DOCSLIB.ORG

The Minor Planet Bulletin 41 (2014) 158 Same Response

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Minor Planet Bulletin 41 (2014) 158 Same Response THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 41, NUMBER 3, A.D. 2014 JULY-SEPTEMBER 139. LIGHTCURVES FOR INVERSION MODEL CANDIDATES about asteroid discovery dates and names comes from the JPL small bodies database (JPLSBD, 2014). The list of observed Daniel A. Klinglesmith III, Jesse Hanowell, Ethan Risley, Janek asteroids is given Table 1. This table contains the asteroid number, Turk, Angelica Vargas, Curtis Alan Warren name, date range, solar phase angle, average solar bisector phase Etscorn Campus Observatory, New Mexico Tech angles, period determination, period error, amplitude, amplitude 101 East Road error. Table 2 summarizes the solar bisector phase angles of Socorro, NM USA 87801 published lightcurves for these asteroids. The previously observed [email protected] solar bisector phase angles were obtained from the Lightcurve data base (LCDB; Warner, 2014). (Received: 15 April) Individual Asteroids We present lightcurves for 12 inversion model candidate 199 Byblis is a main-belt asteroid discovered by C.H.F. Peters at asteroids that will benefit from additional data at another Clinton on 1879 Jul 09. It is also known at 1971 WB. Behrend solar bisector phase angle. We obtained synodic periods reports four period results based on data from different observers: for each asteroid that were within ± 0.002 h. Most have F. Manzini (Behrend, 2008), P = 5.22024 h; R. Roy (Behrend shapes that differed from previously published 2006), P = 5.22024 h; R. Roy et al. (Behrend, 2005), P = 5.22012 lightcurves in both amplitude and shape. ± 0.000240 h; and S. Casulli and L. Bernasconi (Behrend, 2003), P = 5.22022 ± 0.0003. Hanus (2013) in the process of determining shape models reports a sidereal period of 5.22063 hours. We The observations of asteroid lightcurves were obtained at the observed 199 Byblis on 7 nights between 2014 Feb 18 and Apr 01. Etscorn Campus Observatory (ECO, 2014). We used three We can duplicate the periods of the previous researchers of 5.221 ± Celestron 0.35-m Schmidt-Cassegrain telescopes (SCTs) on 0.001 h with an amplitude of A = 0.08 ± 0.10 mag. However that Software Bisque Parmount ME mounts (SB, 2014). Two of the result has only one maximum and one minimum. If we double the telescopes used SBIG STL 1001E CCDs that have 1024x1024 24- period to 10.444 ± 0.001 with A = 0.09 ± 0.10 mag, we get a micron pixels. The third telescope used an SBIG ST10XME with bimodal lightcurve with a slightly better fit. an Optec 0.5x focal reducer. The ST10XME was binned 2x2 providing an image of 1092x736 13.6-micron pixels. The pixel 616 Elly is a main-belt asteroid discovered by A. Kopff at size for the STL-1001E cameras is 1.25 arcsec/pix. This provides a Heidelberg on 1906 Oct 17. It is also known as 1906 VT. Warner 22x22 arc minute field-of-view. The ST10 XME pixel size is 1.28 (2010) reports a period of 5.297 ± 0.003 h with A = 0.48 mag. arcsec/pix. This provides a 20x16 arc minute field-of-view. The Durkee (2010) reports a period of 4.30 ± 0.02 h with A = 0.38 mag. asteroid images were obtained through clear filters. Exposure times Mikulecka (2010) reports a period of 5.297 ± 0.001 h with A = varied between 2 and 5 minutes depending on the brightness of the 0.35 ± 0.05 mag. We observed 616 Elly on 8 nights between 2014 object. Each evening a series of 11 dome flats was obtained and Feb and Mar 22. Our period determination was 5.298 ± 0.002 h combined into a master flat with a median filter. The telescopes with A = 0.36 ± 0.05 mag. were controlled with Software Bisque’s TheSky6 (SB, 2014) and the CCDs were controlled with CCDsoft V5 (SB, 2014). The 620 Drakonia is a main-belt asteroid discovered by J. H. Metcaff at images were dark subtracted and flat field corrected using image Taunton on 1906 Oct 26. It is also known as 1906 WE, 1950 ET, processing tools within MPO Canopus version 10.4.1.9 (Warner, 1950 HS, and 1955 QE1. Warner (2002) reports a period of 5.485 2014). The multi-night data sets for each asteroid were combined ± 0.01 h with A = 0.52 ± 0.02 mag. Bin et al. (2011) report a with the FALC routine (Harris et. al., 1989) within MPO Canopus period of 5.480 ± 0.003 h with A = 0.08 ± 0.01 mag. We observed to provide synodic periods for each asteroid. 620 Drakonia for 9 nights between 2014 Feb 09 and Mar 24. Our period determination is 5.487 ± 0.001 h with A = 0.65 ± Observed Asteroids 0.05 mag. The 12 asteroids observed were taken from the list of possible 822 Lalage is a main-belt asteroid discovered by M. Wolf at inversion model candidates by Warner et al. (2014). All have Heidelberg on 1916 Mar 31. It is also known as 1916 ZD and 1943 periods less than 8 hours. This allowed us, in many cases, to obtain EJ1. Wisniewski et al. (1995) reported a period of 3.345 ± 0.001 h. at least one complete cycle per observing night. The information Higgins (2011) reported a period of 3.3465 ± 0.0006 h with A = Minor Planet Bulletin 41 (2014) Available on line http://www.minorplanet.info/mpbdownloads.html 140 Table 1. Current results # Name 2014 (mm/dd) UT Phase PABL PABB Period P. E Amp A.E. 199 Byblis 02/18 - 04/01 13.6,7.4, 7.6 185 18 5.221 0.001 0.1 0.07 616 Elly 02/18 - 03/22 4.6,4.1,13.4 153 7 5.298 0.002 0.4 0.05 620 Drakonia 02/09 - 03/24 7.8,4.1,14.1 115 8 5.487 0.001 0.7 0.05 822 Lalage 02/08 - 03/11 1.7, ,16.1 143 -1 3.346 0.001 0.5 0.10 855 Newcombia 03/25 - 04/07 8.3, , 0.8 198 0 3.003 0.001 0.3 0.05 1044 Teutonia 01/27 - 02/21 4.4, ,13.1 116 4 3.157 0.001 0.3 0.10 1219 Britta 02/12 - 03/17 19.9, ,27.3 113 5 5.575 0.001 0.7 0.10 1294 Antwerpia 03/19 - 03/24 12.8, ,14.2 146 10 6.623 0.001 0.4 0.10 1299 Mertona 04/02 - 04/04 18.2, ,18.7 144 -2 4.978 0.002 0.6 0.10 1321 Majuba 03/13 - 03/29 2.4, , 6.7 170 -6 5.221 0.001 0.4 0.10 2381 Landi 01/21 - 03/25 5.7, ,23.4 118 -8 3.986 0.001 0.9 0.05 3573 Holmberg 01/27 - 03/25 9.0, ,27.4 115 -2 6.543 0.001 0.9 0.10 Table 2. Previous Solar Bisector Phase Angles number name reference Date PABL PABB 199 Byblis Behrend 2003web 2003 Apr 08 218.5 25.9 199 Byblis Behrend 2005web 2005 Nov 09 46.5 -12 199 Byblis Behrend 2006web 2006 Dec 20 100.8 3.2 199 Byblis Behrend 2008web 2008 Feb 09 159.3 17 616 Elly Warner 2010 MPB 37, 112 2010 Jan 31 161.8 7.2 616 Elly Durkee 2010 MPB 37, 125 2010 Feb 24 162.6 5.4 616 Elly Mikulecka 2011web 2010 Mar 03 162.6 4.9 620 Drakonia Warner 2002b MPB 29, 27 2001 Nov 05 42.9 7.3 620 Drakonia warner 2011f MPB 38, 52 2001 Nov 05 42.9 7.3 620 Drakonia Bin 2011 MPB 38, 179 2001 Mar 02 190.2 -0.7 822 Lalage Wisniewski 1992 Sep 25 0.1 0.5 822 Lalage Higgins 2011a MPB 38,41 2009 Oct 09 9.8 0.3 822 Lalage Stephens 2014 web 2014 Jan 14 139.2 -1 855 Newcombia Cooney 2007 MPB 34, 47 2004 Oct 14 9 -1.4 1044 Teutonia Behrend 2006 web 2006 Jan 11 139.1 5 1044 Teutonia Betzler 2008b MPB 35, 26 2007 Jun 08 256.3 -1.7 1044 Teutonia Behrend 2012 web 2012 Nov 13 28.8 -2.4 1219 Britta Behrend 2003 web 2003 Dec 26 79.4 4.4 1294 Antwerpia Lecrone 2005 MPB 32, 46 2005 Feb 02 127.7 8.4 1294 Antwerpia Behrend 2005web 2006 Mar 26 206.1 9 1294 Antwerpia Stephens 2014web 2014 Jan 16 146.3 9.2 1299 Mertona Monson 2004 MPB 31, 97 2003 Nov 25 50.2 -9.9 1299 Mertona Behrend 2005web 2005 Mar 14 179 2.1 1321 Majuba Ditteon 2007 MPB 34, 59 2006 Nov 09 42.1 11.8 1321 Majuba Behrend 2006web 2006 Nov 11 42.1 11.8 2381 Landi 3573 Holmberg Galad 2008 MPB 35, 78 2007 Jan 12 63.6 0.8 0.58 ± 0.01 mag. We observed 822 Lalage for 6 nights between for 9 nights between 2014 Mar 25 and Apr 07. Our period 2014 Feb 08 and Mar 11. Our period determination was 3.346 ± determination agrees with Cooney et al.: 3.003 ± 0.001 h with A = 0.001 h with A = 0.53 ± 0.10 mag. 0.33 ± 0.05 mag and a very similar shape. 855 Newcombia is a main-belt asteroid discovered by S. 1044 Teutonia is a main-belt asteroid discovered by K.
Load more

Recommended publications
  • Color Changes for the Surface of 6478 Gault (??) Submitted to Apjl
    Draft version August 3, 2020 Typeset using LATEX twocolumn style in AASTeX63 Color changes for the Surface of 6478 Gault (??) 1 2 2 3 4 5 1 Remington Cantelas, Karen J. Meech, Jan T. Kleyna, Erica Bufanda, Alan Fitzsimmons, James Bauer, 2 2 2 6 2 2 Larry Denneau, Robert Weryk, Jacqueline V. Keane, Olivier R. Hainaut, and Richard J. Wainscoat 1 3 University of Central Florida, 4111 Libra Drive, Orlando, FL 32816, USA 2 4 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 3 5 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822 USA 4 6 Astrophysics Research Centre, Queen's University Belfast, Belfast BT7 1NN, UK 5 7 University of Maryland, Dept. of Astronomy, College Park, MD 20742-2421 USA 6 8 European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei M¨unchen,Germany 9 Submitted to ApJL 10 ABSTRACT 11 (6478) Gault is a main belt asteroid in the Phocaea Family which was discovered to have activity in 12 January 2019, and precovery images reveal it has been consistently active since at least September 2013. 13 Gault's activity is believed to be caused by it being a fast rotator near the asteroid break-up limit. We 14 have collected images and photometry from several telescopes dating back several apparitions. Using 15 this data we attempt to produce a reliable rotational light curve and confirm Gault's rotation period. 16 We also investigate possible color variations on the surface of the asteroid by measuring it's spectral 17 reflectivity over the course of 7 months between January and August 2019.
    [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]
  • 1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
    Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H.
    [Show full text]
  • The Minor Planet Bulletin, Alan W
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 42, NUMBER 2, A.D. 2015 APRIL-JUNE 89. ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY SOUTHERN SKY OBSERVATORY: 2014 SEPTEMBER Lucas Bohn, Brianna Hibbler, Gregory Stein, Richard Ditteon Rose-Hulman Institute of Technology, CM 171 5500 Wabash Avenue, Terre Haute, IN 47803, USA [email protected] (Received: 24 November) Photometric data were collected over the course of seven nights in 2014 September for eight asteroids: 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 2699 Kalinin, 3197 Weissman, 7837 Mutsumi, 14927 Satoshi, and (29769) 1999 CE28. Eight asteroids were remotely observed from the Oakley Southern Sky Observatory in New South Wales, Australia. The observations were made on 2014 September 12-14, 16-19 using a 0.50-m f/8.3 Ritchey-Chretien optical tube assembly on a Paramount ME mount and SBIG STX-16803 CCD camera, binned 3x3, with a luminance filter. Exposure times ranged from 90 to 180 sec depending on the magnitude of the target. The resulting image scale was 1.34 arcseconds per pixel. Raw images were processed in MaxIm DL 6 using twilight flats, bias, and dark frames. MPO Canopus was used to measure the processed images and produce lightcurves. In order to maximize the potential for data collection, target asteroids were selected based upon their position in the sky approximately one hour after sunset. Only asteroids with no previously published results were targeted. Lightcurves were produced for 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 3197 Weissman, and (29769) 1999 CE28.
    [Show 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 35, NUMBER 3, A.D. 2008 JULY-SEPTEMBER 95. ASTEROID LIGHTCURVE ANALYSIS AT SCT/ST-9E, or 0.35m SCT/STL-1001E. Depending on the THE PALMER DIVIDE OBSERVATORY: binning used, the scale for the images ranged from 1.2-2.5 DECEMBER 2007 – MARCH 2008 arcseconds/pixel. Exposure times were 90–240 s. Most observations were made with no filter. On occasion, e.g., when a Brian D. Warner nearly full moon was present, an R filter was used to decrease the Palmer Divide Observatory/Space Science Institute sky background noise. Guiding was used in almost all cases. 17995 Bakers Farm Rd., Colorado Springs, CO 80908 [email protected] All images were measured using MPO Canopus, which employs differential aperture photometry to determine the values used for (Received: 6 March) analysis. Period analysis was also done using MPO Canopus, which incorporates the Fourier analysis algorithm developed by Harris (1989). Lightcurves for 17 asteroids were obtained at the Palmer Divide Observatory from December 2007 to early The results are summarized in the table below, as are individual March 2008: 793 Arizona, 1092 Lilium, 2093 plots. The data and curves are presented without comment except Genichesk, 3086 Kalbaugh, 4859 Fraknoi, 5806 when warranted. Column 3 gives the full range of dates of Archieroy, 6296 Cleveland, 6310 Jankonke, 6384 observations; column 4 gives the number of data points used in the Kervin, (7283) 1989 TX15, 7560 Spudis, (7579) 1990 analysis. Column 5 gives the range of phase angles.
    [Show full text]
  • Multiple Outbursts of Asteroid (6478) Gault∗
    Draft version March 14, 2019 Typeset using LATEX default style in AASTeX62 Multiple Outbursts of Asteroid (6478) Gault∗ 1, 2 3 4 5, 6, 5 Quanzhi Ye (叶泉志), Michael S. P. Kelley, Dennis Bodewits, Bryce Bolin, y Lynne Jones, Zhong-Yi Lin (林忠©),7 Eric C. Bellm,5 Richard Dekany,8 Dmitry A. Duev,1 Steven Groom,2 George Helou,2 Shrinivas R. Kulkarni,1 Thomas Kupfer,9 Frank J. Masci,2 Thomas A. Prince,1 and Maayane T. Soumagnac10 1Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, U.S.A. 2Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, U.S.A. 3Department of Astronomy, University of Maryland, College Park, MD 20742, U.S.A. 4Department of Physics, Auburn University, Auburn, AL 36849, U.S.A. 5DIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, U.S.A. 6B612 Asteroid Institute, 20 Sunnyside Ave, Suite 427, Mill Valley, CA 94941, U.S.A. 7Institute of Astronomy, National Central University, 32001, Taiwan 8Caltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, U.S.A. 9Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, U.S.A. 10Department of Particle Physics and Astrophysics, Weizmann Institute of Science 234 Herzl St., Rehovot, 76100, Israel (Received {; Revised {; Accepted {) Submitted to ApJL ABSTRACT Main-belt asteroid (6478) Gault unexpectedly sprouted two tails in late 2018 and early 2019, iden- tifying it as a new active asteroid. Here we present observations obtained by the 1.2-m Zwicky Tran- sient Facility survey telescope that provide detailed time-series coverage of the onset and evolution of Gault's activity.
    [Show 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 41, NUMBER 4, A.D. 2014 OCTOBER-DECEMBER 203. LIGHTCURVE ANALYSIS FOR 4167 RIEMANN Amy Zhao, Ashok Aggarwal, and Caroline Odden Phillips Academy Observatory (I12) 180 Main Street Andover, MA 01810 USA [email protected] (Received: 10 June) Photometric observations of 4167 Riemann were made over six nights in 2014 April. A synodic period of P = 4.060 ± 0.001 hours was derived from the data. 4167 Riemann is a main-belt asteroid discovered in 1978 by L. V. Period analysis was carried out by the authors using MPO Canopus Zhuraveya. Observations of the asteroid were conducted at the and its Fourier analysis feature developed by Harris (Harris et al., Phillips Academy Observatory, which is equipped with a 0.4-m f/8 1989). The resulting lightcurve consists of 288 data points. The reflecting telescope by DFM Engineering. Images were taken with period spectrum strongly favors the bimodal solution. The an SBIG 1301-E CCD camera that has a 1280x1024 array of 16- resulting lightcurve has synodic period P = 4.060 ± 0.001 hours micron pixels. The resulting image scale was 1.0 arcsecond per and amplitude 0.17 mag. Dips in the period spectrum were also pixel. Exposures were 300 seconds and taken primarily at –35°C. noted at 8.1200 hours (2P) and at 6.0984 hours (3/2P). A search of All images were guided, unbinned, and unfiltered. Images were the Asteroid Lightcurve Database (Warner et al., 2009) and other dark and flat-field corrected with Maxim DL.
    [Show full text]
  • The Sporadic Activity of (6478) Gault: a YORP-Driven Event?
    The Astrophysical Journal Letters, 874:L20 (7pp), 2019 April 1 https://doi.org/10.3847/2041-8213/ab0f40 © 2019. The American Astronomical Society. All rights reserved. The Sporadic Activity of (6478) Gault: A YORP-driven Event? Jan T. Kleyna1 , Olivier R. Hainaut2 , Karen J. Meech1 , Henry H. Hsieh3,4 , Alan Fitzsimmons5 , Marco Micheli6,7 , Jacqueline V. Keane1 , Larry Denneau1 , John Tonry1 , Aren Heinze1 , Bhuwan C. Bhatt8 , Devendra K. Sahu8 , Detlef Koschny6,9,10 , Ken W. Smith5 , Harald Ebeling1 , Robert Weryk1 , Heather Flewelling1 , and Richard J. Wainscoat1 1 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 2 European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München, Germany 3 Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719, USA 4 Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan 5 Astrophysics Research Centre, Queen’s University Belfast, Belfast BT7 1NN, UK 6 ESA NEO Coordination Centre, Largo Galileo Galilei, 1, I-00044 Frascati (RM), Italy 7 INAF—Osservatorio Astronomico di Roma, Via Frascati, 33, I-00040 Monte Porzio Catone (RM), Italy 8 Indian Institute for Astrophysics, II Block, Koramangala, Bangalore 560 034, India 9 ESTEC, European Space Agency, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands 10 Chair of Astronautics, Technical University of Munich, Boltzmannstraße 15, D-85748 Garching bei München, Germany Received 2019 February 22; revised 2019 March 13; accepted 2019 March 13; published 2019 April 1 Abstract On 2019 January 5 a streamer associated with the 4–10 km main belt asteroid (6478)Gault was detected by the ATLAS sky survey, a rare discovery of activity around a main belt asteroid.
    [Show full text]
  • Asteroid Belt - Wikipedia
    12/2/2018 Asteroid belt - Wikipedia Asteroid belt The asteroid belt is the circumstellar disc in the Solar System located roughly between the orbits of the planets Mars and Jupiter. It is occupied by numerous irregularly shaped bodies called asteroids or minor planets. The asteroid belt is also termed the main asteroid belt or main belt to distinguish it from other asteroid populations in the Solar System such as near-Earth asteroids and trojan asteroids.[1] About half the mass of the belt is contained in the four largest asteroids: Ceres, Vesta, Pallas, and Hygiea.[1] The total mass of the asteroid belt is approximately 4% that of the Moon, or 22% that of Pluto, and roughly twice that of Pluto's moon Charon (whose diameter is 1200 km). Ceres, the asteroid belt's only dwarf planet, is about 950 km in diameter, whereas 4 Vesta, 2 Pallas, and 10 Hygiea have mean diameters of less than 600 km.[2][3][4][5] The remaining bodies range down to the size of a dust particle. The asteroid material is so thinly distributed that numerous unmanned spacecraft have traversed it without incident.[6] Nonetheless, collisions between large asteroids do occur, and these can produce an asteroid family whose members have similar orbital characteristics and compositions. Individual asteroids within the asteroid belt are categorized by their spectra, with most falling into three basic groups: carbonaceous (C-type), silicate (S-type), and metal-rich (M-type). The asteroid belt formed from the primordial solar nebula as a group of planetesimals.[7] Planetesimals are the The asteroids of the inner Solar System and Jupiter: The donut-shaped asteroid belt is located smaller precursors of the protoplanets.
    [Show full text]
  • New and Updated Convex Shape Models of Asteroids Based on Optical Data from a Large Collaboration Network
    A&A 586, A108 (2016) Astronomy DOI: 10.1051/0004-6361/201527441 & c ESO 2016 Astrophysics New and updated convex shape models of asteroids based on optical data from a large collaboration network J. Hanuš1,2,J.Durechˇ 3, D. A. Oszkiewicz4,R.Behrend5,B.Carry2,M.Delbo2,O.Adam6, V. Afonina7, R. Anquetin8,45, P. Antonini9, L. Arnold6,M.Audejean10,P.Aurard6, M. Bachschmidt6, B. Baduel6,E.Barbotin11, P. Barroy8,45, P. Baudouin12,L.Berard6,N.Berger13, L. Bernasconi14, J-G. Bosch15,S.Bouley8,45, I. Bozhinova16, J. Brinsfield17,L.Brunetto18,G.Canaud8,45,J.Caron19,20, F. Carrier21, G. Casalnuovo22,S.Casulli23,M.Cerda24, L. Chalamet86, S. Charbonnel25, B. Chinaglia22,A.Cikota26,F.Colas8,45, J.-F. Coliac27, A. Collet6,J.Coloma28,29, M. Conjat2,E.Conseil30,R.Costa28,31,R.Crippa32, M. Cristofanelli33, Y. Damerdji87, A. Debackère86, A. Decock34, Q. Déhais36, T. Déléage35,S.Delmelle34, C. Demeautis37,M.Dró˙zd˙z38, G. Dubos8,45, T. Dulcamara6, M. Dumont34, R. Durkee39, R. Dymock40, A. Escalante del Valle85, N. Esseiva41, R. Esseiva41, M. Esteban24,42, T. Fauchez34, M. Fauerbach43,M.Fauvaud44,45,S.Fauvaud8,44,45,E.Forné28,46,†, C. Fournel86,D.Fradet8,45, J. Garlitz47, O. Gerteis6, C. Gillier48, M. Gillon34, R. Giraud34, J.-P. Godard8,45,R.Goncalves49, Hiroko Hamanowa50, Hiromi Hamanowa50,K.Hay16, S. Hellmich51,S.Heterier52,53, D. Higgins54,R.Hirsch4, G. Hodosan16,M.Hren26, A. Hygate16, N. Innocent6, H. Jacquinot55,S.Jawahar56, E. Jehin34, L. Jerosimic26,A.Klotz6,57,58,W.Koff59, P. Korlevic26, E. Kosturkiewicz4,38,88,P.Krafft6, Y. Krugly60, F. Kugel19,O.Labrevoir6, J.
    [Show full text]
  • Synthetic Tracking Using ZTF Deep Drilling Data Sets Chengxing Zhai1 , Quanzhi Ye2,3,4, Michael Shao1, Russell Trahan1, Navtej S
    Publications of the Astronomical Society of the Pacific, 132:064502 (8pp), 2020 June https://doi.org/10.1088/1538-3873/ab828b © 2020. The Astronomical Society of the Pacific Printed in the U.S.A. Synthetic Tracking Using ZTF Deep Drilling Data Sets Chengxing Zhai1 , Quanzhi Ye2,3,4, Michael Shao1, Russell Trahan1, Navtej S. Saini1, Janice Shen1, Thomas A. Prince2, Eric C. Bellm5, Matthew J. Graham2 , George Helou3, Shrinivas R. Kulkarni2, Thomas Kupfer6, Russ R. Laher3, Ashish Mahabal2,3 , Frank J. Masci3 , Ben Rusholme3, Philippe Rosnet7, and David L. Shupe3 1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr, Pasadena, CA 91109, USA; [email protected] 2 Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 3 IPAC, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA 4 University of Maryland, Department of Astronomy, College Park, MD 20742, USA 5 DIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, USA 6 Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA 7 Université Clermont Auvergne, CNRS/IN2P3, LPC, Clermont-Ferrand, France Received 2020 January 13; accepted 2020 March 23; published 2020 April 21 Abstract The Zwicky Transit Facility (ZTF) is a powerful time domain survey telescope with a large field of view of 47 deg2. We apply the synthetic tracking technique to integrate a ZTF’s deep drilling data set, which consists of 133 nominal 30 s exposure frames spanning about 1.5 hr, to search for slowly moving asteroids down to approximately 23rd magnitude.
    [Show full text]
  • Prezentácia Programu Powerpoint
    VÝSKUM ASTEROIDOV A KOMÉT NA ASTRONOMICKOM ÚSTAVE SAV MAREK HUSÁRIK ASTRONOMICKÝ ÚSTAV SAV, T. LOMNICA BEZOVEC 2020 2. OKTÓBER BRIEF HISTORY OF COMET AND ASTEROID RESEARCH • 1943 – starting of comet discoveries and meteor research • 1946 – discovery of the first comet Pajdušáková-Rotbart-Weber • 1946-1959 – 70 new comets discovered over the world, 18 from Skalnate Pleso (Honda- Mrkos-Pajdušáková, Tuttle-Giacobini-Kresák, 1957 V Mrkos,...) • 1964 – asteroid observations and astrometry CURRENT RESEARCH AT THE INTERPLANETARY MATTER DEPARTMENT • Investigation of the activity, physical and dynamical evolution of selected cometary nuclei • Color photometry, lightcurves, and modelling of shapes of the asteroids • Study of transfer orbits, interrelations and evolution among different populations regarding near- Earth objects • Study of the structure of the outer part of the Oort cloud and the Edgeworth-Kuiper belt • Study of structure and dynamics of meteoroid streams, evolution of their parent bodies, the distribution of meteoroid particles in the inner Solar System, search for meteoroid streams of asteroidal origin, search for hyperbolic and interstellar meteoroids • Operation of the all-sky bolide cameras within the European Fireball Network • Study of meteorite properties • Study of the physical and chemical properties of asteroid/comet surfaces and their relevant terrestrial analogs, simulation of effects of space weathering in laboratory conditions • The IAU Meteor Data Center (MDC) operates at the AI SAS under the auspices of Division F (Planetary Systems and Bioastronomy) of the International Astronomical Union (IAU). The MDC is responsible for the designation of meteor showers, for the efficient collection, (computation,) checking and dissemination of trajectory observations and orbits of meteors. It acts as a central depository for meteor orbits obtained by photographic, video and radar techniques.
    [Show full text]