The Minor Planet Bulletin

Total Page:16

File Type:pdf, Size:1020Kb

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. If there are TN1, (13578) 1993 MK, (24819) 1994 XY4, (26471) three values in the column, the phase angle reached a minimum 2000 AS152, (26916) 1996 RR2, and 2008 CN1. with the middle value being the minimum. Columns 6 and 7 give the range of values, or average if the range was relatively small, Observations of 17 asteroids were made at the Palmer Divide for the Phase Angle Bisector (PAB) longitude and latitude Observatory from December 2007 into early March 2008. One of respectively. Columns 8 and 10 give the period and amplitude of four telescopes/camera combinations was used: 0.5m Ritchey- the curve while columns 9 and 11 give the respective errors in Chretien/SBIG STL-1001E, 0.35m SCT/FLI IMG-1001E, 0.35m hours and magnitudes. An “(H)” follows the name of an asteroid Date Range Data Per Amp (mm/dd) # Name Pts Phase PAB PAB (h) PE (mag) AE 2007/08 L B 793 Arizona 01/26-27 107 20.3 60.7 10.1 7.367 0.005 0.25 0.02 1092 Lilium 02/09–03/04 508 8.0,14.9 118.4 0.3 24.60 0.05 0.30 0.02 2093 Genichesk (B) 02/24-28 200 4.4,6.4 146.1 -0.8 11.028 0.006 0.24 0.02 3086 Kalbaugh (H) 01/27-02/02 248 5.6,4.2 133.0 -5.6 5.1790 0.0003 0.47 0.02 4859 Fraknoi (B) 02/06-13 304 10.4,14.1 120.0 -0.6 7.846 0.003 0.15 0.02 5806 Archieroy (H) 01/26-02/06 642 3.6,10.9 120.1 -1.5 12.163 0.011 0.45 0.02 15.65 6296 Cleveland (H) 01/11-15 462 7.9,10.2 101.1 -5.0 0.01 0.11 0.02 31.54 6310 Jankonke (H) 01/14-15 234 16.0 120.1 22.5 3.080 0.003 0.14 0.02 6384 Kervin (H) 12/29-01/13 270 8.4,15.7 90.7 12.7 3.647 0.001 0.06 0.2 7283 1989 TX15 (B) 02/24-28 181 3.4,3.7 155.8 5.2 2.6747 0.0005 0.19 0.02 7560 Spudis (H) 01/26-02/13 328 4.2,12.8 125.0 -7.5 3.5448 0.0004 0.10 0.02 7579 1990 TN1 (H) 12/18-01/05 704 15.4,20.5 75.8 20.3 18.312 0.001 1.10 0.03 13578 1993 MK (H) 12/29-01/12 257 20.2,24.0 71.9 -18.0 7.924 0.003 0.09 0.01 27.73 0.04 24819 1994 XY4 12/29-01/12 584 7.3,17.3 90.0 7.3 0.04 0.01 57.57 0.09 26471 2000 AS152 (H) 02/06-16 193 12.3,16.0 122.0 -17.2 2.687 0.001 0.20 0.02 26916 1996 RR2 (H) 12/29-01/02 342 11.4,10.8 100.3 16.6 10.324 0.003 1.05 0.03 2000 CN1 02/16-24 475 23.6,22.7 158,147 6.0,-2.8 6.0555 0.0002 1.04 0.02 Minor Planet Bulletin 35 (2008) Available on line http://www.minorplanetobserver.com/mpb/default.htm 96 in the table if it is a member of the Hungaria group or family. A the 3.54 h solution in 2008 was not as dominant though still “(B)” follows the name if the asteroid is a member of the significant. Additional data are needed to resolve the ambiguity. Baptistina family. The latter are thought to have been recently formed (160 MY) from a catastrophic collision (Bottke et al., (7579) 1990 TN1. The solution is considered unique since a half- 2007. Nature 449, 48-53) and will be targeted by PDO in the period fit shows a well-fitting monomodal curve. However, given future. the amplitude, that shorter period is not likely. 793 Arizona. This is a follow up to work by the author in early (13578) 1993 MK. Some longer periods were possible but December 2007 (Warner 2008) to determine how the shape and required tri- and multimodal curves and so were rejected as being amplitude changed with increased phase angle. The synodic highly unlikely. period, 7.367 ± 0.005 h, was about 0.03 h less than in December and the amplitude about 0.03 mag greater. Unfortunately, there are (26471) 2000 AS152. The period agrees with the posted by insufficient data from other apparitions, dense or sparse, to Behrend (2008). generate a model at this time. 2008 CN1. This Aten asteroid’s aphelion reaches just beyond the 1092 Lilium. Binzel (1987) reported a period of either 15.66 or Earth’s. It was only 0.044-0.051 AU from Earth when observed in 17.63 based on four nights of data and settled on the latter based February 2008. As might be imagined, it was moving rapidly on the overlap of data points. A search from 15-30 hours using the across the sky and so 13 different sets of comparison stars were 2008 data from PDO found a synodic period of 24.60 ± 0.05 h, required for the 16 February observations but only 7 for the one on which was twice as strong (0.025 versus 0.05 mag RMS fit) as the 24 February. Calibration of the multiple sets was done by a Binzel solutions. Given the considerably better RMS fit and nearly process such that the last 3-5 observations of any given set were month-long span of internally-calibrated data, I believe the 24.60 h measured again as the first few observations of the next set. This solution is the correct one. allowed matching common data points to within 0.01 mag. 2093 Genichesk. This was previously worked by Behrend et al. Acknowledgements (2008), who found a period of 11.028 h. Funding for observations at the Palmer Divide Observatory is 3086 Kalbaugh. This is follow up on work by the author in 2004 provided by NASA grant NNG06GI32G, by National Science December (Warner 2005b). The period from 2008 is virtually the Foundation grant AST-0607505, and by a Gene Shoemaker NEO same as before but the amplitude is about 0.1 mag less, likely due Grant from the Planetary Society. to the different viewing aspect. Again, there are insufficient data from other sources for a model, so additional curves are needed in References the future. Behrend, R. (2008). Observatoire de Geneve web site, 5806 Archieroy. This Hungaria was observed to complement data http://obswww.unige.ch/~behrend/page_cou.html from the author obtained in 2004 (Warner 2005a). The same period was found but the 2008 amplitude was about 0.1 mag Binzel, R.P. (1987). Icarus 72, 135-208. greater. Data from future apparitions will be needed for modeling. Warner, B.D. (2005a). Minor Planet Bulletin 32, 29-32. 6296 Cleveland. This is another Hungaria observed to complement data from previous work by the author (Warner 2006a). The Warner, B.D. (2005b). Minor Planet Bulletin 32, 54-58. synodic period for 2008 was 15.65 ± 0.01 h. However, a longer Warner, B.D. (2006a). Minor Planet Bulletin 33, 85-88. period of 31.54 h, representing a bimodal curve, cannot be ruled out. The 2006 period was 15.38 h with an amplitude of 0.20 mag. Warner, B.D., Pray, D.P., and Pravec, P. (2006b). Minor Planet Usually, that larger amplitude would tend to support to the shorter Bulletin 33, 99. period. However, the data from both apparitions had errors of ±0.03 mag or more, making a definitive solution difficult to find. Warner, B.D. (2008). Minor Planet Bulletin 35, 67-71. Complicating matters was that neither data set could be acceptably forced to fit the period of the other.
Recommended publications
  • Photometry of Asteroids: Lightcurves of 24 Asteroids Obtained in 1993–2005
    ARTICLE IN PRESS Planetary and Space Science 55 (2007) 986–997 www.elsevier.com/locate/pss Photometry of asteroids: Lightcurves of 24 asteroids obtained in 1993–2005 V.G. Chiornya,b,Ã, V.G. Shevchenkoa, Yu.N. Kruglya,b, F.P. Velichkoa, N.M. Gaftonyukc aInstitute of Astronomy of Kharkiv National University, Sumska str. 35, 61022 Kharkiv, Ukraine bMain Astronomical Observatory, NASU, Zabolotny str. 27, Kyiv 03680, Ukraine cCrimean Astrophysical Observatory, Crimea, 98680 Simeiz, Ukraine Received 19 May 2006; received in revised form 23 December 2006; accepted 10 January 2007 Available online 21 January 2007 Abstract The results of 1993–2005 photometric observations for 24 main-belt asteroids: 24 Themis, 51 Nemausa, 89 Julia, 205 Martha, 225 Henrietta, 387 Aquitania, 423 Diotima, 505 Cava, 522 Helga, 543 Charlotte, 663 Gerlinde, 670 Ottegebe, 693 Zerbinetta, 694 Ekard, 713 Luscinia, 800 Kressmania, 1251 Hedera, 1369 Ostanina, 1427 Ruvuma, 1796 Riga, 2771 Polzunov, 4908 Ward, 6587 Brassens and 16541 1991 PW18 are presented. The rotation periods of nine of these asteroids have been determined for the first time and others have been improved. r 2007 Elsevier Ltd. All rights reserved. Keywords: Asteroids; Photometry; Lightcurve; Rotational period; Amplitude 1. Introduction telescope of the Crimean Astrophysics Observatory in Simeiz. Ground-based observations are the main source of knowledge about the physical properties of the asteroid 2. Observations and their reduction population. The photometric lightcurves are used to determine rotation periods, pole coordinates, sizes and Photometric observations of the asteroids were carried shapes of asteroids, as well as to study the magnitude-phase out in 1993–1994 using one-channel photoelectric photo- relation of different type asteroids.
    [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 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]
  • The Minor Planet Bulletin 44 (2017) 142
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 2, A.D. 2017 APRIL-JUNE 87. 319 LEONA AND 341 CALIFORNIA – Lightcurves from all sessions are then composited with no TWO VERY SLOWLY ROTATING ASTEROIDS adjustment of instrumental magnitudes. A search should be made for possible tumbling behavior. This is revealed whenever Frederick Pilcher successive rotational cycles show significant variation, and Organ Mesa Observatory (G50) quantified with simultaneous 2 period software. In addition, it is 4438 Organ Mesa Loop useful to obtain a small number of all-night sessions for each Las Cruces, NM 88011 USA object near opposition to look for possible small amplitude short [email protected] period variations. Lorenzo Franco Observations to obtain the data used in this paper were made at the Balzaretto Observatory (A81) Organ Mesa Observatory with a 0.35-meter Meade LX200 GPS Rome, ITALY Schmidt-Cassegrain (SCT) and SBIG STL-1001E CCD. Exposures were 60 seconds, unguided, with a clear filter. All Petr Pravec measurements were calibrated from CMC15 r’ values to Cousins Astronomical Institute R magnitudes for solar colored field stars. Photometric Academy of Sciences of the Czech Republic measurement is with MPO Canopus software. To reduce the Fricova 1, CZ-25165 number of points on the lightcurves and make them easier to read, Ondrejov, CZECH REPUBLIC data points on all lightcurves constructed with MPO Canopus software have been binned in sets of 3 with a maximum time (Received: 2016 Dec 20) difference of 5 minutes between points in each bin.
    [Show full text]
  • Asteroid Regolith Weathering: a Large-Scale Observational Investigation
    University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved.
    [Show full text]
  • Ground-Based Visible Spectroscopy of Asteroids to Support the Development of an Unsupervised Gaia Asteroid Taxonomy A
    Ground-based visible spectroscopy of asteroids to support the development of an unsupervised Gaia asteroid taxonomy A. Cellino, Ph. Bendjoya, M. Delbo’, Laurent Galluccio, J. Gayon-Markt, P. Tanga, E.F. Tedesco To cite this version: A. Cellino, Ph. Bendjoya, M. Delbo’, Laurent Galluccio, J. Gayon-Markt, et al.. Ground-based visible spectroscopy of asteroids to support the development of an unsupervised Gaia asteroid tax- onomy. Astronomy and Astrophysics - A&A, EDP Sciences, 2020, 10.1051/0004-6361/202038246. hal-02942763 HAL Id: hal-02942763 https://hal.archives-ouvertes.fr/hal-02942763 Submitted on 12 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astronomy & Astrophysics manuscript no. TNGspectra2ndrev c ESO 2020 July 28, 2020 Ground-based visible spectroscopy of asteroids to support development of an unsupervised Gaia asteroid taxonomy A. Cellino1, Ph. Bendjoya2, M. Delbo’3, L. Galluccio3, J. Gayon-Markt3, P. Tanga3, and E. F. Tedesco4 1 INAF, Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese, Italy e-mail: [email protected] 2 Université de la Côte d’Azur - Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Campus Valrose Nice, Nice Cedex 4, France e-mail: [email protected] 3 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, CS34229, 06304, Nice Cedex 4, France e-mail: [email protected], [email protected], [email protected] 4 Planetary Science Institute, Tucson, AZ, USA e-mail: [email protected] Received ..., 2020; accepted ..., 2020 ABSTRACT Context.
    [Show full text]
  • Origin of the Near-Earth Asteroid Phaethon and the Geminids Meteor Shower
    University of Central Florida STARS Faculty Bibliography 2010s Faculty Bibliography 1-1-2010 Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower J. de León H. Campins University of Central Florida K. Tsiganis A. Morbidelli J. Licandro Find similar works at: https://stars.library.ucf.edu/facultybib2010 University of Central Florida Libraries http://library.ucf.edu This Article is brought to you for free and open access by the Faculty Bibliography at STARS. It has been accepted for inclusion in Faculty Bibliography 2010s by an authorized administrator of STARS. For more information, please contact [email protected]. Recommended Citation de León, J.; Campins, H.; Tsiganis, K.; Morbidelli, A.; and Licandro, J., "Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower" (2010). Faculty Bibliography 2010s. 92. https://stars.library.ucf.edu/facultybib2010/92 A&A 513, A26 (2010) Astronomy DOI: 10.1051/0004-6361/200913609 & c ESO 2010 Astrophysics Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower J. de León1,H.Campins2,K.Tsiganis3, A. Morbidelli4, and J. Licandro5,6 1 Instituto de Astrofísica de Andalucía-CSIC, Camino Bajo de Huétor 50, 18008 Granada, Spain e-mail: [email protected] 2 University of Central Florida, PO Box 162385, Orlando, FL 32816.2385, USA e-mail: [email protected] 3 Department of Physics, Aristotle University of Thessaloniki, 54 124 Thessaloniki, Greece 4 Departement Casiopée: Universite de Nice - Sophia Antipolis, Observatoire de la Cˆote d’Azur, CNRS 4, 06304 Nice, France 5 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Spain 6 Department of Astrophysics, University of La Laguna, 38205 La Laguna, Tenerife, Spain Received 5 November 2009 / Accepted 26 January 2010 ABSTRACT Aims.
    [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]
  • Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
    Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals.
    [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 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated.
    [Show full text]
  • A Study of Asteroid Pole-Latitude Distribution Based on an Extended
    Astronomy & Astrophysics manuscript no. aa˙2009 c ESO 2018 August 22, 2018 A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method 1 1 1 2 3 4 5 6 7 J. Hanuˇs ∗, J. Durechˇ , M. Broˇz , B. D. Warner , F. Pilcher , R. Stephens , J. Oey , L. Bernasconi , S. Casulli , R. Behrend8, D. Polishook9, T. Henych10, M. Lehk´y11, F. Yoshida12, and T. Ito12 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holeˇsoviˇck´ach 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 4 Goat Mountain Astronomical Research Station, 11355 Mount Johnson Court, Rancho Cucamonga, CA 91737, USA 5 Kingsgrove, NSW, Australia 6 Observatoire des Engarouines, 84570 Mallemort-du-Comtat, France 7 Via M. Rosa, 1, 00012 Colleverde di Guidonia, Rome, Italy 8 Geneva Observatory, CH-1290 Sauverny, Switzerland 9 Benoziyo Center for Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel 10 Astronomical Institute, Academy of Sciences of the Czech Republic, Friova 1, CZ-25165 Ondejov, Czech Republic 11 Severni 765, CZ-50003 Hradec Kralove, Czech republic 12 National Astronomical Observatory, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan Received 17-02-2011 / Accepted 13-04-2011 ABSTRACT Context. In the past decade, more than one hundred asteroid models were derived using the lightcurve inversion method. Measured by the number of derived models, lightcurve inversion has become the leading method for asteroid shape determination.
    [Show full text]
  • Acua: the AKARI/IRC Mid-Infrared Asteroid Survey
    PASJ: Publ. Astron. Soc. Japan , 1–??, c 2018. Astronomical Society of Japan. AcuA: the AKARI/IRC Mid-infrared Asteroid Survey Fumihiko Usui1, Daisuke Kuroda2, Thomas G. Muller¨ 3, Sunao Hasegawa1, Masateru Ishiguro4, Takafumi Ootsubo5, Daisuke Ishihara6, Hirokazu Kataza1, Satoshi Takita1, Shinki Oyabu6, Munetaka Ueno1, Hideo Matsuhara1, and Takashi Onaka7 1Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210 [email protected] 2Okayama Astrophysical Observatory, National Astronomical Observatory, 3037-5 Honjo, Kamogata, Asakuchi, Okayama 719-0232 3Max-Planck-Institut f¨ur Extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany 4Department of Physics and Astronomy, Seoul National University, San 56-1, Shillim-dong Gwanak-gu, Seoul 151-742, South Korea 5Astronomical Institute, Tohoku University, 6-3 Aoba, Aramaki, Aoba-ku, Sendai 980-8578 6Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, 464-8601 7Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Received 2011 February 10; accepted 2011 June 3) Abstract We present the results of an unbiased asteroid survey in the mid-infrared wavelength with the Infrared Camera (IRC) onboard the Japanese infrared satellite AKARI. About 20% of the point source events recorded in the AKARI All-Sky Survey observations are not used for the IRC Point Source Catalog (IRC- PSC) in its production process because of the lack of multiple detection by position. Asteroids, which are moving objects on the celestial sphere, remain in these “residual events”. We identify asteroids out of the residual events by matching them with the positions of known asteroids.
    [Show full text]
  • The Minor Planet Bulletin Is Open to Papers on All Aspects of 6500 Kodaira (F) 9 25.5 14.8 + 5 0 Minor Planet Study
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 32, NUMBER 3, A.D. 2005 JULY-SEPTEMBER 45. 120 LACHESIS – A VERY SLOW ROTATOR were light-time corrected. Aspect data are listed in Table I, which also shows the (small) percentage of the lightcurve observed each Colin Bembrick night, due to the long period. Period analysis was carried out Mt Tarana Observatory using the “AVE” software (Barbera, 2004). Initial results indicated PO Box 1537, Bathurst, NSW, Australia a period close to 1.95 days and many trial phase stacks further [email protected] refined this to 1.910 days. The composite light curve is shown in Figure 1, where the assumption has been made that the two Bill Allen maxima are of approximately equal brightness. The arbitrary zero Vintage Lane Observatory phase maximum is at JD 2453077.240. 83 Vintage Lane, RD3, Blenheim, New Zealand Due to the long period, even nine nights of observations over two (Received: 17 January Revised: 12 May) weeks (less than 8 rotations) have not enabled us to cover the full phase curve. The period of 45.84 hours is the best fit to the current Minor planet 120 Lachesis appears to belong to the data. Further refinement of the period will require (probably) a group of slow rotators, with a synodic period of 45.84 ± combined effort by multiple observers – preferably at several 0.07 hours. The amplitude of the lightcurve at this longitudes. Asteroids of this size commonly have rotation rates of opposition was just over 0.2 magnitudes.
    [Show full text]