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

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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. No lightcurve results are reported for this object at Antelope Hills Observatory in the United States. (Harris 2004). Observations were made on six nights during the Asteroid 1474 Beira was determined to have a period of period from September 2, 2003 to November 12, 2003. During 4.184 hours ± 0.001 hours, with an amplitude of 0.18 ± the period of the investigation, the phase angle dropped from 35.5 0.02 magnitude. Asteroid 3674 Erbisbuhl exhibited a degrees to 34.0 degrees before increasing to 40.75 degrees. period of 11.28 hours ±0.01 hours and an amplitude of Exposure times for this investigation were two minutes each. 0.40 ± 0.02 magnitude. Images were taken at 2.5-minute intervals. Dark frames and flat fields were used to calibrate each image. A total of 463 observations were used in the solution. Equipment and Procedure Figure 1 shows the resulting lightcurve. The zero point of the In 2002, Antelope Hills Observatory was established as a curve is J.D. 2452887.72249. The synodic period was determined replacement for Thornton Observatory, MPC code 713. The new to be 4.184 hours with a formal error of ± 0.001 hours. The observatory is located near Bennett, Colorado at an elevation of amplitude was 0.18 ± 0.02 magnitude. 1740 meters. The observatory has obtained the MPC code H09. The equipment and instrumentation of Antelope Hills Observatory consists of an 0.25-m f/10 Meade SCT telescope, a True Technology filter wheel, and an Apogee AP47 camera, operated unbinned. The instruments are housed in a clamshell dome, and are operated remotely from the nearby house. Targets were selected from the “Potential Lightcurve Targets” on the CALL website (Warner, 2003), and further refined based on their magnitude and position in the sky. Targets were selected for which no lightcurve data had been previously reported. (Harris, 1997). Mars-crossing asteroids were given priority.

All images reported here were obtained in unfiltered light, using a clear filter with an IR cutoff of 700 nm to prevent fringing. The differential photometry was measured using the program “Canopus” by Brian Warner, which uses aperture photometry. Magnitudes were calculated using reference stars from the USNO- A 2.0 catalog. Comparison stars differed from night-to-night due Figure 1. Lightcurve of 1474 Beira, based on a period of 4.184 to movement of the asteroid. Lightcurves were prepared using hours. Ordinate is relative magnitude. “Canopus”, based on the method developed by Dr. Alan Harris Minor Planet Bulletin 31 (2004) 34

3674 Erbisbuhl LIGHTCURVE ANALYSIS OF ASTEROIDS 110, 196, 776, 804, AND 1825 Erbisbuhl is a Mars-crossing asteroid discovered September 13, 1963 by C. Hoffmeister at Sonneberg. It is approximately 25 km Donald P. Pray in diameter. The aphelion is 3.243 AU, and perihelion is 1.479 Carbuncle Hill Observatory AU. No previously observed lightcurve is reported for this object P.O. Box 946 (Harris 2004). Observations were made on three nights during the Coventry, RI 02816 period from December 17, 2003 to December 26, 2003. During [email protected] the period of the investigation, the phase angle dropped from 15.5 degrees to 11.0 degrees. Exposure times for this investigation (Received: 14 January Revised: 10 February) were two minutes each. Images were taken at 2.5-minute intervals. Dark frames and flat fields were used to calibrate each image. A total of 492 observations were used in the solution. Lightcurve period and amplitude results are reported for five asteroids observed at Carbuncle Hill Observatory Figure 2 shows the resulting lightcurve. The zero point of the during November 2003 through January 2004. The curve is J.D. 2452990.75470. The synodic period was determined following synodic periods and amplitudes were to be 11.28 hours with a formal error of ± 0.01 hours. The determined: 110 Lydia, 10.924+0.003h, 0.14+0.01m; amplitude was 0.40 ± 0.02 magnitude. In addition to the clear 196 Philomela, 8.33+0.02h, 0.10+0.02m; filter images used in the period solution, four images were taken 776 Berbericia, 7.67+0.04h, 0.26+0.01m; 804 Hispania, using V and R filters, and transformed to the standard system. 14.64+0.01h, 0.20+0.02m; 1825 Klare, 4.744+0.009h, The resultant V-R for asteroid 3647 was 0.47 with an estimated 0.75+0.02m error of ±0.05. Introduction

Carbuncle Hill Observatory, MPC code 100, is located about twenty miles west of Providence, RI, in one of the darkest spots in the state. All observations were made using an SBIG ST-10XME CCD camera, binned 3x3, coupled to a 0.35m f6.5 SCT. This combination produced an image dimension of 21x14 arc min. All observations were taken through the “clear” filter.

Most of the selected asteroids were observed as part of the A.L.P.O. Shape Modeling Program. Details of this program may be found at http://www.bitnik.com/mp/alpo/. The aim of the program is to determine the pole position, shape, rotation state and surface scattering properties of asteroids. Lightcurves generated Figure 2. Lightcurve of 3674 Erbisbuhl, based on a period of over several apparitions are generally required to make these 11.28 hours. Ordinate is relative magnitude. determinations. The four asteroids selected for this study already had previously measured periods, so it is the differences between the newly-found lightcurves and those which preceded them that is significant. Targets were also selected based on their location Acknowledgments above the local horizon, as well as for their suitability to the equipment. 1825 Klare was selected from the “Call” website’s Many thanks to Brian Warner for his continuing work on the “List of Potential Lightcurve Targets” (Warner 2003). This target CALL website and the program “Canopus”, which has made it did not have its period published in the list of “Minor Planet possible for amateurs to analyze and share lightcurve data. Lightcurve Parameters” maintained by Harris and Warner (2003).

References Image calibration via dark frames and flat field frames was performed using “MaxIm DL”. Lightcurve construction and Harris, A. W., Young, J. W., Bowell, E., Martin, L. J., Millis, R. analysis was accomplished using “Canopus” developed by Brian L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J., Warner. Differential photometry was used in all cases, and all Debehogne, H., and Zeigler, K. W. (1989). “Photoelectric measurements were corrected for light travel time. Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, pp. 171-186. Observations and Results

Harris, A. W. (2004). “Minor Planet Lightcurve Parameters”, On 110 Lydia the Minor Planet Center website: http://cfa-www.harvard .edu/iau/lists/LightcurveDat.html, or on the CALL website: Discovered by A. Borrelly at Marseille in 1870, 110 Lydia was http://www.MinorPlanetObserver.com/astlc/default.htm determined to have a synodic period of 10.924+0.003h, with an amplitude of 0.14+0.01m. 597 images taken in ten sessions Warner, B. D. (2003). “Potential Lightcurve Targets”, on the between December 2 and December 29, 2003 were used to make CALL website, http://www.MinorPlanetObserver.com/astlc/ this measurement. The lightcurve is shown in Figure 1. This default.htm period is compared to 10.927h, with an amplitude ranging between 0.10 and 0.20m, which is presented in the list of Minor Planet Lightcurve Parameters, Harris and Warner (2003). The IRAS

Minor Planet Bulletin 31 (2004) 35

Minor Planet Survey, as appears in the Small Bodies Node of maxima. If and when their shapes are determined, it should be NASA’s Planetary Data System, (henceforth IRAS V4.0), lists interesting to see what form they take. The list of Minor Planet 110 Lydia as having an assumed absolute magnitude of 7.80, a Lightcurve Parameters states this object as having a period of mean albedo of 0.181, and an effective diameter of 86 km. 7.668h with amplitude estimates between 0.13m and 0.21m. The mean albedo is stated as 0.066 with an assumed absolute magnitude of 7.68, yielding an effective diameter of 151 km, (IRAS V4.0).

Figure 1. The lightcurve of 110 Lydia. The synodic period was found to be 10.924+0.003h with an amplitude of 0.14+0.01m.

196 Philomela Figure 3. The lightcurve for 776 Berbericia. The synodic period was determined to be 7.67+0.04h with an amplitude of C.H.F. Peters discovered this asteroid in 1879 at Clinton. IRAS 0.26+0.01m. V4.0 has estimated a diameter of 136 km for this object with an assumed absolute magnitude of 6.55. During three sessions 804 Hispania between November 16 and November 23, 2003, 559 images were taken to derive a synodic period of 8.33+0.02h with an amplitude Hispania was discovered in 1915 at Barcelona by J. Comas Sola. of 0.10+0.02m. See Figure 2. During this time, the phase angle The mean albedo is listed as 0.052 with an assumed absolute changed from 8.6 to 6.3 degrees. The list of Minor Planet magnitude of 7.84, yielding an effective diameter of 157 km, Lightcurve Parameters lists this object as having a period of (IRAS V4.0). Ambiguity seems to have followed this object 8.343h, with various amplitudes between 0.07 and 0.37m. throughout the years of effort to determine its rotational lightcurve period. The list of Minor Planet Lightcurve Parameters shows a period of 14.840h, and an amplitude between 0.19 and 0.23m. However, examination of the references provided in the list show other determinations have been made in the area of 7.4h, Magnusson and Langerkvist (1991), Calabresi and Roselli (2001).

New lightcurve observations of Hispania were obtained from December 9 to December 28, 2003, during which a total of 177 images were taken during four sessions. My initial analysis showed a synodic period of 7.462+0.015h with an amplitude of

Figure 2. The lightcurve of 196 Philomela. The synodic period was found to be 8.33+0.02h with an amplitude of 0.10+0.02m.

776 Berbericia

This object was discovered at Heidelburg by A. Massinger in 1914. The synodic period was determined to be 7.67+0.04h with an amplitude of 0.26+0.01m. 386 images were taken in two sessions over a three-night span between November 24 and November 26, 2003. This asteroid is seen to have a somewhat unusual lightcurve with four maxima, although one of these is Figure 4. The lightcurve for 804 Hispania. The synodic period quite small. See Figure 3. Interestingly, it has roughly similar was found to be 14.64+0.01h with an amplitude of 0.24+0.01m. features to the lightcurve of 110 Lydia, which also shows four Minor Planet Bulletin 31 (2004) 36

0.20+0.02m. However, consultations with Robert Stevens of Acknowledgments Santana Observatory led me to revise the period upward to nearly double this. Using his much larger data set as a guide for analysis, Special thanks is given to Brian Warner for his continued help and I now derive a period of 14.64+0.01h with an amplitude of support in my development in this area of research, and for his 0.24+0.01m. However, there is a rather large hole in the curve, so continuing improvements to the program, “Canopus”. Thanks are these parameters could well change somewhat with better also given to Bob Stevens for his assistance with the solution of coverage. The lightcurve is shown in Figure 4. the 804 Hispania lightcurve.

1825 Klare References

This asteroid was discovered by K. Reinmuth at Heidelberg in Calabresi, M., and Roselli, G. (2001). “Research Note, The 1954. 438 images were taken between December 27, 2003 and Rotation Period of 804 Hispania. Some Considerations on its January 1, 2004, in five sessions. The measured synodic period Nature.” Astronomy and Astrophysics, 369, 305-307. was 4.744+0.009h with an amplitude of 0.75+0.02m. The large amplitude would suggest a highly irregular shape. It was observed Harris, Alan W., and Warner, Brian D. (2003). “Minor Planet at phase angles varying from 6 to 3.5 degrees. The lightcurve is Lightcurve Parameters”, found on the Minor Planet Center web presented in Figure 5. site: http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html.

IRAS V4.0 from NASA Small Bodies Node of the Planetary Data System, IRAS Minor Planet Survey V4.0. http://pdssbn.astro .umd.edu/nodehtml/sbdb.html

Magnusson, P., and Langerkvist, C. I. (1991). “Physical Studies of Asteroids XXII. Photoelectric Photometry of Asteroids 34, 98, 115, 174, 270, 389, 419 and 804.” Astronomy and Astrophysics Supplement Series 87, 269-275.

Stevens, R. (2004). Private communications. http://home .earthlink.net/~rdstephens/default.htm

Warner, B.D. (2003). Collaborative Asteroid Lightcurve Link (CALL) web site. http://www.MinorPlanetObserver.com/astlc/ default.htm.

Figure 5. The lightcurve for 1825 Klare. The measured synodic period was 4.744+0.009h with an amplitude of 0.75+0.02m.

LIGHTCURVE ANALYSIS FOR NUMBERED ASTEROIDS Observatory is a 0.5m f/8.1 Ritchey-Chretien telescope using a 1351, 1589, 2778, 5076, 5892, AND 6386 Finger Lakes Instruments IMG camera with Kodak KAF-1001E chip. A second instrument also in use was a 0.3m f/9.3 Schmidt- Brian D. Warner Cassegrain using an SBIG ST-9E camera. For this set of asteroids, Palmer Divide Observatory only the 0.5m scope was used. 17995 Bakers Farm Rd. Colorado Springs, CO 80908 Initial targets are determined by referring to the list of lightcurves [email protected] maintained by Dr. Alan Harris (Harris 2003), with additions made by the author to include findings posted in subsequent issues of (Received: 6 January Revised: 17 January) the Minor Planet Bulletin. In addition, reference is made to the Collaborative Asteroid Lightcurve Link (CALL) web site maintained by the author (http://www.MinorPlanetObserver The lightcurves of six numbered asteroids obtained in late .com/astlc/default.htm) where researchers can post their findings 2003 were analyzed. The following synodic periods and pending publication. MPO Canopus, a custom software package amplitudes were determined. 1351 Uzbekistania: written by the author, is used to measure the images. It uses 73.90±0.02h, 0.34±0.02m; 1589 Fanatica: 2.58±0.05h, aperture photometry with derived magnitudes determined by 0.16±0.02m; 2778 Tangshan: 3.461±0.020h, 0.25±0.03m; calibrating images against field or, preferably, standard stars. Raw 5076 Lebedev-Kumach: 3.2190±0.0005h, 0.14±0.02m; instrumental magnitudes are used for period analysis, which is (5892) 1981 YS : 10.60±0.02h, 0.26±0.03m; and (6386) 1 included in the program. The routine is a conversion of the 1989 NK : 3.1381±0.0005h, 0.08±0.02m. 1 original FORTRAN code developed by Alan Harris (Harris et al., 1989). Equipment and Procedures Note: in the following, the orbital elements are taken from the The asteroid lightcurve program at the Palmer Divide Observatory IAU MPCORB data file available at the Minor Planet Center web has been previously described in detail (Warner 2003) so only a site (ftp://cfa-ftp.harvard.edu/pub/MPCORB/). The date of summary is provided now. The main instrument at the osculation for the elements was 2453000.5. Minor Planet Bulletin 31 (2004) 37

The Phase Angle Bisector includes, among others, 48 Doris and 52 Europa. The IRAS survey (Tedesco 1989) gives an effective diameter of 64.91 ± The observation table for each asteroid gives the date, phase angle, 4.31km and mean albedo of 0.0606 ±0.0090. The IAUs and phase angle bisector longitude and latitude. The PAB was MPCORB database gives values of 9.6 and 0.15 respectively for H developed by Alan Harris and Edward Bowell. Harris states and G. The principal orbital elements for Uzbekistania are: semi- (Harris 2003a), “The significance is that the direction that bisects major axis, 3.197AU; inclination, 9.703°; and eccentricity, 0.0610. the directions to the sun and the line of sight is a best approximation to a single ‘viewing direction.’ As an extreme There were 871 data points used in the final analysis that gave a example, if you viewed a rotating ‘cigar’ from its pole it would synodic period of 73.90±0.02h and amplitude of 0.34±0.02m. have no lightcurve amplitude if the sun were also shining from the Figure 1 shows the observations phased against this period. The pole direction, but if the sun were shining at the equator (90° amplitude implies a ratio of 1.37:1 for the projected a/b axes of the phase angle), then you would see a big amplitude. Now if you assumed triaxial ellipsoid. The table below provides a summary reverse the Earth and sun positions so you are viewing from the of the individual observation runs. equator and the sun is shining on the pole, you likewise get a big amplitude, even though in this case the illuminated area is 1589 Fanatica constant, you just see different amounts of it as it rotates. The best approximation you can make to a zero phase angle viewing aspect M. Itzigsohn discovered 1589 Fanatica on 1950 September 13 at is a single line half way in between the illumination and viewing La Plata. The name is in honor of Eva Peron whose devotion and directions. This we call the ‘phase angle bisector’, since it is the enthusiasm for the people of Argentina led her to champion the line that bisects the phase angle.” cause of workers. The name literally means a fanatical woman or feminine zealot. The asteroid has been designated 1935 RD, 1937

Results CF, 1946 OE, 1950 RK, 1950 TM3, and A924 WC.

1351 Uzbekistania The H value from the MPCORB database 12.00. Using a formula provide by Harris (2003), which assumes the asteroid’s albedo Uzbekistania was discovered by G.N. Neujmin at Simeis on 1934 (0.18) and type (S) based on the semi-major axis, the approximate October 5. It’s carried the designations 1925 CA, 1928 QJ, 1931 diameter is 12 km. Kosai (1979) includes Fanatica in his group 15 FK, 1934 TF, A917 SL, and A920 FA. It’s named in honor of the along with 11 Parthenope and 17 Thetis. The principal elements (former) Uzbek Soviet Republic where the discoverer lived during are: semi-major axis, 2.417AU; inclination, 5.261°; and WW II. Kozai (1979) puts the asteroid in his group 63, which eccentricity, 0.0927.

Observations were obtained on three nights in late November and early December, with a total of 261 data points used in the final period analysis (see Figure 2). The synodic period was found to be 2.58±0.05h and the amplitude to be 0.16±0.02m, or a projected

Figure 1. The lightcurve for 1351 Uzbekistania. The synodic period is 73.9±0.02h and the amplitude 0.34±0.02m.

DATE Phase PAB 2003 Angle Long Lat Oct. 09 15.0 58.2 7.5 Figure 2. The lightcurve for 1589 Fanatica phased against a Oct. 12 14.3 58.5 7.6 Nov. 04 7.7 59.4 8.6 synodic period of 2.58±0.05h. The amplitude is 0.16±0.02m. Nov. 15 4.5 59.4 9.0 Nov. 16 4.3 59.4 9.0 DATE Phase PAB Nov. 17 4.1 59.4 9.1 2003 Angle Long Lat Nov. 19 3.8 59.4 9.1 Nov. 29 7.9 52.7 –4.1 Nov. 21 3.6 59.4 9.2 Nov. 30 8.4 52.8 –4.0 Nov. 24 3.7 59.4 9.3 Dec. 01 8.9 52.8 -4.0

Minor Planet Bulletin 31 (2004) 38 a/b ratio of 1.16:1 for the assumed triaxial ellipsoid. The table amplitude to be 0.14±0.02m. Assuming a triaxial ellipsoid, the below provides a summary of the individual observation runs. amplitude gives a ratio of 1.14:1 for the projected a/b axes. Figure 4 shows a phased plot against this period. The table below 2778 Tangshan provides a summary of the individual observation runs.

Tangshan is named for a city in the Hebei province in northern China. It was discovered at the Purple Mountain Observatory at Nanking on 1979 December 14. Its last designation was 1979 XP with its earliest designation being 1948 WL. Using the formula by Harris (2003), the approximate diameter is 8 km when using the MPCORB H value of 13.00 and albedo of 0.18. The principal elements are: semi-major axis, 2.281AU; inclination, 4.616°; and eccentricity 0.1212.

Figure 3 shows the 265 data points obtained on Nov. 26 and Nov. 28, 2003, that were used in the final period analysis. The synodic period of the lightcurve is 3.461±0.020h and its amplitude is 0.25±0.03m, which yields a projected a/b axis ratio of 1.26:1 for the assumed triaxial ellipsoid. The table below provides a summary of the individual observation runs.

Figure 4. The lightcurve for 5076 Lebedev-Kumach. The synodic period is 3.2190±0.0005h with an amplitude of 0.14±0.02m.

DATE Phase PAB 2003 Angle Long Lat Oct. 05 6.2 2.3 1.1 Nov. 15 25.8 8.8 –2.7 Nov. 25 28.3 11.6 –3.5

Figure 3. The lightcurve for 2778 Tangshan. The data is phased against a synodic period of 3.461±0.020h. The amplitude is 0.25±0.03m.

DATE Phase PAB 2003 Angle Long Lat Nov. 26 2.5 61.1 –3.4 Nov. 28 3.3 61.2 –3.3

5076 Lebedev-Kumach

Discovered by L. I. Chernykh on 1973 September 26 at Nauchnyj, Lebedev-Kumach is named for Vasilij Ivanovich Lebedev- Kumach (1898-1949), prominent poet and song-writer, known for his lyrical and patriotic verses for songs for many Soviet films. Figure 5. A phased lightcurve for (5892) 1981 YS1 using a The principal elements are: semi-major axis, 2.416AU; synodic period of 10.60±0.02h. The amplitude is 0.26±0.03m. inclination, 9.481°; and eccentricity 0.2327. Assuming an albedo of 0.18 per Harris (2003) and the H value of 13.00 from the DATE Phase PAB MPCORB data file, the approximate diameter is 8 km. 2003 Angle Long Lat Dec. 10 12.5 64.0 –7.6 Dec. 11 13.1 64.2 –7.6 Observations were obtained in October and November 2003, with Dec. 13 14.2 64.6 -7.6 150 data points used in the final period analysis. The synodic Dec. 14 14.7 64.8 -7.5 period of the lightcurve was found to be 3.2190±0.0005h and the Minor Planet Bulletin 31 (2004) 39 Acknowledgments

(5892) 1981 YS1 Thanks go to Dr. Alan Harris of the Space Science Institute for making available the source code to his Fourier Analysis program This is another discovery from Purple Mountain Observatory at and his continuing support and advice. I also thank Robert D. Nanking (1981 December 23). The asteroid has also carried the Stephens of Santana Observatory, Rancho Cucamonga, for his on- designations 1971 BS1, 1988 QG1, and 1988 UZ. Again using the going advice and support. formula from Harris (2003) and assumed albedo of 0.18, the H value of 13.60 gives an approximate diameter of 6 km. The References principal elements are: semi-major axis, 2.384AU; inclination, 4.585°; and eccentricity 0.3020. References Note: Asteroid names and discovery information are from Schmadel (1999). 358 observations obtained on four nights in December 2003 were used to find a synodic period for the lightcurve of 10.60±0.02h Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., and amplitude of 0.26±0.03m. The latter implies a ratio of 1.27:1 Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, for the projected a/b axes of a triaxial ellipsoid. Figure 5 shows a H., and Zeigler, K.W., (1989). “Photoelectric Observations of phased plot of the observations and the table below gives a Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. summary for each run. Harris, Alan W. (2003). “Minor Planet Lightcurve Parameters. (6386) 1989 NK1 On Minor Planet Center web site: http://cfa- www.harvard.edu/iau/lists/LightcurveDat.html

H.E. Holt discovered 1989 NK1 on 1989 July 10 at Palomar. It Harris, Alan W. (2003a). Private communications. has also been designated 1955 RG1 and 1991 FW4. Assuming an albedo of 0.18, based on Harris (2003), and using the H value of 12.70 from the MPCORB table, the approximate diameter is 9 km. Kozai, Y., (1979). “The dynamical evolution of the Hirayama The principal elements are: semi-major axis, 2.271AU; family.” In Asteroids (T. Geherels, Ed.) pp. 334-358. Univ. of inclination, 8.737°; and eccentricity 0.3008. Arizona Press, Tucson.

Observations were made in October and November 2003. The Schmadel, L. (1999). Dictionary of Minor Planet Names, 4th 211 data points used for analysis are shown in Figure 6 against the edition. Springer-Verlag, Heidelberg, Germany. derived synodic period of 3.1381±0.0005h. The amplitude of the curve is 0.08±0.02m. This would give a ratio of 1.08:1 for the Tedesco, E. F., Tholen, D.J., and Zellner, B. (1989). “UBV colors projected a/b axes of a triaxial ellipsoid. The table below provides and IRAS alebedos and diameters”. In Asteroids II (R.P. Binzel, the viewing aspects for each of the observation runs. T. Gehrels, and M.S. Matthews, Eds.), pp. 1090-1138. Univ. of Arizona Press, Tucson.

Warner, B. D. (2003), “Lightcurve Analysis for [Several] Asteroids”, Minor Planet Bulletin 30, 21-24.

CALL FOR OBSERVATIONS

Frederick Pilcher Figure 6. A phased lightcurve for (6386) 1989 NK1 using a Illinois College Jacksonville, IL 62650 USA synodic period of 3.1381±0.0005h. The amplitude is 0.08±0.02m. Observers who have made visual or photographic measurements DATE Phase PAB of positions of minor planets in calendar 2003 are encouraged to 2003 Angle Long Lat Oct. 15 14.9 27.1 -15.7 report them to this author on or before April 1, 2004. This will be Nov. 04 15.9 31.4 -15.4 the deadline for receipt of reports which can be included in the Nov. 10 17.9 32.8 -15.1 “General Report of Position Observations for 2003,” to be Nov. 14 19.3 33.8 -14.8 published in MPB Vol. 31, No. 3.

Minor Planet Bulletin 31 (2004) 40

PHOTOMETRY OF 804 HISPANIA, 899 JOKASTE, Date Phase PAB PAB No. 1306 SCYTHIA, AND 2074 SHOEMAKER Angle (Long.) (Lat.) Obs. 2003/10/07 4.9 16.4 9.6 130 Robert D. Stephens 2003/10/08 4.8 16.4 9.7 151 11355 Mount Johnson Court 2003/10/09 4.8 16.4 9.8 151 Rancho Cucamonga, CA 91737 USA 2003/10/12 4.9 16.4 10.0 173 [email protected] 2003/10/13 5.1 16.4 10.1 165 (Received: 19 December) Table I: Observing circumstances for 804 Hispania 899 Jokaste Results for the following asteroids (lightcurve period and amplitude) observed from Santana Observatory 899 Jokaste is a main-belt asteroid discovered August 3, 1918 by during the period September to December 2003 are M. Wolf at Heidelberg. It is probably named for a figure in the reported: 804 Hispania (14.845 ± 0.01 hours and 0.21 opera Die Fledermaus by Johann Strauss. Three hundred one mag.), 899 Jokaste (6.245 ± 0.005 hours and 0.28 mag.), observations over three sessions between November 27 and 1306 Scythia (15.05 ± 0.01 hours and 0.18 mag.), 2074 December 3, 2003 were used to derive the synodic rotational Shoemaker (57.02 ± 0.1 hours and 0.45 mag.). period of 6.245 ± 0.005 hours with an amplitude of 0.28 ± 0.02 magnitude. Table II gives the observed range of phase angles.

Santana Observatory (MPC Code 646) is located in Rancho Cucamonga, California at an elevation of 400 meters and is operated by Robert D. Stephens. Details of the equipment and reduction techniques are found in Stephens (2003) and at the author’s web site (http://home.earthlink.net/~rdstephens/ default.htm). All of the asteroids were selected from the “CALL” web site “List of Potential Lightcurve Targets” (Warner 2003). Shoemaker was selected because it is a Hungaria asteroid and because it is named in honor of Eugene Shoemaker.

804 Hispania

Discovered March 20, 1915 by J. Comas Solá at Barcelona, Hispania is a main-belt asteroid. Hispania is the Latin name of Spain. Seven hundred sixty nine observations over five sessions between October 7 and 13, 2003 were used to derive the synodic rotational period of 14.845 ± 0.01 hours with an amplitude of 0.21 ± 0.02 magnitude. Table I gives the phase angles during the observing run. Figure 2: Lightcurve of 899 Jokaste based upon a derived period of 6.245 ± 0.005 hours. Zero phase equals J.D. 2452975.801180 (corrected for light-time).

Date Phase PAB PAB No. Angle (Long.) (Lat.) Obs. 2003/11/27 1.8 67.3 1.9 104 2003/12/02 1.2 67.4 1.5 73 2003/12/03 1.6 67.4 1.4 124 Table II: Observing circumstances for 899 Jokaste 1306 Scythia

Discovered July 22, 1930 by G. N. Neuymin at Simeïs, Scthia is a main-belt asteroid. It is named for the country of the ancient Scythians, comprising parts of Europe and Asia in regions north of the Black sea and east of the Aral Sea. Its estimated size is 34 km in diameter. Three hundred eighty four observations over four sessions between September 23 and 30, 2003 were used to Figure 1: Lightcurve of 804 Hispania based upon a derived period derive the synodic rotational period of 15.05 ± 0.01 hours with an of 14.845 ± 0.01 hours. Zero phase is J.D. 2452920.867512 amplitude of 0.18 ± 0.03 magnitude. Table III gives the phase (corrected for light-time). angles during the observing run.

Minor Planet Bulletin 31 (2004) 41

Figure 3: Lightcurve of 1306 Scythia based upon a derived Figure 4: Lightcurve of 2074 Shoemaker based upon a derived period of 15.05 ± 0.01 hours. Zero phase equals J.D. period of 57.02 ± 0.10 hours. Zero phase equals J.D. 2452908.860012 (corrected for light-time). 2452929.762632 (corrected for light-time).

Date Phase PAB PAB No. Date Phase PAB PAB No. Angle (Long.) (Lat.) Obs. Angle (Long.) (Lat.) Obs. 2003/09/23 9.1 12.5 18.5 72 2003/10/15 4.9 22.1 5.7 86 2003/09/26 8.5 12.5 18.6 101 2003/10/16 4.5 22.1 5.3 82 2003/09/29 8.1 12.6 18.6 109 2003/10/17 4.2 22.0 4.9 103 2003/09/30 8.0 12.6 18.6 102 2003/10/18 4.2 22.0 4.4 81 2003/10/19 4.3 22.0 4.0 76 Table III: Observing circumstances for 1306 Scythia 2003/10/20 4.7 22.0 3.6 78 2074 Shoemaker 2003/10/21 5.1 22.0 3.2 87 2003/10/23 6.4 21.9 2.4 95 2074 Shoemaker is a Hungaria asteroid discovered by E. Helin at 2003/11/03 15.0 22.1 -2.1 34 Palomar on October 17, 1974. It is named in honor of Eugene Table IV: Observing circumstances for 2074 Shoemaker Shoemaker (1928-1997). Based upon its H value, Shoemaker is estimated to be between 4 and 9 km in size. Seven hundred twenty two observations over nine nights between October 15 and November 3, 2003 were used to derive the synodic rotational Acknowledgements period of 57.02 ± 0.10 hours with an amplitude of 0.45 ± 0.03 magnitude. Its long period made it very difficult to get adequate Many thanks to Brian Warner for his continuing work and overlap between the sessions. Each session contributed barely 10 enhancements to the software program “Canopus” which makes it percent to the lightcurve. Finally, the California wildfires, which possible for amateur astronomers to analyze and collaborate on burned to within a half a kilometer of the observatory curtailed asteroid rotational period projects and for maintaining the CALL observations until the asteroid was too low to observe. Because Web site which helps coordinate collaborative projects between the asteroid was moving so fast, each night had to be split into amateur astronomers. two sessions with different comparison stars which were corrected with zero point adjustments. Table IV gives the phase References angles during the observing run. Stephens, R. D. (2003). “Photometry of 2134 Dennispalm, 2258 Viipuri, 3678 Mongmanwai, 4024 Ronan, and 6354 Vangelis.” MPB 30, 46-48.

Stephens, R. D. (2003). http://home.earthlink.net/~rdstephens/default.htm.

Warner, B. (2003). “Potential Lightcurve Targets.” http://www.minorplanetobserver.com/astlc.targets.

Minor Planet Bulletin 31 (2004) 42

CCD PHOTOMETRY OF 1248 JUGURTHA the sum of the squares of the residuals. The resulting values were a period of 12.190 ± 0.002 hours, the additive constant for the Walter E. Worman second night was –0.0875, for the third night was –0.4719, and for Department of Physics and Astronomy the fourth night was 0.3297 magnitudes. These are reasonable as Minnesota State University Moorhead the uncertainties in the Hubble Guide Star Catalog are given to be Moorhead, MN 56563 about ± 0.4 magnitudes. The standard deviation of the residuals was 0.017 magnitudes, which is due to the amplitude difference of Michael P. Olson the last night compared to the previous three. Department of Physics North Dakota State University A period of 12.190 hours was assumed and the second through Fargo, ND 58105 fourth night data were translated to fall on the first night data to give the composite lightcurve shown in Figure 1. The time scale (Received: 8 December Revised: 11 January) is given in rotational phase with the zero corresponding to 0 hr on February 17, 2002 UT. There are clearly two maxima and two CCD observations were made of 1248 Jugurtha on four minima per rotation. The amplitude of the lightcurve is 0.827 ± nights in February and March 2002. The synodic period 0.017 magnitudes for the first day and 0.734 ± 0.017 magnitudes of rotation was found to be 12.190 ± 0.002 hours with for the last day. The phase angle during the first three days of the lightcurve amplitude evolving from 0.827 ± 0.017 to observations varied between 8.9° and 7.3°, and the last day was 0.734 ± 0.017 magnitudes. The period and large 5.4°. We believe that this phase angle change is responsible for amplitude are in agreement with previously reported the amplitude trend as less shadowing occurs on the asteroid at smaller phase angles. values. Reference Observations Koff, R.A. and Gross, J. (2002). “Lightcurve Photometry of The asteroid 1248 Jugurtha is a main-belt asteroid with semi- Asteroid 1248 Jugurtha.” MPB 29, 75-76 major axis of 2.72 AU. Koff and Gross (2002) previously reported a period of 12.1897 ±0.0001 hours with an amplitude in excess of 0.70 magnitudes. The new observations of 1248 Jugurtha we report here were made at the Paul Feder Observatory, located on the Buffalo River Site of the Minnesota State University Moorhead Regional Science Center. Data were collected on the nights of February 17, 21, 22, and March 10, 2002.

The observatory has a 16-inch computer controlled Cassegrain telescope made by DFM. The associated Photometrics Star 1 CCD camera system was used to collect data. In all, 147 images were made of the asteroid during the four nights. Of these, 141 were used in the analysis. The others were rejected because the asteroid image was too close to another star or to dawn. The exposures were 3 minutes long and typically separated by 10 minutes. No filter was used. Dark current and flat field corrections were made to the data. Three stars were used as magnitude standards for each image. The magnitudes were taken from the Guide 7 program (Hubble Guide Star Catalog). A least squares fit was done for each image and the relation between the magnitude and the log of the total count determined. The magnitude of the asteroid was then determined from this Figure 1. Rotational lightcurve for 1248 Jugurtha assuming a relationship. A photometric aperture of 11 pixels by 11 pixels was period of 12.190 hours. The V magnitude scale is approximate used and an equal sized region of the background nearby was used owing to the typical 0.4 mag. uncertainty of the Hubble Guide Star for the background correction. Catalog. Results

Times were corrected for travel time from the asteroid to the Earth and were taken to be at the mid-times for the images. Lightcurves were made for each of the four nights. Relative magnitudes from night to night were uncertain as different comparison stars were used. This was dealt with by using additive constants for the second, third and fourth night magnitudes to bring them into agreement with the first night. A single lightcurve for the four nights was then least squares fit to a Fourier series including nine harmonics. The additive constants for the second through fourth nights and the period were then adjusted so that the fit minimized

Minor Planet Bulletin 31 (2004) 43

THE MINOR PLANET OBSERVER: annual meeting in Big Bear, CA, each year. The group changed MAKING AND READING HISTORY its name in 2003 and is working towards developing a method and process – a network, if you will – to build a pool of high quality Brian Warner observers and give professionals access to that pool. This parallels Palmer Divide Observatory the work that has long be done by the American Association of 17995 Bakers Farm Rd. Variable Star Observers (AAVSO) with whom SAS is trying to Colorado Springs, CO 80908 work along with other groups. If you’d like more information on [email protected] SAS, visit their home page at http://www.socastrosci.org.

The news came in mid-October, 2003: the long lost minor planet One of the pleasures I had while out working on Hermes and other 1937 UB, also known as Hermes, had been recovered. Brian Skiff asteroids late in 2003 was to see a spectacular aurora. It’s rare to of the Lowell Observatory Near-Earth-Object Search (LONEOS) see much, if anything, from my mid-latitude location in Colorado program made the observations that sent astronomers, professional but the heightened solar activity resulted in some spectacular and amateur, scurrying to their instruments. Within a few days, shows of bright green curtains, blood red sheets, rays of all lengths radar and optical observations confirmed that the asteroid was and colors seen by those as far south as the southern tier of the actually two separate bodies rotating around one another. You can United States. Of course, one man’s treasure is another man’s read more about the recovery at http://www.lowell.edu/press_ junk. Some Canadian amateurs were quick to point out that while room/releases/recent_releases/Hermes_rls.html. the show was nice, they see such displays quite often with many so bright that the sky becomes is as if the quarter moon or more As often happens with the announcement of an NEO discovery or was present. This brought to mind a time when I was doing some recovery, there was a rush to gather as much data as possible. In visual variable star estimates and couldn’t figure out why the faint some cases, that amounted to “overkill” as the Minor Planet variable suddenly disappeared. I looked up to see almost the Center received 50 or more astrometric observations a night in the entire sky filled with sheet upon sheet of bright red aurora. I may days immediately following recovery. That’s not meant to marvel at such a display now, but I’ll also wonder if a few discourage or disparage those who did turn in the observations. hundred miles north some other amateur is cursing Mother Nature. Only to note that one wishes there could be such interest more often, even when the targets are more mundane. I’ve been reading a very well done book called “Galileo’s Daughter” by Dava Sobel (ISBN 0-8027-1343-2). It’s not new, I was one of those who jumped into the rush to get optical having been published in 1999, but if you haven’t had a chance to lightcurve data to support findings being reported by radar read it, I recommend it very highly. It’s a tremendous and imaging teams. Two teams of optical observers took the fore on touching insight into Galileo’s writings and times using in part acquiring the data and analyzing it. One was lead by Petr Pravec some or all of the 124 letters written by one of two of his at Ondrejov Observatory, of which I was a part, and Raoul daughters, both of whom he placed in a convent before their Behrend of Geneva Observatory headed the other. A total of sixteenth birthday. It’s an unfortunate part of history that his about 15 observers from Europe, Australia, and the U.S. letters to her did not survive. The mother abbess of the convent contributed data that eventually lead to the finding of an orbital destroyed them soon after Suor Maria Celeste’s death in fear of period for the pair of about 13.9h with an amplitude of 0.07m. reprisals from the Church for having the materials of a declared The analysis further indicated that the objects appear to be locked heretic. in synchronous rotation. It never ceases to amaze me that one can make such determinations for asteroids based simply on the I also managed to read – finally – Donald Yeoman’s book on changing brightness over time. The feat becomes even more comets. This time I was about two decades behind the times. I amazing when applied to eclipsing binary stars, which I’ve done think what started the reading frenzy was getting bogged down in with the aid of the program, Binary Maker by David Bradstreet. the technical side of observing. It’s been a nice diversion to learn a little more about the history and people in astronomy. It also What the episode demonstrates is the value of cooperation and meant renewing a library card that was so old and infrequently collaboration among professionals and among professionals and used that the library district didn’t think I was still alive. I was amateurs. Hermes was a difficult target, not so much because of glad to report such was the case and have rediscovered the joy of its brightness or motion across the sky but because of the low just wandering through the library during my lunch hour from amplitude of the curve and the uncertainty of the initial results. time to time. There’s something old and something new around This was one time where overwhelming the problem with data every corner just waiting to be discovered. was not a waste of time and effort but a strong necessity. With northern summer rapidly approaching, and so the asteroids Most readers of these pages don’t need to be told that pro-am dipping well south of the celestial equator, I’ll be taking more time collaborations can lead to a number of important discoveries and to read some history, and traveling to one or more meetings. I continued advancement in many aspects of astronomy. There are particularly look forward to the latter as it gives me a chance to already many such collaborations among those involved in meet with some of you and learn how to improve my observing asteroids and eclipsing binary stars. Those collaborations have and data analysis skills. I hope to see some new faces and help helped lead to some important developments in recent years and develop new cooperative efforts among professionals and will continue to do so. There are many amateurs available who amateurs. Let there be no doubt: the day of the amateur is far can and do high-level work every day (or night). The problem is from over despite the new large scopes and surveys coming on getting them tied up with professionals who can do the critical line. Clear Skies! analysis if they have the data.

Addressing this problem is just one goal of the Society for Astronomical Sciences, formerly the IAPPP-West, which holds an

Minor Planet Bulletin 31 (2004) 44

LIGHTCURVES AND ROTATIONAL PERIODS OF On 21 September 2003, three days before Beira's particularly 1474 BEIRA, 1309 HYPERBOREA, AND 2525 O'STEEN favorable opposition, the asteroid was observed in B, V, R and I bands. All frames were taken through a standard Johnson-Cousins Gordana Apostolovska set of filters. The reduction to the BVRI standard system of the Institute of Physics, Faculty of Natural Sciences asteroid magnitudes was made by means of the observations of 1000 Skopje two standards fields SA114 and PG0231+051 (Landolt, 1992).

Republic of Macedonia The atmospheric extinctions were kB=0.32±0.03, kV=0.15±0.02,

[email protected] kR=0.140±0.036 and kI=0.07±0.01. The mean values of the color indices of the asteroid were measured as: B-V=0.70±0.049, Violeta Ivanova, Galin Borisov V-I=0.687±0.012, R-I=0.314±0.006, and V-R=0.378±0.025. Institute of Astronomy, Bulgarian Academy of Sciences BG-1786 Sofia Bulgaria [email protected], [email protected]

(Received: 15 January Revised: 5 February)

The V-band lightcurves of the asteroids 1474 Beira, 1309 Hyperborea, 2525 O'Steen, and the mean color indices for 1474 Beira are presented. The CCD observations were carried out at the Bulgarian National Astronomical Observatory Rozhen (MPC Code 071). The calculated synodic periods are: 1474 Beira, 4.184±0.002h; 1309 Hyperborea, 13.95±0.02h; and 2525 O'Steen, 3.55±0.01h.

The observations we report for 1309 Hyperborea, 1474 Beira, and 2525 O'Steen were made at the Bulgarian National Astronomical Figure 1: Lightcurve of 1474 Beira based on a period of Observatory Rozhen (MPC Code 071). The data for Beira and 4.184±0.002 hours. O'Steen were obtained with an SBIG ST-8E (Kodak KAF-1602E, 1536x1024px2, 1px=9µm) CCD camera attached to a 0.50m/0.70m Schmidt telescope. A Photometrics CCD camera (CE200A-SITe, 1024x1024, 1px=24µm) was used with the 2-m RCC for observing of Hyperborea. Until our choice of these objects, there was no reported information for photometric observations of these asteroids in the list of Harris (2003).

In the preliminary reduction, images were dark and flat field subtracted. The flat field correction with precision <1% was made using twilight and dawn sky flat fields. The V-band lightcurves were derived from the differential magnitudes between the asteroid and comparison stars. Aperture photometry was performed using the software program CCDPHOT (Buie, 1998). For lightcurve analysis, we used Asteroid Catalog Software (APC) (Magnuson et al. 1990), that produces composite lightcurves, calculates rotational periods, and provides the Fourier analysis fitting procedure of the lightcurve, which we used. Figure 2: Lightcurve of 1309 Hyperborea based on a period of 13.95 0.014 hours. 1474 Beira ±

Beira is a Mars-crossing asteroid with a semi-major axis of 2.74 (1309) Hyperborea AU, eccentricity 0.49 and inclination of orbit 26.7 degrees. Beira was discovered in 1935 by C. Jackson in Johannesburg. The Hyperborea is a main-belt asteroid discovered in 1931 by G. N. Neujmin in Simeis. It has a semi-major axis of 3.20 AU, assumed diameter of Beira in the IRAS Minor Planet Survey, (Tedesco, 1992) is 39 km. The Tholen taxonomic type (Tholen, eccentricity 0.15 and inclination of orbit 10.28 degrees. The 1989) is FX. At the time of observation asteroid was at 14.6m and diameter of Hyperborea is 59 km (Tedesco, 1992). The observations of this asteroid at Rozhen were carried out in two the solar phase angle was 31.5 degrees. On 24 and 25 of August nights: 12 and 14 January 2002. On the first night, bad weather 2003, Beira was observed for about 6 hours, an interval that was more than the full lightcurve coverage. We determined the conditions permitted only 2 hours of observations. The second night of observations cover 7.5 hours of the lightcurve, which synodic period to be 4.184±0.002 hours. The amplitude of the reveals a nice maximum and very sharp minimum. Assuming a composite lightcurve, Fourier fitted of order 6, is 0.149±0.010 standard lightcurve with two pairs of symmetrical extrema we magnitude. The obtained composite lightcurve has maxima and estimate a period of 13.95±0.02 hours. The amplitude of the minima which slightly differ from each other by shape and height.

Minor Planet Bulletin 31 (2004) 45 composite lightcurve for the presented phase interval is about 0.4 Tholen, D. J., (1989). “ Asteroid taxonomic classifications.” In magnitude. Asteroids II (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp 1139-1150. Univ. Arizona Press, Tucson. (2525) O'Steen

This asteroid was discovered in 1981 by B. A. Skiff in Flagstaff at the Anderson Mesa Station. O'Steen is a main-belt asteroid with a BOOK REVIEW semi-major axis of 3.13 AU, eccentricity 0.195 and inclination of orbit 2.78 degrees. The assumed diameter of 2525 O’Steen is 106 Richard P. Binzel, Editor km (Tedesco, 1992). O'Steen was observed on 23 of September 2003. In the time of the observation the asteroid was 14m and the solar phase angle was 6.98 degrees. One night observations with a A Practical Guide to Lightcurve Photometry and duration of 6 hours covered more than one cycle of the asteroid. Analysis by Brian D. Warner. Bdw Publishing, 2003. The composite lightcurve based on a synodic period of 3.55±0.01 ISBN 0-9743849-0-9, paperback, 266 pages. (Price hours is asymmetric. The amplitude of the composite lightcurve, $30, available at www.MinorPlanetObserver.com) Fourier fitted of order 4, is 0.193±0.009 magnitude. Oh how long we have waited for a book like this! In the distant past, amateurs had to crack their way into the field of lightcurve photometry by tackling papers such as Hardie (1959) and by building their own photometers following the classic book by Frank Bradshaw Wood (1963). Several follow-on books that carried the field forward were published by Willmann-Bell, Inc., including Genet (1983) and Henden and Kaitchuck (1990). The affordability, proliferation, and enabling capabilities of CCD cameras at “amateur” observatories has opened a huge potential for new opportunities for new observers to make valuable lightcurve photometry measurements. Yet a void has existed in detailing how to get started and carry forward a program of lightcurve photometry driven by scientific curiousity.

Brian D. Warner’s Practical Guide now fills that void. It is written from the perspective of one who still remembers what it was like to start as a beginner. Thus the writing comes across in a Figure 3: Lightcurve of 2525 O'Steen based on a period of 3.55± warm and welcoming style. Much advice comes from Warner’s 0.01 hours. The Fourier fit of order 4 is presented with solid line. own experience, building upon works like Henden and Kaitchuck (1990), and it is conveyed as being told from one friend to Acknowledgments another. It is hard to imagine any new person who picks up this book with genuine interest being able to resist taking the author’s This research was supported by contract Num, NZ-904/99 with the extended hand and gently being guided forward. Warner first National Science Fund, Ministry of Education and Sciences, coaxes his readers to take the plunge by tantalizing them with the Bulgaria and by contract with the Ministry of Education and science that comes out of the observations. Those who try CCD Science, Republic of Macedonia. lightcurve photometry because of the technical challenge will do it once or twice and then move to the next challenge elsewhere. References This book’s approach is to capture you for the long term by getting you hooked on the joy and satisfaction of learning and Buie, M. W., (1998). http://www.lowell.edu/users/buie/idl contributing new scientific knowledge about our Universe. It is /ccdphot.html this common passion for new knowledge that erases barriers between “amateur” and professional astronomers. There are no Harris, A. W. (2003). “Minor Planet Lightcurve Parameters”. On barriers here. the Minor Planet Center website: http://cfa-www.harvard.edu /iau/lists/LightcurveDat.html (updated October 2003) About 40 pages of the book are devoted to communicating the fundamentals of photometry, and this is accomplished with the Landolt, A.U., (1992). “UBVRI Photometric standard stars in the clear and concise skill of a patient and expert teacher. Many magnitude range 11.5

New observers who are ready to start their own programs will find Genet, R. M. (1983). Solar System Photometry Handbook. advice on how to get off the ground and choose targets to begin Willmann-Bell, Inc., Richmond, VA. working on. Recognizing that the higher purpose is to communicate one’s results, one of the final sections of the book Hardie, R. H. (1959). “An Improved Method for Measuring describes the task and venues for publication, including the Minor Extinction.” Astrophys. J. 130, 663-669. Planet Bulletin. Many details and technical examples are saved for the Appendices, making the main body of the text smoothly Henden, A. and Kaitchuck, R. (1990). Astronomical Photometry. flowing and readable. Finally the inclusion of standard star fields, Willmann-Bell, Inc., Richmond, VA. reprinted with permission, puts some enormously useful reference material into a single accessible place. The quality and clarity of Wood, F. B. (1963). Photoelectric Astronomy for Amateurs. the printing of the standard star charts enables excellent Macmillan, New York. photocopies of these pages – for personal use and handling ease at the telescope or computer screen.

LIGHTCURVE PHOTOMETRY OPPORTUNITIES For many years, the thrust of this article has been to get APRIL – JUNE 2004 lightcurves on any object since the number of well-established lightcurve parameters was woefully small. The list of spin axis Brian D. Warner values was nearly non-existent. In recent years, there has been a Palmer Divide Observatory dramatic increase in the number of entries on both lists, which are 17995 Bakers Farm Rd. just now beginning to tell part of the tale of the true evolution of Colorado Springs, CO 80908 the asteroid system. This is no time to rest on our laurels but, with the promise of even more exciting and important discoveries to be Mikko Kaasalainen made for the want of more observations, to reinforce our Rolf Nevanlinna Institute determination. Again, let there be no doubt that observations will P.O. Box 4 (Yliopistonkatu 5, room 714) be put to use. The fear that they will be lost in the dark chasms of FIN-00014 University of Helsinki time and neglect should be put aside. Finland So that neither goal – more raw lightcurves and curves for Alan W. Harris shape/axis studies – is neglected, we’re including two lists. The Space Science Institute first contains asteroids that have no or poorly established 4603 Orange Knoll Ave. parameters. Note that this time around we’ve included a number La Canada, CA 91011-3364 with at least preliminary values, some with very long periods. These are challenging, no doubt, but no less important than a Petr Pravec passing NEO spinning several times an hour. In fact, they may be Astronomical Institute more important right now since the slow rotators are, for a large CZ-25165 Ondrejov part, the greatest mystery in the study of spin rates. Czech Republic [email protected] The second list should be of help for those with smaller instruments. They are relatively bright and so should be within Spinning “flat hamburgers”, “potatoes”, and “footballs” are often easy reach. These objects are only a small number of well done used to describe an asteroid when explaining its lightcurve. Even lightcurves away from having their shape and/or spin axis the human head can give a reasonable approximation to some resolved, or at least reasonably known. Those working objects on lightcurves – assuming the person is not bald! The point is that this list should contact co-author Mikko Kaasalainen to coordinate asteroids come in all sorts of shapes and sizes and that it’s their efforts with his and to be sure that the object has not since becoming increasingly important to determine the shapes and been observed well enough to have been modeled. orientation of the spin axis for as many asteroids as possible. Important Notes: 1) The periods that are listed should be A recent review of the known lightcurves and spin axes shows an considered preliminary. Don’t be overly influenced by them and almost certain influence of the YORP effect on the spin rates and try to force your results to the same or similar values. Let the data orientations of asteroids less than about 40km in size. The exact dictate the solution, not vice versa. 2) The Declination is actually shape, or good approximation, of the asteroid is important since for when the asteroid is brightest. In most cases, it is about the the influence of the YORP effect is most powerful when the object same for when at opposition. is highly irregular in shape.

Minor Planet Bulletin 31 (2004) 47

You’ll find a more complete list of lightcurve opportunities for the INSTRUCTIONS FOR AUTHORS current and recent quarters on the CALL web site. (http://www.MinorPlanetObserver.com/astlc/default.htm). Be The Minor Planet Bulletin is open to papers on all aspects of sure to check the link on the CALL site to planned radar minor planet study. Theoretical, observational, historical, review, observations. Optical observations are often needed to support the and other topics from amateur and professional astronomers are radar work. welcome. The level of presentation should be such as to be readily understood by most amateur astronomers. The preferred Lightcurve Opportunities language is English. All observational and theoretical papers will be reviewed by another researcher in the field prior to publication Opposition to insure that results are presented clearly and concisely. It is # Name Date Mag Dec Per Amp hoped that papers will be published within three months of receipt. 498 Tokio 4 06.2 13.4 + 8 >20. >0.36 168 Sibylla 4 06.1 12.9 - 8 23.82 >0.30 However, material submitted by the posted deadline for an issue 203 Pompeja 4 06.0 12.6 - 9 46.6 >0.10 may or may not appear in that issue, depending on available space 744 Aguntina 4 11.2 14.1 + 2 and editorial processing. 265 Anna (F) 3 30.2 13.4 -46 566 Stereoskopia 4 14.2 13.3 - 4 17. 0.08 143 Adria 4 09.2 12.7 -23 11. The MPB will not generally publish articles on instrumentation. 755 Quintilla (F) 4 17.1 13.3 - 8 Persons interested in details of CCD instrumentation should join 1605 Milankovitch 4 19.7 14.5 - 2 13.29 0.15 738 Alagasta 4 19.5 14.0 - 6 the International Amateur-Professional Photoelectric Photometry 1109 Tata 4 17.0 14.2 -16 (IAPPP) and subscribe to their journal. Write to: Dr. Arnold M. 407 Arachne 4 16.5 12.8 -22 44. 0.45 680 Genoveva 4 23.9 12.7 -10 Heiser, Dyer Observatory, 1000 Oman Drive, Brentwood, TN 863 Benkoela 5 06.7 13.9 +21 37027 (email: [email protected]). The MPB will 613 Ginevra 5 09.5 14.1 -27 16.45 0.63 carry only limited information on asteroid occultations because 1728 Goethe Link 5 12.1 14.1 -20 1143 Odysseus 5 14.0 15.0 -18 >12. 0.11 detailed information on observing these events is given in the 1994 Shane 5 18.6 14.9 -22 25.? >0.1 Occultation Newsletter published by the International Occultation 6669 Obi 5 19.2 14.2 -22 Timing Association (IOTA). Persons interested in subscribing to 1353 Maartje 5 21.3 14.4 -14 478 Tergeste 5 21.8 12.3 -18 15. 0.2 this newsletter should write to: Art Lucas. Secretary & Treasurer, 2091 Sampo 5 24.8 14.8 - 7 71.3 0.38 5403 Bluebird Trail, Stillwater, OK 74074 USA 2957 Tatsuo (F) 5 27.9 13.9 -22 ([email protected]). Astrometry measurements should be 159 Aemilia 5 30.8 12.8 -14 25. >0.2 582 Olympia 6 07.0 14.0 +20 36.0 >0.6 submitted to the IAU Minor Planet Center and are no longer being 4558 Janesick 5 28.2 14.2 -27 100. >0.11 published or reproduced in the MPB. 839 Valborg 5 26.6 13.5 -43 227 Philosophia (F) 6 02.2 12.2 -37 3089 Oujianquan (F) 6 06.1 14.0 -16 Manuscript Preparation 427 Galene 6 06.1 13.4 -28 12008 1996 TY9 (F) 5 31.1 12.7 -34 It is strongly preferred that all manuscripts be prepared using the 1246 Chaka 6 07.9 13.9 -38 >20. >0.2 780 Armenia 6 13.5 13.8 + 2 template found at: http://www.minorplanetobserver.com/astlc/ 1274 Delportia 6 16.2 13.9 -31 default.htm Manuscripts should be less than 1000 words. Longer 426 Hippo 6 17.7 12.7 -45 >32. 0.15 manuscripts may be returned for revision or delayed pending 749 Malzovia (F) 6 20.3 13.2 -19 275 Sapientia 6 21.2 12.5 -18 >20. >0.05 available space. For authors not using the template noted above, 954 Li 6 23.1 13.4 -22 14. 0.2 manuscripts may be submitted electronically as ASCII text or on 696 Leonora 6 26.3 14.0 -31 paper as a typescript. Typescripts should be typed double spaced 9601 1991 UE3 (F) 6 30.9 13.9 -29 1031 Arctica 6 30.3 14.3 + 0 51.0 >0.22 and consist of the following: a title page giving the names and 1738 Oosterhoff 6 30.2 13.7 -32 addresses of all authors (editorial correspondence will be conducted with the first author unless otherwise noted), a brief abstract not exceeding four sentences, the text of the paper, acknowledgments, references, tables, figure captions, and figures. Please compile your manuscripts in this order.

For lightcurve articles, authors are encouraged to combine as Shape/Axis Opportunities many objects together in a single article as possible. For general articles, the number of tables plus figures should not exceed two. Opposition Per # Name Date Mag Dec (h) Amp. Tables should be numbered consecutively in Roman numerals, 77 Frigga 4 04.3 12.3 -07 9.012 0.07-0.19 figures in Arabic numerals. We will typeset short tables, if 419 Aurelia 4 20.2 10.6 -14 16.709 0.08 necessary. Longer tables must be submitted in “camera ready” 5 Astraea 4 28.6 9.8 -05 16.800 0.10-0.30 3415 Danby 5 01.3 17.3 -16 2.851 0.09-0.14 format, suitable for direct publication. Font size should be large 344 Desiderata 5 06.0 9.8 -15 10.77 0.17 enough to allow for clear reproduction within the column 36 Atalante 5 10.5 13.8 -40 9.93 0.15-0.17 dimensions described below. We prefer to receive figures in 441 Bathilde 5 15.2 12.5 -23 10.447 0.13 480 Hansa 5 19.4 11.8 -19 5.324 0.29 electronic format, 300 dpi or higher quality, black markings on 1902 Shaposhnikov 5 25.5 14.5 -23 21.2 0.42 white. Because of their high reproduction cost, the MPB will not 51 Nemausa 5 28.7 10.3 -05 7.783 0.10-0.14 print color figures. Labeling should be large enough to be easily 451 Patientia 5 30.8 11.3 -14 9.727 0.05-0.10 48 Doris 5 31.9 11.6 -13 11.89 0.35 readable when reproduced to fit within the MPB column format. 276 Adelheid 6 01.7 13.4 -02 6.328 0.07-0.10 If at all possible, you are strongly encouraged to supply tables and 471 Papagena 6 05.9 11.3 -19 7.113 0.11-0.13 figures at actual size for direct reproduction. Tables and figures 76 Freia 6 09.0 13.3 -21 9.972 0.10-0.33 24 Themis 6 18.3 11.6 -24 8.374 0.09-0.14 intended for direct reproduction to occupy one-half page width 386 Siegena 6 21.7 12.1 +06 9.763 0.11 should be 8.6 cm wide, or full-page width, 17.8 cm. Size your tables and figures to fit one-half page width whenever possible.

Minor Planet Bulletin 31 (2004) 48

Limit the vertical extent of your figures as much as possible. In THE MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly general they should be 9 cm or less. journal of the Minor Planets Section of the Association of Lunar and Planetary Observers. The Minor Planets Section is directed by its References should be cited in the text such as Harris and Young Coordinator, Prof. Frederick Pilcher, Department of Physics, Illinois College, Jacksonville, IL 62650 USA ([email protected]), assisted by (1980) for one or two authors or Bowell et al. (1979) for more Lawrence Garrett, 206 River Road, Fairfax, VT 05454 USA than two authors. The reference section should list papers in ([email protected]). Richard Kowalski, 7630 Conrad St., alphabetical order of the first author’s last name. The reference Zephyrhills, FL 33544-2729 USA (qho@bitnik. com) is Associate format for a journal article, book chapter, and book are as follows: Coordinator for Observation of NEO’s, and Steve Larson, Lunar and Planetary Laboratory, 1629 E. University Blvd., University of Arizona, Harris, A.W., Young, J.W., Bowell, E., Martin, L. J., Millis, R. L., Tucson, AZ 85721 USA ([email protected]) is Scientific Advisor. Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J., The Asteroid Photometry Coordinator is Brian D. Warner, Palmer Divide Debehogne, H, and Zeigler, K. (1989). “Photoelectric Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908 USA ([email protected]). Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. The Minor Planet Bulletin is edited by Dr. Richard P. Binzel, MIT 54-410, Cambridge, MA 02139 USA ([email protected]) and is produced by Dr. Robert Pravec, P., Harris, A. W., and Michalowski, T. (2002). “Asteroid A. Werner, JPL MS 301-150, 4800 Oak Grove Drive, Pasadena, CA 91109 Rotations.” In Asteroids III (W. F. Bottke, A. Cellino, P. USA (robert.a.werner@jpl.nasa.gov). Derald D. Nye serves as the Paolicchi, R. P. Binzel, eds.) pp 113-122. Univ. Arizona Press, distributor. Tucson. The staff of the Minor Planet Section invites MPB subscribers who are not members of our parent organization (Association of Lunar and Planetary Warner, B. D. (2003). A Practical Guide to Lightcurve Observers – ALPO) to join by communicating with: Matthew L. Will, Photometry and Analysis. Bdw Publishing, Colorado Springs, A.L.P.O. Membership Secretary, P.O. Box 13456, Springfield, IL 62791- CO. 3456 ([email protected]).

Authors are asked to carefully comply with the above guidelines The contact for all subscriptions, address changes, etc. is: in order to minimize the time required for editorial tasks. Mr. Derald D. Nye Minor Planet Bulletin Submission 10385 East Observatory Drive Corona de Tucson, AZ 85641-2309 USA All material submitted for publication in the Minor Planet Bulletin ([email protected]) should be sent to the editor: Dr. Richard P. Binzel, MIT 54-410, (Telephone: 520-762-5504) Cambridge, MA 02139, USA (email: [email protected]). Authors are encouraged to submit their manuscripts electronically as email Subscription rates (per year, four issues): attachments or as ASCII text, prepared following the instructions Payment Payment by above. Alternatively, your article may be sent by post on diskette by check credit card (all diskettes must be accompanied by a complete printed copy of North America $14.00 $15.00 all material) or as a typed manuscript. When sending material by All other $19.00 $20.00 post, please include high quality original printed figures and tables that can be directly reproduced. In most cases, proofs of articles To minimize our administrative time, please consider subscribing for two will be sent to authors prior to publication. years. Checks or money orders should be in US dollars, drawn on a US bank, and made payable to the “Minor Planet Bulletin.” To pay by credit card, (Visa, Mastercard, or Discover) please send by mail your credit card number, your name exactly as it appears on the card, and the expiration date. Be sure to specify the desired length of your subscription. Credit card charges will be made through “Roadrunner Mkt, Corona AZ.” When sending your subscription order, be sure to include your full mailing address and an email address, if available. The numbers in the upper-right corner of your mailing label indicate the volume and issue number with which your current subscription expires.

Articles for submission to the MPB should be sent to the editor. All authors should follow the guidelines given in “Instructions for Authors” in issue 30–4 and also available at http://www.MinorPlanetObserver.com/ astlc/default.htm . Authors with access to Apple Macintosh or IBM-PC compatible computers are strongly encouraged to submit their manuscripts by electronic mail ([email protected]) or on diskette. Electronic submissions can be formatted either using a Microsoft Word template document available at the web page just given, or else as text-only. A printed version of the file and figures must also be sent. All materials must arrive by the deadline for each issue. We regret that diskettes cannot be returned. Visual photometry observations, positional observations, any type of observation not covered above, and general information requests should be sent to the Coordinator.

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The deadline for the next issue (31-3) is April 15, 2004. The deadline for issue 31-4 is July 15, 2004.

Minor Planet Bulletin 31 (2004)