WorldWideScience

Sample records for astrographs

  1. Astrographic Positions of Minor Planets

    Science.gov (United States)

    Naskrecki, W.; Swierkowska, S.

    The paper presents the photographic position of minor planets taken in the years 1986/1987 at the Astronomical Observatory of A. Mickiewicz University, Poznan, with an astrograph of the F=1500 mm, d=300 mm.

  2. Optical Design of Astrograph for 'Interplanetary Solar Stereoscopic Observatory'

    International Nuclear Information System (INIS)

    In the project of the 'Interplanetary Solar Stereoscopic Observatory' (ISSO) the astrograph with the high resolution is one of the basic tools. Optical requirements to the tool are discussed. Creation the astrograph as the three-mirror system is offered. Design variants of the scheme with all third-order aberrations correction are presented. Obscuration is considered in the obtained variants

  3. The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)

    CERN Document Server

    Zacharias, Norbert; Girard, Terry; Henden, Arne; Bartlett, Jennifer; Monet, Dave; Zacharias, Marion

    2012-01-01

    The fourth United States Naval Observatory (USNO) CCD Astrograph Catalog, UCAC4 was released in August 2012 (double-sided DVD and CDS data center Vizier catalog I/322). It is the final release in this series and contains over 113 million objects; over 105 million of them with proper motions. UCAC4 is an updated version of UCAC3 with about the same number of stars also covering all-sky. Bugs were fixed, Schmidt plate survey data were avoided, and precise 5-band photometry were added. Astrograph observations have been supplemented for bright stars by FK6, Hipparcos and Tycho-2 data to compile a UCAC4 star catalog complete to about magnitude R = 16. Epoch 1998 to 2004 positions are obtained from observations with the 20 cm aperture USNO Astrograph's red lens, equipped with a 4k by 4k CCD. Mean positions and proper motions are derived by combining these observations with over 140 ground- and space-based catalogs, including Hipparcos/Tycho and the AC2000.2, as well as unpublished measures of over 5000 plates from ...

  4. Astrometric CCD observations of the third and the fourth moons of Uranus with the normal astrograph at the Pulkovo observatory

    Science.gov (United States)

    Dement'eva, A. A.

    2015-09-01

    The results of astrometric CCD observations of two major moons of Uranus (Oberon and Titania) with the Normal Astrograph ( D/F = 0.33 m/3.5 m; CCD S2C with a FOV of 18' × 16') at the Pulkovo Observatory are presented. The observations were conducted in 2008-2011. The CCD image reduction is based on the Turner method with a reference to the UCAC3 catalogue system. The (O-C) values are calculated with the use of the MULTI-SAT server for the ephemerides of planetary moons. The obtained equatorial coordinates are compared to two modern theories of planetary motion: INPOP10 + Lainey (2008) and DE421/LE421 + Lainey (2008). The observations agree well with both theories.

  5. Precise Astrographic Positions of Minor Planets Obtained at the Poznan University Observatory

    Science.gov (United States)

    Matz, D.; Swierkowska, S.

    The paper presents the photographic positions of bright minor planets taken in the years 1984 - 1985 at the Astronomical Observatory of A. Mickiewicz University, Poznań, with a Zeiss refractor (f = 3000 mm, d = 200 mm).

  6. Division i / Commission 8 / Working Group Astrographic Catalogue and Carte du Ciel Plates

    Science.gov (United States)

    Bucciarelli, Beatrice; Fresnau, Alain; Abad, Carlos; Argyle, Robert W.; Biggs, James; Brosch, Noah; Coyne, George V.; Davoust, Emmanuael; De Cuyper, Jean-Pierre M.; van Dessel, Edwin L.; Ducourant, Christine; Fierro, Ivan H. Bustos; Geffert, Michael; Glushkova, Elena V.; Irwin, Michael J.; Jones, Dayton L.; Lumme, Kari A.; Muiños, J. L.; Odenkirchen, Michael; Orellana, Rosa B.; Pauwels, Thierry; Rafferty, Theodore J.; Sanchez, M.; Sanner, Jörg; Tsvetkov, Milcho K.; Vaughan, Alan E.

    2007-12-01

    Various experiments have definitely demonstrated that one-micron accuracy (0.″06) on the definition of stellar images on CdC plates cannot be claimed, as it was speculated back in 1999. More realistically, a 2-3 micron accuracy is achievable, getting worse toward the survey magnitude limit, with an average magnitude error of 0.3. The level of astrometric accuracy corresponds to a 0.″2 - 0.″3 error in position at Epoch 1900, which, once used as first Epoch for proper motion determination in combination with modern epoch observations, can produce errors at the level of 2-5 mas/yr, thereby allowing to detect stellar motions larger than 0.″01/yr, which at a distance of 500 pc from the Sun correspond to ~25-60 km/s tangential velocity. Therefore, the AC/CdC heritage collection can be regarded as a highly valuable first-epoch material, e.g., for the realization of a Tycho-2 extension to fainter magnitudes (~15 photographic), especially in selected areas where radial velocity data are available, for the exploration of stellar kinematics beyond our solar neighborhood.

  7. Matlab在天文底片数字化中的应用%Application of Matlab in Digitization of Astrographic Plates

    Institute of Scientific and Technical Information of China (English)

    傅承启; 赵建海

    2010-01-01

    采用Matlab语言开发了天文底片数字化处理软件SDAPM.利用该软件可以处理商用平板扫描仪输出的照相底片扫描文件.由于Matlab语言强大的图形处理功能,使处理程序比用FORTRAN编制的处理程序大为简化.除了介绍程序的主要流程以外,还对该软件用到的一些Matlab特殊函数的具体用法(特别是曲面拟合)和如何解决内存不足的问题做了简要介绍.

  8. Project "FON" in post-Hipparcos era.

    Science.gov (United States)

    Kislyuk, V. S.; Yatsenko, A. I.; Yatskiv, Ya. S.

    The project of fourfold coverage of the northern hemisphere of the sky known as FON is carried out by means of C. Zeiss (Jena) wide-angle astrographs installed at six observatories of the former USSR. The authors intend to get the FON astrometric catalogue (mB < 13.5) of approximately 2 million stars of the northern hemisphere of the sky.

  9. Positions of Pluto extracted from digitized Pulkovo photographic plates taken in 1930 - 1960

    OpenAIRE

    Khrutskaya, E. V.; Cuyper, J.-P.; Kalinin, S. I.; Berezhnoy, A. A.; Decker, G.

    2013-01-01

    We present the results of determination of Pluto's positions derived from photographic plates taken in 1930 - 1960. Observations were made with Normal Astrograph at Pulkovo Observatory. Digitization of these plates was performed with high precision scanner at Royal Observatory of Belgium (ROB Digitizer). Mean values of standard errors of plate positions (x,y) lie between 12 and 18 mas. The UCAC4 catalogue was used as an astrometric calibrator. Standard errors of equatorial coordinates obtaine...

  10. PIRATE: A Remotely-Operable Telescope Facility for Research and Education

    OpenAIRE

    Holmes, S.; Kolb, U.; Haswell, C. A.; Burwitz, V.; Lucas, R. J.; Rodriguez, J.(Florida International University, Miami, USA); Rolfe, S. M.; Rostron, J.; Barker, J

    2011-01-01

    We introduce PIRATE, a new remotely-operable telescope facility for use in research and education, constructed from 'off-the-shelf' hardware, operated by The Open University. We focus on the PIRATE Mark 1 operational phase where PIRATE was equipped with a widely- used 0.35m Schmidt-Cassegrain system (now replaced with a 0.425m corrected Dall Kirkham astrograph). Situated at the Observatori Astronomic de Mallorca, PIRATE is currently used to follow up potential transiting extrasolar planet can...

  11. Preliminary results of processing of Pulkovo series of photographic observations of double star 61 Cygni measured by automatic machine "Fantasy"

    Science.gov (United States)

    Gorshanov, D. L.; Shakht, N. A.; Kisselev, A. A.; Polyakov, E. V.; Bronnikova, A. A.; Kanaev, I. I.

    2003-11-01

    Two long-term series of photographic observations of one of the nearest double star 61 Cygni have been obtained at Pulkovo by means of normal astrograph in 1895-2000 (I) and by means of 26'' refractor in 1958-2000 (II). All these observations have been measured by means automatic machine "Fantasy" with mean error of yearly positions 0.016'' and 0.008'' for I and II series correspondly. The periodic deviations with period 6.4 +/- 0.5 yr in the residuals in relative distances between components are noticed for series II.

  12. Determination of proper motions and membership of the open star cluster NGC2548

    CERN Document Server

    Wu Zi Yu; Balaguer-Nuñez, L; Jordi, C; Zhao, J L; Guibert, J

    2001-01-01

    Absolute proper motions, their corresponding errors and membership probabilities of 501 stars in the intermediate-age open cluster NGC2548 region are determined from MAMA measurements of 10 photographic plates. The plates have the maximum epoch difference of 82 years and they were taken with the double astrograph at Zo-Se station of Shanghai Observatory, which has an aperture of 40 cm and a plate scale of 30"/mm. The average proper motion precision is 1.18 mas/yr. These proper motions are used to determine the membership probabilities of stars in the region. The number of stars with membership probabilities higher than 0.7 is 165.

  13. Positions of Pluto extracted from digitized Pulkovo photographic plates taken in 1930 - 1960

    CERN Document Server

    Khrutskaya, E V; Kalinin, S I; Berezhnoy, A A; de Decker, G

    2013-01-01

    We present the results of determination of Pluto's positions derived from photographic plates taken in 1930 - 1960. Observations were made with Normal Astrograph at Pulkovo Observatory. Digitization of these plates was performed with high precision scanner at Royal Observatory of Belgium (ROB Digitizer). Mean values of standard errors of plate positions (x,y) lie between 12 and 18 mas. The UCAC4 catalogue was used as an astrometric calibrator. Standard errors of equatorial coordinates obtained are within 85 to 100 mas. Final table contains 63 positions of Pluto referred to the HCRF/UCAC4 frame.

  14. VizieR Online Data Catalog: 1103 parallaxes and proper motions from URAT (Finch+, 2016)

    Science.gov (United States)

    Finch, C. T.; Zacharias, N.

    2016-07-01

    We present 1103 trigonometric parallaxes and proper motions from the United States Naval Observatory (USNO) Robotic Astrometric Telescope (URAT) observations taken at the Naval Observatory Flagstaff Station (NOFS). URAT observes through a single filter (part of the dewar window) to provide a fixed bandpass of about 680 to 760nm. The clear aperture of the USNO astrograph is 206mm with a focal length of only 2m. A single exposure covers 28 square degrees with a resolution of 0.9arcsec/pixel. Each of the four large CCDs in the focal plane covers a 2.65 by 2.65 deg area on the sky. Data of all three years of operations (2012 April to 2015 June) at the NOFS are used here for this parallax investigation. For more details about the project, instrument, and observing the reader is referred to the URAT1 paper (Zacharias et al. 2015, cat. I/329). (3 data files).

  15. Astrometrical Observations of Pluto - Charon System with the Automated Telescopes of Pulkovo Observatory

    CERN Document Server

    Devyatkin, Alexander V; Slesarenko, Vyacheslav Yu

    2015-01-01

    The space probe 'New Horizon' was launched on 19th of January 2006 in order to study Pluto and its moons. Spacecraft will fly by Pluto as close as 12500 km in the middle of July 2015 and will get the most detailed images of Pluto and its moon until this moment. At the same time, observation obtained by the ground-based telescopes may also be helpful for the research of such distant system. Thereby, the Laboratory of observational astrometry of Pulkovo Observatory of RAS made a decision to reprocess observations obtained during last decade. More than 350 positional observations of Pluto - Charon system were carried out with the mirror astrograph ZA-320M at Pulkovo and Maksutov telescope MTM-500M near Kislovodsk. These observations were processed by means of software system APEX-II developed in Pulkovo observatory and numerical simulation was performed to calculate the differences between positions of photocenter and barycenter of Pluto - Charon system.

  16. The Silicon Photomultiplier for High Speed Photometry

    Science.gov (United States)

    Vander Haagen, Gary A.

    2011-05-01

    The Silicon Photomultiplier (SPM) offers sensitivity comparable to conventional photomultipliers with the added advantage of small size, low operating voltages, and robust tolerance to excess/ambient light. A Peltier cooled SPM running at -30°C was used in conjunction with wideband electronics and a 17-inch Astrograph to collect photometric data without a reference star. High speed photometric trials were conducted on eclipsing binary AW UMa demonstrating fast data rate capability. Data shows the SPM exhibits excellent sensitivity, acceptable signal to noise, and bandwidth with sampling times as short as 1 millisecond for brighter targets. Automated digital data acquisition is discussed along with digital signal processing techniques for noise reduction, spectral analysis, and data mining. The SPM demonstrated acceptable signal to noise for fast photometric studies for 8-10th magnitude targets depending on scintillation and background conditions. Future SPM study topics are also discussed.

  17. VizieR Online Data Catalog: BVRI photometry of nova V445 Pup (Goranskij+, 2010)

    Science.gov (United States)

    Goranskij, V. P.; Shugarov, S. Yu.; Zharova, A. V.; Kroll, P.; Barsukova, E. A.

    2012-05-01

    In the Moscow SAI plate collection, we found 51 plates with images of V445 Pup taken with the SAI Crimean Station 40-cm f/4 astrograph and dated between 15 November 1969 and 4 November 1989. We found 56 measurable images of V445 Pup on the plates of the Sonneberg Observatory collection dated between 19 March 1984 and 17 January 1991. Additionally, we measured all the Internet-accessible Digital Sky Survey images of V445 Pup in B,R, and I bands and used 2MASS JHK magnitudes to study the spectral energy distribution of the progenitor. We performed our observations of the V445 Pup remnant between 31 March 2003 and 20 October 2009. These observations were acquired in the Special Astrophysical Observatory (SAO), with the 1-m Zeiss reflector and CCD UBVRcIc photometer equipped with an EEV 42-40 CCD chip. (4 data files).

  18. Carte du Ciel, San Fernando zone

    Science.gov (United States)

    Abad, C.

    2014-06-01

    An updated summary of a future large astrometric catalogue is presented, based on the two most important astrometric projects carried out by the Real Instituto y Observatorio de la Armada de San Fernando (ROA). The goal is to make a catalogue of positions and proper motions based on ROA's Cart du Ciel (CdC) and the Astrographic Catalogue (AC) San Fernando zone plates, and the HAMC2 meridian circle catalogue. The CdC and AC plates are being reduced together to provide first-epoch positions while HAMC2 will provide second-epoch ones. New techniques have been applied, that range from using a commercial flatbed scanner to the proper reduction schemes to avoid systematics from it. Only thirty plates (out of 540) remain to be processed, due to scanning problems that are being solved.

  19. New Variable Stars on Digitized Moscow Collection Plates. Field 66 Ophiuchi (Northern Half)

    CERN Document Server

    Kolesnikova, D M; Sokolovsky, K V; Antipin, S V; Samus, N N

    2008-01-01

    We initiated digitization of the Moscow collection of astronomical plates using flatbed scanners. Techniques of photographic photometry of the digital images were applied, enabling an effective search for new variable stars. Our search for new variables among 140000 stars in the 10 x 5 degrees northern half of the field centered at 66 Oph, photographed with the Sternberg Institute's 40-cm astrograph in 1976--1995, gave 274 new discoveries, among them: 2 probable Population II Cepheids; 81 eclipsing variables; 5 high-amplitude Delta Scuti stars (HADSs); 82 RR Lyr stars; 62 red irregular variables and 41 red semiregular stars; 1 slow irregular variable not red in color. Light elements were determined for periodic variable stars. We detected about 30 variability suspects for follow-up CCD observations, confirmed 11 stars from the New Catalogue of Suspected Variable Stars, and derived new light elements for 2stars already contained in the General Catalogue of Variable Stars.

  20. Astrometrical observations of Pluto-Charon system with the automated telescopes of Pulkovo observatory

    Science.gov (United States)

    Slesarenko, V. Yu.; Bashakova, E. A.; Devyatkin, A. V.

    2016-03-01

    The space probe "New Horizons" was launched on 19th of January 2006 in order to study Pluto and its moons. Spacecraft performed close fly-by to Pluto on 14th of July 2015 and obtained the most detailed images of Pluto and its moon until this moment. At the same time, observation obtained by the ground-based telescopes may also be helpful for the research of such distant system. Thereby, the Laboratory of observational astrometry of Pulkovo Observatory of RAS made a decision to reprocess observations obtained during last decade. More than 350 positional observations of Pluto-Charon system were carried out with the mirror astrograph ZA-320M at Pulkovo and Maksutov telescope MTM-500M near Kislovodsk. These observations were processed by means of software system APEX-II developed in Pulkovo observatory and numerical simulations were performed to calculate the differences between positions of photocenter and barycenter of Pluto-Charon system.

  1. First results of the Kourovka Planet Search: discovery of transiting exoplanet candidates in the first three target fields

    CERN Document Server

    Burdanov, Artem Y; Krushinsky, Vadim V; Popov, Alexander A; Sokov, Evgenii N; Sokova, Iraida A; Rusov, Sergei A; Lyashenko, Artem Yu; Ivanov, Kirill I; Moiseev, Alexei V; Rastegaev, Denis A; Dyachenko, Vladimir V; Balega, Yuri Yu; Baştürk, Özgür; Özavcı, Ibrahim; Puchalski, Damian; Marchini, Alessandro; Naves, Ramon; Shadick, Stan; Bretton, Marc

    2016-01-01

    We present the first results of our search for transiting exoplanet candidates as part of the Kourovka Planet Search (KPS) project. The primary objective of the project is to search for new hot Jupiters which transit their host stars, mainly in the Galactic plane, in the $R_c$ magnitude range of 11 to 14 mag. Our observations were performed with the telescope of the MASTER robotic network, installed at the Kourovka astronomical observatory of the Ural Federal University (Russia), and the Rowe-Ackermann Schmidt Astrograph, installed at the private Acton Sky Portal Observatory (USA). As test observations, we observed three celestial fields of size $2\\times2$ deg$^2$ during the period from 2012 to 2015. As a result, we discovered four transiting exoplanet candidates among the 39000 stars of the input catalogue. In this paper, we provide the description of the project and analyse additional photometric, spectral, and speckle interferometric observations of the discovered transiting exoplanet candidates. Three of ...

  2. Proper motions and CCD photometry of stars in the region of the open cluster NGC 6866

    Science.gov (United States)

    Frolov, V. N.; Ananjevskaja, Yu. K.; Gorshanov, D. L.; Polyakov, E. V.

    2010-05-01

    We present the results of our comprehensive study of the Galactic open star cluster NGC 6866. The positions of stars in the investigated region have been obtained with the “Fantasy” automatic measuring machine from 10 plates of the normal astrograph at the Pulkovo Astronomical Observatory. The size of the investigated field is 40' × 40', the limiting magnitude is B ˜ 16{·/ m }6, and the maximum epoch difference is 79 yr. For 1202 field stars, we have determined the relative proper motions with an rms error of 2.5 mas yr-1. Out of them, 423 stars may be considered cluster members with a probability P > 70% according to the astrometric criterion. Photometric diagrams have been used as an additional criterion. We have performed two-color BV CCD photometry of stars with the Pulkovo ZA-320M mirror astrograph. The U magnitudes from the literature have also been used to construct the two-color diagrams. A total of 267 stars have turned out to be members of NGC 6866 according to the two criteria. We present refined physical parameters of the cluster and its age estimate (5.6 × 108 yr). The cluster membership of red and blue giants, variable, double, and multiple stars is considered. We have found an almost complete coincidence of the positions of one of the stars in the region (a cluster nonmember) and a soft X-ray source in the ROSAT catalog. The “Fantasy” automatic measuring machine is described in the Appendix.

  3. Astrometry of Pluto from 1930-1951 observations: The Lampland plate collection

    International Nuclear Information System (INIS)

    We present a new analysis of 843 photographic plates of Pluto taken by Carl Lampland at Lowell Observatory from 1930–1951. This large collection of plates contains useful astrometric information that improves our knowledge of Pluto's orbit. This improvement provides critical support to the impending flyby of Pluto by New Horizons. New Horizons can do inbound navigation of the system to improve its targeting. This navigation is capable of nearly eliminating the sky-plane errors but can do little to constrain the time of closest approach. Thus the focus on this work was to better determine Pluto's heliocentric distance and to determine the uncertainty on that distance with a particular eye to eliminating systematic errors that might have been previously unrecognized. This work adds 596 new astrometric measurements based on the USNO CCD Astrograph Catalog 4. With the addition of these data the uncertainty of the estimated heliocentric position of Pluto in Developmental Ephemerides 432 (DE432) is at the level of 1000 km. This new analysis gives us more confidence that these estimations are accurate and are sufficient to support a successful flyby of Pluto by New Horizons.

  4. Astrometry of Pluto from 1930-1951 observations: The Lampland plate collection

    Energy Technology Data Exchange (ETDEWEB)

    Buie, Marc W. [Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302 (United States); Folkner, William M., E-mail: buie@boulder.swri.edu, E-mail: william.m.folkner@jpl.nasa.gov [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109-8099 (United States)

    2015-01-01

    We present a new analysis of 843 photographic plates of Pluto taken by Carl Lampland at Lowell Observatory from 1930–1951. This large collection of plates contains useful astrometric information that improves our knowledge of Pluto's orbit. This improvement provides critical support to the impending flyby of Pluto by New Horizons. New Horizons can do inbound navigation of the system to improve its targeting. This navigation is capable of nearly eliminating the sky-plane errors but can do little to constrain the time of closest approach. Thus the focus on this work was to better determine Pluto's heliocentric distance and to determine the uncertainty on that distance with a particular eye to eliminating systematic errors that might have been previously unrecognized. This work adds 596 new astrometric measurements based on the USNO CCD Astrograph Catalog 4. With the addition of these data the uncertainty of the estimated heliocentric position of Pluto in Developmental Ephemerides 432 (DE432) is at the level of 1000 km. This new analysis gives us more confidence that these estimations are accurate and are sufficient to support a successful flyby of Pluto by New Horizons.

  5. The astrometric Gaia-FUN-SSO observation campaign of 99 942 Apophis

    CERN Document Server

    Thuillot, W; Ivantsov, A; Desmars, J; Assafin, M; Eggl, S; Hestroffer, D; Rocher, P; Carry, B; David, P; Abe, L; Andreev, M; Arlot, J -E; Asami, A; Ayvasian, V; Baransky, A; Belcheva, M; Bendjoya, Ph; Bikmaev, I; Burkhonov, O A; Camci, U; Carbognani, A; Colas, F; Devyatkin, A V; Ehgamberdiev, Sh A; Enikova, P; Eyer, L; Galeev, A; Gerlach, E; Godunova, V; Golubaev, A V; Gorshanov, D L; Gumerov, R; Hashimoto, N; Helvaci, M; Ibryamov, S; Inasaridze, R Ya; Khamitov, I; Kostov, A; Kozhukhov, A M; Kozyryev, Y; Krugly, Yu N; Kryuchkovskiy, V; Kulichenko, N; Maigurova, N; Manilla-Robles, A; Martyusheva, A A; Molotov, I E; Nikolov, G; Nikolov, P; Nishiyama, K; Okumura, S; Palaversa, L; Parmonov, O; Peng, Q Y; Petrova, S N; Pinigin, G I; Pomazan, A; Rivet, J -P; Sakamoto, T; Sakhibullin, N; Sergeev, O; Sergeyev, A V; Shulga, O V; Suarez, O; Sybiryakova, Y; Takahashi, N; Tarady, V; Todd, M; Urakawa, S; Uysal, O; Vaduvescu, O; Vovk, V; Zhang, X -L

    2015-01-01

    Astrometric observations performed by the Gaia Follow-Up Network for Solar System Objects (Gaia-FUN-SSO) play a key role in ensuring that moving objects first detected by ESA's Gaia mission remain recoverable after their discovery. An observation campaign on the potentially hazardous asteroid (99 942) Apophis was conducted during the asteroid's latest period of visibility, from 12/21/2012 to 5/2/2013, to test the coordination and evaluate the overall performance of the Gaia-FUN-SSO . The 2732 high quality astrometric observations acquired during the Gaia-FUN-SSO campaign were reduced with the Platform for Reduction of Astronomical Images Automatically (PRAIA), using the USNO CCD Astrograph Catalogue 4 (UCAC4) as a reference. The astrometric reduction process and the precision of the newly obtained measurements are discussed. We compare the residuals of astrometric observations that we obtained using this reduction process to data sets that were individually reduced by observers and accepted by the Minor Plane...

  6. A search for new variable stars using digitized Moscow collection plates

    CERN Document Server

    Sokolovsky, Kirill; Kolesnikova, Daria; Lebedev, Alexandr; Samus, Nikolai; Sat, Lyudmila; Zubareva, Alexandra

    2014-01-01

    By digitizing astronomical photographic plates one may extract full information stored on them, something that could not be practically achieved with classical analogue methods. We are developing algorithms for variable objects search using digitized photographic images and apply them to 30cm (10x10 deg. field of view) plates obtained with the 40cm astrograph in 1940-90s and digitized with a flatbed scanner. Having more than 100 such plates per field, we conduct a census of high-amplitude (>0.3m) variable stars changing their brightness in the range 13

  7. Discovery of Japan’s Oldest Photographic Plates of a Starfield

    Science.gov (United States)

    Watanabe, Jun-ichi; Sasaki, Goro; Nakagiri, Masao; Ohshima, Norio

    2015-08-01

    The Public Outreach and Archive Office in NAOJ has been inspecting as many as 20,000 old photographic plates, which were found in a pile of cardboard cartons. In the course of their inspections, we have discovered 437 plates recorded from the end of the 19th century to the beginning of the 20th century. This was the first era in which observations were recorded using photographic plates in Japan.Most of the plates were obtained by using the Brashear astrograph at Azabubu in the 19th century. The oldest photographic plate was marked (delete ‘as’) No.13 and was recorded on March 5, 1899. We also found a number of historically important plates; among these are images of the first minor planet “TOKIO” that was detected in Japan and named after our country, and of a star 61 Cyg, with a large proper motion.We have long known that Tokyo Observatory of Tokyo Imperial University began its observations at Azabu. However, for many years, everyone believed that all the plates and observational instruments were lost in the chaos following the Great Kanto earthquake (1923) and in a fire that damaged Tokyo Observatory’s main building during the World War II, events that took place before and after the Observatory’s move to Mitaka. We made a catalogue of these plates and will present some statistics along with our effort for archives in our observatory.

  8. {\\Delta}{\\mu} Binaries among Stars with Large Proper Motions

    CERN Document Server

    Khovritchev, M Yu

    2016-01-01

    Based on observations performed with the Pulkovo normal astrograph in 2008-2015 and data from sky surveys (DSS, 2MASS, SDSS DR12, WISE), we have investigated the motions of 1308 stars with proper motions larger than 300 mas/yr down to magnitude 17. The main idea of our search for binary stars based on this material is reduced to comparing the quasi-mean (POSS2-POSS1; an epoch difference of $\\approx$50 yr) and quasi-instantaneous (2MASS, SDSS, WISE, Pulkovo; an epoch difference of $\\approx$10 yr) proper motions. If the difference is statistically significant compared to the proper motion errors, then the object may be considered as a {\\Delta}{\\mu}-binary candidate. One hundred and twenty one stars from among those included in the observational program satisfy this requirement. Additional confirmations of binarity for a number of stars have been obtained by comparing the calculated proper motions with the data from several programs of stellar trigonometric parallax determinations and by analyzing the asymmetry ...

  9. VizieR Online Data Catalog: Galilean satellites & Jupiter positions (Narizhnaya, 2015)

    Science.gov (United States)

    Narizhnaya, N. V.

    2016-03-01

    All observations were carried out with the Normal Astrograph (D/F=330mm/ 3467mm) at Pulkovo (code is 084). A S2C CCD camera was used as a detector (with a field of view of 18'x16' and a scale of 0.952"/pixel). The CCD_frames with object image were obtained by series including 5, 10, 50, 100 images, depending on exposures of 60, 30, 10 and 5 s, respectively. The IZMCCD software package developed by Izmailov I.S. (2005, http://iznccd.puldb.ru/ izmccdrus) was used in processing the CCD images. Astrometric reduction algorithm is based on Turner's method with using UCAC4 catalog as reference one. Ephemerides for comparison are given by web-server "Natural Satellites Ephemeride Server MULTI-SAT" developed by N.V. Emelyanov (http://lnfm1.sai.msu.ru/neb/nss/nssephmr.htm). Two catalogue are presented: 140 normal positions of Galilean satellites and 42 Jupiter positions. (2 data files).

  10. PIRATE: A Remotely-Operable Telescope Facility for Research and Education

    CERN Document Server

    Holmes, S; Haswell, C A; Burwitz, V; Lucas, R J; Rodriguez, J; Rolfe, S M; Rostron, J; Barker, J

    2011-01-01

    We introduce PIRATE, a new remotely-operable telescope facility for use in research and education, constructed from 'off-the-shelf' hardware, operated by The Open University. We focus on the PIRATE Mark 1 operational phase where PIRATE was equipped with a widely- used 0.35m Schmidt-Cassegrain system (now replaced with a 0.425m corrected Dall Kirkham astrograph). Situated at the Observatori Astronomic de Mallorca, PIRATE is currently used to follow up potential transiting extrasolar planet candidates produced by the SuperWASP North experiment, as well as to hunt for novae in M31 and other nearby galaxies. It is operated by a mixture of commercially available software and proprietary software developed at the Open University. We discuss problems associated with performing precision time series photometry when using a German Equatorial Mount, investigating the overall performance of such 'off-the-shelf' solutions in both research and teaching applications. We conclude that PIRATE is a cost-effective research fac...

  11. The astrometric Gaia-FUN-SSO observation campaign of 99942 Apophis

    Science.gov (United States)

    Thuillot, W.; Bancelin, D.; Ivantsov, A.; Desmars, J.; Assafin, M.; Eggl, S.; Hestroffer, D.; Rocher, P.; Carry, B.; David, P.; Abe, L.; Andreev, M.; Arlot, J.-E.; Asami, A.; Ayvasian, V.; Baransky, A.; Belcheva, M.; Bendjoya, Ph.; Bikmaev, I.; Burkhonov, O. A.; Camci, U.; Carbognani, A.; Colas, F.; Devyatkin, A. V.; Ehgamberdiev, Sh. A.; Enikova, P.; Eyer, L.; Galeev, A.; Gerlach, E.; Godunova, V.; Golubaev, A. V.; Gorshanov, D. L.; Gumerov, R.; Hashimoto, N.; Helvaci, M.; Ibryamov, S.; Inasaridze, R. Ya.; Khamitov, I.; Kostov, A.; Kozhukhov, A. M.; Kozyryev, Y.; Krugly, Yu N.; Kryuchkovskiy, V.; Kulichenko, N.; Maigurova, N.; Manilla-Robles, A.; Martyusheva, A. A.; Molotov, I. E.; Nikolov, G.; Nikolov, P.; Nishiyama, K.; Okumura, S.; Palaversa, L.; Parmonov, O.; Peng, Q. Y.; Petrova, S. N.; Pinigin, G. I.; Pomazan, A.; Rivet, J.-P.; Sakamoto, T.; Sakhibullin, N.; Sergeev, O.; Sergeyev, A. V.; Shulga, O. V.; Suarez, O.; Sybiryakova, Y.; Takahashi, N.; Tarady, V.; Todd, M.; Urakawa, S.; Uysal, O.; Vaduvescu, O.; Vovk, V.; Zhang, X.-L.

    2015-11-01

    Aims: Astrometric observations performed by the Gaia Follow-Up Network for Solar System Objects (Gaia-FUN-SSO) play a key role in ensuring that moving objects first detected by ESA's Gaia mission remain recoverable after their discovery. An observation campaign on the potentially hazardous asteroid (99 942) Apophis was conducted during the asteroid's latest period of visibility, from 12/21/2012 to 5/2/2013, to test the coordination and evaluate the overall performance of the Gaia-FUN-SSO . Methods: The 2732 high quality astrometric observations acquired during the Gaia-FUN-SSO campaign were reduced with the Platform for Reduction of Astronomical Images Automatically (PRAIA), using the USNO CCD Astrograph Catalogue 4 (UCAC4) as a reference. The astrometric reduction process and the precision of the newly obtained measurements are discussed. We compare the residuals of astrometric observations that we obtained using this reduction process to data sets that were individually reduced by observers and accepted by the Minor Planet Center. Results: We obtained 2103 previously unpublished astrometric positions and provide these to the scientific community. Using these data we show that our reduction of this astrometric campaign with a reliable stellar catalog substantially improves the quality of the astrometric results. We present evidence that the new data will help to reduce the orbit uncertainty of Apophis during its close approach in 2029. We show that uncertainties due to geolocations of observing stations, as well as rounding of astrometric data can introduce an unnecessary degradation in the quality of the resulting astrometric positions. Finally, we discuss the impact of our campaign reduction on the recovery process of newly discovered asteroids. Full Table 3 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/583/A59

  12. Investigation of the open star cluster NGC 6800

    Science.gov (United States)

    Ananjevskaja, Yu. K.; Frolov, V. N.; Polyakov, E. V.

    2015-07-01

    The results of a comprehensive study of the Galactic open cluster NGC 6800 are presented. The positions of stars to a limiting magnitude B ≃ 16{./ m }5 in an 80' × 80' field centered at the cluster were measured on eight plates from the Pulkovo normal astrograph with a maximum epoch difference of 57 years. The measurements were performed with the Pulkovo "Fantasy" automated measuring system. The corresponding field from the 2MASS catalogue was used as an additional plate. As a result, the relative proper motions of stars were obtained with a root-mean-square error of 3.0 mas yr-1. A catalogue of BV and JHK magnitudes for objects in the investigated region was compiled from available published resources. The astrometric selection of cluster members was made by the maximum likelihood method. An individual cluster membership probability of a star P ≥ 60% served as the first selection criterion. The position of a star on the photometric color-magnitude ( V ~ B - V, J ~ J - K s ) diagrams was considered as the second selection criterion. On the basis of these criteria, it was established that 109 stars are members of NGC 6800, These data were used to refine the physical parameters of the cluster: the mean reddening E( B - V) = 0 m . 40, the true distance modulus ( V - M V )0 = 10{./ m }05, and the cluster age ~250 Myr. The luminosity and mass functions were constructed. The position of the center of the cluster NGC 6800 was improved: α = 19h27m11{./s}2 and δ = +25°07'24〃(2000). The catalogue of relative proper motions for stars in the field is available in electronic form only.

  13. Max Wolf's Discovery of Near-Earth Asteroid 887 Alinda

    Science.gov (United States)

    Connors, Martin; Mandel, Holger; Demleitner, Markus; Heidelberg Digitized Astronomical Plates Project

    2016-01-01

    Max Wolf, director of the Heidelberg Observatory (Landessternwarte Königsstuhl), was the most prodigious discoverer of asteroids in the early twentieth century. He is now best known for the discovery of the Trojan asteroids associated with Jupiter in 1906, but was a pioneer in the application of photographic techniques to astronomy, particularly for conducting asteroid surveys. His attention to detail and perseverance also led to the discovery of the near-Earth asteroid 887 Alinda, which is the eponym of an orbital class in 3:1 resonance with Jupiter. Alinda class contains several potentially hazardous asteroids, and has been particularly instructive in development of theories of eccentricity increase for resonant asteroids. Alinda was discovered on January 3, 1918, on the very edge of one of two plates taken with the 40 cm aperture Bruce double astrograph. The inability to reduce a long trail going off the plate meant that only one month later could the object again be found with the Bruce telescope, and later observed with the follow-up instrument, the 72 cm aperture Waltz reflector. In what Wolf referred to as "the greatest embarrassment of my life", reflector observations had him conclude that Alinda had a satellite. At a time when plates had to be exposed for several hours, laboriously developed and analyzed, and in the case of high eccentricity objects like Alinda, predicted with inadequate theories, Wolf's persistence allowed it never to be lost. Despite this, its essential resonant nature was not determined until 1969, despite the pioneering work by Brown (1911) on resonance in the asteroid belt and the knowledge dating to the late nineteenth century work of Kirkwood that commensurabilities were important in its structure. The majority of Wolf's plates are available as online scans through the Heidelberg Digitized Astronomical Plates project of the German Astrophysical Virtual Observatory, but the Alinda discovery plate, which was broken, was scanned

  14. CSU's MWV Observatory: A Facility for Research, Education and Outreach

    Science.gov (United States)

    Hood, John; Carpenter, N. D.; McCarty, C. B.; Samford, J. H.; Johnson, M.; Puckett, A. W.; Williams, R. N.; Cruzen, S. T.

    2014-01-01

    The Mead Westvaco Observatory (MWVO), located in Columbus State University's Coca-Cola Space Science Center, is dedicated to education and research in astronomy through hands-on engagement and public participation. The MWVO has recently received funding to upgrade from a 16-inch Meade LX-200 telescope to a PlaneWave CDK 24-inch Corrected Dall-Kirkham Astrograph telescope. This and other technological upgrades will allow this observatory to stream live webcasts for astronomical events, allowing a worldwide public audience to become a part of the growing astronomical community. This poster will explain the upgrades that are currently in progress as well as the results from the current calibrations. The goal of these upgrades is to provide facilities capable of both research-class projects and widespread use in education and public outreach. We will present our initial calibration and tests of the observatory equipment, as well as its use in webcasts of astronomical events, in solar observing through the use of specialized piggy-backed telescopes, and in research into such topics as asteroids, planetary and nebula imaging. We will describe a pilot research project on asteroid orbit refinement and light curves, to be carried out by Columbus State University students. We will also outline many of the K-12 educational and public outreach activities we have designed for these facilities. Support and funding for the acquisition and installation of the new PlaneWave CDK 24 has been provided by the International Museum and Library Services via the Museums for America Award.

  15. UCAC4 nearby star survey: A search for our stellar neighbors

    Energy Technology Data Exchange (ETDEWEB)

    Finch, Charlie T.; Zacharias, Norbert [U.S. Naval Observatory, Washington, DC 20392–5420 (United States); Subasavage, John P. [U.S. Naval Observatory, Flagstaff, AZ 86005–8521 (United States); Henry, Todd J. [RECONS Institute, Chambersburg, PA 17201 (United States); Riedel, Adric R., E-mail: finch@usno.navy.mil [Hunter College, New York, NY 10065 (United States)

    2014-12-01

    We use data from the U.S. Naval Observatory fourth CCD Astrograph Catalog (UCAC4) in combination with photometry from the AAVSO Photometric All-Sky Survey and Two Micron All-Sky Survey to identify stars within 25 pc of the Sun. A sample of nearby stars with accurate trigonometric parallaxes from the Research Consortium On Nearby Stars is used to generate a set of 16 new photometric color–M{sub K{sub s}} relations that provide distance estimates with uncertainties of 15%. This work expands the available suites of well-calibrated photometric distance relations that can be used to identify nearby stellar systems. The distance relations are used with quality cuts to extract an initial sample of stars from the UCAC4 estimated to be within 25 pc. Color, proper motion, and existing literature sources are then used to obtain a clean sample of red dwarfs, while limiting the amount of contamination from background giants, resulting in a sample of 1761 candidate nearby stars within 25 pc. Of these, 339 are new discoveries with no previously known published parallax or distance estimate, primarily with proper motions less than 0.2 arcsec yr{sup −1}. Five stars are estimated to be within 10 pc, with the nearest, TYC 3980 1081 1, with V=10.50 estimated to be at 5.9 pc. That several hundred new stars have been revealed so close to the Sun illustrates once again that there is considerable work yet to be done to map the solar neighborhood and that additional nearby stars are likely still to be discovered.

  16. Progressive Research and Outreach at the WestRock Observatory

    Science.gov (United States)

    Brown, Johnny Eugene; Lantz Caughey, Austin; O'Keeffe, Brendon; Johnson, Michael; Murphy Williams, Rosa Nina

    2016-01-01

    The WestRock Observatory (WRO), located in Columbus State University's Coca-Cola Space Science Center (CCSSC), is dedicated to education and research in astronomy through hands-on engagement and public participation. The WRO has recently received funding to upgrade the PlaneWave CDK 24-inch Corrected Dall-Kirkham Astrograph telescope. Recent additions to the telescope include an all-new Apogee Alta F16 CCD camera complete with a filter wheel (with narrowband and broadband filters) and a Minor Planet Center Observatory Code (W22). These new upgrades have allowed Astrophysics students to conduct unique research ranging from high precision minor planet astrometry, to broad- and narrow-band imaging of nebulae, to light curve analysis for variable star photometry. These new endeavours, in conjunction with an existing suite of Solar telescopes, gives the WRO the ability to live-stream solar and night-time observing. These streams are available both online and through interactive displays at the CCSSC making the WRO an educational outreach program for a worldwide public audience and a growing astronomical community.Current funding is allowing students to get even more research experience than previously attainable further enabling the expansion of our publicly available gallery of nebula and galaxy images. Support and funding for the acquirement,installation, and upgrading of the new PlaneWave CDK24 has been provided by the International Museum and Library Services via the Museums for America Award Additionally, individual NASA Space Grant Scholarships have helped to secure a number of student interns partially responsible for recent improvements.

  17. PARALLAXES OF SOUTHERN EXTREMELY COOL OBJECTS. I. TARGETS, PROPER MOTIONS, AND FIRST RESULTS

    International Nuclear Information System (INIS)

    We present results from the PARallaxes of Southern Extremely Cool objects (PARSEC) program, an observational program begun in 2007 April to determine parallaxes for 122 L and 28 T southern hemisphere dwarfs using the Wide Field Imager on the ESO 2.2 m telescope. The results presented here include parallaxes of 10 targets from observations over 18 months and a first version proper motion catalog. The proper motions were obtained by combining PARSEC observations astrometrically reduced with respect to the Second US Naval Observatory CCD Astrograph Catalog, and the Two Micron All Sky Survey Point Source Catalog. The resulting median proper motion precision is 5 mas yr-1 for 195,700 sources. The 140 0.3 deg2 fields sample the southern hemisphere in an unbiased fashion with the exception of the galactic plane due to the small number of targets in that region. The proper motion distributions are shown to be statistically well behaved. External comparisons are also fully consistent. We will continue to update this catalog until the end of the program, and we plan to improve it including also observations from the GSC2.3 database. We present preliminary parallaxes with a 4.2 mas median precision for 10 brown dwarfs, two of which are within 10 pc. These increase the present number of L dwarfs by 20% with published parallaxes. Of the 10 targets, seven have been previously discussed in the literature: two were thought to be binary, but the PARSEC observations show them to be single; one has been confirmed as a binary companion and another has been found to be part of a binary system, both of which will make good benchmark systems. These results confirm that the foreseen precision of PARSEC can be achieved and that the large field of view will allow us to identify wide binary systems. Observations for the PARSEC program will end in early 2011 providing three to four years of coverage for all targets. The main expected outputs are: more than a 100% increase in the number of L

  18. Automatic detection of asteroids and meteoroids --- a wide-field survey

    Science.gov (United States)

    Vereš, P.; Tóth, J.; Jedicke, R.; Tonry, J.; Denneau, L.; Wainscoat, R.; Kornoš, L.; Šilha, J.

    2014-07-01

    The small Near-Earth Asteroids (NEAs) represent a potential risk but also an easily accessible space resource for future robotic or human in-situ space exploration or commercial activities. However, the population of 1--300 m NEAs is not well understood in terms of size- frequency and orbital distribution. NEAs with diameters below 200 m tend to have much faster spin rates than large objects and they are believed to be monolithic and not rubble-pile like their large counterparts. Moreover, the current surveys do not systematically search for the small NEAs that are mostly overlooked. We propose a low- cost robotic optical survey (ADAM-WFS) aimed at small NEAs based on four state-of-the-art telescopes having extremely wide fields of view. The four Houghton-Terebizh 30-cm astrographs (Fig. left) with 4096×4096 -pixel CCD cameras will acquire 96 square degrees in one exposure with the plate scale of 4.4 arcsec/pixel. In 30 seconds, the system will be able to reach +17.5 mag in unfiltered mode. The survey will be operated on semi-automatic basis, covering the entire night sky three times per night and optimized toward fast moving targets recognition. The advantage of the proposed system is the usage of existing of-the-shelf components and software for the image processing and object identification and linking (Denneau et al., 2013). The one-year simulation of the survey (Fig. right) at the testing location at AGO Modra observatory in Slovakia revealed that we will detect 60--240 NEAs between 1--300 m that get closer than 10 lunar distances from the Earth. The number of detections will rise by a factor of 1.5--2 in case the survey is placed at a superb observing location such as Canary Islands. The survey will also serve as an impact warning system for imminent impactors. Our simulation showed that we have a 20 % chance of finding a 50-m NEA on a direct impact orbit. The survey will provide multiple byproducts from the all-sky scans, such as comet discoveries, sparse

  19. Reduction of EAO Positional Observations Database

    Science.gov (United States)

    Nefedyev, Yuri; Andreev, Alexey; Demina, Natalya; Churkin, Konstantin

    2016-07-01

    There is a large data bank of positional observations of Solar System bodies at Engelhadt Astronomical Observatory (EAO). The positional observations include the major planets, except Jupiter. Modern technologies replace classical methods of observations in astronomy and in astrometry as well. At the same time many positional observations have been gathered at astronomical observatories. So taking into account that observations of the past epochs have presenteda great value for astronomy and as times goes by their importance is growing it is obvious that positional astrometry will not lose its practical importance. This was noted in B3 XXIV IAU resolution by the General Assembly. The results of reduction of solar system bodies observations were published mainly in Proceeding of EAO and Transactions of Kazan City Astronomical Observatory. Earlier there have been made about three thousand observations at EAO and Zelenchuk station with the Zeiss telescope (D=400mm, f=2000mm), AFR-18 (photo visual, D=200, f=2000), refractor (D=400mm, f=3450mm), Meniscus camera (D=340mm, f=1200mm), Schmidt camera (D=350mm, f=2000mm). The major planets except Pluto and Neptune were observed with a special cassette chamber equipped with a rotating disk which had an open sector to reduce the brightness of the planets. The dimension of the sector was chosen accordingto the brightness of the planets. The disk was placed in the centre of the astrograph's field. The stars' true brightness was preserved. A large number of catalogues were compiled by the end of the 20th century. We used Tycho-2 catalogue for reducing our observations. As it is known the catalogue Tycho-2 (Tycho-2 catalogue, 2000) includes 2539913 stars. The stars' proper motions given in the catalogue were obtained by comparing positions from Tycho-2 with positions from the Astrographic Catalogue. Therefore they are considered to be highly accurate. The accuracy of stellar positions in Tycho-2 is about 60 mas and the accuracy of

  20. Obituary: Frank K. Edmondson (1912-2008)

    Science.gov (United States)

    Pilachowski, Catherine A.; Olson, Margaret K. Edmondson; Edmondson, Frank K., Jr.

    2009-12-01

    Observatory in Brooklyn, IN, (a gift from Dr. Goethe Link, a noted Indianapolis physician and avid amateur astronomer), established a graduate program in astronomy, and enlarged the Department of Astronomy from two faculty members to eight. In one of his favorite stories, Edmondson bet Professor Cogshall a chocolate ice cream cone that President Herman B Wells would fund a new position for the Department, knowing full well that Wells had already agreed. Frank retired from IU in 1983. When many asteroids were lost during World War II, Frank and his colleague James Cuffey established the Indiana University Asteroid Program. Frank is credited with determining the orbits of 119 asteroids from 7000 photographic plates taken with a 10" astrographic telescope at the Goethe Link Observatory. Frank selected names for each of these asteroids, honoring IU Presidents, prominent scholars, and important Hoosier and astronomical landmarks. Asteroid 4300 Marg Edmondson he named for his wife Margaret. During his years as a faculty member at Indiana University, Frank advised Dr. Alfred Kinsey on statistical techniques for his pioneering studies of human sexuality, and also shared with Kinsey an abiding interest in classical music. The music and the programs at the IU School of Music brought great joy to Frank over his career at IU. His memory for programs he had heard in the past was phenomenal. Frank is best known in Bloomington for his remarkable skill as an educator. He loved teaching. He taught elementary astronomy to literally thousands of students, often taking advantage of his knowledge of music to introduce astronomical topics with appropriate musical selections. His popular, award-winning, televised astronomy course was broadcast to students throughout the state and is widely remembered even today. Following in the tradition of IU's legendary President Herman B Wells, whom he greatly admired, Frank devoted his career to service. In 1957 Indiana University became one of the seven