DOCSLIB.ORG

The Minor Planet Bulletin

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Minor Planet Bulletin THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 43, NUMBER 4, A.D. 2016 OCTOBER-DECEMBER 283. LIGHTCURVES FOR TWO NEAR-EARTH-ASTEROIDS BY Observatory Telescope (meters) CCD ASTEROIDS OBSERVERS (OBAS) – MPPD: C.A.A.T. 0.45 DK SBIG STL-11002 2016 APRIL - MAY Zonalunar 0.20 NW QHY6 Vicente Mas Martinez, Gonzalo Fornas Silva, Angel Flores Vallbona 0.25 SCT SBIG ST7-XME Martinez, CAAT - Centro Astronómico del Alto Turia, SPAIN TRZ 0.20 R-C QHY8 [email protected] Elche 0.25 DK SBIG ST8-XME Alfonso Carreño Garcerán Oropesa 0.20 SCT Atik 16I Zonalunar Observatory,Valencia, SPAIN Bétera 0.23 SCT Atik 314L+ Serra Observatory 0.25 NW Atik 414L+ Enrique Arce Mansego Table I. List of instruments used for the observations. SCT is Vallbona Observatory, Valencia, SPAIN Schmidt-Cassegrain. R-C is Ritchey-Chrétien. DK is Dall-Kirkham. NW is Newton. Pedro Brines Rodriguez TRZ Observatory, Valencia, SPAIN Table I shows the equipment at the observatories that participated in this work. We concentrated on asteroids with no reported period Juan Lozano de Haro and those where the reported period was poorly established and Elche Observatory, Alicante, SPAIN needed confirmation. All the targets were selected from the Collaborative Asteroid Lightcurve (CALL) website at Alvaro Fornas Silva (http://www.minorplanet.info/call.html) and Minor Planet Center Oropesa Observatory, Castellón, SPAIN (http://www.minorplanet.net) Onofre Rodrigo Chiner Images were measured using MPO Canopus (Bdw Publishing) Bétera Observatory, Valencia, SPAIN with a differential photometry technique. David Herrero Porta (35396) 1997 XF11 was discovered in 1997 December (Sugie et Serra Observatory, Valencia, SPAIN al., 1997) and remained fainter than V ~ 18 until its predicted (Received: 2016 Jun 14) brightening to V = 13.4 in mid-2002. It won’t reach this brightness again until 2028. We report on the results of photometric analysis of two In 1998 March, then-unnumbered 1997 XF11 made headlines in near-Earth asteroids (NEA) by Asteroids Observers the popular media after some interpretations of preliminary (OBAS). This work is part of the Minor Planet calculations of its orbit suggested that it could collide with Earth in Photometric Database (MPPD) project initiated by a 2028. Disagreement among researchers about how close it was group of Spanish amateur astronomers. We have likely to pass to Earth and how to characterize the uncertainties managed to obtain a number of accurate and complete involved Marsden (1999), Chodas and Yeomans (1999), Milani lightcurves as well as some additional incomplete and Valsecchi (1999) Yeomans et al. (1998), Helin et al. (1998), lightcurves to help analysis at future oppositions. and Scotti and Shelus (1998) and how best to communicate such information to the media. This led to confusion and sensationalism. The incident raised important issues about impact risk assessment In this paper we publish the results of lightcurve analysis for two and how best to balance the interests of scientific research with near-Earth asteroids observed under the Minor Planet Photometric those of the public’s right to know. Database project (http://www.minorplanet.es). The data and results were made possible thanks to the collaboration of the The OBAS group obtained images of (35396) 1997 XF11 on three Astronomical Center Alto Turia (CAAT) Observatory located in nights 2016 April, when the sky motion was 3 arcsec/min and so Aras de los Olmos and operated by members of the Valencia exposures were no more than 60 seconds. Three OBAS group Astronomy Association (AVA) (http://www.astroava.org). observatories worked together to obtain these results, especially the team of the Astronomical Center Alto Turia (CAAT). From our Minor Planet Bulletin 43 (2016) Available on line http://www.minorplanet.info/mpbdownloads.html 284 data, we derived a rotation period of 3.252 ± 0.002 h and Marsden. B.G. (1999). “Asteroid 1997 XF11 Could Collide with amplitude of 0.60 mag. Earth.” AAS/Division of Dynamical Astronomy Meeting. Scotti. I.V. Shelus, P.J. (1998). “1997 XF11”. IAUC 6837. Sugie, A., Scotti, J.V., Kojima, T., Williams, G.V. (1997). “1997 XF11.” Minor Planet Electronic Circular (MPEC) 1997-Y11. Yeomans, D., Chodas, P., Muinonen, K., Bowell, E., Shoemaker, E.M., Williams, G.V., Marsden, B.G. (1998). “1997 XF11”. IAUC 6879. THE ROTATION PERIOD OF ASTEROIDS 4931 TOMSK AND 5232 JORDAENS Russell I. Durkee, Shed of Science Observatory Minneapolis, MN 55410, USA [email protected] Jessie L. Houghton, Carmen L. Eggleston (154555) 2003 HA was discovered in 2003 April by LINEAR. The Minnetonka High School Minnetonka, MN 55345, USA OBAS group obtained images on three nights in 2016 May. At the time, the asteroid’s sky motion was 4 arcsec/min, which limited (Received: 2016 Jun 25) exposures to 60 seconds or less. From our data we derive a rotation period of 5.171 ± 0.004 hours and amplitude of 0.36 magnitudes. Three OBAS group observatories worked together to obtain these CCD observations of two main-belt asteroids were made results, especially the team of the Astronomical Center Alto Turia in 2016 March and May. Analysis of the data for 4931 (CAAT). Tomsk indicates a synodic period of P = 7.02 ± 0.01 h, A = 0.46 ± 0.10 mag. For 5232 Jordaens, the analysis indicates a synodic period of P = 10.58 ± 0.01 h, A = 0.73 ± 0.15 mag. CCD photometry observations of the main-belt asteroids 4931 Tomsk and 5232 Jordaens were made in 2016. At the Shed of Science Observatory, a 0.35-m Schmidt Cassegrain (SCT) working at f/8.5 and SBIG ST-10XE CCD camera were used. The resulting plate scale was 0.94 acrsec/pixel. Exposures were made through a Celestron UHC LPR filter. The R-COP telescope at Perth Observatory used a 0.35-m Schmidt Cassegrain (SCT) working at f/6.0 and SBIG ST-10XME camera. The plate scale was 0.67 arcsec/pixel. The exposures were unfiltered. All images were dark and flat-field corrected. Images were measured using MPO Canopus (Bdw Publishing) with a differential photometry technique. The MPO Canopus Comp Star Selector was used to link sessions. The data were light-time corrected. Period analysis was also done with MPO Canopus, Acknowledgements incorporating the Fourier analysis algorithm developed by Harris We would like to express our gratitude to Brian Warner for (Harris et al., 1989). supporting the CALL web site and his suggestions made to the 4931 Tomsk was observed over two nights in 2016 March from OBAS group. the Shed of Science Observatory. The third night used the R-COP References telescope at the Bickley Observatory in Perth, Australia, through the Skynet observatory network. Conditions did not allow more Chodas, P.W., Yeomans, D.K. (1999). “Could Asteroid 1997 XF11 than three nights of observations. As a result, there are possible Collide with Earth After 2028?” AAS/Division of Dynamical solutions other than the period given here. Additional observations Astronomy Meeting. of this object are required to refine the period. Helin, E.F., Lawrence, K.I., Roman, B., Williams, G.V., Yeomans, D, K., Chodas, P., Muinonen, K., Bowell, E. (1998). “l997 XF11”. IAUC 6839. Minor Planet Bulletin 43 (2016) 285 LIGHTCURVE ANALYSIS OF NEA (331471) 1984 QY1: A TUMBLING ASTEROID Brian D. Warner Center for Solar System Studies – Palmer Divide Station 446 Sycamore Ave. Eaton, CO 80615 USA [email protected] Vladimir Benishek Belgrade Astronomical Observatory Volgina 7, 11060 Belgrade 38, SERBIA (Received: 9 July 2016) Analysis of CCD photometric observations of the near- Earth asteroid (331471) 1984 QY1 show that it is likely in non-principal axis rotation (NPAR), or tumbling. A single period analysis found a dominant period of 45.5 ± 5232 Jordaens was observed over three nights in 2016 May from 0.5 h, but the true periods of rotation and precession the Shed of Science Observatory. Conditions were not suitable for could not be determined. more than three nights of observations before the object became too dim. Additional observations of this object are needed to refine the period. CCD photometric observations were made of the near-Earth asteroid (331471) 1984 QY1 from 2016 June 6-20. Table I lists the equipment and dates of observation for each observer. Obs Telescope 2016 June Warner 0.35-m 6-10,12,14,15-17,20 Benishek 0.35-m 8,9,14,17 Table I. List of telescopes used and dates of observations for each observer. In all, more than 2000 observations were made using a clear or no filter to obtain maximum SNR. Exposures ranged from 60 to 90 seconds, while the asteroid faded from V ~ 15.5 to 16.3. Longer exposures were not possible because of the asteroid’s sky motion, which started at about 9 arcsec/min and decreased to 4 arcsec/min. Each observer used MPO Canopus to process the raw images with dark and flat field frames and then to perform differential photometry. Because of slight trailing, elliptical apertures were used for the asteroid, the major axis being kept parallel to the asteroid’s motion. Acknowledgements Up to five solar colored comparison stars were used each night to help minimize errors due to color differences between the asteroid Partial funding for work at the Shed of Science Observatory is and comparison stars. V magnitudes from the MPOSC3 catalog provided by 2009 and 2010 Shoemaker NEO Grants from the supplied with MPO Canopus were used for the comparison Planetary Society. Access to the R-COP telescope at the Perth stars. This catalog is based on the 2MASS catalog Observatory was made possible thanks to R.
Load more

Recommended publications
  • The Minor Planet Bulletin
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin.
    [Show full text]
  • Occultation Newsletter Volume 8, Number 4
    Volume 12, Number 1 January 2005 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Article Page The Largest Members Of Our Solar System – 2005 . 4 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . .11 IOTA European Section (IOTA/ES) . .11 IOTA on the World Wide Web. Back Cover ON THE COVER: Steve Preston posted a prediction for the occultation of a 10.8-magnitude star in Orion, about 3° from Betelgeuse, by the asteroid (238) Hypatia, which had an expected diameter of 148 km. The predicted path passed over the San Francisco Bay area, and that turned out to be quite accurate, with only a small shift towards the north, enough to leave Richard Nolthenius, observing visually from the coast northwest of Santa Cruz, to have a miss. But farther north, three other observers video recorded the occultation from their homes, and they were fortuitously located to define three well- spaced chords across the asteroid to accurately measure its shape and location relative to the star, as shown in the figure. The dashed lines show the axes of the fitted ellipse, produced by Dave Herald’s WinOccult program. This demonstrates the good results that can be obtained by a few dedicated observers with a relatively faint star; a bright star and/or many observers are not always necessary to obtain solid useful observations. – David Dunham Publication Date for this issue: July 2005 Please note: The date shown on the cover is for subscription purposes only and does not reflect the actual publication date.
    [Show full text]
  • Ty996i the Astronomical Journal Volume 71, Number
    coPC THE ASTRONOMICAL JOURNAL VOLUME 71, NUMBER 6 AUGUST 1966 TY996I Observations of Comets, Minor Planets, and Satellites Elizabeth Roemer* and Richard E. Lloyd U. S. Naval Observatory, Flagstaff Station, Arizona (Received 10 May 1966) Accurate positions and descriptive notes are presented for 38 comets, 33 minor planets, 5 faint natural satellites, and Pluto, for which astrometric reduction of the series of Flagstaff observations has been completed. THE 1022 positions and descriptive notes presented reference star positions; therefore, she bears responsi- here supplement those given by Roemer (1965), bility for the accuracy of the results given here. who also described the program, the equipment used, Coma diameters and tail dimensions given in the and the procedures of observation and of reduction. Notes to Table I refer to the exposures taken for In this paper as in the earlier one, the participation astrometric purposes unless otherwise stated. In of those who shared in critical phases of the work is general, longer exposures show more extensive head and indicated in the Obs/Meas column of Table I according tail structure. to the following letters: For brighter comets the minimum exposure is determined by the necessity of recording measurable R=Elizabeth Roemer. images of 12th-13th magnitude reference stars. On Part-time assistants under contract Nonr-3342(00) such exposures the position of the nuclear condensation with Lowell Observatory: may be more or less obscured by the overexposed coma and be correspondingly difficult and uncertain to L = Richard E. Lloyd, measure. T = Maryanna Thomas, A colon has been used to indicate greater than normal S = Marjorie K.
    [Show full text]
  • On the Accuracy of Restricted Three-Body Models for the Trojan Motion
    DISCRETE AND CONTINUOUS Website: http://AIMsciences.org DYNAMICAL SYSTEMS Volume 11, Number 4, December 2004 pp. 843{854 ON THE ACCURACY OF RESTRICTED THREE-BODY MODELS FOR THE TROJAN MOTION Frederic Gabern1, Angel` Jorba1 and Philippe Robutel2 Departament de Matem`aticaAplicada i An`alisi Universitat de Barcelona Gran Via 585, 08007 Barcelona, Spain1 Astronomie et Syst`emesDynamiques IMCCE-Observatoire de Paris 77 Av. Denfert-Rochereau, 75014 Paris, France2 Abstract. In this note we compare the frequencies of the motion of the Trojan asteroids in the Restricted Three-Body Problem (RTBP), the Elliptic Restricted Three-Body Problem (ERTBP) and the Outer Solar System (OSS) model. The RTBP and ERTBP are well-known academic models for the motion of these asteroids, and the OSS is the standard model used for realistic simulations. Our results are based on a systematic frequency analysis of the motion of these asteroids. The main conclusion is that both the RTBP and ERTBP are not very accurate models for the long-term dynamics, although the level of accuracy strongly depends on the selected asteroid. 1. Introduction. The Restricted Three-Body Problem models the motion of a particle under the gravitational attraction of two point masses following a (Keple- rian) solution of the two-body problem (a general reference is [17]). The goal of this note is to discuss the degree of accuracy of such a model to study the real motion of an asteroid moving near the Lagrangian points of the Sun-Jupiter system. To this end, we have considered two restricted three-body problems, namely: i) the Circular RTBP, in which Sun and Jupiter describe a circular orbit around their centre of mass, and ii) the Elliptic RTBP, in which Sun and Jupiter move on an elliptic orbit.
    [Show full text]
  • Perturbations in the Motion of the Quasicomplanar Minor Planets For
    Publications of the Department of Astronom} - Beograd, N2 ID, 1980 UDC 523.24; 521.1/3 osp PERTURBATIONS IN THE MOTION OF THE QUASICOMPLANAR MI­ NOR PLANETS FOR THE CASE PROXIMITIES ARE UNDER 10000 KM J. Lazovic and M. Kuzmanoski Institute of Astronomy, Faculty of Sciences, Beograd Received January 30, 1980 Summary. Mutual gravitational action during proximities of 12 quasicomplanar minor pla­ nets pairs have been investigated, whose minimum distances were under 10000 km. In five of the pairs perturbations of several orbital elements have been stated, whose amounts are detectable by observations from the Earth. J. Lazovic, M. Kuzmanoski, POREMECAJI ELEMENATA KRETANJA KVAZIKOM­ PLANARNIH MALIH PLANETA U PROKSIMITETIMA NJIHOVIH PUTANJA SA DA­ LJINAMA MANJIM OD 10000 KM - Ispitali smo medusobna gravitaciona de;stva pri proksi­ mitetima 12 parova kvazikomplanarnih malih planeta sa minimalnim daljinama ispod 10000 km. Kod pet parova nadeni su poremecaji u vi~e putanjskih elemenata, ~iji bi se iznosi mogli ustano­ viti posmatranjima sa Zemlje. Earlier we have found out 13 quasicomplanar minor planets pairs (the angle I between their orbital planes less than O~500), whose minimum mutual distances (pmin) were less than 10000 km (Lazovic, Kuzmanoski, 1978). The shortest pro­ ximity distance of only 600 km among these pairs has been stated with minor planet pair (215) Oenone and 1851 == 1950 VA. The corresponding perturbation effects in this pair have been calculated (Lazovic, Kuzmanoski, 1979a). This motivated us to investigate the mutual perturbing actions in the 12 remaining minor planets pairs for the case they found themselves within the proximities of their correspon­ ding orbits.
    [Show full text]
  • Astrocladistics of the Jovian Trojan Swarms
    MNRAS 000,1–26 (2020) Preprint 23 March 2021 Compiled using MNRAS LATEX style file v3.0 Astrocladistics of the Jovian Trojan Swarms Timothy R. Holt,1,2¢ Jonathan Horner,1 David Nesvorný,2 Rachel King,1 Marcel Popescu,3 Brad D. Carter,1 and Christopher C. E. Tylor,1 1Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD, Australia 2Department of Space Studies, Southwest Research Institute, Boulder, CO. USA. 3Astronomical Institute of the Romanian Academy, Bucharest, Romania. Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The Jovian Trojans are two swarms of small objects that share Jupiter’s orbit, clustered around the leading and trailing Lagrange points, L4 and L5. In this work, we investigate the Jovian Trojan population using the technique of astrocladistics, an adaptation of the ‘tree of life’ approach used in biology. We combine colour data from WISE, SDSS, Gaia DR2 and MOVIS surveys with knowledge of the physical and orbital characteristics of the Trojans, to generate a classification tree composed of clans with distinctive characteristics. We identify 48 clans, indicating groups of objects that possibly share a common origin. Amongst these are several that contain members of the known collisional families, though our work identifies subtleties in that classification that bear future investigation. Our clans are often broken into subclans, and most can be grouped into 10 superclans, reflecting the hierarchical nature of the population. Outcomes from this project include the identification of several high priority objects for additional observations and as well as providing context for the objects to be visited by the forthcoming Lucy mission.
    [Show full text]
  • An Anisotropic Distribution of Spin Vectors in Asteroid Families
    Astronomy & Astrophysics manuscript no. families c ESO 2018 August 25, 2018 An anisotropic distribution of spin vectors in asteroid families J. Hanuš1∗, M. Brož1, J. Durechˇ 1, B. D. Warner2, J. Brinsfield3, R. Durkee4, D. Higgins5,R.A.Koff6, J. Oey7, F. Pilcher8, R. Stephens9, L. P. Strabla10, Q. Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, Ngunnawal ACT 2913, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), Italy Received x-x-2013 / Accepted x-x-2013 ABSTRACT Context. Current amount of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study not only the spin-vector properties of the whole population of MBAs, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the HCM method as members of ten collisional families, among them are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes.
    [Show full text]
  • Nd AAS Meeting Abstracts
    nd AAS Meeting Abstracts 101 – Kavli Foundation Lectureship: The Outreach Kepler Mission: Exoplanets and Astrophysics Search for Habitable Worlds 200 – SPD Harvey Prize Lecture: Modeling 301 – Bridging Laboratory and Astrophysics: 102 – Bridging Laboratory and Astrophysics: Solar Eruptions: Where Do We Stand? Planetary Atoms 201 – Astronomy Education & Public 302 – Extrasolar Planets & Tools 103 – Cosmology and Associated Topics Outreach 303 – Outer Limits of the Milky Way III: 104 – University of Arizona Astronomy Club 202 – Bridging Laboratory and Astrophysics: Mapping Galactic Structure in Stars and Dust 105 – WIYN Observatory - Building on the Dust and Ices 304 – Stars, Cool Dwarfs, and Brown Dwarfs Past, Looking to the Future: Groundbreaking 203 – Outer Limits of the Milky Way I: 305 – Recent Advances in Our Understanding Science and Education Overview and Theories of Galactic Structure of Star Formation 106 – SPD Hale Prize Lecture: Twisting and 204 – WIYN Observatory - Building on the 308 – Bridging Laboratory and Astrophysics: Writhing with George Ellery Hale Past, Looking to the Future: Partnerships Nuclear 108 – Astronomy Education: Where Are We 205 – The Atacama Large 309 – Galaxies and AGN II Now and Where Are We Going? Millimeter/submillimeter Array: A New 310 – Young Stellar Objects, Star Formation 109 – Bridging Laboratory and Astrophysics: Window on the Universe and Star Clusters Molecules 208 – Galaxies and AGN I 311 – Curiosity on Mars: The Latest Results 110 – Interstellar Medium, Dust, Etc. 209 – Supernovae and Neutron
    [Show full text]
  • WG Photometry and Polarimetry of Asteroids
    PHOTOMETRY AND POLARIMETRY OF ASTEROIDS: IMPACT ON COLLABORATION Abstracts The International Workshop -2 80 0 60 2 40 4 20 6 Relative Magnitude Polarization Degree 0 8 10 -20 0 20 40 60 80 100 120 140 160 180 Phase Angle June 15–18, 2003, Kharkiv, Ukraine Organized by Research Institute of Astronomy of V. N. Karazin Kharkiv National University, Ukrainian Astronomical Association Ministry of Education and Science of Ukraine Sponsored by Kharkiv City Charity Fund “AVEC” PHOTOMETRY AND POLARIMETRY OF ASTEROIDS: IMPACT ON COLLABORATION The International Workshop June 15–18, 2003 Kharkiv, Ukraine A B S T R A C T S The Organizing Committee: Lupishko Dmitrij (co-Chairman), Kiselev Nikolai (co-Chairman), Belskaya Irina, Krugly Yurij, Shevchenko Vasilij, Velichko Fiodor, Luk’yanyk Igor Kharkiv - 2003 2 Contents Belskaya I.N., Shevchenko V.G., Efimov Yu.S., Shakhovskoj N.M., Gaftonyuk N.M., Krugly Yu.N., Chiorny V.G. Opposition Polarimetry and Photometry of Asteroids 5 Bochkov V.V., Prokof’eva V.V. Spectrophotometric Observations of Asteroids in the Crimean Astrophysical Observatory 6 Butenko G., Gerashchenko O., Ivashchenko Yu., Kazantsev A., Koval’chuk G., Lokot V. Estimates of Rotation Periods of Asteroids Derived from CCD- Observations in Andrushivka Astronomical Observatory 7 Bykov O.P., L'vov V.N. Method of accuracy estimation of asteroid positional CCD observations and results its application with EPOS Software 7 Cellino A., Gil Hutton R., Di Martino M., Tedesco E.F., Bendjoya Ph. Polarimetric Observations of Asteroids with the Torino UBVRI Photopolarimeter 9 Chiorny V.G., Shevchenko V.G., Krugly Yu.N., Velichko F.P., Gaftonyuk N.M.
    [Show full text]
  • U.S. Naval Observatory Washington, DC 20392-5420 This Report Covers the Period July 2001 Through June Dynamical Astronomy in Order to Meet Future Needs
    1 U.S. Naval Observatory Washington, DC 20392-5420 This report covers the period July 2001 through June dynamical astronomy in order to meet future needs. J. 2002. Bangert continued to serve as Department head. I. PERSONNEL A. Civilian Personnel A. Almanacs and Other Publications Marie R. Lukac retired from the Astronomical Appli- cations Department. The Nautical Almanac Office ͑NAO͒, a division of the Scott G. Crane, Lisa Nelson Moreau, Steven E. Peil, and Astronomical Applications Department ͑AA͒, is responsible Alan L. Smith joined the Time Service ͑TS͒ Department. for the printed publications of the Department. S. Howard is Phyllis Cook and Phu Mai departed. Chief of the NAO. The NAO collaborates with Her Majes- Brian Luzum and head James R. Ray left the Earth Ori- ty’s Nautical Almanac Office ͑HMNAO͒ of the United King- entation ͑EO͒ Department. dom to produce The Astronomical Almanac, The Astronomi- Ralph A. Gaume became head of the Astrometry Depart- cal Almanac Online, The Nautical Almanac, The Air ment ͑AD͒ in June 2002. Added to the staff were Trudy Almanac, and Astronomical Phenomena. The two almanac Tillman, Stephanie Potter, and Charles Crawford. In the In- offices meet twice yearly to discuss and agree upon policy, strument Shop, Tie Siemers, formerly a contractor, was hired science, and technical changes to the almanacs, especially to fulltime. Ellis R. Holdenried retired. Also departing were The Astronomical Almanac. Charles Crawford and Brian Pohl. Each almanac edition contains data for 1 year. These pub- William Ketzeback and John Horne left the Flagstaff Sta- lications are now on a well-established production schedule.
    [Show full text]
  • Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets
    University of Central Florida STARS Electronic Theses and Dissertations, 2004-2019 2014 Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets Nathaniel Lust University of Central Florida Part of the Astrophysics and Astronomy Commons, and the Physics Commons Find similar works at: https://stars.library.ucf.edu/etd University of Central Florida Libraries http://library.ucf.edu This Doctoral Dissertation (Open Access) is brought to you for free and open access by STARS. It has been accepted for inclusion in Electronic Theses and Dissertations, 2004-2019 by an authorized administrator of STARS. For more information, please contact [email protected]. STARS Citation Lust, Nathaniel, "Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets" (2014). Electronic Theses and Dissertations, 2004-2019. 4635. https://stars.library.ucf.edu/etd/4635 CREATION AND APPLICATION OF ROUTINES FOR DETERMINING PHYSICAL PROPERTIES OF ASTEROIDS AND EXOPLANETS FROM LOW SIGNAL-TO-NOISE DATA-SETS by NATE B LUST B.S. University of Central Florida, 2007 A dissertation submitted in partial fulfilment of the requirements for the degree of Doctor of Philosophy in Physics in the Department of Physics in the College of Sciences at the University of Central Florida Orlando, Florida Fall Term 2014 Major Professor: Daniel Britt © 2014 Nate B Lust ii ABSTRACT Astronomy is a data heavy field driven by observations of remote sources reflecting or emitting light. These signals are transient in nature, which makes it very important to fully utilize every observation.
    [Show full text]
  • Callhorizons Documentation Release 1.0.5
    callHORIZONS Documentation Release 1.0.5 Michael Mommert Jul 19, 2018 Contents 1 Installation 3 1.1 PIP....................................................3 1.2 GitHub..................................................3 2 How to Use It? 5 3 Examples 9 4 callhorizons 11 4.1 callhorizons module........................................... 11 5 Indices and tables 17 Python Module Index 19 i ii callHORIZONS Documentation, Release 1.0.5 CALLHORIZONS is a Python interface to access JPL HORIZONS ephemerides and orbital elements of Solar System bodies. Please note that CALLHORIZONS is not maintained anymore. Please use astroquery.jplhorizons instead, which will be maintained in the future and offers additional functionality. I apologize for any inconvenience. Contents 1 callHORIZONS Documentation, Release 1.0.5 2 Contents CHAPTER 1 Installation Please note that CALLHORIZONS is not maintained anymore. Please use [astroquery.jplhorizons](http:// astroquery.readthedocs.io/en/latest/jplhorizons/jplhorizons.html) instead, which will be maintained in the future and offers additional functionality. I apologize for any inconvenience. 1.1 PIP Using PIP, simply call: pip install callhorizons 1.2 GitHub Using git, simply clone the code from GitHub: git clone https://github.com/mommermi/callhorizons or, download and unpack the zip file with all the files from GitHub and then run from the callhorizons directory: python setup.py install 3 callHORIZONS Documentation, Release 1.0.5 4 Chapter 1. Installation CHAPTER 2 How to Use It? Please note that CALLHORIZONS is not maintained anymore. Please use [astroquery.jplhorizons](http:// astroquery.readthedocs.io/en/latest/jplhorizons/jplhorizons.html) instead, which will be maintained in the future and offers additional functionality. I apologize for any inconvenience.
    [Show full text]