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The Minor Planet Bulletin 29 THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 31, NUMBER 2, A.D. 2004 APRIL-JUNE 29. CCD OBSERVATIONS AND PERIOD DETERMINATION photometric R (red) filter, although some observations required a OF FIFTEEN MINOR PLANETS C (clear glass) filter for an improved signal-to-noise ratio. Kevin Ivarsen In general we selected asteroids that did not have periods listed in Sarah Willis an October 2003 revision of the list of Harris (2003) and that Laura Ingleby would be near opposition at the time of observation. At the Dan Matthews beginning of this project, eleven of the asteroids had undetermined Melanie Simet periods. However, by the project’s completion asteroids 1645 Waterfield and 228 Agathe were being studied by other Department of Physics and Astronomy astronomers as posted on the CALL website Van Allen Hall (http://www.minorplanetobserver.com/astlc/default.htm). Monson University of Iowa (2004) presents a preliminary period determination for 1645 Iowa City, IA 52242 Waterfield that agrees with our data. No result for 228 had been [email protected] released at the time this paper was reviewed. (Received: 17 November Revised: 15 February) To ensure the quality and accuracy of our experimental method, we observed four asteroids with existing entries in the Harris list and confirmed their periods. These asteroids are 174 Phaedra, 354 We have determined the periods of fifteen minor planets Eleonora, 575 Renate, and 1084 Tamariwa. Asteroid 1084 using differential photometry. Eleven of these minor Tamariwa previously had two reported periods of 6.153 hours and planets had unknown periods, one had an uncertain 7.08 hours. Our initial period estimate matched the 7.08 hour period, and three had well-known periods. We observed result, although this resulted in a very noisy combined lightcurve. a minimum of two epochs for each object in order to Further analysis revealed 6.19 hours as being a much better result. construct composite lightcurves. The periods ranged We believe that the 7.08 hour period estimate can be discounted from 3.7 to 15.2 hours. The objects we report results for with a high level of confidence. are: 174 Phaedra, 228 Agathe, 342 Endymion, 354 Eleonora, 365 Corduba, 373 Melusina, 575 Renate, Information about each epoch of observation is displayed in 1084 Tamariwa, 1171 Rusthawelia, 1388 Aphrodite, Table I. Our results are summarized in Table II, and our 1501 Baade, 1544 Vinterhanseni, 1645 Waterfield, 1799 lightcurves are shown in the Appendix. Additional information Koussevitzky, and 2097 Galle. and data for all of our observations may be obtained from our website, http://phobos.physics.uiowa.edu/research/asteroids. Our results may also be found on the CALL website. We observed several minor planets from September 27 to October 21, 2003 using the Rigel Telescope (MPC Code 857; see We thank Alan Harris for his careful review of the first draft of http://phobos.physics.uiowa.edu/tech/rigel.html) at the Winer this paper. Observatory near Sonoita, Arizona (31° 39’ N 110° 37’ W). The Rigel Telescope is a robotic facility operated remotely by faculty References and students at the University of Iowa for research and educational use. We chose a site in Arizona because of the favorable seeing Harris, A. W. (2003). http://cfa-www.harvard.edu/iau/lists/Light conditions (2.5 to 3.5 arcsecond FWHM) and the number of clear curveDat.html nights per year. The telescope is scheduled nightly and controlled over the Internet. Monson, A. (2004). http://krypton.mnsu.edu/~monsoa1/welcome_files/Asteroid.htm The telescope is a 37 cm f/14 classical Cassegrain with a 16-bit CCD camera. The camera is an FLI IMG-1024 with a backside EDITOR’S NOTE: The team of Ivarsen et al. are to be illuminated CCD sensor. In this telescope configuration the congratulated for their prolific results accomplished using a camera has an image scale of 1 arcsecond per pixel. A signal to robotic telescope at a distant favorable location. Their results noise estimate for 30-second exposures is shown in Figure 1. clearly demonstrate the highly productive capabilities of such Most of the images were taken using a Johnson-Cousins systems for asteroid lightcurve work. Minor Planet Bulletin 31 (2004) 30 Table I – Observation details Table II – Asteroid rotation results Ast# Epoch Filter Exposure #Images Mag P.A.B. 174 01 Oct 03 R 15 84 13.0 Ast. Long. Lat. P.A. Range Period (H) Amp 174 11 Oct 03 R 30 38 12.8 174* 8 +10 4.0- 7.3 5.75 ±0.001 0.52 174 15 Oct 03 R 30 49 12.8 228 18 +4 3.8- 6.5 6.47 ±0.01 0.30 174 16 Oct 03 R 30 38 12.5 342 21 +5 2.8- 3.3 7.05 ±0.01 0.18 174 17 Oct 03 R 30 54 12.5 354* 352 -13 7.6-12.3 4.277 ±0.001 0.15 228 16 Oct 03 R 30 39 13.5 365 359 +1 2.3-11.1 6.354 ±0.001 0.20 228 17 Oct 03 R 30 60 13.4 373 0 0 2.5- 9.3 12.97 ±0.01 0.23 228 21 Oct 03 R 30 38 13.6 575* 359. +4 3.4- 4.4 3.678 ±0.001 0.18 342 13 Oct 03 R 30 62 12.6 1084* 20 -1 0.6- 1.7 6.19 ±0.01 0.25 342 14 Oct 03 R 30 62 12.5 1171 26 -4 1.9- 2.0 10.98 ±0.01 0.36 342 16 Oct 03 R 15 27 12.8 1388 7 -10 4.5- 8.1 11.95 ±0.01 0.50 342 19 Oct 03 R 30 58 12.8 1501 21 +1 0.6- 1.5 15.25 ±0.01 0.33 354 01 Oct 03 R 30 37 11.0 1544 9 -3 6.2- 9.3 13.7 ±0.1 0.28 354 13 Oct 03 R 30 38 11.5 1645 15 +1 3.4- 3.8 4.876 ±0.01 0.23 354 14 Oct 03 R 30 35 11.4 1799 9 -8 3.6- 7.4 6.325 ±0.001 0.37 354 16 Oct 03 R 15 14 11.5 2097 9 +5 2.8- 7.5 7.310 ±0.005 0.45 354 19 Oct 03 R 30 32 11.7 365 27 Sep 03 C 15 133 12.8 * = Existing entry in Harris List as of Oct 2003 365 28 Sep 03 R 30 56 12.3 365 16 Oct 03 R 30 42 12.6 373 29 Sep 03 R 15 68 13.6 373 13 Oct 03 R 15 23 14.0 373 14 Oct 03 R 15 16 13.6 373 15 Oct 03 R 15 44 13.9 575 27 Sep 03 C 15 131 13.7 575 28 Sep 03 R 30 54 13.8 575 29 Sep 03 R 30 69 14.1 1084 12 Oct 03 R 15 10 14.1 1084 13 Oct 03 R 15 10 13.9 1084 14 Oct 03 R 15 43 13.5 1084 17 Oct 03 R 15 67 14.1 1171 19 Oct 03 R 15 84 13.4 1171 20 Oct 03 R 15 41 13.0 1388 01 Oct 03 R 15 36 15.3 1388 02 Oct 03 R 30 31 15.4 1388 13 Oct 03 R 30 44 15.4 1388 14 Oct 03 R 30 47 15.6 1388 15 Oct 03 R 15 34 15.8 1388 19 Oct 03 R 30 45 16.0 1501 14 Oct 03 R 15 47 13.7 1501 15 Oct 03 R 15 49 13.9 1501 17 Oct 03 R 15 73 14.0 1544 13 Oct 03 R 30 55 15.2 Figure 1. Signal to noise estimate for the Rigel telescope. 1544 14 Oct 03 R 30 53 15.0 1544 15 Oct 03 R 15 35 15.0 1544 16 Oct 03 R 15 29 15.3 1544 19 Oct 03 R 30 53 15.6 1645 16 Oct 03 R 30 59 14.2 APPENDIX: 1645 17 Oct 03 C 20 100 14.4 Composite lightcurves for 15 asteroids observed at the Winer 1799 01 Oct 03 R 15 64 15.4 Observatory, September – October 2003. 1799 02 Oct 03 R 20 47 15.3 1799 16 Oct 03 R 30 38 15.7 1799 17 Oct 03 C 20 45 15.6 2097 30 Sep 03 R 30 98 14.6 2097 11 Oct 03 R 30 50 15.5 2097 15 Oct 03 R 30 50 15.4 2097 17 Oct 03 R 30 55 15.2 Minor Planet Bulletin 31 (2004) 31 Minor Planet Bulletin 31 (2004) 32 Minor Planet Bulletin 31 (2004) 33 LIGHTCURVE PHOTOMETRY OF MARS-CROSSING (Harris et al., 1989). This program allows compensation for night- ASTEROIDS 1474 BEIRA AND 3674 ERBISBUHL to-night comparison star variation by manually shifting individual night’s magnitude scales to obtain a best fit. Robert A. Koff 980 Antelope Drive West Observations and Results Bennett, CO 80102 [email protected] 1474 Beira (Received: 2 January) Beira, a Mars-crossing asteroid, was discovered August 20, 1935 by C. Jackson at Johannesburg, S. A. It is approximately 19 km in diameter. The aphelion is 4.072 AU and the perihelion is This is a report on the lightcurve measurement program 1.400 AU.
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