Neutron Stars and Black Holes New clues from Chandra and XMM-Newton

CERN Multimedia

CERN. Geneva. Audiovisual Unit

2002-01-01

Neutron stars and black holes, the most compact astrophysical objects, have become observable in many different ways during the last few decades. We will first review the phenomenology and properties of neutron stars and black holes (stellar and supermassive) as derived from multiwavelength observatories. Recently much progress has been made by means of the new powerful X-ray observatories Chandra and XMM-Newton which provide a substantial increase in sensitivity as well as spectral and angular resolution compared with previous satellites like ROSAT and ASCA. We shall discuss in more detail two recent topics: (1) The attempts to use X-ray spectroscopy for measuring the radii of neutron stars which depend on the equation of state at supranuclear densities. Have quark stars been detected? (2) The diagnostics of the strong gravity regions around supermassive black holes using X-ray spectroscopy.

A SEARCH FOR HYPERLUMINOUS X-RAY SOURCES IN THE XMM-NEWTON SOURCE CATALOG

Energy Technology Data Exchange (ETDEWEB)

Zolotukhin, I.; Webb, N. A.; Godet, O.; Barret, D. [CNRS, IRAP, 9 av. Colonel Roche, BP 44346, F-31028 Toulouse cedex 4 (France); Bachetti, M., E-mail: ivan.zolotukhin@irap.omp.eu [INAF/Osservatorio Astronomico di Cagliari, via della Scienza 5, I-09047 Selargius (Italy)

2016-02-01

We present a new method to identify luminous off-nuclear X-ray sources in the outskirts of galaxies from large public redshift surveys, distinguishing them from foreground and background interlopers. Using the 3XMM-DR5 catalog of X-ray sources and the SDSS DR12 spectroscopic sample of galaxies, with the help of this off-nuclear cross-matching technique, we selected 98 sources with inferred X-ray luminosities in the range 10{sup 41} < L{sub X} < 10{sup 44} erg s{sup −1}, compatible with hyperluminous X-ray objects (HLX). To validate the method, we verify that it allowed us to recover known HLX candidates such as ESO 243–49 HLX–1 and M82 X–1. From a statistical study, we conservatively estimate that up to 71 ± 11 of these sources may be foreground- or background sources, statistically leaving at least 16 that are likely to be HLXs, thus providing support for the existence of the HLX population. We identify two good HLX candidates and using other publicly available data sets, in particular the VLA FIRST in radio, UKIRT Infrared Deep Sky Survey in the near-infrared, GALEX in the ultraviolet and Canada–France–Hawaii Telescope Megacam archive in the optical, we present evidence that these objects are unlikely to be foreground or background X-ray objects of conventional types, e.g., active galactic nuclei, BL Lac objects, Galactic X-ray binaries, or nearby stars. However, additional dedicated X-ray and optical observations are needed to confirm their association with the assumed host galaxies and thus secure their HLX classification.

Il fenomeno abachistico a supporto dei cambiamenti socio-economici: Arezzo tra il XIII ed il XVI secolo = The role of the abacus tradition for the economic and social development of the society: evidence from Tuscany (Italy between XIII and XVI century

Directory of Open Access Journals (Sweden)

Maria Pia Maraghini

2011-12-01

Full Text Available Este artículo indaga sobre los orígenes de la contabilidad con el objetivo de analizar el comportamiento económico. En particular, se examinan los primeros lugares específica-mente dispuestos y organizados para la enseñanza del conocimiento contable así como los medios de estudio para su transmisión: las escuelas y los libros de ábaco. Ampliamente extendidos en Italia entre los siglos XIII y XVI tenían la finalidad de transmitir, por un lado, el conocimiento generalmente difundido como matemática práctica y, por otro, las técnicas para realizar operaciones aritméticas y las reglas prácticas para la resolución de problemas comerciales y financieros.El objetivo de esta investigación es profundizar en el estudio de las escuelas y de los libros de ábaco evidenciando el papel desempeñado en el origen de la contabilidad y en el desarrollo económico y social en la época medieval y los primeros siglos del Renacimiento.Con este fin, el estudio se basa en algunas evidencias sobre la evolución de los estudios y las escuelas de ábaco en Arezzo (Toscana, Italia entre los siglos XIII y XVI. Combinando evidencias similares con el análisis teórico el estudio revela la contribución de la tradición del ábaco en el mejor desarrollo de la vida pública en época medieval y renacentista. La constatación de esta contribución ha sido la base del creciente interés mostrado hacia la cultura del ábaco por las autoridades locales de la época.This paper focuses on the “origins” of the book-keeping art which aims to record economic behaviour. In particular, this research investigates the early specific “places” arranged and organized to teach the accounting knowledge and the primitive “means” of study with which it could be handed over: the abacus schools and books. They prevalently spread in Italy between XIII and XVI century with the aim of transferring the knowledge generally defined as “practical maths”, such as the

Quiet but still bright: XMM-Newton observations of the soft gamma-ray repeater SGR 0526-66

International Nuclear Information System (INIS)

Tiengo, A.; Esposito, P.; Mereghetti, S.; Esposito, P.; Israel, G.L.; Stella, L.; Turolla, R.; Turolla, R.; Zane, S.; Rea, N.; Gotz, D.; Feroci, M.

2009-01-01

SGR 0526-66 was the first soft gamma-ray repeater from which a giant flare was detected in 1979 March, suggesting the existence of magnetars, i.e. neutron stars powered by the decay of their extremely strong magnetic field. Since then, very little information has been obtained on this object, mainly because it has been burst inactive since 1983 and the study of its persistent X-ray emission has been hampered by its large distance and its location in a X-ray bright supernova remnant in the Large Magellanic Cloud. Here, we report on a comprehensive analysis of all the available XMM-Newton observations of SGR 0526-66. In particular, thanks to a deep observation taken in 2007, we measured its pulsation period (P = 8.0544 ± 0.0002 s) 6 years after its latest detection by Chandra. This allowed us to detect for the first time a significant reduction of its spin-down rate. From a comparison with two shorter XMM-Newton observations performed in 2000 and 2001, we found no significant changes in the spectrum, which is well modelled by an absorbed power law with nH = 4.6E+21 cm -2 and photon index = 3.27. The high luminosity about 4E+35 erg/s, in the 1-10 keV energy band) still observed about 25 years after the latest detection of bursting activity places SGR 0526-66 in the group of bright and persistent magnetar candidates. (authors)

Gestión odontológica en los niveles de la educación básica regular en la UGEL 01 Papa León XIII - Chilca, 2015

OpenAIRE

Cornejo Serna, Manuel Elias

2016-01-01

El objetivo del presente trabajo de investigación es determinar nivel de percepción de la gestión odontológica en los niveles de la educación básica regular, en la UGEL 01, Papa León XIII - Chilca, 2015. El tipo de investigación es descriptiva y comparativa su diseño de la investigación fue de tipo no experimental de corte transversal. La población estuvo conformada por los padres de familia de la institución educativa de Papa León XIII de los niveles de educación básica reg...

Finding X-ray counterparts for unidentified sources in the 105 months BAT survey - 2

Science.gov (United States)

Stephen, J. B.; Bassani, L.; Malizia, A.; Masetti, N.; Ubertini, P.

2018-02-01

We provide X-ray counterparts for unidentified Swift/BAT sources in the 105 month catalogue (Oh et al. 2018, ApJS in press). They were found by cross-correlating the list of U1,U2 and U3 sources with the ROSAT Bright (RASSBSC, Voges et al. 1999, A & A, 349, 389) and XMM-Newton Slew (XMMSlew, Saxton et al. 2008, A & A, 480, 611) catalogues and optically identified as reported in Atel #11340.

A cluster in a crowded environment: XMM-Newton and Chandra observations of A3558

Science.gov (United States)

Rossetti, M.; Ghizzardi, S.; Molendi, S.; Finoguenov, A.

2007-03-01

Combining XMM-Newton and Chandra data, we have performed a detailed study of Abell 3558. Our analysis shows that its dynamical history is more complicated than previously thought. We have found some traits typical of cool core clusters (surface brightness peaked at the center, peaked metal abundance profile) and others that are more common in merging clusters, like deviations from spherical symmetry in the thermodynamic quantities of the ICM. This last result has been achieved with a new technique for deriving temperature maps from images. We have also detected a cold front and, with the combined use of XMM-Newton and Chandra, we have characterized its properties, such as the speed and the metal abundance profile across the edge. This cold front is probably due to the sloshing of the core, induced by the perturbation of the gravitational potential associated with a past merger. The hydrodynamic processes related to this perturbation have presumably produced a tail of lower entropy, higher pressure and metal rich ICM, which extends behind the cold front for~500 kpc. The unique characteristics of A3558 are probably due to the very peculiar environment in which it is located: the core of the Shapley supercluster. Appendices A and B are only available in electronic form at http://www.aanda.org

THE HETDEX PILOT SURVEY. I. SURVEY DESIGN, PERFORMANCE, AND CATALOG OF EMISSION-LINE GALAXIES

International Nuclear Information System (INIS)

Adams, Joshua J.; Blanc, Guillermo A.; Gebhardt, Karl; Hao, Lei; Byun, Joyce; Fry, Alex; Jeong, Donghui; Komatsu, Eiichiro; Hill, Gary J.; Cornell, Mark E.; MacQueen, Phillip J.; Drory, Niv; Bender, Ralf; Hopp, Ulrich; Kelzenberg, Ralf; Ciardullo, Robin; Gronwall, Caryl; Finkelstein, Steven L.; Gawiser, Eric; Kelz, Andreas

2011-01-01

We present a catalog of emission-line galaxies selected solely by their emission-line fluxes using a wide-field integral field spectrograph. This work is partially motivated as a pilot survey for the upcoming Hobby-Eberly Telescope Dark Energy Experiment. We describe the observations, reductions, detections, redshift classifications, line fluxes, and counterpart information for 397 emission-line galaxies detected over 169 □' with a 3500-5800 A bandpass under 5 A full-width-half-maximum (FWHM) spectral resolution. The survey's best sensitivity for unresolved objects under photometric conditions is between 4 and 20x 10 -17 erg s -1 cm -2 depending on the wavelength, and Lyα luminosities between 3 x 10 42 and 6 x 10 42 erg s -1 are detectable. This survey method complements narrowband and color-selection techniques in the search of high-redshift galaxies with its different selection properties and large volume probed. The four survey fields within the COSMOS, GOODS-N, MUNICS, and XMM-LSS areas are rich with existing, complementary data. We find 105 galaxies via their high-redshift Lyα emission at 1.9 44 □' which appear to be extended Lyα nebulae. We also find three high-z objects with rest-frame Lyα EW above the level believed to be achievable with normal star formation, EW 0 >240 A. Future papers will investigate the physical properties of this sample.

XMM-Newton Spectroscopy of the Accretion-driven Millisecond X-Ray Pulsar XTE J1751-305 in Outburst

NARCIS (Netherlands)

Miller, J. M.; Wijnands, R.; Méndez, M.; Kendziorra, E.; Tiengo, A.; van der Klis, M.; Chakrabarty, D.; Gaensler, B. M.; Lewin, W. H. G.

2003-01-01

We present an analysis of the first high-resolution spectra measured from an accretion-driven millisecond X-ray pulsar in outburst. We observed XTE J1751-305 with XMM-Newton on 2002 April 7 for approximately 35 ks. Using a simple absorbed blackbody plus power-law model, we measure an unabsorbed flux

NuSTAR and XMM-Newton observations of NGC 1365: Extreme absorption variability and a constant inner accretion disk

DEFF Research Database (Denmark)

Walton, D. J.; Risaliti, G.; Harrison, F. A.

2014-01-01

We present a spectral analysis of four coordinated NuSTAR+XMM-Newton observations of the Seyfert galaxy NGC 1365. These exhibit an extreme level of spectral variability, which is primarily due to variable line-of-sight absorption, revealing relatively unobscured states in this source for the first...

XMM-Newton X-ray Observatory Guest Observer program (AO-1) at CASA

Science.gov (United States)

Skinner, Stephen L.

2003-01-01

In this research program, we obtained and analyzed X-ray observations of the Wolf-Rayet (WR) star WR 110 (HD 165688) using the XMM-Newton space-based observatory. Radio observations were also obtained using the Very Large Array (VLA) radio telescope located in New Mexico and operated by the Natl. Radio Astronomy Observatory (NRAO). This star was targeted for observations primarily because it is believed to be a single WR star without a companion. Single WR stars are thought to emit X-rays from cool plasma in shocks distributed throughout their powerful stellar winds. However, there has been little observational work done to test this idea since single WR stars are relatively weak X-ray sources and have been difficult to detect with previous generation telescopes. The launch of XMM-Newton provides a new telescope that is much more sensitive than its predecessors, allowing single WR stars to be studied in detail for the first time. X-ray emission was clearly detected from WR 110. Analysis of its spectrum yields a surprising result. Its X-ray emitting plasma is distributed over a range of temperatures and is dominated by relatively cool plasma with a characteristic temperature T is approximately 6 million K. Such plasma can be explained by existing theoretical wind shock models. However, the spectrum also shows hotter plasma whose temperature is uncertain but is thought to be in excess of T approximately 30 million K. The origin of this hotter plasma is yet unknown, but possible mechanisms are identified

The Broadband XMM-Newton and NuSTAR X-ray Spectra of Two Ultraluminous X-ray Sources in the Galaxy IC 342

DEFF Research Database (Denmark)

Rana, Vikram; Harrison, Fiona A.; Bachetti, Matteo

2015-01-01

We present results for two Ultraluminous X-ray Sources (ULXs), IC 342 X-1 and IC 342 X-2, using two epochs of XMM-Newton and NuSTAR observations separated by ∼7 days. We observe little spectral or flux variability above 1 keV between epochs, with unabsorbed 0.3-30 keV luminosities being $1.04+0.0...

Deep Extragalactic VIsible Legacy Survey (DEVILS): Motivation, Design and Target Catalogue

Science.gov (United States)

Davies, L. J. M.; Robotham, A. S. G.; Driver, S. P.; Lagos, C. P.; Cortese, L.; Mannering, E.; Foster, C.; Lidman, C.; Hashemizadeh, A.; Koushan, S.; O'Toole, S.; Baldry, I. K.; Bilicki, M.; Bland-Hawthorn, J.; Bremer, M. N.; Brown, M. J. I.; Bryant, J. J.; Catinella, B.; Croom, S. M.; Grootes, M. W.; Holwerda, B. W.; Jarvis, M. J.; Maddox, N.; Meyer, M.; Moffett, A. J.; Phillipps, S.; Taylor, E. N.; Windhorst, R. A.; Wolf, C.

2018-06-01

The Deep Extragalactic VIsible Legacy Survey (DEVILS) is a large spectroscopic campaign at the Anglo-Australian Telescope (AAT) aimed at bridging the near and distant Universe by producing the highest completeness survey of galaxies and groups at intermediate redshifts (0.3 < z < 1.0). Our sample consists of ˜60,000 galaxies to Y<21.2 mag, over ˜6 deg2 in three well-studied deep extragalactic fields (Cosmic Origins Survey field, COSMOS, Extended Chandra Deep Field South, ECDFS and the X-ray Multi-Mirror Mission Large-Scale Structure region, XMM-LSS - all Large Synoptic Survey Telescope deep-drill fields). This paper presents the broad experimental design of DEVILS. Our target sample has been selected from deep Visible and Infrared Survey Telescope for Astronomy (VISTA) Y-band imaging (VISTA Deep Extragalactic Observations, VIDEO and UltraVISTA), with photometry measured by PROFOUND. Photometric star/galaxy separation is done on the basis of NIR colours, and has been validated by visual inspection. To maximise our observing efficiency for faint targets we employ a redshift feedback strategy, which continually updates our target lists, feeding back the results from the previous night's observations. We also present an overview of the initial spectroscopic observations undertaken in late 2017 and early 2018.

Business plan for a national ''Hellas liberty'' ship memorial museum

OpenAIRE

Μόρφη, Ξανθή

2012-01-01

Το παρόν Επιχειρηματικό Σχέδιο επικεντρώνεται στο εγχείρημα της μετατροπής του πλοίου liberty με όνομα 'SS Arthur M. Huddell' (γνωστού ως Liberty Hellas) σε πλωτό μουσείο, το οποίο θα ονομαστεί Εθνικό Μουσείο Μνήμης Πλοίου Liberty. Στο επιχειρησιακό πλάνο περιλαμβάνονται τα ακόλουθα στοιχεία: αποστολή, βασικές αρχές, στρατηγικοί στόχοι, κόστος εκκίνησης, περιγραφή της επιχείρησης, σύντομη ιστορία των πλοίων liberty, ανάλυση επιχειρηματικού περιβάλλοντος, ανάλυση αγοράς, στρατηγική προώθησης, ...

XMM-Newton observation of the NLS1 galaxy Ark 564. I. Spectral analysis of the time-average spectrum

NARCIS (Netherlands)

Papadakis, I.E.; Brinkmann, W.; Page, M.J.; McHardy, I.; Uttley, P.

2007-01-01

Context: .We present the results from the spectral analysis of the time-average spectrum of the Narrow Line Seyfert 1 (NLS1) galaxy Ark 564 from a ~100 ks XMM-Newton observation. Aims: .Our aim is to characterize accurately the shape of the time-average, X-ray continuum spectrum of the source and

The cooling, mass and radius of the neutron star in EXO 0748-676 in quiescence with XMM-Newton

NARCIS (Netherlands)

Cheng, Zheng; Méndez, Mariano; Díaz-Trigo, María; Costantini, Elisa

2017-01-01

We analyse four XMM-Newton observations of the neutron-star low-mass X-ray binary EXO 0748-676 in quiescence. We fit the spectra with an absorbed neutron-star atmosphere model, without the need for a high-energy (power-law) component; with a 95 per cent confidence the power law contributes less than

Symbiotic Stars in X-rays. II. Faint Sources Detected with XMM-Newton and Chandra

Science.gov (United States)

Nunez, N. E.; Luna, G. J. M.; Pillitteri, I.; Mukai, K.

2014-01-01

We report the detection from four symbiotic stars that were not known to be X-ray sources. These four object show a ß-type X-ray spectrum, that is, their spectra can be modeled with an absorbed optically thin thermal emission with temperatures of a few million degrees. Photometric series obtained with the Optical Monitor on board XMM-Newton from V2416 Sgr and NSV 25735 support the proposed scenario where the X-ray emission is produced in a shock-heated region inside the symbiotic nebulae.

El consulado genovés de Sevilla (siglos XIII-XV. Aspectos jurisdiccionales, comerciales y fiscales

Directory of Open Access Journals (Sweden)

José Damián GONZÁLEZ ARCE

2011-02-01

Full Text Available El presente artículo analiza el funcionamiento del consulado genovés de Sevilla, entre los siglos XIII y XV, a partir de los privilegios concedidos por los reyes castellanos y otros documentos donde se contienen noticias sobre la actividad de estos italianos. En primer lugar, se estudian las competencias jurisdiccionales de dicho consulado y las facultades judiciales de sus cónsules. Luego son descritas las actividades mercantiles de la colonia ligur en el marco del consulado, así como otros aspectos ligados al comercio, como seguros y transportes. Y, finalmente, las exacciones fiscales a las que fueron sometidas esta colonia y las mercancías con las que traficó.

Swift , XMM - Newton , and NuSTAR Observations of PSR J2032+4127/MT91 213

Energy Technology Data Exchange (ETDEWEB)

Li, K. L. [Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 (United States); Kong, A. K. H. [Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH (United Kingdom); Tam, P. H. T. [School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082 (China); Hou, X. [Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming 650216 (China); Takata, J. [Institute of Particle Physics and Astronomy, Huazhong University of Science and Technology (China); Hui, C. Y., E-mail: liliray@pa.msu.edu [Department of Astronomy and Space Science, Chungnam National University, Daejeon (Korea, Republic of)

2017-07-10

We report our recent Swift , NuSTAR , and XMM - Newton X-ray and Lijiang optical observations on PSR J2032+4127/MT91 213, the γ -ray binary candidate with a period of 45–50 years. The coming periastron of the system was predicted to be in 2017 November, around which high-energy flares from keV to TeV are expected. Recent studies with Chandra and Swift X-ray observations taken in 2015/2016 showed that its X-ray emission has been brighter by a factors of ∼10 than that before 2013, probably revealing some ongoing activities between the pulsar wind and the stellar wind. Our new Swift /XRT lightcurve shows no strong evidence of a single vigorous brightening trend, but rather several strong X-ray flares on weekly to monthly timescales with a slowly brightening baseline, namely the low state. The NuSTAR and XMM - Newton observations taken during the flaring and the low states, respectively, show a denser environment and a softer power-law index during the flaring state, implying that the pulsar wind interacted with the stronger stellar winds of the companion to produce the flares. These precursors would be crucial in studying the predicted giant outburst from this extreme γ -ray binary during the periastron passage in late 2017.

Of decentralization of public power Ukrainian land that belonged to Lithuanian (XIII – the early XVII century

Directory of Open Access Journals (Sweden)

C. V. Manuilova

2016-06-01

Full Text Available A comprehensive crisis in Ukraine and continued military confrontation in the Donbass demonstrated the urgent need to establish effective governance, which would imply decentralization of public power. Note that in implementing the decentralization of power in Ukraine insists the International Monetary Fund; United Nations Development Program; the transfer of authority to the field and decentralization of power in Ukraine is one of the points of the Minsk agreements and obligations of Ukraine to the EU. The article deals with the Ukrainian lands topical issue features the decentralization of public power in the XIII - the beginning of XVII century. The importance of the topic due to the need to study the historical experience of the implementation of decentralization. It was, emphasized that the success of the reforms depends largely because of the historical experience and features of the decentralization of public power in the past. Characterized by the development of local government in the Ukrainian lands was part of the Lithuanian state. The purpose of the article is to clarify the characteristics of decentralization of public authority on Ukrainian lands were part of the Lithuanian state during the XVII century XIII. To address this goal, outline decentralization of public power in the state; analyze, competence of local government in the Ukrainian lands that belonged to the Lith uanian State; determine how close to the power of the people. The level of decentralization of public power in the Grand Duchy of Lithuania in the XIII - the beginning of XVII century was high. It was, found that Lithuania had not established a centralized state. It is, noted that the Board of the nobility limited the princely power. The effect of delegated deputies from different parts of the Lithuanian statehood solutions nobility Council.Clarified the facts that confirm the existence of decentralization of public power in Lithuania: the functioning of local

PIXE and IL analysis of an archeologically problematic XIII century ceramic production

Energy Technology Data Exchange (ETDEWEB)

Zucchiatti, Alessandro, E-mail: alessandro.zucchiatti@uam.es [Centro de Micro-Análisis de Materiales, Universidad Autónoma de Madrid, C/Faraday 3, Madrid (Spain); Jiménez-Rey, David [Centro de Micro-Análisis de Materiales, Universidad Autónoma de Madrid, C/Faraday 3, Madrid (Spain); Laboratorio Nacional de Fusión CIEMAT, E06.P2.09, Madrid (Spain); Climent-Font, Aurelio [Centro de Micro-Análisis de Materiales, Universidad Autónoma de Madrid, C/Faraday 3, Madrid (Spain); Departamento di Física Aplicada, Universidad Autónoma de Madrid, Madrid (Spain); Martina, Silvia [Centro de Micro-Análisis de Materiales, Universidad Autónoma de Madrid, C/Faraday 3, Madrid (Spain); Universitá degli Studi di Torino, Turin (Italy); Faieta, Rosangela [Centro de Micro-Análisis de Materiales, Universidad Autónoma de Madrid, C/Faraday 3, Madrid (Spain); Universitá della Tuscia, Viterbo (Italy); Maggi, Marco [Musei Vaticani, Ufficio del Conservatore, Rome (Italy); Giuntini, Lorenzo; Calusi, Silvia [INFN – Laboratorio di tecniche Nucleari per i Beni Culturali, Florence (Italy)

2015-11-15

At the beginning of the XIII century the archaeologists have found evidence of a singular, transitional, pottery technique limited to a small area around western Liguria (Northwest of Italy). Known as Ligurian Protomajolica (PML), it shows in the same ceramic body and on the same surface white slip and enamel together, addressing questions about the technical reasons of this unusual combination, its origin and evolution. To integrate previous morphological and mineralogical studies, we have analysed by particle induced X-ray emission (also with mapping) and ionoluminescence (IL) the ceramic body, slip and glaze composition of 56 samples, of which 25 PML’s. We have identified some PML’s compositional features which are distinct from those of other coeval or later productions from the same area. A few PML imitations are described. A plausible explanation of the origin of the PML’s, based both on the archaeometric results and the archaeological and historical knowledge, is presented.

Constraints on decaying Dark Matter from XMM-Newton observations of M31

CERN Document Server

Boyarsky, Alexey; Ruchayskiy, Oleg; Savchenko, Vladimir

2007-01-01

We derive constraints on parameters of the radiatively decaying Dark Matter (DM) particles, using XMM-Newton EPIC spectra of the Andromeda galaxy (M31). Using the observations of the outer (5'-13') parts of M31 we improve the existing constraints. For the case of sterile neutrino DM, combining our constraints with the latest computation of abundances of sterile neutrino in the Dodelson-Widrow (DW) scenario, we obtain the lower mass limit m_s 5.6 kev), we argue that the scenario in which all the DM is produced via DW mechanism is ruled out. We discuss however other production mechanisms and note that the sterile neutrino remains a viable candidate of Dark Matter, either warm or cold.

A NuSTAR survey of nearby ultraluminous infrared galaxies

DEFF Research Database (Denmark)

Teng, Stacy H.; Rigby, Jane R.; Stern, Daniel

2015-01-01

We present a Nuclear Spectroscopic Telescope Array (NuSTAR), Chandra, and XMM-Newton survey of nine of the nearest ultraluminous infrared galaxies (ULIRGs). The unprecedented sensitivity of NuSTAR at energies above 10 keV enables spectral modeling with far better precision than was previously......] line luminosity than do Seyfert 1 galaxies. We identify IRAS 08572+3915 as another candidate intrinsically X-ray weak source, similar to Mrk 231. We speculate that the X-ray weakness of IRAS 08572+3915 is related to its powerful outflow observed at other wavelengths....

The NuSTAR Extragalactic Surveys: Initial Results and Catalog from the Extended Chandra Deep Field South

DEFF Research Database (Denmark)

Mullaney, J. R.; Del-Moro, A.; Aird, J.

2015-01-01

We present the initial results and the source catalog from the Nuclear Spectroscopic Telescope Array (NuSTAR) survey of the Extended Chandra Deep Field South (hereafter, ECDFS)—currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full ≈30......V fluxes) span the range L10 40 keV (0.7 300) 10 erg s» - ´ 43 1 -- ,sampling below the “knee” of the X-ray luminosity function out to z ~ 0.8-1. Finally, we identify oneNuSTAR source that has neither a Chandra nor an XMM-Newton counterpart, but that shows evidence of nuclearactivity at infrared...

New Gener. High-Energy Spectra of the Blazar 3C 279 with XMM-Newton and GLAST

Science.gov (United States)

Collmar, Werner

2007-10-01

We propose two 20 ksec XMM-Newton observations of the X-ray bright gamma-ray blazar 3C~279 simultaneous with GLAST/LAT. The main goal is to measure its X-ray properties (spectrum, variability) in order to (1) improve our knowledge on the X-ray emission of the blazar, and (2) to supplement and correlate them to simultaneous GLAST/LAT Gamma-ray observations (30 MeV-300 GeV). Simultaneous GLAST observations of 3C 279 are guaranteed (assuming proper operation then). The high-energy data will be supplemented by ground-based measurements, adding finally up to multifrequency spectra which have unprecedented accuracy and will extend up to high-energy gamma-rays. Such high-quality SEDs will provide severe constraints on their modeling and have the potential to discriminate among models.

Acquired Factor Xiii Deficiency: An Uncommon But Easily Missed Cause Of Severe Bleeding

LENUS (Irish Health Repository)

Fogarty, H

2018-05-01

Factor XIII (FXIII) is a plasma clotting protein involved in clot stabilization. Severe FXIII deficiency may present with severe, even fatal bleeding. Critically however, routine coagulation assays may be normal and only specific FXIII assays will detect the abnormality. Herein we discuss a case report of a patient with acquired FXIII deficiency in order to highlight the clinical challenges associated with establishing the diagnosis and discuss the treatment approach. A 70-year-old man presented with a gluteal haematoma despite no preceding personal history of bleeding. Extensive initial haemostatic investigations were normal until a specific FXIII assay showed a marked reduction in FXIII levels. With directed treatment, bleeding episodes ceased and remission was achieved. Clinical awareness of FXIII deficiency is important, so appropriate testing can be implemented in patients with unexplained bleeding diatheses, particularly those in whom bleeding responds poorly to standard replacement therapy.

The soft-X-ray emission of Ark 120. XMM-Newton, NuSTAR, and the importance of taking the broad view

DEFF Research Database (Denmark)

Matt, G.; Marinucci, A.; Guainazzi, M.

2014-01-01

We present simultaneous XMM-Newton and NuSTAR observations of the 'bare' Seyfert 1 galaxy, Ark 120, a system in which ionized absorption is absent. The NuSTAR hard-X-ray spectral coverage allows us to constrain different models for the excess soft-X-ray emission. Among phenomenological models, a ...

Multi-wavelength study of the Seyfert 1 galaxy NGC 3783 with XMM-Newton

CERN Document Server

Blustin, A J; Behar, E; Kaastra, J S; Kahn, S M; Page, M J; Sako, M; Steenbrugge, K C

2002-01-01

We present the analysis of multi-wavelength XMM-Newton data from the Seyfert galaxy NGC 3783, including UV imaging, X-ray and UV lightcurves, the 0.2-10 keV X-ray continuum, the iron K-alpha emission line, and high-resolution spectroscopy and modelling of the soft X-ray warm absorber. The 0.2-10 keV spectral continuum can be well reproduced by a power-law at higher energies; we detect a prominent Fe K-alpha emission line, with both broad and narrow components, and a weaker emission line at 6.9 keV which is probably a combination of Fe K-beta and Fe XXVI. We interpret the significant deficit of counts in the soft X-ray region as being due to absorption by ionised gas in the line of sight. This is demonstrated by the large number of narrow absorption lines in the RGS spectrum from iron, oxygen, nitrogen, carbon, neon, argon, magnesium, silicon and sulphur. The wide range of iron states present in the spectrum enables us to deduce the ionisation structure of the absorbing medium. We find that our spectrum contai...

NuSTAR and XMM-Newton Observations of the 2015 Outburst Decay of GX 339-4

Energy Technology Data Exchange (ETDEWEB)

Stiele, H.; Kong, A. K. H., E-mail: hstiele@mx.nthu.edu.tw [National Tsing Hua University, Department of Physics and Institute of Astronomy, No. 101 Sect. 2 Kuang-Fu Road, 30013, Hsinchu, Taiwan (China)

2017-07-20

The extent of the accretion disk in the low/hard state of stellar mass black hole X-ray binaries remains an open question. There is some evidence suggesting that the inner accretion disk is truncated and replaced by a hot flow, while the detection of relativistic broadened iron emission lines seems to require an accretion disk extending fully to the innermost stable circular orbit. We present comprehensive spectral and timing analyses of six Nuclear Spectroscopic Telescope Array and XMM-Newton observations of GX 339–4 taken during outburst decay in the autumn of 2015. Using a spectral model consisting of a thermal accretion disk, Comptonized emission, and a relativistic reflection component, we obtain a decreasing photon index, consistent with an X-ray binary during outburst decay. Although we observe a discrepancy in the inner radius of the accretion disk and that of the reflector, which can be attributed to the different underlying assumptions in each model, both model components indicate a truncated accretion disk that resiles with decreasing luminosity. The evolution of the characteristic frequency in Fourier power spectra and their missing energy dependence support the interpretation of a truncated and evolving disk in the hard state. The XMM-Newton data set allowed us to study, for the first time, the evolution of the covariance spectra and ratio during outburst decay. The covariance ratio increases and steeps during outburst decay, consistent with increased disk instabilities.

X-Ray Temperatures, Luminosities, and Masses from XMM-Newton Follow-up of the First Shear-selected Galaxy Cluster Sample

Energy Technology Data Exchange (ETDEWEB)

Deshpande, Amruta J.; Hughes, John P. [Department of Physics and Astronomy, Rutgers the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854 (United States); Wittman, David, E-mail: amrejd@physics.rutgers.edu, E-mail: jph@physics.rutgers.edu, E-mail: dwittman@physics.ucdavis.edu [Department of Physics, University of California, Davis, One Shields Avenue, Davis, CA 95616 (United States)

2017-04-20

We continue the study of the first sample of shear-selected clusters from the initial 8.6 square degrees of the Deep Lens Survey (DLS); a sample with well-defined selection criteria corresponding to the highest ranked shear peaks in the survey area. We aim to characterize the weak lensing selection by examining the sample’s X-ray properties. There are multiple X-ray clusters associated with nearly all the shear peaks: 14 X-ray clusters corresponding to seven DLS shear peaks. An additional three X-ray clusters cannot be definitively associated with shear peaks, mainly due to large positional offsets between the X-ray centroid and the shear peak. Here we report on the XMM-Newton properties of the 17 X-ray clusters. The X-ray clusters display a wide range of luminosities and temperatures; the L {sub X} − T {sub X} relation we determine for the shear-associated X-ray clusters is consistent with X-ray cluster samples selected without regard to dynamical state, while it is inconsistent with self-similarity. For a subset of the sample, we measure X-ray masses using temperature as a proxy, and compare to weak lensing masses determined by the DLS team. The resulting mass comparison is consistent with equality. The X-ray and weak lensing masses show considerable intrinsic scatter (∼48%), which is consistent with X-ray selected samples when their X-ray and weak lensing masses are independently determined.

La expansión del posesivo pospuesto a la luz de documentación navarra (y aragonesa) del siglo XIII

OpenAIRE

Romero Cambrón, Angeles

2016-01-01

En los primitivos documentos romances el posesivo sólo aparece antepuesto al sustantivo (“(el) nuestro padre”). La posposición (“padre nuestro”) se empieza a registrar en el siglo XIII en aragonés y en dialecto navarro. Considerando principalmente la documentación de esta segunda variedad, el presente trabajo tiene como objetivo determinar el modo en que el posesivo adquirió la capacidad de aparecer pospuesto. Este cambio se vio impulsado por factores de naturaleza estructural. Uno de ellos e...

Clot retraction is mediated by factor XIII-dependent fibrin-αIIbβ3-myosin axis in platelet sphingomyelin-rich membrane rafts.

Science.gov (United States)

Kasahara, Kohji; Kaneda, Mizuho; Miki, Toshiaki; Iida, Kazuko; Sekino-Suzuki, Naoko; Kawashima, Ikuo; Suzuki, Hidenori; Shimonaka, Motoyuki; Arai, Morio; Ohno-Iwashita, Yoshiko; Kojima, Soichi; Abe, Mitsuhiro; Kobayashi, Toshihide; Okazaki, Toshiro; Souri, Masayoshi; Ichinose, Akitada; Yamamoto, Naomasa

2013-11-07

Membrane rafts are spatially and functionally heterogenous in the cell membrane. We observed that lysenin-positive sphingomyelin (SM)-rich rafts are identified histochemically in the central region of adhered platelets where fibrin and myosin are colocalized on activation by thrombin. The clot retraction of SM-depleted platelets from SM synthase knockout mouse was delayed significantly, suggesting that platelet SM-rich rafts are involved in clot retraction. We found that fibrin converted by thrombin translocated immediately in platelet detergent-resistant membrane (DRM) rafts but that from Glanzmann's thrombasthenic platelets failed. The fibrinogen γ-chain C-terminal (residues 144-411) fusion protein translocated to platelet DRM rafts on thrombin activation, but its mutant that was replaced by A398A399 at factor XIII crosslinking sites (Q398Q399) was inhibited. Furthermore, fibrin translocation to DRM rafts was impaired in factor XIII A subunit-deficient mouse platelets, which show impaired clot retraction. In the cytoplasm, myosin translocated concomitantly with fibrin translocation into the DRM raft of thrombin-stimulated platelets. Furthermore, the disruption of SM-rich rafts by methyl-β-cyclodextrin impaired myosin activation and clot retraction. Thus, we propose that clot retraction takes place in SM-rich rafts where a fibrin-αIIbβ3-myosin complex is formed as a primary axis to promote platelet contraction.

NUSTAR AND XMM-NEWTON OBSERVATIONS OF THE EXTREME ULTRALUMINOUS X-RAY SOURCE NGC 5907 ULX1: A VANISHING ACT

Energy Technology Data Exchange (ETDEWEB)

Walton, D. J.; Stern, D. [Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States); Harrison, F. A.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.; Rana, V. [Space Radiation Laboratory, California Institute of Technology, Pasadena, CA 91125 (United States); Bachetti, M.; Barret, D.; Webb, N. [Universite de Toulouse, UPS-OMP, IRAP, Toulouse (France); Boggs, S. E.; Craig, W. W. [Space Sciences Laboratory, University of California, Berkeley, CA 94720 (United States); Christensen, F. E. [DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby (Denmark); Hailey, C. J. [Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (United States); Middleton, M. J. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA (United Kingdom); Roberts, T. P.; Sutton, A. D. [Department of Physics, Durham University, South Road, Durham DH1 3LE (United Kingdom); Zhang, W. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States)

2015-02-01

We present results obtained from two broadband X-ray observations of the extreme ultraluminous X-ray source (ULX) NGC 5907 ULX1, known to have a peak X-ray luminosity of ∼5 × 10{sup 40} erg s{sup –1}. These XMM-Newton and NuSTAR observations, separated by only ∼4 days, revealed an extreme level of short-term flux variability. In the first epoch, NGC 5907 ULX1 was undetected by NuSTAR, and only weakly detected (if at all) with XMM-Newton, while in the second NGC 5907 ULX1 was clearly detected at high luminosity by both missions. This implies an increase in flux of ∼2 orders of magnitude or more during this ∼4 day window. We argue that this is likely due to a rapid rise in the mass accretion rate, rather than to a transition from an extremely obscured to an unobscured state. During the second epoch we observed the broadband 0.3-20.0 keV X-ray luminosity to be (1.55 ± 0.06) × 10{sup 40} erg s{sup –1}, similar to the majority of the archival X-ray observations. The broadband X-ray spectrum obtained from the second epoch is inconsistent with the low/hard accretion state observed in Galactic black hole binaries, but is well modeled with a simple accretion disk model incorporating the effects of photon advection. This strongly suggests that when bright, NGC 5907 ULX1 is a high-Eddington accretor.

A hard X-ray study of the ultraluminous X-ray source NGC 5204 X-1 with NuSTAR and XMM-Newton

DEFF Research Database (Denmark)

Mukherjee, E. S.; Walton, D. J.; Bachetti, M.

2015-01-01

We present the results from coordinated X-ray observations of the ultraluminous X-ray source NGC 5204 X-1 performed by the Nuclear Spectroscopic Telescope Array and XMM-Newton in early 2013. These observations provide the first detection of NGC 5204 X-1 above 10 keV, extending the broadband cover...

76 FR 67761 - Certain Light-Emitting Diodes and Products Containing Same Determination Not To Review an Initial...

Science.gov (United States)

2011-11-02

..., under section 337 of the Tariff Act of 1930, as amended, 19 U.S.C. 1337, on behalf of LG Electronics..., Germany, Hella Electronics Corp. of Plymouth Township, Michigan, Hella Corporate Center USA of Plymouth Township, Michigan, Hella, Inc. of Peachtree City, Georgia, (collectively, ``Hella''), Automotive Lighting...

Are QSO2 hiding among EROs?

OpenAIRE

Brusa, Marcella

2004-01-01

We present the results of a deep (80 ks) XMM-Newton survey of one of the largest sample of near-infrared selected Extremely Red Objects (R-K>5) available to date (~300 objects, Daddi et al. 2000). The fraction of individually detected, X-ray emitting EROs is of the order of ~3.5%, down to F_x > 4x10^-15 cgs and Ks

NUSTAR and Xmm-Newton Observations of the Extreme Ultraluminous X-Ray Source NGC 5907 UlX1: A Vanishing Act

DEFF Research Database (Denmark)

Walton, D. J.; Harrison, F. A.; Bachetti, M.

2015-01-01

We present results obtained from two broadband X-ray observations of the extreme ultraluminous X-ray source (ULX) NGC 5907 ULX1, known to have a peak X-ray luminosity of ~5 × 1040 erg s–1. These XMM-Newton and NuSTAR observations, separated by only ~4 days, revealed an extreme level of short-term...

EDITORIAL: XIII Mexican Workshop on Particles and Fields

Science.gov (United States)

Barranco, Juan; Contreras, Guillermo; Delepine, David; Napsuciale, Mauro

2012-08-01

Juan Barranco Physics Department, Guanajuato University, Loma del Bosque 103, col. Loma del Campestre, 37150, Leon (Mexico) jbarranc@fisica.ugto.mx Guillermo Contreras Departamento de Fisica Aplicada Centro de Investigacion y de Estudios Avanzados del Instituto Politecnico Nacional, Merida (Mexico) jgcn@mda.cinvestav.mx David Delepine Physics Department, Guanajuato University, Loma del Bosque 103, col. Loma del Campestre, 37150, Leon (Mexico) delepine@fisica.ugto.mx Mauro Napsuciale Physics Department, Guanajuato University, Loma del Bosque 103, col. Loma del Campestre, 37150, Leon (Mexico) mauro@fisica.ugto.mx The XIII Mexican Workshop on Particles and Fields (MWPF) took place from 20-26 October 2011, in the city of León, Guanajuato, México. This is a biennial meeting organized by the Division of Particles and Fields of the Mexican Physical Society designed to gather specialists in different areas of high energy physics to discuss the latest developments in the field. The thirteenth edition of this meeting was hosted by the Department of Cultural Studies of Guanajuato University in a nice environment dedicated to the Arts and Culture. The XIII MWPF was organized by three working groups who organized the corresponding sessions around three topics. The first one was Strings, Cosmology, Astroparticles and Physics Beyond the Standard Model. In this category we included: Cosmic Rays, Gamma Ray Bursts, Physics Beyond the Standard Model (theory and experimental searches), Strings and Cosmology. The working group for this topic was formed by Arnulfo Zepeda, Oscar Loaiza, Axel de la Macorra and Myriam Mondragón. The second topic was Hadronic Matter which included Perturbative QCD, Jets and Diffractive Physics, Hadronic Structure, Soft QCD, Hadron Spectroscopy, Heavy Ion Collisions and Soft Physics at Hadron Colliders, Lattice Results and Instrumentation. The working group for this topic was integrated by Wolfgang Bietenholz and Mariana Kirchbach. The third topic was

Phase-resolved XMM-Newton and swift observations of WR 25

Energy Technology Data Exchange (ETDEWEB)

Pandey, J. C.; Pandey, S. B.; Karmakar, Subhajeet, E-mail: jeewan@aries.res.in [Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital 263 002 (India)

2014-06-10

We present an analysis of long-term X-ray and optical observations of the Wolf-Rayet binary, WR 25. Using archival data from observations with the XMM-Newton and the Swift observatories, spanning over ∼10 yr, we show that WR 25 is a periodic variable in X-rays with a period of 208 ± 3 days. X-ray light curves in the 0.5-10.0 keV energy band show phase-locked variability, where the flux increased by a factor of ∼2 from minimum to maximum, being maximum near periastron passage. The light curve in the soft energy band (0.5-2.0 keV) shows two minima indicating the presence of two eclipses. However, the light curve in the hard energy band (2.0-10.0 keV) shows only one minimum during the apastron passage. The X-ray spectra of WR 25 were explained by a two-temperature plasma model. Both the cool and the hot plasmas were constant at 0.628 ± 0.008 and 2.75 ± 0.06 keV throughout an orbital cycle, where the cooler plasma could be due to small scale shocks in a radiation-driven outflow and the high temperature plasma could be due to the collision of winds. The column density varied with the orbital phase and was found to be maximum after the periastron passage, when the WN star is in front of the O star. The abundances of WR 25 were found to be non-solar. Optical V-band data of WR 25 also show the phase-locked variability, being at maximum near periastron passage. The results based on the present analysis indicate that WR 25 is a colliding wind binary where the presence of soft X-rays is attributed to individual components; however, hard X-rays are due to the collision of winds.

Comparative Analysis and Variability of the Jovian X-Ray Spectra Detected by the Chandra and XMM-Newton Observatories

Energy Technology Data Exchange (ETDEWEB)

Hui, Yawei [ORNL; Schultz, David Robert [ORNL; Kharchenko, Vasili A [ORNL; Bhardwaj, Anil [Vikram Sarabhai Space Center, Trivandrum, India; Branduardi-Raymont, Graziella [University College, London; Stancil, Phillip C. [University of Georgia, Athens, GA; Cravens, Thomas E. E. [University of Kansas; Lisse, Carey M. [Johns Hopkins University; Dalgarno, A. [Harvard-Smithsonian Center for Astrophysics

2010-01-01

Expanding upon recent work, a more comprehensive spectral model based on charge exchange induced X-ray emission by ions precipitating into the Jovian atmosphere is used to provide new understanding of the polar auroras. In conjunction with the Xspec spectral fitting software, the model is applied to analyze observations from both Chandra and XMM-Newton by systematically varying the initial precipitating ion parameters to obtain the best fit model for the observed spectra. In addition to the oxygen and sulfur ions considered previously, carbon is included to discriminate between solar wind and Jovian magnetospheric ion origins, enabled by the use of extensive databases of both atomic collision cross sections and radiative transitions. On the basis of fits to all the Chandra observations, we find that carbon contributes negligibly to the observed polar X-ray emission suggesting that the highly accelerated precipitating ions are of magnetospheric origin. Most of the XMM-Newton fits also favor this conclusion with one exception that implies a possible carbon contribution. Comparison among all the spectra from these two observatories in light of the inferred initial energies and relative abundances of precipitating ions from the modeling show that they are significantly variable in time (observation date) and space (north and south polar X-ray auroras).

XIII International science and technology conference High-tech chemical technologies-2010 with elements of Scientific school for young people Innovations in chemistry: achievements and prospects. Summaries of reports

International Nuclear Information System (INIS)

2010-01-01

Materials of the XIII International science and technology conference High-tech chemical technologies-2010 with elements of Scientific school for young people Innovations in chemistry: achievements and prospects (29 June-2 July 2010, Ivanovo) are presented. During the conference the following areas: theoretical aspects of chemical technology; technology of deep oil refining and the production of organic substances; technology of drugs and biologically active substances; technology of inorganic materials, polymers and composites based on them - the technological principles and methods of synthesis, modification, and processing; environmental and economic problems of chemical technologies and their solutions are considered [ru

XMM-Newton X-ray and HST weak gravitational lensing study of the extremely X-ray luminous galaxy cluster Cl J120958.9+495352 (z = 0.902)

Science.gov (United States)

Thölken, Sophia; Schrabback, Tim; Reiprich, Thomas H.; Lovisari, Lorenzo; Allen, Steven W.; Hoekstra, Henk; Applegate, Douglas; Buddendiek, Axel; Hicks, Amalia

2018-03-01

Context. Observations of relaxed, massive, and distant clusters can provide important tests of standard cosmological models, for example by using the gas mass fraction. To perform this test, the dynamical state of the cluster and its gas properties have to be investigated. X-ray analyses provide one of the best opportunities to access this information and to determine important properties such as temperature profiles, gas mass, and the total X-ray hydrostatic mass. For the last of these, weak gravitational lensing analyses are complementary independent probes that are essential in order to test whether X-ray masses could be biased. Aims: We study the very luminous, high redshift (z = 0.902) galaxy cluster Cl J120958.9+495352 using XMM-Newton data. We measure global cluster properties and study the temperature profile and the cooling time to investigate the dynamical status with respect to the presence of a cool core. We use Hubble Space Telescope (HST) weak lensing data to estimate its total mass and determine the gas mass fraction. Methods: We perform a spectral analysis using an XMM-Newton observation of 15 ks cleaned exposure time. As the treatment of the background is crucial, we use two different approaches to account for the background emission to verify our results. We account for point spread function effects and deproject our results to estimate the gas mass fraction of the cluster. We measure weak lensing galaxy shapes from mosaic HST imaging and select background galaxies photometrically in combination with imaging data from the William Herschel Telescope. Results: The X-ray luminosity of Cl J120958.9+495352 in the 0.1-2.4 keV band estimated from our XMM-Newton data is LX = (13.4+1.2-1.0) × 1044 erg/s and thus it is one of the most X-ray luminous clusters known at similarly high redshift. We find clear indications for the presence of a cool core from the temperature profile and the central cooling time, which is very rare at such high redshifts. Based

Del "scriptor" al "publicus notarius" : los escribanos de Madrid en el siglo XIII

Directory of Open Access Journals (Sweden)

María Teresa Carrasco Lazareno

2003-01-01

Full Text Available Estudio diplomático y jurídicoinstitucional de las escribanías de Madrid en el siglo XIII. Se analiza su evolución desde los primeros "Scriptores» prenotariales conocidos, clérigos y laicos de libre profesión, documentados hasta 1260, hasta la consolidación definitiva de la institución notarial y del instrumento público en el último cuarto del siglo XIII. Se estudian con detenimiento la compleja etapa de transición, en las décadas centrales de la centuria, la figura del «escrivano de congejo de Madrit», profesional estable y antecedente inmediato del escribano público, y la instauración del notariado, de acuerdo con la legislación alfonsina, así como de la escribanía municipal, por otorgamiento de Alfonso X, en 1264. A través de la documentación conservada, se analiza, asimismo, la transformación de la simple carta o «scriptura» testifical en «publicum instrumentum», mediante la valoración de la pervivencia de elementos tradicionales y la aparición de fórmulas diplomáticas que revelan la paulatina introducción.This is a diplomatic and a legal — institutional study about the actuarles offices in Madrid during the Xlllth century Its evolution is analyzed from the first known prenotarial "scriptores», priests and liberal professionals seculars, documented until 1260, until the final consolidation of the notary institution and the public instrument during the last quarter of the Xlllth century There is a detailed study about the complexity of the transitional period, during the central decades of that century, the figure of the «Notary of the Madrid Town Council», as a stable professional and immediate predecessor of the public actuary the establishment of the body of actuarles, according to the Alphonsine legislation, an the municipal actuary office, established by King Alphonse Xth., in 1264. Through the preserved documentation, it is analized, at the same time, the transformation of the simple letter, or

NuSTAR and XMM-Newton Observations of the Hard X-Ray Spectrum of Centaurus A

DEFF Research Database (Denmark)

Fürst, F.; Müller, C.; Madsen, K. K.

2016-01-01

with an absorbed power-law witha photon index Γ = 1.815 ± 0.005 and a fluorescent Fe Kα line in good agreement with literature values.The spectrum does not require a high-energy exponential rollover, with a constraint of Efold > 1 MeV. Athermal Comptonization continuum describes the data well, with parameters....... We use archival Chandra data to estimatethe contribution from diffuse emission, extra-nuclear point-sources, and the X-ray jet to the observed NuSTAR and XMM-Newton X-ray spectra and find the contribution to be negligible. We discuss different scenarios forthe physical origin of the observed X...

Chandra and XMM-Newton Observations of the Abell 3395/Abell 3391 Intercluster Filament

Science.gov (United States)

Alvarez, Gabriella E.; Randall, Scott W.; Bourdin, Hervé; Jones, Christine; Holley-Bockelmann, Kelly

2018-05-01

We present Chandra and XMM-Newton X-ray observations of the Abell 3391/Abell 3395 intercluster filament. It has been suggested that the galaxy clusters Abell 3395, Abell 3391, and the galaxy group ESO-161 -IG 006 located between the two clusters, are in alignment along a large-scale intercluster filament. We find that the filament is aligned close to the plane of the sky, in contrast to previous results. We find a global projected filament temperature kT = {4.45}-0.55+0.89 keV, electron density {n}e={1.08}-0.05+0.06× {10}-4 cm‑3, and {M}gas}={2.7}-0.1+0.2 × {10}13 M ⊙. The thermodynamic properties of the filament are consistent with that of the intracluster medium (ICM) of Abell 3395 and Abell 3391, suggesting that the filament emission is dominated by ICM gas that has been tidally disrupted during an early stage merger between these two clusters. We present temperature, density, entropy, and abundance profiles across the filament. We find that the galaxy group ESO-161 may be undergoing ram-pressure-stripping in the low-density environment at or near the virial radius of both clusters, due to its rapid motion through the filament.

Evaluating Factor XIII Specificity for Glutamine-Containing Substrates Using a MALDI-TOF Mass Spectrometry Assay

Science.gov (United States)

Doiphode, Prakash G.; Malovichko, Marina V.; Mouapi, Kelly Njine; Maurer, Muriel C.

2014-01-01

Activated Factor XIII (FXIIIa) catalyzes the formation of γ-glutamyl-ε-lysyl cross-links within the fibrin blood clot network. Although several cross-linking targets have been identified, the characteristic features that define FXIIIa substrate specificity are not well understood. To learn more about how FXIIIa selects its targets, a matrix-assisted laser desorption ionization – time of flight mass spectrometry (MALDI-TOF MS) based assay was developed that could directly follow the consumption of a glutamine-containing substrate and the formation of a cross-linked product with glycine ethylester. This FXIIIa kinetics assay is no longer reliant on a secondary coupled reaction, on substrate labeling, or on detecting the final deacylation portion of the transglutaminase reaction. With the MALDI-TOF MS assay, glutamine-containing peptides derived from α2-antiplasmin, S. Aureus fibronectin binding protein A, and thrombin activatable fibrinolysis inhibitor were examined directly. Results suggest that the FXIIIa active site surface responds to changes in substrate residues following the reactive glutamine. The P-1 substrate position is sensitive to charge character and the P-2 and P-3 to the broad FXIIIa substrate specificity pockets. The more distant P-8 to P-11 region serves as a secondary substrate anchoring point. New knowledge on FXIIIa specificity may be used to design better substrates or inhibitors of this transglutaminase. PMID:24751466

Planck 2013 results. XIII. Galactic CO emission

CERN Document Server

Ade, P.A.R.; Alves, M.I.R.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A.J.; Barreiro, R.B.; Bartlett, J.G.; Battaner, E.; Benabed, K.; Benoit, A.; Benoit-Levy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J.J.; Bonaldi, A.; Bond, J.R.; Borrill, J.; Bouchet, F.R.; Boulanger, F.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R.C.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, L. -Y; Chiang, H.C.; Christensen, P.R.; Church, S.; Clements, D.L.; Colombi, S.; Colombo, L.P.L.; Combet, C.; Couchot, F.; Coulais, A.; Crill, B.P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R.D.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Dempsey, J.T.; Desert, F. -X.; Dickinson, C.; Diego, J.M.; Dole, H.; Donzelli, S.; Dore, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enblin, T.A.; Eriksen, H.K.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.; Fukui, Y.; Galeotta, S.; Ganga, K.; Giard, M.; Giraud-Heraud, Y.; Gonzalez-Nuevo, J.; Gorski, K.M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Handa, T.; Hansen, F.K.; Hanson, D.; Harrison, D.; Henrot-Versille, S.; Hernandez-Monteagudo, C.; Herranz, D.; Hildebrandt, S.R.; Hily-Blant, P.; Hivon, E.; Hobson, M.; Holmes, W.A.; Hornstrup, A.; Hovest, W.; Huffenberger, K.M.; Hurier, G.; Jaffe, T.R.; Jaffe, A.H.; Jewell, J.; Jones, W.C.; Juvela, M.; Keihanen, E.; Keskitalo, R.; Kisner, T.S.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lahteenmaki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R.J.; Lawrence, C.R.; Leonardi, R.; Leon-Tavares, J.; Lesgourgues, J.; Liguori, M.; Lilje, P.B.; Linden-Vornle, M.; Lopez-Caniego, M.; Lubin, P.M.; Macias-Perez, J.F.; Maffei, B.; Mandolesi, N.; Maris, M.; Marshall, D.J.; Martin, P.G.; Martinez-Gonzalez, E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschenes, M. -A.; Moneti, A.; Montier, L.; Moore, T.J.T.; Morgante, G.; Morino, J.; Mortlock, D.; Munshi, D.; Nakajima, T.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C.B.; Norgaard-Nielsen, H.U.; Noviello, F.; Novikov, D.; Novikov, I.; Okuda, T.; Osborne, S.; Oxborrow, C.A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G.W.; Preezeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J.P.; Reach, W.T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson, M.; Rubino-Martin, J.A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M.D.; Shellard, E.P.S.; Spencer, L.D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J.A.; Tavagnacco, D.; Terenzi, L.; Thomas, H.S.; Toffolatti, L.; Tomasi, M.; Torii, K.; Tristram, M.; Tucci, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L.A.; Wandelt, B.D.; Wehus, I.K.; Yoda, H. Yamamoto T.; Yvon, D.; Zacchei, A.; Zonca, A.

2014-10-29

Rotational transition lines of CO play a major role in molecular radio astronomy and in particular in the study of star formation and the Galactic structure. Although a wealth of data exists in the Galactic plane and some well-known molecular clouds, there is no available CO high sensitivity all-sky survey to date. Such all-sky surveys can be constructed using the \\Planck\\ HFI data because the three lowest CO rotational transition lines at 115, 230 and 345 GHz significantly contribute to the signal of the 100, 217 and 353 GHz HFI channels respectively. Two different component separation methods are used to extract the CO maps from Planck HFI data. The maps obtained are then compared to one another and to existing external CO surveys. From these quality checks the best CO maps in terms of signal to noise and/or residual foreground contamination are selected. Three sets of velocity-integrated CO emission maps are produced: Type 1 maps of the CO (1-0), (2-1), and (3-2) rotational transitions with low foreground ...

An X-ray view of the very faint black hole X-ray transient Swift J1357.2-0933 during its 2011 outburst

NARCIS (Netherlands)

Armas Padilla, M.; Wijnands, R.; Altamirano, D.; Méndez, M.; Miller, J. M.; Degenaar, N.

We report on the X-ray spectral (using XMM-Newton data) and timing behaviour [using XMM-Newton and Rossi X-ray Timing Explorer (RXTE) data] of the very faint X-ray transient and black hole system Swift J1357.2-0933 during its 2011 outburst. The XMM-Newton X-ray spectrum of this source can be

La formazione di un’aristocrazia: monache e monasteri femminili a Venezia tra IX e XIII secolo

Directory of Open Access Journals (Sweden)

Rapetti, Anna

2014-06-01

Full Text Available This paper examines the processes that shaped the identity of the Venetian aristocracy from the 9th to the 13th centuries and the role played by the relationship between patrician families and some female monasteries. The important female monastery of San Zaccaria and some other nunneries created in the lagoon between the 12th and the 13th centuries are taken into account in the analysis of the formation of Venetian aristocracy from this innovative perspective. By analysing the behaviour of the aristocratic families towards these nunneries, the paper points out how Venetian ruling groups made use of the long-term relationship with nuns as a particularly useful instrument of political competition. The article also shows how some female monasteries were relevant social actors in the process of defi nition of Venetian identity, largely coinciding with their own ruling groups, and in particular with the aristocracy, and with the exercise of power.[it] L’articolo si propone di esaminare il processo di definizione dell’identità del ceto dirigente di Venezia nel periodo IX-XIII secolo e il ruolo occupato dalle relazioni tra le famiglie dell’aristocrazia che costituivano quel ceto e alcuni monasteri femminili. In questa prospettiva, innovativa nell’analisi della formazione dell’aristocrazia di Venezia, si prenderà in esame l’importante monastero femminile di San Zaccaria e si farà inoltre riferimento ad alcuni altri, sorti sulle isole della laguna tra XII e XIII secolo, espressione di un clima religioso e sociale nuovo e particolare. Attraverso l’analisi dei comportamenti adottati dalle famiglie aristocratiche nei confronti di questi monasteri, si dimostra che il ceto dirigente veneziano si servì delle relazioni costanti con le monache come di uno strumento della lotta politica particolarmente utilizzato dalle famiglie dell’aristocrazia della città. Si osserva anche che alcuni monasteri femminili furono a loro volta soggetti attivi

Modelling of X-ray emission supernova remnants observed by the European satellite XMM-Newton

International Nuclear Information System (INIS)

Cassam-Chenai, G.

2004-01-01

This thesis deals with the X-ray emission of supernova remnants (SNRs) observed by the European satellite XMM-Newton. In SNRs, the matter heated to millions of degrees shines brightly in X-rays. This emission depends on the hydrodynamical evolution of the SNR, on the chemical composition of the ejected matter and on the ambient medium. Moreover, the blast-wave is considered to be the prime site of the production and the acceleration of cosmic-rays in our Galaxy. XMM-Newton is one of the first to allow the investigation of these different aspects thanks to its spatially-resolved spectroscopy and its very good sensitivity. l first studied Kepler's SNR (SN 1604) whose X-ray emission is dominated by the ejecta. Its observation has allowed to obtain information on the nucleosynthesis products, on their spatial distribution and on the temperature structure in the shocked ejecta. This gives strong constraints on the physics of the explosion and on the progenitor's type. l have shown also that the X-ray emission at the shock is likely to be non-thermal. Then, l studied the SNR G347.3-0.5 whose X-ray emission is entirely due to the synchrotron radiation of relativistic (TeV) electrons accelerated at the shock. From five pointing, l made a full mapping of the X-ray emission characteristics (brightness, absorption and spectral index) at small scale. Combined to radio observations, these results have indicated a clear interaction between the SNR and molecular clouds located at 1 kpc and not at 6 kpc as previously estimated. Lastly, in the framework of a self-similar hydrodynamical model coupled with non-linear particle acceleration, l have obtained the synchrotron emission profile in SNRs, including the adiabatic and radiative losses of the accelerated electrons. (author) [fr

Broadband X-ray spectra of the ultraluminous x-ray source Holmberg IX X-1 observed with NuSTAR, XMM-Newton, and Suzaku

DEFF Research Database (Denmark)

Walton, D. J.; Harrison, F. A.; Grefenstette, B. W.

2014-01-01

We present results from the coordinated broadband X-ray observations of the extreme ultraluminous X-ray source Holmberg IX X-1 performed by NuSTAR, XMM-Newton, and Suzaku in late 2012. These observations provide the first high-quality spectra of Holmberg IX X-1 above 10 keV to date, extending the...

Energy Levels and Radiative Rates for Transitions in F-like Sc XIII and Ne-like Sc XII and Y XXX

Directory of Open Access Journals (Sweden)

Kanti M. Aggarwal

2018-05-01

Full Text Available Energy levels, radiative rates and lifetimes are reported for F-like Sc XIII and Ne-like Sc XII and Y XXX for which the general-purpose relativistic atomic structure package (GRASP has been adopted. For all three ions, limited data exist in the literature but comparisons have been made wherever possible to assess the accuracy of the calculations. In the present work, the lowest 102, 125 and 139 levels have been considered for the respective ions. Additionally, calculations have also been performed with the flexible atomic code (FAC to (particularly confirm the accuracy of energy levels.

Energy Levels and Radiative Rates for Transitions in F-like Sc XIII and Ne-like Sc XII and Y XXX

Science.gov (United States)

Aggarwal, Kanti

2018-05-01

Energy levels, radiative rates and lifetimes are reported for F-like Sc~XIII and Ne-like Sc~XII and Y~XXX for which the general-purpose relativistic atomic structure package ({\\sc grasp}) has been adopted. For all three ions limited data exist in the literature but comparisons have been made wherever possible to assess the accuracy of the calculations. In the present work the lowest 102, 125 and 139 levels have been considered for the respective ions. Additionally, calculations have also been performed with the flexible atomic code ({\\sc fac}) to (particularly) confirm the accuracy of energy levels.

Radiation protection in the 2000s - Theory and practice. Nordic Society for Radiation Protection. Proceedings of the XIII ordinary meeting

International Nuclear Information System (INIS)

Paile, W.

2003-06-01

The XIII ordinary meeting of the Nordic Society for Radiation Protection (NSFS) was held on August 25-29, 2002 in Turku (Aabo), Finland. The main topics included: protection of the environment, information and ethics, natural radiation, reactor safety and waste management, emergency preparedness, medical use of radiation, radiation in industrial use, education and certification, radiation biology and epidemiology, and radioecology and monitoring. The proceedings of the meeting includes all the papers of the oral presentations as well as the poster presentations. Papers presenting scientific results have been subject to a referee process with evaluation of independent experts

A DEEP XMM-NEWTON OBSERVATION OF THE QUASAR 3C 287

International Nuclear Information System (INIS)

Salvesen, G.; Miller, J. M.; Cackett, E.; Siemiginowska, A.

2009-01-01

We report on an XMM-Newton observation of the z = 1.055 quasar and Gigahertz Peaked Spectrum (GPS) source 3C 287. Our 62.3 ks observation provides an exceptional X-ray view of a prominent member of this important subclass of active galactic nuclei (AGNs). The X-ray spectra of 3C 287 are consistent with a simple absorbed power law with a spectral index of Γ = 1.72 ± 0.02. Our fits imply a bolometric luminosity of L = 5.8 ± 0.2 x 10 45 erg s -1 over the 0.3-10.0 keV band; this gives a mass lower limit of M BHmin ≥ 4.6 x 10 7 M sun assuming X-rays contribute 10% of the bolometric luminosity and radiation at the Eddington limit. Iron emission lines are common in the X-ray spectra of many AGNs, but the observed spectra appear to rule out strong emission lines in 3C 287. The simple power-law spectrum and the absence of strong emission lines may support a picture where our line of sight intersects a relativistic jet. Milliarcsecond radio imaging of 3C 287 appears to support this interpretation. We discuss our results in the context of different AGNs subclasses and the possibility that GPS sources harbor newly formed black hole jets.

Averroes en la revolución intelectual del siglo XIII: bases para una reinterpretación de la Modernidad

OpenAIRE

Herráiz Oliva, Pilar

2016-01-01

El objetivo de esta tesis es mostrar cómo, en el siglo XIII, en la facultad de artes de la Universidad de París, el averroísmo, o el aristotelismo radical, emergió como movimiento filosófico que defendía la autonomía de la razón, de la filosofía y de la ciencia. Otro de los objetivos de esta tesis es mostrar que la secularización y la especialización de las distintas ciencias, tal y como las concebimos hoy, tienen su origen en la nueva forma de hacer filosofía que surge de las exigencias meto...

Contributions of the "Great" X-Ray Observatories (XMM-Newton and Chandra) to Astronomy and Astrophysics

Science.gov (United States)

Weisskopf, Martin

2011-01-01

NASA s Chandra X-ray Observatory and ESA s XMM-Newton made their first observations over a decade ago. The unprecedented and complementary capabilities of these observatories to detect, image, and measure the energy of cosmic X-rays, achieved less than 50 years after the first detection of an extra-solar X-ray source, represent an increase in sensitivity comparable in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. In this presentation we highlight some of the many discoveries made using these powerful X-ray observatories that have transformed 21st century astronomy. We briefly discuss future prospects for this truly exciting field.

Spectral re-distribution and surface loss effects in Swift XRT (XMM-Newton EPIC) MOS CCDs

CERN Document Server

Short, A D; Turner, M J L

2002-01-01

In the course of testing and selecting the EPIC MOS CCDs for the XMM-Newton observatory, the developed a Monte-Carlo model of the CCD response. Among other things, this model was used to investigate surface loss effects evident at low energies. By fitting laboratory data, these losses were characterised as a simple function of X-ray interaction depth and this result enabled the spectral re-distribution itself to be modelled as a simple analytical function. Subsequently, this analytical function has been used to generate the response matrix for the EPIC MOS instruments and will now be employed to model the spectral re-distribution for the Swift XRT CCD.

NuSTAR, XMM-Newton and Suzaku Observations of the Ultraluminous X-Ray Source Holmberg II X-1

DEFF Research Database (Denmark)

Walton, D. J.; Middleton, M. J.; Rana, V.

2015-01-01

We present the first broadband 0.3-25.0 keV X-ray observations of the bright ultraluminous X-ray source (ULX) Holmberg II X-1, performed by NuSTAR, XMM-Newton, and Suzaku in 2013 September. The NuSTAR data provide the first observations of Holmberg II X-1 above 10 keV and reveal a very steep high...

A systematic analysis of the XMM-Newton background: IV. Origin of the unfocused and focused components

Science.gov (United States)

Gastaldello, F.; Ghizzardi, S.; Marelli, M.; Salvetti, D.; Molendi, S.; De Luca, A.; Moretti, A.; Rossetti, M.; Tiengo, A.

2017-12-01

We show the results obtained in the FP7 European program EXTraS and in the ESA R&D ATHENA activity AREMBES aimed at a deeper understanding of the XMM-Newton background to better design the ATHENA mission. Thanks to an analysis of the full EPIC archive coupled to the information obtained by the Radiation Monitor we show the cosmic ray origin of the unfocused particle background and its anti-correlation with the solar activity. We show the first results of the effort to obtain informations about the particle component of the soft proton focused background.

XMM-NEWTON OBSERVATION OF THE VERY OLD PULSAR J0108-1431

Energy Technology Data Exchange (ETDEWEB)

Posselt, B.; Arumugasamy, P.; Pavlov, G. G. [Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 (United States); Manchester, R. N.; Shannon, R. M. [CSIRO Astronomy and Space Science, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710 (Australia); Kargaltsev, O., E-mail: posselt@psu.edu [Department of Physics, The George Washington University, Washington, DC 20052 (United States)

2012-12-20

We report on an X-ray observation of the 166 Myr old radio pulsar J0108-1431 with XMM-Newton. The X-ray spectrum can be described by a power-law model with a relatively steep photon index {Gamma} Almost-Equal-To 3 or by a combination of thermal and non-thermal components, e.g., a power-law component with fixed photon index {Gamma} = 2 plus a blackbody component with a temperature of kT = 0.11 keV. The two-component model appears more reasonable considering different estimates for the hydrogen column density N{sub H}. The non-thermal X-ray efficiency in the single power-law model is {eta}{sup PL}{sub 1-10{sub keV}}= L{sup PL}{sub 1-10{sub keV}}/ E-dot {approx}0.003, higher than in most other X-ray-detected pulsars. In the case of the combined model, the non-thermal and thermal X-ray efficiencies are even higher, {eta}{sup PL}{sub 1-10{sub keV}}{approx}{eta}{sup bb}{sub PC}{approx}0.006. We detected X-ray pulsations at the radio period of P Almost-Equal-To 0.808 s with significance of Almost-Equal-To 7{sigma}. The pulse shape in the folded X-ray light curve (0.15-2 keV) is asymmetric, with statistically significant contributions from up to five leading harmonics. Pulse profiles at two different energy ranges differ slightly: the profile is asymmetric at low energies, 0.15-1 keV, while at higher energies, 1-2 keV, it has a nearly sinusoidal shape. The radio pulse peak leads the 0.15-2 keV X-ray pulse peak by {phi} = 0.06 {+-} 0.03.

THE XMM-Newton and integral observations of the Supergiant Fast X-Ray Transient IGR J16328-4726

OpenAIRE

Fiocchi, M.; Bazzano, A.; Natalucci, L.; Ubertini, P.; Sguera, V.; Bird, A. J.; Boon, C.M.; Persi, P.; Piro, L.

2016-01-01

The accretion mechanism producing the short flares observed from the Supergiant Fast X-ray Transients (SFXT) is still highly debated and forms a major part in our attempts to place these X-ray binaries in the wider context of the High Mass X-ray Binaries. We report on a 216 ks INTEGRAL observation of the SFXT IGR J16328-4726 (2014 August 24–27) simultaneous with two fixed-time observations with XMM-Newton (33 and 20 ks) performed around the putative periastron passage, in order to investigate...

Tentative detection of warm intervening gas towards PKS 0548-322 with XMM-Newton

Energy Technology Data Exchange (ETDEWEB)

Barcons, X.

2005-03-17

We present the results of a long ({approx} 93 ksec) XMM-Newton observation of the bright BL-Lac object PKS 0548-322 (z = 0.069). Our Reflection Grating Spectrometer (RGS) spectrum shows a single absorption feature at an observed wavelength {lambda} = 23.33 {+-} 0.01 {angstrom} which we interpret as OVI K{alpha} absorption at z = 0.058, i.e., {approx} 3000 km s{sup -1} from the background object. The observed equivalent width of the absorption line {approx} 30m {angstrom}, coupled with the lack of the corresponding absorption edge in the EPIC pn data, implies a column density N{sub OVI} {approx} 2 x 10{sup 16} cm{sup -2} and turbulence with a Doppler velocity parameter b > 100 km s{sup -1}. Within the limitations of our RGS spectrum, no OVII or OV K{alpha} absorption are detected. Under the assumption of ionization equilibrium by both collisions and the extragalactic background, this is only marginally consistent if the gas temperature is {approx} 2.5 x 10{sup 5} K, with significantly lower or higher values being excluded by our limits on OV or OVII. If confirmed, this would be the first X-ray detection of a large amount of intervening warm absorbing gas through OVI absorption. The existence of such a high column density absorber, much stronger than any previously detected one in OVI, would place stringent constraints on the large-scale distribution of baryonic gas in the Universe.

THE RISE OF AN IONIZED WIND IN THE NARROW-LINE SEYFERT 1 GALAXY Mrk 335 OBSERVED BY XMM-NEWTON AND HST

International Nuclear Information System (INIS)

Longinotti, A. L.; Krongold, Y.; Kriss, G. A.; Ely, J.; Gallo, L.; Grupe, D.; Komossa, S.; Mathur, S.; Pradhan, A.

2013-01-01

We present the discovery of an outflowing ionized wind in the Seyfert 1 galaxy Mrk 335. Despite having been extensively observed by most of the largest X-ray observatories in the last decade, this bright source was not known to host warm absorber gas until recent XMM-Newton observations in combination with a long-term Swift monitoring program have shown extreme flux and spectral variability. High-resolution spectra obtained by the XMM-Newton Reflection Grating Spectrometer (RGS) detector reveal that the wind consists of three distinct ionization components, all outflowing at a velocity of ∼5000 km s –1 . This wind is clearly revealed when the source is observed at an intermediate flux state (2-5 × 10 –12 erg cm –2 s –1 ). The analysis of multi-epoch RGS spectra allowed us to compare the absorber properties at three very different flux states of the source. No correlation between the warm absorber variability and the X-ray flux has been determined. The two higher ionization components of the gas (log ξ ∼ 2.3 and 3.3) may be consistent with photoionization equilibrium, but we can exclude this for the only ionization component that is consistently present in all flux states (log ξ ∼ 1.8). We have included archival, non-simultaneous UV data from Hubble Space Telescope (FOS, STIS, COS) with the aim of searching for any signature of absorption in this source that so far was known for being absorption-free in the UV band. In the Cosmic Origins Spectrograph (COS) spectra obtained a few months after the X-ray observations, we found broad absorption in C IV lines intrinsic to the active galactic nucleus and blueshifted by a velocity roughly comparable to the X-ray outflow. The global behavior of the gas in both bands can be explained by variation of the covering factor and/or column density, possibly due to transverse motion of absorbing clouds moving out of the line of sight at broad line region scale.

Extreme Ultraviolet Emission Lines of Iron Fe XI-XIII

Science.gov (United States)

Lepson, Jaan; Beiersdorfer, P.; Brown, G. V.; Liedahl, D. A.; Brickhouse, N. S.; Dupree, A. K.

2013-04-01

The extreme ultraviolet (EUV) spectral region (ca. 20--300 Å) is rich in emission lines from low- to mid-Z ions, particularly from the middle charge states of iron. Many of these emission lines are important diagnostics for astrophysical plasmas, providing information on properties such as elemental abundance, temperature, density, and even magnetic field strength. In recent years, strides have been made to understand the complexity of the atomic levels of the ions that emit the lines that contribute to the richness of the EUV region. Laboratory measurements have been made to verify and benchmark the lines. Here, we present laboratory measurements of Fe XI, Fe XII, and Fe XIII between 40-140 Å. The measurements were made at the Lawrence Livermore electron beam ion trap (EBIT) facility, which has been optimized for laboratory astrophysics, and which allows us to select specific charge states of iron to help line identification. We also present new calculations by the Hebrew University - Lawrence Livermore Atomic Code (HULLAC), which we also utilized for line identification. We found that HULLAC does a creditable job of reproducing the forest of lines we observed in the EBIT spectra, although line positions are in need of adjustment, and line intensities often differed from those observed. We identify or confirm a number of new lines for these charge states. This work was supported by the NASA Solar and Heliospheric Program under Contract NNH10AN31I and the DOE General Plasma Science program. Work was performed in part under the auspices of the Department of Energy by Lawrence Livermore National Laboratory under Contract DEAC52-07NA27344.

INTEGRAL and XMM-Newton observations of the low-luminosity and X-ray-rich burst GRB 040223

Energy Technology Data Exchange (ETDEWEB)

McGlynn, S.; Hanlon, L.; Foley, S. [College Univ., Dublin (Iran, Islamic Republic of). Department of Experimental Physics; McBreen, S. [ESTEC, Noordwijk (Netherlands). Astrophysics Mission Division, RSSD of ESA; Moran, L. [Southampton Univ., Southampton (United Kingdom). School of Physics and Astronomy; Preece, R. [Alabama Univ., Huntsville (United States); Kienlin, A. von [Max-Planck-Institut fur extraterrestrische Physik, Garching (Germany); Williams, O.R. [SCI-SDG, Noordwijk (Netherlands). Science Operation and Data Systems Division of ESA-ESTEC

2005-07-15

GRB 040223 was observed by INTEGRAL and XMM-Newton. GRB 040223 has a peak flux of (1.6{+-}0.13) x 10{sup -8} ergs cm{sup -2} s{sup -1}, a fluence of (4.4{+-}0.4) x 10{sup -7} ergs cm{sup -2} and a steep photon power law index of -2.3{+-}0.2, in the energy range 20-200 keV. The steep spectrum implies it is an X-ray-rich GRB with emission up to 200 keV and E{sub peak} < 20 keV. If E{sub peak} is < 10 keV, it would qualify as an X-ray flash with high-energy emission. The X-ray data has a spectral index {beta}{sub x} = -1.7{+-}0.2, a temporal decay of t{sup -0.75{+-}}{sup 0.25} and a large column density of 1.8 x 10{sup 22} cm{sup -2}. The luminosity-lag relationship was used to obtain a redshift z 0.1{sub -0.02}{sup +0.04}. The isotropic energy radiated in {gamma}-rays and X-ray luminosity after 10 hours are factors of 1000 and 100 less than classical GRBs. GRB 040223 is consistent with the extrapolation of the Amati relation into the region that includes XRF 030723 and XRF 020903.

EMISSION LINES BETWEEN 1 AND 2 keV IN COMETARY X-RAY SPECTRA

Energy Technology Data Exchange (ETDEWEB)

Ewing, Ian; Christian, Damian J. [Department of Physics and Astronomy, California State University, 18111 Nordhoff Street, Northridge, CA 91330 (United States); Bodewits, Dennis [Department of Astronomy, University of Maryland, College Park, MD 20742 (United States); Dennerl, Konrad [Max-Planck-Institut fuer extraterrestrische Physik, Postfach 1312, D-85741 Garching Germany (Germany); Lisse, Carey M. [Planetary Exploration Group, Space Department, Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 (United States); Wolk, Scott J., E-mail: ian.ewing.794@my.csun.edu, E-mail: daman.christian@csun.edu [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)

2013-01-20

We present the detection of new cometary X-ray emission lines in the 1.0-2.0 keV range using a sample of comets observed with the Chandra X-Ray Observatory and ACIS spectrometer. We have selected five comets from the Chandra sample with good signal-to-noise spectra. The surveyed comets are C/1999 S4 (LINEAR), C/1999 T1 (McNaught-Hartley), 153P/2002 (Ikeya-Zhang), 2P/2003 (Encke), and C/2008 8P (Tuttle). We modeled the spectra with an extended version of our solar wind charge exchange (SWCX) emission model. Above 1 keV, we find Ikeya-Zhang to have strong emission lines at 1340 and 1850 eV which we identify as being created by SWCX lines of Mg XI and Si XIII, respectively, and weaker emission lines at 1470, 1600, and 1950 eV formed by SWCX of Mg XII, Mg XI, and Si XIV, respectively. The Mg XI and XII and Si XIII and XIV lines are detected at a significant level for the other comets in our sample (LS4, MH, Encke, 8P), and these lines promise additional diagnostics to be included in SWCX models. The silicon lines in the 1700-2000 eV range are detected for all comets, but with the rising background and decreasing cometary emission, we caution that these detections need further confirmation with higher resolution instruments.

O Star Wind Mass-Loss Rates and Shock Physics from X-ray Line Profiles in Archival XMM RGS Data

Science.gov (United States)

Cohen, David

O stars are characterized by their dense, supersonic stellar winds. These winds are the site of X-ray emission from shock-heated plasma. By analyzing high-resolution X-ray spectra of these O stars, we can learn about the wind-shock heating and X-ray production mechanism. But in addition, the X-rays can also be used to measure the mass-loss rate of the stellar wind, which is a key observational quantity whose value affects stellar evolution and energy, momentum, and mass input to the Galactic interstellar medium. We make this X-ray based mass-loss measurement by analyzing the profile shapes of the X-ray emission lines observed at high resolution with the Chandra and XMM-Newton grating spectrometers. One advantage of our method is that it is insensitive to small-scale clumping that affects density-squared diagnostics. We are applying this analysis technique to O stars in the Chandra archive, and are finding mass-loss rates lower than those traditionally assumed for these O stars, and in line with more recent independent determinations that do account for clumping. By extending this analysis to the XMM RGS data archive, we will make significant contributions to the understanding of both X-ray production in O stars and to addressing the issue of the actual mass-loss rates of O stars. The XMM RGS data archive provides several extensions and advantages over the smaller Chandra HETGS archive: (1) there are roughly twice as many O and early B stars in the XMM archive; (2) the longer wavelength response of the RGS provides access to diagnostically important lines of nitrogen and carbon; (3) the very long, multiple exposures of zeta Pup provide the opportunity to study this canonical O supergiant's X-ray spectrum in unprecedented detail, including looking at the time variability of X-ray line profiles. Our research team has developed a sophisticated empirical line profile model as well as a computational infrastructure for fitting the model to high-resolution X-ray spectra

X-ray spectroscopy of the mixed morphology supernova remnant W 28 with XMM-Newton

Science.gov (United States)

Nakamura, Ryoko; Bamba, Aya; Ishida, Manabu; Yamazaki, Ryo; Tatematsu, Ken'ichi; Kohri, Kazunori; Pühlhofer, Gerd; Wagner, Stefan J.; Sawada, Makoto

2014-06-01

We report on spatially resolved X-ray spectroscopy of the north-eastern part of the mixed morphology supernova remnant (SNR) W 28 with XMM-Newton. The observed field of view includes a prominent and twisted shell emission forming the edge of this SNR as well as part of the center-filled X-ray emission brightening toward the south-west edge of the field of view. The shell region spectra are in general represented by an optically thin thermal plasma emission in collisional ionization equilibrium with a temperature of ˜ 0.3 keV and a density of ˜ 10 cm-3, which is much higher than the density obtained for inner parts. In contrast, we detected no significant X-ray flux from one of the TeV γ-ray peaks with an upper-limit flux of 2.1 × 10-14 erg cm-2 s-1 in the 2-10 keV band. The large flux ratio of TeV to X-ray, larger than 16, and the spatial coincidence of the molecular cloud and the TeV γ-ray emission site indicate that the TeV γ-ray of W 28 is π0-decay emission originating from collisions between accelerated protons and molecular cloud protons. Comparing the spectrum in the TeV band and the X-ray upper limit, we obtained a weak upper limit on the magnetic field strength B ≲ 1500 μG.

XMM-Newton confirmation of a new intermediate polar: XMMU J185330.7-012815

Science.gov (United States)

Hui, C. Y.; Sriram, K.; Choi, C.-S.

2012-01-01

We report on the results of a detailed spectro-imaging and temporal analysis of an archival XMM-Newton observation of a new intermediate polar XMMU J185330.7-012815. Its X-ray spectrum can be well described by a multitemperature thermal plasma model with the K lines of heavy elements clearly detected. Possible counterparts of XMMU J185330.7-012815 have been identified in optical and ultraviolet (UV) bands. The low values of the inferred X-ray-to-UV and X-ray-to-optical flux ratios safely rule out the possibility of its being an isolated neutron star. We confirm the X-ray periodicity of ˜238 s but, differently from the previous preliminary results, we do not find any convincing evidence of phase shift in this observation. We further investigate its properties through an energy-resolved temporal analysis and find that the pulsed fraction monotonically increases with energy.

UV, X-ray, and Optical Variability of the Young Star T Cha Produced by Inner Disk Obscuration: Results from a Coordinated HST, XMM-Newton, LCOGT, and SMARTS Observing Campaign

Science.gov (United States)

Brown, Alexander; France, Kevin; Walter, Frederick M.; Schneider, P. Christian; Brown, Timothy M.; Andrews, Sean M.; Wilner, David J.

2018-06-01

The young (7 Myr) 1.5 solar mass T Tauri star T Chamaeleontis shows dramatic variability. The optical extinction varies by at least 3 magnitudes on few hour time-scales with no obvious periodicity. The obscuration is produced by material at the inner edge of the circumstellar disk and therefore characterizing the absorbing material can reveal important clues regarding the transport of gas and dust within such disks. The inner disk of T Cha is particularly interesting, because T Cha has a transitional disk with a large gap at 0.2-15 AU in the dust disk and allows study of the gas and dust structure in the terrestrial planet formation zone during this important rapid phase of protoplanetary disk evolution. For this reason we have conducted a major multi-spectral-region observing campaign to study the UV/X-ray/optical variability of T Cha. During 2018 February/March we monitored the optical photometric and spectral variability using LCOGT (Chile/South Africa/Australia) and the SMARTS telescopes in Chile. These optical data provide a broad context within which to interpret our shorter UV and X-ray observations. We observed T Cha during 3 coordinated observations (each 5 HST orbits + 25 ksec XMM; on 2018 Feb 22, Feb 26, Mar 2) using the HST COS/STIS spectrographs to measure the FUV/NUV spectra and XMM-Newton to measure the corresponding X-ray energy distribution. The observed spectral changes are well correlated and demonstrate the influence of the same absorbing material in all the spectral regions observed. By examining which spectral features change and by how much we can determine the location of different emitting regions relative to the absorbers along the line-of-sight to the star. In this poster we provide an overview of the variability seen in the different spectral regions and quantify the dust and gas content of T Cha's inner disk edge.(This work is supported by grant HST-GO-15128 and time awarded by HST, XMM-Newton, LCOGT, and SMARTS. We acknowledge the

The BUFFALO HST Survey

Science.gov (United States)

Steinhardt, Charles; Jauzac, Mathilde; Capak, Peter; Koekemoer, Anton; Oesch, Pascal; Richard, Johan; Sharon, Keren q.; BUFFALO

2018-01-01

Beyond Ultra-deep Frontier Fields And Legacy Observations (BUFFALO) is an astronomical survey built around the six Hubble Space Telescope (HST) Frontier Fields clusters designed to learn about early galactic assembly and clustering and prepare targets for observations with the James Webb Space Telescope. BUFFALO will place significant new constraints on how and when the most massive and luminous galaxies in the universe formed and how early galaxy formation is linked to dark matter assembly. The same data will also probe the temperature and cross section of dark matter in the massive Frontier Fields galaxy clusters, and tell us how the dark matter, cluster gas, and dynamics of the clusters influence the galaxies in and around them. These studies are possible because the Spitzer Space Telescope, Chandra X-ray Observatory, XMM-Newton, and ground based telescopes have already invested heavily in deep observations around the Frontier Fields, so that the addition of HST observations can yield significant new results.

Scientific session NRNU MEPHI-2010. XIII International Telecommunication Conference of students and young scientists Young people and science. Book of abstracts. In three parts. Part 1

International Nuclear Information System (INIS)

2010-01-01

In the collection of works there are the abstracts of reports included in the program of XIII International Telecommunication Conference of students and young scientists Young people and science which took place in the Internet in November-December, 2009 on the NRNU MEPhI site http://www.molod.mephi.ru/. The topics of the conference cover a wide range of problems: applied physics and energetics, ecology, development of new materials, medical physics, nanotechnologies, automatics and electronics, information-telecommunication systems and others [ru

The 2-79 keV X-ray spectrum of the Circinus galaxy with NuSTAR, XMM-Newton, and Chandra: a fully Compton-thick active galactic nucleus

International Nuclear Information System (INIS)

Arévalo, P.; Bauer, F. E.; Puccetti, S.; Walton, D. J.; Fuerst, F.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.; Koss, M.; Boggs, S. E.; Craig, W. W.; Brandt, W. N.; Luo, B.; Brightman, M.; Christensen, F. E.; Comastri, A.; Gandhi, P.; Hailey, C. J.; Madejski, G.; Marinucci, A.

2014-01-01

The Circinus galaxy is one of the closest obscured active galactic nuclei (AGNs), making it an ideal target for detailed study. Combining archival Chandra and XMM-Newton data with new NuSTAR observations, we model the 2-79 keV spectrum to constrain the primary AGN continuum and to derive physical parameters for the obscuring material. Chandra's high angular resolution allows a separation of nuclear and off-nuclear galactic emission. In the off-nuclear diffuse emission, we find signatures of strong cold reflection, including high equivalent-width neutral Fe lines. This Compton-scattered off-nuclear emission amounts to 18% of the nuclear flux in the Fe line region, but becomes comparable to the nuclear emission above 30 keV. The new analysis no longer supports a prominent transmitted AGN component in the observed band. We find that the nuclear spectrum is consistent with Compton scattering by an optically thick torus, where the intrinsic spectrum is a power law of photon index Γ = 2.2-2.4, the torus has an equatorial column density of N H = (6-10) × 10 24 cm –2 , and the intrinsic AGN 2-10 keV luminosity is (2.3-5.1) × 10 42 erg s –1 . These values place Circinus along the same relations as unobscured AGNs in accretion rate versus Γ and L X versus L IR phase space. NuSTAR's high sensitivity and low background allow us to study the short timescale variability of Circinus at X-ray energies above 10 keV for the first time. The lack of detected variability favors a Compton-thick absorber, in line with the spectral fitting results.

A PILOT DEEP SURVEY FOR X-RAY EMISSION FROM fuvAGB STARS

Energy Technology Data Exchange (ETDEWEB)

Sahai, R. [Jet Propulsion Laboratory, MS 183-900, California Institute of Technology, Pasadena, CA 91109 (United States); Sanz-Forcada, J.; Sánchez Contreras, C. [Astrobiology Center (CSIC-INTA), ESAC campus, E-28691 Villanueva de la Canada, Madrid (Spain); Stute, M. [Institute for Astronomy and Astrophysics, Eberhard Karls Universität Tübingen, Auf der Morgenstelle 10, D-72076, Tübingen (Germany)

2015-09-01

We report the results of a pilot survey for X-ray emission from a newly discovered class of AGB stars with far-ultraviolet excesses (fuvAGB stars) using XMM-Newton and Chandra. We detected X-ray emission in three of six fuvAGB stars observed—the X-ray fluxes are found to vary in a stochastic or quasi-periodic manner on roughly hour-long timescales, and simultaneous UV observations using the Optical Monitor on XMM for these sources show similar variations in the UV flux. These data, together with previous studies, show that X-ray emission is found only in fuvAGB stars. From modeling the spectra, we find that the observed X-ray luminosities are ∼(0.002–0.2) L{sub ⊙} and the X-ray-emitting plasma temperatures are ∼(35–160) × 10{sup 6} K. The high X-ray temperatures argue against the emission arising in stellar coronae, or directly in an accretion shock, unless it occurs on a WD companion. However, none of the detected objects is a known WD-symbiotic star, suggesting that if WD companions are present, they are relatively cool (<20,000 K). In addition, the high X-ray luminosities specifically argue against emission originating in the coronae of main-sequence companions. We discuss several models for the X-ray emission and its variability and find that the most likely scenario for the origin of the X-ray (and FUV) emission involves accretion activity around a companion star, with confinement by strong magnetic fields associated with the companion and/or an accretion disk around it.

The Asamblea del Año XIII in the Rio de la Plata: Eternal Laurels to End the Revolution

Directory of Open Access Journals (Sweden)

Esteban Buch

2016-09-01

Full Text Available The Asamblea del año XIII, the 1813 Constitutional Assembly in the Río de la Plata, represents at its best revolutionary velocity, with its allegro rhythm towards wider liberties and a more perfect equality, towards an independence of the nation that, without being officially declared, inspires many of its gestures, like the creation of Argentina’s national anthem. A contemporary observer fond of anachronisms might find in it a confirmation that movement is an essential element of democracy. Yet, this dynamic perception should be balanced by reminding that the Assembly’s main project is not to accelerate the revolution, but to terminate it. “Close the period of the revolution, open the epoch of peace and freedom”, says its inaugural declaration. This paper focuses on the tension between these two conceptions of historical temporality.

Spatially resolved spectroscopy analysis of the XMM-Newton large program on SN1006

Science.gov (United States)

Li, Jiang-Tao; Decourchelle, Anne; Miceli, Marco; Vink, Jacco; Bocchino, Fabrizio

2016-04-01

We perform analysis of the XMM-Newton large program on SN1006 based on our newly developed methods of spatially resolved spectroscopy analysis. We extract spectra from low and high resolution meshes. The former (3596 meshes) is used to roughly decompose the thermal and non-thermal components and characterize the spatial distributions of different parameters, such as temperature, abundances of different elements, ionization age, and electron density of the thermal component, as well as photon index and cutoff frequency of the non-thermal component. On the other hand, the low resolution meshes (583 meshes) focus on the interior region dominated by the thermal emission and have enough counts to well characterize the Si lines. We fit the spectra from the low resolution meshes with different models, in order to decompose the multiple plasma components at different thermal and ionization states and compare their spatial distributions. In this poster, we will present the initial results of this project.

On-the-fly Data Reprocessing and Analysis Capabilities from the XMM-Newton Archive

Science.gov (United States)

Ibarra, A.; Sarmiento, M.; Colomo, E.; Loiseau, N.; Salgado, J.; Gabriel, C.

2017-10-01

The XMM-Newton Science Archive (XSA) includes since last release the possibility to perform on-the-fly data processing with SAS through the Remote Interface for Science Analysis (RISA) server. It enables scientists to analyse data without any download and installation of data and software. The analysis options presently available include extraction of spectra and light curves of user-defined EPIC source regions and full reprocessing of data for which currently archived pipeline products were processed with older SAS versions or calibration files. The current pipeline is fully aligned with the most recent SAS and calibration, while the last full reprocessing of the archive was performed in 2013. The on-the-fly data processing functionality in this release is an experimental version and we invite the community to test and let us know their results. Known issues and workarounds are described in the 'Watchouts' section of the XSA web page. Feedback on how this functionality should evolve will be highly appreciated.

EDDINGTON RATIO DISTRIBUTION OF X-RAY-SELECTED BROAD-LINE AGNs AT 1.0 < z < 2.2

International Nuclear Information System (INIS)

Suh, Hyewon; Hasinger, Günther; Steinhardt, Charles; Silverman, John D.; Schramm, Malte

2015-01-01

We investigate the Eddington ratio distribution of X-ray-selected broad-line active galactic nuclei (AGNs) in the redshift range 1.0 < z < 2.2, where the number density of AGNs peaks. Combining the optical and Subaru/Fiber Multi Object Spectrograph near-infrared spectroscopy, we estimate black hole masses for broad-line AGNs in the Chandra Deep Field South (CDF-S), Extended Chandra Deep Field South (E-CDF-S), and the XMM-Newton Lockman Hole (XMM-LH) surveys. AGNs with similar black hole masses show a broad range of AGN bolometric luminosities, which are calculated from X-ray luminosities, indicating that the accretion rate of black holes is widely distributed. We find a substantial fraction of massive black holes accreting significantly below the Eddington limit at z ≲ 2, in contrast to what is generally found for luminous AGNs at high redshift. Our analysis of observational selection biases indicates that the “AGN cosmic downsizing” phenomenon can be simply explained by the strong evolution of the comoving number density at the bright end of the AGN luminosity function, together with the corresponding selection effects. However, one might need to consider a correlation between the AGN luminosity and the accretion rate of black holes, in which luminous AGNs have higher Eddington ratios than low-luminosity AGNs, in order to understand the relatively small fraction of low-luminosity AGNs with high accretion rates in this epoch. Therefore, the observed downsizing trend could be interpreted as massive black holes with low accretion rates, which are relatively fainter than less-massive black holes with efficient accretion

The peculiar galactic center neutron star X-ray binary XMM J174457-2850.3

Energy Technology Data Exchange (ETDEWEB)

Degenaar, N.; Reynolds, M. T.; Miller, J. M. [Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109 (United States); Wijnands, R. [Anton Pannekoek Institute of Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam (Netherlands); Altamirano, D. [School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ (United Kingdom); Kennea, J. [Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802 (United States); Gehrels, N. [Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Haggard, D. [CIERA, Physics and Astronomy Department, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 (United States); Ponti, G., E-mail: degenaar@umich.edu [Max Planck Institute fur Extraterrestriche Physik, D-85748 Garching (Germany)

2014-09-10

The recent discovery of a millisecond radio pulsar experiencing an accretion outburst similar to those seen in low mass X-ray binaries, has opened up a new opportunity to investigate the evolutionary link between these two different neutron star manifestations. The remarkable X-ray variability and hard X-ray spectrum of this object can potentially serve as a template to search for other X-ray binary/radio pulsar transitional objects. Here we demonstrate that the transient X-ray source XMM J174457-2850.3 near the Galactic center displays similar X-ray properties. We report on the detection of an energetic thermonuclear burst with an estimated duration of ≅2 hr and a radiated energy output of ≅ 5 × 10{sup 40} erg, which unambiguously demonstrates that the source harbors an accreting neutron star. It has a quiescent X-ray luminosity of L {sub X} ≅ 5 × 10{sup 32}(D/6.5 kpc){sup 2} erg s{sup –1} and exhibits occasional accretion outbursts during which it brightens to L {sub X} ≅ 10{sup 35}-10{sup 36}(D/6.5 kpc){sup 2} erg s{sup –1} for a few weeks (2-10 keV). However, the source often lingers in between outburst and quiescence at L {sub X} ≅ 10{sup 33}-10{sup 34}(D/6.5 kpc){sup 2} erg s{sup –1}. This peculiar X-ray flux behavior and its relatively hard X-ray spectrum, a power law with an index of Γ ≅ 1.4, could possibly be explained in terms of the interaction between the accretion flow and the magnetic field of the neutron star.

Studying The Spectral Shape And The X-ray/uv Variability Of Active Galactic Nuclei With Data From Swift And Xmm Archives

Science.gov (United States)

Turriziani, Sara

2011-01-01

Many efforts have been made in understanding the underlying origin of variability in Active Galactic Nuclei (AGN), but at present they could give still no conclusive answers. Since a deeper knowledge of variability will enable to understand better the accretion process onto supermassive black holes, I built the first ensemble struction function analysis of the X-ray variability of samples of quasars with data from Swift and XMM-Newton archives in order to study the average properties of their variability. Moreover, it is known that UV and X-ray luminosities of quasars are correlated and recent studies quantified this relation across 5 orders of magnitude. In this context, I presents results on the X-ray/UV ratio from simultaneous observations in UV and X-ray bands of a sample of quasars with data from XMM-Newton archive. Lastly, I will present a complete sample of Swift/SDSS faint blazars and other non-thermal dominated AGNs. I used this sample to calculate the general statistical properties of faint blazars and radio galaxies and in particular their Radio LogN-LogS with fluxes down to 10 mJy, in order to gain knowledge on the contribution to Cosmic Microwave Background (CMB) and gamma-ray background radiation from the faint tail of the radio population. I acknowledge financial support through Grant ASI I/088/06/0.

LONG-TERM X-RAY VARIABILITY STUDY OF IC342 FROM XMM-NEWTON OBSERVATIONS

International Nuclear Information System (INIS)

Mak, Daisy S. Y.; Pun, Chun S. J.; Kong, Albert K. H.

2011-01-01

We presented the results of an analysis of four XMM-Newton observations of the starburst galaxy IC342 taken over a four-year span from 2001 to 2005, with an emphasis on investigating the long-term flux and spectral variability of the X-ray point sources. We detected a total of 61 X-ray sources within 35' x 30' of the galaxy down to a luminosity of (1-2) x 10 37 erg s -1 depending on the local background. We found that 39 of the 61 detected sources showed long-term variability, in which 26 of them were classified as X-ray transients. We also found 19 sources exhibiting variations in hardness ratios or undergoing spectral transitions among observations, and were identified as spectral variables. In particular, eight of the identified X-ray transients showed spectral variability in addition to flux variability. The diverse patterns of variability observed are indicative of a population of X-ray binaries. We used X-ray colors, flux and spectral variability, and in some cases the optical or radio counterparts to classify the detected X-ray sources into several stellar populations. We identified a total of 11 foreground stars, 1 supersoft source (SSS), 3 quasisoft sources (QSSs), and 2 supernova remnants (SNRs). The identified SSS/QSSs are located near or on the spiral arms, associated with young stellar populations; the 2 SNRs are very close to the starburst nucleus where current star formation activities are dominated. We also discovered a spectral change in the nuclear source of IC342 for the first time by a series of X-ray spectrum analysis.

VizieR Online Data Catalog: XXL Survey: First results (Pierre+, 2016)

Science.gov (United States)

Pierre, M.; Pacaud, F.; Adami, C.; Alis, S.; Altieri, B.; Baran, B.; Benoist, C.; Birkinshaw, M.; Bongiorno, A.; Bremer, M. N.; Brusa, M.; Butler, A.; Ciliegi, P.; Chiappetti, L.; Clerc, N.; Corasaniti, P. S.; Coupon, J.; De Breuck, C.; Democles, J.; Desai, S.; Delhaize, J.; Devriendt, J.; Dubois, Y.; Eckert, D.; Elyiv, A.; Ettori, S.; Evrard, A.; Faccioli, L.; Farahi, A.; Ferrari, C.; Finet, F.; Fotopoulou, S.; Fourmanoit, N.; Gandhi, P.; Gastaldello, F.; Gastaud, R.; Georgantopoulos, I.; Giles, P.; Guennou, L.; Guglielmo, V.; Horellou, C.; Husband, K.; Huynh, M.; Iovino, A.; Kilbinger, M.; Koulouridis, E.; Lavoie, S.; Le Brun, A. M. C.; Lefevre, J. P.; Lidman, C.; Lieu, M.; Lin, C. A.; Mantz, A.; Maughan, B. J.; Maurogordato, S.; McCarthy, I. G.; McGee, S.; Melin, J. B.; Melnyk, O.; Menanteau, F.; Novak, M.; Paltani, S.; Plionis, M.; Poggianti, B. M.; Pomarede, D.; Pompei, E.; Ponman, T. J.; Ramos-Ceja, M. E.; Ranalli, P.; Rapetti, D.; Raychaudury, S.; Reiprich, T. H.; Rottgering, H.; Rozo, E.; Ryko, E.; Sadibekova, T.; Santos, J.; Sauvageot, J. L.; Schimd, C.; Sereno, M.; Smith, G. P.; Smolcic, V.; Snowden, S.; Spergel, D.; Stanford, S.; Surdej, J.; Valageas, P.; Valotti, A.; Valtchanov, I.; Vignali, C.; Willis, J.; Ziparo, F.

2016-03-01

Paper I. Scientific motivations - XMM-Newton observing plan. Follow-up observations and simulation programme. The table xxlpoint.dat is a list of all XMM survey-type observations (quality and ancillary information. Paper II. The bright cluster sample: catalogue and luminosity function. Paper III. Luminosity-temperature relation of the bright cluster sample. Paper IV. Mass-temperature relation of the bright cluster sample. This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3*10-14erg/cm2/s on the source flux within a 1' aperture. The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. The bright cluster sample consists of systems with masses between M500=7*10+14 and 3*10+14Mȯ, mostly located between z=0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of σ8 and/or ΩM appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z~1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters. We provide the XXL-100-GC catalogue (xxl100gc.dat), the master catalogue of the 100 brightest galaxy clusters from the XXL Survey

Valor y sentido del conocimiento en las órdenes mendicantes del Siglo XIII - doi: 10.4025/actascieduc.v32i2.9775

Directory of Open Access Journals (Sweden)

Gerald Cresta

2010-12-01

Full Text Available El Siglo XIII se expresa por medio de un concepto propio de la Universidad en que todo el saber debía estar orientado a la sapientia sacrae paginae, que fue expresada por la teología. Esta cuestión representaba sin duda un ideal de la Iglesia, pero asimismo un desafío especulativo para los pensadores de entonces. Con la complejidad epistemológica heredada del siglo XII y la inserción de las órdenes mendicantes en la labor académica, principalmente dominicos y franciscanos, esta fase de la historia de las ideas asistía a un antagonismo fundamental: el naturalismo de la herencia clásica -junto con el aporte del pensamiento árabe- y el humanismo cristiano se disputan la explicación del fin último del hombre. El valor y el sentido del conocimiento dependería en gran medida de la respuesta dada a esta diversidad de orientaciones. Y si bien es un hecho clave la influencia de los grandes autores antiguos, aristotelismo y neoplatonismo no son prerrogativa de una y otra orden. En los escritos de Santo Tomás está presente el neoplatonismo y es asimismo significativa la orientación empírica de la escuela franciscana en Inglaterra. Unos y otros, sin embargo, concordarían en una unidad del saber que podríamos interpretar bajo el signo de los trascendentales del ser. 

IACHEC CROSS-CALIBRATION OF CHANDRA , NuSTAR , SWIFT , SUZAKU , XMM-NEWTON WITH 3C 273 ANDPKS 2155-304

Energy Technology Data Exchange (ETDEWEB)

Madsen, Kristin K.; Forster, Karl [Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125 (United States); Beardmore, Andrew P.; Page, Kim L. [X-ray and Observational Astronomy Group, Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH (United Kingdom); Guainazzi, Matteo [Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa, 252-5201 (Japan); Marshall, Herman L.; Miller, Eric D. [Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Ave., Cambridge, MA 02139 (United States); Stuhlinger, Martin [European Space Astronomy Centre (ESAC), P.O. Box 78, E-28691 Villanueva de la Caada, Madrid (Spain)

2017-01-01

On behalf of the International Astronomical Consortium for High Energy Calibration, we present results from the cross-calibration campaigns in 2012 on 3C 273 and in 2013 on PKS 2155-304 between the then active X-ray observatories Chandra , NuSTAR , Suzaku , Swift, and XMM-Newton . We compare measured fluxes between instrument pairs in two energy bands, 1–5 keV and 3–7 keV, and calculate an average cross-normalization constant for each energy range. We review known cross-calibration features and provide a series of tables and figures to be used for evaluating cross-normalization constants obtained from other observations with the above mentioned observatories.

AN X-RAY SURVEY OF THE YOUNG STELLAR POPULATION OF THE LYNDS 1641 AND IOTA ORIONIS REGIONS

Energy Technology Data Exchange (ETDEWEB)

Pillitteri, I.; Wolk, S. J.; Myers, P.; Walter, F. [SAO-Harvard Center for Astrophysics, Cambridge, MA 02138 (United States); Megeath, S. T. [Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606 (United States); Allen, L. [National Optical Astronomy Observatory, Tucson, AZ 85719 (United States); Bally, J. [University of Colorado, Boulder, CO 80309 (United States); Gagne, M. [Department of Geology and Astronomy, West Chester University, West Chester, PA 19383 (United States); Gutermuth, R. A. [Department of Astronomy, University of Massachusetts, Amherst, MA 01003 (United States); Hartman, L. [University of Michigan, Ann Arbor, MI 48109 (United States); Micela, G.; Sciortino, S. [INAF-Osservatorio Astronomico di Palermo, I-90134 Palermo (Italy); Oliveira, J. M. [School of Physical and Geographical Sciences, Lennard-Jones Laboratories, Keele University, Staffordshire ST5 5BG (United Kingdom); Rebull, L.; Stauffer, J., E-mail: ipillitteri@cfa.harvard.edu [CALTECH, Pasadena, CA 91125 (United States)

2013-05-10

We present an XMM-Newton survey of the part of the Orion A cloud south of the Orion Nebula. This survey includes the Lynds 1641 (L1641) dark cloud, a region of the Orion A cloud with very few massive stars and hence a relatively low ambient UV flux, and the region around the O9 III star {iota} Orionis. In addition to proprietary data, we used archival XMM data of the Orion Nebula Cluster (ONC) to extend our analysis to a major fraction of the Orion A cloud. We have detected 1060 X-ray sources in L1641 and the {iota} Ori region. About 94% of the sources have Two Micron All Sky Survey and Spitzer counterparts, 204 and 23 being Class II and Class I or protostar objects, respectively. In addition, we have identified 489 X-ray sources as counterparts to Class III candidates, given they are bright in X-rays and appear as normal photospheres at mid-IR wavelengths. The remaining 205 X-ray sources are likely distant active galactic nuclei or other galactic sources not related to Orion A. We find that Class III candidates appear more concentrated in two main clusters in L1641. The first cluster of Class III stars is found toward the northern part of L1641, concentrated around {iota} Ori. The stars in this cluster are more evolved than those in the Orion Nebula. We estimate a distance of 300-320 pc for this cluster showing that it is in the foreground of the Orion A cloud. Another cluster rich in Class III stars is located in L1641 South and appears to be a slightly older cluster embedded in the Orion A cloud. Furthermore, other evolved Class III stars are found north of the ONC toward NGC 1977.

AN X-RAY SURVEY OF THE YOUNG STELLAR POPULATION OF THE LYNDS 1641 AND IOTA ORIONIS REGIONS

International Nuclear Information System (INIS)

Pillitteri, I.; Wolk, S. J.; Myers, P.; Walter, F.; Megeath, S. T.; Allen, L.; Bally, J.; Gagné, M.; Gutermuth, R. A.; Hartman, L.; Micela, G.; Sciortino, S.; Oliveira, J. M.; Rebull, L.; Stauffer, J.

2013-01-01

We present an XMM-Newton survey of the part of the Orion A cloud south of the Orion Nebula. This survey includes the Lynds 1641 (L1641) dark cloud, a region of the Orion A cloud with very few massive stars and hence a relatively low ambient UV flux, and the region around the O9 III star ι Orionis. In addition to proprietary data, we used archival XMM data of the Orion Nebula Cluster (ONC) to extend our analysis to a major fraction of the Orion A cloud. We have detected 1060 X-ray sources in L1641 and the ι Ori region. About 94% of the sources have Two Micron All Sky Survey and Spitzer counterparts, 204 and 23 being Class II and Class I or protostar objects, respectively. In addition, we have identified 489 X-ray sources as counterparts to Class III candidates, given they are bright in X-rays and appear as normal photospheres at mid-IR wavelengths. The remaining 205 X-ray sources are likely distant active galactic nuclei or other galactic sources not related to Orion A. We find that Class III candidates appear more concentrated in two main clusters in L1641. The first cluster of Class III stars is found toward the northern part of L1641, concentrated around ι Ori. The stars in this cluster are more evolved than those in the Orion Nebula. We estimate a distance of 300-320 pc for this cluster showing that it is in the foreground of the Orion A cloud. Another cluster rich in Class III stars is located in L1641 South and appears to be a slightly older cluster embedded in the Orion A cloud. Furthermore, other evolved Class III stars are found north of the ONC toward NGC 1977.

FE K EMISSION AND ABSORPTION FEATURES IN THE XMM-EPIC SPECTRUM OF THE SEYFERT GALAXY IC 4329A

Science.gov (United States)

Markowitz, A.; Reeves, J. N.; Braito, V.

2001-01-01

We present a re-analysis of the XMM-Newton long-look of the X-ray bright Seyfert galaxy IC 4329a. The Fe K bandpass is dominated by two peaks, consistent with emission from neutral or near-neutral Fe Ka and KP. A relativistic diskline model whereby both peaks are the result of one doubly-peaked diskline profile is found to be a poor description of the data. Models using two relativistic disklines are found to describe the emission profile well. A low-inclination, moderately-relativistic dual-diskline model is possible if the contribution from narrow components, due to distant material, is small or absent. A high-inclination, moderately relativistic profile for each peak is possible if there are roughly equal contributions from both the broad and narrow components. Upper limits on Fe XXV and Fe XXVI emission and absorption at the systemic velocity of IC 4329a are obtained. We also present the results of RXTE monitoring of this source obtained so far; the combined XMM-Newton and RXTE data sets allow us to explore the time-resolved spectral behavior of this source on time scales ranging from hours to 2 years. We find no strong evidence for variability of the Fe Ka emission line on any time scale probed, likely due to the minimal level of continuum variability. We detect a narrow absorption line, at a energy of 7.68 keV in the rest frame of the source; its significance has been confirmed using Monte Carlo simulations. This feature is most likely due to absorption from Fe XXVI blueshifted to approximately 0.1c relative to the systemic velocity, making IC 4329a the lowest-redshift AGN known with a high-velocity, highly-ionized outflow component. As is often the case with similar outflows seen in high-luminosity quasars, the estimated mass outflow rate is larger than the inflow accretion rate, signaling that the outflow represents a substantial portion of the total energy budget of the AGN. The outflow could arise from a radiatively-driven disk wind, or it may be in the

Tomo XIII: ética, equidad e inclusión. Reseña de la Colección Internacional de Investigación Educativa Editorial Redipe 2018

OpenAIRE

Julio César Arboleda

2018-01-01

ÉTICA, EQUIDAD E INCLUSIÓN son los temas centrales de este tomo XIII, inherentes a procesos investigativos y reflexivos. El primer trabajo, por ejemplo, reivindica la visión ética y antropológica de la educación, que sigue constituyendo un pasivo en los procesos de reflexión y formación. Le siguen producciones en torno a la inclusión y la equidad educativa y social. Los demás capítulos constituyen aportaciones de diversas áreas del conocimiento.

2MASS - The 2 Micron All Sky Survey

Science.gov (United States)

Kleinmann, S. G.

1992-01-01

This paper describes a new sky survey to be carried out in three wavebands, J(1.25 m), H(1.65 m), and K(2.2 m). The limiting sensitivity of the survey, 10 sigma detection of point sources with K not greater than 14 mag, coupled with its all-sky coverage, were selected primarily to support studies of the large-scale structure of the Milky Way and the Local Universe. The survey requires construction of a pair of observing facilities, one each for the Northern and Southern Hemispheres. Operations are scheduled to begin in 1995. The data will begin becoming publicly available soon thereafter.

Automatic classification of time-variable X-ray sources

Energy Technology Data Exchange (ETDEWEB)

Lo, Kitty K.; Farrell, Sean; Murphy, Tara; Gaensler, B. M. [Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW 2006 (Australia)

2014-05-01

To maximize the discovery potential of future synoptic surveys, especially in the field of transient science, it will be necessary to use automatic classification to identify some of the astronomical sources. The data mining technique of supervised classification is suitable for this problem. Here, we present a supervised learning method to automatically classify variable X-ray sources in the Second XMM-Newton Serendipitous Source Catalog (2XMMi-DR2). Random Forest is our classifier of choice since it is one of the most accurate learning algorithms available. Our training set consists of 873 variable sources and their features are derived from time series, spectra, and other multi-wavelength contextual information. The 10 fold cross validation accuracy of the training data is ∼97% on a 7 class data set. We applied the trained classification model to 411 unknown variable 2XMM sources to produce a probabilistically classified catalog. Using the classification margin and the Random Forest derived outlier measure, we identified 12 anomalous sources, of which 2XMM J180658.7–500250 appears to be the most unusual source in the sample. Its X-ray spectra is suggestive of a ultraluminous X-ray source but its variability makes it highly unusual. Machine-learned classification and anomaly detection will facilitate scientific discoveries in the era of all-sky surveys.

Automatic classification of time-variable X-ray sources

International Nuclear Information System (INIS)

Lo, Kitty K.; Farrell, Sean; Murphy, Tara; Gaensler, B. M.

2014-01-01

To maximize the discovery potential of future synoptic surveys, especially in the field of transient science, it will be necessary to use automatic classification to identify some of the astronomical sources. The data mining technique of supervised classification is suitable for this problem. Here, we present a supervised learning method to automatically classify variable X-ray sources in the Second XMM-Newton Serendipitous Source Catalog (2XMMi-DR2). Random Forest is our classifier of choice since it is one of the most accurate learning algorithms available. Our training set consists of 873 variable sources and their features are derived from time series, spectra, and other multi-wavelength contextual information. The 10 fold cross validation accuracy of the training data is ∼97% on a 7 class data set. We applied the trained classification model to 411 unknown variable 2XMM sources to produce a probabilistically classified catalog. Using the classification margin and the Random Forest derived outlier measure, we identified 12 anomalous sources, of which 2XMM J180658.7–500250 appears to be the most unusual source in the sample. Its X-ray spectra is suggestive of a ultraluminous X-ray source but its variability makes it highly unusual. Machine-learned classification and anomaly detection will facilitate scientific discoveries in the era of all-sky surveys.

Investigating a Possible New Heavyweight Champion for Stellar Mass Black Holes with XMM-Newton

Science.gov (United States)

Barnard, Robin

luminosities > 3E+37 erg/s (10% Eddington for the most massive known neutron star) then we classify the XB as a BHC. XBo 135 is associated with the globular cluster Bo 135 in M31, making it a very likely XB. The highest quality XMM-Newton spectrum to date revealed a low state spectrum at a luminosity of 4.4 E+38 erg/s, while Chandra observations suggest low state emission up to 6 E+38 erg/s (0.3-10 keV). We infer from these results a black hole mass >50 solar masses; the current champion is IC10 X-1, which is a dynamically confirmed BH + Wolf-Rayet binary with a 33 solar mass BH. We have been granted a 120 ks XMM-Newton observation of XBo 135 in order to test theoretical scenarios for creating such a monster. In particular, we will be estimating the metallicity of the environs of XBo 135, to determine whether direct collapse of a metal poor, high mass star is feasible. Stars with metallicity 40 solar masses are expected to form 30-80 solar mass black holes via direct collapse, because the low metallicity prevents significant mass loss from the stellar wind over the stars lifetimes. We will follow a published method that was used to determine the metallicities of several so-called ultra-luminous X-ray sources (ULXs), which have X-ray luminosities that exceed the Eddington limit for typical stellar mass black holes ( 2 E+39 erg/s). The key parameters to measure are the hydrogen abundance, a 542 eV oxygen K absorption edge, and an 851 eV iron L absorption edge. We will fit CCD (pn + MOS) and grating (RGS) spectra simultaneously to get the best measurements of these features. If XBo 135 were found to be a 50 solar mass BH formed in a globular cluster via direct collapse, then its importance would exceed that of just being the heaviest known stellar mass black hole- similar systems could form intermediate mass black holes, and possibly even supermassive black holes.

Analysis of Quasi-periodic Oscillations and Time Lag in Ultraluminous X-Ray Sources with XMM-Newton

Energy Technology Data Exchange (ETDEWEB)

Li, Zi-Jian; Xiao, Guang-Cheng; Zhang, Shu; Ma, Xiang; Yan, Lin-Li; Qu, Jin-Lu [Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, 19B Yuquan Road, Beijing 100049 (China); Chen, Li; Bu, Qing-Cui; Zhang, Liang, E-mail: lizijian@ihep.ac.cn, E-mail: qujl@ihep.ac.cn [Department of Astronomy, Beijing Normal University, Beijing 100875 (China)

2017-04-10

We investigated the power density spectrum (PDS) and time lag of ultraluminous X-ray sources (ULXs) observed by XMM-Newton . We determined the PDSs for each ULX and found that five of them show intrinsic variability due to obvious quasi-periodic oscillations (QPOs) of mHz–1 Hz, consistent with previous reports. We further investigated these five ULXs to determine their possible time lag. The ULX QPOs exhibit a soft time lag that is linearly related to the QPO frequency. We discuss the likelihood of the ULX QPOs being type-C QPO analogs, and the time lag models. The ULXs might harbor intermediate-mass black holes if their QPOs are type-C QPO analogs. We suggest that the soft lag and the linearity may be due to reverberation.

THE XMM-NEWTON/EPIC X-RAY LIGHT CURVE ANALYSIS OF WR 6

International Nuclear Information System (INIS)

Ignace, R.; Gayley, K. G.; Hamann, W.-R.; Oskinova, L. M.; Huenemoerder, D. P.; Pollock, A. M. T.; McFall, M.

2013-01-01

We obtained four pointings of over 100 ks each of the well-studied Wolf-Rayet star WR 6 with the XMM-Newton satellite. With a first paper emphasizing the results of spectral analysis, this follow-up highlights the X-ray variability clearly detected in all four pointings. However, phased light curves fail to confirm obvious cyclic behavior on the well-established 3.766 day period widely found at longer wavelengths. The data are of such quality that we were able to conduct a search for event clustering in the arrival times of X-ray photons. However, we fail to detect any such clustering. One possibility is that X-rays are generated in a stationary shock structure. In this context we favor a corotating interaction region (CIR) and present a phenomenological model for X-rays from a CIR structure. We show that a CIR has the potential to account simultaneously for the X-ray variability and constraints provided by the spectral analysis. Ultimately, the viability of the CIR model will require both intermittent long-term X-ray monitoring of WR 6 and better physical models of CIR X-ray production at large radii in stellar winds

THE XMM-NEWTON/EPIC X-RAY LIGHT CURVE ANALYSIS OF WR 6

Energy Technology Data Exchange (ETDEWEB)

Ignace, R. [Department of Physics and Astronomy, East Tennessee State University, Johnson City, TN 37663 (United States); Gayley, K. G. [Department of Physics and Astronomy, University of Iowa, Iowa City, IA 52245 (United States); Hamann, W.-R.; Oskinova, L. M. [Institute for Physics and Astronomy, University Potsdam, D-14476 Potsdam (Germany); Huenemoerder, D. P. [Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, 70 Vassar Street, Cambridge, MA 02139 (United States); Pollock, A. M. T. [European Space Agency XMM-Newton Science Operations Centre, European Space Astronomy Centre, Apartado 78, Villanueva de la Cañada, E-28691 Madrid (Spain); McFall, M., E-mail: ignace@etsu.edu [Department of Physics, 191 W. Woodruff Avenue, Ohio State University, Columbus, OH 43210 (United States)

2013-09-20

We obtained four pointings of over 100 ks each of the well-studied Wolf-Rayet star WR 6 with the XMM-Newton satellite. With a first paper emphasizing the results of spectral analysis, this follow-up highlights the X-ray variability clearly detected in all four pointings. However, phased light curves fail to confirm obvious cyclic behavior on the well-established 3.766 day period widely found at longer wavelengths. The data are of such quality that we were able to conduct a search for event clustering in the arrival times of X-ray photons. However, we fail to detect any such clustering. One possibility is that X-rays are generated in a stationary shock structure. In this context we favor a corotating interaction region (CIR) and present a phenomenological model for X-rays from a CIR structure. We show that a CIR has the potential to account simultaneously for the X-ray variability and constraints provided by the spectral analysis. Ultimately, the viability of the CIR model will require both intermittent long-term X-ray monitoring of WR 6 and better physical models of CIR X-ray production at large radii in stellar winds.

XMM-Newton and NuSTAR Simultaneous X-Ray Observations of IGR J11215-5952

International Nuclear Information System (INIS)

Sidoli, L.; Tiengo, A.; Paizis, A.; Sguera, V.; Lotti, S.; Natalucci, L.

2017-01-01

We report the results of an XMM - Newton and NuSTAR coordinated observation of the Supergiant Fast X-ray Transient (SFXT) IGR J11215–5952, performed on 2016 February 14, during the expected peak of its brief outburst, which repeats every ∼165 days. Timing and spectral analysis were performed simultaneously in the energy band 0.4–78 keV. A spin period of 187.0 (±0.4) s was measured, consistent with previous observations performed in 2007. The X-ray intensity shows a large variability (more than one order of magnitude) on timescales longer than the spin period, with several luminous X-ray flares that repeat every 2–2.5 ks, some of which simultaneously observed by both satellites. The broadband (0.4–78 keV) time-averaged spectrum was well deconvolved with a double-component model (a blackbody plus a power law with a high energy cutoff) together with a weak iron line in emission at 6.4 keV (equivalent width, EW, of 40 ± 10 eV). Alternatively, a partial covering model also resulted in an adequate description of the data. The source time-averaged X-ray luminosity was 10 36 erg s −1 (0.1–100 keV; assuming 7 kpc). We discuss the results of these observations in the framework of the different models proposed to explain SFXTs, supporting a quasi-spherical settling accretion regime, although alternative possibilities (e.g., centrifugal barrier) cannot be ruled out.

XMM-Newton and NuSTAR Simultaneous X-Ray Observations of IGR J11215-5952

Energy Technology Data Exchange (ETDEWEB)

Sidoli, L.; Tiengo, A.; Paizis, A. [INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via E. Bassini 15, I-20133 Milano (Italy); Sguera, V. [INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via Gobetti 101, I-40129 Bologna (Italy); Lotti, S.; Natalucci, L., E-mail: sidoli@iasf-milano.inaf.it [INAF, Istituto di Astrofisica e Planetologia Spaziali, Via Fosso del Cavaliere 100, I-00133 Roma (Italy)

2017-04-01

We report the results of an XMM - Newton and NuSTAR coordinated observation of the Supergiant Fast X-ray Transient (SFXT) IGR J11215–5952, performed on 2016 February 14, during the expected peak of its brief outburst, which repeats every ∼165 days. Timing and spectral analysis were performed simultaneously in the energy band 0.4–78 keV. A spin period of 187.0 (±0.4) s was measured, consistent with previous observations performed in 2007. The X-ray intensity shows a large variability (more than one order of magnitude) on timescales longer than the spin period, with several luminous X-ray flares that repeat every 2–2.5 ks, some of which simultaneously observed by both satellites. The broadband (0.4–78 keV) time-averaged spectrum was well deconvolved with a double-component model (a blackbody plus a power law with a high energy cutoff) together with a weak iron line in emission at 6.4 keV (equivalent width, EW, of 40 ± 10 eV). Alternatively, a partial covering model also resulted in an adequate description of the data. The source time-averaged X-ray luminosity was 10{sup 36} erg s{sup −1} (0.1–100 keV; assuming 7 kpc). We discuss the results of these observations in the framework of the different models proposed to explain SFXTs, supporting a quasi-spherical settling accretion regime, although alternative possibilities (e.g., centrifugal barrier) cannot be ruled out.

A ROSAT Survey of Contact Binary Stars

Science.gov (United States)

Geske, M. T.; Gettel, S. J.; McKay, T. A.

2006-01-01

Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope with X-ray data from the ROSAT All Sky Survey (RASS) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory. From these data we confirm the emission of X-rays from all contact binary systems, with typical luminosities of approximately 1.0×1030 ergs s-1. Combining calculated luminosities with an estimated contact binary space density, we find that contact binaries do not have strong enough X-ray emission to account for a significant portion of the Galactic X-ray background.

Proceedings of VII International Symposium on Nuclear and Related Techniques. XIII Workshop on Nuclear Physics. WONP-NURT 2011

International Nuclear Information System (INIS)

2011-02-01

This year the XIII Workshop on Nuclear Physics (WONP) and the VII Symposium on Nuclear and Related Techniques (NURT) are organized jointly, by Instituto Superior de Tecnologias y Ciencias Aplicadas and Centro de Aplicaciones Tecnologicas y Desarrollo Nuclear. Both events gather scientists from several countries with top research work on nuclear physics and its applications. WONP has been carried out since 1994 promoting an ever-exchanging exchange between professionals of various nuclear and applied physics fields, those related to environmental and health care. NURT is one of the key Cuban scientific meetings since 1997 dealing with the peaceful applications of nuclear techniques in several domains of the society. WONP and NURT provide an unique opportunity for the national and international scientific community to meet outstanding researchers and discuss current trends in several areas of theoretical, experimental and applied nuclear physics and related topics. The papers submitted to this event are presented in this CD-ROM

The changing source of X-ray reflection in the radio-intermediate Seyfert 1 galaxy III Zw 2

Science.gov (United States)

Gonzalez, A. G.; Waddell, S. G. H.; Gallo, L. C.

2018-03-01

We report on X-ray observations of the radio-intermediate, X-ray bright Seyfert 1 galaxy, III Zw 2, obtained with XMM-Newton, Suzaku, and Swift over the past 17 yr. The source brightness varies significantly over yearly time-scales, but more modestly over periods of days. Pointed observations with XMM-Newton in 2000 and Suzaku in 2011 show spectral differences despite comparable X-ray fluxes. The Suzaku spectra are consistent with a power-law continuum and a narrow Gaussian emission feature at ˜6.4 keV, whereas the earlier XMM-Newton spectrum requires a broader Gaussian profile and soft-excess below ˜2 keV. A potential interpretation is that the primary power-law emission, perhaps from a jet base, preferentially illuminates the inner accretion disc in 2000, but the distant torus in 2011. The interpretation could be consistent with the hypothesized precessing radio jet in III Zw 2 that may have originated from disc instabilities due to an ongoing merging event.

Materiales y técnicas constructivas en la Murcia andalusí (siglos X-XIII

Directory of Open Access Journals (Sweden)

Navarro Palazón, Julio

2011-12-01

Full Text Available The evolution of the materials and building techniques of the andalusian city of Murcia between the 9th and 13th centuries are here studied, mainly based on the new information provided by the numerous archaeological excavations that have been carried out in the city for the last thirty years, related especially to residential architecture. After its accuracy analysis, some differences between the buildings techniques manufactured in the 10th and 11th centuries and those later attributed to 12th and 13th centuries have been identified, being thus highly important to describe them by remarking at the same time those distinguishing features. Problems related to the absolute chronology of these building techniques are also discussed, highlighting the definitive information currently known. With the main aim of analysing how general these remarks are or, on the contrary, if they depend on the regionalization phenomenon characterizing the andalusian recording material, we will compare the information obtained in Murcia with those coming from other andalusian sites, located these far away from the studied area. Finally, we will check if there are differences between the rural and urban environments by comparing the materials and building techniques recorded in two coetaneous sites in Murcia, both sited close to the same river Segura and 40 km distant from each other: the city of Murcia (a large madîna and the deserted settlement of Siyâsa (a hisn.En el presente trabajo estudiamos la evolución de los materiales y técnicas constructivas en la Murcia andalusí, durante un periodo de tiempo que se extiende entre los siglos X y XIII, para lo que nos basaremos especialmente en la rica información extraída de las numerosas excavaciones efectuadas en dicha ciudad, que se refiere sobre todo a arquitectura residencial. Tras su exhaustivo análisis hemos identificado algunas diferencias entre las fábricas de los siglos X y XI y las posteriores de los

Quid facundia posset / re patuit (Οu., Μet. XIII 382-383: the oratorical strategies of Ulysses in the Ovidian armorum iudicium

Directory of Open Access Journals (Sweden)

Eleonora Tola

2010-12-01

Full Text Available In book XIII of his Metamorphoses Ovid presents the contest for the arms of Achilles between Ajax and Ulysses. The speeches that they address to the assembly of Greek show a judicial process according to the norms of Roman rhetoric. Through his traditional facundia Ulysses persuades his public and gains victory after a confrontation that relates to a verbal fight. I will explore the construction of Ulysses’s discursive superiority focusing especially on two key-places of his speech, exordium (128-139 and peroratio (339-381. I will identify different syntactic, metrical and stylistic strategies with which Ulysses captivates his interlocutors. From a metapoetic perspective, Ovid’s tale establishes some resonances between the character’s Fama and its own textual mechanisms.

Matching microlensing events with X-ray sources

Science.gov (United States)

Sartore, N.; Treves, A.

2012-03-01

Aims: The detection of old neutron stars and stellar mass black holes in isolation is one of the most sought after goals of compact object astrophysics. Microlensing surveys may help in achieving this aim because the lensing mechanism is independent of the emission properties of the lens. Several black hole candidates have indeed been detected by means of microlensing observations have been reported in the literature. The identification of counterparts, especially in the X-rays, would be a strong argument in favor of the compact nature of these lenses. Methods: We perform a cross-correlation between the catalogs of microlensing events produced by the OGLE, MACHO, and MOA teams, and those of X-rays sources from the data acquired by the XMM-Newton and Chandra satellites. On the basis of our previous work, we select only microlensing events with durations longer than one hundred days, which should contain a large fraction of lenses as compact objects. Our matching criterion takes into account the positional coincidence on the sky. Results: We find a single match between a microlensing event, OGLE-2004-BLG-081 (tE ~ 103 days), and the X-ray source 2XMM J180540.5-273427. The angular separation is ~0.5 arcsec, i.e. well within the 90% error box of the X-ray source. The hardness ratios reported in the 2XMM catalog imply that it has a hard spectrum with a peak between 2 keV and 4.5 keV or it has a softer but highly absorbed spectrum. Moreover, the microlensing event is not fully constrained, and other authors propose a possible association of the source star with either a flaring cataclysmic variable or a RS Canum Venaticorum-like star. Conclusions: The very small angular separation (within uncertainties) is a strong indicator that 2XMM J180540.5-273427 is the X-ray counterpart of the OGLE event. However, the uncertainties in the nature of both the lensed system and the lens itself challenge the interpretation of 2XMM J180540.5-273427 as the first confirmed isolated black

Report: Ordine del sentire e apertura al mondo. Filosofia delle emozioni e processo di individuazione della persona XIII Convegno internazionale della Max-Scheler-Gesellschaft Università di Verona 27-30 Maggio 2015

OpenAIRE

Maria Teresa Speranza

2015-01-01

An interesting debate on the issue of personal identity and its ethical implications has animated the days of the XIII International Congress of Max Scheler‐Gesellschaft. A large program of work has garnered numerous perspectives on the philosophy of person and the phenomenology of otherness, investigating in particular the role of emotions in the formation of person process. The main topic of conference was the Max Scheler’s phenomenology of emotions, which is an i...

A broadband X-ray study of the Geminga pulsar with NuSTAR And XMM-Newton

International Nuclear Information System (INIS)

Mori, Kaya; Gotthelf, Eric V.; Halpern, Jules P.; Beloborodov, Andrei M.; Hailey, Charles J.; Dufour, Francois; Kaspi, Victoria M.; An, Hongjun; Bachetti, Matteo; Boggs, Steven E.; Craig, William W.; Christensen, Finn E.; Harrison, Fiona A.; Kouveliotou, Chryssa; Pivovaroff, Michael J.; Stern, Daniel; Zhang, William W.

2014-01-01

We report on the first hard X-ray detection of the Geminga pulsar above 10 keV using a 150 ks observation with the Nuclear Spectroscopic Telescope Array (NuSTAR) observatory. The double-peaked pulse profile of non-thermal emission seen in the soft X-ray band persists at higher energies. Broadband phase-integrated spectra over the 0.2-20 keV band with NuSTAR and archival XMM-Newton data do not fit to a conventional two-component model of a blackbody plus power law, but instead exhibit spectral hardening above ∼5 keV. We find that two spectral models fit the data well: (1) a blackbody (kT 1 ∼ 42 eV) with a broken power law (Γ 1 ∼ 2.0, Γ 2 ∼ 1.4 and E break ∼ 3.4 keV) and (2) two blackbody components (kT 1 ∼ 44 eV and kT 2 ∼ 195 eV) with a power-law component (Γ ∼ 1.7). In both cases, the extrapolation of the Rayleigh-Jeans tail of the thermal component is consistent with the UV data, while the non-thermal component overpredicts the near-infrared data, requiring a spectral flattening at E ∼ 0.05-0.5 keV. While strong phase variation of the power-law index is present below ∼5 keV, our phase-resolved spectroscopy with NuSTAR indicates that another hard non-thermal component with Γ ∼ 1.3 emerges above ∼5 keV. The spectral hardening in non-thermal X-ray emission as well as spectral flattening between the optical and X-ray bands argue against the conjecture that a single power law may account for multi-wavelength non-thermal spectra of middle-aged pulsars.

Isotope hydrology investigations in Latin America 1994. Investigations on hydrology and hydrogeology in Latin America on water resources and groundwater pollution. Results achieved during the implementation of the project RLA/8/014 - ARCAL XIII: Application of isotope techniques in hydrology; Estudios de hidrologia isotopica en America Latina 1994. Estudios hidrologicos e hidrogeologicos en America Latina sobre los recursos hidricos y la contaminacion de las aguas subterraneas. Resultados obtenidos en el marco del proyecto RLA/8/014 - ARCAL XIII: Aplicacion de tecnicas isotopicas en hidrologia

Energy Technology Data Exchange (ETDEWEB)

NONE

1995-10-01

This IAEA Technical Document contains 17 articles about the results achieved during the implementation of the project RLA/8/014, ARCAL XIII, aimed at the application of isotope techniques in hydrology in the Caribbean and Latin America. Also included is the list of 19 participants in the project. Refs, figs and tabs.

Safety of Factor XIII Concentrate: Analysis of More than 20 Years of Pharmacovigilance Data

Science.gov (United States)

Solomon, Cristina; Korte, Wolfgang; Fries, Dietmar; Pendrak, Inna; Joch, Christine; Gröner, Albrecht; Birschmann, Ingvild

2016-01-01

Background Plasma-derived factor XIII (FXIII) concentrate is an effective treatment for FXIII deficiency. We describe adverse drug reactions (ADRs) reported during pharmacovigilance monitoring of Fibrogammin®/Corifact® and review published safety data. Methods Postmarketing safety reports recorded by CSL Behring from June 1993 to September 2013 were analyzed. Clinical studies published during the same period were also reviewed. Results Commercial data indicated that 1,653,450,333 IU FXIII concentrate were distributed over the review period, equivalent to 1,181,036 doses for a 70 kg patient. 75 cases were reported (one/15,700 standard doses or 22,046,000 IU). Reports of special interest included 12 cases of possible hypersensitivity reactions (one/98,400 doses or 137,787,500 IU), 7 with possible thromboembolic events (one/168,700 doses or 236,207,200 IU), 5 of possible inhibitor development (one/236,200 doses or 330,690,100 IU), and 20 of possible pathogen transmission (one/59,100 doses or 82,672,500 IU). 19 pathogen transmission cases involved viral infection; 4 could not be analyzed due to insufficient data, but for all others a causal relationship to the product was assessed as unlikely. A review of published literature revealed a similar safety profile. Conclusion Assessment of ADRs demonstrated that FXIII concentrate carries a low risk of ADRs across various clinical situations, suggesting a favorable safety profile. PMID:27781024

Isotope hydrology investigations in Latin America 1994. Investigations on hydrology and hydrogeology in Latin America on water resources and groundwater pollution. Results achieved during the implementation of the project RLA/8/014 - ARCAL XIII: Application of isotope techniques in hydrology

International Nuclear Information System (INIS)

1995-10-01

This IAEA Technical Document contains 17 articles about the results achieved during the implementation of the project RLA/8/014, ARCAL XIII, aimed at the application of isotope techniques in hydrology in the Caribbean and Latin America. Also included is the list of 19 participants in the project. Refs, figs and tabs

INTEGRAL and XMM-Newton observations of the puzzling binary system LSI +61 303

Science.gov (United States)

Chernyakova, Masha; Neronov, A.; Walter, R.

LSI +61° 303 is one of the few X-ray binaries with Be star companion from which both radio and high-energy gamma-ray emission have been observed. We present XMM-Newton and INTE- GRAL observations which reveal variability of the X-ray spectral index of the system. The X-ray spectrum is hard (photon index Γ ≃ 1.5) during the orbital phases of both high and low X-ray flux. However, the spectrum softens at the moment of transition from high to low X-ray state. The spectrum of the system in the hard X-ray band does not reveal the presence of a cut-off (or, at least a spectral break) at 10-60 keV energies, expected if the compact object is an accreting neu- tron star. The observed spectrum and spectral variability can be explained if the compact object in the system is a rotation powered pulsar. In this case the recently found X-ray spectral variability of the system on the several kiloseconds time scale can be explained by the clumpy structure of the Be star disk.

NuSTAR Search for Hard X-ray Emission from the Star Formation Regions in Sh2-104

Science.gov (United States)

Gotthelf, Eric V.

2016-04-01

We present NuSTAR hard X-ray observations of Sh2-104, a compact Hii region containing several young massive stellar clusters (YMSCs). We have detected distinct hard X-ray sources coincident with localized VERITAS TeV emission recently resolved from the giant gamma-ray complex MGRO J2019+37 in the Cygnus region. Faint, diffuse X-ray emission coincident with the eastern YMSC in Sh2-104 is likely the result of colliding winds of component stars. Just outside the radio shell of Sh2-104 lies 3XMM J201744.7+365045 and nearby nebula NuSTAR J201744.3+364812, whose properties are most consistent with extragalactic objects. The combined XMM-Newton and NuSTAR spectrum of 3XMM J201744.7+365045 is well-fit to an absorbed power-law model with NH = (3.1+/-1.0)E22 1/cm^2 and photon index Gamma = 2.1+/-0.1. Based on possible long-term flux variation and lack of detected pulsations (Sh2-104 will help identify the nature of the X-ray sources and their relation to MGRO J2019+37.

Las capillas y capellanías reales castellano-leonesas en la Baja Edad Media (siglos XIII-XV: algunas precisiones institucionales

Directory of Open Access Journals (Sweden)

Nogales Rincón, David

2005-12-01

Full Text Available The study of royal chapels and royal chaplaincies is focus on the analysis of the relationships between de Palace Chapel and the cathedral/monastic royal chapels from a institucional, ideologic and functional criterions, on making a systematization of them and on presenting some general notes about their characteristics, ideal patterns and development in the late Middle Ages in Castille (13th-15th centuries.

El estudio de las capillas y capellanías reales se centra en el análisis de las relaciones entre la Capilla Palacio y las capillas reales catedralicias/monásticas desde un punto de vista institucional, ideológico y funcional, en llevar a cabo una sistematización de éstas y ofrecer algunas notas generales sobre sus características, modelos ideales y evolución en la Castilla bajomedieval (siglos XIII-XV.

Ciudades y poder político en al-Andalus. Una hipótesis sobre el origen de las revueltas urbanas en Murcia en el siglo XIII

Directory of Open Access Journals (Sweden)

Frey Sánchez, Antonio Vicente

2014-12-01

Full Text Available Throughout the 13th century a succession of urban revolts took place in al-Andalus, which caused the withdrawal of the Almohad Empire and the establishment of the third taifas, initially led by Muhammad b. Yūsuf b. Hūd al-Mutawakkil. The inability of this emir to hold together this newly-built state, and the continuous insurrections inside and utside of Murcia have led historians to investigate the nature of political power during this period. This article examines each one of these proposals and, on the basis of an analysis of some socio-economic aspects relating to Murcia (being a representative city of al-Andalus and capital of the hūdí movement during the first half of the thirteenth century, proposes a hypothesis on the nature of its power.Durante el siglo XIII se produjo una serie de revueltas urbanas en al-Andalus que ocasionó la retirada del Imperio almohade y la formación de las terceras taifas, inicialmente encabezadas por Muḥammad b. Yūsuf b. Hūd al-Mutawakkil. La incapacidad de este emir para mantener unido el estado que había creado y las continuas insurrecciones fuera y dentro de Murcia ha llevado a historiadores y filólogos a indagar sobre la naturaleza del poder político en este periodo. Este artículo estudia cada una de estas interpretaciones y, a partir del análisis de algunos aspectos socio-económicos de Murcia, ciudad representativa en al-Andalus y capital del movimiento hūdí durante la primera mitad del siglo XIII, presenta una propuesta sobre la naturaleza de su poder.

200-UP-2 operable unit radiological surveys

International Nuclear Information System (INIS)

Wendling, M.A.

1994-01-01

This report summarizes and documents the results of the radiological surveys conducted from August 17 through December 16, 1993 over a partial area of the 200-UP-2 Operable Unit, 200-W Area, Hanford Site, Richland, Washington. In addition, this report explains the survey methodology of the Mobile Surface Contamination Monitor 11 (MSCM-II) and the Ultra Sonic Ranging And Data System (USRADS). The radiological survey of the 200-UP-2 Operable Unit was conducted by the Site Investigative Surveys/Environmental Restoration Health Physics Organization of the Westinghouse Hanford Company. The survey methodology for the majority of area was based on utilization of the MSCM-II or the USRADS for automated recording of the gross beta/gamma radiation levels at or near six (6) inches from the surface soil

45 CFR 2508.4 - When can Corporation records be disclosed?

Science.gov (United States)

2010-10-01

...) To a recipient who has provided the Corporation with advance adequate written assurance that the... perform a survey, audit, or other review of the Corporation's procedures and operations; and (xiii) To a...

Laser Obstacle Detection System Flight Testing

National Research Council Canada - National Science Library

Davis, Timothy

2003-01-01

...). The Aviation Applied Technology Directorate (AATD) was contracted to mount the HELLAS sensor on the nose of a UH-60L Blackhawk helicopter and to conduct flight tests to evaluate the HELLAS obstacle detection sensor...

Ambient concentrations of total suspended particulate matter and its elemental constituents at the wider area of the mining facilities of TVX Hellas in Chalkidiki, Greece.

Science.gov (United States)

Gaidajis, George

2003-01-01

To assess ambient air quality at the wider area of TVX Hellas mining facilities, the Total Suspended Particulate matter (TSP) and its content in characteristic elements, i.e., As, Cd, Cu, Fe, Mn, Pb, Zn are being monitored for more than thirty months as part of the established Environmental Monitoring Program. High Volume air samplers equipped with Tissue Quartz filters were employed for the collection of TSP. Analyses were effected after digestion of the suspended particulate with an HNO3-HCl solution and determination of elemental concentrations with an Atomic Absorption Spectroscopy equipped with graphite furnace. The sampling stations were selected to record representatively the existing ambient air quality in the vicinity of the facilities and at remote sites not affected from industrial activities. Monitoring data indicated that the background TSP concentrations ranged from 5-60 microg/m3. Recorded TSP concentrations at the residential sites close to the facilities ranged between 20-100 microg/m3, indicating only a minimal influence from the mining and milling activities. Similar spatial variation was observed for the TSP constituents and specifically for Pb and Zn. To validate the monitoring procedures, a parallel sampling campaign took place with different High Volume samplers at days where low TSP concentrations were expected. The satisfactory agreement (+/- 11%) at low concentrations (50-100 microg/m3) clearly supported the reproducibility of the techniques employed specifically at the critical range of lower concentrations.

Tobacco taxation: the importance of earmarking the revenue to health care and tobacco control.

Science.gov (United States)

Vardavas, Constantine I; Filippidis, Filippos T; Agaku, Israel; Mytaras, Vasileios; Bertic, Monique; Connolly, Gregory N; Tountas, Yannis; Behrakis, Panagiotis

2012-01-01

Increases in tobacco taxation are acknowledged to be one of the most effective tobacco control interventions. This study aimed at determining the mediating role of socioeconomical status (SES) and the earmarking of revenue to healthcare and tobacco control, in influencing population support for the adoption of a 2 Euro tobacco tax increase in Greece, amid the challenging economic environment and current austerity measures. Data was collected from two national household surveys, the "Hellas Health III" survey, conducted in October 2010 and the "Hellas Tobacco survey" conducted in September 2012. Data was analyzed from 694 and 1066 respondents aged 18 years or more, respectively. Logistic regression models were fitted to measure the adjusted relationship between socio-economic factors for the former, and support for increased taxation on tobacco products for the latter. In 2012 amidst the Greek financial crisis, population support for a flat two euro tax increase reached 72.1%, if earmarked for health care and tobacco control, a percentage high both among non-smokers (76%) and smokers (64%) alike. On the contrary, when not earmarked, only 43.6% of the population was in support of the equivalent increase. Women were more likely to change their mind and support a flat two-euro increase if the revenue was earmarked for health care and tobacco control (aOR = 1.70; 95% C.I: 1.22-2.38, p = 0.002). Furthermore, support for an increase in tobacco taxation was not associated with SES and income. Despite dire austerity measures in Greece, support for an increase in tobacco taxation was high among both smokers and non-smokers, however, only when specifically earmarked towards health care and tobacco control. This should be taken into account not only in Greece, but within all countries facing social and economic reform.

X-ray Observations of Eight Young Open Star Clusters: I ...

Indian Academy of Sciences (India)

XMM-Newton View of Eight Young Open Star Clusters. 395 ... Multi-wavelength surveys of young open clusters provide an effective way to iden- tify young cluster .... First, the input images were built in two energy ranges, a soft band (0.3–2.0 keV) and ..... 3.2 Color-magnitude diagram of X-ray sources with NIR counterparts.

“Et qui or me vaurra entendre, cuer et oreilles me doit rendre”: espacios de lectura y público de los roman courtois de Chrétien de Troyes (siglos XII-XIII

Directory of Open Access Journals (Sweden)

Diego Carlo Améndolla Spinola

2016-06-01

Full Text Available Basado en los planteamientos de la lógica social del texto, este artículo presenta un estudio del público que escuchaba los romances corteses entre los siglo XII y XIII, específicamente los realizados por Chrétien de Troyes –clérigo lector de la Corte de Leonor de Aquitania y de Enrique II Plantagenet–, además de establecer y analizar las diversas salas de los castillos donde estas obras literarias eran narradas.

Quando rey perdemos nunq[u]a bien nos fallamos. La muerte del rey en la Castilla del siglo XIII

Directory of Open Access Journals (Sweden)

Pérez Monzón, Olga

2007-12-01

Full Text Available This article deals with the funeral spaces of the Castilian kings during the 13th century, and the iconography of their tombs as the reflection of a political ideational system tending toward the sanctification of the monarchy. This elevation of royalty provoked an open conflict with certain members of the nobility and the royal family, as well as a political and artistic response.

El presente artículo trata sobre los ámbitos fúnebres de los reyes castellanos durante el siglo XIII y la particularidad iconográfica de sus monumentos tumulares como reflejo de un ideario político tendente a la sacralización de la monarquía. El encumbramiento de la realeza provocó un abierto conflicto con determinados miembros de la realeza y la familia real y una respuesta política y artística.

Suzaku and XMM-Newton observations of the North Polar Spur: Charge exchange or ISM absorption?

Science.gov (United States)

Gu, Liyi; Mao, Junjie; Costantini, Elisa; Kaastra, Jelle

2016-10-01

By revisiting the Suzaku and XMM-Newton data of the North Polar Spur, we discovered that the spectra are inconsistent with the traditional model consisting of pure thermal emission and neutral absorption. The most prominent discrepancies are the enhanced O vii and Ne ix forbidden-to-resonance ratios, and a high O viii Lyβ line relative to other Lyman series. A collisionally ionized absorption model can naturally explain both features, while a charge exchange component can only account for the former. By including the additional ionized absorption, the plasma in the North Polar Spur can be described by a single-phase collisional ionization equilibrium (CIE) component with a temperature of 0.25 keV, and nitrogen, oxygen, neon, magnesium, and iron abundances of 0.4-0.8 solar. The abundance pattern of the North Polar Spur is well in line with those of the Galactic halo stars. The high nitrogen-to-oxygen ratio reported in previous studies can be migrated to the large transmission of the O viii Lyα line. The ionized absorber is characterized by a balance temperature of 0.17-0.20 keV and a column density of 3-5 × 1019 cm-2. Based on the derived abundances and absorption, we speculate that the North Polar Spur is a structure in the Galactic halo, so that the emission is mostly absorbed by the Galactic interstellar medium in the line of sight.

Black Holes in Bulgeless Galaxies: An XMM-Newton Investigation of NGC 3367 AND NGC 4536

Science.gov (United States)

McAlpine, W.; Satyapal, S.; Gliozzi, M.; Cheung, C. C.; Sambruna, R. M.; Eracleous, Michael

2012-01-01

The vast majority of optically identified active galactic nuclei (AGNs) in the local Universe reside in host galaxies with prominent bulges, supporting the hypothesis that black hole formation and growth is fundamentally connected to the build-up of galaxy bulges. However, recent mid-infrared spectroscopic studies with Spitzer of a sample of optically "normal" late-type galaxies reveal remarkably the presence of high-ionization [NeV] lines in several sources, providing strong evidence for AGNs in these galaxies. We present follow-up X-ray observations recently obtained with XMM-Newton of two such sources, the late-type optically normal galaxies NGC 3367 and NGC 4536. Both sources are detected in our observations. Detailed spectral analysis reveals that for both galaxies, the 2-10 keV emission is dominated by a power law with an X-ray luminosity in the L(sub 2- 10 keV) approximates 10(exp 39) - 10(exp 40) ergs/s range, consistent with low luminosity AGNs. While there is a possibility that X-ray binaries account for some fraction of the observed X-ray luminosity, we argue that this fraction is negligible. These observations therefore add to the growing evidence that the fraction of late-type galaxies hosting AGNs is significantly underestimated using optical observations alone. A comparison of the midinfrared [NeV] luminosity and the X-ray luminosities suggests the presence of an additional highly absorbed X-ray source in both galaxies, and that the black hole masses are in the range of 10(exp 5) - 10(exp 7) solar M for NGC 3367 and 10(exp 4) - (exp 10) solar M for NGC 4536

Performance of an optical filter for the XMM focal plane CCD camera EPIC

Science.gov (United States)

Stephan, Karl-Heinz; Reppin, C.; Hirschinger, M.; Maier, H. J.; Frischke, D.; Fuchs, Detlef; Mueller, Peter; Guertler, Peter

1996-10-01

We have been developing optical filters for ESA's x-ray astronomy project XMM (x-ray multi mirror mission). Specific CCDs will be used as detectors in the focal plane on board the observatory. Since these detectors are sensitive from the x-ray to the NIR (near infrared) spectral range, x-ray observations require optical filters, which combine a high transparency for photon energies in the soft x-ray region and a high opacity for UV (ultraviolet) and VIS (visible) radiation as well. With respect to the mission goal in orbit three types of flight model filters are designed having different spectral transmittance functions. We report on one of these types, a so-called 'thick' filter, which has been realized within the EQM (electrical qualification model)- phase of the project. The filter features a cut-off in the EUV (extreme ultraviolet) spectral range and suppresses radiation below 10 eV photon energy by more than 8 orders of magnitude. It has an effective aperture of 73 mm without any support structure. A 0.35 micrometer thick polypropylene carrier foil is coated with metallic films of Al and Sn. The manufacturing process, the qualification measurements and the environmental tests are described, and the resulting performance data is presented.

Soft x-ray transmission measurements on thin films used for XMM CCD-filters

Science.gov (United States)

Stephan, K.-H.; Reppin, C.; Maier, H. J.; Frischke, D.; Fuchs, D.; Müller, P.

1997-02-01

We have been developing optical filters for ESA's X-ray astronomy project XMM (X-ray Multi Mirror Mission). Specific CCDs will be used as detectors in the focal plane on board the observatory (1). Since these detectors are sensitive from the X-ray to the near infrared spectral range, X-ray observations require optical filters, which combine a high transparency for photon energies in the soft X-ray region and a high opacity for ultraviolet and visible radiation as well. With respect to the mission goal in orbit three types of flight model filters are designed having different spectral transmittance functions. We report on one of these types, a so-called "thick" filter, which has been realized within the EQM (Electrical Qualification Model)-phase of the project. The filter features a cut-off in the extreme ultraviolet spectral range and suppresses radiation below ˜10 eV photon energy by more than 8 orders of magnitude. It has an effective aperture of 73 mm without any support structure. A 0.35 μm thick polypropylene carrier foil is coated with metallic films of Al and Sn. We describe transmission measurements in the soft X-ray photon energy range to determine the thickness of the individual layers and present the optical performance data of the filter.

Technologies for Hemostasis and Stabilization of the Acute Traumatic Wound

Science.gov (United States)

2012-10-01

purified fibrinogen from USARMY donated plasma. 6. Generation of purified recombinant activated Factor XIII (rFXIIIA2-a) made from yeast fermentation ...Figure 5. SDS-PAGE of purified recombinant activated Factor XIII, from fermentation of Pichia pastoris. Lane 1: molecular weight marker...fibrinogen (FI) and activated Factor XIII (FXIIIa) were generated in the milk of transgenic cows and in yeast , respectively; human r- thrombin (FIIa

A multi-level quantum mechanics and molecular mechanics study of SN2 reaction at nitrogen: NH2Cl + OH(-) in aqueous solution.

Science.gov (United States)

Lv, Jing; Zhang, Jingxue; Wang, Dunyou

2016-02-17

We employed a multi-level quantum mechanics and molecular mechanics approach to study the reaction NH2Cl + OH(-) in aqueous solution. The multi-level quantum method (including the DFT method with both the B3LYP and M06-2X exchange-correlation functionals and the CCSD(T) method, and both methods with the aug-cc-pVDZ basis set) was used to treat the quantum reaction region in different stages of the calculation in order to obtain an accurate potential of mean force. The obtained free energy activation barriers at the DFT/MM level of theory yielded a big difference of 21.8 kcal mol(-1) with the B3LYP functional and 27.4 kcal mol(-1) with the M06-2X functional respectively. Nonetheless, the barrier heights become very close when shifted from DFT to CCSD(T): 22.4 kcal mol(-1) and 22.9 kcal mol(-1) at CCSD(T)(B3LYP)/MM and CCSD(T)(M06-2X)/MM levels of theory, respectively. The free reaction energy obtained using CCSD(T)(M06-2X)/MM shows an excellent agreement with the one calculated using the available gas-phase data. Aqueous solution plays a significant role in shaping the reaction profile. In total, the water solution contributes 13.3 kcal mol(-1) and 14.6 kcal mol(-1) to the free energy barrier heights at CCSD(T)(B3LYP)/MM and CCSD(T)(M06-2X)/MM respectively. The title reaction at nitrogen is a faster reaction than the corresponding reaction at carbon, CH3Cl + OH(-).

Enhancing the view of a million galaxies

Science.gov (United States)

2004-06-01

Composite image hi-res Size hi-res: 851 KB Credits: ESA/Univ. of Leicester/I. Stewart and M. Watson XMM-Newton X-ray spectral colour composite image XMM-Newton X-ray spectral colour composite image of the Subaru/XMM-Newton Deep Field. The view gives an X-ray pseudo-colour representation of all the sources, coded according to their X-ray energy. More energetic sources are shown in blue and less energetic ones in red. This mosaic image, composed of 7 partially overlapping pointings, maps the full extent of the SXDF and corresponds to an exposure time exceeding one hundred hours. These data form the largest contiguous area over which deep X-ray observations have been performed. Composite image hi-res Size hi-res: 6215 KB Credits: NAOJ/Subaru Telescope XMM-Newton/Subaru colour composite image A colour composite image obtained by combining data taken with the Subaru Telescope in blue, red and near-infrared light. The image, worth over two hundred hours of exposure time, covers an area of sky seven times larger than the full moon. The images in blue light show details several hundred million times fainter than what can be seen with the naked eye. SXDS field hi-res Size hi-res: 448 KB Credits: NAOJ/Subaru Telescope SXDS field A particular of the SXDS field. The teardrop-shaped galaxy in the upper right portion of the frame is likely to have suffered from a collision with another galaxy. SXDS field hi-res Size hi-res: 358 KB Credits: NAOJ/Subaru Telescope SXDS field A particular of the SXDS field. The prominent spiral galaxy near the centre may be ineracting with a less-conspicuous dwarf galaxy to its lower right. One of the fundamental goals of modern astronomy is understanding the history of the Universe, and in particular learning about the processes that shape the formation and evolution of galaxies. To observe these processes as they unfold, astronomers must survey galaxies near and far, spanning a large enough volume of the Universe, so that local variations in the

A Peek into a Cul-De-Sac and a Mews of Martian Dust Storm Activity: Western Hellas and Syria-Claritas Fossae During Mars Year 29

Science.gov (United States)

Heavens, N. G.

2016-12-01

Western Hellas Planitia (WHP) and the region encompassed by Syria Planum and Claritas Fossae are the main centers of textured dust storm activity in Mars's southern low to mid-latitudes. (Texture in this context refers to distinct fine structure at the cloud tops indicative of active lifting.) WHP is a well-known initiation zone for regional and global dust storm activity and often the end point of the Utopia "flushing storm" track. Syria-Claritas Fossae (SCF), too, can be a lifting center in global dust storm activity. Indeed, SCF and the area to its west was the region most denuded of dust by the Mars Year (MY) 25 global dust storm, perhaps suggesting that SCF contained the principal lifting center of the storm. Thus, if the Acidalia and Utopia storm tracks are Mars's dust storm alleys, through which dust storms pass quickly again and again; WHP might be a cul-de-sac and SCF something like a mews, where dust storm activity can enter more or less easily but may not as easily leave. In this presentation, I will focus on dust storm activity in these areas in a typical non-global dust storm year, MY 29. Synthesizing visible imagery by the Mars Color Imager (MARCI) on board Mars Reconnaissance Orbiter (MRO) and Mars Climate Sounder (MCS) also on board MRO, I will consider the climatology, morphology, texture, and vertical structure of dust storm activity in these areas in order to infer their governing dynamics. This investigation has two aims: (1) to understand why these areas are centers of textured dust storm activity; and (2) to connect the characteristics of smaller-scale dust storm activity in these regions to the underlying dynamics in order to understand the role of WHP and SCF in the dynamics of global dust storms. This work is supported by NASA's Mars Data Analysis Program (NNX14AM32G).

Cre/lox Studies Identify Resident Macrophages as the Major Source of Circulating Coagulation Factor XIII-A.

Science.gov (United States)

Beckers, Cora M L; Simpson, Kingsley R; Griffin, Kathryn J; Brown, Jane M; Cheah, Lih T; Smith, Kerrie A; Vacher, Jean; Cordell, Paul A; Kearney, Mark T; Grant, Peter J; Pease, Richard J

2017-08-01

To establish the cellular source of plasma factor (F)XIII-A. A novel mouse floxed for the F13a1 gene, FXIII-A flox/flox (Flox), was crossed with myeloid- and platelet-cre-expressing mice, and cellular FXIII-A mRNA expression and plasma and platelet FXIII-A levels were measured. The platelet factor 4-cre.Flox cross abolished platelet FXIII-A and reduced plasma FXIII-A to 23±3% ( P cre on plasma FXIII-A was exerted outside of the megakaryocyte lineage because plasma FXIII-A was not reduced in the Mpl -/- mouse, despite marked thrombocytopenia. In support of this, platelet factor 4-cre depleted FXIII-A mRNA in brain, aorta, and heart of floxed mice, where FXIII-A pos cells were identified as macrophages as they costained with CD163. In the integrin αM-cre.Flox and the double copy lysozyme 2-cre.cre.Flox crosses, plasma FXIII-A was reduced to, respectively, 75±5% ( P =0.003) and 30±7% ( P <0.001), with no change in FXIII-A content per platelet, further consistent with a macrophage origin of plasma FXIII-A. The change in plasma FXIII-A levels across the various mouse genotypes mirrored the change in FXIII-A mRNA expression in aorta. Bone marrow transplantation of FXIII-A +/+ bone marrow into FXIII-A -/- mice both restored plasma FXIII-A to normal levels and replaced aortic and cardiac FXIII-A mRNA, while its transplantation into FXIII-A +/+ mice did not increase plasma FXIII-A levels, suggesting that a limited population of niches exists that support FXIII-A-releasing cells. This work suggests that resident macrophages maintain plasma FXIII-A and exclude the platelet lineage as a major contributor. © 2017 The Authors.

O moio-medida e o moio dos preços em Portugal nos séculos Xl a XIII

Directory of Open Access Journals (Sweden)

Seabra Lopes, Luis

2005-06-01

Full Text Available In this paper, the value of the modius (modio, moyo, moio in Portugal in the 11th to the 13th centuries is studied. By this time, the modius was both a measure of capacity and a unit used in the specification of prices. The author concludes that, while the modius-measure had a capacity not under the horse charge (210 to 220 litters in the legal systems used in Portugal from the end of the 11th century onwards, some smaller modii continued to be used in rural areas far away from the main urban centers. These smaller modii had a capacity around 50 to 75 litters. With respect to the modius-price, the information gathered by the author indicates a value between 25 and 55 litters of cereal. Therefore, it becomes clear that the modius-price was not equivalent to the standard modius-measure, although it could be equivalent to the smaller modii still in use in rural areas. The gathered evidence also suggests that, from the 10th to the 13th centuries, independently of inflation, the modius-price remained approximately equivalent to the currency unit known as solidus

Neste artigo, estuda-se o valor do moio (modius, modio, moyo em Portugal nos séculos XI a XIII. Nesta época, o moio era simultaneamente uma medida de capacidade e uma unidade usada na especificação dos preços. Este estudo permite concluir que, enquanto o moio-medida tinha, nos sistemas legais em vigor em Portugal a partir de finais do século XI, uma capacidade não inferior à carga de cavalo (210 a 220 litros, alguns moios mais pequenos continuaram a ser utilizados em áreas rurais afastadas dos principais centros urbanos. Estes moios mais pequenos tinham capacidades em torno de 50 a 75 litros. Relativamente ao moi-preço, a informação reunida indica um valor entre 25 e 55 litros de cereal, Torna-se, assim, evidente, que o moio-preço não era equivalente ao moio-medida comum, podendo, no entanto, ser equivalente aos moios menores que ainda sobreviviam nas áreas rurais. A

The DENIS & 2MASS Near Infrared Surveys

OpenAIRE

Mamon, Gary

1996-01-01

The DENIS and 2MASS near infrared surveys are presented. Their applications in extragalactic astronomy and cosmology are listed. The prospects for a rapid spectroscopic followup survey of a near infrared selected sample of nearly $10^5$ galaxies are illustrated with Monte-Carlo simulations.

The cosmological analysis of X-ray cluster surveys - I. A new method for interpreting number counts

Science.gov (United States)

Clerc, N.; Pierre, M.; Pacaud, F.; Sadibekova, T.

2012-07-01

We present a new method aimed at simplifying the cosmological analysis of X-ray cluster surveys. It is based on purely instrumental observable quantities considered in a two-dimensional X-ray colour-magnitude diagram (hardness ratio versus count rate). The basic principle is that even in rather shallow surveys, substantial information on cluster redshift and temperature is present in the raw X-ray data and can be statistically extracted; in parallel, such diagrams can be readily predicted from an ab initio cosmological modelling. We illustrate the methodology for the case of a 100-deg2XMM survey having a sensitivity of ˜10-14 erg s-1 cm-2 and fit at the same time, the survey selection function, the cluster evolutionary scaling relations and the cosmology; our sole assumption - driven by the limited size of the sample considered in the case study - is that the local cluster scaling relations are known. We devote special attention to the realistic modelling of the count-rate measurement uncertainties and evaluate the potential of the method via a Fisher analysis. In the absence of individual cluster redshifts, the count rate and hardness ratio (CR-HR) method appears to be much more efficient than the traditional approach based on cluster counts (i.e. dn/dz, requiring redshifts). In the case where redshifts are available, our method performs similar to the traditional mass function (dn/dM/dz) for the purely cosmological parameters, but constrains better parameters defining the cluster scaling relations and their evolution. A further practical advantage of the CR-HR method is its simplicity: this fully top-down approach totally bypasses the tedious steps consisting in deriving cluster masses from X-ray temperature measurements.

Tres Violantes: las mujeres de una familia en el poder a lo largo del siglo XIII

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Fuente Pérez, María Jesús

2016-06-01

Full Text Available The power of women, in particular the power of queens, has been a topic of great interest to historians, medievalists in particular; though much has been written about the subject, many questions remain. “Three Violantes” will look at the role of two Iberian queens and one Spanish princess in the thirteenth century Iberian kingdoms. In England and in other European kingdoms of that time, queens had lost authority and their agency was limited to the power of intercession and mediation, I will try to determine whether this also holds true for the Iberian queens.El interés por el tema del poder de las mujeres, en particular de las reinas, ha planteado muchos interrogantes sobre la naturaleza de ese poder. “Tres Violantes” examina la participación de dos reinas y una infanta de una misma familia, en aspectos diversos de la vida de las coronas de Aragón y Castilla en el siglo XIII, con el objetivo de apreciar si el papel de las reinas hispanas, en particular su participación política, siguió un camino similar al de las reinas de ese tiempo que, como bien se ha estudiado para las inglesas, fueron perdiendo autoridad y se vieron limitadas a ejercer poder a través de la intercesión y mediación.

Geology of -30247, -35247, and -40247 Quadrangles, Southern Hesperia Planum, Mars

Science.gov (United States)

Mest, S. C.; Crown, D. A.

2010-01-01

Geologic mapping of MTM -30247, -35247, and -40247 quadrangles is being used to characterize Reull Vallis (RV) and examine the roles and timing of volatile-driven erosional and depositional processes. This study complements earlier investigations of the eastern Hellas region, including regional analyses [1-6], mapping studies of circum-Hellas canyons [7-10], and volcanic studies of Hadriaca and Tyrrhena Paterae [11-13]. Key scientific objectives include 1) characterizing RV in its "fluvial zone," and evaluating its history of formation, 2) analyzing channels in the surrounding plains and potential connections to RV, and 3) examining young, possibly sedimentary plains along RV.

THE XMM-NEWTON LONG LOOK OF NGC 1365: LACK OF A HIGH/SOFT STATE IN ITS ULTRALUMINOUS X-RAY SOURCES

International Nuclear Information System (INIS)

Soria, R.; Risaliti, G.; Elvis, M.; Fabbiano, G.; Bianchi, S.; Kuncic, Z.

2009-01-01

Based on our long (∼300 ks) 2007 XMM-Newton observation of the Seyfert galaxy NGC 1365, we report here on the spectral and timing behavior of two ultraluminous X-ray sources (ULXs), which had previously reached isotropic X-ray luminosities L X ∼ 4 x 10 40 erg s -1 (0.3-10 keV band). In 2007, they were in a lower state (L X ∼ 5 x 10 39 and 1.5 x 10 39 erg s -1 for X1 and X2, respectively). Their X-ray spectra were dominated by power laws with photon indices Γ ∼ 1.8 and 1.2, respectively. Thus, their spectra were similar to those at their outburst peaks. Both sources have been seen to vary by a factor of 20 in luminosity over the years, but their spectra are always dominated by a hard power law; unlike most stellar-mass black holes, they have never been found in a canonical high/soft state dominated by a standard disk. The lack of a canonical high/soft state seems to be a common feature of ULXs. We speculate that the different kind of donor star and/or a persistently super-Eddington accretion rate during their outbursts may prevent accretion flows in ULXs from settling into steady standard disks.

EXTraS discovery of a 1.2-s X-ray pulsar in M31

Science.gov (United States)

Esposito, P.; Israel, G.; Belfiore, A.; Novara, G.; Sidoli, L.; Rodriguez Castillo, G.; De Luca, A.; Tiengo, A.; Haberl, F.; Salvaterra, R.

2017-10-01

A systematic search for periodic signals in the XMM-Newton's EPIC archive carried out within the EXTraS project resulted in the discovery of a 1.2-s flux modulation in 3XMM J004301.4+413017. It is the first accreting neutron star in M31 for which the spin period has been detected. Besides this distinction, 3XMM J0043 proved to be an interesting system. Doppler shifts of the spin modulation revealed an orbital motion with period of 1.27 d and the analysis of optical data shows that, while the source is likely associated to a globular cluster, a counterpart with V ˜ 22 outside the cluster cannot be excluded. The emission of the pulsar appears rather hard (most data are described by a power law with photon index <1) and, assuming the distance to M31, the 0.3-10 keV luminosity was variable, from ˜3×10^{37} to 2×10^{38} erg/s. Based on this, we discuss two main possible scenarios for 3X J0043: a peculiar low-mass X-ray binary, perhaps similar to 4U 1822-37 or 4U 1626-67, or an intermediate-mass X-ray binary akin Her X-1.

Finding X-ray counterparts for unidentified sources in the 105 months BAT survey - 1

Science.gov (United States)

Stephen, J. B.; Bassani, L.; Malizia, A.; Masetti, N.; Ubertini, P.

2018-02-01

We provide X-ray counterparts for the unidentified Swift/BAT sources listed in the 105 month catalogue (Oh et al. 2018, ApJS in press). These associations were found by cross-correlating the list of U1,U2 and U3 sources with the ROSAT Bright (RASSBSC, Voges et al. 1999, A & A, 349, 389) and the XMM-Newton Slew (XMMSlew, Saxton et al. 2008, A & A, 480, 611) catalogues.

The MEXSAS2 Sample and the Ensemble X-ray Variability of Quasars

Energy Technology Data Exchange (ETDEWEB)

Serafinelli, Roberto [Dipartimento di Fisica, Università di Roma Tor Vergata, Rome (Italy); Dipartimento di Fisica, Università di Roma Sapienza, Rome (Italy); Vagnetti, Fausto; Chiaraluce, Elia [Dipartimento di Fisica, Università di Roma Tor Vergata, Rome (Italy); Middei, Riccardo, E-mail: roberto.serafinelli@roma2.infn.it [Dipartimento di Matematica e Fisica, Università Roma Tre, Rome (Italy)

2017-10-11

We present the second Multi-Epoch X-ray Serendipitous AGN Sample (MEXSAS2), extracted from the 6th release of the XMM Serendipitous Source Catalog (XMMSSC-DR6), cross-matched with Sloan Digital Sky Survey quasar Catalogs DR7Q and DR12Q. Our sample also includes the available measurements for masses, bolometric luminosities, and Eddington ratios. Analyses of the ensemble structure function and spectral variability are presented, together with their dependences on such parameters. We confirm a decrease of the structure function with the X-ray luminosity, and find a weak dependence on the black hole mass. We introduce a new spectral variability estimator, taking errors on both fluxes and spectral indices into account. We confirm an ensemble softer when brighter trend, with no dependence of such estimator on black hole mass, Eddington ratio, redshift, X-ray and bolometric luminosity.

The XMM Cluster Outskirts Project (X-COP): Thermodynamic properties of the intracluster medium out to R200 in Abell 2319

Science.gov (United States)

Ghirardini, V.; Ettori, S.; Eckert, D.; Molendi, S.; Gastaldello, F.; Pointecouteau, E.; Hurier, G.; Bourdin, H.

2018-06-01

Aims: We present the joint analysis of the X-ray and Sunyaev-Zel'dovich (SZ) signals in Abell 2319, the galaxy cluster with the highest signal-to-noise ratio in SZ Planck maps and that has been surveyed within our XMM-Newton Cluster Outskirts Project (X-COP), a very large program which aims to grasp the physical condition in 12 local (z 3 × 1014 M⊙) galaxy clusters out to R200 and beyond. Methods: We recover the profiles of the thermodynamic properties by the geometrical deprojection of the X-ray surface brightness, of the SZ Comptonization parameter, and accurate and robust spectroscopic measurements of the gas temperature out to 3.2 Mpc (1.6 R200), 4 Mpc (2 R200), and 1.6 Mpc (0.8 R200), respectively. We resolve the clumpiness of the gas density to be below 20% over the entire observed volume. We also demonstrate that most of this clumpiness originates from the ongoing merger and can be associated with large-scale inhomogeneities (the "residual" clumpiness). We estimate the total mass through the hydrostatic equilibrium equation. This analysis is done both in azimuthally averaged radial bins and in eight independent angular sectors, enabling us to study in detail the azimuthal variance of the recovered properties. Results: Given the exquisite quality of the X-ray and SZ datasets, their radial extension, and their complementarity, we constrain at R200 the total hydrostatic mass, modelled with a Navarro-Frenk-White profile at very high precision (M200 = 10.7 ± 0.5stat. ± 0.9syst. × 1014 M⊙). We identify the ongoing merger and how it is affecting differently the gas properties in the resolved azimuthal sectors. We have several indications that the merger has injected a high level of non-thermal pressure in this system: the clumping free density profile is above the average profile obtained by stacking Rosat/PSPC observations; the gas mass fraction recovered using our hydrostatic mass profile exceeds the expected cosmic gas fraction beyond R500; the pressure

Homens de letras e homens de leis ao serviço da monarquia portuguesa (séculos XII-XIII

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Armando Norte

2014-06-01

Full Text Available Ao longo da primeira dinastia, os letrados ao serviço da Coroa portuguesa desempenharam um papel decisivo e cada vez mais importante na afirmação do poder real. Homens de leis e homens de letras serviram à casa real como oficiais, representaram os reis portugueses em atos políticos e diplomáticos e exerceram um grande leque de funções na esfera da administração central - políticas, jurídicas, médicas, económicas, administrativas. A presença desses elementos ao lado dos monarcas fez-se sentir desde a fundação do reino, logo desde o reinado de D. Afonso Henriques, coincidindo o corolário deste processo de recrutamento com a chegada de D. Afonso III ao trono, numa política continuada, de forma firme, por D. Dinis. O conjunto de eruditos recenseados junto dos reis portugueses da época fundacional constitui, nessa medida, um interessante estudo de caso para compreender, em parte, em que consistia um círculo áulico, à luz dos valores do século XII e XIII.

X-ray Luminosity and Absorption Column Fluctuations in the H2O Maser Galaxy NGC 4258 from Weeks to Years

International Nuclear Information System (INIS)

Argon, A.

2004-01-01

The authors report monitoring of the 0.3-10 keV spectrum of NGC 4258 with the XMM-Newton observatory at five epochs over 1.5 years. They also report reprocessing of an overlapping four epoch series of archival Chandra observations (0.5-10 keV). By including earlier ASCA and Beppo-SAX observations, they present a new, nine year time-series of models fit to the X-ray spectrum of NGC 4258. They model the Chandra and XMM-Newton data self-consistently with partially absorbed, hard power-law, soft thermal plasma, and soft power-law components. Over the nine years, the photo-electric absorbing column (∼ 10 23 cm -2 ) did not vary detectably, except for a ∼ 40% drop between two ASCA epochs separated by 3 years (in 1993 and 1996) and a ∼ 60% rise between two XMM-Newton epochs separated by just 5 months (in 2001 and 2002). In contrast, factor of 2-3 changes are seen in absorbed flux on the timescale of years. These are uncorrelated with changes in absorbing column and indicative of central engine variability. The most rapid change in luminosity (5-10 keV) that the authors detect (with XMM-Newton and Chandra) is on the order of 30% over 19 days. The warped disk that is a known source of H 2 O maser emission in NGC 4258 is believed to cross the line of sight to the central engine. They propose that the variations in absorbing column arise from inhomogeneities in the rotating disk, as they sweep across the line of sight. They estimate that the inhomogeneities are ∼ 10 15 cm in size

X-ray and optical substructures of the DAFT/FADA survey clusters

Science.gov (United States)

Guennou, L.; Durret, F.; Adami, C.; Lima Neto, G. B.

2013-04-01

We have undertaken the DAFT/FADA survey with the double aim of setting constraints on dark energy based on weak lensing tomography and of obtaining homogeneous and high quality data for a sample of 91 massive clusters in the redshift range 0.4-0.9 for which there were HST archive data. We have analysed the XMM-Newton data available for 42 of these clusters to derive their X-ray temperatures and luminosities and search for substructures. Out of these, a spatial analysis was possible for 30 clusters, but only 23 had deep enough X-ray data for a really robust analysis. This study was coupled with a dynamical analysis for the 26 clusters having at least 30 spectroscopic galaxy redshifts in the cluster range. Altogether, the X-ray sample of 23 clusters and the optical sample of 26 clusters have 14 clusters in common. We present preliminary results on the coupled X-ray and dynamical analyses of these 14 clusters.

Probing for Pulsars: An XMM Study of the Composite SNRS G327.1-1.1 and CTA1

Science.gov (United States)

Slane, Patrick; Mushotzky, Richard F. (Technical Monitor)

2003-01-01

The subject grant is for analysis of XMM data from the supernova remnant CTA1. Our investigation centered on the study of the compact source Rx 50007.0+7302 that, based on our previous observations, appears to be a neutron star powering a wind nebula in the remnant interior. This compact source has also been suggested as the counterpart of the EGRET source 2EG J0008+7307. The analysis of the data from the compact source is complete. We find that the spectrum of the source is well described by a power law with the addition of a soft thermal component that may correspond to emission from hot polar cap regions or to cooling emission from a light element atmosphere over the entire star. There is evidence of extended emission on small spatial scales which may correspond to structure in the underlying synchrotron nebula. Extrapolation of the nonthermal emission component to gamma-ray energies yields a flux that is consistent with that of 2EG J0008+7307, thus strengthening the proposition that there is a gamma-ray emitting pulsar at the center of CTA 1. Our timing studies with the EPIC pn data revealed no evidence for pulsations, however; we set an upper limit of 61% on the pulsed fraction from this source. The results from this study were presented in a poster at the recent IAU Symposium in Sydney, Australia. A paper summarizing these results, entitled "Xray Observations of the Compact Source in CTA 1" (Slane et al.) has been submitted for publication in the Astrophysical Journal.

Y2K Survey Results: Counties, Cities, School Districts.

Science.gov (United States)

Petro, Jim

Survey data obtained in recent audits updated Ohio's local government units' assessment of Year 2000 (Y2K) readiness. The survey was developed with three intended objectives: (1) to provide an accurate assessment of the efforts to remediate the Y2K problem in Ohio's school districts, cities and counties; (2) to identify issues that could affect…

Deep Chandra Survey of the Small Magellanic Cloud. II. Timing Analysis of X-Ray Pulsars

Energy Technology Data Exchange (ETDEWEB)

Hong, JaeSub; Antoniou, Vallia; Zezas, Andreas; Drake, Jeremy J.; Plucinsky, Paul P. [Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (United States); Haberl, Frank [Max-Planck-Institut für extraterrestrische Physik, Giessenbach straße, D-85748 Garching (Germany); Sasaki, Manami [Friedrich-Alexander-Universität Erlangen-Nürnberg, Sternwartstrasse 7, 96049 Bamberg (Germany); Laycock, Silas, E-mail: jaesub@head.cfa.harvard.edu [Department of Physics, University of Massachusetts Lowell, MA 01854 (United States)

2017-09-20

We report the timing analysis results of X-ray pulsars from a recent deep Chandra survey of the Small Magellanic Cloud (SMC). We analyzed a total exposure of 1.4 Ms from 31 observations over a 1.2 deg{sup 2} region in the SMC under a Chandra X-ray Visionary Program. Using the Lomb–Scargle and epoch-folding techniques, we detected periodic modulations from 20 pulsars and a new candidate pulsar. The survey also covered 11 other pulsars with no clear sign of periodic modulation. The 0.5–8 keV X-ray luminosity ( L {sub X} ) of the pulsars ranges from 10{sup 34} to 10{sup 37} erg s{sup −1} at 60 kpc. All of the Chandra sources with L {sub X} ≳ 4 × 10{sup 35} erg s{sup −1} exhibit X-ray pulsations. The X-ray spectra of the SMC pulsars (and high-mass X-ray binaries) are in general harder than those of the SMC field population. All but SXP 8.02 can be fitted by an absorbed power-law model with a photon index of Γ ≲ 1.5. The X-ray spectrum of the known magnetar SXP 8.02 is better fitted with a two-temperature blackbody model. Newly measured pulsation periods of SXP 51.0, SXP 214, and SXP 701, are significantly different from the previous XMM-Newton and RXTE measurements. This survey provides a rich data set for energy-dependent pulse profile modeling. Six pulsars show an almost eclipse-like dip in the pulse profile. Phase-resolved spectral analysis reveals diverse spectral variations during pulsation cycles: e.g., for an absorbed power-law model, some exhibit an (anti)-correlation between absorption and X-ray flux, while others show more intrinsic spectral variation (i.e., changes in photon indices).

A combined HST and XMM-Newton campaign for the magnetic O9.7 V star HD 54879. Constraining the weak-wind problem of massive stars

Science.gov (United States)

Shenar, T.; Oskinova, L. M.; Järvinen, S. P.; Luckas, P.; Hainich, R.; Todt, H.; Hubrig, S.; Sander, A. A. C.; Ilyin, I.; Hamann, W.-R.

2017-10-01

Context. HD 54879 (O9.7 V) is one of a dozen O-stars for which an organized atmospheric magnetic field has been detected. Despite their importance, little is known about the winds and evolution of magnetized massive stars. Aims: To gain insights into the interplay between atmospheres, winds, and magnetic fields of massive stars, we acquired UV and X-ray data of HD 54879 using the Hubble Space Telescope and the XMM-Newton satellite. In addition, 35 optical amateur spectra were secured to study the variability of HD 54879. Methods: A multiwavelength (X-ray to optical) spectral analysis is performed using the Potsdam Wolf-Rayet (PoWR) model atmosphere code and the xspec software. Results: The photospheric parameters (T∗ = 30.5 kK, log g = 4.0 [cm s-2], log L = 4.45 [L⊙]) are typical for an O9.7 V star. The microturbulent, macroturbulent, and projected rotational velocities are lower than previously suggested (ξph,vmac,vsini ≤ 4 km s-1). An initial mass of 16 M⊙ and an age of 5 Myr are inferred from evolutionary tracks. We derive a mean X-ray emitting temperature of log TX = 6.7 [K] and an X-ray luminosity of LX = 1 × 1032 erg s-1. Short- and long-scale variability is seen in the Hα line, but only a very long period of P ≈ 5 yr could be estimated. Assessing the circumstellar density of HD 54879 using UV spectra, we can roughly estimate the mass-loss rate HD 54879 would have in the absence of a magnetic field as log ṀB = 0 ≈ -9.0 [M⊙ yr-1]. The magnetic field traps the stellar wind up to the Alfvén radius rA ≳ 12 R∗, implying that its true mass-loss rate is log Ṁ ≲ -10.2 [M⊙ yr-1]. Hence, density enhancements around magnetic stars can be exploited to estimate mass-loss rates of non-magnetic stars of similar spectral types, essential for resolving the weak wind problem. Conclusions: Our study confirms that strongly magnetized stars lose little or no mass, and supplies important constraints on the weak-wind problem of massive main sequence

A deep X-ray view of the bare AGN Ark 120. IV. XMM-Newton and NuSTAR spectra dominated by two temperature (warm, hot) Comptonization processes

Science.gov (United States)

Porquet, D.; Reeves, J. N.; Matt, G.; Marinucci, A.; Nardini, E.; Braito, V.; Lobban, A.; Ballantyne, D. R.; Boggs, S. E.; Christensen, F. E.; Dauser, T.; Farrah, D.; Garcia, J.; Hailey, C. J.; Harrison, F.; Stern, D.; Tortosa, A.; Ursini, F.; Zhang, W. W.

2018-01-01

Context. The physical characteristics of the material closest to supermassive black holes (SMBHs) are primarily studied through X-ray observations. However, the origins of the main X-ray components such as the soft X-ray excess, the Fe Kα line complex, and the hard X-ray excess are still hotly debated. This is particularly problematic for active galactic nuclei (AGN) showing a significant intrinsic absorption, either warm or neutral, which can severely distort the observed continuum. Therefore, AGN with no (or very weak) intrinsic absorption along the line of sight, so-called "bare AGN", are the best targets to directly probe matter very close to the SMBH. Aims: We perform an X-ray spectral analysis of the brightest and cleanest bare AGN known so far, Ark 120, in order to determine the process(es) at work in the vicinity of the SMBH. Methods: We present spectral analyses of data from an extensive campaign observing Ark 120 in X-rays with XMM-Newton (4 × 120 ks, 2014 March 18-24), and NuSTAR (65.5 ks, 2014 March 22). Results: During this very deep X-ray campaign, the source was caught in a high-flux state similar to the earlier 2003 XMM-Newton observation, and about twice as bright as the lower-flux observation in 2013. The spectral analysis confirms the "softer when brighter" behavior of Ark 120. The four XMM-Newton/pn spectra are characterized by the presence of a prominent soft X-ray excess and a significant Fe Kα complex. The continuum is very similar above about 3 keV, while significant variability is present for the soft X-ray excess. We find that relativistic reflection from a constant-density, flat accretion disk cannot simultaneously produce the soft excess, broad Fe Kα complex, and hard X-ray excess. Instead, Comptonization reproduces the broadband (0.3-79 keV) continuum well, together with a contribution from a mildly relativistic disk reflection spectrum. Conclusions: During this 2014 observational campaign, the soft X-ray spectrum of Ark 120 below 0

Alometría y dimorfismo sexual del fémur de Homo sapiens y Homo neanderthalensis en un contexto evolutivo

OpenAIRE

Anaya García, Noelia; Rosas, Antonio; Bastir, Markus; Estalrrich, Almudena; García-Tabernero, Antonio; Huguet, Rosa; Rasilla, Marco de la; Pastor, Francisco

2015-01-01

Comunicación presentada en el XIII Encuentro en Jóvenes Investigadores en Paleontología (XIII EJIP) - XIII Meeting of Early-Stage Researchers in Paleontology (XIII EJIP): Cercedilla, 15 - 18 de Abril de 2015

A new window to an old world: reconstructing the Middle Eocene of Messel for Hessisches Landesmuseum Darmstadt

OpenAIRE

Sanisidro, Óscar; Micklich, Norbert; Sandrock, Oliver

2015-01-01

Comunicación presentada en el XIII Encuentro en Jóvenes Investigadores en Paleontología (XIII EJIP) - XIII Meeting of Early-Stage Researchers in Paleontology (XIII EJIP): Cercedilla, 15 - 18 de Abril de 2015

Synthesis of 2-[4-(10H-Substituted Phenothiazine-3-yl-6-Pyrimidin-2-Phenylthiol/ol/amine/thiol] Pyrroles

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Meghasham Narule

2007-01-01

Full Text Available 2-[4-Hydroxy benz-1(propene-1-one]Pyrrole II on treatment with phenyl thiourea, guanidine carbonate, urea and thiourea in alcoholic KOH yielded compounds III, IV, V, VI which on treatment with different aryl anilines gave compounds VII, VIII, IX, X which under goes cyclisation with sulphur and iodine to give 2-[4-(10H-substituted phenothiazine-3-yl-6-pyrimidin-2-phenylthiol/-ol/-amine/-thiol] pyrrole XI(a-j, XII(a-j, XIII(a-j and XIV(a-j respectively. The structural products were characterized by elemental analysis and spectral data.

XMM-Newton Detection of Hard X-Ray Emission in the Nitrogen-Type Wolf-Rayet Star WR 110

Science.gov (United States)

Skinner, Stephen L.; Zhekov, Svetozar A.; Güdel, Manuel; Schmutz, Werner

2002-06-01

We have used the excellent sensitivity of XMM-Newton to obtain the first high-quality X-ray spectrum of a Wolf-Rayet (W-R) star that is not known to be a member of a binary system. Our target, the nitrogen-type star WR 110 (HD 165688), was also observed and detected with the Very Large Array at four different frequencies. The radio flux density increases with frequency according to a power law Sν~ν+0.64+/-0.10, in very good agreement with the behavior expected for free-free wind emission. The radio data give an ionized mass-loss rate M=4.9×10-5 Msolar yr-1 for an assumed spherical constant-velocity wind. The undispersed CCD X-ray spectra reveal strong emission lines from He-like ions of Mg, Si, and S. The emission measure distribution shows a dominant contribution from cool plasma with a characteristic temperature kTcool~0.5 keV (~6 MK). Little or no excess absorption of this cool component above the value expected from the visual extinction is present. We conclude that the bulk of the cool plasma detected by XMM-Newton lies at hundreds of stellar radii or more if the wind is approximately spherical and homogeneous, but it could lie closer to the star if the wind is clumped. If the cool plasma is due to instability-driven wind shocks, then typical shock velocities are vs~340-550 km s-1 and the average filling factor of X-ray-emitting gas in the wind is no larger than f~10-6. A surprising result is the unambiguous detection of a hard X-ray component that is clearly seen in the hard-band images and the spectra. This hard component accounts for about half of the observed flux and can be acceptably fitted by a hot, optically thin thermal plasma or a power-law model. If the emission is thermal, then a temperature kThot>=3 keV is derived. Such high temperatures are not predicted by current instability-driven wind shock models, and a different mechanism is thus required to explain the hard X-rays. We examine several possible mechanisms and show that the hard emission

RESEÑA de : López Villalba, José Miguel. Las finanzas de un concejo castellano: Piedrahíta, siglos xv–xvii. Estudio y documentos. Volumen XIII (1521–1522. Ávila: Ediciones de la Institución Gran Duque de Alba de la Excma. Diputación Provincial de Ávila.

Directory of Open Access Journals (Sweden)

Pedro Luis Lorenzo Cadarso

2015-06-01

Full Text Available RESEÑA de : López Villalba, José Miguel. Las finanzas de un concejo castellano: Piedrahíta, siglos xv–xvii. Estudio y documentos. Volumen XIII (1521–1522. Ávila: Ediciones de la Institución Gran Duque de Alba de la Excma. Diputación Provincial de Ávila.

The MEXSAS2 Sample and the Ensemble X-ray Variability of Quasars

Directory of Open Access Journals (Sweden)

Roberto Serafinelli

2017-10-01

Full Text Available We present the second Multi-Epoch X-ray Serendipitous AGN Sample (MEXSAS2, extracted from the 6th release of the XMM Serendipitous Source Catalog (XMMSSC-DR6, cross-matched with Sloan Digital Sky Survey quasar Catalogs DR7Q and DR12Q. Our sample also includes the available measurements for masses, bolometric luminosities, and Eddington ratios. Analyses of the ensemble structure function and spectral variability are presented, together with their dependences on such parameters. We confirm a decrease of the structure function with the X-ray luminosity, and find a weak dependence on the black hole mass. We introduce a new spectral variability estimator, taking errors on both fluxes and spectral indices into account. We confirm an ensemble softer when brighter trend, with no dependence of such estimator on black hole mass, Eddington ratio, redshift, X-ray and bolometric luminosity.

The NuSTAR Serendipitous Survey: Hunting for the Most Extreme Obscured AGN at >10 keV

Science.gov (United States)

Lansbury, G. B.; Alexander, D. M.; Aird, J.; Gandhi, P.; Stern, D.; Koss, M.; Lamperti, I.; Ajello, M.; Annuar, A.; Assef, R. J.; Ballantyne, D. R.; Baloković, M.; Bauer, F. E.; Brandt, W. N.; Brightman, M.; Chen, C.-T. J.; Civano, F.; Comastri, A.; Del Moro, A.; Fuentes, C.; Harrison, F. A.; Marchesi, S.; Masini, A.; Mullaney, J. R.; Ricci, C.; Saez, C.; Tomsick, J. A.; Treister, E.; Walton, D. J.; Zappacosta, L.

2017-09-01

We identify sources with extremely hard X-ray spectra (I.e., with photon indices of {{Γ }}≲ 0.6) in the 13 deg2 NuSTAR serendipitous survey, to search for the most highly obscured active galactic nuclei (AGNs) detected at > 10 {keV}. Eight extreme NuSTAR sources are identified, and we use the NuSTAR data in combination with lower-energy X-ray observations (from Chandra, Swift XRT, and XMM-Newton) to characterize the broadband (0.5-24 keV) X-ray spectra. We find that all of the extreme sources are highly obscured AGNs, including three robust Compton-thick (CT; {N}{{H}}> 1.5× {10}24 cm-2) AGNs at low redshift (z< 0.1) and a likely CT AGN at higher redshift (z = 0.16). Most of the extreme sources would not have been identified as highly obscured based on the low-energy (< 10 keV) X-ray coverage alone. The multiwavelength properties (e.g., optical spectra and X-ray-mid-IR luminosity ratios) provide further support for the eight sources being significantly obscured. Correcting for absorption, the intrinsic rest-frame 10-40 keV luminosities of the extreme sources cover a broad range, from ≈ 5× {10}42 to 1045 erg s-1. The estimated number counts of CT AGNs in the NuSTAR serendipitous survey are in broad agreement with model expectations based on previous X-ray surveys, except for the lowest redshifts (z< 0.07), where we measure a high CT fraction of {f}{CT}{obs}={30}-12+16 % . For the small sample of CT AGNs, we find a high fraction of galaxy major mergers (50% ± 33%) compared to control samples of “normal” AGNs.

12 CFR 1732.2 - Definitions.

Science.gov (United States)

2010-01-01

...) Act means the Federal Housing Enterprises Financial Safety and Soundness Act of 1992, Title XIII of...) Users are allowed to communicate under specified conditions; and (4) Messages are held in storage until... (e.g., e-mail, databases, spreadsheets, PowerPoint presentations, electronic reporting systems...

Venezuela-MEM/USA-DOE Fossil Energy Report XIII-1, Supporting Technology for Enhanced Oil Recovery, Microbial EOR

Energy Technology Data Exchange (ETDEWEB)

Ziritt, Jose Luis

1999-11-03

The results from Annex XIII of the Cooperative Agreement between the United States Department of Energy (DOE) and the Ministry of Energy and Mines of the Republic of Venezuela (MEMV) have been documented and published with many researchers involved. Integrate comprehensive research programs in the area of Microbial Enhanced Oil Recovery (MEOR) ranged from feasibility laboratory studies to full-scale multi-well field pilots. The objective, to cooperate in a technical exchange of ideas and information was fully met throughout the life of the Annex. Information has been exchanged between the two countries through published reports and technical meetings between experts in both country's research communities. The meetings occurred every two years in locations coincident with the International MEOR conferences & workshops sponsored by DOE (June 1990, University of Oklahoma, September 1992, Brookhaven, September 1995, National Institute of Petroleum and Energy Research). Reports and publications produced during these years are listed in Appendix B. Several Annex managers have guided the exchange through the years. They included Luis Vierma, Jose Luis Zirritt, representing MEMV and E. B. Nuckols, Edith Allison, and Rhonda Lindsey, representing the U.S. DOE. Funding for this area of research remained steady for a few years but decreased in recent years. Because both countries have reduced research programs in this area, future exchanges on this topic will occur through ANNEX XV. Informal networks established between researchers through the years should continue to function between individuals in the two countries.

Review of Brookhaven nuclear transparency measurements in (p,2p ...

Indian Academy of Sciences (India)

In this contribution we summarize the results of two experiments to measure ... Nuclear; color transparency; protons; alternating gradient synchrotron; large angle. ..... Proceedings of the XIII International Symposium on Multi-particle Dynamics.

1980 Annual status report: utilization of research results

International Nuclear Information System (INIS)

1981-01-01

Patents and licences were part of normal JRC activity since its origin: the new feature of this programme is that through an increased JRC activity in this field as well as a structured support to D.G. XIII, the process of utilization can be started at an earlier stage, with the deliberate purpose of achieving practical results as early as possible, through an adequate R and D effort. Key element of this process is the systematic identification, within JRC programme, of those research areas, concepts, ideas, that might present interest for industry and for the public sector. In this respect D.G. XIII by its market survey and contacts with industry is providing JRC with the essential information to carry out this programme

Verslag: �Society of Biblical Literature (SBL 1989 International Meeting�, 6 tot 9 Augustus 1989 te Kopenhagen, Denemarke; en �The XIII Congress of the International Organization for the study of the Old Testament (IOSOT�, 27 Augustus tot 1 September 19

Directory of Open Access Journals (Sweden)

W. S. Prinsloo

1990-08-01

Full Text Available "Society of Biblical Literature (SBL 1989 International Meeting". 6-9 August 1989, Copenhagen, Denmark; and "The XIII Congress of the International Organization for the study of the Old Testament (IOSOT". 27 August to 1 September 1989, Leuven, Belgium This article is a report on the IOSOT Congress at Leuven. Belgium, and the SBL Congress in Copenhagen, Denmark. It contains brief summaries of the more important papers read and indicates some of the more significant trends which emerged at the two congresses.

Peering through the dust: NuSTAR observations of two first-2MASS red quasars

DEFF Research Database (Denmark)

LaMassa, Stephanie M.; Ricarte, Angelo; Glikman, Eilat

2016-01-01

through this gas and dust, revealing the properties of circumnuclear obscuration. Here, we present NuSTAR and XMM-Newton/Chandra observations of FIRST-2MASS-selected red quasars F2M 0830+3759 and F2M 1227+3214. We find that though F2M 0830+3759 is moderately obscured (NH,Z = (2.1 ± 0.2) ×  1022 cm−2...

The Carnegie-Spitzer-IMACS redshift survey of galaxy evolution since z = 1.5. I. Description and methodology

Energy Technology Data Exchange (ETDEWEB)

Kelson, Daniel D.; Williams, Rik J.; Dressler, Alan; McCarthy, Patrick J.; Shectman, Stephen A.; Mulchaey, John S.; Villanueva, Edward V.; Crane, Jeffrey D.; Quadri, Ryan F. [The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101 (United States)

2014-03-10

We describe the Carnegie-Spitzer-IMACS (CSI) Survey, a wide-field, near-IR selected spectrophotometric redshift survey with the Inamori Magellan Areal Camera and Spectrograph (IMACS) on Magellan-Baade. By defining a flux-limited sample of galaxies in Spitzer Infrared Array Camera 3.6 μm imaging of SWIRE fields, the CSI Survey efficiently traces the stellar mass of average galaxies to z ∼ 1.5. This first paper provides an overview of the survey selection, observations, processing of the photometry and spectrophotometry. We also describe the processing of the data: new methods of fitting synthetic templates of spectral energy distributions are used to derive redshifts, stellar masses, emission line luminosities, and coarse information on recent star formation. Our unique methodology for analyzing low-dispersion spectra taken with multilayer prisms in IMACS, combined with panchromatic photometry from the ultraviolet to the IR, has yielded high-quality redshifts for 43,347 galaxies in our first 5.3 deg{sup 2} of the SWIRE XMM-LSS field. We use three different approaches to estimate our redshift errors and find robust agreement. Over the full range of 3.6 μm fluxes of our selection, we find typical redshift uncertainties of σ {sub z}/(1 + z) ≲ 0.015. In comparisons with previously published spectroscopic redshifts we find scatters of σ {sub z}/(1 + z) = 0.011 for galaxies at 0.7 ≤ z ≤ 0.9, and σ {sub z}/(1 + z) = 0.014 for galaxies at 0.9 ≤ z ≤ 1.2. For galaxies brighter and fainter than i = 23 mag, we find σ {sub z}/(1 + z) = 0.008 and σ {sub z}/(1 + z) = 0.022, respectively. Notably, our low-dispersion spectroscopy and analysis yields comparable redshift uncertainties and success rates for both red and blue galaxies, largely eliminating color-based systematics that can seriously bias observed dependencies of galaxy evolution on environment.

Synthesis of some new thiophene and thiopyrimidine compounds of expected anticancer activity and studying the augmenting effect of gamma radiation

International Nuclear Information System (INIS)

Zaher, N.H.M.

2010-01-01

The present investigation comprises a survey on the synthesis of, thiophene, thieno[2,3-d]pyrimidines, triazolothieno[2,3-d]-pyrimidines, thiadiazolothieno[2,3-d]pyrimidines. The thesis involves the synthesis of the following reported starting and intermediate compounds needed for the synthesis of the new intermediates and final compounds: Diethyl 5-amino-3-methylthiophene-2,4-dicarboxylate (I).+ Diethyl-5-isothiocyanato-3-methylthiophene-2,4-dicarboxylate (II) Diethyl 5-(hydrazinecarbothioamido)-3-methylthiophene-2,4- dicarboxylate (XI). Potassium 3-amino-6-(ethoxycarbonyl)-5-methyl-4-oxo-3,4- dihydrothieno[2,3-d]pyrimidine-2-thiolate (XII). .. Ethyl 3-amino-5-methyl-4-oxo-2-sulfanyl-1,2,3,4-tetrahydrothieno[ 2,3-d]pyrimidine-6-carboxylate (XIII) Ethyl 5-amino-4-cyano-3-methylthiophene-2-carboxylate (XXV). Diethyl 5-isothiocyanato-3-methylthiophene-2,4-dicarboxylate (II) was synthesized by thiophosogenation of diethyl 5-amino-3-methylthiophene- 2,4-dicarboxylate (I). Ethyl 3-amino-5-methyl-4-oxo-2-sulfanyl-1,2,3,4-tetrahydrothieno[ 2,3-d]pyrimidine-6-carboxylate (XIII) was prepared by reacting (II) with hydrazine hydrate in dichloromethane at room temperature. The new potassium salt (XII) was obtained by heating diethyl 5-(hydrazinecarbothioamido)- 3-methylthiophene-2,4-dicarboxylate (XI) in an ethanolic potassium hydroxide solution. Acidification of an aqueous solution of potassium 3-amino-6-(ethoxycarbonyl)-5-methyl-4-oxo-3,4- dihydrothieno[2,3-d]pyrimidine-2-thiolate (XII) gave the sulfanyl-Namino substituted thienopyrimidine compound (XIII). Ethyl 5-amino-4-cyano-3-methylthiophene-2-carboxylate (XXV) was synthesized by the reaction of ethylacetoacetate, sulfur, malononitrile and diethylamine in ethanol stirred in ice bath. Ethyl 4-cyano-5- ethoxymethylene amino-3-methylthiophene-2-carboxylate, (XXVI) a VI new intermediate was obtained upon the nucleophilic reaction of (XXV) with triethylorthoformate in acetic anhydride. The reaction of (XXVI) with hydrazine

THE X-RAY PROPERTIES OF THE OPTICALLY BRIGHTEST MINI-BAL QUASARS FROM THE SLOAN DIGITAL SKY SURVEY

International Nuclear Information System (INIS)

Wu Jianfeng; Brandt, W. N.; Comins, M. L.; Garmire, Gordon P.; Schneider, Donald P.; Gibson, Robert R.; Shemmer, Ohad

2010-01-01

We have compiled a sample of 14 of the optically brightest radio-quiet quasars (m i ≤ 17.5 and z ≥ 1.9) in the Sloan Digital Sky Survey Data Release 5 quasar catalog that have C IV mini-broad absorption lines (mini-BALs) present in their spectra. X-ray data for 12 of the objects were obtained via a Chandra snapshot survey using ACIS-S, while data for the other two quasars were obtained from archival XMM-Newton observations. Joint X-ray spectral analysis shows that the mini-BAL quasars have a similar average power-law photon index (Γ ∼ 1.9) and level of intrinsic absorption (N H ∼ 21 cm -2 ) as non-BMB (neither BAL nor mini-BAL) quasars. Mini-BAL quasars are more similar to non-BMB quasars than to BAL quasars in their distribution of relative X-ray brightness (assessed with Δα ox ). Relative colors indicate mild dust reddening in the optical spectra of mini-BAL quasars. Significant correlations between Δα ox and UV absorption properties are confirmed for a sample of 56 sources combining mini-BAL and BAL quasars with high signal-to-noise ratio rest-frame UV spectra, which generally supports models in which X-ray absorption is important in enabling driving of the UV absorption-line wind. We also propose alternative parameterizations of the UV absorption properties of mini-BAL and BAL quasars, which may better describe the broad absorption troughs in some respects.

PRIMUS: INFRARED AND X-RAY AGN SELECTION TECHNIQUES AT 0.2 < z < 1.2

Energy Technology Data Exchange (ETDEWEB)

Mendez, Alexander J.; Coil, Alison L.; Aird, James; Diamond-Stanic, Aleksandar M. [Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Dr., La Jolla, San Diego, CA 92093 (United States); Moustakas, John [Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211 (United States); Blanton, Michael R. [Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003 (United States); Cool, Richard J. [Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Eisenstein, Daniel J. [Harvard College Observatory, 60 Garden St., Cambridge, MA 02138 (United States); Wong, Kenneth C. [Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721 (United States); Zhu Guangtun [Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218 (United States)

2013-06-10

We present a study of Spitzer/IRAC and X-ray active galactic nucleus (AGN) selection techniques in order to quantify the overlap, uniqueness, contamination, and completeness of each. We investigate how the overlap and possible contamination of the samples depend on the depth of both the IR and X-ray data. We use Spitzer/IRAC imaging, Chandra and XMM-Newton X-ray imaging, and spectroscopic redshifts from the PRism MUlti-object Survey to construct galaxy and AGN samples at 0.2 < z < 1.2 over 8 deg{sup 2}. We construct samples over a wide range of IRAC flux limits (SWIRE to GOODS depth) and X-ray flux limits (10 ks to 2 Ms). We compare IR-AGN samples defined using both the IRAC color selection of Stern et al. and Donley et al. with X-ray-detected AGN samples. For roughly similar depth IR and X-ray surveys, we find that {approx}75% of IR-selected AGNs are also identified as X-ray AGNs. This fraction increases to {approx}90% when comparing against the deepest X-ray data, indicating that at most {approx}10% of IR-selected AGNs may be heavily obscured. The IR-AGN selection proposed by Stern et al. suffers from contamination by star-forming galaxies at various redshifts when using deeper IR data, though the selection technique works well for shallow IR data. While similar overall, the IR-AGN samples preferentially contain more luminous AGNs, while the X-ray AGN samples identify a wider range of AGN accretion rates including low specific accretion rate AGNs, where the host galaxy light dominates at IR wavelengths. The host galaxy populations of the IR and X-ray AGN samples have similar rest-frame colors and stellar masses; both selections identify AGNs in blue, star-forming and red, quiescent galaxies.

AN INFRARED/X-RAY SURVEY FOR NEW MEMBERS OF THE TAURUS STAR-FORMING REGION

International Nuclear Information System (INIS)

Luhman, K. L.; Allen, P. R.; Mamajek, E. E.; 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 distribution, which indicates that it could be in the protostellar class I stage (star+disk+envelope). Upon inspection of archival images from various observatories, we find that one of the new young stars has a large edge-on disk (r = 2.''5 = 350 AU). The scattered light from this disk has undergone significant variability on a timescale of days in optical images from the Canada-France-Hawaii Telescope. Using the updated census of Taurus, we have measured the initial mass function for the fields observed by XMM-Newton. The resulting mass function is similar to previous ones that we have reported for Taurus, showing a surplus of stars at spectral types of K7-M1 (0.6-0.8 M sun ) relative to other nearby star-forming regions, such as IC 348, Chamaeleon I, and the Orion Nebula Cluster.

Venezuela-MEM/USA-DOE Fossil Energy Report XIII-1, Supporting Technology for Enhanced Oil Recovery, Microbial EOR; FINAL

International Nuclear Information System (INIS)

Ziritt, Jose Luis

1999-01-01

The results from Annex XIII of the Cooperative Agreement between the United States Department of Energy (DOE) and the Ministry of Energy and Mines of the Republic of Venezuela (MEMV) have been documented and published with many researchers involved. Integrate comprehensive research programs in the area of Microbial Enhanced Oil Recovery (MEOR) ranged from feasibility laboratory studies to full-scale multi-well field pilots. The objective, to cooperate in a technical exchange of ideas and information was fully met throughout the life of the Annex. Information has been exchanged between the two countries through published reports and technical meetings between experts in both country's research communities. The meetings occurred every two years in locations coincident with the International MEOR conferences and workshops sponsored by DOE (June 1990, University of Oklahoma, September 1992, Brookhaven, September 1995, National Institute of Petroleum and Energy Research). Reports and publications produced during these years are listed in Appendix B. Several Annex managers have guided the exchange through the years. They included Luis Vierma, Jose Luis Zirritt, representing MEMV and E. B. Nuckols, Edith Allison, and Rhonda Lindsey, representing the U.S. DOE. Funding for this area of research remained steady for a few years but decreased in recent years. Because both countries have reduced research programs in this area, future exchanges on this topic will occur through ANNEX XV. Informal networks established between researchers through the years should continue to function between individuals in the two countries

Castillos, poder feudal y reorganización espacial en la Transierra madrileña (siglos XII-XIII

Directory of Open Access Journals (Sweden)

Iñaki Martín Viso

2000-01-01

Full Text Available Algunos castillos de la Transierra madrileña en los siglos xii y xiii son herederos de los husün musulmanes, pero se convierten en esa época en centros de poder señorial sobre unas débiles comunidades. No obstante, sólo su transformación en concejos permitirá la supervivencia de algunos de ellos, aunque se observa también un desplazamiento del habitat hacia el llano, resultado de la formación de un nuevo sistema productivo basado en la agricultura cerealfstica y la propiedad feudal, por lo que el papel de los castillos es limitado. En las zonas serranas su relevancia es aún menor y nunca estructuraron el paisaje, labor que ejercieran los sexmos de la Tierra de Segovia.Some castles of the Madrid's Transierra in the xii"" and xiif" centuries are inheritors of the muslim husün, but they viere converted during this age in centres of a lordship power which was imposed to the weak communities. However, only some of them could survive through their conversión In town counciis (concejos, although there is also an habitat's displacement to the plain, that is the result of the new producing system based on the grain agrículture and the feudal property, so the role of the castles was reduced. In the mountain áreas the landscape was never structured by castles, but by the rural distrícts (sexmos ofthe Segovia's Land.

12 CFR 544.2 - Charter amendments.

Science.gov (United States)

2010-01-01

... raise capital, which shall be unlimited, by accepting payments on savings, demand, or other accounts, as... purchase, hold, and convey real estate and personalty consistent with its objects, purposes, and powers; (xiii) To mortgage or lease any real estate and personalty and take such property by gift, devise, or...

Procès inquisitorial contra el castellà d'Amposta Fra Pedro Roiç de Moros a la cúria pontificia del papa Benet XIII (I414-1418

Directory of Open Access Journals (Sweden)

Alanyà i Roig, Josep

2002-06-01

Full Text Available The Arxiu de la Corona d'Aragó in Barcelona houses the original commital proceedings instituted by a court of cardinals set up by pope Benedict XIII in the year 1414 and teh trial itself of the lord of Amposta, Fra Pedro Roiç de Moros, knight of the Order of St. John of Jerusalem, who had been charged with indictable offences—concubinage, robbery, housing apostates, oath breaking and counterfeiting money, mismanagement of the Castlery's assets, excesses against his vassals, wasteful use of assets, dereliction and property abandonment— of which he was found guilty, and thereafter sentenced to losing the dignity of his lordship. Roiç de Moros appealed to the Council of Constance as well as to pope Martin V. It would be to no avail. Roiç de Moros paid a very high price for choosing to support count Jaume d'Urgell and deciding to oppose Ferran dAntequera and the policies of pope Benedict XIII. The follow up and analysis of the court´s records are very interesting for their human variety and interesting informations about fortresses, houses, barns, treaures and services there were in different locations of the Castlery of Amposta, such as Batea, Gandesa, Miravet, Ulldecona, Ascó and other towns and villages along the Ribera d´Ebre. The whole criminal prosecution bears a very peculiar historic interest mainly because the protagonists, the court procedures, and their causes are the link between the Interregnum in the Aragonese Crown and the fìnal days of the Western Schism.

A l'Arxiu de la Corona d'Aragó de Barcelona es conserva el procés original instruït per un tribunal de cardenals creat pel papa Benet XIII l'any 1414 per jutjar el Castella d'Amposta, l'hospitaler Fra Pedro Roiç de Moros, acusat de crims greus —concubinat, bandositats, recepció d’apòstates, perjuri i fabricació de moneda falsa, mala administració dels bens de la Castellania, comissió d'excessos contra els seus vassalls, dilapidado de bens i abando

A novel Sarcocystis neurona genotype XIII is associated with severe encephalitis in an unexpectedly broad range of marine mammals from the northeastern Pacific Ocean.

Science.gov (United States)

Barbosa, Lorraine; Johnson, Christine K; Lambourn, Dyanna M; Gibson, Amanda K; Haman, Katherine H; Huggins, Jessica L; Sweeny, Amy R; Sundar, Natarajan; Raverty, Stephen A; Grigg, Michael E

2015-08-01

Sarcocystis neurona is an important cause of protozoal encephalitis among marine mammals in the northeastern Pacific Ocean. To characterise the genetic type of S. neurona in this region, samples from 227 stranded marine mammals, most with clinical or pathological evidence of protozoal disease, were tested for the presence of coccidian parasites using a nested PCR assay. The frequency of S. neurona infection was 60% (136/227) among pinnipeds and cetaceans, including seven marine mammal species not previously known to be susceptible to infection by this parasite. Eight S. neurona fetal infections identified this coccidian parasite as capable of being transmitted transplacentally. Thirty-seven S. neurona-positive samples were multilocus sequence genotyped using three genetic markers: SnSAG1-5-6, SnSAG3 and SnSAG4. A novel genotype, referred to as Type XIII within the S. neurona population genetic structure, has emerged recently in the northeastern Pacific Ocean and is significantly associated with an increased severity of protozoal encephalitis and mortality among multiple stranded marine mammal species. Published by Elsevier Ltd.

A Potential Cyclotron Resonant Scattering Feature in the Ultraluminous X-Ray Source Pulsar NGC 300 ULX1 Seen by NuSTAR and XMM-Newton

Science.gov (United States)

Walton, D. J.; Bachetti, M.; Fürst, F.; Barret, D.; Brightman, M.; Fabian, A. C.; Grefenstette, B. W.; Harrison, F. A.; Heida, M.; Kennea, J.; Kosec, P.; Lau, R. M.; Madsen, K. K.; Middleton, M. J.; Pinto, C.; Steiner, J. F.; Webb, N.

2018-04-01

Based on phase-resolved broadband spectroscopy using XMM-Newton and NuSTAR, we report on a potential cyclotron resonant scattering feature (CRSF) at E ∼ 13 keV in the pulsed spectrum of the recently discovered ultraluminous X-ray source (ULX) pulsar NGC 300 ULX1. If this interpretation is correct, the implied magnetic field of the central neutron star is B ∼ 1012 G (assuming scattering by electrons), similar to that estimated from the observed spin-up of the star, and also similar to known Galactic X-ray pulsars. We discuss the implications of this result for the connection between NGC 300 ULX1 and the other known ULX pulsars, particularly in light of the recent discovery of a likely proton cyclotron line in another ULX, M51 ULX-8.

Centre-excised X-ray luminosity as an efficient mass proxy for future galaxy cluster surveys

Science.gov (United States)

Mantz, Adam B.; Allen, Steven W.; Morris, R. Glenn; von der Linden, Anja

2018-01-01

The cosmological constraining power of modern galaxy cluster catalogues can be improved by obtaining low-scatter mass proxy measurements for even a small fraction of sources. In the context of large upcoming surveys that will reveal the cluster population down to the group scale and out to high redshifts, efficient strategies for obtaining such mass proxies will be valuable. In this work, we use high-quality weak-lensing and X-ray mass estimates for massive clusters in current X-ray-selected catalogues to revisit the scaling relations of the projected, centre-excised X-ray luminosity (Lce), which previous work suggests correlates tightly with total mass. Our data confirm that this is the case with Lce having an intrinsic scatter at fixed mass comparable to that of gas mass, temperature or YX. Compared to the other proxies, however, Lce is less susceptible to systematic uncertainties due to background modelling, and can be measured precisely with shorter exposures. This opens up the possibility of using Lce to estimate masses for large numbers of clusters discovered by new X-ray surveys (e.g. eROSITA) directly from the survey data, as well as for clusters discovered at other wavelengths with relatively short follow-up observations. We describe a simple procedure for making such estimates from X-ray surface brightness data, and comment on the spatial resolution required to apply this method as a function of cluster mass and redshift. We also explore the potential impact of Chandra and XMM-Newton follow-up observations over the next decade on dark energy constraints from new cluster surveys.

Observational study with XMM-Newton of the physics of the formation of cosmic structure: from galaxies to merging of nearby galaxy clusters

International Nuclear Information System (INIS)

Belsole, Elena

2002-01-01

relationship between the X-ray and radio media in the region called the 'external lobes' of M87. The results presented here show that the X-ray emission from the lobes is thermic and multi-phase. This region is at a lower temperature compared to the ambient medium at the same distance from the centre. The temperature and dynamic structure in the region of the lobes is adequately explained by the floating bubble model, in which cold gas from the core is transported to larger distances by the adiabatic expansion of a bubble of non-thermal gas (observable in radio). The study of the temperature structure at larger scales shows that the gas is isothermal locally, meaning that the gas at a certain distance from the centre can be well described by a single temperature model. In M87, the radial temperature distribution follows the kT = 1.52(±0.02)R"0"."2"3"±"0"."0"1 (pour R≥2'). This analysis shows that the greater part of the region is filled with a component with spherical symmetry. The study of the temperature structure and of the mass distribution in the central region shows that two components contribute to the mass and density profile: the gravitational potential due to the cluster and that due to the central galaxy, M87 itself. The single phase nature of the hot gas and the non-detection of cold gas below 0.8 keV are in conflict with the standard multi-phase cooling flow model. It is suggested that the reduction in the cooling mass deposition rate is connected to a mechanism which depends on the central engine. The third and final part of this thesis concerns the study of the formation process in its most energetic manifestation: galaxy cluster mergers. The instruments on board XMM-Newton have allowed us to study for the first time in great detail the temperature structure of two merging clusters, A1750 and A3921. In both cases, the detection of a hotter region in the zone of interaction between the components confirms that each is undergoing an interaction as we see them

CHANDRA AND XMM-NEWTON X-RAY OBSERVATIONS OF THE HYPERACTIVE T TAURI STAR RY TAU

Energy Technology Data Exchange (ETDEWEB)

Skinner, Stephen L. [Center for Astrophysics and Space Astronomy (CASA), Univ. of Colorado, Boulder, CO 80309-0389 (United States); Audard, Marc [Dept. of Astronomy, University of Geneva, Ch. d’Ecogia 16, CH-1290 Versoix (Switzerland); Güdel, Manuel, E-mail: stephen.skinner@colorado.edu, E-mail: marc.audard@unige.ch, E-mail: manuel.guedel@univie.ac.at [Dept. of Astrophysics, Univ. of Vienna, Türkenschanzstr. 17, A-1180 Vienna (Austria)

2016-07-20

We present results of pointed X-ray observations of the accreting jet-driving T Tauri star RY Tau using Chandra and XMM-Newton . We obtained high-resolution grating spectra and excellent-quality CCD spectra and light curves with the objective of identifying the physical mechanisms underlying RY Tau’s bright X-ray emission. Grating spectra reveal numerous emission lines spanning a broad range of temperature superimposed on a hot continuum. The X-ray emission measure distribution is dominated by very hot plasma at T {sub hot} ∼ 50 MK, but higher temperatures were present during flares. A weaker cool plasma component is also present as revealed by low-temperature lines such as O viii. X-ray light curves show complex variability consisting of short-duration (∼hours) superhot flares accompanied by fluorescent Fe emission at 6.4 keV superimposed on a slowly varying (∼one day) component that may be tied to stellar rotation. The hot flaring component is undoubtedly of magnetic (e.g., coronal) origin. Soft- and hard-band light curves undergo similar slow variability implying that at least some of the cool plasma shares a common magnetic origin with the hot plasma. Any contribution to the X-ray emission from cool shocked plasma is small compared to the dominant hot component but production of individual low-temperature lines such as O viii in an accretion shock is not ruled out.

XMM-Newton and Chandra Observations of the Remarkable Dynamics of the Intracluster Medium and Radio Sources in the Clusters Abell 2061 and 3667

Science.gov (United States)

Sarazin, C.; Hogge, T.; Chatzikos, M.; Wik, D.; Giacintucci, S.; Clarke, T.; Wong, K.; Gitti, M.; Finoguenov, A.

2014-07-01

XMM-Newton and Chandra observations of remarkable dynamic structures in the X-ray gas and connected radio sources in three clusters are presented. Abell 2061 is a highly irregular, merging cluster in the Corona Borealis supercluster. X-ray observations show that there is a plume of very cool gas (˜1 keV) to the NE of the cluster, and a hot (7.6 keV) shock region just NE of the center. There is a very bright radio relic to the far SW of the cluster, and a central radio halo/relic with an extension to the NE. Comparison to SLAM simulations show that this is an offset merger of a ˜5 × 10^{13} M⊙ subcluster with a ˜2.5 × 10^{14} M⊙ cluster seen after first core passage. The plume is the cool-core gas from the subcluster, which has been ``slingshot'' to the NE of the cluster. The plume gas is now falling back into the cluster center, and shocks when it hits the central gas. The model predicts a strong shock to the SW at the location of the bright radio relic, and another shock at the NE radio extension. Time permitting, the observations of Abell 2626 and Abell 3667 will also be presented.

7 CFR 612.2 - Snow survey and water supply forecast activities.

Science.gov (United States)

2010-01-01

... 7 Agriculture 6 2010-01-01 2010-01-01 false Snow survey and water supply forecast activities. 612... SUPPLY FORECASTS § 612.2 Snow survey and water supply forecast activities. To carry out the cooperative snow survey and water supply forecast program, NRCS: (a) Establishes, maintains, and operates manual...

A study of the dynamical state of the hot plasma in galaxy clusters using XMM-Newton data and numerical simulation

International Nuclear Information System (INIS)

Solovyeva, Lilia

2008-01-01

Cluster of galaxies are the largest and youngest objects in the Universe and these objects are very interesting for study the cosmology. In this moment with the capacity of the instruments (XMM-Newton, Chandra) and with numerical simulations it is possible to study the dynamical state of gas in the cluster during their formation. And plus, now, we have the possibility to study the cluster in different wavelengths (optics, radio, X-ray). Our study helps us to understand the physics processes in clusters. In our work we studied the galaxy cluster around the maximum core collapse. We used the X-ray data, how the first indicators of dynamical state of gas. After with the help of numerical simulation and optics data we performed the completed analysis with the proposition of merger scenario possible. We performed the detailed analysis of two clusters (CL0016+16 and A548b), these clusters presents the signature of major merger and also we studied the cluster from numerical simulation (Cluster 6) around the major merger. (author) [fr

The FIRST-2MASS Red Quasar Survey

International Nuclear Information System (INIS)

Glikman, E; Helfand, D J; White, R L; Becker, R H; Gregg, M D; Lacy, M

2007-01-01

Combining radio observations with optical and infrared color selection--demonstrated in our pilot study to be an efficient selection algorithm for finding red quasars--we have obtained optical and infrared spectroscopy for 120 objects in a complete sample of 156 candidates from a sky area of 2716 square degrees. Consistent with our initial results, we find our selection criteria--J-K > 1.7,R-K > 4.0--yield a ∼ 50% success rate for discovering quasars substantially redder than those found in optical surveys. Comparison with UVX- and optical color-selected samples shows that ∼> 10% of the quasars are missed in a magnitude-limited survey. Simultaneous two-frequency radio observations for part of the sample indicate that a synchrotron continuum component is ruled out as a significant contributor to reddening the quasars spectra. We go on to estimate extinctions for our objects assuming their red colors are caused by dust. Continuum fits and Balmer decrements suggest E(B-V) values ranging from near zero to 2.5 magnitudes. Correcting the K-band magnitudes for these extinctions, we find that for K (le) 14.0, red quasars make up between 25% and 60% of the underlying quasar population; owing to the incompleteness of the 2MASS survey at fainter K-band magnitudes, we can only set a lower limit to the radio-detected red quasar population of > 20-30%

Relative ion expansion velocity in laser-produced plasmas

International Nuclear Information System (INIS)

Goldsmith, S.; Moreno, J.C.; Griem, H.R.; Cohen, L.; Richardson, M.C.

1988-01-01

The spectra of highly ionized titanium, TiXIII through TiXXI, and CVI Lyman lines were excited in laser-produced plasmas. The plasma was produced by uniformly irradiating spherical glass microballoons coated with thin layers of titanium and parylene. The 24-beam Omega laser system produced short, 0.6 ns, and high intensity, 4 x 10 14 W/cm, 2 laser pulses at a wavelength of 351 nm. The measured wavelength for the 2p-3s TiXIII resonance lines had an average shift of +0.023 A relative to the CVI and TiXX spectral lines. No shift was found between the CVI, TiXIX, and TiXX lines. The shift is attributed to a Doppler effect, resulting from a difference of (2.6 +- 0.2) x 10 7 cm/s in the expansion velocities of TiXIX and TiXX ions compared to TiXIII ions

The International Scientific-Practical Conference XIII Faizkhanov Readings “The Heritage of the Golden Horde in the Nationhood and Cultural Traditions of the Peoples of Eurasia” (St. Petersburg, May 4–6, 2016

Directory of Open Access Journals (Sweden)

R.Yu. Pochekaev

2017-03-01

Full Text Available XIII Faizkhanov Readings have been held in St. Petersburg on May 4–6, 2016. This year the conference was devoted to the Golden Horde and its heritage in Eurasia on occasion of the 750 years from foundation of this state. The conference was organized by the Spiritual Administration of Moslems of the Russian Federation, State Hermitage, Moscow State University, St. Petersburg State University, Institute of Oriental Studies, Institute of Oriental Manuscripts and others. There were two plenary sessions and four sections with about 100 speakers from different regions of Russia as well as from Finland, France, Kazakhstan, Ukraine, Uzbekistan. Most part of presentations caused questions and debates. The proceeding of the conference is to be published this year.

Greek architecture now

DEFF Research Database (Denmark)

Skousbøll, Karin Merete

2006-01-01

With the author's Scandinavian viewpoint the aim of this book has been an investigation into contemporary Greek architecture and at the same time providing an understanding for its essential characteristics based on the historic, cultural heritage of Hellas.......With the author's Scandinavian viewpoint the aim of this book has been an investigation into contemporary Greek architecture and at the same time providing an understanding for its essential characteristics based on the historic, cultural heritage of Hellas....

Esclavos musulmanes en los hospitales de cautivos de la Orden Militar de Santiago (siglos XII y XIII

Directory of Open Access Journals (Sweden)

Echevarría Arsuaga, Ana

2007-12-01

Full Text Available Military Orders had slave manpower in their lands since their foundation. However, the hospitals for ransoming captives owned by the Order of Santiago are the best example of how slavery worked in the kingdom of Leon-Castile during the twelfth and thirteenth centuries. These houses had enough room to provide lodging for captives while ransoms were being negotiated. They also helped to redistribute those Muslims who, lacking this possibility, became slaves of the order itself, or were sold in the slave markets of the kingdom. The scarce records kept in the Archivo Histórico Nacional, section Órdenes Militares, referring to slaves, help to understand the development of traffic, work and manumission of these people.

Las órdenes militares dispusieron desde su fundación de mano de obra esclava en sus tierras, pero la institución que mejor sirve para estudiar la esclavitud en los siglos XII y XIII en los reinos de León y Castilla son los hospitales para la redención de cautivos de la Orden de Santiago. Estas instituciones disponían de espacio para alojar a los cautivos mientras se negociaban rescates con los poderes islámicos, y atendían a la redistribución de aquellos musulmanes que, por no haber sido redimidos, pasaban a ser esclavos de la propia orden o a ser vendidos en los mercados de los reinos cristianos. Los escasos documentos de la sección de Órdenes Militares del Archivo Histórico Nacional dedicados a esclavos ayudan a comprender el funcionamiento del tráfico, trabajo y liberación de este colectivo.

Target Selection for the SDSS-IV APOGEE-2 Survey

International Nuclear Information System (INIS)

Zasowski, G.; Cohen, R. E.; Carlberg, J. K.; Fleming, Scott W.; Chojnowski, S. D.; Holtzman, J.; Santana, F.; Oelkers, R. J.; Bird, J. C.; Andrews, B.; Beaton, R. L.; Bender, C.; Cunha, K.; Bovy, J.; Covey, K.; Dell’Agli, F.; García-Hernández, D. A.; Frinchaboy, P. M.; Harding, P.; Johnson, J. A.

2017-01-01

APOGEE-2 is a high-resolution, near-infrared spectroscopic survey observing ∼3 × 10 5 stars across the entire sky. It is the successor to APOGEE and is part of the Sloan Digital Sky Survey IV (SDSS-IV). APOGEE-2 is expanding on APOGEE’s goals of addressing critical questions of stellar astrophysics, stellar populations, and Galactic chemodynamical evolution using (1) an enhanced set of target types and (2) a second spectrograph at Las Campanas Observatory in Chile. APOGEE-2 is targeting red giant branch and red clump stars, RR Lyrae, low-mass dwarf stars, young stellar objects, and numerous other Milky Way and Local Group sources across the entire sky from both hemispheres. In this paper, we describe the APOGEE-2 observational design, target selection catalogs and algorithms, and the targeting-related documentation included in the SDSS data releases.

Toxicity of inhaled 90SrCl2 in Beagle dogs. XIII

International Nuclear Information System (INIS)

Muggenburg, B.A.; Hahn, F.F.; Boecker, B.B.; Jones, R.K.; McClellan, R.O.; Pickrell, J.A.

1979-01-01

The metabolism, dosimetry and biological effects of inhaled 90 SrCl 2 in the Beagle dog are being studied to provide a basis for assessing the consequences of inhaling 90 Sr such as might be released in certain nuclear accidents. Seventy-two dogs were exposed to aerosols containing 90 Sr resulting in initial body burdens ranging from 2.5 to 250 μCi 90 Sr/kg body weight. To date, 60 90 Sr-exposed dogs have died or have been euthanized, six during the first 31 days after inhalation of 90 Sr with bone marrow aplasia and 54 between 585 and 5109 days after inhalation of 90 Sr. The latter group includes 32 dogs with bone-related neoplasms, two with upper respiratory tract carcinomas and five dogs with various diseases of the lower respiratory tract and heart. The other 15 dogs and diseases in organs that received little or no radiation dose, such as the gastrointestinal tract, urinary tract and the central nervous system. The skeletons of the dogs dying with bone-related neoplasms received initial radiation dose rates of 3.2 to 55 rads/day and cumulative doses to death of 2800 to 22 000 rads. Fourteen control dogs have died or been euthanized, two during the last year with mammary carcinoma and intestinal lymphosarcoma. Serial observations are continuing on the six surviving 90 Sr dogs and six controls

Radiological survey results at 2 Porter Street, Beverly, Massachusetts (VB005)

International Nuclear Information System (INIS)

Foley, R.D.; Carrier, R.F.

1992-08-01

At the request of the US Department of Energy (DOE), a team from Oak Ridge National Laboratory conducted a radiological survey at 2 Porter Street, Beverly, Massachusetts. The survey was performed in May 1991. The purpose of the survey was to determine if uranium dust from work performed under government contract at the former Ventron facility had migrated off-site to neighboring areas. The survey included a surface gamma scan and the collection of soil samples fore radionuclide analyses. Results of the survey demonstrated no radionuclide concentrations or radiation measurements in excess of the DOE Formerly Utilized Sites Remedial Action Program guidelines

Uncovering extreme AGN variability in serendipitous X-ray source surveys

Science.gov (United States)

Moran, Edward C.; Garcia Soto, Aylin; LaMassa, Stephanie; Urry, Meg

2018-01-01

Constraints on the duty cycle and duration of accretion episodes in active galactic nuclei (AGNs) are vital for establishing how most AGNs are fueled, which is essential for a complete picture of black hole/galaxy co-evolution. Perhaps the best handle we have on these activity parameters is provided by AGNs that have displayed dramatic changes in their bolometric luminosities and, in some cases, spectroscopic classifications. Given that X-ray emission is directly linked to black-hole accretion, X-ray surveys should provide a straightforward means of identifying AGNs that have undergone dramatic changes in their accretion states. However, it appears that such events are very rare, so wide-area surveys separated in time by many years are needed to maximize discovery rates. We have cross-correlated the Einstein IPC Two-Sigma Catalog with the ROSAT All-Sky Survey Faint Source Catalog to identify a sample of soft X-ray sources that varied by factors ranging from 7 to more than 100 over a ten year timescale. When possible, we have constructed long-term X-ray light curves for the sources by combining the Einstein and RASS fluxes with those obtained from serendipitous pointed observations by ROSAT, Chandra,XMM, and Swift. Optical follow-up observations indicate that many of the extremely variable sources in our sample are indeed radio-quiet AGNs. Interestingly, the majority of objects that dimmed between ~1980 and ~1990 are still (or are again) broad-line AGNs rather than“changing-look” candidates that have more subtle AGN signatures in their spectra — despite the fact that none of the sources examined thus far has returned to its highest observed luminosity. Future X-ray observations will provide the opportunity to characterize the X-ray behavior of these anonymous, extreme AGNs over a four decade span.

Target Selection for the SDSS-IV APOGEE-2 Survey

Energy Technology Data Exchange (ETDEWEB)

Zasowski, G. [Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 (United States); Cohen, R. E.; Carlberg, J. K.; Fleming, Scott W. [Space Telescope Science Institute, Baltimore, MD 21218 (United States); Chojnowski, S. D.; Holtzman, J. [Department of Astronomy, New Mexico State University, Las Cruces, NM 88001 (United States); Santana, F. [Departamento de Astronomía, Universidad de Chile, Santiago (Chile); Oelkers, R. J.; Bird, J. C. [Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235 (United States); Andrews, B. [PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260 (United States); Beaton, R. L. [The Observatories of the Carnegie Institution for Science, Pasadena, CA 91101 (United States); Bender, C.; Cunha, K. [Steward Observatory, The University of Arizona, Tucson, AZ 85719 (United States); Bovy, J. [Department of Astronomy and Astrophysics and Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4 (Canada); Covey, K. [Department of Physics and Astronomy, Western Washington University, Bellingham, WA 98225 (United States); Dell’Agli, F.; García-Hernández, D. A. [Departamento de Astrofísica, Universidad de La Laguna, and Instituto de Astrofísica de Canarias, La Laguna, Tenerife (Spain); Frinchaboy, P. M. [Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129 (United States); Harding, P. [Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106 (United States); Johnson, J. A., E-mail: gail.zasowski@gmail.com [Department of Astronomy, The Ohio State University, Columbus, OH 43210 (United States); and others

2017-11-01

APOGEE-2 is a high-resolution, near-infrared spectroscopic survey observing ∼3 × 10{sup 5} stars across the entire sky. It is the successor to APOGEE and is part of the Sloan Digital Sky Survey IV (SDSS-IV). APOGEE-2 is expanding on APOGEE’s goals of addressing critical questions of stellar astrophysics, stellar populations, and Galactic chemodynamical evolution using (1) an enhanced set of target types and (2) a second spectrograph at Las Campanas Observatory in Chile. APOGEE-2 is targeting red giant branch and red clump stars, RR Lyrae, low-mass dwarf stars, young stellar objects, and numerous other Milky Way and Local Group sources across the entire sky from both hemispheres. In this paper, we describe the APOGEE-2 observational design, target selection catalogs and algorithms, and the targeting-related documentation included in the SDSS data releases.

2d forward modelling of marine CSEM survey geometry for seabed logging

International Nuclear Information System (INIS)

Hussain, N.; Noh, M.; Yahya, N.B.

2011-01-01

Hydrocarbon reserve exploration in deep water is done by geophysical surveys. Previously seismic geophysical surveys were explicitly used but it has indistinct results for both water and hydrocarbon saturated reservoir. Recent development for the detection of hydrocarbon reservoir in deeper water is Marine Controlled Source Electromagnetic (MCSEM) geophysical survey. MCSEM is sensitive to electrical conductivity of rocks by which it can differentiate between hydrocarbon reservoir and water saturated reservoir. MCSEM survey geometry put vital role and may causes for anomalies in synthetic data. Consequentially MCSEM is sensitive to survey geometry (e.g. source dipping, rotation and speed, receivers' orientation etc) which causes anomalies. The interpretation for delineating subsurface structure from survey data need to well understand the effects of survey geometry anomalies. Forward modelling is an alternative rather real time survey to study the aforementioned anomalies. In this paper finite difference method (FDM) is implemented for 2D forward modelling in the sense of qualitative understanding to how induced Electromagnetic (EM) signal changes its overall pattern while interact with physical earth properties. A stratified earth structure is developed and modelled in MatLabTM software to study the behaviour of EM field with physical earth properties. Obtained results of 2D geological models are also discussed in this paper. (author)

Accuracy and precision of glucose monitoring are relevant to treatment decision-making and clinical outcome in hospitalized patients with diabetes.

Science.gov (United States)

Voulgari, Christina; Tentolouris, Nicholas

2011-07-01

The accuracy and precision of three blood glucose meters (BGMs) were evaluated in 600 hospitalized patients with type 1 (n = 200) or type 2 (n = 400) diabetes. Capillary blood glucose values were analyzed with Accu-Chek(®) Aviva [Roche (Hellas) S.A., Maroussi, Greece], Precision-Xceed(®) [Abbott Laboratories (Hellas) S.A., Alimos, Greece], and Glucocard X-Sensor(®) (Menarini Diagnostics S.A., Argyroupolis, Greece). At the same time plasma glucose was analyzed using the World Health Organization's glucose oxidase method. Median plasma glucose values (141.2 [range, 13-553] mg/dL) were significantly different from that produced by the BGMs (P diabetes patients. In all cases, the BGMs were unreliable in sensing hypoglycemia. Multivariate linear regression analysis demonstrated that low blood pressure and hematocrit significantly affected glucose measurements obtained with all three BGMs (P diabetes patients, all three frequently used BGMs undersensed hypoglycemia and oversensed hyperglycemia to some extent. Patients and caregivers should be aware of these restrictions of the BGMs.

Joint XMM-Newton and Chandra observations of the NGC 1407/1400 complex: A tail of an early-type galaxy and a tale of a nearby merging group

Energy Technology Data Exchange (ETDEWEB)

Su, Yuanyuan [Department of Physics and Astronomy, University of California at Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697 (United States); Gu, Liyi [Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo (Japan); White III, Raymond E.; Irwin, Jimmy, E-mail: yuanyuas@uci.edu [Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487 (United States)

2014-05-10

The nearby group centered on its bright central galaxy NGC 1407 has been suggested by previous kinematic studies to be an unusually dark system. It is also known for hosting a bright galaxy, NGC 1400, with a large radial velocity (1200 km s{sup –1}) with respect to the group center. Previous ROSAT X-ray observations revealed an extended region of enhanced surface brightness just eastward of NGC 1400. We investigate the NGC 1407/1400 complex with XMM-Newton and Chandra observations. We find that the temperature and metallicity of the enhanced region are different (cooler and more metal rich) than those of the surrounding group gas but are consistent with those of the interstellar medium (ISM) in NGC 1400. The relative velocity of NGC 1400 is large enough that much of its ISM could have been ram pressure stripped while plunging through the group atmosphere. We conclude that the enhanced region is likely to be hot gas stripped from the ISM of NGC 1400. We constrain the motion of NGC 1400 using the pressure jump at its associated stagnation front and the total mass profile of the NGC 1407 group. We conclude that NGC 1400 is moving within ∼30° of the line of sight with Mach number M≲3. We do not detect any obvious shock features in this complex, perhaps because of the high line-of-sight motion of NGC 1400. With an XMM-Newton pointing on the relatively relaxed eastern side of NGC 1407, we derive a hydrostatic mass for this group of ∼1 × 10{sup 13} M {sub ☉} within 100 kpc. The total mass extrapolated to the virial radius (681 kpc) is 3.8 × 10{sup 13} M {sub ☉}, which puts an upper limit of ∼300 M{sub ⊙}/L{sub B{sub ⊙}} on the mass-to-light ratio of this group. This suggests that the NGC 1407 group is not an unusually dark group.

The SCUBA-2 Cosmology Legacy Survey: 850 μm maps, catalogues and number counts

NARCIS (Netherlands)

Geach, J. E.; Dunlop, J. S.; Halpern, M.; Smail, Ian; van der Werf, P.; Alexander, D. M.; Almaini, O.; Aretxaga, I.; Arumugam, V.; Asboth, V.; Banerji, M.; Beanlands, J.; Best, P. N.; Blain, A. W.; Birkinshaw, M.; Chapin, E. L.; Chapman, S. C.; Chen, C.-C.; Chrysostomou, A.; Clarke, C.; Clements, D. L.; Conselice, C.; Coppin, K. E. K.; Cowley, W. I.; Danielson, A. L. R.; Eales, S.; Edge, A. C.; Farrah, D.; Gibb, A.; Harrison, C. M.; Hine, N. K.; Hughes, D.; Ivison, R. J.; Jarvis, M.; Jenness, T.; Jones, S. F.; Karim, A.; Koprowski, M.; Knudsen, K. K.; Lacey, C. G.; Mackenzie, T.; Marsden, G.; McAlpine, K.; McMahon, R.; Meijerink, R.; Michałowski, M. J.; Oliver, S. J.; Page, M. J.; Peacock, J. A.; Rigopoulou, D.; Robson, E. I.; Roseboom, I.; Rotermund, K.; Scott, Douglas; Serjeant, S.; Simpson, C.; Simpson, J. M.; Smith, D. J. B.; Spaans, M.; Stanley, F.; Stevens, J. A.; Swinbank, A. M.; Targett, T.; Thomson, A. P.; Valiante, E.; Wake, D. A.; Webb, T. M. A.; Willott, C.; Zavala, J. A.; Zemcov, M.

2017-01-01

We present a catalogue of ˜3000 submillimetre sources detected (≥3.5σ) at 850 μm over ˜5 deg2 surveyed as part of the James Clerk Maxwell Telescope (JCMT) SCUBA-2 Cosmology Legacy Survey (S2CLS). This is the largest survey of its kind at 850 μm, increasing the sample size of 850 μm selected

The reduction of CO{sub 2} emissions from a turbocharged DI gasoline engine through optimised cooling system control; CO{sub 2}-Minderung bei einem Turbo-DI-Ottomotor durch optimiertes Thermomanagement

Energy Technology Data Exchange (ETDEWEB)

Edwards, S.; Mueller, R.; Feldhaus, G. [Behr GmbH, Stuttgart (Germany); Finkeldei, T. [BHTC GmbH, Lippstadt (Germany); Neubauer, M. [AVL List GmbH, Graz (Austria)

2008-01-15

In a joint project Behr, Behr-Hella Thermocontrol (BHTC) and AVL List have investigated various thermomanagement technologies in order to reduce the CO{sub 2} emissions of a turbocharged direct injection gasoline engine. Through the use of cooled EGR the fuel consumption at part load was reduced by up to 5%; at full load the consumption was reduced by up to 18% since no enrichment was needed. Under real driving conditions a saving of 6% was achieved. A further reduction of about 3% in the NEDC was possible via coolant stand still during the engine warm-up. Additionally, it was shown that a change in the engine coolant temperature of 10 K, made possible by the application of a map controlled thermostat, has the potential for savings of up to 1.4%. (orig.)

Decreased store operated Ca2+ entry in dendritic cells isolated from mice expressing PKB/SGK-resistant GSK3.

Science.gov (United States)

Schmid, Evi; Yan, Jing; Nurbaeva, Meerim K; Russo, Antonella; Yang, Wenting; Faggio, Caterina; Shumilina, Ekaterina; Lang, Florian

2014-01-01

Dendritic cells (DCs), key players of immunity, are regulated by glycogen synthase kinase GSK3. GSK3 activity is suppressed by PKB/Akt and SGK isoforms, which are in turn stimulated by the PI3K pathway. Exposure to bacterial lipopolysaccharides increases cytosolic Ca(2+)-concentration ([Ca(2+)]i), an effect augmented in DCs isolated from mutant mice expressing PKB/SGK-resistant GSK3α,β (gsk3(KI) ). Factors affecting [Ca(2+)]i include Ca(2+)-release from intracellular stores (CRIS), store-operated Ca(2+)-entry (SOCE) through STIM1/STIM2-regulated Orai1, K(+)-dependent Na(+)/Ca(2+)-exchangers (NCKX), K(+)-independent Na(+)/Ca(2+)-exchangers (NCX) and calbindin-D28k. The present study explored whether PKB/SGK-dependent GSK3α, β-activity impacts on CRIS, SOCE, NCKX, NCX or calbindin. DCs were isolated from gsk3(KI) mice and respective wild-type mice (gsk3(WT) ), [Ca(2+)]i estimated from Fura2 fluorescence, Orai1, STIM1, STIM2 as well as calbindin-D28k protein abundance determined by Western blotting and mRNA levels quantified by real time PCR. As a result, thapsigargin-induced CRIS and SOCE were significantly blunted by GSK3-inhibitors SB216763 (1-10 µM, 30 min) or GSK-XIII (10 µM, 30 min) but were significantly lower in gsk3(WT) than in gsk3(KI) DCs. Orai1, STIM1 and STIM2 protein abundance was significantly lower and calbindin-D28k abundance significantly higher in gsk3(KI) than in gsk3(WT) DCs. Activity of NCKX and NCX was significantly higher in gsk3(KI) than in gsk3(WT) DCs and was significantly increased by SB216763 (1 µM, 30 min) or GSK-XIII (10 µM, 30 min). Treatment of gsk3(WT) DCs with SB216763 (1 µM, 4-24 h) or GSK-XIII (10 µM, 4-24 h) did not significantly modify the protein abundance of Orai1, STIM1 and STIM2. The present observations point to a dual role of GSK3 in the regulation of Ca(2+) in DCs. Acute inhibition of GSK3 blunted the increase of [Ca(2+)]i following CRIS and SOCE and stimulated NCKX/NCX activity. However, expression of PKB

Application of Physics Model in prediction of the Hellas Euro election results

Directory of Open Access Journals (Sweden)

L. Magafas

2009-01-01

Full Text Available In this paper we use chaos theory to predict the Hellenic Euro election results in the form of time series for Hellenic political parties New Democracy (ND, Panhellenic Socialistic Movement (PASOK, Hellenic Communistic Party (KKE , Coalition of the Radical Left (SYRIZA and (Popular Orthodox Rally LAOS, using the properties of the reconstructed strange attrac-tor of the corresponding non linear system, creating a new scientific field called “DemoscopoPhysics”. For this purpose we found the optimal delay time, the correlation and embedding dimension with the method of Grassberger and Procassia. With the help of topological properties of the corresponding strange attractor we achieved up to a 60 time steps out of sample pre-diction of the public survey.

Gravitational lensing statistics with extragalactic surveys; 2, Analysis of the Jodrell Bank-VLA Astrometric Survey

NARCIS (Netherlands)

Helbig, P.; Marlow, D. R.; Quast, R.; Wilkinson, P. N.; Browne, I. W. A.; Koopmans, L. V. E.

1999-01-01

Published in: Astron. Astrophys. Suppl. Ser. 136 (1999) no. 2, pp.297-305 citations recorded in [Science Citation Index] Abstract: We present constraints on the cosmological constant $lambda_{0}$ from gravitational lensing statistics of the Jodrell Bank-VLA Astrometric Survey (JVAS). Although this

La visita del papa Benet XIII a València de 1414-1415: una aproximació a la seua memòria en la tradició historiogràfica valenciana

Directory of Open Access Journals (Sweden)

Blai Josep Server Server

2017-06-01

Full Text Available L’article analitza els testimonis de la visita de Benet XIII, Pero Martínez de Luna, a la ciutat de València entre desembre de 1414 i juliol de 1415 conservats en la tradició historiogràfica valenciana. En concret, s’hi examinen les obres valencianes de caràcter memorialístic (cròniques i dietaris, principalment que, des del segle XV i fins a l’actualitat, han parat atenció a l’esdeveniment, per concloure que la memòria del mateix es conservà sobretot en els cercles del poder eclesiàstic –particularment entorn de la Seu– i municipal de la ciutat. Més enllà d’aquests àmbits, la visita papal fou progressivament oblidada, a pesar de l’impacte notable que degué tindre sobre aquells que la visqueren directament o en tingueren notícia indirectament a l’inici del segle XV.

Antroponimia femminile nella Scozia del XIII secolo: la testimonianza del Ragman Roll (1296 Feminine anthroponyms in 13th-century Scotland: the Ragman Roll (1296

Directory of Open Access Journals (Sweden)

Valeria Di Clemente

2012-10-01

Full Text Available La serie di documenti nota come Ragman Roll raccoglie i giuramenti di fedeltà e l’omaggio feudale resi da aristocratici, ecclesiastici, proprietari terrieri e borghesi di Scozia a Edoardo I Plantageneto dopo la campagna di occupazione inglese della primavera-estate 1296. In questa veste, essa riporta nomi e cognomi di circa 1800 persone, rappresentando una fonte preziosa per lo studio dell’antroponimia in uso in Scozia nella seconda metà del XIII secolo. Il presente saggio esamina gli antroponimi femminili nelle forme ricorrenti nel documento, ricostruendone la vicenda storico-etimologica e culturale.

The documents known as Ragman Roll collect the fealty oaths sworn and the homages rendered by Scottish nobility, clergy, landowners and burgesses to Edward I Plantagenet after the English invasion of Scotland in the spring and summer of 1296. These documents record personal names and surnames of ca. 1800 people, being a precious source for the study of Scottish anthroponymy in the second half of the 13^th century. This paper focuses on the feminine anthroponyms occurring in the Ragman Roll, on their form and on their historical-etymological and cultural background.

Detection of DCIS using 99mTc-MIBI scintimammography in patients with suspected primary breast cancer, comparison with conventional mammography

International Nuclear Information System (INIS)

Cwikla, J.B.; Buscombe, J.R.; Hilson, A.J.W.

2000-01-01

Background: Scintimammography using Tc-99m MIBI (SMM) is often used clinically as a second line diagnostic test for the detection of breast cancer in cases where there is concern about the results of x-ray mammography (XMM) and ultrasound. Both of these methods, but particularly XMM, may miss a significant proportion of ductal carcinoma in situ (DCIS). MATERIAL AND METHODS: This study was performed to determine the possible accuracy of SMM in finding DCIS and comparing this with the accuracy of XMM in the same patient. Over a 3 year period 353 patients with no previous history of breast cancer were imaged with both XMM and SMM. The histology of any suspect area was verified by pathological examination of biopsy material. There were 203 malignant breast tumours. RESULTS: In those 203 cancers there were 15 pure DCIS cancers. SMM correctly diagnosed 12 of these (sensitivity was 80%). XMM diagnosed correctly 8 DCIS (sensitivity 53%) and was equivocal in 2. Combining of both SMM and XMM provided the best result with all but one DCIS identified (sensitivity 93%). CONCLUSIONS: This study shows that the SMM is helpful in detecting DCIS in those cases where XMM failed to detect DCIS or was equivocal. The combination of the two techniques produces a higher sensitivity result than either modality alone. (author)

The NuSTAR  Extragalactic Surveys: X-Ray Spectroscopic Analysis of the Bright Hard-band Selected Sample

Science.gov (United States)

Zappacosta, L.; Comastri, A.; Civano, F.; Puccetti, S.; Fiore, F.; Aird, J.; Del Moro, A.; Lansbury, G. B.; Lanzuisi, G.; Goulding, A.; Mullaney, J. R.; Stern, D.; Ajello, M.; Alexander, D. M.; Ballantyne, D. R.; Bauer, F. E.; Brandt, W. N.; Chen, C.-T. J.; Farrah, D.; Harrison, F. A.; Gandhi, P.; Lanz, L.; Masini, A.; Marchesi, S.; Ricci, C.; Treister, E.

2018-02-01

We discuss the spectral analysis of a sample of 63 active galactic nuclei (AGN) detected above a limiting flux of S(8{--}24 {keV})=7× {10}-14 {erg} {{{s}}}-1 {{cm}}-2 in the multi-tiered NuSTAR extragalactic survey program. The sources span a redshift range z=0{--}2.1 (median =0.58). The spectral analysis is performed over the broad 0.5–24 keV energy range, combining NuSTAR with Chandra and/or XMM-Newton data and employing empirical and physically motivated models. This constitutes the largest sample of AGN selected at > 10 {keV} to be homogeneously spectrally analyzed at these flux levels. We study the distribution of spectral parameters such as photon index, column density ({N}{{H}}), reflection parameter ({\\boldsymbol{R}}), and 10–40 keV luminosity ({L}{{X}}). Heavily obscured ({log}[{N}{{H}}/{{cm}}-2]≥slant 23) and Compton-thick (CT; {log}[{N}{{H}}/{{cm}}-2]≥slant 24) AGN constitute ∼25% (15–17 sources) and ∼2–3% (1–2 sources) of the sample, respectively. The observed {N}{{H}} distribution agrees fairly well with predictions of cosmic X-ray background population-synthesis models (CXBPSM). We estimate the intrinsic fraction of AGN as a function of {N}{{H}}, accounting for the bias against obscured AGN in a flux-selected sample. The fraction of CT AGN relative to {log}[{N}{{H}}/{{cm}}-2]=20{--}24 AGN is poorly constrained, formally in the range 2–56% (90% upper limit of 66%). We derived a fraction (f abs) of obscured AGN ({log}[{N}{{H}}/{{cm}}-2]=22{--}24) as a function of {L}{{X}} in agreement with CXBPSM and previous zvalues.

Violet Grove CO{sub 2} injection project : monitoring with timelapse VSP surveys

Energy Technology Data Exchange (ETDEWEB)

Coueslan, M.; Lawton, D. [Calgary Univ., Calgary, AB (Canada); Jones, M. [Schlumberger Canada Ltd., Calgary, AB (Canada)

2006-07-01

Several oil and gas fields in western Canada have been depleted through primary production and secondary recovery methods. Injecting carbon dioxide (CO{sub 2}) into a reservoir can enhance oil recovery (EOR) and has the potential benefit of CO{sub 2} sequestration, which reduces greenhouse gas emissions into the atmosphere. It has been estimated that western Canada has a practical CO{sub 2} storage capacity of about 3.3 Gt in its oil and gas reservoirs. In order to claim a reduction in CO{sub 2} emissions, however, the injected CO{sub 2} must be monitored to prove that it is being trapped in these reservoirs. For that reason, the Violet Grove site, near Drayton Valley, Alberta was chosen as a pilot site to study CO{sub 2} injection into a reservoir for enhanced recovery and carbon sequestration purposes. The reservoir is located in the Cardium Formation in the Pembina Field. It was expected that the CO{sub 2} would flow preferentially in the reservoir's dominant fracture orientation, which is northeast-southwest. Simultaneously acquired time-lapse multicomponent surface and borehole seismic surveys were used to monitor changes in the reservoir. Prior to CO{sub 2} injection, a baseline survey was acquired in March 2005. A second survey was acquired 8 months after CO{sub 2} injection. The borehole seismic data displayed higher bandwidth and increased resolution compared to the surface seismic data. The PS-wave borehole seismic data in particular showed much better results. Together, these seismic surveys provide lateral coverage of the area as well as high resolution images near the observation well. Preliminary results from the time-lapse analysis show an increase of 30 to 60 per cent in the reservoir reflectivity amplitudes in the 8 months between the baseline and monitor surveys, suggesting that the CO{sub 2} flood has progressed southwest of the injector, most likely along the dominant fracture trend. 7 refs., 5 figs.

R cookbook

National Research Council Canada - National Science Library

Teetor, Paul; Loukides, Michael Kosta

2011-01-01

... . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . xiii 1. Getting Started and Getting Help . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 1.1 Downloading and Installing R 2...

THE BROADBAND XMM-NEWTON AND NuSTAR X-RAY SPECTRA OF TWO ULTRALUMINOUS X-RAY SOURCES IN THE GALAXY IC 342

Energy Technology Data Exchange (ETDEWEB)

Rana, Vikram; Harrison, Fiona A.; Walton, Dominic J.; Furst, Felix; Grefenstette, Brian W.; Madsen, Kristin K. [Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125 (United States); Bachetti, Matteo; Barret, Didier; Webb, Natalie A. [Université de Toulouse, UPS-OMP, IRAP, Toulouse (France); Miller, Jon M. [Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109-1042 (United States); Fabian, Andrew C. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA (United Kingdom); Boggs, Steven E.; Craig, William W. [Space Sciences Laboratory, University of California, Berkeley, CA 94720 (United States); Christensen, Finn C. [DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby (Denmark); Hailey, Charles J. [Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (United States); Ptak, Andrew F.; Zhang, William W. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Stern, Daniel [Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States)

2015-02-01

We present results for two ultraluminous X-ray sources (ULXs), IC 342 X-1 and IC 342 X-2, using two epochs of XMM-Newton and NuSTAR observations separated by ∼7 days. We observe little spectral or flux variability above 1 keV between epochs, with unabsorbed 0.3-30 keV luminosities being 1.04{sub −0.06}{sup +0.08}×10{sup 40} erg s{sup –1} for IC 342 X-1 and 7.40 ± 0.20 × 10{sup 39} erg s{sup –1} for IC 342 X-2, so that both were observed in a similar, luminous state. Both sources have a high absorbing column in excess of the Galactic value. Neither source has a spectrum consistent with a black hole binary in low/hard state, and both ULXs exhibit strong curvature in their broadband X-ray spectra. This curvature rules out models that invoke a simple reflection-dominated spectrum with a broadened iron line and no cutoff in the illuminating power-law continuum. X-ray spectrum of IC 342 X-1 can be characterized by a soft disk-like blackbody component at low energies and a cool, optically thick Comptonization continuum at high energies, but unique physical interpretation of the spectral components remains challenging. The broadband spectrum of IC 342 X-2 can be fit by either a hot (3.8 keV) accretion disk or a Comptonized continuum with no indication of a seed photon population. Although the seed photon component may be masked by soft excess emission unlikely to be associated with the binary system, combined with the high absorption column, it is more plausible that the broadband X-ray emission arises from a simple thin blackbody disk component. Secure identification of the origin of the spectral components in these sources will likely require broadband spectral variability studies.

THE DEEP2 GALAXY REDSHIFT SURVEY: DESIGN, OBSERVATIONS, DATA REDUCTION, AND REDSHIFTS

International Nuclear Information System (INIS)

Newman, Jeffrey A.; Cooper, Michael C.; Davis, Marc; Faber, S. M.; Guhathakurta, Puragra; Koo, David C.; Phillips, Andrew C.; Conroy, Charlie; Harker, Justin J.; Lai, Kamson; Coil, Alison L.; Dutton, Aaron A.; Finkbeiner, Douglas P.; Gerke, Brian F.; Rosario, David J.; Weiner, Benjamin J.; Willmer, C. N. A.; Yan Renbin; Kassin, Susan A.; Konidaris, N. P.

2013-01-01

We describe the design and data analysis of the DEEP2 Galaxy Redshift Survey, the densest and largest high-precision redshift survey of galaxies at z ∼ 1 completed to date. The survey was designed to conduct a comprehensive census of massive galaxies, their properties, environments, and large-scale structure down to absolute magnitude M B = –20 at z ∼ 1 via ∼90 nights of observation on the Keck telescope. The survey covers an area of 2.8 deg 2 divided into four separate fields observed to a limiting apparent magnitude of R AB = 24.1. Objects with z ∼ 0.7 to be targeted ∼2.5 times more efficiently than in a purely magnitude-limited sample. Approximately 60% of eligible targets are chosen for spectroscopy, yielding nearly 53,000 spectra and more than 38,000 reliable redshift measurements. Most of the targets that fail to yield secure redshifts are blue objects that lie beyond z ∼ 1.45, where the [O II] 3727 Å doublet lies in the infrared. The DEIMOS 1200 line mm –1 grating used for the survey delivers high spectral resolution (R ∼ 6000), accurate and secure redshifts, and unique internal kinematic information. Extensive ancillary data are available in the DEEP2 fields, particularly in the Extended Groth Strip, which has evolved into one of the richest multiwavelength regions on the sky. This paper is intended as a handbook for users of the DEEP2 Data Release 4, which includes all DEEP2 spectra and redshifts, as well as for the DEEP2 DEIMOS data reduction pipelines. Extensive details are provided on object selection, mask design, biases in target selection and redshift measurements, the spec2d two-dimensional data-reduction pipeline, the spec1d automated redshift pipeline, and the zspec visual redshift verification process, along with examples of instrumental signatures or other artifacts that in some cases remain after data reduction. Redshift errors and catastrophic failure rates are assessed through more than 2000 objects with duplicate

Structure of the Milky Way stellar halo out to its outer boundary with blue horizontal-branch stars

Science.gov (United States)

Fukushima, Tetsuya; Chiba, Masashi; Homma, Daisuke; Okamoto, Sakurako; Komiyama, Yutaka; Tanaka, Masayuki; Tanaka, Mikito; Arimoto, Nobuo; Matsuno, Tadafumi

2018-06-01

We present the structure of the Milky Way stellar halo beyond Galactocentric distances of r = 50 kpc traced by blue horizontal-branch (BHB) stars, which are extracted from the survey data in the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We select BHB candidates based on (g, r, i, z) photometry, where the z-band is on the Paschen series and the colors that involve the z-band are sensitive to surface gravity. About 450 BHB candidates are identified between r = 50 kpc and 300 kpc, most of which are beyond the reach of previous large surveys, including the Sloan Digital Sky Survey. We find that the global structure of the stellar halo in this range has substructures, which are especially remarkable in the GAMA15H and XMM-LSS fields in the HSC-SSP. We find that the stellar halo can be fitted to a single power-law density profile with an index of α ≃ 3.3 (3.5) with (without) these fields and its global axial ratio is q ≃ 2.2 (1.3). Thus, the stellar halo may be significantly disturbed and be made in a prolate form by halo substructures, perhaps associated with the Sagittarius stream in its extension beyond r ˜ 100 kpc. For a broken power-law model allowing different power-law indices inside/outside a break radius, we obtain a steep power-law slope of α ≃ 5 outside a break radius of ˜100 kpc (200 kpc) for the case with (without) GAMA15H and XMM-LSS. This radius of 200 kpc might be as close as a halo boundary if there is any, although a larger BHB sample is required from further HSC-SSP surveys to increase its statistical significance.

FXIIIA and TGF-beta over-expression produces normal musculo-skeletal phenotype in TG2-/- mice.

Science.gov (United States)

Tarantino, U; Oliva, F; Taurisano, G; Orlandi, A; Pietroni, V; Candi, E; Melino, G; Maffulli, N

2009-04-01

Transglutaminase (TGs) enzymes and proteins crosslinking have for long time been implicated in the formation of hard tissue development, matrix maturation and mineralization. Among the TGs family members, in the context of connective tissue formation, TG2 and Factor XIII are expressed in cartilage by hypertrophic chondrocytes. Here, we analyse the morphological consequences of TG2 deficiency, during the development of skeletal elements. When TG2 is absent, there are not gross abnormalities in the development of the skeletal system, probably from compensatory mechanisms resulting in increased expression of FXIIIA and TGF-beta 1. In vivo other TGs may be involved in promoting chondrocytes and osteoblast differentiation and matrix mineralisation.

Star formation history of Canis Major OB1. II. A bimodal X-ray population revealed by XMM-Newton

Science.gov (United States)

Santos-Silva, T.; Gregorio-Hetem, J.; Montmerle, T.; Fernandes, B.; Stelzer, B.

2018-02-01

Aims: The Canis Major OB1 Association has an intriguing scenario of star formation, especially in the region called Canis Major R1 (CMa R1) traditionally assigned to a reflection nebula, but in reality an ionized region. This work is focussed on the young stellar population associated with CMa R1, for which our previous results from ROSAT, optical, and near-infrared data had revealed two stellar groups with different ages, suggesting a possible mixing of populations originated from distinct star formation episodes. Methods: The X-ray data allow the detected sources to be characterized according to hardness ratios, light curves, and spectra. Estimates of mass and age were obtained from the 2MASS catalogue and used to define a complete subsample of stellar counterparts for statistical purposes. Results: A catalogue of 387 XMM-Newton sources is provided, of which 78% are confirmed as members or probable members of the CMa R1 association. Flares (or similar events) were observed for 13 sources and the spectra of 21 bright sources could be fitted by a thermal plasma model. Mean values of fits parameters were used to estimate X-ray luminosities. We found a minimum value of log(LX [erg/s] ) = 29.43, indicating that our sample of low-mass stars (M⋆ ≤ 0.5 M⊙), which are faint X-ray emitters, is incomplete. Among the 250 objects selected as our complete subsample (defining our "best sample"), 171 are found to the east of the cloud, near Z CMa and dense molecular gas, of which 50% of them are young (10 Myr). The opposite happens to the west, near GU CMa, in areas lacking molecular gas: among 79 objects, 30% are young and 50% are older. These findings confirm that a first episode of distributed star formation occurred in the whole studied region 10 Myr ago and dispersed the molecular gas, while a second, localized episode (<5 Myr) took place in the regions where molecular gas is still present.

Toward the standard population synthesis model of the X-ray background: Evolution of X-ray luminosity and absorption functions of active galactic nuclei including Compton-thick populations

Energy Technology Data Exchange (ETDEWEB)

Ueda, Yoshihiro [Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502 (Japan); Akiyama, Masayuki [Astronomical Institute, Tohoku University, 6-3 Aramaki, Aoba-ku, Sendai 980-8578 (Japan); Hasinger, Günther [Institute for Astronomy, 2680 Woodlawn Drive Honolulu, HI 96822-1839 (United States); Miyaji, Takamitsu [Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, Baja California (Mexico); Watson, Michael G. [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom)

2014-05-10

We present the most up to date X-ray luminosity function (XLF) and absorption function of active galactic nuclei (AGNs) over the redshift range from 0 to 5, utilizing the largest, highly complete sample ever available obtained from surveys performed with Swift/BAT, MAXI, ASCA, XMM-Newton, Chandra, and ROSAT. The combined sample, including that of the Subaru/XMM-Newton Deep Survey, consists of 4039 detections in the soft (0.5-2 keV) and/or hard (>2 keV) band. We utilize a maximum likelihood method to reproduce the count rate versus redshift distribution for each survey, by taking into account the evolution of the absorbed fraction, the contribution from Compton-thick (CTK) AGNs, and broadband spectra of AGNs, including reflection components from tori based on the luminosity- and redshift-dependent unified scheme. We find that the shape of the XLF at z ∼ 1-3 is significantly different from that in the local universe, for which the luminosity-dependent density evolution model gives much better description than the luminosity and density evolution model. These results establish the standard population synthesis model of the X-ray background (XRB), which well reproduces the source counts, the observed fractions of CTK AGNs, and the spectrum of the hard XRB. The number ratio of CTK AGNs to the absorbed Compton-thin (CTN) AGNs is constrained to be ≈0.5-1.6 to produce the 20-50 keV XRB intensity within present uncertainties, by assuming that they follow the same evolution as CTN AGNs. The growth history of supermassive black holes is discussed based on the new AGN bolometric luminosity function.

The x-ray luminous galaxy cluster population at 0.9 < z ≲ 1.6 as revealed by the XMM-Newton Distant Cluster Project

International Nuclear Information System (INIS)

Fassbender, R; Böhringer, H; Nastasi, A; Šuhada, R; Mühlegger, M; Mohr, J J; Pierini, D; De Hoon, A; Kohnert, J; Lamer, G; Schwope, A D; Pratt, G W; Quintana, H; Rosati, P; Santos, J S

2011-01-01

We present the largest sample to date of spectroscopically confirmed x-ray luminous high-redshift galaxy clusters comprising 22 systems in the range 0.9 2 of non-contiguous deep archival XMM-Newton coverage, of which 49.4 deg 2 are part of the core survey with a quantifiable selection function and 17.7 deg 2 are classified as ‘gold’ coverage as the starting point for upcoming cosmological applications. Distant cluster candidates were followed up with moderately deep optical and near-infrared imaging in at least two bands to photometrically identify the cluster galaxy populations and obtain redshift estimates based on the colors of simple stellar population models. We test and calibrate the most promising redshift estimation techniques based on the R-z and z-H colors for efficient distant cluster identifications and find a good redshift accuracy performance of the z-H color out to at least z ∼ 1.5, while the redshift evolution of the R-z color leads to increasingly large uncertainties at z ≳ 0.9. Photometrically identified high-z systems are spectroscopically confirmed with VLT/FORS 2 with a minimum of three concordant cluster member redshifts. We present first details of two newly identified clusters, XDCP J0338.5+0029 at z = 0.916 and XDCP J0027.2+1714 at z = 0.959, and investigate the x-ray properties of SpARCS J003550-431224 at z = 1.335, which shows evidence for ongoing major merger activity along the line-of-sight. We provide x-ray properties and luminosity-based total mass estimates for the full sample of 22 high-z clusters, of which 17 are at z ⩾ 1.0 and seven populate the highest redshift bin at z > 1.3. The median system mass of the sample is M 200 ≃ 2 × 10 14 M ⊙ , while the probed mass range for the distant clusters spans approximately (0.7-7) × 10 14 M ⊙ . The majority (>70%) of the x-ray selected clusters show rather regular x-ray morphologies, albeit in most cases with a discernible elongation along one axis. In contrast to

[The general survey for chondromalacia of 2,743 Chinese population].

Science.gov (United States)

Guo, K; Ye, Q; Zeng, X; Lin, J; Wu, Z

1998-06-01

To evaluate the distribution of chondromalacia patella in Chinese population. A random cluster sampling survey was performed covering 2,743 subjects varied in age, sex and occupation in 1995. The prevalence rate is 36.2%. The occurrence in women was higher than that in men (P chondromalacia patella in China.

Synthesis and antiinflammatory activity of some 2-arylamino-2-thiazoline-4-ones.

Science.gov (United States)

Lesyk, Roman; Zimenkovsky, Boris; Subtelna, Ivanna; Nektegayev, Igor; Kazmirchuk, Gennadij

2003-01-01

A mild and efficent method of synthesis of 2-arylamino-2-thiazoline-4-ones was established using 2-carboethoxymethylthio-2-thiazolin-4-one (II) as a key intermediate. Reaction of 2-carboethoxymethylthio-2-thiazolin-4-one with m- or p-aminophenole afforded 2-(3-or4-oxyphenylamino)-2-thiazoline-4-ones (V, XV). Condensation of V, XV with aromatic aldehydes, according to the Knoevenagel, gives respective 5-arylidene derivatives V-XIII, XVI-XXIX, which were obtained alternatively using m- or p-oxyarylthioureas. 5-Carboxymethylderivatives XIV, XXX were synthesized by condensation of arylthioureas and maleic anhydride in acetic acid. Quantum-chemical calculations were made to confirm the possibility of dynamic amino-imino tautomerism of synthesized compounds. Structure and tautomerism of the obtained substances were confirmed by UV, IR, MS and NMR spectra. Biological activity prediction using the computer program PASS C&T has been made. According to these prediction results, some compounds were tested in vivio for their antiinflammatory activity. 5-[2-Chloro-3-(4-nitrophenyl)-2-propenilidene]-2-(3-hydroxyanilino-2-thiazoline-4-one (XII) possess significant antiinflammatory effect in comparison with diclofenac sodium, aspirin, acetaminofen and phenylbutazone.

Special Session 2: Cosmic Evolution of Groups and Clusters

Science.gov (United States)

Vrtilek, J. M.; David, L. P.

2015-03-01

During the past decade observations across the electromagnetic spectrum have led to broad progress in the understanding of galaxy clusters and their far more abundant smaller siblings, groups. From the X-rays, where Chandra and XMM have illuminated old phenomena such as cooling cores and discovered new ones such as shocks, cold fronts, bubbles and cavities, through rich collections of optical data (including vast and growing arrays of redshifts), to the imaging of AGN outbursts of various ages through radio observations, our access to cluster and group measurements has leaped forward, while parallel advances in theory and modeling have kept pace. This Special Session offered a survey of progress to this point, an assessment of outstanding problems, and a multiwavelength overview of the uses of the next generation of observatories. Holding the symposium in conjuction with the XXVIIIth General Assembly provided the significant advantage of involving not only a specialist audience, but also interacting with a broad cross-section of the world astronomical community.

A ∼ 3.8 hr PERIODICITY FROM AN ULTRASOFT ACTIVE GALACTIC NUCLEUS CANDIDATE

Energy Technology Data Exchange (ETDEWEB)

Lin, Dacheng; Irwin, Jimmy A. [Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487 (United States); Godet, Olivier; Webb, Natalie A.; Barret, Didier, E-mail: dlin@ua.edu [CNRS, IRAP, 9 avenue du Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4 (France)

2013-10-10

Very few galactic nuclei are found to show significant X-ray quasi-periodic oscillations (QPOs). After carefully modeling the noise continuum, we find that the ∼3.8 hr QPO in the ultrasoft active galactic nucleus candidate 2XMM J123103.2+110648 was significantly detected (∼5σ) in two XMM-Newton observations in 2005, but not in the one in 2003. The QPO root mean square (rms) is very high and increases from ∼25% in 0.2-0.5 keV to ∼50% in 1-2 keV. The QPO probably corresponds to the low-frequency type in Galactic black hole X-ray binaries, considering its large rms and the probably low mass (∼10{sup 5} M {sub ☉}) of the black hole in the nucleus. We also fit the soft X-ray spectra from the three XMM-Newton observations and find that they can be described with either pure thermal disk emission or optically thick low-temperature Comptonization. We see no clear X-ray emission from the two Swift observations in 2013, indicating lower source fluxes than those in XMM-Newton observations.

Radio/X-ray monitoring of the broad-line radio galaxy 3C 382. High-energy view with XMM-Newtonand NuSTAR

Science.gov (United States)

Ursini, F.; Petrucci, P.-O.; Matt, G.; Bianchi, S.; Cappi, M.; Dadina, M.; Grandi, P.; Torresi, E.; Ballantyne, D. R.; De Marco, B.; De Rosa, A.; Giroletti, M.; Malzac, J.; Marinucci, A.; Middei, R.; Ponti, G.; Tortosa, A.

2018-05-01

We present the analysis of five joint XMM-Newton/NuSTARobservations, 20 ks each and separated by 12 days, of the broad-line radio galaxy 3C 382. The data were obtained as part of a campaign performed in September-October 2016 simultaneously with VLBA. The radio data and their relation with the X-ray ones will be discussed in a following paper. The source exhibits a moderate flux variability in the UV/X-ray bands, and a limited spectral variability especially in the soft X-ray band. In agreement with past observations, we find the presence of a warm absorber, an iron Kα line with no associated Compton reflection hump, and a variable soft excess well described by a thermal Comptonization component. The data are consistent with a "two-corona" scenario, in which the UV emission and soft excess are produced by a warm (kT ≃ 0.6 keV), optically thick (τ ≃ 20) corona consistent with being a slab fully covering a nearly passive accretion disc, while the hard X-ray emission is due to a hot corona intercepting roughly 10% of the soft emission. These results are remarkably similar to those generally found in radio-quiet Seyferts, thus suggesting a common accretion mechanism.

Intracranial Hemorrhage: A Devastating Outcome of Congenital Bleeding Disorders-Prevalence, Diagnosis, and Management, with a Special Focus on Congenital Factor XIII Deficiency.

Science.gov (United States)

Alavi, Seyed Ezatolla Rafiee; Jalalvand, Masumeh; Assadollahi, Vahideh; Tabibian, Shadi; Dorgalaleh, Akbar

2018-04-01

Intracranial hemorrhage (ICH) is a medical emergency. In congenital bleeding disorders, ICH is a devastating presentation accompanied with a high rate of morbidity and mortality. The prevalence of ICH is highly variable among congenital bleeding disorders, with the highest incidence observed in factor (F) XIII deficiency (FXIIID) (∼30%). This life-threatening presentation is less common in afibrinogenemia, FVIII, FIX, FVII, and FX deficiencies, and is rare in severe FV and FII deficiencies, type 3 von Willebrand disease and inherited platelet function disorders (IPFDs). In FXIIID, this diathesis most often occurs after trauma in children, whereas spontaneous ICH is more frequent in adults. About 15% of patients with FXIIID and ICH die; the bleeding causes 80% of deaths in this coagulopathy. Although in FXIIID, the bleed most commonly is intraparenchymal (> 90%), epidural, subdural, and subarachnoid hemorrhages also have been reported, albeit rarely. As this life-threatening bleeding causes neurological complications, early diagnosis can prevent further expansion of the hematoma and secondary damage. Neuroimaging plays a crucial role in the diagnosis of ICH, but signs and symptoms in patients with severe FXIIID should trigger replacement therapy even before establishment of the diagnosis. Although a high dose of FXIII concentrate can reduce the rate of morbidity and mortality of ICH in FXIIID, it may occasionally trigger inhibitor development, thus complicating ICH management and future prophylaxis. Nevertheless, replacement therapy is the mainstay of treatment for ICH in FXIIID. Neurosurgery is performed in patients with FXIIID and epidural hematoma and a hemorrhage diameter exceeding 2 cm or a volume of ICH is more than 30 cm 3 . Contact sports are not recommended in people with FXIIID as they can elicit ICH. However, a considerable number of safe sports and activities have been suggested to have more benefits than dangers for patients with congenital bleeding

Hubble Space Telescope Snapshot Survey for Resolved Companions of Galactic Cepheids

Science.gov (United States)

Evans, Nancy Remage; Bond, Howard E.; Schaefer, Gail H.; Mason, Brian D.; Tingle, Evan; Karovska, Margarita; Pillitteri, Ignazio

2016-05-01

We have conducted an imaging survey with the Hubble Space Telescope Wide Field Camera 3 (WFC3) of 70 Galactic Cepheids, typically within 1 kpc, with the aim of finding resolved physical companions. The WFC3 field typically covers the 0.1 pc area where companions are expected. In this paper, we identify 39 Cepheids having candidate companions, based on their positions in color-magnitude diagrams, and having separations ⩾ 5'' from the Cepheids. We use follow-up observations of 14 of these candidates with XMM-Newton, and of one of them with ROSAT, to separate X-ray-active young stars (probable physical companions) from field stars (chance alignments). Our preliminary estimate, based on the optical and X-ray observations, is that only 3% of the Cepheids in the sample have wide companions. Our survey easily detects resolved main-sequence companions as faint as spectral type K. Thus the fact that the two most probable companions (those of FF Aql and RV Sco) are earlier than type K is not simply a function of the detection limit. We find no physical companions having separations larger than 4000 au in the X-ray survey. Two Cepheids are exceptions in that they do have young companions at significantly larger separations (δ Cep and S Nor), but both belong to a cluster or a loose association, so our working model is that they are not gravitationally bound binary members, but rather cluster/association members. All of these properties provide constraints on both star formation and subsequent dynamical evolution. The low frequency of true physical companions at separations > 5'' is confirmed by examination of the subset of the nearest Cepheids and also the density of the fields. Based on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.

The Physical Relation between Disc and Coronal Emission in Quasars

Directory of Open Access Journals (Sweden)

Elisabeta Lusso

2018-01-01

Full Text Available We propose a modified version of the observed non-linear relation between the X-ray (2 keV and the ultraviolet (2,500 Å emission in quasars (i.e., LX∝LUVγ which involves the full width at half-maximum, FWHM, of the broad emission line, i.e., LX∝LUVγ^ FWHMβ^. By analyzing a sample of 550 optically selected non-jetted quasars in the redshift range of 0.36–2.23 from the Sloan Digital Sky Survey cross matched with the XMM-Newton catalog 3XMM-DR6, we found that the additional dependence of the observed LX − LUV correlation on the FWHM of the Mgii broad emission line is statistically significant. Our statistical analysis leads to a much tighter relation with respect to the one neglecting FWHM, and it does not evolve with redshift. We interpret this new relation within an accretion disc corona scenario where reconnection and magnetic loops above the accretion disc can account for the production of the primary X-ray radiation. For a broad line region size depending on the disc luminosity as Rblr∝Ldisc0.5, we find that LX∝LUV4/7 FWHM4/7, which is in very good agreement with the observed correlation.

Resolved Companions of Cepheids: Testing the Candidates with X-Ray Observations

Science.gov (United States)

Evans, Nancy Remage; Pillitteri, Ignazio; Wolk, Scott; Karovska, Margarita; Tingle, Evan; Guinan, Edward; Engle, Scott; Bond, Howard E.; Schaefer, Gail H.; Mason, Brian D.

2016-04-01

We have made XMM-Newton observations of 14 Galactic Cepheids that have candidate resolved (≥5″) companion stars based on our earlier HST Wide Field Camera 3 (WFC3) imaging survey. Main-sequence stars that are young enough to be physical companions of Cepheids are expected to be strong X-ray producers in contrast to field stars. XMM-Newton exposures were set to detect essentially all companions hotter than spectral type M0 (corresponding to 0.5 M⊙). The large majority of our candidate companions were not detected in X-rays, and hence are not confirmed as young companions. One resolved candidate (S Nor #4) was unambiguously detected, but the Cepheid is a member of a populous cluster. For this reason, it is likely that S Nor #4 is a cluster member rather than a gravitationally bound companion. Two further Cepheids (S Mus and R Cru) have X-ray emission that might be produced by either the Cepheid or the candidate resolved companion. A subsequent Chandra observation of S Mus shows that the X-rays are at the location of the Cepheid/spectroscopic binary. R Cru and also V659 Cen (also X-ray bright) have possible companions closer than 5″ (the limit for this study) which are the likely sources of X-rays. One final X-ray detection (V473 Lyr) has no known optical companion, so the prime suspect is the Cepheid itself. It is a unique Cepheid with a variable amplitude. The 14 stars that we observed with XMM constitute 36% of the 39 Cepheids found to have candidate companions in our HST/WFC3 optical survey. No young probable binary companions were found with separations of ≥5″ or 4000 au. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).

RELIABLE IDENTIFICATIONS OF ACTIVE GALACTIC NUCLEI FROM THE WISE, 2MASS, AND ROSAT ALL-SKY SURVEYS

International Nuclear Information System (INIS)

Edelson, R.; Malkan, M.

2012-01-01

We have developed the ''S IX '' statistic to identify bright, highly likely active galactic nucleus (AGN) candidates solely on the basis of Wide-field Infrared Survey Explorer (WISE), Two Micron All-Sky Survey (2MASS), and ROSAT all-sky survey (RASS) data. This statistic was optimized with data from the preliminary WISE survey and the Sloan Digital Sky Survey, and tested with Lick 3 m Kast spectroscopy. We find that sources with S IX 95% likelihood of being an AGN (defined in this paper as a Seyfert 1, quasar, or blazar). This statistic was then applied to the full WISE/2MASS/RASS dataset, including the final WISE data release, to yield the ''W2R'' sample of 4316 sources with S IX 2 , permitting construction of AGN samples in any sufficiently large region of sky.

DETECTING THE WARM-HOT INTERGALACTIC MEDIUM THROUGH X-RAY ABSORPTION LINES

Energy Technology Data Exchange (ETDEWEB)

Yao Yangsen; Shull, J. Michael; Cash, Webster [Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309 (United States); Wang, Q. Daniel, E-mail: yaoys@colorado.edu [Department of Astronomy, University of Massachusetts, Amherst, MA 01003 (United States)

2012-02-20

The warm-hot intergalactic medium (WHIM) at temperatures 10{sup 5}-10{sup 7} K is believed to contain 30%-50% of the baryons in the local universe. However, all current X-ray detections of the WHIM at redshifts z > 0 are of low statistical significance ({approx}< 3{sigma}) and/or controversial. In this work, we aim to establish the detection limits of current X-ray observatories and explore requirements for next-generation X-ray telescopes for studying the WHIM through X-ray absorption lines. We analyze all available grating observations of Mrk 421 and obtain spectra with signal-to-noise ratios (S/Ns) of {approx}90 and 190 per 50 mA spectral bin from Chandra and XMM-Newton observations, respectively. Although these spectra are two of the best ever collected with Chandra and XMM-Newton, we cannot confirm the two WHIM systems reported by Nicastro et al. in 2005. Our bootstrap simulations indicate that spectra with such high S/N cannot constrain the WHIM with O VII column densities N{sub Ovii}{approx}10{sup 15} cm{sup -2} (corresponding to an equivalent width of 2.5 mA for a Doppler velocity of 50 km s{sup -1}) at {approx}> 3{sigma} significance level. The simulation results also suggest that it would take >60 Ms for Chandra and 140 Ms for XMM-Newton to measure the N{sub Ovii} at {>=}4{sigma} from a spectrum of a background QSO with flux of {approx}0.2 mCrab (1 Crab = 2 Multiplication-Sign 10{sup -8} erg s{sup -1} cm{sup -2} at 0.5-2 keV). Future X-ray spectrographs need to be equipped with spectral resolution R {approx} 4000 and effective area A {>=} 100 cm{sup 2} to accomplish the similar constraints with an exposure time of {approx}2 Ms and would require {approx}11 Ms to survey the 15 QSOs with flux {approx}> 0.2 mCrab along which clear intergalactic O VI absorbers have been detected.

The 2.3 GHz continuum survey of the GEM project

Science.gov (United States)

Tello, C.; Villela, T.; Torres, S.; Bersanelli, M.; Smoot, G. F.; Ferreira, I. S.; Cingoz, A.; Lamb, J.; Barbosa, D.; Perez-Becker, D.; Ricciardi, S.; Currivan, J. A.; Platania, P.; Maino, D.

2013-08-01

Context. Determining the spectral and spatial characteristics of the radio continuum of our Galaxy is an experimentally challenging endeavour for improving our understanding of the astrophysics of the interstellar medium. This knowledge has also become of paramount significance for cosmology, since Galactic emission is the main source of astrophysical contamination in measurements of the cosmic microwave background (CMB) radiation on large angular scales. Aims: We present a partial-sky survey of the radio continuum at 2.3GHz within the scope of the Galactic Emission Mapping (GEM) project, an observational program conceived and developed to reveal the large-scale properties of Galactic synchrotron radiation through a set of self-consistent surveys of the radio continuum between 408MHz and 10GHz. Methods: The GEM experiment uses a portable and double-shielded 5.5-m radiotelescope in altazimuthal configuration to map 60-degree-wide declination bands from different observational sites by circularly scanning the sky at zenithal angles of 30° from a constantly rotating platform. The observations were accomplished with a total power receiver, whose front-end high electron mobility transistor (HEMT) amplifier was matched directly to a cylindrical horn at the prime focus of the parabolic reflector. The Moon was used to calibrate the antenna temperature scale and the preparation of the map required direct subtraction and destriping algorithms to remove ground contamination as the most significant source of systematic error. Results: We used 484 h of total intensity observations from two locations in Colombia and Brazil to yield 66% sky coverage from to . The observations in Colombia were obtained with a horizontal HPBW of and a vertical HPBW of . The pointing accuracy was and the RMS sensitivity was 11.42 mK. The observations in Brazil were obtained with a horizontal HPBW of and a vertical HPBW of . The pointing accuracy was and the RMS sensitivity was 8.24 mK. The zero

Implications of the Utopia Gravity Anomaly for the Resurfacing of the Northern Plains of Mars

Science.gov (United States)

Banerdt, W. B.

2004-01-01

Whereas the surface units of the northern plain of Mars generally exhibit ages ranging from late Hesperian to Amazonian, interpretation of precise topographic measurements indicate that the age of the underlying "basement" is early Noachian, or almost as old as the southern highlands. This suggests that widespread but relatively superficial resurfacing has occurred throughout the northern plains since the end of early heavy bombardment. In this abstract I examine some of the possible implications of the subsurface structure inferred for the Utopia basin from gravity data on the nature of this resurfacing. The large, shallow, circular depression in Utopia Planitia has been identified as a huge impact basin, based on both geological evidence and detailed analysis of MOLA topography. Its diameter (approx. 3000 km) is equivalent to that of the Hellas basin, as is its inferred age (early Noachian). However, whereas Hellas is extremely deep with rough terrain and large slopes, the Utopia basin is a smooth, shallow, almost imperceptible bowl. Conversely, Utopia displays one of the largest (non-Tharsis-related) positive geoid anomalies on Mars, in contrast to a much more subdued negative anomaly over Hellas.

Relative effects of plasma, fibrinogen concentrate, and factor XIII on ROTEM coagulation profiles in an in vitro model of massive transfusion in trauma.

Science.gov (United States)

Schmidt, David E; Halmin, Märit; Wikman, Agneta; Östlund, Anders; Ågren, Anna

2017-10-01

Massive traumatic haemorrhage is aggravated through the development of trauma-induced coagulopathy, which is managed by plasma transfusion and/or fibrinogen concentrate administration. It is yet unclear whether these treatments are equally potent in ensuring adequate haemostasis, and whether additional factor XIII (FXIII) administration provides further benefits. In this study, we compared ROTEM whole blood coagulation profiles after experimental massive transfusion with different transfusion regimens in an in vitro model of dilution- and transfusion-related coagulopathy. Healthy donor blood was mixed 1 + 1 with six different transfusion regimens. Each regimen contained RBC, platelet concentrate, and either fresh frozen plasma (FFP) or Ringer's acetate (RA). The regimens were further augmented through addition of a low- or medium-dose fibrinogen concentrate and FXIII. Transfusion with FFP alone was insufficient to maintain tissue-factor activated clot strength, coincidental with a deficiency in fibrin-based clot strength. Fibrinogen concentrate conserved, but did not improve coagulation kinetics and overall clot strength. Only combination therapy with FFP and low-dose fibrinogen concentrate improved both coagulation kinetics and fibrin-based clot strength. Administration of FXIII did not result in an improvement of clot strength. In conclusion, combination therapy with both FFP and low-dose fibrinogen concentrate improved clotting time and produced firm clots, representing a possible preferred first-line regimen to manage trauma-induced coagulopathy when RBC and platelets are also transfused. Further research is required to identify optimal first-line transfusion fluids for massive traumatic haemorrhage.

Dwarfs Cooler Than M: The Definition of Spectral Type L Using Discoveries from the 2-Micron All-Sky Survey (2MASS)

Science.gov (United States)

Kirkpatrick, J.; Reid, I.; Liebert, J.; Cutri, R.; Nelson, B.; Beichman, C.; Dahn, C.; Monet, D.; Gizis, J.; Skrutskie, M.

1998-01-01

Before the 2-Micron All-Sky Survey (2MASS) began, only six objects were known with spectral types later than M9.5 V. In the first 371 sq. deg. of actual 2MASS survey data, we have identified another twenty such objects spectroscopically confirmed using the Low Resolution Imaging Spectrograph (LRIS) at the W.M. Keck Observatory.

SPLASH-SXDF Multi-wavelength Photometric Catalog

Science.gov (United States)

Mehta, Vihang; Scarlata, Claudia; Capak, Peter; Davidzon, Iary; Faisst, Andreas; Hsieh, Bau Ching; Ilbert, Olivier; Jarvis, Matt; Laigle, Clotilde; Phillips, John; Silverman, John; Strauss, Michael A.; Tanaka, Masayuki; Bowler, Rebecca; Coupon, Jean; Foucaud, Sébastien; Hemmati, Shoubaneh; Masters, Daniel; McCracken, Henry Joy; Mobasher, Bahram; Ouchi, Masami; Shibuya, Takatoshi; Wang, Wei-Hao

2018-04-01

We present a multi-wavelength catalog in the Subaru/XMM-Newton Deep Field (SXDF) as part of the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH). We include the newly acquired optical data from the Hyper-Suprime-Cam Subaru Strategic Program, accompanied by IRAC coverage from the SPLASH survey. All available optical and near-infrared data is homogenized and resampled on a common astrometric reference frame. Source detection is done using a multi-wavelength detection image including the u-band to recover the bluest objects. We measure multi-wavelength photometry and compute photometric redshifts as well as physical properties for ∼1.17 million objects over ∼4.2 deg2, with ∼800,000 objects in the 2.4 deg2 HSC-Ultra-Deep coverage. Using the available spectroscopic redshifts from various surveys over the range of 0 fraction of 3.2%. The SPLASH-SXDF catalog is a valuable, publicly available resource, perfectly suited for studying galaxies in the early universe and tracing their evolution through cosmic time.

NuSTAR Reveals Extreme Absorption in z < 0.5 Type 2 Quasars

Science.gov (United States)

Lansbury, G. B.; Gandhi, P.; Alexander, D. M.; Assef, R. J.; Aird, J.; Annuar, A.; Ballantyne, D. R.; Baloković, M.; Bauer, F. E.; Boggs, S. E.; Brandt, W. N.; Brightman, M.; Christensen, F. E.; Civano, F.; Comastri, A.; Craig, W. W.; Del Moro, A.; Grefenstette, B. W.; Hailey, C. J.; Harrison, F. A.; Hickox, R. C.; Koss, M.; LaMassa, S. M.; Luo, B.; Puccetti, S.; Stern, D.; Treister, E.; Vignali, C.; Zappacosta, L.; Zhang, W. W.

2015-08-01

The intrinsic column density (NH) distribution of quasars is poorly known. At the high obscuration end of the quasar population and for redshifts z 1.5 × 1024 cm-2) type 2 quasars (CTQSO2s); five new NuSTAR observations are reported herein, and four have been previously published. The candidate CTQSO2s lie at z < 0.5, have observed [O iii] luminosities in the range 8.4\\lt {log}({L}[{{O} {{III}}]}/{L}⊙ )\\lt 9.6, and show evidence for extreme, Compton-thick absorption when indirect absorption diagnostics are considered. Among the nine candidate CTQSO2s, five are detected by NuSTAR in the high-energy (8-24 keV) band: two are weakly detected at the ≈3σ confidence level and three are strongly detected with sufficient counts for spectral modeling (≳90 net source counts at 8-24 keV). For these NuSTAR-detected sources direct (i.e., X-ray spectral) constraints on the intrinsic active galactic nucleus properties are feasible, and we measure column densities ≈2.5-1600 times higher and intrinsic (unabsorbed) X-ray luminosities ≈10-70 times higher than pre-NuSTAR constraints from Chandra and XMM-Newton. Assuming the NuSTAR-detected type 2 quasars are representative of other Compton-thick candidates, we make a correction to the NH distribution for optically selected type 2 quasars as measured by Chandra and XMM-Newton for 39 objects. With this approach, we predict a Compton-thick fraction of {f}{CT}={36}-12+14 %, although higher fractions (up to 76%) are possible if indirect absorption diagnostics are assumed to be reliable.

Radiation Effects on Polymers - XIII

DEFF Research Database (Denmark)

El-Awady, N. I.; Ghanem, N. A.; Bo, P.

1979-01-01

Using computerized programs, the water flux and salt rejection properties in reverse osmosis of cellulose acetate-g-acrylamide membranes are determined. Comparisons are made with ungrafted commercial cellulose acetate membranes, using 0.1 and 1.0 M sodium chloride, sodium sulphate and ammonium su...... sulphate solutions. The grafted cellulose acetates show improved water flux but reduced NaCl rejection. However, they show promising prospects in bigger ion separation as for Na2SO4 and (NH4)2SO4 solutions....

Effect of Factor XIII-A G185T Polymorphism on Visual Prognosis after Photodynamic Therapy for Neovascular Macular Degeneration

Directory of Open Access Journals (Sweden)

Francesco Parmeggiani

2015-08-01

Full Text Available Macular degenerations represent leading causes of central blindness or low vision in developed countries. Most of these severe visual disabilities are due to age-related macular degeneration (AMD and pathologic myopia (PM, both of which are frequently complicated by subfoveal choroidal neovascularization (CNV. Photodynamic therapy with verteporfin (PDT-V is still employed for CNV treatment in selected cases or in combined regimen. In Caucasian patients, the common polymorphism G185T of factor XIII-A gene (FXIII-A-G185T; rs5985 has been described as predictor of poor angiographic CNV responsiveness to PDT-V. Nevertheless, the prognostic implications of this pharmacogenetic determinant on long-term visual outcome after a PDT-V regimen have not been evaluated. We retrospectively selected Caucasian patients presenting with treatment-naive CNV and receiving standardized PDT-V protocol for two years. The study population included patients affected by subfoveal CNV secondary to AMD or PM. We assessed the correlations between the polymorphic allele T of FXIII-A-G185T and: (1 total number of photodynamic treatments; and (2 change in visual acuity from baseline to the end of the follow-up period. Considering a total study population of 412 patients with neovascular AMD or PM, the carriers of 185 T-allele of FXIII-A (GT or TT genotype received a higher number of photodynamic treatments than patients without it (GG wild-type genotype (p < 0.01; mean number of PDT-V: 5.51 vs. 3.76, respectively. Moreover, patients with 185 T-allele of FXIII-A had a more marked worsening of visual acuity at 24 months than those with the GG-185 wild genotype (p < 0.01; mean difference in logMAR visual acuity: 0.22 vs. 0.08, respectively. The present findings show that the G185T polymorphism of the FXIII-A gene is associated with significant differences in the long-term therapeutic outcomes of patients treated with standardized PDT-V protocol. The comprehensive appraisal of

Las armas de los Limia y sus derivaciones (siglos XIII-XV

Directory of Open Access Journals (Sweden)

Eduardo PARDO DE GUEVARA Y VALDÉS

2011-07-01

Full Text Available En los primeros tiempos del fenómeno emblemático-heráldico, la adopción de unas armerías no respondía a un proceso reflexivo, tal y como ahora parecería natural, sino a unos impulsos espontáneos, en los que predominaba el simple gusto o capricho, cuando no la directa imitación o aceptación de modelos ya existentes, con independencia de la significación o valor social que se les reconociera. Un buen testimonio de ello lo ofrecen las armas traídas ya antes de mediar el siglo XIII por el linaje renombrado Limia, cuyo análisis ofrece lecturas interesantes para comprender el sentido y alcance de estos procedimientos habituales. Como se trata aquí, los palos y palados de los Limia fueron traídos después por los Valcárcel y, más tarde, por un pequeño número de linajes de ellos derivados, aunque las modificaciones introducidas parecen ocultar este origen: las varillas de los Varela, las correas de los Isorna, las lanzas parlantes de los Lanzós -o Lanzones- o las estacas de los Quiroga, así como la losa de los Losada y las fórmulas fusionadas de palos y calderas, cuyo inicio pudo estar en los Biedma y que no tardaría en identificar también al grupo de los Taboada y Noguerol.Aux premiers temps du phénomène emblématique-héraldique, l’adoption d'armoiries répondait moins à un processus réfléchi comme on s’y attendrait aujourd’hui, qu’à des élans spontanés guidés par le simple plaisir ou le caprice, ou même par l’imitation ou l’adoption de quelques modèles déjà existants, indépendamment de la signification ou de la valeur sociale qu’on pourrait leur reconnaître. Tel est le cas des armes portées dans la première moitié du XIIIe siècle par le lignage des Limia, dont l’analyse permet de  comprendre le sens et la portée de ces procédés. Comme il sera dit dans cette étude, les pals et palés des Limia ont été ensuite portés par les Valcárcel et, plus tard, par un petit nombre de lignages

The Complete Calibration of the Color–Redshift Relation (C3R2) Survey: Survey Overview and Data Release 1

Energy Technology Data Exchange (ETDEWEB)

Masters, Daniel C. [Infrared Processing and Analysis Center, Pasadena, CA 91125 (United States); Stern, Daniel K.; Rhodes, Jason D. [Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States); Cohen, Judith G. [California Institute of Technology, Pasadena, CA 91125 (United States); Capak, Peter L. [Spitzer Science Center, Pasadena, CA 91125 (United States); Castander, Francisco J. [Institut de Ciències de lEspai (ICE, IEEC/CSIC), E-08193 Bellaterra (Barcelona) (Spain); Paltani, Stéphane [Department of Astronomy, University of Geneva, Ch. dEcogia 16, 1290 Versoix (Switzerland)

2017-06-01

A key goal of the Stage IV dark energy experiments Euclid , LSST, and WFIRST is to measure the growth of structure with cosmic time from weak lensing analysis over large regions of the sky. Weak lensing cosmology will be challenging: in addition to highly accurate galaxy shape measurements, statistically robust and accurate photometric redshift (photo- z ) estimates for billions of faint galaxies will be needed in order to reconstruct the three-dimensional matter distribution. Here we present an overview of and initial results from the Complete Calibration of the Color–Redshift Relation (C3R2) survey, which is designed specifically to calibrate the empirical galaxy color–redshift relation to the Euclid depth. These redshifts will also be important for the calibrations of LSST and WFIRST . The C3R2 survey is obtaining multiplexed observations with Keck (DEIMOS, LRIS, and MOSFIRE), the Gran Telescopio Canarias (GTC; OSIRIS), and the Very Large Telescope (VLT; FORS2 and KMOS) of a targeted sample of galaxies that are most important for the redshift calibration. We focus spectroscopic efforts on undersampled regions of galaxy color space identified in previous work in order to minimize the number of spectroscopic redshifts needed to map the color–redshift relation to the required accuracy. We present the C3R2 survey strategy and initial results, including the 1283 high-confidence redshifts obtained in the 2016A semester and released as Data Release 1.

The Complete Calibration of the Color–Redshift Relation (C3R2) Survey: Survey Overview and Data Release 1

International Nuclear Information System (INIS)

Masters, Daniel C.; Stern, Daniel K.; Rhodes, Jason D.; Cohen, Judith G.; Capak, Peter L.; Castander, Francisco J.; Paltani, Stéphane

2017-01-01

A key goal of the Stage IV dark energy experiments Euclid , LSST, and WFIRST is to measure the growth of structure with cosmic time from weak lensing analysis over large regions of the sky. Weak lensing cosmology will be challenging: in addition to highly accurate galaxy shape measurements, statistically robust and accurate photometric redshift (photo- z ) estimates for billions of faint galaxies will be needed in order to reconstruct the three-dimensional matter distribution. Here we present an overview of and initial results from the Complete Calibration of the Color–Redshift Relation (C3R2) survey, which is designed specifically to calibrate the empirical galaxy color–redshift relation to the Euclid depth. These redshifts will also be important for the calibrations of LSST and WFIRST . The C3R2 survey is obtaining multiplexed observations with Keck (DEIMOS, LRIS, and MOSFIRE), the Gran Telescopio Canarias (GTC; OSIRIS), and the Very Large Telescope (VLT; FORS2 and KMOS) of a targeted sample of galaxies that are most important for the redshift calibration. We focus spectroscopic efforts on undersampled regions of galaxy color space identified in previous work in order to minimize the number of spectroscopic redshifts needed to map the color–redshift relation to the required accuracy. We present the C3R2 survey strategy and initial results, including the 1283 high-confidence redshifts obtained in the 2016A semester and released as Data Release 1.

Constraints on Modified Gravity from the Abundance of X-ray Luminous Galaxy Clusters

DEFF Research Database (Denmark)

Rapetti Serra, David Angelo

2011-01-01

n December 2010, the XXL survey, an XMM-Newton Very Large Programme, has been granted time to map two extragalactic regions of 25 deg2, at a depth of ~5×10-15 erg/cm2/s (using 10 ks observations). While the main goal of the project is to constrain the Dark Energy equation of state using clusters...... of galaxies (cf. http://arxiv.org/abs/1009.3182), it will also have lasting legacy value for cluster scaling laws and studies of AGNs and XRB. The project is open to any scientist belonging to the international astronomical community, and interested in actively contributing to the general legacy effort...

The Environmental Assessment and Management (TEAM) Guide: Colorado Supplement

Science.gov (United States)

2010-03-01

Nest c. Flattops d. Great Sand Dunes e. La Garita f. Maroon Bells -- Snowmass g. Mount Zirkel h. Rawah i. Weminuche j. West Elk B. All...of Sections XIII.D., XIII.E., or XIII.F.: 1. National Monuments a. Florissant Fossil Beds b. Colorado c. Dinosaur d. Great Sand Dunes (those...that the minimum distance between tanks and toe of interior dike walls is 5 ft (1.5 m). Verify that drains for diked area are controlled in a manner so

Development of Vertical Cable Seismic System for Hydrothermal Deposit Survey (2) - Feasibility Study

Science.gov (United States)

Asakawa, E.; Murakami, F.; Sekino, Y.; Okamoto, T.; Mikada, H.; Takekawa, J.; Shimura, T.

2010-12-01

In 2009, Ministry of Education, Culture, Sports, Science and Technology(MEXT) started the survey system development for Hydrothermal deposit. We proposed the Vertical Cable Seismic (VCS), the reflection seismic survey with vertical cable above seabottom. VCS has the following advantages for hydrothermal deposit survey. . (1) VCS is an effective high-resolution 3D seismic survey within limited area. (2) It achieves high-resolution image because the sensors are closely located to the target. (3) It avoids the coupling problems between sensor and seabottom that cause serious damage of seismic data quality. (4) Various types of marine source are applicable with VCS such as sea-surface source (air gun, water gun etc.) , deep-towed or ocean bottom sources. (5) Autonomous recording system. Our first experiment of 2D/3D VCS surveys has been carried out in Lake Biwa, JAPAN. in November 2009. The 2D VCS data processing follows the walk-away VSP, including wave field separation and depth migration. The result gives clearer image than the conventional surface seismic. Prestack depth migration is applied to 3D data to obtain good quality 3D depth volume. Uncertainty of the source/receiver poisons in water causes the serious problem of the imaging. We used several transducer/transponder to estimate these positions. The VCS seismic records themselves can also provide sensor position using the first break of each trace and we calibrate the positions. We are currently developing the autonomous recording VCS system and planning the trial experiment in actual ocean to establish the way of deployment/recovery and the examine the position through the current flow in November, 2010. The second VCS survey will planned over the actual hydrothermal deposit with deep-towed source in February, 2011.

Revival of the Magnetar PSR J1622–4950: Observations with MeerKAT, Parkes, XMM-Newton, Swift, Chandra, and NuSTAR

Science.gov (United States)

Camilo, F.; Scholz, P.; Serylak, M.; Buchner, S.; Merryfield, M.; Kaspi, V. M.; Archibald, R. F.; Bailes, M.; Jameson, A.; van Straten, W.; Sarkissian, J.; Reynolds, J. E.; Johnston, S.; Hobbs, G.; Abbott, T. D.; Adam, R. M.; Adams, G. B.; Alberts, T.; Andreas, R.; Asad, K. M. B.; Baker, D. E.; Baloyi, T.; Bauermeister, E. F.; Baxana, T.; Bennett, T. G. H.; Bernardi, G.; Booisen, D.; Booth, R. S.; Botha, D. H.; Boyana, L.; Brederode, L. R. S.; Burger, J. P.; Cheetham, T.; Conradie, J.; Conradie, J. P.; Davidson, D. B.; De Bruin, G.; de Swardt, B.; de Villiers, C.; de Villiers, D. I. L.; de Villiers, M. S.; de Villiers, W.; De Waal, C.; Dikgale, M. A.; du Toit, G.; du Toit, L. J.; Esterhuyse, S. W. P.; Fanaroff, B.; Fataar, S.; Foley, A. R.; Foster, G.; Fourie, D.; Gamatham, R.; Gatsi, T.; Geschke, R.; Goedhart, S.; Grobler, T. L.; Gumede, S. C.; Hlakola, M. J.; Hokwana, A.; Hoorn, D. H.; Horn, D.; Horrell, J.; Hugo, B.; Isaacson, A.; Jacobs, O.; Jansen van Rensburg, J. P.; Jonas, J. L.; Jordaan, B.; Joubert, A.; Joubert, F.; Józsa, G. I. G.; Julie, R.; Julius, C. C.; Kapp, F.; Karastergiou, A.; Karels, F.; Kariseb, M.; Karuppusamy, R.; Kasper, V.; Knox-Davies, E. C.; Koch, D.; Kotzé, P. P. A.; Krebs, A.; Kriek, N.; Kriel, H.; Kusel, T.; Lamoor, S.; Lehmensiek, R.; Liebenberg, D.; Liebenberg, I.; Lord, R. T.; Lunsky, B.; Mabombo, N.; Macdonald, T.; Macfarlane, P.; Madisa, K.; Mafhungo, L.; Magnus, L. G.; Magozore, C.; Mahgoub, O.; Main, J. P. L.; Makhathini, S.; Malan, J. A.; Malgas, P.; Manley, J. R.; Manzini, M.; Marais, L.; Marais, N.; Marais, S. J.; Maree, M.; Martens, A.; Matshawule, S. D.; Matthysen, N.; Mauch, T.; McNally, L. D.; Merry, B.; Millenaar, R. P.; Mjikelo, C.; Mkhabela, N.; Mnyandu, N.; Moeng, I. T.; Mokone, O. J.; Monama, T. E.; Montshiwa, K.; Moss, V.; Mphego, M.; New, W.; Ngcebetsha, B.; Ngoasheng, K.; Niehaus, H.; Ntuli, P.; Nzama, A.; Obies, F.; Obrocka, M.; Ockards, M. T.; Olyn, C.; Oozeer, N.; Otto, A. J.; Padayachee, Y.; Passmoor, S.; Patel, A. A.; Paula, S.; Peens-Hough, A.; Pholoholo, B.; Prozesky, P.; Rakoma, S.; Ramaila, A. J. T.; Rammala, I.; Ramudzuli, Z. R.; Rasivhaga, M.; Ratcliffe, S.; Reader, H. C.; Renil, R.; Richter, L.; Robyntjies, A.; Rosekrans, D.; Rust, A.; Salie, S.; Sambu, N.; Schollar, C. T. G.; Schwardt, L.; Seranyane, S.; Sethosa, G.; Sharpe, C.; Siebrits, R.; Sirothia, S. K.; Slabber, M. J.; Smirnov, O.; Smith, S.; Sofeya, L.; Songqumase, N.; Spann, R.; Stappers, B.; Steyn, D.; Steyn, T. J.; Strong, R.; Struthers, A.; Stuart, C.; Sunnylall, P.; Swart, P. S.; Taljaard, B.; Tasse, C.; Taylor, G.; Theron, I. P.; Thondikulam, V.; Thorat, K.; Tiplady, A.; Toruvanda, O.; van Aardt, J.; van Balla, T.; van den Heever, L.; van der Byl, A.; van der Merwe, C.; van der Merwe, P.; van Niekerk, P. C.; van Rooyen, R.; van Staden, J. P.; van Tonder, V.; van Wyk, R.; Wait, I.; Walker, A. L.; Wallace, B.; Welz, M.; Williams, L. P.; Xaia, B.; Young, N.; Zitha, S.

2018-04-01

New radio (MeerKAT and Parkes) and X-ray (XMM-Newton, Swift, Chandra, and NuSTAR) observations of PSR J1622–4950 indicate that the magnetar, in a quiescent state since at least early 2015, reactivated between 2017 March 19 and April 5. The radio flux density, while variable, is approximately 100× larger than during its dormant state. The X-ray flux one month after reactivation was at least 800× larger than during quiescence, and has been decaying exponentially on a 111 ± 19 day timescale. This high-flux state, together with a radio-derived rotational ephemeris, enabled for the first time the detection of X-ray pulsations for this magnetar. At 5%, the 0.3–6 keV pulsed fraction is comparable to the smallest observed for magnetars. The overall pulsar geometry inferred from polarized radio emission appears to be broadly consistent with that determined 6–8 years earlier. However, rotating vector model fits suggest that we are now seeing radio emission from a different location in the magnetosphere than previously. This indicates a novel way in which radio emission from magnetars can differ from that of ordinary pulsars. The torque on the neutron star is varying rapidly and unsteadily, as is common for magnetars following outburst, having changed by a factor of 7 within six months of reactivation.

Tracking the Iron Kα line and the Ultra Fast Outflow in NGC 2992 at different accretion states

Science.gov (United States)

Marinucci, A.; Bianchi, S.; Braito, V.; Matt, G.; Nardini, E.; Reeves, J.

2018-06-01

The Seyfert 2 galaxy NGC 2992 has been monitored eight times by XMM-Newton in 2010 and then observed again in 2013, while in 2015 it was simultaneously targeted by Swift and NuSTAR. XMM-Newton always caught the source in a faint state (2-10 keV fluxes ranging from 0.3 to 1.6× 10-11 erg cm-2 s-1) but NuSTAR showed an increase in the 2-10 keV flux up to 6× 10-11 erg cm-2 s-1. We find possible evidence of an Ultra Fast Outflow with velocity v1 = 0.21 ± 0.01c (detected at about 99% confidence level) in such a flux state. The UFO in NGC 2992 is consistent with being ejected at a few tens of gravitational radii only at accretion rates greater than 2% of the Eddington luminosity. The analysis of the low flux 2010/2013 XMM data allowed us to determine that the Iron Kα emission line complex in this object is likely the sum of three distinct components: a constant, narrow one due to reflection from cold, distant material (likely the molecular torus); a narrow, but variable one which is more intense in brighter observations and a broad relativistic one emitted in the innermost regions of the accretion disk, which has been detected only in the 2003 XMM observation.

On two reports associated with James Wood-Mason and Alfred William Alcock published by the Indian Museum and the Indian Marine Survey between 1890 and 1891: implications for malacostracan nomenclature.

Science.gov (United States)

Huys, Rony; Low, Martyn E Y; De Grave, Sammy; Ng, Peter K L; Clark, Paul F

2014-01-29

Two rare documents associated with the Indian Museum and the Indian Marine Survey for the administrative year April 1890 to March 1891 have been examined and found to have nomenclatural consequences for malacostracan crustaceans. Even though they constitute available published works according to the International Code for Zoological Nomenclature, these reports have rarely been cited. Dating these two publications is of importance as they make decapod scientific names available and, in a few instances, describe the same taxa. After searching the collections deposited in the Asian and African Room, British Library, the Administration Report of the Indian Marine for the year April 1890 to March 1891 could be dated with some degree of certainty as 25 August 1891. In contrast, dating the Indian Museum Annual Report proved more difficult because after examination of copies held by the General Library in the Natural History Museum, London, it was evident that not all of these reports were consistently published on time to meet an end of year deadline. However, the publication of volume XXII of the Indian Museum Annual Report for the year April 1890 to March 1891 appeared to be contemporary with the year printed at the bottom of the title page. As no exact date could be established with confidence, the publication date for this volume was fixed as 31 December 1891 in accordance with ICZN Art. 21.3.2. Therefore the Administration Report of the Indian Marine (published 25 August 1891) is considered to take precedence over the Indian Museum Annual Report (published 31 December 1891) and as such the names made available in the former take priority. As original copies of the Administration Report of the Indian Marine are not readily available in most libraries and few scientists have actually had access to these publications, the relevant Appendix No. XIII, in which the names of several malacostracan taxa are made available, is reproduced here. Since the appendix is not

Report: Ordine del sentire e apertura al mondo. Filosofia delle emozioni e processo   di individuazione della persona. XIII Convegno internazionale della Max‐Scheler‐Gesellschaft Università di Verona 27‐30 Maggio 2015

Directory of Open Access Journals (Sweden)

Speranza, Maria Teresa

2015-06-01

Full Text Available An interesting debate on the issue of personal identity and its ethical implications has animated the days of the XIII International Congress of Max Scheler‐Gesellschaft. A large program of work has garnered numerous perspectives on the philosophy of person and the phenomenology of otherness, investigating in particular the role of emotions in the formation of person process. The main topic of conference was the Max Scheler’s phenomenology of emotions, which is an important turning point in the philosophy of twentieth century. The formation of ordo amoris, or rather order of feeling, generates the self‐ transcendence of the immediate feeling in virtue, in which the person realizes her singularity. The emotion, therefore, doesn’t remain confined in a state of mind and inner private but acts in the world, creating the emotional breakthrough (emotioneller Durchbruch that makes me exist in a new way in the world, which allows me to act according to my ordo amoris.

A Chandra grating observation of the dusty Wolf-Rayet star WR 48a

Energy Technology Data Exchange (ETDEWEB)

Zhekov, Svetozar A. [Space Research and Technology Institute, Akad. G. Bonchev Str., bl.1, Sofia 1113 (Bulgaria); Gagné, Marc [Department of Geology and Astronomy, West Chester University, West Chester, PA 19383 (United States); Skinner, Stephen L., E-mail: szhekov@space.bas.bg, E-mail: mgagne@wcupa.edu, E-mail: stephen.skinner@colorado.edu [CASA, University of Colorado, Boulder, CO 80309 (United States)

2014-04-10

We present results of a Chandra High-Energy Transmission Grating (HETG) observation of the carbon-rich Wolf-Rayet (WR) star WR 48a. These are the first high-resolution spectra of this object in X-ray. Blueshifted centroids of the spectral lines of ∼ – 360 km s{sup –1} and line widths of 1000-1500 km s{sup –1} (FWHM) were deduced from the analysis of the line profiles of strong emission lines. The forbidden line of Si XIII is strong and not suppressed, indicating that the rarified 10-30 MK plasma forms far from strong sources of far-ultraviolet emission, most likely in a wind collision zone. Global spectral modeling showed that the X-ray spectrum of WR 48a suffered higher absorption in the 2012 October Chandra observation compared with a previous 2008 January XMM-Newton observation. The emission measure of the hot plasma in WR 48a decreased by a factor ∼3 over the same period of time. The most likely physical picture that emerges from the analysis of the available X-ray data is that of colliding stellar winds in a wide binary system with an elliptical orbit. We propose that the unseen secondary star in the system is another WR star or perhaps a luminous blue variable.

THE XMM CLUSTER SURVEY: GALAXY MORPHOLOGIES AND THE COLOR-MAGNITUDE RELATION IN XMMXCS J2215.9 - 1738 AT z = 1.46

International Nuclear Information System (INIS)

Hilton, Matt; Stanford, S. Adam; Stott, John P.; Collins, Chris A.; Hoyle, Ben; Nichol, Robert C.; Davidson, Michael; Mann, Robert G.; Hosmer, Mark; Liddle, Andrew R.; Lloyd-Davies, Ed; Mehrtens, Nicola; Romer, A. Kathy; Sabirli, Kivanc; Sahlen, Martin; Kay, Scott T.; Miller, Christopher J.; Viana, Pedro T. P.; West, Michael J.; Barbary, Kyle

2009-01-01

We present a study of the morphological fractions and color-magnitude relation (CMR) in the most distant X-ray selected galaxy cluster currently known, XMMXCS J2215.9 - 1738 at z = 1.46, using a combination of optical imaging data obtained with the Hubble Space Telescope Advanced Camera for Surveys, and infrared data from the Multi-Object Infrared Camera and Spectrograph, mounted on the 8.2 m Subaru telescope. We find that the morphological mix of the cluster galaxy population is similar to clusters at z ∼ 1. Within the central 0.5 Mpc, approximately ∼62% of the galaxies identified as likely cluster members are ellipticals or S0s; and ∼38% are spirals or irregulars. Therefore, early-type galaxies were already entrenched as the dominant galaxy population in at least some clusters approximately ∼4.5 Gyr after the big bang. We measure the CMRs for the early-type galaxies, finding that the slope in the z 850 -J relation is consistent with that measured in the Coma cluster, some ∼9 Gyr earlier, although the uncertainty is large. In contrast, the measured intrinsic scatter about the CMR is more than three times the value measured in Coma, after conversion to rest-frame U - V. From comparison with stellar population synthesis models, the intrinsic scatter measurements imply mean luminosity-weighted ages for the early-type galaxies in J2215.9 - 1738 of ∼3 Gyr, corresponding to the major epoch of star formation coming to an end at z f ∼ 3-5. We find that the cluster exhibits evidence of the 'downsizing' phenomenon: the fraction of faint cluster members on the red sequence expressed using the Dwarf-to-Giant Ratio (DGR) is 0.32 ± 0.18 within a radius of 0.5R 200 . This is consistent with extrapolation of the redshift evolution of the DGR seen in cluster samples at z 1 clusters, we find a lack of very bright galaxies within the cluster.

77 FR 75189 - Certain Light-Emitting Diodes and Products Containing Same; Commission Determination Not To...

Science.gov (United States)

2012-12-19

... Corporate Center USA, Hella, Inc., Automotive Lighting Reutlingen GmbH, Automotive Lighting LLC, Tecnologia..., Inc., Automotive Lighting Reutlingen GmbH, Automotive Lighting, LLC, and [[Page 75190

The role of scintimammography and mammography in recurrent breast cancer. Evaluation of their accuracy using ROC curves

International Nuclear Information System (INIS)

Kolasinska, A.D.; Buscombe, J.R.; Cwikla, J.B.; Hilson, A.J.W.; Holloway, B.; Parbhoo, S.P.; Davidson, T.

2001-01-01

With the increasing demand for breast conservation surgery, the probability of recurrent tumour within the breast increases. Traditionally x-ray mammography (XMM) was used to assess the post-surgical breast, but post-surgery and radiotherapy changes have reduced the accuracy of this method. Scintimammography (SMM) has also been proposed and appears to be more accurate than XMM. A total of 101 women received Tc99m MIBI SMM and 88 had a subsequent XMM. There were 142 sites suspected of loco-regional recurrence breast cancer. During the study the patients did not receive any treatment other then hormonotherapy. SMM was performed by the standard Diggles-Khalkhali method and XMM was performed using standard 2 views. Analysis was performed and the results of each type of imaging compared with histology. In the ROC curve analysis 5 points of certainty were used: from 1 being definitely normal to 5 being definitely cancer; grades 4 and 5 were counted as positive. The overall sensitivity value of SMM was 84% and specificity was 85%, compared with a sensitivity of 52% for XMM and a specificity of 84%. Analysis of areas under ROC curves provides statistically significant difference between SMM and XMM (p < 0.05). Combining the two tests did not significantly improve the diagnostic accuracy of sequence imaging over SMM. ROC curve analysis demonstrates that scintimammography should be the primary investigation in suspected local recurrence following breast conservation surgery. (author)

Effects of Age, Season, Gender and Urban-Rural Status on Time-Activity: Canadian Human Activity Pattern Survey 2 (CHAPS 2)

OpenAIRE

Matz, Carlyn J.; Stieb, David M.; Davis, Karelyn; Egyed, Marika; Rose, Andreas; Chou, Benedito; Brion, Orly

2014-01-01

Estimation of population exposure is a main component of human health risk assessment for environmental contaminants. Population-level exposure assessments require time-activity pattern distributions in relation to microenvironments where people spend their time. Societal trends may have influenced time-activity patterns since previous Canadian data were collected 15 years ago. The Canadian Human Activity Pattern Survey 2 (CHAPS 2) was a national survey conducted in 2010–2011 to collect time-...

Huygens Crater: Insights into Noachian Volcanism, Stratigraphy, and Aqueous Processes

Science.gov (United States)

Ackiss, S. E.; Wray, J. J.; Seelos, K. D.; Niles, P. B.

2015-01-01

Huygens crater is a well preserved peak ring structure on Mars centered at 13.5 deg S, 55.5 deg E in the Noachian highlands between Terras Tyrrhena and Sabaea near the NW rim of Hellas basin. With a diameter of approximately 470 km, it uplifted and exhumed pre-Noachian crustal materials from depths greater than 25 km, penetrating below the thick, ubiquitous layer of Hellas ejecta. In addition, Huygens served as a basin for subsequent aqueous activity, including erosion/deposition by fluvial valley networks and subsurface alteration that is now exposed by smaller impacts. Younger mafic-bearing plains that partially cover the basin floor and surrounding intercrater areas were likely emplaced by later volcanism.

CO (3 – 2) HIGH-RESOLUTION SURVEY OF THE GALACTIC PLANE: R1

Energy Technology Data Exchange (ETDEWEB)

Dempsey, J. T.; Thomas, H. S.; Currie, M. J., E-mail: j.dempsey@jach.hawaii.edu, E-mail: h.thomas@jach.hawaii.edu, E-mail: m.currie@jach.hawaii.edu [Joint Astronomy Centre, 660 N. Aohoku Place, Hilo, HI 96720 (United States)

2013-11-01

We present the first release (R1) of data from the CO High-Resolution Survey (COHRS), which maps a strip of the inner Galactic plane in {sup 12}CO (J = 3 → 2). The data are taken using the Heterodyne Array Receiver Programme on the James Clerk Maxwell Telescope (JCMT) in Hawaii, which has a 14 arcsec angular resolution at this frequency. When complete, this survey will cover |b| ≤ 0.°5 between 10° < l < 65°. This first release covers |b| ≤ 0.°5 between 10.°25 < l < 17.°5 and 50.°25 < l < 55.°25, and |b| ≤ 0.°25 between 17.°5 < l < 50.°25. The data are smoothed to a velocity resolution of 1 km s{sup –1}, a spatial resolution of 16 arcsec and achieve a mean rms of ∼1 K. COHRS data are available to the community online at http://dx.doi.org/10.11570/13.0002. In this paper we describe the data acquisition and reduction techniques used and present integrated intensity images and longitude-velocity maps. We also discuss the noise characteristics of the data. The high resolution is a powerful tool for morphological studies of bubbles and filaments while the velocity information shows the spiral arms and outflows. These data are intended to complement both existing and upcoming surveys, e.g., the Bolocam Galactic Plane Survey (BGPS), ATLASGAL, the Herschel Galactic Plane Survey (Hi-GAL) and the JCMT Galactic Plane Survey with SCUBA-2 (JPS)

As parroquias do Porriño, Cans e Atios na documentación do mosteiro cisterciense de Santa María de Melón. Séculos XII e XIII

Directory of Open Access Journals (Sweden)

Gradín Fernández, Isis

2011-12-01

Full Text Available After the introduction and criteria of transcription, 31 papers are published from the twelfth and thirteenth centuries belonging to the Cistercian monastery of Santa Maria de Melon, specifically those that permit the reconstruction of old possessions, focusing on the current council of O Porriño -which was the monastery of San Miguel de Cans, absorbed by the cistercian monks of Melon. A paleographic and historical approximation of this documentation is done, which is complemented with the corresponding index of names and place names.

[gl] Trala introducción e criterios de transcripción, edítanse 31 documentos dos séculos XII e XIII pertencentes ó mosteiro cisterciense de Santa María de Melón, concretamente aqueles que permiten reconstruír as antigas posesións –centradas sobre o actual concello de O Porriño- do que foi o mosteiro de San Miguel de Cans, absorvido polos monxes cistercienses de Melón. Faise unha aproximación paleográfica e histórica da documentación, que se complementa cos correspondentes índices onomásticos e toponímicos.

A survey of electric and hybrid vehicles simulation programs. Volume 2: Questionnaire responses

Science.gov (United States)

Bevan, J.; Heimburger, D. A.; Metcalfe, M. A.

1978-01-01

The data received in a survey conducted within the United States to determine the extent of development and capabilities of automotive performance simulation programs suitable for electric and hybrid vehicle studies are presented. The survey was conducted for the Department of Energy by NASA's Jet Propulsion Laboratory. Volume 1 of this report summarizes and discusses the results contained in Volume 2.

THE BOLOCAM GALACTIC PLANE SURVEY. IX. DATA RELEASE 2 AND OUTER GALAXY EXTENSION

Energy Technology Data Exchange (ETDEWEB)

Ginsburg, Adam; Glenn, Jason; Ellsworth-Bowers, Timothy P.; Battersby, Cara; Bally, John; Stringfellow, Guy [CASA, University of Colorado, 389-UCB, Boulder, CO 80309 (United States); Rosolowsky, Erik [Department of Physics, 4-181 CCIS, University of Alberta, Edmonton, AB T6G 2E1 (Canada); Dunham, Miranda [Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520 (United States); Merello, Manuel; Evans II, Neal J. [Department of Astronomy, The University of Texas, 2515 Speedway, Stop C1400 Austin, TX 78712-1205 (United States); Shirley, Yancy [Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States); Aguirre, James, E-mail: Adam.Ginsburg@colorado.edu [Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104 (United States)

2013-10-01

We present a re-reduction and expansion of the Bolocam Galactic Plane Survey (BGPS), first presented by Aguirre et al. and Rosolowsky et al. The BGPS is a 1.1 mm survey of dust emission in the Northern galactic plane, covering longitudes –10° < l < 90° and latitudes |b| < 0.°5 with a typical 1σ rms sensitivity of 30-100 mJy in a ∼33'' beam. Version 2 of the survey includes an additional ∼20 deg{sup 2} of coverage in the third and fourth quadrants and ∼2 deg{sup 2} in the first quadrant. The new data release has improved angular recovery, with complete recovery out to ∼80'' and partial recovery to ∼300'', and reduced negative bowls around bright sources resulting from the atmospheric subtraction process. We resolve the factor of 1.5 flux calibration offset between the v1.0 data release and other data sets and determine that there is no offset between v2.0 and other data sets. The v2.0 pointing accuracy is tested against other surveys and is demonstrated to be accurate and an improvement over v1.0. We present simulations and tests of the pipeline and its properties, including measurements of the pipeline's angular transfer function. The Bolocat cataloging tool was used to extract a new catalog, which includes 8594 sources, with 591 in the expanded regions. We have demonstrated that the Bolocat 40'' and 80'' apertures are accurate even in the presence of strong extended background emission. The number of sources is lower than in v1.0, but the amount of flux and area included in identified sources is larger.

Geology of Libya Montes and the Interbasin Plains of Northern Tyrrhena Terra, Mars: First Year Results and Second Year Work Plan

Science.gov (United States)

Skinner, J. A., Jr.; Rogers, A. D.; Seelos, K. D.

2010-01-01

The Libya Montes-Tyrrhena Terra highland-lowland transitional zone of Mars is a complex tectonic and erosional region that contains some of the oldest exposed materials on the Martian surface as well as aqueous mineral signatures that may be potential chemical artifacts of early highland formational processes. Our 1:1M scale mapping project includes the geologic materials and landforms contained within MTMs 00282, -05282, -10282, 00277, - 05277, and -10277, which cover the highland portion of the transitional zone. The map region extends from the Libya Montes southward into Tyrrhena Terra and to the northern rim of Hellas basin and includes volcanic rocks of Syrtis Major Planum and a broad lowlying plain (palus) that forms a topographic divide between Isidis and Hellas basins. The objective of this project is to describe the geologic history of regional massif and plains materials by combining geomorphological and compositional mapping observations. This abstract summarizes the technical approaches and interim scientific results of Year 1 efforts and the expected work plan for Year 2 efforts.

National Beneficiary Survey (NBS) Round 2

Data.gov (United States)

Social Security Administration — A cross-sectional survey of a nationally representative sample of 4,864 social security beneficiaries age 18-64 receiving disability benefits in active pay status as...

VizieR Online Data Catalog: The GALFA-HI survey data release 2 (Peek+, 2018)

Science.gov (United States)

Peek, J. E. G.; Babler, B. L.; Zheng, Y.; Clark, S. E.; Douglas, K. A.; Korpela, E. J.; Putman, M. E.; Stanimirovic, S.; Gibson, S. J.; Heiles, C.

2018-03-01

The GALFA-HI survey is conducted with the William E. Gordon Arecibo Observatory 305m telescope, located south of Arecibo Puerto Rico. This survey owes its name to the instrument with which it was conducted, the ALFA, a 7-beam array of heterodyne detectors, sensitive from 1225 to 1525MHz. The observational strategy of DR2 is one of the significant differences from DR1 (Peek+ 2011ApJS..194...20P); see section 2.2. Region North-1 was included in DR1, but otherwise all of the Arecibo HI data presented in this work are new. (3 data files).

THE ALLWISE MOTION SURVEY, PART 2

Energy Technology Data Exchange (ETDEWEB)

Kirkpatrick, J. Davy; Kellogg, Kendra; Fajardo-Acosta, Sergio; Gelino, Christopher R.; Schurr, Steven D.; Cutri, Roc M.; Conrow, Tim [Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, Pasadena, CA 91125 (United States); Schneider, Adam C.; Cushing, Michael C.; Greco, Jennifer [Department of Physics and Astronomy, MS 111, University of Toledo, 2801 W. Bancroft Street, Toledo, OH 43606-3328 (United States); Mace, Gregory N. [Department of Astronomy, University of Texas at Austin, Austin, TX 78712 (United States); Wright, Edward L.; Logsdon, Sarah E.; Martin, Emily C.; McLean, Ian S. [Department of Physics and Astronomy, UCLA, 430 Portola Plaza, Box 951547, Los Angeles, CA 90095-1547 (United States); Eisenhardt, Peter R. M.; Stern, Daniel [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States); Faherty, Jacqueline K.; Sheppard, Scott S. [Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015 (United States); Lansbury, George B., E-mail: davy@ipac.caltech.edu [Department of Physics, Durham University, Durham DH1 3LE (United Kingdom)

2016-06-01

We use the AllWISE Data Release to continue our search for Wide-field Infrared Survey Explorer ( WISE )-detected motions. In this paper, we publish another 27,846 motion objects, bringing the total number to 48,000 when objects found during our original AllWISE motion survey are included. We use this list, along with the lists of confirmed WISE -based motion objects from the recent papers by Luhman and by Schneider et al., and candidate motion objects from the recent paper by Gagné et al., to search for widely separated, common-proper-motion systems. We identify 1039 such candidate systems. All 48,000 objects are further analyzed using color–color and color–mag plots to provide possible characterizations prior to spectroscopic follow-up. We present spectra of 172 of these, supplemented with new spectra of 23 comparison objects from the literature, and provide classifications and physical interpretations of interesting sources. Highlights include: (1) the identification of three G/K dwarfs that can be used as standard candles to study clumpiness and grain size in nearby molecular clouds because these objects are currently moving behind the clouds, (2) the confirmation/discovery of several M, L, and T dwarfs and one white dwarf whose spectrophotometric distance estimates place them 5–20 pc from the Sun, (3) the suggestion that the Na i “D” line be used as a diagnostic tool for interpreting and classifying metal-poor late-M and L dwarfs, (4) the recognition of a triple system including a carbon dwarf and late-M subdwarf, for which model fits of the late-M subdwarf (giving [Fe/H] ≈ −1.0) provide a measured metallicity for the carbon star, and (5) a possible 24 pc distant K5 dwarf + peculiar red L5 system with an apparent physical separation of 0.1 pc.

THE ALLWISE MOTION SURVEY, PART 2

International Nuclear Information System (INIS)

Kirkpatrick, J. Davy; Kellogg, Kendra; Fajardo-Acosta, Sergio; Gelino, Christopher R.; Schurr, Steven D.; Cutri, Roc M.; Conrow, Tim; Schneider, Adam C.; Cushing, Michael C.; Greco, Jennifer; Mace, Gregory N.; Wright, Edward L.; Logsdon, Sarah E.; Martin, Emily C.; McLean, Ian S.; Eisenhardt, Peter R. M.; Stern, Daniel; Faherty, Jacqueline K.; Sheppard, Scott S.; Lansbury, George B.

2016-01-01

We use the AllWISE Data Release to continue our search for Wide-field Infrared Survey Explorer ( WISE )-detected motions. In this paper, we publish another 27,846 motion objects, bringing the total number to 48,000 when objects found during our original AllWISE motion survey are included. We use this list, along with the lists of confirmed WISE -based motion objects from the recent papers by Luhman and by Schneider et al., and candidate motion objects from the recent paper by Gagné et al., to search for widely separated, common-proper-motion systems. We identify 1039 such candidate systems. All 48,000 objects are further analyzed using color–color and color–mag plots to provide possible characterizations prior to spectroscopic follow-up. We present spectra of 172 of these, supplemented with new spectra of 23 comparison objects from the literature, and provide classifications and physical interpretations of interesting sources. Highlights include: (1) the identification of three G/K dwarfs that can be used as standard candles to study clumpiness and grain size in nearby molecular clouds because these objects are currently moving behind the clouds, (2) the confirmation/discovery of several M, L, and T dwarfs and one white dwarf whose spectrophotometric distance estimates place them 5–20 pc from the Sun, (3) the suggestion that the Na i “D” line be used as a diagnostic tool for interpreting and classifying metal-poor late-M and L dwarfs, (4) the recognition of a triple system including a carbon dwarf and late-M subdwarf, for which model fits of the late-M subdwarf (giving [Fe/H] ≈ −1.0) provide a measured metallicity for the carbon star, and (5) a possible 24 pc distant K5 dwarf + peculiar red L5 system with an apparent physical separation of 0.1 pc.

First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt

Energy Technology Data Exchange (ETDEWEB)

Ward-Thompson, Derek; Pattle, Kate; Kirk, Jason M. [Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE (United Kingdom); Bastien, Pierre; Coudé, Simon [Centre de recherche en astrophysique du Québec and département de physique, Université de Montréal, C.P. 6128, Succ. Centre-ville, Montréal, QC, H3C 3J7 (Canada); Furuya, Ray S. [Tokushima University, Minami Jousanajima-machi 1-1, Tokushima 770-8502 (Japan); Kwon, Woojin; Choi, Minho; Hoang, Thiem [Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055 (Korea, Republic of); Lai, Shih-Ping [Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu 30013, Taiwan (China); Qiu, Keping [School of Astronomy and Space Science, Nanjing University, 163 Xianlin Avenue, Nanjing 210023 (China); Berry, David; Friberg, Per; Graves, Sarah F. [East Asian Observatory, 660 N. A‘ohōkū Place, University Park, Hilo, HI 96720 (United States); Francesco, James Di; Johnstone, Doug [NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7 (Canada); Franzmann, Erica [Department of Physics and Astronomy, The University of Manitoba, Winnipeg, Manitoba R3T2N2 (Canada); Greaves, Jane S. [School of Physics and Astronomy, Cardiff University, The Parade, Cardiff, CF24 3AA (United Kingdom); Houde, Martin [Department of Physics and Astronomy, The University of Western Ontario, 1151 Richmond Street, London N6A 3K7 (Canada); Koch, Patrick M., E-mail: dward-thompson@uclan.ac.uk, E-mail: kmpattle@uclan.ac.uk, E-mail: jmkirk@uclan.ac.uk, E-mail: spseyres@uclan.ac.uk [Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan (China); and others

2017-06-10

We present the first results from the B-fields In STar-forming Region Observations (BISTRO) survey, using the Sub-millimetre Common-User Bolometer Array 2 camera, with its associated polarimeter (POL-2), on the James Clerk Maxwell Telescope in Hawaii. We discuss the survey’s aims and objectives. We describe the rationale behind the survey, and the questions that the survey will aim to answer. The most important of these is the role of magnetic fields in the star formation process on the scale of individual filaments and cores in dense regions. We describe the data acquisition and reduction processes for POL-2, demonstrating both repeatability and consistency with previous data. We present a first-look analysis of the first results from the BISTRO survey in the OMC 1 region. We see that the magnetic field lies approximately perpendicular to the famous “integral filament” in the densest regions of that filament. Furthermore, we see an “hourglass” magnetic field morphology extending beyond the densest region of the integral filament into the less-dense surrounding material, and discuss possible causes for this. We also discuss the more complex morphology seen along the Orion Bar region. We examine the morphology of the field along the lower-density northeastern filament. We find consistency with previous theoretical models that predict magnetic fields lying parallel to low-density, non-self-gravitating filaments, and perpendicular to higher-density, self-gravitating filaments.

Spectral Characteristics of Young Stars Associated with the Sh2-296 Nebula

Science.gov (United States)

Fernandes, Beatriz; Gregorio-Hetem, Jane

Aiming to contribute to the understanding of star formation and evolution in the Canis Major (CMa R1) Molecular Clouds Complex, we analyze the spectral characteristics of a population of young stars associated with the arc-shaped nebula Sh2-296. Our XMM/Newton observations detected 109 X-ray sources in the region and optical spectroscopy was performed with Gemini telescope for 85 optical counterparts. We identified and characterized 51 objects that present features typically found in young objects, such as Hα emission and strong absorption on the Li I line.

Hella hingega karmid naised / Krista Kaer

Index Scriptorium Estoniae

Kaer, Krista

1996-01-01

Tänapäeva kriminaalromaani inglise ja ameerika autoritest (Dame Phyllis Dorothy James, Joan Smith, Lynda La Plante (inglise); Sara Paretsky, Sue Grafton, Patricia Cornwell (ameerika) ja nende poolt loodud naisdetektiivi kujudest

The APM galaxy survey: Pt. 2; Photometric corrections

Energy Technology Data Exchange (ETDEWEB)

Maddox, S.J.; Efstathiou, G.; Sutherland, W.J. (Oxford Univ. (UK). Dept. of Astrophysics)

1990-10-01

We describe the methods that we have used to establish accurate photometry in a survey of two million galaxies brighter then b{sub j} 20.5 covering over 4300 square degrees of the South Galactic cap. We apply a field correction for vignetting and differential desensitization which is accurate to ''< approx''0.04 mag across each of 185 Schmidt plates. Images in the overlapping regions of neighbouring plate pairs are used to establish a uniform magnitude system over the entire survey. We discuss the residual magnitude differences in the overlaps and the propagation of plate-to-plate magnitude errors across the network of plates. We argue that the rms plate zero-point error in the final matched survey is 0.04 mag. CCD photometry of 40 faint galaxy sequences is used to calibrate the matched magnitudes and to set stringent limits on large-scale gradients in the matched survey photometry. (author).

Second ROSAT all-sky survey (2RXS) source catalogue

Science.gov (United States)

Boller, Th.; Freyberg, M. J.; Trümper, J.; Haberl, F.; Voges, W.; Nandra, K.

2016-04-01

Aims: We present the second ROSAT all-sky survey source catalogue, hereafter referred to as the 2RXS catalogue. This is the second publicly released ROSAT catalogue of point-like sources obtained from the ROSAT all-sky survey (RASS) observations performed with the position-sensitive proportional counter (PSPC) between June 1990 and August 1991, and is an extended and revised version of the bright and faint source catalogues. Methods: We used the latest version of the RASS processing to produce overlapping X-ray images of 6.4° × 6.4° sky regions. To create a source catalogue, a likelihood-based detection algorithm was applied to these, which accounts for the variable point-spread function (PSF) across the PSPC field of view. Improvements in the background determination compared to 1RXS were also implemented. X-ray control images showing the source and background extraction regions were generated, which were visually inspected. Simulations were performed to assess the spurious source content of the 2RXS catalogue. X-ray spectra and light curves were extracted for the 2RXS sources, with spectral and variability parameters derived from these products. Results: We obtained about 135 000 X-ray detections in the 0.1-2.4 keV energy band down to a likelihood threshold of 6.5, as adopted in the 1RXS faint source catalogue. Our simulations show that the expected spurious content of the catalogue is a strong function of detection likelihood, and the full catalogue is expected to contain about 30% spurious detections. A more conservative likelihood threshold of 9, on the other hand, yields about 71 000 detections with a 5% spurious fraction. We recommend thresholds appropriate to the scientific application. X-ray images and overlaid X-ray contour lines provide an additional user product to evaluate the detections visually, and we performed our own visual inspections to flag uncertain detections. Intra-day variability in the X-ray light curves was quantified based on the

Estimating photometric redshifts for X-ray sources in the X-ATLAS field using machine-learning techniques

Science.gov (United States)

Mountrichas, G.; Corral, A.; Masoura, V. A.; Georgantopoulos, I.; Ruiz, A.; Georgakakis, A.; Carrera, F. J.; Fotopoulou, S.

2017-12-01

We present photometric redshifts for 1031 X-ray sources in the X-ATLAS field using the machine-learning technique TPZ. X-ATLAS covers 7.1 deg2 observed with XMM-Newton within the Science Demonstration Phase of the H-ATLAS field, making it one of the largest contiguous areas of the sky with both XMM-Newton and Herschel coverage. All of the sources have available SDSS photometry, while 810 additionally have mid-IR and/or near-IR photometry. A spectroscopic sample of 5157 sources primarily in the XMM/XXL field, but also from several X-ray surveys and the SDSS DR13 redshift catalogue, was used to train the algorithm. Our analysis reveals that the algorithm performs best when the sources are split, based on their optical morphology, into point-like and extended sources. Optical photometry alone is not enough to estimate accurate photometric redshifts, but the results greatly improve when at least mid-IR photometry is added in the training process. In particular, our measurements show that the estimated photometric redshifts for the X-ray sources of the training sample have a normalized absolute median deviation, nmad ≈ 0.06, and a percentage of outliers, η = 10-14%, depending upon whether the sources are extended or point like. Our final catalogue contains photometric redshifts for 933 out of the 1031 X-ray sources with a median redshift of 0.9. The table of the photometric redshifts is 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/608/A39

U.S. Army Corps of Engineers Surveying Requirements Meeting, 2-5 February 1982,

Science.gov (United States)

1982-04-01

performance and economical performance, has been in effect in prior legislation since the 1920’s. 2. PL 95-269 has a new provision - that the Corps...please hire and train your crew locally.* (This is also in conformance with the Legislative directive to utilize local community resources.) Seriously...Glennon Equipment Westminister Park John Lorea Contract Surveys E. Providence, RI 02914 (401) 438-1780 Riley Park Hayden Ralph L. Hayden Contract Surveys

Gifts to Colleges Rose 8.2% in 2011, Survey Finds

Science.gov (United States)

Biemiller, Lawrence

2012-01-01

The author discusses the results of an annual "Voluntary Support of Education" survey by the Council for Aid to Education. According to the report, after two lackluster years, donations to U.S. colleges and universities rose last year by a healthy 8.2 percent, to an estimated $30.3-billion. The total raised comes close to the amount seen in 2008,…

Comparison of smoking cessation between education groups: findings from 2 US National Surveys over 2 decades.

Science.gov (United States)

Zhuang, Yue-Lin; Gamst, Anthony C; Cummins, Sharon E; Wolfson, Tanya; Zhu, Shu-Hong

2015-02-01

We examined smoking cessation rate by education and determined how much of the difference can be attributed to the rate of quit attempts and how much to the success of these attempts. We analyzed data from the National Health Interview Survey (NHIS, 1991-2010) and the Tobacco Use Supplement to the Current Population Survey (TUS-CPS, 1992-2011). Smokers (≥ 25 years) were divided into lower- and higher-education groups (≤ 12 years and >12 years). A significant difference in cessation rate between the lower- and the higher-education groups persisted over the last 2 decades. On average, the annual cessation rate for the former was about two thirds that of the latter (3.5% vs 5.2%; Peducation group have consistently lagged behind their higher-education counterparts in quitting. In addition to the usual concern about improving their success in quitting, tobacco control programs need to find ways to increase quit attempts in this group.

Factors controlling volume errors through 2D gully erosion assessment: guidelines for optimal survey design

Science.gov (United States)

Castillo, Carlos; Pérez, Rafael

2017-04-01

The assessment of gully erosion volumes is essential for the quantification of soil losses derived from this relevant degradation process. Traditionally, 2D and 3D approaches has been applied for this purpose (Casalí et al., 2006). Although innovative 3D approaches have recently been proposed for gully volume quantification, a renewed interest can be found in literature regarding the useful information that cross-section analysis still provides in gully erosion research. Moreover, the application of methods based on 2D approaches can be the most cost-effective approach in many situations such as preliminary studies with low accuracy requirements or surveys under time or budget constraints. The main aim of this work is to examine the key factors controlling volume error variability in 2D gully assessment by means of a stochastic experiment involving a Monte Carlo analysis over synthetic gully profiles in order to 1) contribute to a better understanding of the drivers and magnitude of gully erosion 2D-surveys uncertainty and 2) provide guidelines for optimal survey designs. Owing to the stochastic properties of error generation in 2D volume assessment, a statistical approach was followed to generate a large and significant set of gully reach configurations to evaluate quantitatively the influence of the main factors controlling the uncertainty of the volume assessment. For this purpose, a simulation algorithm in Matlab® code was written, involving the following stages: - Generation of synthetic gully area profiles with different degrees of complexity (characterized by the cross-section variability) - Simulation of field measurements characterised by a survey intensity and the precision of the measurement method - Quantification of the volume error uncertainty as a function of the key factors In this communication we will present the relationships between volume error and the studied factors and propose guidelines for 2D field surveys based on the minimal survey

NuSTAR J033202-2746.8: Direct constraints on the Compton reflection in a heavily obscured quasar at z ≈ 2

Energy Technology Data Exchange (ETDEWEB)

Del Moro, A.; Mullaney, J. R.; Alexander, D. M.; Aird, J. A.; Gandhi, P. [Department of Physics, Durham University, South Road, Durham, DH1 3LE (United Kingdom); Comastri, A.; Vignali, C.; Gilli, R. [INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna (Italy); Bauer, F. E. [Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, 306, Santiago 22 (Chile); Treister, E. [Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción (Chile); Stern, D. [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Mail Stop 169-221, Pasadena, CA 91109 (United States); Civano, F. [Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755 (United States); Ranalli, P. [National Observatory of Athens, Institute of Astronomy, Astrophysics, Space Applications and Remote Sensing, Metaxa and Pavlou St., 15236 Penteli (Greece); Ballantyne, D. R. [Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, Atlanta, GA 30332 (United States); Baloković, M. [Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology, Pasadena, CA 91125 (United States); Boggs, S. E. [Space Sciences Laboratory, University of California, Berkeley, CA 94720 (United States); Brandt, W. N. [Department of Astronomy and Astrophysics, 525 Davey Lab, The Pennsylvania State University, University Park, PA 16802 (United States); Christensen, F. E. [DTU Space-National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby (Denmark); Craig, W. W. [Lawrence Livermore National Laboratory, Livermore, CA 94550 (United States); Hailey, C. J., E-mail: agnese.del-moro@durham.ac.uk [Columbia Astrophysics Laboratory, 550 W 120th Street, Columbia University, NY 10027 (United States); and others

2014-05-01

We report Nuclear Spectroscopic Telescope Array (NuSTAR) observations of NuSTAR J033202-2746.8, a heavily obscured, radio-loud quasar detected in the Extended Chandra Deep Field-South, the deepest layer of the NuSTAR extragalactic survey (∼400 ks, at its deepest). NuSTAR J033202-2746.8 is reliably detected by NuSTAR only at E > 8 keV and has a very flat spectral slope in the NuSTAR energy band (Γ=0.55{sub −0.64}{sup +0.62}; 3-30 keV). Combining the NuSTAR data with extremely deep observations by Chandra and XMM-Newton (4 Ms and 3 Ms, respectively), we constrain the broad-band X-ray spectrum of NuSTAR J033202-2746.8, indicating that this source is a heavily obscured quasar (N{sub H}=5.6{sub −0.8}{sup +0.9}×10{sup 23} cm{sup –2}) with luminosity L {sub 10-40} {sub keV} ≈ 6.4 × 10{sup 44} erg s{sup –1}. Although existing optical and near-infrared (near-IR) data, as well as follow-up spectroscopy with the Keck and VLT telescopes, failed to provide a secure redshift identification for NuSTAR J033202-2746.8, we reliably constrain the redshift z = 2.00 ± 0.04 from the X-ray spectral features (primarily from the iron K edge). The NuSTAR spectrum shows a significant reflection component (R=0.55{sub −0.37}{sup +0.44}), which was not constrained by previous analyses of Chandra and XMM-Newton data alone. The measured reflection fraction is higher than the R ∼ 0 typically observed in bright radio-loud quasars such as NuSTAR J033202-2746.8, which has L {sub 1.4} {sub GHz} ≈ 10{sup 27} W Hz{sup –1}. Constraining the spectral shape of active galactic nuclei (AGNs), including bright quasars, is very important for understanding the AGN population, and can have a strong impact on the modeling of the X-ray background. Our results show the importance of NuSTAR in investigating the broad-band spectral properties of quasars out to high redshift.

FY 1998 report on the verification survey of geothermal exploration technology, etc. 2/2. Survey of deep geothermal resource; 1998 nendo chinetsu tansa gijutsu nado kensho chosa hokokusho. 2/2. Shinbu chinetsu shigen chosa

Energy Technology Data Exchange (ETDEWEB)

NONE

1999-12-01

For the purpose of commercializing deep geothermal resource, a deep exploration well of 4000m class was drilled in the existing geothermal development area to survey the situation of deep geothermal resource existence and the availability. Concretely, the deep geothermal exploration well was drilled for study in the Kakkonda area, Shizukuishi town, Iwate prefecture, to clarify the situation of deep geothermal resource existence and the whole image of geothermal system. Consideration was made of the deep geothermal exploration method, systematization of deep high temperature drilling technology, and availability of deep geothermal resource. The results of the survey were summed up as follows: 1) general remarks; 2) deep exploration well drilling work; 3) details of the study. This report contained 3). In 3), the items were as follows: heightening of accuracy of the deep geothermal resource exploration method, making of a geothermal model in the Kakkonda area, study of deep drilling technology, study of deep fluid utilization technology, and making of a guide for deep geothermal resource exploration/development in the Kakkonda area. As to the technology of high temperature deep geothermal well drilling, studies were made of the borehole cooling method, mud water cooling method, survey of deterioration of casing with age, etc. (NEDO)

AKARI NEAR-INFRARED SPECTROSCOPIC SURVEY FOR CO2 IN 18 COMETS

International Nuclear Information System (INIS)

Ootsubo, Takafumi; Kawakita, Hideyo; Hamada, Saki; Kobayashi, Hitomi; Yamaguchi, Mitsuru; Usui, Fumihiko; Nakagawa, Takao; Ueno, Munetaka; Ishiguro, Masateru; Sekiguchi, Tomohiko; Watanabe, Jun-ichi; Sakon, Itsuki; Shimonishi, Takashi; Onaka, Takashi

2012-01-01

We conducted a spectroscopic survey of cometary volatiles with the Infrared Camera on board the Japanese infrared satellite AKARI in the wavelength range from 2.5 to 5 μm. In our survey, 18 comets, including both the Oort cloud comets and the Jupiter-family comets, were observed in the period from 2008 June to 2010 January, most of which were observed at least twice. The prominent emission bands in the observed spectra are the fundamental vibrational bands of water (H 2 O) at 2.7 μm and carbon dioxide (CO 2 ) at 4.3 μm. The fundamental vibrational band of carbon monoxide (CO) around 4.7 μm and the broad emission feature, probably related to carbon-hydrogen-bearing molecules, can also be recognized around the 3.3-3.5-μm region in some of the comets. With respect to H 2 O, gas production rate ratios of CO 2 have been derived in 17 comets, except for the comet 29P/Schwassmann-Wachmann 1. Our data set provides the largest homogeneous database of CO 2 /H 2 O production rate ratios in comets obtained so far. The CO 2 /H 2 O production rate ratios are considered to reflect the composition of cometary ice when a comet is observed at a heliocentric distance within ∼2.5 AU, since H 2 O ice fully sublimates there. The CO 2 /H 2 O ratio in cometary ice spans from several to ∼30% among the comets observed at 2 in the comets seems to be smaller than unity based on our observations, although we only obtain upper limits for CO in most of the comets.

SURVEY OBSERVATIONS OF A POSSIBLE GLYCINE PRECURSOR, METHANIMINE (CH{sub 2}NH)

Energy Technology Data Exchange (ETDEWEB)

Suzuki, Taiki; Ohishi, Masatoshi; Hirota, Tomoya; Saito, Masao [Department of Astronomy, the Graduate University for Advanced Studies (SOKENDAI), Osawa 2-21-1, Mitaka, Tokyo 181-8588 (Japan); Majumdar, Liton; Wakelam, Valentine, E-mail: taiki.suzuki@nao.ac.jp [Univ. Bordeaux, LAB, UMR 5804, F-33270, Floirac (France)

2016-07-01

We conducted survey observations of a glycine precursor, methanimine, or methylenimine (CH{sub 2}NH), with the Nobeyama Radio Observatory 45 m telescope and the Sub-Millimeter Radio telescope toward 12 high-mass and two low-mass star-forming regions in order to increase the number of known CH{sub 2}NH sources and to better understand the characteristics of CH{sub 2}NH sources. As a result of our survey, CH{sub 2}NH was detected in eight sources, including four new sources. The estimated fractional abundances were ∼10{sup −8} in Orion KL and G10.47+0.03, while they were ∼10{sup −9} toward the other sources. Our hydrogen recombination line and past studies suggest that CH{sub 2}NH-rich sources have less (this mean not so evolved) evolved H ii regions. The lower destruction rates from UV flux from the central star would contribute to the high CH{sub 2}NH abundances toward CH{sub 2}NH-rich sources. Our gas-grain chemical simulations suggest that CH{sub 2}NH is mostly formed in the gas phase by neutral–neutral reactions, rather than being the product of thermal evaporation from dust surfaces.

X-ray diving in the center of Sh2-129: looking for the driving source of Ou4

Science.gov (United States)

Grosso, Nicolas

2012-10-01

The outflow phenomenon is associated both with the early and the last phase of the stellar evolution. Recently, a unique bipolar outflow with an angular size of 1.2 degrees was discovered in the blister HII region Sh2-129. Ou4, nicknamed "The Giant Squid", is to our knowledge the bipolar outflow with the largest angular size ever found. We propose joint XMM-Newton/EPIC (35 ks) and Chandra/HRC-I (16 ks) observations to look for the driving source of Ou4 and to clarify the nature of this object.

The optical, infrared and radio properties of extragalactic sources observed by SDSS, 2mass and first surveys

International Nuclear Information System (INIS)

Z. Ivezic et al.

2002-01-01

We positionally match sources observed by the Sloan Digital Sky Survey (SDSS), the Two Micron All Sky Survey (2MASS), and the Faint Images of the Radio Sky at Twenty-cm (FIRST) survey. Practically all 2MASS sources are matched to an SDSS source within 2 arcsec; ∼ 11% of them are optically resolved galaxies and the rest are dominated by stars. About 1/3 of FIRST sources are matched to an SDSS source within 2 arcsec; ∼ 80% of these are galaxies and the rest are dominated by quasars. Based on these results, we project that by the completion of these surveys the matched samples will include about 10 7 and 10 6 galaxies observed by both SDSS and 2MASS, and about 250,000 galaxies and 50,000 quasars observed by both SDSS and FIRST. Here we present a preliminary analysis of the optical, infrared and radio properties for the extragalactic sources from the matched samples. In particular, we find that the fraction of quasars with stellar colors missed by the SDSS spectroscopic survey is probably not larger than ∼ 10%, and that the optical colors of radio-loud quasars are ∼ 0.05 mag. redder (with 4σ significance) than the colors of radio-quiet quasars

RELIABLE IDENTIFICATIONS OF ACTIVE GALACTIC NUCLEI FROM THE WISE, 2MASS, AND ROSAT ALL-SKY SURVEYS

Energy Technology Data Exchange (ETDEWEB)

Edelson, R. [Department of Astronomy, University of Maryland, College Park, MD 20742-2421 (United States); Malkan, M., E-mail: rickedelson@gmail.com [Department of Physics and Astronomy, University of California Los Angeles, Los Angeles, CA 90095-1547 (United States)

2012-05-20

We have developed the ''S{sub IX}'' statistic to identify bright, highly likely active galactic nucleus (AGN) candidates solely on the basis of Wide-field Infrared Survey Explorer (WISE), Two Micron All-Sky Survey (2MASS), and ROSAT all-sky survey (RASS) data. This statistic was optimized with data from the preliminary WISE survey and the Sloan Digital Sky Survey, and tested with Lick 3 m Kast spectroscopy. We find that sources with S{sub IX} < 0 have a {approx}>95% likelihood of being an AGN (defined in this paper as a Seyfert 1, quasar, or blazar). This statistic was then applied to the full WISE/2MASS/RASS dataset, including the final WISE data release, to yield the ''W2R'' sample of 4316 sources with S{sub IX} < 0. Only 2209 of these sources are currently in the Veron-Cetty and Veron (VCV) catalog of spectroscopically confirmed AGNs, indicating that the W2R sample contains nearly 2000 new, relatively bright (J {approx}< 16) AGNs. We utilize the W2R sample to quantify biases and incompleteness in the VCV catalog. We find that it is highly complete for bright (J < 14), northern AGNs, but the completeness drops below 50% for fainter, southern samples and for sources near the Galactic plane. This approach also led to the spectroscopic identification of 10 new AGNs in the Kepler field, more than doubling the number of AGNs being monitored by Kepler. The W2R sample contains better than 1 bright AGN every 10 deg{sup 2}, permitting construction of AGN samples in any sufficiently large region of sky.

A comparative study of set up variations and bowel volumes in supine versus prone positions of patients treated with external beam radiation for carcinoma rectum.

Science.gov (United States)

Rajeev, K R; Menon, Smrithy S; Beena, K; Holla, Raghavendra; Kumar, R Rajaneesh; Dinesh, M

2014-01-01

A prospective study was undertaken to evaluate the influence of patient positioning on the set up variations to determine the planning target volume (PTV) margins and to evaluate the clinical relevance volume assessment of the small bowel (SB) within the irradiated volume. During the period of months from December 2011 to April 2012, a computed tomography (CT) scan was done either in supine position or in prone position using a belly board (BB) for 20 consecutive patients. All the patients had histologically proven rectal cancer and received either post- or pre-operative pelvic irradiation. Using a three-dimensional planning system, the dose-volume histogram for SB was defined in each axial CT slice. Total dose was 46-50 Gy (2 Gy/fraction), delivered using the 4-field box technique. The set up variation of the study group was assessed from the data received from the electronic portal imaging device in the linear accelerator. The shift along X, Y, and Z directions were noted. Both systematic and random errors were calculated and using both these values the PTV margin was calculated. The systematic errors of patients treated in the supine position were 0.87 (X-mm), 0.66 (Y-mm), 1.6 (Z-mm) and in the prone position were 1.3 (X-mm), 0.59 (Y-mm), 1.17 (Z-mm). The random errors of patients treated in the supine positions were 1.81 (X-mm), 1.73 (Y-mm), 1.83 (Z-mm) and in prone position were 2.02 (X-mm), 1.21 (Y-mm), 3.05 (Z-mm). The calculated PTV margins in the supine position were 3.45 (X-mm), 2.87 (Y-mm), 5.31 (Z-mm) and in the prone position were 4.91 (X-mm), 2.32 (Y-mm), 5.08 (Z-mm). The mean volume of the peritoneal cavity was 648.65 cm 3 in the prone position and 1197.37 cm 3 in the supine position. The prone position using BB device was more effective in reducing irradiated SB volume in rectal cancer patients. There were no significant variations in the daily set up for patients treated in both supine and prone positions.

Survey of 1 1/2D transport codes

International Nuclear Information System (INIS)

Grad, H.

1978-10-01

A survey is given of a family of classical transport codes, recently termed ''1 1/2D'', which efficiently and accurately follow the evolution of plasma configurations on a long time scale, following coupled changes in plasma shape and topology with transport (but not wave motion). Codes have been constructed and operated (since 1974) which include various combinations of finite beta, general plasma cross-section and aspect, various topologies (Doublet, tearing, reversed-field mirror) including time dependent transitions in topology resulting from external coil variation and plasma transport, with models including (classical) tensor resistivity and heat flow as well as the adiabatic limiting case

The XII Century Towers, a Benchmark of the Rome Countryside almost Cancelled: the Safeguard Plan by Low Cost Uav and Terrestrial Dsm Photogrammetry Surveying and 3d Web GIS Applications

Science.gov (United States)

Barelli, L.; Paolini, P.; Forti, G.

2017-11-01

"Giving a bird-fly look at the Rome countryside, throughout the Middle Age central period, it would show as if the multiple city towers has been widely spread around the territory" on a radial range of maximum thirty kilometers far from the Capitol Hill center (Carocci and Vendittelli, 2004). This is the consequence of the phenomenon identified with the "Incasalamento" neologism, described in depth in the following paper, intended as the general process of expansion of the urban society interests outside the downtown limits, started from the half of the XII and developed through all the XIII century, slowing down and ending in the following years. From the XIX century till today the architectural finds of this reality have raised the interest of many national and international scientists, which aimed to study and catalog them all to create a complete framework that, cause of its extension, didn't allow yet attempting any element by element detailed analysis. From the described situation has started our plan of intervention, we will apply integrated survey methods and technologies of terrestrial and UAV near stereo-photogrammetry, by the use of low cost drones, more than action cameras and reflex on extensible rods, integrated and referenced with GPS and topographic survey. In the final project we intend to produce some 3D scaled and textured surface models of any artifact (almost two hundreds were firstly observed still standing), to singularly study the dimensions and structure, to analyze the building materials and details and to formulate an hypothesis about any function, based even on the position along the territory. These models, successively georeferenced, will be imported into a 2D and 3D WebGIS and organized in layers made visible on basemaps of reference, as much as on historical maps.

New Fast Lane towards Discoveries of Clusters of Galaxies Inaugurated

Science.gov (United States)

2003-07-01

Space and Ground-Based Telescopes Cooperate to Gain Deep Cosmological Insights Summary Using the ESA XMM-Newton satellite, a team of European and Chilean astronomers [2] has obtained the world's deepest "wide-field" X-ray image of the cosmos to date. This penetrating view, when complemented with observations by some of the largest and most efficient ground-based optical telescopes, including the ESO Very Large Telescope (VLT), has resulted in the discovery of several large clusters of galaxies. These early results from an ambitious research programme are extremely promising and pave the way for a very comprehensive and thorough census of clusters of galaxies at various epochs. Relying on the foremost astronomical technology and with an unequalled observational efficiency, this project is set to provide new insights into the structure and evolution of the distant Universe. PR Photo 19a/03: First image from the XMM-LSS survey. PR Photo 19b/03: Zoom-in on PR Photo 19b/03. PR Photo 19c/03: XMM-Newton contour map of the probable extent of a cluster of galaxies, superimposed upon a CHFT I-band image. PR Photo 19d/03: Velocity distribution in the cluster field shown in PR Photo 19c/03. The universal web Unlike grains of sand on a beach, matter is not uniformly spread throughout the Universe. Instead, it is concentrated into galaxies which themselves congregate into clusters (and even clusters of clusters). These clusters are "strung" throughout the Universe in a web-like structure, cf. ESO PR 11/01. Our Galaxy, the Milky Way, for example, belongs to the so-called Local Group which also comprises "Messier 31", the Andromeda Galaxy. The Local Group contains about 30 galaxies and measures a few million light-years across. Other clusters are much larger. The Coma cluster contains thousands of galaxies and measures more than 20 million light-years. Another well known example is the Virgo cluster, covering no less than 10 degrees on the sky ! Clusters of galaxies are the most

The survey of the Omagari fault using electric survey

International Nuclear Information System (INIS)

Matsuo, Koichi; Kishimoto, Munemaru; Negi, Tateyuki; Teshima, Minoru

2005-08-01

The present document is to report the results of geophysical survey by electric survey around a site proposed for the Horonobe Underground Research Program at Horonobe-cho, Hokkaido by the Japan Nuclear Cycle Development Institute. Electric survey using dipole-dipole array was carried out at 2,061 points using 101 electrodes over 1 km survey line in the area of Hokushin in Horonobe-cho near presumed Omagari-fault. Two dimensional resistivity inversion analysis was carried out and the resistivity structure from the surface to 250 m below sea level became clear. The resistivity structure was studied by comparing structure presumed from existing geological and geophysical informations. Resistivity distribution near surface was about 100 ohm-m and it became from 10 to 2 ohm-m as the depth increasing. Resistivity near presumed Omagari-fault was relatively lower than around that fault. Resistivity distribution was good agreement with two dimensional resistivity structure perfumed by AMT survey (2003) and existing electrical resistivity log data. Resistivity distribution of shallow zone at survey area was clear because the density of survey points were very high. (author)

78 FR 9636 - Airworthiness Directives; Cessna Aircraft Company Airplanes

Science.gov (United States)

2013-02-11

...)(ix) through (k)(3)(xiii) of this AD. (i) Open the battery door. (ii) Disconnect the main battery... warning tag that reads: ``WARNING: Do not connect the battery connector during the maintenance in progress... external power receptacle. (xii) Connect the battery and restore electrical power to the airplane. (xiii...

RESOLVED COMPANIONS OF CEPHEIDS: TESTING THE CANDIDATES WITH X-RAY OBSERVATIONS

Energy Technology Data Exchange (ETDEWEB)

Evans, Nancy Remage; Pillitteri, Ignazio; Wolk, Scott; Karovska, Margarita; Tingle, Evan [Smithsonian Astrophysical Observatory, MS 4, 60 Garden St., Cambridge, MA 02138 (United States); Guinan, Edward; Engle, Scott [Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Ave., Villanova, PA 19085 (United States); Bond, Howard E. [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Schaefer, Gail H. [The CHARA Array of Georgia State University, Mount Wilson, California 91023 (United States); Mason, Brian D., E-mail: nevans@cfa.harvard.edu, E-mail: heb11@psu.edu, E-mail: schaefer@chara-array.org [US Naval Observatory, 3450 Massachusetts Ave., NW, Washington, DC 20392-5420 (United States)

2016-04-15

We have made XMM-Newton observations of 14 Galactic Cepheids that have candidate resolved (≥5″) companion stars based on our earlier HST Wide Field Camera 3 (WFC3) imaging survey. Main-sequence stars that are young enough to be physical companions of Cepheids are expected to be strong X-ray producers in contrast to field stars. XMM-Newton exposures were set to detect essentially all companions hotter than spectral type M0 (corresponding to 0.5 M{sub ⊙}). The large majority of our candidate companions were not detected in X-rays, and hence are not confirmed as young companions. One resolved candidate (S Nor #4) was unambiguously detected, but the Cepheid is a member of a populous cluster. For this reason, it is likely that S Nor #4 is a cluster member rather than a gravitationally bound companion. Two further Cepheids (S Mus and R Cru) have X-ray emission that might be produced by either the Cepheid or the candidate resolved companion. A subsequent Chandra observation of S Mus shows that the X-rays are at the location of the Cepheid/spectroscopic binary. R Cru and also V659 Cen (also X-ray bright) have possible companions closer than 5″ (the limit for this study) which are the likely sources of X-rays. One final X-ray detection (V473 Lyr) has no known optical companion, so the prime suspect is the Cepheid itself. It is a unique Cepheid with a variable amplitude. The 14 stars that we observed with XMM constitute 36% of the 39 Cepheids found to have candidate companions in our HST/WFC3 optical survey. No young probable binary companions were found with separations of ≥5″ or 4000 au.

RESOLVED COMPANIONS OF CEPHEIDS: TESTING THE CANDIDATES WITH X-RAY OBSERVATIONS

International Nuclear Information System (INIS)

Evans, Nancy Remage; Pillitteri, Ignazio; Wolk, Scott; Karovska, Margarita; Tingle, Evan; Guinan, Edward; Engle, Scott; Bond, Howard E.; Schaefer, Gail H.; Mason, Brian D.

2016-01-01

We have made XMM-Newton observations of 14 Galactic Cepheids that have candidate resolved (≥5″) companion stars based on our earlier HST Wide Field Camera 3 (WFC3) imaging survey. Main-sequence stars that are young enough to be physical companions of Cepheids are expected to be strong X-ray producers in contrast to field stars. XMM-Newton exposures were set to detect essentially all companions hotter than spectral type M0 (corresponding to 0.5 M ⊙ ). The large majority of our candidate companions were not detected in X-rays, and hence are not confirmed as young companions. One resolved candidate (S Nor #4) was unambiguously detected, but the Cepheid is a member of a populous cluster. For this reason, it is likely that S Nor #4 is a cluster member rather than a gravitationally bound companion. Two further Cepheids (S Mus and R Cru) have X-ray emission that might be produced by either the Cepheid or the candidate resolved companion. A subsequent Chandra observation of S Mus shows that the X-rays are at the location of the Cepheid/spectroscopic binary. R Cru and also V659 Cen (also X-ray bright) have possible companions closer than 5″ (the limit for this study) which are the likely sources of X-rays. One final X-ray detection (V473 Lyr) has no known optical companion, so the prime suspect is the Cepheid itself. It is a unique Cepheid with a variable amplitude. The 14 stars that we observed with XMM constitute 36% of the 39 Cepheids found to have candidate companions in our HST/WFC3 optical survey. No young probable binary companions were found with separations of ≥5″ or 4000 au

Бертольт Брехт все еще наш современник / Борис Тух

Index Scriptorium Estoniae

Тух, Борис, 1946-

2009-01-01

Bertolt Brechti näidend, mis kirjutatud Hella Wuolijoe jutustuste ja näidendikavandi järgi "Härra Punttila ja tema sulane Matti". Lavastaja Kalju Komissarov, esietendus 19. juunil Ugala tiigi kaldal

Mõisahärra Puntila teeb komejanti / Mari Hiiemäe

Index Scriptorium Estoniae

Hiiemäe, Mari

2009-01-01

Bertolt Brechti näidend, mis kirjutatud Hella Wuolijoe jutustuste ja näidendikavandi järgi "Härra Punttila ja tema sulane Matti". Lavastaja Kalju Komissarov, esietendus 19. juunil Ugala tiigi kaldal

Reportaaž hilissuviselt Hämemaalt / Meelis Oidsalu

Index Scriptorium Estoniae

Oidsalu, Meelis, 1978-

2009-01-01

Bertolt Brechti näidend, mis kirjutatud Hella Wuolijoe jutustuste ja näidendikavandi järgi "Härra Punttila ja tema sulane Matti". Lavastaja Kalju Komissarov, esietendus 19. juunil Ugala tiigi kaldal

Effects of Age, Season, Gender and Urban-Rural Status on Time-Activity: Canadian Human Activity Pattern Survey 2 (CHAPS 2

Directory of Open Access Journals (Sweden)

Carlyn J. Matz

2014-02-01

Full Text Available Estimation of population exposure is a main component of human health risk assessment for environmental contaminants. Population-level exposure assessments require time-activity pattern distributions in relation to microenvironments where people spend their time. Societal trends may have influenced time-activity patterns since previous Canadian data were collected 15 years ago. The Canadian Human Activity Pattern Survey 2 (CHAPS 2 was a national survey conducted in 2010–2011 to collect time-activity information from Canadians of all ages. Five urban and two rural locations were sampled using telephone surveys. Infants and children, key groups in risk assessment activities, were over-sampled. Survey participants (n = 5,011 provided time-activity information in 24-hour recall diaries and responded to supplemental questionnaires concerning potential exposures to specific pollutants, dwelling characteristics, and socio-economic factors. Results indicated that a majority of the time was spent indoors (88.9%, most of which was indoors at home, with limited time spent outdoors (5.8% or in a vehicle (5.3%. Season, age, gender and rurality were significant predictors of time activity patterns. Compared to earlier data, adults reported spending more time indoors at home and adolescents reported spending less time outdoors, which could be indicative of broader societal trends. These findings have potentially important implications for assessment of exposure and risk. The CHAPS 2 data also provide much larger sample sizes to allow for improved precision and are more representative of infants, children and rural residents.

Effects of age, season, gender and urban-rural status on time-activity: CanadianHuman Activity Pattern Survey 2 (CHAPS 2).

Science.gov (United States)

Matz, Carlyn J; Stieb, David M; Davis, Karelyn; Egyed, Marika; Rose, Andreas; Chou, Benedito; Brion, Orly

2014-02-19

Estimation of population exposure is a main component of human health risk assessment for environmental contaminants. Population-level exposure assessments require time-activity pattern distributions in relation to microenvironments where people spend their time. Societal trends may have influenced time-activity patterns since previous Canadian data were collected 15 years ago. The Canadian Human Activity Pattern Survey 2 (CHAPS 2) was a national survey conducted in 2010-2011 to collect time-activity information from Canadians of all ages. Five urban and two rural locations were sampled using telephone surveys. Infants and children, key groups in risk assessment activities, were over-sampled. Survey participants (n = 5,011) provided time-activity information in 24-hour recall diaries and responded to supplemental questionnaires concerning potential exposures to specific pollutants, dwelling characteristics, and socio-economic factors. Results indicated that a majority of the time was spent indoors (88.9%), most of which was indoors at home, with limited time spent outdoors (5.8%) or in a vehicle (5.3%). Season, age, gender and rurality were significant predictors of time activity patterns. Compared to earlier data, adults reported spending more time indoors at home and adolescents reported spending less time outdoors, which could be indicative of broader societal trends. These findings have potentially important implications for assessment of exposure and risk. The CHAPS 2 data also provide much larger sample sizes to allow for improved precision and are more representative of infants, children and rural residents.

Effects of Age, Season, Gender and Urban-Rural Status on Time-Activity: Canadian Human Activity Pattern Survey 2 (CHAPS 2)

Science.gov (United States)

Matz, Carlyn J.; Stieb, David M.; Davis, Karelyn; Egyed, Marika; Rose, Andreas; Chou, Benedito; Brion, Orly

2014-01-01

Estimation of population exposure is a main component of human health risk assessment for environmental contaminants. Population-level exposure assessments require time-activity pattern distributions in relation to microenvironments where people spend their time. Societal trends may have influenced time-activity patterns since previous Canadian data were collected 15 years ago. The Canadian Human Activity Pattern Survey 2 (CHAPS 2) was a national survey conducted in 2010–2011 to collect time-activity information from Canadians of all ages. Five urban and two rural locations were sampled using telephone surveys. Infants and children, key groups in risk assessment activities, were over-sampled. Survey participants (n = 5,011) provided time-activity information in 24-hour recall diaries and responded to supplemental questionnaires concerning potential exposures to specific pollutants, dwelling characteristics, and socio-economic factors. Results indicated that a majority of the time was spent indoors (88.9%), most of which was indoors at home, with limited time spent outdoors (5.8%) or in a vehicle (5.3%). Season, age, gender and rurality were significant predictors of time activity patterns. Compared to earlier data, adults reported spending more time indoors at home and adolescents reported spending less time outdoors, which could be indicative of broader societal trends. These findings have potentially important implications for assessment of exposure and risk. The CHAPS 2 data also provide much larger sample sizes to allow for improved precision and are more representative of infants, children and rural residents. PMID:24557523

Characteristic tests of ionization chamber and GM counter survey meters for beta-rays, (2)

International Nuclear Information System (INIS)

Suga, Shin-ichi; Bingo, Kazuyoshi; Kajimoto, Yoichi

1979-03-01

To estimate a beta-ray absorbed dose rate of contaminated skin, measurements were done twice by a survey meter without and with a filter, keeping the distance from the contaminated skin surface to the survey meter at 10 mm. The absorbed dose rate was obtained multiplying a net reading (equals a reading of survey meter's indicator measured without the filter minus that measured with the filter) by a multiplying factor. Calibrations were made with reference plane sources of natural uranium, 198 Au and 204 Tl, varying their area. The five types of ionization chamber survey meters had nearly same multiplying factors when the diameter of source was larger than the diameter of the chamber cylinder. Estimation of the absorbed doses due to beta-emitting nuclides was possible when the measured value without filter was larger by 20% or more than that of with filter. In the case of small sources, the multiplying factor varied significantly with area of the source. The multiplying factors agreed within +-30% in the respective types i.e. manufacturers and in maximum beta-ray energies from 0.7 up to 2.5 MeV. In the source to detector distance of 1 cm +-0.2 cm, the multiplying factor varied within +-20%. The multiplying factor of a GM counter survey meter varied with beta-ray energy, the multiplying factor for uranium was 1/3 that of 204 Tl. (author)

Swainson's Hawk Survey Grid - DFG Region 2 [ds697

Data.gov (United States)

California Natural Resource Agency — 5 km x 5 km landscape blocks used for Ca. Dept. of Fish and Game central valley Swainson's hawk nest surveys since 2000, edited for 2009 surveys using the following...

A survey of the 5C2 region with the Westerbork synthesis radio telescope at 1415 MHz (the third Westerbork survey), ch. 2

International Nuclear Information System (INIS)

Katgert, P.

1977-01-01

The 5C2 region, observed originally with the Cambridge One-Mile Telescope at 408 MHz, has been reobserved at l4l5 MHz. The resulting source list contains 238 sources with attenuated flux densities exceeding the catalogue limit of 6.25 m.f.u. Out of a total of 190 5C2 sources (i.e. all 5C2 sources within the 10 dB attenuation contour of the present survey), 128 were detected with flux densities above the catalogue limit. Another 22 5C2 sources were detected with flux densities below the catalogue limit. A discussion is given of the procedures used for determining source parameters. Special attention has been given to the determination of flux density and angular size as well as to the question of completeness of the source list as a function of flux density and angular size

Roman Policies towards Antiochus III and the Greeks from Winter 197/196 B.C. to Autumn 196 B.C.

Directory of Open Access Journals (Sweden)

Deutschmann, Eike Hellmut

2012-01-01

Full Text Available In the Second Macedonian War (200-196 B.C., the res publica reduced the strength of the enemy King Philip V apparently to establish a new political order in Southern Balkans: Assumedly a pro-Roman balance of forces should prevail there, untainted by influence of another major power. A particular senatorial policy towards the Greeks probably did not exist before the fighting in Hellas came to an end in summer 197 B.C. In the same year, the Seleucid king Antiochus III brought large parts of the west coast of Asia Minor under control and set about crossing the Hellespont. Rome subsequently stylized itself as the guardian of freedom for the Greeks living in Hellas and Asia Minor. The statesmen of the res publica could have perceived Antiochus’ expansion as a threat to the mentioned new order. Therefore, the Roman Policy of Freedom was possibly applied primarily to take action against the Seleucid king. Die res publica verminderte im Zweiten Makedonischen Krieg (200-196 a.c. die Macht des gegnerischen Königs Philipp V - anscheinend um eine neue politische Ordnung im südlichen Balkanraum zu etablieren: Vermutlich sollte dort ein romfreundliches Kräftegleichgewicht vorherrschen, auf das keine andere Großmacht Einfluß hat. Eine speziell an die Griechen gerichtete Politik seitens des römischen Senats gab es wahrscheinlich nicht vor Ende der Kampfhandlungen in Hellas im Sommer 197 a.c. In dem Jahr erweiterte der seleukidische König Antiochos III. seinen Einflussbereich auf große Teile der kleinasiatischen Westküste und schickte sich an, den Hellespont zu überqueren. Rom stilisierte sich in der Folgezeit zum Freiheitsgarant der in Hellas und Kleinasien lebenden Griechen. Antiochos Expansion könnte von den Staatsmännern der res publica als Bedrohung der genannten neuen Ordnung angesehen worden sein. Demzufolge wurde die römische Freiheitspolitik möglicherweise in erster Linie angewendet, um gegen den seleukidischen König vorzugehen.

A weak lensing analysis of the PLCK G100.2-30.4 cluster

Science.gov (United States)

Radovich, M.; Formicola, I.; Meneghetti, M.; Bartalucci, I.; Bourdin, H.; Mazzotta, P.; Moscardini, L.; Ettori, S.; Arnaud, M.; Pratt, G. W.; Aghanim, N.; Dahle, H.; Douspis, M.; Pointecouteau, E.; Grado, A.

2015-07-01

We present a mass estimate of the Planck-discovered cluster PLCK G100.2-30.4, derived from a weak lensing analysis of deep Subaru griz images. We perform a careful selection of the background galaxies using the multi-band imaging data, and undertake the weak lensing analysis on the deep (1 h) r -band image. The shape measurement is based on the Kaiser-Squires-Broadhurst algorithm; we adopt the PSFex software to model the point spread function (PSF) across the field and correct for this in the shape measurement. The weak lensing analysis is validated through extensive image simulations. We compare the resulting weak lensing mass profile and total mass estimate to those obtained from our re-analysis of XMM-Newton observations, derived under the hypothesis of hydrostatic equilibrium. The total integrated mass profiles agree remarkably well, within 1σ across their common radial range. A mass M500 ~ 7 × 1014M⊙ is derived for the cluster from our weak lensing analysis. Comparing this value to that obtained from our reanalysis of XMM-Newton data, we obtain a bias factor of (1-b) = 0.8 ± 0.1. This is compatible within 1σ with the value of (1-b) obtained in Planck 2015 from the calibration of the bias factor using newly available weak lensing reconstructed masses. Based on data collected at Subaru Telescope (University of Tokyo).

W. Richard Scott, Institutions and Organizations: Ideas, Interests, and Identities

DEFF Research Database (Denmark)

Jakobsen, Michael

2014-01-01

Book review of: W. Richard Scott: Institutions and Organizations: Ideas, Interests, and Identities. 4th edition. Thousand Oaks, CA: SAGE Publications, 2014. xiii, 345 pp.......Book review of: W. Richard Scott: Institutions and Organizations: Ideas, Interests, and Identities. 4th edition. Thousand Oaks, CA: SAGE Publications, 2014. xiii, 345 pp....

FY 1998 report on the verification survey of geothermal exploration technology, etc. 1/2. Survey of deep geothermal resource; 1998 nendo chinetsu tansa gijutsu nado kensho chosa hokokusho. 1/2. Shinbu chinetsu shigen chosa

Energy Technology Data Exchange (ETDEWEB)

NONE

1999-12-01

For the purpose of commercializing deep geothermal resource, a deep exploration well of 4000m class was drilled in the existing geothermal development area to survey the situation of deep geothermal resource existence and the availability. Concretely, the deep geothermal exploration well was drilled for study in the Kakkonda area, Shizukuishi town, Iwate prefecture, to clarify the situation of deep geothermal resource existence and the whole image of geothermal system. Consideration was made of the deep geothermal exploration method, systematization of deep high temperature drilling technology, and availability of deep geothermal resource. The results of the survey were summed up as follows: 1) general remarks; 2) deep exploration well drilling work; 3) details of the study. 1) and 2) were included in this report, and 3) in the next report. In 1), the items were as follows: the study plan/gist of study execution, the details and results of the deep geothermal resource survey, the outline of the deep exploration well drilling work, and the outline of the results of the FY 1998 study. In 2), the drilling work plan/the actual results of the drilling work were summed up. As to the results of the study, summarized were the acquisition of survey data on deep exploration well, heightening of accuracy of the deep geothermal resource exploration method, etc. (NEDO)

The Hyper Suprime-Cam SSP Survey: Overview and survey design

Science.gov (United States)

Aihara, Hiroaki; Arimoto, Nobuo; Armstrong, Robert; Arnouts, Stéphane; Bahcall, Neta A.; Bickerton, Steven; Bosch, James; Bundy, Kevin; Capak, Peter L.; Chan, James H. H.; Chiba, Masashi; Coupon, Jean; Egami, Eiichi; Enoki, Motohiro; Finet, Francois; Fujimori, Hiroki; Fujimoto, Seiji; Furusawa, Hisanori; Furusawa, Junko; Goto, Tomotsugu; Goulding, Andy; Greco, Johnny P.; Greene, Jenny E.; Gunn, James E.; Hamana, Takashi; Harikane, Yuichi; Hashimoto, Yasuhiro; Hattori, Takashi; Hayashi, Masao; Hayashi, Yusuke; Hełminiak, Krzysztof G.; Higuchi, Ryo; Hikage, Chiaki; Ho, Paul T. P.; Hsieh, Bau-Ching; Huang, Kuiyun; Huang, Song; Ikeda, Hiroyuki; Imanishi, Masatoshi; Inoue, Akio K.; Iwasawa, Kazushi; Iwata, Ikuru; Jaelani, Anton T.; Jian, Hung-Yu; Kamata, Yukiko; Karoji, Hiroshi; Kashikawa, Nobunari; Katayama, Nobuhiko; Kawanomoto, Satoshi; Kayo, Issha; Koda, Jin; Koike, Michitaro; Kojima, Takashi; Komiyama, Yutaka; Konno, Akira; Koshida, Shintaro; Koyama, Yusei; Kusakabe, Haruka; Leauthaud, Alexie; Lee, Chien-Hsiu; Lin, Lihwai; Lin, Yen-Ting; Lupton, Robert H.; Mandelbaum, Rachel; Matsuoka, Yoshiki; Medezinski, Elinor; Mineo, Sogo; Miyama, Shoken; Miyatake, Hironao; Miyazaki, Satoshi; Momose, Rieko; More, Anupreeta; More, Surhud; Moritani, Yuki; Moriya, Takashi J.; Morokuma, Tomoki; Mukae, Shiro; Murata, Ryoma; Murayama, Hitoshi; Nagao, Tohru; Nakata, Fumiaki; Niida, Mana; Niikura, Hiroko; Nishizawa, Atsushi J.; Obuchi, Yoshiyuki; Oguri, Masamune; Oishi, Yukie; Okabe, Nobuhiro; Okamoto, Sakurako; Okura, Yuki; Ono, Yoshiaki; Onodera, Masato; Onoue, Masafusa; Osato, Ken; Ouchi, Masami; Price, Paul A.; Pyo, Tae-Soo; Sako, Masao; Sawicki, Marcin; Shibuya, Takatoshi; Shimasaku, Kazuhiro; Shimono, Atsushi; Shirasaki, Masato; Silverman, John D.; Simet, Melanie; Speagle, Joshua; Spergel, David N.; Strauss, Michael A.; Sugahara, Yuma; Sugiyama, Naoshi; Suto, Yasushi; Suyu, Sherry H.; Suzuki, Nao; Tait, Philip J.; Takada, Masahiro; Takata, Tadafumi; Tamura, Naoyuki; Tanaka, Manobu M.; Tanaka, Masaomi; Tanaka, Masayuki; Tanaka, Yoko; Terai, Tsuyoshi; Terashima, Yuichi; Toba, Yoshiki; Tominaga, Nozomu; Toshikawa, Jun; Turner, Edwin L.; Uchida, Tomohisa; Uchiyama, Hisakazu; Umetsu, Keiichi; Uraguchi, Fumihiro; Urata, Yuji; Usuda, Tomonori; Utsumi, Yousuke; Wang, Shiang-Yu; Wang, Wei-Hao; Wong, Kenneth C.; Yabe, Kiyoto; Yamada, Yoshihiko; Yamanoi, Hitomi; Yasuda, Naoki; Yeh, Sherry; Yonehara, Atsunori; Yuma, Suraphong

2018-01-01

Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of the 8.2-m Subaru telescope on the summit of Mauna Kea in Hawaii. A team of scientists from Japan, Taiwan, and Princeton University is using HSC to carry out a 300-night multi-band imaging survey of the high-latitude sky. The survey includes three layers: the Wide layer will cover 1400 deg2 in five broad bands (grizy), with a 5 σ point-source depth of r ≈ 26. The Deep layer covers a total of 26 deg2 in four fields, going roughly a magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter still in two pointings of HSC (a total of 3.5 deg2). Here we describe the instrument, the science goals of the survey, and the survey strategy and data processing. This paper serves as an introduction to a special issue of the Publications of the Astronomical Society of Japan, which includes a large number of technical and scientific papers describing results from the early phases of this survey.

Thyroid-stimulating immunoglobulins as measured in a reporter bioassay are not detected in patients with Hashimoto’s thyroiditis and ophthalmopathy or isolated upper eyelid retraction

Directory of Open Access Journals (Sweden)

Wall JR

2014-10-01

Full Text Available Jack R Wall,1 Hooshang Lahooti,1 Ilhem El Kochairi,1 Simon D Lytton,2 Bernard Champion1 1Department of Medicine, the University of Sydney, Penrith, NSW, Australia; 2SeraDiaLogistics, Munich, Germany Abstract: Although ophthalmopathy is mainly associated with Graves’ hyperthyroidism, milder eye changes are also found in about 25% of patients with Hashimoto’s thyroiditis (HT. The recent finding of negative thyrotropin receptor (TSHR antibodies, as measured in the ­Thyretain™ thyroid-stimulating immunoglobulin (TSI reporter bioassay, in patients with euthyroid Graves’ disease raises the possibility that TSHR antibodies are not the cause of ophthalmopathy in all situations. Here, we have tested serum from patients with HT with and without ophthalmopathy or isolated upper eyelid retraction (UER for TSHR antibodies, using the TSI reporter bioassay and collagen XIII as a marker of autoimmunity against the orbital fibroblast. Study groups were 23 patients with HT with ophthalmopathy, isolated UER, or both eye features and 17 patients without eye signs. Thyretain™ TSI results were expressed as a percentage of the sample-to-reference ratio, with a positive test being taken as a sample-to-reference ratio of more than 140%. Serum collagen XIII antibodies were measured in standard enzyme-linked immunosorbent assay. TSI tests were positive in 22% of patients with HT with no eye signs but in no patient with eye signs. In contrast, TSI tests were positive in 94% of patients with Graves’ ophthalmopathy. Tests were negative in all normal subjects tested. Collagen XIII antibodies were detected in 83% of patients with ophthalmopathy, UER, or both eye features, but in only 30% of patients with no eye signs. Our findings suggest that TSHR antibodies do not play a major role in the pathogenesis of ophthalmopathy or isolated UER in patients with HT. Moreover, the role of TSHR antibodies in the development of ophthalmopathy in patients with Graves�

XMM-NEWTON MONITORING OF THE CLOSE PRE-MAIN-SEQUENCE BINARY AK SCO. EVIDENCE OF TIDE-DRIVEN FILLING OF THE INNER GAP IN THE CIRCUMBINARY DISK

Energy Technology Data Exchange (ETDEWEB)

Gomez de Castro, Ana Ines [S. D. Astronomia y Geodesia and Instituto de Matematica Interdisciplinar, Fac. de CC Matematicas, Universidad Complutense, E-28040 Madrid (Spain); Lopez-Santiago, Javier [Departamento de Astrofisica, Fac de CC Fisicas, Universidad Complutense, E-28040 Madrid (Spain); Talavera, Antonio [European Space Astronomy Center, Villanueva de la Canada, E-28691, Madrid (Spain); Sytov, A. Yu.; Bisikalo, D. [Institute of Astronomy of the Russian Academy of Sciences, Pyatnitskaya St. 48, 109017 Moscow (Russian Federation)

2013-03-20

AK Sco stands out among pre-main-sequence binaries because of its prominent ultraviolet excess, the high eccentricity of its orbit, and the strong tides driven by it. AK Sco consists of two F5-type stars that get as close as 11 R{sub *} at periastron passage. The presence of a dense (n{sub e} {approx} 10{sup 11} cm{sup -3}) extended envelope has been unveiled recently. In this article, we report the results from an XMM-Newton-based monitoring of the system. We show that at periastron, X-ray and UV fluxes are enhanced by a factor of {approx}3 with respect to the apastron values. The X-ray radiation is produced in an optically thin plasma with T {approx} 6.4 Multiplication-Sign 10{sup 6} K and it is found that the N{sub H} column density rises from 0.35 Multiplication-Sign 10{sup 21} cm{sup -2} at periastron to 1.11 Multiplication-Sign 10{sup 21} cm{sup -2} at apastron, in good agreement with previous polarimetric observations. The UV emission detected in the Optical Monitor band seems to be caused by the reprocessing of the high-energy magnetospheric radiation on the circumstellar material. Further evidence of the strong magnetospheric disturbances is provided by the detection of line broadening of 278.7 km s{sup -1} in the N V line with Hubble Space Telescope/Space Telescope Imaging Spectrograph. Numerical simulations of the mass flow from the circumbinary disk to the components have been carried out. They provide a consistent scenario with which to interpret AK Sco observations. We show that the eccentric orbit acts like a gravitational piston. At apastron, matter is dragged efficiently from the inner disk border, filling the inner gap and producing accretion streams that end as ring-like structures around each component of the system. At periastron, the ring-like structures come into contact, leading to angular momentum loss, and thus producing an accretion outburst.

2D Bayesian automated tilted-ring fitting of disc galaxies in large H I galaxy surveys: 2DBAT

Science.gov (United States)

Oh, Se-Heon; Staveley-Smith, Lister; Spekkens, Kristine; Kamphuis, Peter; Koribalski, Bärbel S.

2018-01-01

We present a novel algorithm based on a Bayesian method for 2D tilted-ring analysis of disc galaxy velocity fields. Compared to the conventional algorithms based on a chi-squared minimization procedure, this new Bayesian-based algorithm suffers less from local minima of the model parameters even with highly multimodal posterior distributions. Moreover, the Bayesian analysis, implemented via Markov Chain Monte Carlo sampling, only requires broad ranges of posterior distributions of the parameters, which makes the fitting procedure fully automated. This feature will be essential when performing kinematic analysis on the large number of resolved galaxies expected to be detected in neutral hydrogen (H I) surveys with the Square Kilometre Array and its pathfinders. The so-called 2D Bayesian Automated Tilted-ring fitter (2DBAT) implements Bayesian fits of 2D tilted-ring models in order to derive rotation curves of galaxies. We explore 2DBAT performance on (a) artificial H I data cubes built based on representative rotation curves of intermediate-mass and massive spiral galaxies, and (b) Australia Telescope Compact Array H I data from the Local Volume H I Survey. We find that 2DBAT works best for well-resolved galaxies with intermediate inclinations (20° < i < 70°), complementing 3D techniques better suited to modelling inclined galaxies.

40 CFR 82.13 - Recordkeeping and reporting requirements for class I controlled substances.

Science.gov (United States)

2010-07-01

... subpart) and will not be resold or used in manufacturing. (xiii) The amount of class I, Group VI... class II controlled substances; (xii) The U.S. Customs entry form; (xiii) Dated records documenting the..., an annual list of the amount of critical use methyl bromide bought; (ii) For critical uses of class I...

Multiwavelength follow-up observations of the tidal disruption event candidate 2XMMi J184725.1-631724

Science.gov (United States)

Lin, Dacheng; Strader, Jay; Carrasco, Eleazar R.; Godet, Olivier; Grupe, Dirk; Webb, Natalie A.; Barret, Didier; Irwin, Jimmy A.

2018-03-01

The ultrasoft X-ray flare 2XMMi J184725.1-631724 was serendipitously detected in two XMM-Newton observations in 2006 and 2007, with a peak luminosity of 6 × 1043 erg s-1. It was suggested to be a tidal disruption event (TDE) because its position is consistent with the centre of an inactive galaxy. It is the only known X-ray TDE candidate whose X-ray spectra showed evidence of a weak steep power-law component besides a dominant supersoft thermal disc. We have carried out multiwavelength follow-up observations of the event. Multiple X-ray monitorings show that the X-ray luminosity has decayed significantly after 2011. Especially, in our deep Chandra observation in 2013, we detected a very faint counterpart that supports the nuclear origin of 2XMMi J184725.1-631724 but had an X-ray flux a factor of ˜1000 lower than in the peak of the event. Compared with follow-up ultraviolet (UV) observations, we found that there might be some enhanced UV emission associated with the TDE in the first XMM-Newton observation. We also obtained a high-quality UV-optical spectrum with the Southern Astrophysical Research (SOAR) Telescope and put a very tight constraint on the persistent nuclear activity, with a persistent X-ray luminosity expected to be lower than the peak of the flare by a factor of >2700. Therefore, our multiwavelength follow-up observations strongly support the TDE explanation of the event.

The protostar OMC-2 FIR 4: Results from the CHESS Herschel/HIFI spectral survey

Science.gov (United States)

Kama, Mihkel; Lopez-Sepulcre, Ana; Ceccarelli, Cecilia; Dominik, Carsten; Caux, Emmanuel; Fuente, Asuncion

2013-07-01

The intermediate-mass protostar OMC-2 FIR 4 in Orion is the focus of several ongoing studies, including a CHESS key programme Herschel/HIFI spectral survey. In this poster, we review recent CHESS results on this source, including the properties of the central hot core, the presence of a compact outflow, the spatial variation of the chemical composition, and the discovery of a tenuous foreground cloud. The HIFI spectrum of FIR 4 contains 719 lines from 40 species and isotopologs. Cooling by lines detectable with our sensitivity contributes 2% of the total in the 480 to 1900 GHz range. The total line flux is dominated by CO, followed by H2O and CH3OH. Initial comparisons with spectral surveys of other sources will also be presented.

Fiscal 1996 survey of potential international cooperation for a long-term scenario on CO2 reduction; 1996 nendo CO2 sakugen ni kakawaru choki shinario ni kansuru kokusai kyoryoku kanosei chosa

Energy Technology Data Exchange (ETDEWEB)

NONE

1997-03-01

For the purpose of working out a CO2 reduction scenario and a CO2 policy introduction scenario, a survey was conducted of comparisons between ten and several models which are world-known and models of the New Earth 21, potential international cooperation to be carried out in the future, etc. The survey included organizations which are developing CO2 policy evaluation models, survey reports made in the past, details of literature for the analysis and arrangement. From the result, details of the questionnaire survey and organizations to be surveyed were decided on for the questionnaire survey. Objects for the survey were 7 countries and 22 organizations, and survey items were places for information exchange, sending/receiving of researchers, exchange of input data, comparative calculation based on the common database, joint research work, economy, the carbon tax, impact, renewable energy, how to handle and think of the carbon isolation, etc. As a result of the survey, proposed were a workshop on CO2 reduction, a comparative study of simulation models, etc. 25 refs., 50 figs., 12 tabs.

Microtensile Bond Strength and Micromorphology of Bur-cut Enamel Using Five Adhesive Systems.

Science.gov (United States)

Vinagre, Alexandra; Ramos, João; Messias, Ana; Marques, Fernando; Caramelo, Francisco; Mata, António

2015-04-01

This study compared the microtensile bond strengths (μTBS) of two etch-and-rinse (ER) (OptiBond FL [OBFL]; Prime & Bond NT [PBNT]) and three self-etching (SE) (Clearfil SE Bond [CSEB]; Xeno III [XIII]; Xeno V+ [XV+]) adhesives systems to bur-prepared human enamel considering active (AA) and passive (PA) application of the self-etching systems. Ninety-six enamel surfaces were prepared with a medium-grit diamond bur and randomly allocated into 8 groups to receive adhesive restorations: G1: OBFL; G2: PBNT; G3: CSEB/PA; G4: CSEB/ AA; G5: XIII/PA; G6: XIII/AA; G7: XV+/PA; G8: XV+/AA. After composite buildup, samples were sectioned to obtain a total of 279 bonded sticks (1 mm2) that were submitted to microtensile testing (μTBS; 0.5 mm/min) after 24-h water storage (37°C). Etching patterns and adhesive interfacial ultramorphology were also evaluated with confocal laser scanning (CLSM) and scanning electron microscopy (SEM). Data was analyzed with one-way ANOVA (α = 0.05). Weibull probabilistic distribution was also determined. Regarding μTBS, both adhesive system and application mode yielded statistically significant differences (p systems together with CSEB/AA and XIII/PA recorded the highest and statistically similar bond strength results. XV+ presented very low bond strength values, regardless of the application mode. Among self-etching adhesives, CSEB produced significantly higher μTBS values when applied actively. Qualitative evaluation by SEM and CLSM revealed substantial differences between groups both in adhesive interfaces and enamel conditioning patterns. ER and SE adhesive systems presented distinctive bond strengths to bur-cut enamel. The application mode effect was adhesive dependent. Active application improved etching patterns and resin interfaces micromorphology.

Diuretics: from classical carbonic anhydrase inhibitors to novel applications of the sulfonamides.

Science.gov (United States)

Supuran, Claudiu T

2008-01-01

The widely clinically used benzothiadiazines and high ceiling diuretics, such as hydrochlorothiazide, hydroflumethiazide, quinethazone, metolazone, chlorthalidone, indapamide, furosemide and bumetanide, contain SO(2)NH(2) moieties acting as an effective zinc-binding function in carbonic anhydrases (CAs, EC 4.2.1.1) inhibitors. These drugs were launched in a period when only isoform CA II was known and considered physiologically/pharmacologically relevant. Although acting as moderate-weak inhibitors of CA II, all these drugs considerably inhibit other CA isozymes known nowadays to be involved in critical physiologic processes, among the 16 CAs present in vertebrates. Some low nanomolar (or even subnanomolar) inhibitors against such isoforms were recently detected, such as metholazone against CA VII, XII and XIII, chlorthalidone against CA VB, VII, IX, XII and XIII, indapamide against CA VII, IX, XII and XIII, furosemide against CA I, II and XIV, and bumethanide against CA IX and XII. The X-ray crystal structure of the CA II-indapamide adduct was also reported recently, revealing interesting aspects useful for the drug design of CA inhibitors. It has also been proposed that the recently observed beneficial effect of indapamide for the treatment of patients with hypertension and type 2 diabetes might be due to its potent inhibition of CA isoforms present in kidneys and blood vessels, which would thus explain both the blood pressure lowering effects as well as organ-protective activity of the drug. Thus, these old drugs may be useful as leads for new applications.

An internet survey of 2,596 people with fibromyalgia

Directory of Open Access Journals (Sweden)

Turk Dennis C

2007-03-01

Full Text Available Abstract Background This study explored the feasibility of using an Internet survey of people with fibromyalgia (FM, with a view to providing information on demographics, sources of information, symptoms, functionality, perceived aggravating factors, perceived triggering events, health care utilization, management strategies, and medication use. Methods A survey questionnaire was developed by the National Fibromyalgia Association (NFA in conjunction with a task force of "experts in the field". The questionnaire underwent several rounds of testing to improve its face validity, content validity, clarity and readability before it was mounted on the internet. The questionnaire consisted of 121 items and is available online at the website of the National Fibromyalgia Association. Results The questionnaire was completed by 2,569 people. Most were from the United States, with at least one respondent from each of the 50 states. Respondents were predominantly middle-aged Caucasian females, most of whom had FM symptoms for ≥ 4 years. The most common problems were morning stiffness, fatigue, nonrestorative sleep, pain, concentration, and memory. Aggravating factors included: emotional distress, weather changes, insomnia, and strenuous activity. Respondents rated the most effective management modalities as rest, heat, pain medications, antidepressants, and hypnotics. The most commonly used medications were: acetaminophen, ibuprofen, naproxen, cyclobenzaprine, amitriptyline, and aspirin. The medications perceived to be the most effective were: hydrocodone preparations, aprazolam, oxycodone preparations, zolpidem, cyclobenzaprine, and clonazepam. Conclusion This survey provides a snap-shot of FM at the end of 2005, as reported by a self-selected population of people. This descriptive data has a heuristic function, in that it identifies several issues for further research, such as the prescribing habits of FM health care providers, the role of emotional

Melhoramento do cafeeiro: XIII - Café bourbon amarelo Coffee breeding: XIII - yellow bourbon coffee

Directory of Open Access Journals (Sweden)

A. Carvalho

1957-01-01

Full Text Available Um conjunto de 30 plantas matrizes de Bourbon Amarelo foi selecionado em 1945, em Jaú, na propriedade "Fazendinha". As progênies dêsses cafeeiros foram plantadas nas Estações Experimentais do Instituto Agronômico em Campinas, Ribeirão Preto, Pindorama, Mococa e Jaú, em linhas de 20 plantas. Diversas observações foram feitas relativas ao desenvolvimento dos cafeeiros, produção e tipos de sementes. De maneira geral o desenvolvimento foi considerado muito bom, com exceção de Mococa, onde as plantas apresentaram porte e produção menores devido ao terreno mais pobre onde foram plantadas. Embora tenha havido variações acentuadas no comportamento das progênies quanto à produção, verificou-se que as de n. J 30, J 3, J 8, J 10, J 11 e J 24 classificaram-se como as melhores nas cinco localidades, ao fim de oito anos seguidos de produção. As melhores plantas das boas progênies já foram incluídas em campos de aumento e suas sementes vêm sendo distribuídas aos lavradores. Notou-se acentuada variação de produção anual do conjunto de progênies, principalmente a partir do quarto ano de colheita. As produções bienais cresceram até o terceiro biênio, estacionando ou diminuindo no quarto. Notou-se que algumas progénies são tardias na produção, de modo que não será aconselhável a seleção precoce de progênies de Bourbon Amarelo eliminando-se as menos produtivas logo após o primeiro biênio de produção. Verificou-se, também, que as plantas de maior produção total pertencem, em grande parte, a progênies que apresentam produção média geral elevada, as quais, por sua vez, possuem variabilidade menor de produção. A curva de distribuição da produção total das plantas individuais mostrou-se variável.nas diferentes localidades; em tôdas verificou-se a ocorrência de plantas muito pouco produtivas, com produções médias inferiores à média geral subtraída de 2,57 vezes o desvio padrão geral do lote. A

Europe's latest space telescope is off to a good start

Science.gov (United States)

1999-12-01

The world's most powerful observatory for X-ray astronomy, the European Space Agency's XMM satellite, set off into space from Kourou, French Guiana, at 15:32 Paris time on 10 December. The mighty Ariane 5 launcher, making its very first commercial launch, hurled the 3.9-tonne spacecraft into a far-ranging orbit. Within one hour of lift-off the European Space Operations Centre at Darmstadt, Germany, confirmed XMM was under control with electrical power available from the solar arrays. "XMM is the biggest and most innovative scientific spacecraft developed by ESA so far," said Roger Bonnet, ESA's Director of Science. "The world's space agencies now want the new technology that ESA and Europe's industries have put into XMM's amazingly sensitive X-ray telescopes. And the world's astronomers are queuing up to use XMM to explore the hottest places in the universe. We must ask them to be patient while we get XMM fully commissioned." XMM's initial orbit carries it far into space, to 114,000 kilometres from the Earth at its most distant point. On its return the satellite's closest approach, or perigee, will be at 850 kilometres. The next phase of the operation, expected to take about a week, will raise that perigee to 7000 kilometres by repeated firing of XMM's own thrusters. The spacecraft will then be on its intended path, spending 40 hours out of every 48-hour orbit clear of the radiation belts which spoil the view of the X-ray universe. Technical commissioning and verification of the performance of the telescopes and scientific instruments will then follow. XMM should be fully operational for astronomy in the spring of 2000. All of ESA's science missions present fresh technological challenges to Europe's aerospace industries. In building XMM, the prime contractor Dornier Satellitensysteme in Friedrichshafen in Germany (part of DaimlerChrysler Aerospace) has led an industrial consortium involving 46 companies from 14 European countries and one in the United States. XMM

Independent verification survey report for exposure units Z2-24, Z2-31, Z2-32, AND Z2-36 in zone 2 of the East Tennessee technology park Oak Ridge, Tennessee

Energy Technology Data Exchange (ETDEWEB)

King, David A. [Oak Ridge Inst. for Science and Education (ORISE), Oak Ridge, TN (United States)

2013-10-01

The U.S. Department of Energy (DOE) Oak Ridge Office of Environmental Management selected Oak Ridge Associated Universities (ORAU), through the Oak Ridge Institute for Science and Education (ORISE) contract, to perform independent verification (IV) at Zone 2 of the East Tennessee Technology Park (ETTP) in Oak Ridge, Tennessee. ORAU has concluded IV surveys, per the project-specific plan (PSP) (ORAU 2013a) covering exposure units (EUs) Z2-24, -31, -32, and -36. The objective of this effort was to verify the target EUs comply with requirements in the Zone 2 Record of Decision (ROD) (DOE 2005), as implemented by using the dynamic verification strategy presented in the dynamic work plan (DWP) (BJC 2007); and confirm commitments in the DWP were adequately implemented, as verified via IV surveys and soil sampling.

Redshift Survey Strategies

Science.gov (United States)

Jones, A. W.; Bland-Hawthorn, J.; Kaiser, N.

1994-12-01

In the first half of 1995, the Anglo-Australian Observatory is due to commission a wide field (2.1(deg) ), 400-fiber, double spectrograph system (2dF) at the f/3.3 prime focus of the AAT 3.9m bi-national facility. The instrument should be able to measure ~ 4000 galaxy redshifts (assuming a magnitude limit of b_J ~\\ 20) in a single dark night and is therefore ideally suited to studies of large-scale structure. We have carried out simple 3D numerical simulations to judge the relative merits of sparse surveys and contiguous surveys. We generate a survey volume and fill it randomly with particles according to a selection function which mimics a magnitude-limited survey at b_J = 19.7. Each of the particles is perturbed by a gaussian random field according to the dimensionless power spectrum k(3) P(k) / 2pi (2) determined by Feldman, Kaiser & Peacock (1994) from the IRAS QDOT survey. We introduce some redshift-space distortion as described by Kaiser (1987), a `thermal' component measured from pairwise velocities (Davis & Peebles 1983), and `fingers of god' due to rich clusters at random density enhancements. Our particular concern is to understand how the window function W(2(k)) of the survey geometry compromises the accuracy of statistical measures [e.g., P(k), xi (r), xi (r_sigma ,r_pi )] commonly used in the study of large-scale structure. We also examine the reliability of various tools (e.g. genus) for describing the topological structure within a contiguous region of the survey.

Fundamentos históricos e teóricos da noção de soberania: a contribuição dos "Papas juristas" do século XIII

Directory of Open Access Journals (Sweden)

Raquel Kritsch

2010-12-01

Full Text Available O objetivo deste artigo é discutir a contribuição do pensamento eclesiástico medieval tardio para a formação do conceito de soberania. Como o Estado moderno, tal conceito tem uma gênese demorada: é parte de um processo de transformação jurídica e política, do qual resulta um novo mapeamento do poder e das lealdades na Europa. A conformação desse novo sistema de poder tem como contrapartida a constituição de uma nova ordem jurídica. Essa ordem redefine os vínculos de comando e obediência, constituindo unida des políticas como áreas de jurisdição exclusiva e estabelecendo, entre essas unidades, relações de igualdade: nenhuma se reconhece como subordinada a outra. Todas essas questões podem ser entendidas como disputas de jurisdição. Trata-se de saber quem julga e quem pune delitos civis ou violações de normas religiosas. Os poderes de legislar, de mudar a lei, de resolver como últi ma instância e de controlar o uso da violência constituem o que os autores modernos nomearam soberania. Apontar a contribuição dos chamados Papas juristas do século XIII para a formulação de alguns elementos centrais a esta definição é a tarefa a ser leva da a cabo neste estudo.

AKARI NEAR-INFRARED SPECTROSCOPIC SURVEY FOR CO{sub 2} IN 18 COMETS

Energy Technology Data Exchange (ETDEWEB)

Ootsubo, Takafumi [Astronomical Institute, Graduate School of Science, Tohoku University, Aramaki, Aoba-ku, Sendai 980-8578 (Japan); Kawakita, Hideyo; Hamada, Saki; Kobayashi, Hitomi; Yamaguchi, Mitsuru [Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-Ku, Kyoto 603-8555 (Japan); Usui, Fumihiko; Nakagawa, Takao; Ueno, Munetaka [Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210 (Japan); Ishiguro, Masateru [Department of Physics and Astronomy, Seoul National University, 599 Gwanak-ro, Gwanak-gu, Seoul 151-742 (Korea, Republic of); Sekiguchi, Tomohiko [Department of Teacher Training, Hokkaido University of Education, Asahikawa Campus, Hokumon 9, Asahikawa, Hokkaido 070-8621 (Japan); Watanabe, Jun-ichi [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Sakon, Itsuki; Shimonishi, Takashi; Onaka, Takashi, E-mail: ootsubo@astr.tohoku.ac.jp [Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan)

2012-06-10

We conducted a spectroscopic survey of cometary volatiles with the Infrared Camera on board the Japanese infrared satellite AKARI in the wavelength range from 2.5 to 5 {mu}m. In our survey, 18 comets, including both the Oort cloud comets and the Jupiter-family comets, were observed in the period from 2008 June to 2010 January, most of which were observed at least twice. The prominent emission bands in the observed spectra are the fundamental vibrational bands of water (H{sub 2}O) at 2.7 {mu}m and carbon dioxide (CO{sub 2}) at 4.3 {mu}m. The fundamental vibrational band of carbon monoxide (CO) around 4.7 {mu}m and the broad emission feature, probably related to carbon-hydrogen-bearing molecules, can also be recognized around the 3.3-3.5-{mu}m region in some of the comets. With respect to H{sub 2}O, gas production rate ratios of CO{sub 2} have been derived in 17 comets, except for the comet 29P/Schwassmann-Wachmann 1. Our data set provides the largest homogeneous database of CO{sub 2}/H{sub 2}O production rate ratios in comets obtained so far. The CO{sub 2}/H{sub 2}O production rate ratios are considered to reflect the composition of cometary ice when a comet is observed at a heliocentric distance within {approx}2.5 AU, since H{sub 2}O ice fully sublimates there. The CO{sub 2}/H{sub 2}O ratio in cometary ice spans from several to {approx}30% among the comets observed at <2.5 AU (13 out of the 17 comets). Alternatively, the ratio of CO/CO{sub 2} in the comets seems to be smaller than unity based on our observations, although we only obtain upper limits for CO in most of the comets.