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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.
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    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.
  • 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 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.