On the Formation of the C2H6O Isomers Ethanol (C2H5OH) and Dimethyl Ether (CH3OCH3) in Star-forming Regions

    Science.gov (United States)

    Bergantini, Alexandre; Maksyutenko, Pavlo; Kaiser, Ralf I.

    2017-06-01

    The structural isomers ethanol (CH3CH2OH) and dimethyl ether (CH3OCH3) were detected in several low-, intermediate-, and high-mass star-forming regions, including Sgr B2, Orion, and W33A, with the relative abundance ratios of ethanol/dimethyl ether varying from about 0.03 to 3.4. Until now, no experimental data regarding the formation mechanisms and branching ratios of these two species in laboratory simulation experiments could be provided. Here, we exploit tunable photoionization reflectron time-of-flight mass spectrometry (PI-ReTOF-MS) to detect and analyze the production of complex organic molecules (COMs) resulting from the exposure of water/methane (H2O/CH4) ices to energetic electrons. The main goal is to understand the formation mechanisms in star-forming regions of two C2H6O isomers: ethanol (CH3CH2OH) and dimethyl ether (CH3OCH3). The results show that the experimental branching ratios favor the synthesis of ethanol versus dimethyl ether (31 ± 11:1). This finding diverges from the abundances observed toward most star-forming regions, suggesting that production routes on interstellar grains to form dimethyl ether might be missing; alternatively, ethanol can be overproduced in the present simulation experiments, such as via radical-radical recombination pathways involving ethyl and hydroxyl radicals. Finally, the PI-ReTOF-MS data suggest the formation of methylacetylene (C3H4), ketene (CH2CO), propene (C3H6), vinyl alcohol (CH2CHOH), acetaldehyde (CH3CHO), and methyl hydroperoxide (CH3OOH), in addition to ethane (C2H6), methanol (CH3OH), and CO2 detected from infrared spectroscopy. The yield of all the confirmed species is also determined.

  4. Comparison of B{sub 2}O{sub 3} and BN deposited by atomic layer deposition for forming ultrashallow dopant regions by solid state diffusion

    Energy Technology Data Exchange (ETDEWEB)

    Consiglio, Steven, E-mail: steve.consiglio@us.tel.com; Clark, Robert D.; O' Meara, David; Wajda, Cory S.; Tapily, Kandabara; Leusink, Gert J. [TEL Technology Center, America, LLC, 255 Fuller Rd., Albany, New York 12203 (United States)

    2016-01-15

    In this study, the authors investigated atomic layer deposition (ALD) of B{sub 2}O{sub 3} and BN for conformal, ultrashallow B doping applications and compared the effect of dopant-containing overlayers on sheet resistance (R{sub s}) and B profiles for both types of films subjected to a drive-in thermal anneal. For the deposition of B{sub 2}O{sub 3}, tris(dimethylamido)borane and O{sub 3} were used as coreactants and for the deposition of BN, BCl{sub 3} and NH{sub 3} were used as coreactants. Due to the extreme air instability of B{sub 2}O{sub 3} films, physical analysis was performed on B{sub 2}O{sub 3} films, which were capped in-situ with ∼30 Å ALD grown Al{sub 2}O{sub 3} layers. For the BN films, in-situ ALD grown Si{sub 3}N{sub 4} capping layers (∼30 Å) were used for comparison. From spectroscopic ellipsometry, a thickness decrease was observed after 1000 °C, 30 s anneal for the B{sub 2}O{sub 3} containing stack with 60 ALD cycles of B{sub 2}O{sub 3}, whereas the BN containing stacks showed negligible thickness decrease after the annealing step, regardless of the number of BN cycles tested. The postanneal reduction in film thickness as well as decrease in R{sub s} for the B{sub 2}O{sub 3} containing stack suggests that the solid state diffusion dopant mechanism is effective, whereas for the BN containing stacks this phenomenon seems to be suppressed. Further clarification of the effectiveness of the B{sub 2}O{sub 3} containing layer compared to the film stacks with BN was evidenced in backside secondary ion mass spectrometry profiling of B atoms. Thus, B{sub 2}O{sub 3} formed by an ALD process and subsequently capped in-situ followed by a drive-in anneal offers promise as a dopant source for ultrashallow doping, whereas the same method using BN seems ineffective. An integrated approach for B{sub 2}O{sub 3} deposition and annealing on a clustered tool also demonstrated controllable R{sub s} reduction without the use of a capping layer.

  5. Millimeter- and Submillimeter-Wave Observations of the OMC-2/3 region. IV Interaction between the Outflow and the Dense Gas in the Cluster Forming Region of OMC-2 FIR 6

    CERN Document Server

    Shimajiri, Yoshito; Takakuwa, Shigehisa; Saito, Masao; Kawabe, Ryohei

    2009-01-01

    We have conducted millimeter interferometric observations of the Orion Molecular Cloud-2 (OMC-2) FIR 6 region at an angular resolution of $\\sim$ 4$\\arcsec$ - 7$\\arcsec$ with the Nobeyama Millimeter Array (NMA). In the 3.3 mm continuum emission we detected dusty core counterparts of the previously identified FIR sources (FIR 6a, 6b, 6c, and 6d), and moreover, resolved FIR 6a into three dusty cores. The size and mass of these cores are estimated to be 1100-5900 AU and 0.19-5.5 M$_{\\odot}$, respectively. We found that in the $^{12}$CO ($J$=1--0) emission FIR 6b, 6c, and 6d eject the molecular outflow and that the FIR 6c outflow also exhibits at least two collimated jet-like components in the SiO ($J$=2--1) emission. At the tip of one of the SiO components there appears abrupt increase of the SiO line width ($\\sim$ 15 km s$^{-1}$), where the three resolved cores in FIR 6a seem to delineate the tip. These results imply the presence of the interaction and the bowshock front between the FIR 6c molecular outflow and ...

  6. Tidal Forms

    Science.gov (United States)

    Bolla Pittaluga, M.; Seminara, G.; Tambroni, N.

    2003-04-01

    We give an overview of some recent investigations on the mechanics of the processes whereby forms develop in tidal environments. The viewpoint taken here is mechanistic. Some of the questions which deserve an answer may be summarised as follows: i) do tidal channels tend to some altimetric long term equilibrium? ii) why are they typically convergent and weakly meandering? iii) how is such equilibrium affected by the hydrodynamics and morphodynamics of tidal inlets? iv) what is the hydrodynamic and morphodynamic role played by tidal flats adjacent to the channels? Some of the above questions have received a considerable attention in the last few years. Schuttelaars and de Swart (1996), Lanzoni and Seminara (2002) and, more recently, Bolla Pittaluga (2003) have investigated the first problem. In particular, the latter two contributions have shown that a straight tidal channel connected to a tidal sea at one end and closed at the other end tends to reach a long term equilibrium profile, which is slightly concave seaward and convex landward where a beach forms. The equilibrium profile is strongly sensitive to the harmonic content of the tidal forcing as well as to the value of sediment concentration established by the coastal hydrodynamics in the far field of the inlet region. Less important are the effect of channel convergence and the role of settling lag in the transport of suspended load. Insufficient attention has been devoted to the understanding of what mechanisms control channel convergence and meandering, though some similarities and differences between tidal and fluvial channels have emerged from some recent works. In particular, free bars form in tidal channels due to an instability mechanism essentially similar to that occurring under steady conditions though the oscillatory character of the flow field makes the bar pattern non migrating (Seminara and Tubino, 2001). Similarly, forced bars in curved tidal channels are driven by the development of

  7. Characterizing filaments in regions of high-mass star formation: High-resolution submilimeter imaging of the massive star-forming complex NGC 6334 with ArTéMiS

    Science.gov (United States)

    André, Ph.; Revéret, V.; Könyves, V.; Arzoumanian, D.; Tigé, J.; Gallais, P.; Roussel, H.; Le Pennec, J.; Rodriguez, L.; Doumayrou, E.; Dubreuil, D.; Lortholary, M.; Martignac, J.; Talvard, M.; Delisle, C.; Visticot, F.; Dumaye, L.; De Breuck, C.; Shimajiri, Y.; Motte, F.; Bontemps, S.; Hennemann, M.; Zavagno, A.; Russeil, D.; Schneider, N.; Palmeirim, P.; Peretto, N.; Hill, T.; Minier, V.; Roy, A.; Rygl, K. L. J.

    2016-07-01

    Context. Herschel observations of nearby molecular clouds suggest that interstellar filaments and prestellar cores represent two fundamental steps in the star formation process. The observations support a picture of low-mass star formation according to which filaments of ~0.1 pc width form first in the cold interstellar medium, probably as a result of large-scale compression of interstellar matter by supersonic turbulent flows, and then prestellar cores arise from gravitational fragmentation of the densest filaments. Whether this scenario also applies to regions of high-mass star formation is an open question, in part because the resolution of Herschel is insufficient to resolve the inner width of filaments in the nearest regions of massive star formation. Aims: In an effort to characterize the inner width of filaments in high-mass star-forming regions, we imaged the central part of the NGC 6334 complex at a resolution higher by a factor of >3 than Herschel at 350 μm. Methods: We used the large-format bolometer camera ArTéMiS on the APEX telescope and combined the high-resolution ArTéMiS data at 350 μm with Herschel/HOBYS data at 70-500 μm to ensure good sensitivity to a broad range of spatial scales. This allowed us to study the structure of the main narrow filament of the complex with a resolution of 8″ or inner width remains as narrow as W ~ 0.15 ± 0.05 pc all along the filament length, within a factor of Belt. Conclusions: While it is not completely clear whether the NGC 6334 filament will form massive stars in the future, it is two to three orders of magnitude denser than the majority of filaments observed in Gould Belt clouds, and has a very similar inner width. This points to a common physical mechanism for setting the filament width and suggests that some important structural properties of nearby clouds also hold in high-mass star-forming regions. This publication is based on data acquired with the Atacama Pathfinder Experiment (APEX) in ESO program

  8. Regionalism, Regionalization and Regional Development

    Directory of Open Access Journals (Sweden)

    Liviu C. Andrei

    2016-03-01

    Full Text Available Sustained development is a concept associating other concepts, in its turn, in the EU practice, e.g. regionalism, regionalizing and afferent policies, here including structural policies. This below text, dedicated to integration concepts, will limit on the other hand to regionalizing, otherwise an aspect typical to Europe and to the EU. On the other hand, two aspects come up to strengthen this field of ideas, i.e. the region (al-regionalism-(regional development triplet has either its own history or precise individual outline of terms.

  9. Narrative form

    CERN Document Server

    Keen, Suzanne

    2015-01-01

    This revised and expanded handbook concisely introduces narrative form to advanced students of fiction and creative writing, with refreshed references and new discussions of cognitive approaches to narrative, nonfiction, and narrative emotions.

  10. Polarized light from star forming regions

    Science.gov (United States)

    Weintraub, D.; Goodman, A.; Akeson, A.

    2000-01-01

    Studies of polarized radiation from molecular clouds and the environments of protostars are providing information about the orientations and strengths of magnetic fields and the sizes andcompositions of dust grains in these environments.

  11. Star forming regions of the southern galaxy

    Science.gov (United States)

    Kuiper, T. B. H.; Er, J. W., the molecular gas, a

    1987-01-01

    A catalog of southern dust cloud properties is being compiled to aid in the planning and analysis of radio spectral line surveys in the southern hemisphere. Ultimately, images of dust temperature and column density will be produced. For the interim, a list of the 60 and 100 micron fluxes was prepared for the cores and adjacent backgrounds of 65 prominent dust clouds. Dust temperatures and column densities were derived.

  12. Fri form

    DEFF Research Database (Denmark)

    Jensen, Henrik

    2006-01-01

    Dette Kompendiun er lavet i forbindelse med en workshop i møbeldesign. En række af form-Z's værktøjer til konstruktion af dobbeltkrumme flader gennemgås. Kompendiet kan bruges til selvstudie.......Dette Kompendiun er lavet i forbindelse med en workshop i møbeldesign. En række af form-Z's værktøjer til konstruktion af dobbeltkrumme flader gennemgås. Kompendiet kan bruges til selvstudie....

  13. Hubble Space Telescope Hx Imaging of Star-forming Galaxies at z approximately equal to 1-1.5: Evolution in the Size and Luminosity of Giant H II Regions

    Science.gov (United States)

    Livermore, R. C.; Jones, T.; Richard, J.; Bower, R. G.; Ellis, R. S.; Swinbank, A. M.; Rigby, J. R.; Smail, Ian; Arribas, S.; Rodriguez-Zaurin, J.; hide

    2013-01-01

    We present Hubble Space Telescope/Wide Field Camera 3 narrow-band imaging of the Ha emission in a sample of eight gravitationally lensed galaxies at z = 1-1.5. The magnification caused by the foreground clusters enables us to obtain a median source plane spatial resolution of 360 pc, as well as providing magnifications in flux ranging from approximately 10× to approximately 50×. This enables us to identify resolved star-forming HII regions at this epoch and therefore study their Ha luminosity distributions for comparisons with equivalent samples at z approximately 2 and in the local Universe. We find evolution in the both luminosity and surface brightness of HII regions with redshift. The distribution of clump properties can be quantified with an HII region luminosity function, which can be fit by a power law with an exponential break at some cut-off, and we find that the cut-off evolves with redshift. We therefore conclude that 'clumpy' galaxies are seen at high redshift because of the evolution of the cut-off mass; the galaxies themselves follow similar scaling relations to those at z = 0, but their HII regions are larger and brighter and thus appear as clumps which dominate the morphology of the galaxy. A simple theoretical argument based on gas collapsing on scales of the Jeans mass in a marginally unstable disc shows that the clumpy morphologies of high-z galaxies are driven by the competing effects of higher gas fractions causing perturbations on larger scales, partially compensated by higher epicyclic frequencies which stabilize the disc.

  14. Automorphic Forms

    DEFF Research Database (Denmark)

    von Essen, Flemming Brændgaard

    systems. For automorphic forms wrt. Hecke triangle groups and Fuchsian groups with no elliptic elements and genus 0, we show that some logarithms of multiplier systems can be interpreted as a linking number. Finally we show a "twisted" version of the prime geodesics theorem, and logarithms of multiplier...

  15. Cosmic Forms

    CERN Document Server

    Kleman, Maurice

    2011-01-01

    The continuous 1D defects of an isotropic homogeneous material in an Euclidean 3D space are classified by a construction method, the Volterra process (VP). We employ the same method to classify the continuous 2D defects (which we call \\textit{cosmic forms}) of a vacuum in a 4D maximally symmetric spacetime. These defects fall into three different classes: i)- $m$-forms, akin to 3D space disclinations, related to ordinary rotations and analogous to Kibble's global cosmic strings (except that being continuous any deficit angle is allowed); ii)- $t$-forms, related to Lorentz boosts (hyperbolic rotations); iii)- $r$-forms, never been considered so far, related to null rotations. A detailed account of their metrics is presented. Their inner structure in many cases appears as a non-singular \\textit{core} separated from the outer part by a timelike hypersurface with distributional curvature and/or torsion, yielding new types of geometrical interactions with cosmic dislocations and other cosmic disclinations. Whereas...

  16. Characterizing filaments in regions of high-mass star formation: High-resolution submilimeter imaging of the massive star-forming complex NGC 6334 with ArT\\'eMiS

    CERN Document Server

    André, Ph; Könyves, V; Arzoumanian, D; Tigé, J; Gallais, P; Roussel, H; Pennec, J Le; Rodriguez, L; Doumayrou, E; Dubreuil, D; Lortholary, M; Martignac, J; Talvard, M; Delisle, C; Visticot, F; Dumaye, L; De Breuck, C; Shimajiri, Y; Motte, F; Bontemps, S; Hennemann, M; Zavagno, A; Russeil, D; Schneider, N; Palmeirim, P; Peretto, N; Hill, T; Minier, V; Roy, A; Rygl, K L J

    2016-01-01

    Herschel observations of nearby molecular clouds suggest that interstellar filaments and prestellar cores represent two fundamental steps in the star formation process. The observations support a picture of low-mass star formation according to which ~ 0.1 pc-wide filaments form first in the cold interstellar medium, probably as a result of large-scale compression of interstellar matter by supersonic turbulent flows, and then prestellar cores arise from gravitational fragmentation of the densest filaments. Whether this scenario also applies to regions of high-mass star formation is an open question, in part because Herschel data cannot resolve the inner width of filaments in the nearest regions of massive star formation. We used the bolometer camera ArTeMiS on the APEX telescope to map the central part of the NGC6334 complex at a factor of > 3 higher resolution than Herschel at 350 microns. Combining ArTeMiS data with Herschel data allowed us to study the structure of the main filament of the complex with a re...

  17. Increased expression of phosphorylated forms of heat-shock protein-27 and p38MAPK in macrophage-rich regions of fibro-fatty atherosclerotic lesions in the rabbit.

    Science.gov (United States)

    Shafi, Shahida; Codrington, Rosalind; Gidden, Lewis Michael; Ferns, Gordon Ashley Anthony

    2016-02-01

    We aimed to assess the expression and distribution of Hsp27, pHsp27 (Ser82), p38MAPK and p-p38MAPK in fibro-fatty atherosclerotic lesions and the myocardium of hypercholesterolaemic rabbits. Male New Zealand white rabbits were fed a high-cholesterol diet for 18 weeks, maintaining serum cholesterol at approximately 20 mmol/l over this period. Aortic arch and myocardial tissues were analysed by Western blot, immunohistochemistry and double immunofluorescence. Plasma Hsp27 levels were measured by ELISA. There was a significant increase in the expression of monomeric and dimeric forms of Hsp27, together with pHsp27 (Ser82), p38MAPK and p-p38MAPK in the fibro-fatty atherosclerotic lesions (P < 0.01; P < 0.05; P < 0.001; and P < 0.001, respectively) and the myocardial tissues (P < 0.001) from the cholesterol-fed rabbits compared with equivalent tissues from controls when the plasma concentration was low. Immunohistochemical analysis of the fibro-fatty lesions showed marked increases in Hsp27 and pHsp27 (Ser82) immunoreactivity. Double immunostaining showed intense expression of pHsp27 and p-p38MAPK in regions that were rich in macrophages, suggesting a close association with these inflammatory cells, whereas, in regions rich in smooth muscle cells, only p-p38MAPK was found to be strongly expressed. An increased expression of pHsp27 (Ser82) was spatially associated with increased p-p38MAPK within fibro-fatty atherosclerotic lesions and was colocalized to regions rich in macrophages. The initial increase in plasma Hsp27 levels may reflect the increase in systemic inflammation and oxidative stress in the early phases of disease. The falling concentrations subsequently may be coincident with the development of the advanced atherosclerotic lesions.

  18. Concept Definition and Scale Development of Regional Environmental Advantage From the Perspective of Regional Brand Forming%区域环境优势的概念界定与量表开发基于区域品牌形成的视角

    Institute of Scientific and Technical Information of China (English)

    徐明; 盛亚军; 魏胜

    2015-01-01

    The creation and cultivation of regional brands has become a powerful booster to develop regional economy and regional image, and regional environmental advantage serves as an important factor that affects regional brand forming,but its concept definition and measurement require improving. The concept of regional environmental advantage was first defined, and the measurement scale was then developed by following such steps as item pool establishment, item purification, and reliability and validity testing. It was concluded that regional environmental advantage is composed of five dimensions:resources environment, cultural environment, investing and financing environment,institutional environment and social environment.The findings may provide the decision-making basis and theoretical guidance for developing regional brands in many other regions.%创建、培育区域品牌已经成为发展区域经济和塑造区域形象的有力助推器,区域品牌形成所处的区域环境优势成为影响其形成的重要因素之一,但其概念界定与测量问题并不尽完善。界定了区域环境优势的概念,遵循题项库的建立、题项净化、信度和效度检验等步骤开发了区域环境优势的测量量表,得出区域环境优势由资源环境优势、文化环境优势、投融资环境优势、制度环境优势和社会关系环境优势等5个维度构成的研究结论,为其他地区发展区域品牌提供决策依据和理论指导。

  19. Contributors Form

    Directory of Open Access Journals (Sweden)

    Chief Editor

    2016-06-01

    to produce preprints or reprints and translate into languages other than English for sale or free distribution; and 4 the right to republish the work in a collection of articles in any other mechanical or electronic format. We give the rights to the corresponding author to make necessary changes as per the request of the journal, do the rest of the correspondence on our behalf and he/she will act as the guarantor for the manuscript on our behalf. All persons who have made substantial contributions to the work reported in the manuscript, but who are not contributors, are named in the Acknowledgment and have given me/us their written permission to be named. If I/we do not include an Acknowledgment that means I/we have not received substantial contributions from non-contributors and no contributor has been omitted.S NoAuthors' NamesContribution (IJCME Guidelines{1 substantial contributions to conception and design, acquisition of data, or analysis and interpretation of data; 2 drafting the article or revising it critically for important intellectual content; and 3 final approval of the version to be published. Authors should meet conditions 1, 2, and 3}.SignatureDate                              Note: All the authors are required to sign independently in this form in the sequence given above. In case an author has left the institution/country and whose whereabouts are not known, the senior author may sign on his/her behalf taking the responsibility.No addition/deletion/ or any change in the sequence of the authorship will be permissible at a later stage, without valid reasons and permission of the Editor.If the authorship is contested at any stage, the article will be either returned or will not be processed for publication till the issue is solved.Maximum up to 4 authors for short communication and up to 6 authors for original article.

  20. STUDY ON THE PROBLEMS IN THE STAGES OF FILLING OUT THE APPLICATION FORM AND TECHNICAL-FINANCIAL REPORTING ENCOUNTERED BY THE PUBLIC INSTITUTIONS IN THE CENTRE REGION IN ACCESSING EUROPEAN FUNDS

    Directory of Open Access Journals (Sweden)

    DUMITRASCU DANUT

    2012-07-01

    Full Text Available The article has as main field the project management, specifically, identifying the negative factors on European projects. The article assumes that there is a connection between the absorption of European funds and the maturity of the Romanian society in terms of project management. The main objective of the research is to identify the problems faced by public institutions from Centre Region in accessing European funds. The purpose of the research is to identify the causes that led to the low absorption of European funds, with devastating effects on the current economic situation. The present research is based on a preliminary analysis performed by the author on the rate of accessing European funds published in an article entitled “The current state of European funds absorption through funding programmes – measure of the Romanian performances in the project management practice”. The small degree of absorption of European funds resulting from the analysis shows a poor practice of the theory on project management. To identify the causes of this problem, a research was carried out to recognise the issues that led to this situation. The investigation included two successive surveys, the first one qualitative, exploratory type, interview-based, meant to demonstrate the qualitative aspects of the investigated phenomena and the other one, quantitative, based on a questionnaire in the form of occasional surveys. The qualitative and quantitative research methods are used in combination; this approach has become necessary especially due to the very complex reality whose trueness cannot be captured through one method. The investigation has however a highly quantitative character, the purpose of the qualitative research being to provide the prerequisites for achieving the quantitative research. The qualitative research revealed the existence of some problems faced by institutions in relation to accessing and developing projects that focus

  1. Pion form factor

    Energy Technology Data Exchange (ETDEWEB)

    Ryong Ji, C.; Pang, A.; Szczepaniak, A. [North Carolina State Univ., Raleigh, NC (United States)

    1994-04-01

    It is pointed out that the correct criterion to define the legal PQCD contribution to the exclusive processes in the lightcone perturbative expansion should be based on the large off-shellness of the lightcone energy in the intermediate states. In the lightcone perturbative QCD calculation of the pion form factor, the authors find that the legal PQCD contribution defined by the lightcone energy cut saturates in the smaller Q{sup 2} region compared to that defined by the gluon four-momentum square cut. This is due to the contribution by the highly off-energy-shell gluons in the end point regions of the phase space, indicating that the gluon four-momentum-square cut may have cut too much to define the legal PQCD.

  2. Densified waste form and method for forming

    Science.gov (United States)

    Garino, Terry J.; Nenoff, Tina M.; Sava Gallis, Dorina Florentina

    2015-08-25

    Materials and methods of making densified waste forms for temperature sensitive waste material, such as nuclear waste, formed with low temperature processing using metallic powder that forms the matrix that encapsulates the temperature sensitive waste material. The densified waste form includes a temperature sensitive waste material in a physically densified matrix, the matrix is a compacted metallic powder. The method for forming the densified waste form includes mixing a metallic powder and a temperature sensitive waste material to form a waste form precursor. The waste form precursor is compacted with sufficient pressure to densify the waste precursor and encapsulate the temperature sensitive waste material in a physically densified matrix.

  3. Conceptual Foundations of Improving the Living Standards of Territorial Community Based on the Introduction and Development of New Forms of Innovation and Investment Cooperation Between Regional Authorities and the Local Community

    Directory of Open Access Journals (Sweden)

    Popadynets, V.I.

    2015-03-01

    Full Text Available The main provisions have been formulated for elaboration, implementation and development of the regional target programs based on new methodological and financial resources and realization of sales of the most significant products of regional companies and organizations for the sustainable improvement of the local community living standards.

  4. Forming Spirals From Shadows

    Science.gov (United States)

    Kohler, Susanna

    2016-07-01

    What causes the large-scale spiral structures found in some protoplanetary disks? Most models assume theyre created by newly-forming planets, but a new study suggests that planets might have nothing to do with it.Perturbations from Planets?In some transition disks protoplanetary disks with gaps in their inner regions weve directly imaged large-scale spiral arms. Many theories currently attribute the formation of these structures to young planets: either the direct perturbations of a planet embedded in the disk cause the spirals, or theyre indirectly caused by the orbit of a planetary body outside of the arms.Another example of spiral arms detected in a protoplanetary disk, MWC 758. [NASA/ESA/ESO/M. Benisty et al.]But what if you could get spirals without any planets? A team of scientists led by Matas Montesinos (University of Chile) have recently published a study in which they examine what happens to a shadowed protoplanetary disk.Casting Shadows with WarpsIn the teams setup, they envision a protoplanetary disk that is warped: the inner region is slightly tilted relative to the outer region. As the central star casts light out over its protoplanetary disk, this disk warping would cause some regions of the disk to be shaded in a way that isnt axially symmetric with potentially interesting implications.Montesinos and collaborators ran 2D hydrodynamics simulations to determine what happens to the motion of particles within the disk when they pass in and out of the shadowed regions. Since the shadowed regions are significantly colder than the illuminated disk, the pressure in these regions is much lower. Particles are therefore accelerated and decelerated as they pass through these regions, and the lack of axial symmetry causes spiral density waves to form in the disk as a result.Initial profile for the stellar heating rate per unit area for one of the authors simulations. The regions shadowed as a result of the disk warp subtend 0.5 radians each (shown on the left

  5. THE METHODICAL APPROACH TO THE ESTIMATION OF THE IMPORTANCE OF TAXES IN FORMING OF INCOMES OF BUDGETARY SYSTEM OF THE RUSSIAN FEDERATION ON THE EXAMPLE OF THE BELGOROD REGION

    Directory of Open Access Journals (Sweden)

    Valentina F. Tarasova

    2016-01-01

    Full Text Available Article is devoted questions of formation of tax incomes of budgetary system of the Russian Federation. Approaches of a regional tax policy are proved by granting of tax privileges. The system of factors allowing quantitatively to estimate value of tax payments in formation own and aggregate prots of the budget is offered; approbation on an example of the budget of the Belgorod region is spent.

  6. Careers (A Course of Study). Unit V: Forms, Forms, Forms.

    Science.gov (United States)

    Turley, Kay

    Designed to enable special needs students to understand and complete various job-related forms, this set of activities devoted to forms encountered before and after one obtains a job is the fifth in a nine-unit secondary level careers course intended to provide handicapped students with the knowledge and tools necessary to succeed in the world of…

  7. “Mid-G” Region Sequences of the Glycoprotein Gene of Austrian Infectious Hematopoietic Necrosis Virus Isolates Form Two Lineages within European Isolates and Are Distinct from American and Asian Lineages▿

    OpenAIRE

    Kolodziejek, Jolanta; Schachner, Oskar; Dürrwald, Ralf; Latif, Muna; Nowotny, Norbert

    2007-01-01

    Infectious hematopoietic necrosis virus (IHNV) is one of the most important pathogens of salmonid fish. In this study a comprehensive phylogenetic analysis of the genetic evolution and variety of Austrian IHNV strains, as well as selected strains ensuring worldwide coverage, is presented. The phylogenetic investigation is based on sequences comprising the “mid-G” region of the G gene, and it includes all currently available IHNV sequences of the G gene with a length of at least 615 bp. Austri...

  8. The Problem of the Golden Horde “Imperial Culture” Formation and its Role as an Area-Forming Factor for the Peoples of the Ural-Volga Region

    Directory of Open Access Journals (Sweden)

    Ivanov Vladimir A.

    2013-06-01

    Full Text Available The problem of formation and existence of a common imperial culture of the Golden Horde and the degree of influence of this state on the culture of neighboring peoples inhabiting the Urals and the Volga regions. The results of the comparison between the culture of the Golden Horde cities and the nomadic steppe population demonstrate significant differences and a very low degree of interpenetration of their traditions. In the material culture of the peoples of the Volga-Kama and the Cis-Urals regions, drawn into the Golden Horde sphere of influence (the Mari, the Udmurts, the Mordvinians, the Bashkirs, the local tradition was kept intact, items produced in the Golden Horde were as rarely met as imported ones, and did not affect the local production of weapons, jewelry, etc. All this makes it possible to conclude that the concept of "imperial culture of the Golden Horde" is an artificial one, and its influence on the cultures of the neighboring peoples of the Volga-Ural region cannot be traced on the basis of archaeological materials.

  9. PIC Reading Readiness Test Form.

    Science.gov (United States)

    Short, N. J.

    This rating form concerns the measurement of basic skills in connection with assessing reading readiness. Motor skills, ability to adjust to learning situations, familiarity with the alphabet, and general knowledge are assessed. See TM 001 111 for details of the Regional PIC program in which it is used. (DLG)

  10. On good ETOL forms

    DEFF Research Database (Denmark)

    Skyum, Sven

    1978-01-01

    This paper continues the study of ETOL forms and good EOL forms done by Maurer, Salomaa and Wood. It is proven that binary very complete ETOL forms exist, good synchronized ETOL forms exist and that no propagating or synchronized ETOL form can be very complete.......This paper continues the study of ETOL forms and good EOL forms done by Maurer, Salomaa and Wood. It is proven that binary very complete ETOL forms exist, good synchronized ETOL forms exist and that no propagating or synchronized ETOL form can be very complete....

  11. Star-forming regions at the periphery of the supershell surrounding the Cyg OB1 association. I. The star cluster vdB 130 and its ambient gas and dust medium

    CERN Document Server

    Sitnik, T G; Lozinskaya, T A; Moiseev, A V; Rastorguev, A S; Tatarnikov, A M; Tatarnikova, A A; Wiebe, D S; Zabolotskikh, M V

    2015-01-01

    Stellar population and the interstellar gas-dust medium in the vicinity of the open star cluster vdB 130 are analysed using optical observations taken with the 6-m telescope of the SAO RAS and the 125-cm telescope of the SAI MSU along with the data of Spitzer and Herschel. Based on proper motions and BV and JHKs 2MASS photometric data, we select additional 36 stars as probable cluster members. Some stars in vdB 130 are classified as B stars. Our estimates of minimum colour excess, apparent distance modulus and the distance are consistent with young age (from 5 to 10 Myrs) of the cluster vdB 130. We suppose the large deviations from the conventional extinction law in the cluster direction, with $R_V$ ~ 4 - 5. The cluster vdB 130 appears to be physically related to the supershell around Cyg OB1, a cometary CO cloud, ionized gas, and regions of infrared emission. There are a few regions of bright mid-infrared emission in the vicinity of vdB 130. The largest of them is also visible on H-alpha and [SII] emission m...

  12. Les villes frontalières thaïlandaises dans la régionalisation Thai Bordertowns in the Regionalization Process: Spatial Planing and Production of New Urban Forms

    Directory of Open Access Journals (Sweden)

    Elsa Lainé

    2013-04-01

    decentralization process initiated in the 1970’s and regional cooperation are two dynamics deeply affecting the role of international borders and putting emphasize on border regions and towns, which used to be land-locked areas at the national scale. Following this idea, bordertowns have been included in governmental spatial planning and public funds have been invested since the beginning of the 1990’s in order to upgrade infrastructures in these cities. Even if Thai bordertowns differ drastically in the national urban frame, as far as demography, economy or infrastructures level are concerned, they are nowadays facing an unprecedented dynamism sustained by regional cooperation. Case studies of three towns located on economic corridors and targeted by national plans show that their spatial organization is changing: new urban centers are emerging, interactions with the areas located on the other side of the border are being reorganized and news actors, private as public, are impacting the urban landscape and functions. These modifications are creating new challenges for local authorities, as they are also likely to promote these cities at the national and regional scales.

  13. "Mid-G" region sequences of the glycoprotein gene of Austrian infectious hematopoietic necrosis virus isolates form two lineages within European isolates and are distinct from American and Asian lineages.

    Science.gov (United States)

    Kolodziejek, Jolanta; Schachner, Oskar; Dürrwald, Ralf; Latif, Muna; Nowotny, Norbert

    2008-01-01

    Infectious hematopoietic necrosis virus (IHNV) is one of the most important pathogens of salmonid fish. In this study a comprehensive phylogenetic analysis of the genetic evolution and variety of Austrian IHNV strains, as well as selected strains ensuring worldwide coverage, is presented. The phylogenetic investigation is based on sequences comprising the "mid-G" region of the G gene, and it includes all currently available IHNV sequences of the G gene with a length of at least 615 bp. Austrian IHNVs are located--together with other European IHNV isolates--in two clusters of genogroup M (M-Eur1 and M-Eur2) and are clearly separated from American and Asian lineages. The genetic clustering, however, could not be linked to certain clinical symptoms or significant differences in the mortality rates.

  14. Modular Forms and Weierstrass Mock Modular Forms

    Directory of Open Access Journals (Sweden)

    Amanda Clemm

    2016-02-01

    Full Text Available Alfes, Griffin, Ono, and Rolen have shown that the harmonic Maass forms arising from Weierstrass ζ-functions associated to modular elliptic curves “encode” the vanishing and nonvanishing for central values and derivatives of twisted Hasse-Weil L-functions for elliptic curves. Previously, Martin and Ono proved that there are exactly five weight 2 newforms with complex multiplication that are eta-quotients. In this paper, we construct a canonical harmonic Maass form for these five curves with complex multiplication. The holomorphic part of this harmonic Maass form arises from the Weierstrass ζ-function and is referred to as the Weierstrass mock modular form. We prove that the Weierstrass mock modular form for these five curves is itself an eta-quotient or a twist of one. Using this construction, we also obtain p-adic formulas for the corresponding weight 2 newform using Atkin’s U-operator.

  15. Massive star forming environments

    Science.gov (United States)

    Devine, Kathryn Elizabeth

    2010-12-01

    We present a study of the earliest stages of massive star formation, in which we focus on Infrared Dark Clouds (IRDCs) and young massive clusters. We present Very Large Array spectral line observations of ammonia (NH 3) and CCS toward four IRDCs. The NH3 lines provide diagnostics of the temperature and density structure within IRDCs. Based upon the NH 3 column density, IRDCs have masses of ˜ 103 to 10 4 M⊙ . We detect twenty NH3 clumps within four IRDCs, with radii regions are presented from the Near Infrared Imager (NIRIM) camera on the 3.5 m WIYN telescope. We report J, H, and K' band photometry in the clusters AFGL437, AFGL5180, and AFGL5142 and use these results to probe the stellar populations, extinction, and ages of the clusters. We find that all three clusters suffer significant extinction (AK ˜1), have ages ≤ 5 Myr, and are actively forming stars. We conclude that the properties of these embedded clusters are consistent with their evolving from IRDC clumps.

  16. Adaptive municipal electronic forms

    NARCIS (Netherlands)

    Kuiper, Pieter; Dijk, van Betsy; Bondarouk, Tanya; Ruël, Huub; Guiderdoni-Jourdain, Karine; Oiry, Ewan

    2009-01-01

    Adaptation of electronic forms (e-forms) seems to be a step forward to reduce the burden for people who fill in forms. Municipalities more and more offer e-forms online that can be used by citizens to request a municipal product or service or by municipal employees to place a request on behalf of a

  17. Manufacturing processes 4 forming

    CERN Document Server

    Klocke, Fritz

    2013-01-01

    This book provides essential information on metal forming, utilizing a practical distinction between bulk and sheet metal forming. In the field of bulk forming, it examines processes of cold, warm and hot bulk forming, as well as rolling and a new addition, the process of thixoforming. As for the field of sheet metal working, on the one hand it deals with sheet metal forming processes (deep drawing, flange forming, stretch drawing, metal spinning and bending). In terms of special processes, the chapters on internal high-pressure forming and high rate forming have been revised and refined. On the other, the book elucidates and presents the state of the art in sheet metal separation processes (shearing and fineblanking). Furthermore, joining by forming has been added to the new edition as a new chapter describing mechanical methods for joining sheet metals. The new chapter “Basic Principles” addresses both sheet metal and bulk forming, in addition to metal physics, plastomechanics and computational basics; ...

  18. NC INCREMENTAL SHEET METAL FORMING PROCESS AND VERTICAL WALL SQUARE BOX FORMING

    Institute of Scientific and Technical Information of China (English)

    Zhou Liuru; Mo Jianhua; Xiao Xiangzhi

    2004-01-01

    The forming principle and deformation analysis of NC incremental sheet metal forming process as well as the process planning, experiment and key process parameters of vertical wall square box forming are presented. Because the deformation of sheet metal only occurs around the tool head and the deformed region is subjected to stretch deformation, the deformed region of sheet metal thins, and surface area increases. Sheet metal forming stepwise is to lead to the whole sheet metal deformation. The forming half-apex angle θ and corner radius R are the main process parameters in NC incremental forming of vertical wall square box. According to sine law, a vertical wall square box can't be formed by NC incremental sheet metal forming process in a single process, rather, it must be formed in multi processes. Thus, the parallel line type tool path process method is presented to form the vertical wall square box, and the experiment and analysis are made to verify it.

  19. The faintest star forming galaxies

    CERN Document Server

    Ranalli, P

    2003-01-01

    I briefly report on the X-ray detection of 10 radio sub-mJy sources in the 2 Ms Chandra observation of the Hubble Deep Field North region. These sources follow the same radio/X-ray luminosities relation which holds for nearby galaxies. Making use of this relation, X-ray number counts from star forming galaxies are predicted from the deep radio Log N-Log S's.

  20. Maass Forms and Quantum Modular Forms

    Science.gov (United States)

    Rolen, Larry

    This thesis describes several new results in the theory of harmonic Maass forms and related objects. Maass forms have recently led to a flood of applications throughout number theory and combinatorics in recent years, especially following their development by the work of Bruinier and Funke the modern understanding Ramanujan's mock theta functions due to Zwegers. The first of three main theorems discussed in this thesis concerns the integrality properties of singular moduli. These are well-known to be algebraic integers, and they play a beautiful role in complex multiplication and explicit class field theory for imaginary quadratic fields. One can also study "singular moduli" for special non-holomorphic functions, which are algebraic but are not necessarily algebraic integers. Here we will explain the phenomenon of integrality properties and provide a sharp bound on denominators of symmetric functions in singular moduli. The second main theme of the thesis concerns Zagier's recent definition of a quantum modular form. Since their definition in 2010 by Zagier, quantum modular forms have been connected to numerous different topics such as strongly unimodal sequences, ranks, cranks, and asymptotics for mock theta functions. Motivated by Zagier's example of the quantum modularity of Kontsevich's "strange" function F(q), we revisit work of Andrews, Jimenez-Urroz, and Ono to construct a natural vector-valued quantum modular form whose components. The final chapter of this thesis is devoted to a study of asymptotics of mock theta functions near roots of unity. In his famous deathbed letter, Ramanujan introduced the notion of a mock theta function, and he offered some alleged examples. The theory of mock theta functions has been brought to fruition using the framework of harmonic Maass forms, thanks to Zwegers. Despite this understanding, little attention has been given to Ramanujan's original definition. Here we prove that Ramanujan's examples do indeed satisfy his