LIGHTCURVE of 755 QUINTILLA the Nightly Zero-Point Was Determined by Imaging a Landolt Standard Field That Was Fortuitously Only a Few Degrees Away from Robert K

Home , 1021 Flammario, 1373 Cincinnati, 138 Tolosa, 1605 Milankovitch, 170 Maria, 179 Klytaemnestra

BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS

VOLUME 32, NUMBER 1, A.D. 2005 JANUARY-MARCH 1.

LIGHTCURVE OF 755 QUINTILLA The nightly zero-point was determined by imaging a Landolt standard field that was fortuitously only a few degrees away from Robert K. Buchheim the asteroid, thereby avoiding the need to account for air mass Altimira Observatory (G76) difference. The standard field was measured in B, V, and R filters 18 Altimira, Coto de Caza, CA 92679 immediately before and after imaging of the asteroid. [email protected] The asteroid imaging sequence was V-R-B-B-R-V. During this Donald Pray 25-minute imaging sequence, the asteroid’s rotational phase Carbuncle Hill Observatory (I00) orientation (referring to Figure) ranged from 0.63 to 0.73, so the Greene, Rhode Island measured absolute magnitude during this sequence is quite close [email protected] to the mean brightness (averaged over the lightcurve).

(Received: 27 June Revised: 3 September) The measured color indices were: (B-V) = 0.67 ± 0.03 (which is in good agreement with the Small Bodies Node), and (V-R) = 0.41 ± The lightcurve period of 755 Quintilla is 4.552 ± 0.001 0.03. The observed V = 14.61, when adjusted for distance from hours, with an amplitude of 0.38 mag. We also report the Earth and Sun gives a reduced magnitude of VR = 10.88 at color indices of B-V=0.67±0.03 and V-R=0.41±0.03. solar phase angle = 19.1 degrees. Using an (assumed) slope parameter G= 0.15, this implies an absolute magnitude of H= 9.9, which is in good agreement with the H= 9.81 reported by the Lightcurve observations of 755 Quintilla were made at Carbuncle Small Bodies Node. Observatory and Altimira Observatory during April 2004, on dates near the asteroid’s opposition. In June 2004, one evening was devoted to determining its color indices. At Carbuncle, we utilized a 0.35 m SCT (F/4.1) with a ST-7 ME CCD. At Altimira, we utilized a 0.28 m SCT (F/6.3) with a ST-8 XE CCD.

No previous lightcurves have been published for this asteroid. The composite lightcurve from our observations shows a rotation period of 4.552 ± 0.001 hours. Our observations, wrapped to this inferred period, are shown in the Figure. Details on our observing locations and data collection are given in Table I.

Table I: Observing Details Date Observatory Filter Exp, sec 4-10-2004 Carbuncle clear 90 4-11-2004 Carbuncle clear 90 4-22-2004 Altimira R 240 4-23-2004 Altimira R 240 4-24-2004 Altimira R 240 4-24-2004 Altimira V 240

The Small Bodies Node (http://pdssbn.astro.umd.edu/) reports a color index (B-V) = 0.688 ± 0.029 for this asteroid, and absolute magnitude H= 9.81 (using slope parameter G= 0.15). On 12 June 2004 UT, Altimira Observatory observed the asteroid in B, V, and R bands, to determine its V-magnitude and color indices. The transformation coefficients for Altimira Observatory’s instrument have been previously determined. They were updated for this project, with no significant change noted during the past 6 months. Minor Planet Bulletin 32 (2005) Available on line http://www.minorplanetobserver.com/mpb/default.htm 2

ROTATIONAL PERIODS OF 96 AEGLE, 386 SIEGENA, 544 Jetta. 396 observations over three sessions between August 390 ALMA, 544 JETTA, 2771 POLZUNOV, AND 17 and 21, 2004 were used to derive the synodic rotational period (5917) 1991 NG of 7.745 ± 0.005 hours with an amplitude of 0.50 ± 0.02 magnitude. Robert D. Stephens 11355 Mount Johnson Court 2771 Polzunov. 601 observations over eight sessions between Rancho Cucamonga, CA 91737 USA July 22 and August 6, 2004 were used to derive the synodic [email protected] rotational period of 11.66 ± 0.01 hours with an amplitude of 0.15 ± 0.03 magnitude. (Received: 9 September) (5917) 1991 NG. 318 observations over three sessions between Results for the following asteroids (lightcurve period August 9 and 11, 2004 were used to derive the synodic rotational and amplitude) observed from Santana Observatory period of 2.65 ± 0.01 hours with an amplitude of 0.38 ± 0.03 during the period July to September 2004 are reported: magnitude. 96 Aegle 13.82±0.01 hr, 0.15 mag; 386 Siegena 15.98±0.01 hr, 0.24 mag; 390 Alma 3.74±0.01 hr, 0.48 Acknowledgments mag; 544 Jetta 7.745±0.005 hr, 0.50 mag; 2771 Polzunov 11.66±0.01 hr, 0.15 mag; (5917) 1991 NG Many thanks to Brian Warner for his continuing work and 2.65±0.01 hr, 0.38 mag. enhancements to the software program “Canopus” and for maintaining the CALL Web site that helps coordinate Santana Observatory (MPC Code 646) is located in Rancho collaborative projects between amateur astronomers. Also thanks Cucamonga, California at an elevation of 400 meters and is operated by Robert D. Stephens. Details of the equipment used can be 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 2004).

96 Aegle. 639 observations over five sessions between August 26 and 30, 2004 were used to derive the synodic rotational period of 13.82 ± 0.01 hours with an amplitude of 0.15 ± 0.02 magnitude. I observed Aegle around the time of the Full Moon and used a Johnsons-Cousins red filter to increase the signal-to-noise ratio. Typical FWHM was around 3.6 arcseconds and signal-to-noise was around 120. Aegle was a very difficult target due to the shape of its lightcurve. The lightcurve is not bimodal and has a very small amplitude making it difficult to identify repeating features. It was first observed in 1980 by Harris and Young (1989). They suspected a period of around 10 hours. Wetter (1997) observed it in 1996 but was not able to refine the period. Blanco (2000) observed it in 1996 reporting a period of 10.470 hours. Finally Figure 1: Lightcurve of 96 Aegle based upon a derived period of Slivan and Roller (2001) observed it in 2001 reporting a period of 13.82 ± 0.01 hours. The 0% Phase is equal to 2453246.900133 JD 26.53 hours and a quality code of 2, while commenting on the lack (corrected for light-time). of repeating features.

386 Siegena. 579 observations over nine sessions between July 3 and 20, 2004 were used to derive the synodic rotational period of 15.98 ± .01 hours with an amplitude of 0.24 ± 0.04 magnitude. Siegena was originally reported to have a 9.763 hour period (Zappala 1982). It was observed again in 1979 and 1980 Harris and Young (1989). The resulting period was inconclusive but consistent with the Zappala period. The amplitude in 1979 was about 0.1 magninudes and somewhat higher in 1980; both far less than it appears in 2004. Since the resulting period is almost exactly two thirds of the Earth’s rotation, it was not possible to get a complete composite lightcurve in the short summer nights. However, both of the minima were repeatedly observed lending confidence in the resulting period.

390 Alma. 209 observations on August 7 and 8, 2004 were used to derive the synodic rotational period of 3.74 ± 0.01 hours with an amplitude of 0.48 ± 0.03 magnitude. Figure 2: Lightcurve of 386 Siegna based upon a derived period of 15.98 ± 0.01 hours. The 0% Phase is equal to 2453199.800670 JD (corrected for light-time).

Minor Planet Bulletin 32 (2005) 3 to Stephen Slivan who reran his 96 Aegle data against this new Stephens, R. D. (2004). period. http://home.earthlink.net/~rdstephens/default.htm.

References Warner, B. (2004). “Potential Lightcurve Targets”. http://www.minorplanetobserver.com/astlc.targets. Blanco, C., Martino, M. D. and Riccioli, D. (2000). “New rotational periods of 18 asteroids”. Planetary and Space Science Wetter, C. J. (1997). “CCD photometry of asteroids at the U. S. 48, 271-284. Air Force Academy Observatory during 1996”. Minor Planet Bulletin 24, 32. Harris, A. W., and Young, J. (1989). “Asteroid lightcurve observations from 1979-1981” Icarus 81, 314-364. Zappala, V., Scaltriti, F., Lagervist, C., Rickman, H., and Harris, A. W., (1982). “Photometric photometry of asteroids 33 Slivan, S., and Roller, E., (2001). “New lightcurve observations of Polyhymnia and 386 Siegena”. Icarus 52, 196-201. 96 Aegle”. Minor Planet Bulletin 28, 69-71.

Stephens, R. D. (2003). “Photometry of 2134 Dennispalm, 2258 Viipuri, 3678 Mongmanwai, 4024 Ronan, and 6354 Vangelis”. Minor Planet Bulletin 30(3), 46-48

Figure 3: Lightcurve of 390 Alma based upon a derived period of Figure 5: Lightcurve of 2771 Polzunov based upon a derived 3.74 ± 0.01 hours. The 0% Phase is equal to 2453224.962753 JD period of 11.66 ± 0.01 hours. The 0% Phase is equal to (corrected for light-time). 2453216.821233 JD (corrected for light-time).

Figure 4: Lightcurve of 544 Jetta based upon a derived period of Figure 6: Lightcurve of (5917) 1991 NG based upon a derived 7.745 ± 0.005 hours. The 0% Phase is equal to 2453234.785610 period of 2.65 ± 0.01 hours. The 0% Phase is equal to JD (corrected for light-time). 2453228.781523 JD (corrected for light-time).

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LIGHTCURVE ANALYSIS FOR ASTEROIDS 242 Kriemhild. Discovered by J. Palisa at Vienna on 1884 Sept. 242, 893, 921, 1373, 1853, 2120, 2448, 3022, 6490, 6517, 22, Kriemhild is a main-belt (IIIb) member. The IRAS study 7187, 7757, AND 18108 (Tedesco 1989) gives a diameter of 38±2 km with an albedo 0.159±0.019. The 0.35m SCT and FLI 1001E system were used Brian D. Warner for unfiltered observations on Aug. 8, and 12-16. Palmer Divide Observatory 17995 Bakers Farm Rd. 893 Leopoldina. Originally carrying the designation 1935 OL, this Colorado Springs, CO 80908 asteroid was discovered by M. Wolf at Heidelberg on 1918 May [email protected] 31. Tholen (1989) classifies it as taxonomic type XF. The IRAS survey (Tedesco 1989) gives a diameter of 76±4 km and albedo of (Received: 7 September) 0.005±0.006. The orbital elements make Leopoldina a main-belt IIIb member. The 0.25m SCT with ST-9 were used for unfiltered observations on Aug. 4, 8, and 12-15. Lightcurves of thirteen asteroids were obtained in mid- 2004 and the following synodic periods and amplitudes 921 Jovita. Discovered on 1919 Sept. 4 at Heidelberg by K. were determined: 242 Kriemhild: 4.543±0.005h, Reinmuth, Jovita was previously designated 1976 WM. Kozai 0.08±0.02m; 893 Leopoldina: 10.51±0.01h, 0.35±0.02m; (1979) puts the asteroid in his family 67 while the orbital elements 921 Jovita: 15.64±0.02h, 0.12±0.02m; 1373 Cincinnati: make it a main-belt IIIb member. The IRAS survey (Tedesco 5.28±0.01h, 0.14±0.02m; 1853 McElroy: 8.01±0.01h, 1989) gives a diameter of 58±2 km and albedo of 0.030±0.003. 0.20±0.03m; 2120 Tyumenia: 2.7690±0.0005h, 0.33± The 0.25m SCT and ST-9 were used to obtain R filter 0.02m; 2448 Sholokhov: 10.065±0.005h, 0.63±0.03m; observations on Aug. 28-30 and Sept. 1-3. 3022 Dobermann: 10.32±0.01h, 0.85±0.03m; (6490) 1991 NR2: 4.468±0.005h, 0.26±0.02m; (6517) 1990 BW: 1373 Cincinnati. Named after the city in Ohio, Cincinnati was 8.642±0.005h, 0.64±0.03m; 7187 Isobe: 2.440±0.002h, discovered on 1935 Aug. 30 by E. Hubble at Mount Wilson. Initial 0.24±0.03m; (7757) 1990 KO: 5.97±0.01h, 0.13±0.02m; observations using the 0.5m Ritchey-Chretien and FLI SITe (18108) 2000 NT5: 2.912±0.005h, 0.15±0.02m. camera indicated a long period or at least one that would be difficult for a single station to resolve. Furthermore, the data from Equipment and Procedures each session was sparse at times because of contamination from field stars. The assistance of the group of observers working with The asteroid lightcurve program at the Palmer Divide Observatory Dr. Raoul Behrend of Geneva Observatory was requested. Rene has been previously described in detail (Warner 2003) so only a Roy attempted runs on two occasions but both also suffered from summary is provided now. The observatory uses three instruments field star contamination. Regardless, Behrend’s attempt at analysis under automated control to obtain lightcurves during unattended and a conversation with another observer regarding comparisons sessions. This has greatly increased productivity. The systems in stars too close to saturation lead to remeasuring all the images use are: a 0.5m f/8.1 Ritchey-Chretien telescope using a Finger taken on Aug. 21-26. The synodic period was then found to be Lakes Instruments IMG camera with either a SITe TK-1024 or 5.28±0.01h with an amplitude of 0.14±0.02m. The curve is not the Kodak 1001E chip; a 0.35m f/9.1 SCT using an FLI IMG with typical bimodal shape. However, barring additional observations Kodak 1001E chip; and a 0.25 f/10.1 SCT combined with an to the contrary, the solution provides a reasonable fit to the data. SBIG ST-9E camera. Almost all observations are unfiltered, with some being in R, especially when the moon is near full to help 1853 McElroy. McElroy was discovered by Goethe Link reduce sky background. Exposure times varied in order provide a Observatory on 1957 Dec. 15. Tedesco (1989) gives a diameter of sufficient S/N for a given asteroid. 21±1 km and albedo of 0.25±0.03. The asteroid is a member of the main-belt IIIb group. Unfiltered observations were made using the Initial targets are determined by referring to the list of lightcurves 0.25m SCT and ST-9 camera on August 23-26. maintained by Dr. Alan Harris (Harris 2003), with additions made by the author to include findings posted in subsequent issues of 2120 Tyumenia. This asteroid is a main-belt IIIb group member. It the Minor Planet Bulletin. In addition, reference is made to the was discovered by T. Smirnova at Nauchnyj on 1967 Sept. 9. The Collaborative Asteroid Lightcurve Link (CALL) web site IRAS survey (Tedesco 1989) gives a diameter of 41±2 km and maintained by the author (http://www.MinorPlanetObserver.com/ albedo of 0.072±0.009. The 0.35m SCT and FLI 1001E camera astlc/default.htm) where researchers can post their findings were used to make unfiltered observations on July 11-13, 27, and pending publication. MPO Canopus, a custom software package August 1. written by the author, is used to measure the images. It uses aperture photometry with derived magnitudes determined by 2448 Sholokhov. Sholokhov was discovered on 1975 Jan. 18 by L. calibrating images against field or, preferably, standard stars. Raw Chernykh at Nauchnyj. It is a main-belt IIb member. Tedesco instrumental magnitudes are used for period analysis, which is (1989) gives a diameter of 30±3km and albedo of 0.13±0.03. The included in the program and is a conversion of the original 0.35m SCT was used with the ST-9 camera for unfiltered FORTRAN code developed by Alan Harris (Harris et al., 1989). observations on June 23-24. The same telescope with the FLI 1001E camera was used for additional observations on July 3. Results 3022 Dobermann. Dobermann was discovered by Z. Vavrova at The plots for the measured asteroids are shown at the end of this Klet on 1980 Sept. 16 and was originally designated 1980 SH. article. The data is phased against the period listed in the abstract. Using an H of 13.4 and albedo of 0.180, the implied diameter is 6.5km. The asteroid is a member of the Hungaria family.

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Angeli et al. (2001) found a period of 10.42h and amplitude of something unusual with the curve, possibly a trimodal curve or 1.24m based on four nights of observations that did not provide there being a satellite. I sent my available data to Petr Pravec of full coverage of the curve. Despite having what appeared to be a Ondrejov Observatory, Czech Republic, who had Peter Kusnirak reasonable solution, the asteroid was selected for observations for observe the asteroid in addition to analyzing the available data. the chance to refine the period based on complete coverage and to Before Kusnirak could report his results, an additional night was see if the large amplitude remained at a different apparition and so obtained at the Palmer Divide Observatory that, along with help with future shape modeling. The 0.5m Ritchey-Chretien and checking the original data indicated the lightcurve showed nothing FLI SITe camera were used for R filter observations on Aug. 29- unusual. Regardless, the Kusnirak observations were merged with 30 and Sept. 1-3. The derived synodic period is slightly less than those from PDO, which helped refine the period and confirm that Angeli, 10.32±0.01h, as is the amplitude of 0.85±0.03m. the results obtained independently at the two observatories agreed to within ±0.001h.

(6490) 1991 NR2. H. E. Holt discovered this asteroid from Palomar on 1991 July 12. The orbital elements put it on the edge References of two groups, the Marian and main-belt II. Using an H of 14.1 and albedo of 0.18, the estimated diameter is 4.7km. The 0.5m References Note: Asteroid names and discovery information are Ritchey-Chretien and FLI 1001E camera were used to obtain from Schmadel (1999). unfiltered observations on August 6 and 8. Angeli, C. A., Guimaraes, T. A., Lazzaro, D., Duffard, R., (6517) 1990 BW. In addition to the reason of it having no Fernandez, S., Florczak, A., Mothe-Diniz, T., Carvano, J. M., previously known lightcurve data, this asteroid was selected for its Betzler, A. S. (2001), Astronomical. Journal 121, 2245-2252. designation, specifically, “BW” being the author’s initials. Sometimes pure science gives way to other considerations. E. F. Harris, A. W., Young, J. W., Bowell, E., Martin, L. J., Millis, R. Helin found 1990 BW at Palomar on 1990 Jan. 21. It is a Hungaria L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J., family member. The implied diameter using an H of 13.8 and Debehogne, H., and Zeigler, K. W., (1989). “Photoelectric albedo of 0.18 is 5.4km. The 0.5m Ritchey-Chretien and FLI SITe Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, camera were used to obtain unfiltered observations on July 3, 9, 171-186. and 11. Kozai, Y., (1979). “The dynamical evolution of the Hirayama 7187 Isobe. Isobe was discovered by E.F. Helin at Palomar on family.” In Asteroids (T. Geherels, Ed.) pp. 334-358. Univ of 1992 Jan. 30. Based on H=13.40 and an assumed albedo of 0.18, Arizona Press, Tucson. the diameter is 6.5km. The asteroid is a member of the Hungaria region. The 0.35m SCT and FLI 1001E were used on four Schmadel, L. (1999). Dictionary of Minor Planet Names, 4th sessions, Aug. 29-30 and Sept. 1-2. The synodic period was found edition. Springer-Verlag, Heidelberg, Germany. to be 2.440±0.002h with an amplitude of 0.24±0.03m. This puts it very near the “spin barrier” that divides monolithic versus “rubble Tedesco, E. F., Tholen, D. J., and Zellner, B. (1989). “UBV colors pile” asteroids. and IRAS alebedos and diameters”. In Asteroids II (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 1090-1138. Univ. of (7757) 1990 KO. This is another discovery of E. F. Helin at Arizona Press, Tucson. Palomar (1990 May 22). It is a Phocaea region member with an implied diameter of 7.9km, based on an H of 13.0 and albedo of Tholen, D. J. (1989). “Asteroid Taxonomic Classifications”. In 0.18. The 0.5m Ritchey-Chretien and SITe camera were used to Asteroids II (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), obtain unfiltered observations on August 8, 12, 13, 15, 16, and 18. pp. 1139-1150. Univ. of Arizona Press, Tucson. The lightcurve shows the data phased against a synodic period of 5.97±0.01h and amplitude of 0.13±0.02m. This is the “best guess” Warner, B. D. (2003). “Lightcurve Analysis for (Several) period. Plots against periods of 7.96h and 11.94h show equally Asteroids”, Minor Planet Bulletin 30, 21-24. good fits to the data and indicate a classic case of aliasing where the number of revolutions per 24-hour period – the interval between sessions – cannot be uniquely resolved. Unfortunately, short Northern Hemisphere nights and a fading asteroid prevented finding a better solution. This asteroid should be made the target of a collaborative effort among observers separated by two to four hours in longitude. Separations of six, eight, or twelve hours could likely lead to observations that cover the same part of the curve, but on different revolutions.

(18108) 2000 NT5. The LINEAR project at Socorro discovered 2000 NT5 on July 8, 2000. The orbital elements make it a typical main-belt II member. It has carried several other designations:

1984 YB4, 1998 BV15, and 1999 LS32. All three instruments were used to observe the asteroid, with each one used on a different night in the period of August 16-18. The diameter is 9km, based on an H of 12.7 and albedo of 0.18. The plot is phased against the derived synodic period of 2.912±0.005h and has an amplitude of 0.15±0.02m. Initial observations indicated the possibility of

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LIGHTCURVE ANALYSIS OF ASTEROIDS km with an assumed absolute V magnitude of 9.70, and albedo of 276, 539, 1014, 1067, 3693 AND 4774 0.0800. During six sessions between September 24 and October 8, 2004, 485 images were taken to derive a synodic period of Donald P. Pray 13.903+0.001h with an amplitude of 0.10+0.01m. See Figure 2. Carbuncle Hill Observatory During this time, the phase angle changed from 6.8 to 6.9 degrees. P.O. Box 946 Coventry, RI 02816 1014 Semphyra. 1014 Semphyra was discovered in 1924 at [email protected] Heidelberg by K. Reinmuth (IRAS V4.0). From February 12 to February 16, 2004, a total of 241 images were taken during three (Received: 15 October Revised: 18 October) sessions. I derive a period of 5.636+0.002h with an amplitude of 0.12+0.01m. The lightcurve is shown in Figure 3. The observed Lightcurve period and amplitude results are reported for phase angle range was 1.6 to 2.9 degrees. six asteroids observed at Carbuncle Hill Observatory during January 2004 — October 2004: 276 Adelheid, 1067 Lunaria. This object was discovered at Heidelburg by K. 6.315+0.002h, 0.17+0.02m; 539 Pamina, 13.903+0.001h, Reinmuth in 1926. The synodic period was determined to be 0.10+0.01m; 1014 Semphyra, 5.636+0.002h, 6.057+0.001h with an amplitude of 0.27+0.02m. 327 images were 0.12+0.01m; 1067 Lunaria, 6.057+0.001h, 0.27+0.02m; taken in ten sessions over a twenty-nine-night span between 3693 Barringer, 6.626+0.001h, 0.54+0.02m; 4774 September 4 and October 4, 2004. The assumed absolute V Hobetsu, 3.577+0.001h, 0.23+0.02m. magnitude is 10.99, and it has a Kozai family classification of 40 (IRAS V4.0). This asteroid was observed as part of Stephen Carbuncle Hill Observatory, MPC code I00, is located about Slivan’s Koronis Family study, and is a member of a control group twenty miles west of Providence, RI, in one of the darkest spots in within that study (Slivan 2004). The lighcurve is shown in Figure the state. Observations were made using two telescope/CCD 4. systems housed in separate buildings. One is an SBIG ST-10XME CCD camera, binned 3x3, coupled to a 0.35m f/6.5 SCT. The 3693 Barringer. This asteroid was discovered by E. Bowell at other consists of an SBIG ST-7ME CCD camera, binned 1x1, Flagstaff (AM) in 1982 (IRAS V4.0). 274 images were taken coupled to a 0.32m f/3 Newtonian. These systems produced image between September 2, and September 14, 2004, in six sessions. dimensions of 21x14 arc min, and 25x16 arc min, respectively. All The measured synodic period was 6.626+0.001h with an observations were taken through the “clear” filter. Image amplitude of 0.54+0.02m. The observed phase angle range was calibration via dark frames, bias frame and flat field frames was 3.3 to 4.6 degrees. The lightcurve is presented in Figure 5. performed using “MaxIm DL”. Lightcurve construction and analysis was accomplished using “Canopus” developed by Brian 4774 Hobetsu. Ueda and Kaneda discovered this asteroid in 1991 Warner. Differential photometry was used in all cases, and all at Kushiro. Hobetsu is a member of the Flora family (IRAS V4.0). measurements were corrected for light-time. It was observed between January 1 and January 25, 2004, with phase angles ranging between 3.5 and 10.4 degrees. Four sessions All targets except for 276 Adelheid were selected from the “Call” were conducted to gather 181 data points. See its lightcurve in website’s “List of Potential Lightcurve Targets” (Warner 2004). Figure 6. These asteroids did not have their rotation periods published in the list of “Minor Planet Lightcurve Parameters” maintained by Harris Acknowledgements and Warner (2003). 276 Adelheid was observed as part of the A.L.P.O. Shape Modeling Program. Details of this program may Special thanks are given to Brian Warner for his continued help be found at http://www.bitnik.com/mp/alpo/. The aim of the and support in my development in this area of research, and for his program is to determine the pole position, shape, rotation state and continuing improvements to the program, “Canopus”. Thanks are surface scattering properties of asteroids. Lightcurves generated given to Petr Pravec for his encouragement and assistance with the over several apparitions are generally required to make these solution of the 3693 Barringer lightcurve. determinations. References Results Harris, A. W., and Warner, B. D. (2003). “Minor Planet 276 Adelheid. Discovered in 1888 at Vienna by J. Palisa, 276 Lightcurve Parameters”, found on the Minor Planet Center web Adelheid was determined to have a synodic period of 6.315+ site: http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html. 0.002h, with an amplitude of 0.17+0.02m. 245 images taken in four sessions between June 13 and June 22, 2004 were used to IRAS V4.0 from NASA Small Bodies Node of the Planetary Data make this measurement. The lightcurve is shown in Figure 1. The System, IRAS Minor Planet Survey V4.0. derived period agrees well with the 6.328h value presented in the http://pdssbn.astro.umd.edu/nodehtml/sbdb.html list of Minor Planet Lightcurve Parameters, Harris and Warner (2003). The IRAS Minor Planet Survey, as appears in the Small Slivan, S. M., Koronis Family Asteroids Rotation Lightcurve Bodies Node of NASA’s Planetary Data System, (henceforth Observing Program web site. http://www.koronisfamily.com/ IRAS V4.0), lists Adelheid as having an assumed absolute V magnitude of 8.56, a mean albedo of 0.0450 ± 0.006, and an Warner, B. D. (2004). Collaborative Asteroid Lightcurve Link effective diameter of 121.60 ± 7.7 km. (CALL) web site. http://www.MinorPlanetObserver.com/astlc/default.htm. 539 Pamina. M. Wolf discovered this asteroid in 1904 at Heidelberg. IRAS V4.0 lists an estimated diameter of 53.97 ± 3.4

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Figure 1. The lightcurve of 276 Adelheid. Figure 4. The lightcurve for 1067 Lunaria.

Figure 2. The lightcurve of 539 Pamina. Figure 5. The lightcurve for 3693 Barringer.

Figure 3. The lightcurve for 1014 Semphyra. Figure 6. The lightcurve for 4774 Hobetsu.

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CLOSE MUTUAL APPROACHES OF MINOR PLANETS IN 2005 The table gives the following data: 1. Date: date and time of closest geocentric approach (in U.T.). Edwin Goffin All other information is given for this instant. Aartselaarstraat 14 2. Closest approach: gives the minimum geocentric distance (in B-2660 Hoboken (Antwerpen) seconds of arc) and the position angle (in degrees) of the nearest Belgium minor planet with respect to the farthest one. [email protected] 3. Minor planet 1: information on the nearest minor planet: • number and name visual magnitude, (Received: 4 October) • parallax in seconds of arc, • apparent motion in seconds of arc per hour, • position angle of the direction of motion in degrees. Tabulated are 39 cases where one minor planet comes to 4. Minor planet 2: information about the farthest minor planet. within 120" of another and both are magnitude 16 or The same data as for the nearest one are given. In addition the brighter. A challenge for minor planet observers! right ascension and declination (2000) are printed. 5. Sun and Moon: Here I present a list of close approaches between numbered minor • elongation of the Sun in degrees, planets larger than 40 km during 2005 where: • elongation of the Moon (degrees), • the elongation of the Sun is more than 30°, • illuminated fraction of the Moon in %. • both minor planets are brighter than visual magnitude 16, • and the minimum geocentric separation is less than 120". The author acknowledges the Computer Center of Agfa-Gevaert N.V. (Mortsel, Belgium), site of the computations.

Close mutual approaches of minor planets ======" 0 (Dist. < 120 ; El. Sun > 30 ; magn. < 16.0)

D a t e (U.T.) Min. Pos. M i n o r p l a n e t 1 M i n o r p l a n e t 2 dist. ang. N a m e Vis. Hor. Motion N a m e Vis. Hor. Motion Right Decli- Elon- Ill. mag. par. per pos. mag. par. per pos. ascens. nation gation frac. hour ang. hour ang. (2000.0) (2000.0) Sun Moon Moon

h m " 0 " "/h 0 " "/h 0 h m 0 ' 0 0 % 2005 jan 14 5 50.7 83.97 133 115 Thyra 10.26 7.07 41.33 264 383 Janina 14.15 4.49 29.22 291 8 55.21 +19 33.0 163 145 19 jan 19 19 3.2 115.19 69 1112 Polonia 15.87 3.00 16.39 144 322 Phaeo 15.04 2.83 11.84 138 12 49.76 -14 32.7 102 134 72 jan 24 13 40.7 97.38 263 162 Laurentia 15.20 2.26 41.85 63 107 Camilla 13.72 2.15 40.33 70 23 50.51 - 3 38.6 51 118 98 feb 17 15 54.4 47.38 160 270 Anahita 13.23 3.30 86.53 68 108 Hecuba 14.48 2.11 47.45 66 0 13.79 + 3 00.8 35 74 65 mar 9 18 21.9 108.11 163 527 Euryanthe 15.44 2.66 66.96 66 259 Aletheia 14.12 2.11 48.59 64 1 29.64 + 1 29.0 32 42 1

mar 9 20 9.0 34.14 291 1171 Rusthawelia 14.82 3.89 16.97 290 830 Petropolitana14.11 3.79 17.54 277 9 06.83 +18 10.6 144 152 0 mar 10 4 20.7 97.38 25 34 Circe 13.09 4.39 19.09 80 392 Wilhelmina 15.37 3.17 12.47 53 15 51.44 -16 18.0 110 107 0 mar 17 7 18.4 55.67 340 539 Pamina 14.75 3.08 70.47 77 764 Gedania 15.25 2.57 54.87 79 2 44.65 +18 56.1 47 40 45 mar 26 17 20.7 64.81 344 126 Velleda 14.27 3.22 68.23 75 82 Alkmene 14.60 2.30 41.24 75 21 02.04 -19 28.4 53 117 99 apr 2 6 22.9 42.45 55 829 Academia 15.60 3.92 28.26 120 618 Elfriede 14.26 2.85 14.43 89 7 41.00 +27 27.8 99 159 47

apr 4 5 7.4 117.00 161 37 Fides 13.00 2.68 48.04 74 82 Alkmene 14.58 2.36 38.67 75 21 11.29 -18 52.9 59 12 26 apr 17 19 18.5 43.15 157 949 Hel 14.35 4.29 22.24 102 1242 Zambesia 15.61 3.32 15.94 119 18 49.20 -34 55.3 107 142 62 apr 18 3 20.5 28.50 169 21 Lutetia 12.78 2.75 62.19 80 279 Thule 15.80 1.77 36.12 81 4 31.70 +22 03.8 41 66 65 apr 19 6 51.6 14.92 286 2 Pallas 7.86 5.69 34.59 334 410 Chloris 12.11 5.48 23.91 271 12 11.08 +17 23.0 142 35 75 apr 23 13 48.6 7.86 134 326 Tamara 11.40 8.38 61.97 249 767 Bondia 14.97 3.53 29.08 289 13 37.17 - 7 14.4 171 6 99

apr 27 14 55.8 108.34 145 186 Celuta 12.85 5.22 27.55 269 828 Lindemannia 15.34 3.79 18.05 292 12 10.61 - 1 28.8 145 76 86 may 4 22 47.0 92.51 146 799 Gudula 14.55 4.87 8.15 317 415 Palatia 14.96 3.11 11.46 281 18 08.80 -15 49.1 131 90 13 may 14 17 53.5 18.46 155 138 Tolosa 13.42 3.51 74.69 67 449 Hamburga 15.31 2.60 49.52 68 0 05.16 - 2 15.9 53 125 35 may 30 6 51.4 48.84 125 458 Hercynia 15.18 2.65 61.04 92 50 Virginia 14.87 2.60 58.07 97 7 28.10 +20 10.0 41 134 52 jun 1 10 2.6 104.56 4 393 Lampetia 13.00 3.57 73.12 71 838 Seraphina 15.41 2.96 61.16 66 0 52.96 +14 05.2 53 17 30

jun 10 19 25.1 33.44 177 223 Rosa 15.60 2.38 54.95 72 162 Laurentia 15.02 2.23 49.73 70 2 39.40 +15 01.3 37 82 15 jun 20 23 4.2 106.15 145 834 Burnhamia 13.49 5.08 6.83 275 380 Fiducia 13.72 4.77 14.06 253 14 59.73 -11 48.7 136 28 96 jul 9 17 41.4 59.29 28 301 Bavaria 15.28 3.49 40.38 117 201 Penelope 13.92 3.09 31.44 116 12 46.96 + 0 07.8 83 49 10 jul 12 0 42.3 67.30 9 425 Cornelia 15.53 2.48 60.07 110 359 Georgia 14.97 2.22 50.59 112 9 39.48 +17 17.5 31 29 25 jul 23 16 5.8 12.33 339 468 Lina 15.32 2.92 53.27 78 586 Thekla 15.10 2.63 47.13 79 3 56.38 +20 32.4 59 89 92

jul 25 15 11.3 6.68 75 446 Aeternitas 13.45 4.48 8.77 100 704 Interamnia 11.69 3.32 14.34 19 15 43.73 -28 47.6 117 120 77 aug 15 8 55.1 56.69 260 200 Dynamene 13.82 3.24 20.40 83 704 Interamnia 11.95 3.04 21.04 65 15 51.34 -27 15.3 98 29 73 sep 22 18 31.8 10.11 155 151 Abundantia 14.56 3.15 51.23 94 466 Tisiphone 14.52 2.48 37.15 107 7 41.49 +26 11.2 67 55 74 oct 2 3 5.3 64.85 290 162 Laurentia 13.97 3.73 5.48 11 1712 Angola 15.72 2.97 8.50 206 4 19.79 +23 22.4 121 107 2 oct 2 16 19.0 19.99 27 45 Eugenia 12.88 3.09 57.29 103 95 Arethusa 14.12 2.40 38.48 95 16 43.54 -17 21.4 62 71 1

oct 4 7 39.5 103.30 356 1085 Amaryllis 15.32 2.66 44.45 101 511 Davida 12.92 2.17 32.19 107 17 04.86 -18 28.8 65 56 1 oct 19 6 50.2 18.48 347 479 Caprera 14.89 3.05 54.47 106 49 Pales 13.69 2.61 44.91 112 9 56.49 +11 18.3 58 99 95 nov 2 21 52.4 111.45 6 39 Laetitia 11.13 3.62 44.31 88 76 Freia 14.53 2.32 22.81 80 20 21.94 -17 27.2 83 74 2 nov 7 2 21.2 82.99 194 253 Mathilde 14.45 4.35 74.87 86 170 Maria 14.80 3.12 45.40 73 19 50.38 -17 14.3 71 12 29 nov 22 4 52.9 26.65 57 312 Pierretta 14.36 2.65 61.39 116 365 Corduba 15.30 2.30 48.51 107 13 09.92 - 7 08.1 41 67 65

nov 22 19 24.2 40.89 200 30 Urania 13.05 2.70 58.89 114 830 Petropolitana15.42 2.20 46.98 115 13 06.34 - 8 33.0 41 60 60 dec 8 14 53.6 12.78 33 449 Hamburga 14.20 4.16 15.20 51 1390 Abastumani 15.21 3.03 15.22 15 0 24.45 - 0 56.1 108 17 52 dec 18 21 41.5 64.55 55 188 Menippe 15.10 2.79 35.32 123 1102 Pepita 15.65 2.53 29.98 119 12 18.77 -13 50.3 77 64 89 dec 31 0 12.2 26.75 24 27 Euterpe 12.01 3.38 56.01 109 358 Apollonia 15.15 2.56 40.04 106 14 11.65 -11 45.4 64 64 2

Minor Planet Bulletin 32 (2005) 11

ARCHIVING LIGHTCURVE DATA IN THE NASA allows users and others to reference the archived data in the PLANETARY DATA SYSTEM (PDS) scientific literature. PDS is also transmitting citation information to the NASA Astrophysics Data System Abstract Service, which Mark V. Sykes, David Tarico, Rose Early provides links directly back to the data in the PDS. Planetary Science Institute 1700 E. Fort Lowell, Suite 106, Readers of the Minor Planet Bulletin are invited to archive their Tucson, Arizona 85719 data in the PDS through OLAF. Online and telephone support are [email protected] available.

(Received: 30 August Revised: 18 November) OLAF was developed under a grant from the NASA Applied Information Systems Research Program. Groundbased observers may submit data to the NASA Planetary Data System using a new web-based interface, the PDS On-Line Archiving Facility (OLAF). REVISED PERIOD FOR 5036 TUTTLE The PDS is a peer-reviewed data archive in which data are sufficiently characterized so as to be useful beyond Quentin Jamieson the lifetime of the submitter. PDS data are given Daniel A. Klinglesmith III citations for reference in publications, and are widely New Mexico Tech distributed electronically. Magdalena Ridge Observatory 801 Leroy Place Groundbased observations of solar system objects play a Socorro, NM 87801 significant role in the development of mission definitions, science [email protected] goals, and the interpretation of mission data. The NASA (Received: 15 October) Planetary Data System has for years archived these data, particularly in the areas of asteroids, comets, rings and planetary atmospheres, but this has been limited by the difficulty users Our previously reported period of 5036 Tuttle (MPB understandably have learning to create required support files 31, 88) was inadvertently doubled. The correct period conforming to PDS standards detailed in a several hundred page should be 3.750 ± 0.004h. document, and the limited manpower available at PDS to make corrections to those files when submitted. In a final processing stage for Jamieson and Klinglesmith (2004, This problem has been overcome through the development of a MPB 31, 88-89) we inadvertently doubled the reported period for web-based interface in which PDS standards are imbedded in its 5036 Tuttle. The correct value should be 3.75 ± 0.004h. This software so that the user need only fill out forms and upload a correction brings the period for 5036 Tuttle in agreement with the “tar” or “gzip” file containing their data. This is the PDS On-Line value given by LeCrone et al. (2004, MPB 31, 78-80). Archive Facility, or OLAF. OLAF is able to accept data in the form of ASCII tables or FITS images (no Word, PDF, or Excel, for instance). Specialized interfaces for common data types such as time-series or spectra are included.

Time series data (e.g., lightcurves) are required to have three columns in an ASCII table - time, observable (e.g., magnitude), and uncertainty or error (optional). There should be only one table per target object. All the information about the observations is gathered in an index file (described in OLAF) or in the forms you are asked to fill out. Once submitted, the software checks for internal consistencies and, when acccessed by the PDS, automatically generates all required PDS standards-compliant support files using the information you input. So less work for you, and less work for PDS. OLAF is accessible at http://dorothy.as.arizona.edu/olaf

Because archived data are expected to be of value for many decades or longer, all data and their ancillary information submitted to the PDS undergo peer review. This ensures that all information needed for long-term understanding and use of the data is included and that the data are usable. PDS datasets are now given citations (with information provided by the submitter). Optionally, each data product (e.g., an individual spectrum or lightcurve) can also be given a citation. Citation information Figure 1: Corrected lightcurve, 5036 Tuttle, P= 3.750 ± 0.004 h.

Minor Planet Bulletin 32 (2005) 12

ASTEROID-DEEPSKY APPULSES IN 2005 The table gives the following data:

Brian D. Warner Date/Time Universal Date (MM DD) and Time of closest Palmer Divide Observatory approach 17995 Bakers Farm Rd. #/Asteroid The number and name of the asteroid Colorado Springs, CO 80908 [email protected] RA/Dec The J2000 position of the asteroid AM The approximate visual magnitude of the asteroid (Received: 11 September Revised: 26 October) Sep/PA The separation in arcseconds and the position The following list is a very small subset of the results of a search angle from the DSO to the asteroid for asteroid-deepsky appulses for 2005, presenting only the DSO The DSO name or catalog designation highlights for the year based on close approaches of brighter DM The approximate total magnitude of the DSO asteroids to brighter DSOs. The complete set of predictions is Type The type of DSO: OC = Open Cluster; GC = available at Globular Cluster; G = Galaxy http://www.minorplanetobserver.com/htms/dso_appulses.htm SE/ME The elongation in degrees from the sun and moon respectively For any event not covered, the Minor Planet Center's web site at MP The phase of the moon: 0 = New, 1.0 = Full. http://scully.harvard.edu/~cgi/CheckMP Positive = waxing; Negative = waning allows you to enter the location of a suspected asteroid or supernova and check if there are any known targets in the area.

Date UT # Name RA Dec AM Sep PA DSO DM Type SE ME MP ------01 03 18:40 804 Hispania 8 07.39 +39 12.3 12.5 40 192 NGC 2528 12.6 G 158 79 -0.495 01 13 15:05 133 Cyrene 9 40.50 +14 55.3 12.9 16 10 NGC 2954 12.4 G 151 165 0.141 03 06 02:01 204 Kallisto 19 44.95 -14 47.8 13.8 176 165 NGC 6822 8.8 G 50 14 -0.241 03 07 16:40 13 Egeria 11 58.98 +25 12.4 10.1 97 191 NGC 4022 13.0 G 157 139 -0.100 03 09 05:01 13 Egeria 11 57.35 +25 16.1 10.1 248 10 NGC 3987 12.9 G 157 156 -0.019 03 11 21:32 26 Proserpina 18 24.50 -24 52.4 12.5 23 182 M28 6.9 GC 76 96 0.030 03 13 14:47 250 Bettina 10 20.63 +25 25.7 12.0 197 172 NGC 3209 12.7 G 151 112 0.127 03 14 23:29 38 Leda 2 28.15 +19 38.8 13.5 174 344 NGC 935 12.9 G 47 12 0.236 04 03 18:35 925 Alphonsina 12 35.55 -39 57.5 12.3 214 192 NGC 4507 12.1 G 145 97 -0.303 04 07 09:26 206 Hersilia 18 31.59 -19 14.0 13.9 63 350 M25 4.6 OC 100 82 -0.026 04 13 17:37 545 Messalina 17 38.29 -37 33.1 13.8 86 55 Cr 338 8.0 OC 117 170 0.239 04 15 20:20 247 Eukrate 21 31.47 -38 32.8 13.8 191 352 NGC 7075 12.7 G 75 150 0.429 05 02 05:56 118 Peitho 9 46.80 +22 01.0 13.6 3 33 NGC 2991 12.6 G 100 175 -0.387 05 05 23:20 694 Ekard 23 23.78 + 9 39.7 13.4 49 335 NGC 7648 13.0 G 51 24 -0.063 06 03 11:20 1365 Henyey 16 17.02 -22 58.5 13.4 31 28 M80 7.2 GC 173 146 -0.117 06 30 05:25 410 Chloris 12 26.49 + 8 52.8 13.0 15 219 NGC 4411A 12.7 G 84 153 -0.343 07 04 17:29 563 Suleika 23 37.63 -15 10.6 13.1 226 197 NGC 7717 13.0 G 113 95 -0.030 07 05 00:34 179 Klytaemnestra 2 27.91 +20 19.7 13.6 20 159 NGC 930 12.4 G 62 45 -0.021 07 06 06:43 201 Penelope 12 44.42 + 0 26.6 13.9 158 206 UGC 7911 12.9 G 86 88 -0.001 07 07 03:45 35 Leukothea 10 08.38 +12 17.5 13.7 33 205 UGC 5470 10.2 G 45 38 0.006 07 09 20:27 393 Lampetia 1 59.36 +18 53.6 13.0 208 166 NGC 770 12.9 G 73 109 0.100 07 11 20:42 179 Klytaemnestra 2 37.43 +21 04.8 13.6 74 161 NGC 992 12.6 G 66 124 0.240 07 13 00:29 218 Bianca 12 13.91 + 7 12.4 13.4 25 21 NGC 4191 12.8 G 70 7 0.341 07 29 18:29 123 Brunhild 23 48.92 + 4 10.8 13.4 117 66 NGC 7757 12.7 G 127 57 -0.332 07 30 05:01 287 Nephthys 2 39.30 + 6 32.8 12.9 47 358 NGC 1026 12.6 G 88 25 -0.291 07 31 09:05 393 Lampetia 2 28.54 +20 12.9 12.9 249 172 NGC 938 12.4 G 87 35 -0.193 08 01 22:13 674 Rachele 12 19.74 + 5 58.1 13.2 277 212 NGC 4269 12.9 G 53 87 -0.091 08 02 14:51 247 Eukrate 21 59.77 -43 16.7 12.2 138 348 NGC 7162 12.7 G 151 141 -0.057 08 04 16:25 10 Hygiea 12 53.03 - 9 10.8 11.1 74 20 NGC 4776 13.0 G 64 69 -0.002 08 05 10:08 686 Gersuind 0 07.33 +27 41.8 12.7 27 115 NGC 1 12.9 G 117 118 0.002 08 05 23:18 397 Vienna 2 03.62 +24 03.2 13.1 49 161 UGC 1551 12.5 G 96 105 0.008 08 28 01:50 247 Eukrate 21 24.84 -42 33.3 12.2 280 209 NGC 7057 12.6 G 145 129 -0.356 08 30 09:39 241 Germania 14 42.94 -18 24.8 13.6 138 13 NGC 5726 12.8 G 67 115 -0.164 08 30 11:57 173 Ino 6 03.14 +10 30.4 12.8 265 7 NGC 2141 9.4 OC 67 27 -0.157 09 05 23:01 925 Alphonsina 14 06.99 -30 00.8 13.9 46 188 NGC 5464 13.0 G 58 36 0.045 09 10 21:52 269 Justitia 17 56.79 -19 02.0 13.4 58 192 M23 5.5 OC 101 20 0.437 09 28 15:33 21 Lutetia 9 16.02 +17 34.1 13.1 242 196 NGC 2795 12.8 G 50 5 -0.199 10 05 05:06 317 Roxane 20 23.58 -19 17.2 13.7 110 350 NGC 6903 11.9 G 112 91 0.033 10 05 08:43 23 Thalia 1 01.84 - 7 38.2 10.8 135 164 NGC 337A 12.2 G 167 152 0.038 10 09 01:13 655 Briseis 1 28.87 - 0 53.1 13.4 262 333 NGC 570 12.8 G 170 116 0.310 10 25 09:52 313 Chaldaea 2 38.11 + 2 10.7 11.9 281 322 NGC 1016 11.6 G 166 89 -0.464 10 27 13:05 397 Vienna 2 28.39 +19 33.8 11.3 211 127 NGC 935 12.9 G 172 110 -0.271 10 27 15:43 809 Lundia 3 08.43 + 4 06.3 13.8 50 151 NGC 1218 12.7 G 163 107 -0.262 11 01 03:08 72 Feronia 20 53.54 -12 37.6 12.9 340 173 M72 9.4 GC 94 105 -0.008 11 24 10:19 42 Isis 21 40.34 -23 09.3 11.7 114 334 M30 7.5 GC 78 161 -0.451 11 26 01:17 212 Medea 9 05.52 +18 22.9 13.5 253 24 NGC 2749 11.8 G 110 44 -0.301 11 26 19:06 233 Asterope 19 44.92 -14 46.7 13.4 105 173 NGC 6822 8.8 G 51 109 -0.237 12 04 12:43 665 Sabine 5 28.76 +35 45.8 13.5 256 168 M38 6.4 OC 163 152 0.111

Minor Planet Bulletin 32 (2005) 13

LIGHTCURVE PERIODS FOR 1701 OKAVANGO, 689 Zita. A previous attempt at a lightcurve was published 689 ZITA, 981 MARTINA AND (14653) 1998 YV11 (Robinson, 2003) providing only an estimate in the vicinity of 4 hours. Zita is a main-belt asteroid discovered on 12 September David J Higgins 1909 by J. Palisa at Vienna. It has an absolute magnitude of 7 Mawalan Street 12.15, an albedo of 0.10 + 0.03 and an estimated diameter of 15.0 Ngunnawal, ACT, 2913 + 2.6 km. The results of the observing run conducted between Australia August 19 and August 22 show a synodic rotation of 6.425 + 0.001 hrs with amplitude of 0.50 + 0.02 mag. This was an (Received: 30 July Revised: 16 September) interesting case as the software initially resolved a period of 7.4941 hrs. After consultation with Brian Warner, some issues became apparent. First the curve was very symmetrical, second CCD photometry results from Hunters Hill Observatory the end points of the curve did not look like they would meet up in during July-August 2004 are reported for four asteroids. the original solution and third, my observations were taken 24hrs The periods and amplitudes are: 1701 Okavango, apart i.e. 24/7.5 = 3.2 which equates to one-half the period of what 13.204 + 0.004 h, 0.45 + 0.02 mag; 689 Zita, 6.425 + turned out to be the actual synodic rotation. These issues strongly 0.001 h, 0.50 + 0.02 mag; 981 Martina, 11.2675 + indicated an alias and probably meant that at least one of the 0.0028 h, 0.20 + 0.02 mag; (14653) 1998 YV11 11.3894 nights had been phased to the wrong half of the curve. The + 0.0017 h, 0.17 + 0.04mag solution was to try other periods, starting at 3.2hr x 2, for a more solid result. This lightcurve investigation was carried out at Hunters Hill Observatory located at Ngunnawal in Canberra, Australia. Targets were chosen from the list the CALL website (Warner 2004) and were observed using an 0.36m SCT at f/2.95 and Starlight Xpress MX716 CCD camera with Clear filter producing an image resolution of 1.69”/pixel. During each session, a continuous flow of 120 second (Okavango and Martina) or 180 second (Zita) integrations with a break mid session to capture dark frame were taken. Images were calibrated with darks and artificial flats and measured using MPO Canopus version 7.6.2.0. Data from all imaging sessions spanning the observing period were used. However, those images that showed interference by a field star with the measuring aperture were dropped during the measuring process.

1701 Okavango. During the Okavango investigation, several hundred images were taken but due to the relatively crowded nature of the fields in which the object was located, approximately 60% of them had to be discarded due to interference with the 981 Martina. A previous attempt at a lightcurve has been measuring aperture by background field stars. According to the attempted but not published (Harris, 2003) providing only an list of Minor Planet Lightcurves (Harris 2003), no previous estimate in the vicinity of 8 hours. Martina is a main-belt asteroid attempts have been published for Okavango. It is a main-belt discovered on 23 September 1917 by S. Beljavski at Simeis. It asteroid discovered on 06 July 1953 by J Churms at Johannesburg, has an absolute magnitude of 10.57, an albedo of 0.083 + 0.011 South Africa. It has an absolute magnitude of 10.3, an albedo of and an estimated diameter of 31.2 + 2.0 km. The results of the 0.13 + 0.10 and an estimated diameter of 29.7 + 1.7km. The observing run conducted between August 23 and September 02 results of the observing run conducted between July 8 and July 22 show a synodic rotation of 11.2675 + 0.0028 hrs with amplitude of show a synodic rotation of 13.204 + 0.004 hrs with amplitude of 0.20 + 0.02 mag. 0.45 + 0.02mag.

Minor Planet Bulletin 32 (2005) 14

(14653) 1998 YV11. No previous attempt at a lightcurve has been Acknowledgements published (Harris, 2003). 1998 YV11 is a main-belt asteroid discovered on 26 December 1998 by K. Kobayashi at Oizumi. It Thanks go to Brian Warner for his mentoring support and for the has an absolute magnitude of 13.7, and an estimated diameter of development and improvements made to the MPO Canopus 12.0 km. The results of the observing run conducted between software and for maintaining the CALL web site which advises us August 27 and September 12 show a synodic rotation of 11.3894 + on suitable targets to follow. 0.0017 hrs with amplitude of 0.17 + 0.04mag. References

Harris, A.W. (2003). “Minor Planet Lightcurve Parameters”, on Minor Planet Centre Web Site.

Warner, B.W. (2004). CALL website: http://www.minorplanetobserver.com/astlc/default.htm

Robinson, L.: (2003), http://btboar.tripod.com/lightcurves/.

PERIOD AND AMPLITUDE DETERMINATION OF period of 201 ± 1 min, or 3.35 ± 0.02 hours. From the PDM ASTEROID 10142 SAKKA solution we had to select the right period by visual criteria. We could have considered the period of 187 min because its phase S. Roland, F. Benitez, R. Salvo, A. Errico diagram looks nice, but in the 201 min period, the phase diagram Los Molinos Astronomical Observatory reaches a more consistent shape than the 187 min one. Within the Camino de Los Molinos 5769 scatter of the measurements we estimate the overall amplitude to 12400 Montevideo, Uruguay be 0.4 magnitude. The results are shown in Figure 1. [email protected] References (Received: 25 August Revised: 29 October) Gallardo & Ferraz-Mello (1997), Astr.J. 113(2), 863

At Los Molinos Astronomical Observatory, we observed Spectra software: asteroid 10142 Sakka for period and amplitude http://www.fisica.edu.uy/~gallardo/spectra1.html determination, finding the result 3.35 ± 0.02 h and 0.4 mag.

Asteroid 10142 Sakka is a main-belt asteroid discovered in 1993 that was a candidate on the December 2002 CALL lightcurve target list. At the Astronomical Observatory of Los Molinos, (Montevideo – Uruguay; IAU code 844), we observed it during the night of 13 Nov and noticed a magnitude variation in less than an hour. From 14 Nov. to 01 Dec. we took 633 images in about 17 hours total observation time. Differential photometry was done using MaxIm DL software and pre-processed images (Dark, Flat and Bias frames using the median of 15 images).

After that, using Spectra software (following Gallardo & Ferraz- Mello, 1997), we adjusted each night to a sinusoidal curve and aligned the different nights using the central axes of each fitting as a zero point magnitude. Then we ran a new fitting for all nights together searching for periods from 50 min to 330 min, this time using PDM algorithm in AVE software as well as Spectra one. The Figure 1. Lightcurve for 10142 Sakka based on a rotation period resulting period was the same using both software packages. We of 3.35 ± 0.02 h. have had already noticed, that there was an obvious periodicity of about 200 min in the lightcurve. Then we zoomed the period searching in the 160 – 240 minute interval obtaining the best fitted Minor Planet Bulletin 32 (2005) 15

LIGHTCURVE RESULTS FOR MINOR PLANETS refines the synodic period for Ljuba to be 33.8 ± 0.2 hours. The 228 AGATHE, 297 CAECILLIA, 744 AGUNTINA, amplitude was found to be 0.17 ± 0.02 magnitudes. A slope 1062 LJUBA, 1605 MILANKOVITCH, AND 3125 HAY parameter of 0.15 resulted in a reasonable fit of the data over which the phase angle changed from 2 to 5 degrees. Walter R. Cooney, Jr. 1927 Fairview Dr. 1605 Milankovitch. The lightcurve summary list of Harris (2003) Port Allen, LA 70767 lists some unpublished results for Milankovitch but no result has [email protected] appeared in the literature. This work finds a period for Milankovitch of 11.60 ± 0.05 hours with an amplitude of 0.12 ± (Received: 28 August) 0.03 magnitudes. These data were unfiltered and reference stars were not calibrated between nights.

Based on differential lightcurve photometry, we report 3125 Hay. No previous period has been published for Hay per synodic period and amplitude results for six asteroids: Harris (2003). This work finds a period of 14.31 ± 0.03 hours 228 Agathe 6.484 ± 0.01 h, 0.27 mag.; 297 Caecillia with an amplitude of 0.5 ± 0.05 magnitudes. The data were 4.163 ± 0.004 h, 0.20 mag.; 744 Aguntina 17.47 ± 0.05 unfiltered and reference stars were not calibrated between nights. h, 0.50 mag.; 1062 Ljuba 33.8 ± 0.2 h, 0.17 mag.; 1605 Milankovitch 11.60 ± 0.05 h, 0.12 mag.; 3125 Hay Acknowledgements 14.31 ± 0.03 h, 0.5 mag. The author wishes to thank Brian Warner for writing and maintaining his (CALL) website which greatly facilitates target We report results from Blackberry Observatory (MPC 929) which selection and communication to others. Thanks also to Dr. employs a 12” SCT and Apogee AP-7 CCD camera. See Cooney Richard Binzel who provided the author with a reprint of Binzel and Robinson (2002) for details on the equipment and methods. (1987) and to Dr. Alan Harris for his continuing help as mentor for Integration times of 4 minutes were used. Images were reduced this author and many more. with MIRA. Data were corrected for light travel time from the asteroids and are for mid-exposure. Dates are in UT. References

228 Agathe. Agathe was imaged with a Bessel prescription R Binzel, Richard P. (1987). “A Photoelectric Survey of 130 filter. All data for Agathe were put on a single instrumental r- Asteroids”. Icarus 72, 135-208. magnitude scale by calibrating the reference stars against each other. This allowed for the multiple night data to be phased with Cooney, W. R. Jr., and Robinson, L. (2002). “Rotation Periods only two adjustable parameters, rotation period and slope and Light Curves of Minor Planets (412) Elisabetha, (547) parameter, G. The Agathe data benefited from the fact that Praxedis, and (7564) 1988 CA”. Minor Planet Bulletin 29 (4), 78- Agathe was moving in parallel to Ljuba and was imaged each 79. night in the same field as Ljuba. The calibrations were done in order to add confidence to the period solution for the slow rotator, Harris, Alan W. (2003). “Minor Planet Light Curve Parameters”, Ljuba. The same r-instrumental calibrated reference stars were on Minor Planet Center web site: used to reduce the data for both Agathe and Ljuba. The proposed http:cfa-www.Harvard.edu/iau/lists/LightcurveDat.html. synodic period for Agathe is 6.484 ± 0.01 hours with an amplitude of 0.27 ± 0.03 magnitudes. The best fit slope parameter was 0.0 Ivarsen, K., Willis, S., Ingleby, L., Mathews, D., and Simet, M. indicating a low albedo. The phase angle varied from (2004). “CCD Observations and Period Determination of Fifteen approximately 4 to 8 degrees over the course of the observations. Minor Planets”. Minor Planet Bulletin 31, 29-33. This asteroid was also imaged by another team during the same time period. Ivarsen et al. (2004) published a period of 6.47 ± Warner, Brian D., “Collaborative Asteroid Lightcurve Link” 0.01 hours, consistent with our results. (CALL) web page at http://www.minorplanetobserver.com/astlc/default.htm 297 Caecillia. This work on Caecillia finds a period of 4.163 ± 0.004 hours with an amplitude of 0.20 ± 0.02 magnitudes. The data were unfiltered and the reference stars were not calibrated between nights. Edwin Sheridan published a period for Caecillia of 4.1505 ± 0.0002 hours and an amplitude of 0.15 magnitudes on Brian Warner’s CALL website, statistically similar to the results we report here.

744 Aguntina. There is no previously published period for Aguntina per Harris (2003). This work finds a period of 17.47 ± 0.05 hours with an amplitude of 0.50 ±0.05 magnitudes. These data were unfiltered and were phased by shifting individual nights along the magnitude access to obtain a consistent lightcurve.

1062 Ljuba. The same r-instrumental calibrated reference stars were used to reduce the data of Ljuba. Previous work by Binzel (1987) indicated a period of 36 hours ± 2 hours from 13 total data points over the course of three consecutive nights. Using 976 data points collected over 10 nights spaced over two weeks, this work Minor Planet Bulletin 32 (2005) 16

Phased Differential Photometry for (228) Agathe Phased Differential Photometry for (1062) Ljuba Period = 6.484 +/- 0.01 hours Period = 33.8 +/- 0.2 hours G = 0. G=.15 -0.1 -0.1 -0.05 10/16/2003 10/16/2003 -0.05 0 10/17/2003 10/17/2003 0.05 10/18/2003 10/18/2003 0 0.1 10/19/2003 10/19/2003 0.05 0.15 10/20/2003 10/20/2003 0.2 10/21/2003 10/21/2003 0.1 0.25 10/22/2003 10/22/2003 Magnitude r(inst) 0.3 10/23/2003 0.15 10/23/2003 Magnitude r(inst) 0.35 10/29/2003 0 = J.D. 2452928.569213 0.2 0.4 0 = J.D. 2452928.558171 10/30/2003 0 0.2 0.4 0.6 0.8 1 0.25 Phase 0 0.2 0.4 0.6 0.8 1 Phase

Phased Differential Photometry for (297) Caecillia Period = 4.163 +/- 0.005 hours Phased Differential Photometry for (1605) -0.100 Milankovitch Period = 11.60 +/- 0.05 hours -0.100 -0.050 0 = J.D. 2453111.590028

0.000 -0.050

0.050 0.000 9/18/2003 4/16/2004 0.100 9/23/2003 4/17/2004 0.050 4/19/2004 0.150 Magnitude 4/27/2004 Magnitude 0.200 0.100

0.250 0.150 0 = J.D. 2452900.537506 0.300 0.200 0 0.2 0.4 0.6 0.8 1 0 0.2 0.4 0.6 0.8 1 Phase Phase

Phased Differential Photometry for (744) Aguntina Phased Differential Photometry for (3125) Hay Period = 17.47 +/- 0.05 hours Period = 14.31 +/- 0.03 hours -0.1 -0.1

0 0

0.1 3/18/2004 0.1 0.2 3/19/2004 2/2/2003 0.2 3/22/2004 2/5/2003 0.3 3/30/2004 0.3 2/11/2003 0.4 4/9/2004 2/12/2003 Magnitude

Magnitude 0.4 4/13/2004 2/13/2003 0.5 0.5 0.6 0 = J.D. 2453082.654580 0.6 0.7 0 = J.D. 2452672.628884 0 0.2 0.4 0.6 0.8 1 0.7 Phase 0 0.2 0.4 0.6 0.8 1 Phase

Minor Planet Bulletin 32 (2005) 17

LIGHTCURVE ANALYSIS OF (5892) 1981 YS1 REVISITED “This is an excellent example of why you should plot each day with different symbols, so the composite can be Brian D. Warner "unscrewed". In addition to being unable to judge the quality Palmer Divide Observatory of a composite, if the composite turns out to be a wrong 17995 Bakers Farm Rd. period, the value of the underlying data is preserved if one can Colorado Springs, CO 80908 "unscrew" it and put it back together with the right period.” [email protected] Once the combined data was available, Warner tried searches Richard Ditteon around both periods and others – to be certain a third solution did Rose-Hulman Institute of Technology CM171 not present itself. The result was a slight revision of the solution, 5500 Wabash Ave. i.e., 10.59±0.02h instead of 10.60±0.02h. The amplitude is Terre Haute, IN 47803 0.27±0.03 mag. The revised lightcurve is shown in Fig. 1. [email protected] Nothing critical should be taken from this episode. Instead, it (Received: 7 September) shows the better aspects of lightcurve work: collaboration among observers, the willingness to re-examine results in light of new In previous issues of the Minor Planet Bulletin, the data, and learning yet another lesson about the pitfalls that lie in waiting for the unsuspecting researcher. authors reported independent findings for the period of asteroid (5892) 1981 YS . The analysis of the curves was 1 This also brings up the question of whether or not an asteroid with re-examined and the parameters previously reported by a published period should be worked by a later observer, if the Warner were found to be the more likely solution. The goal is simply period determination and not for other reasons such process brought to light some of the pitfalls of data as shape modeling or H-G determinations. In this case, both analysis, especially regarding aliases. The combined data papers were in process and so neither knew about the other’s led to a slightly changed synodic period, 10.59±0.02h work. Also in this case, it proved beneficial that there were two with an amplitude of 0.27±0.03mag. independent findings as it led to establishing an even firmer solution. If an asteroid has a rating of ‘2’, it would be a good idea Initial Findings and Re-examination to try to find the original paper and see if the asteroid deserves additional work. A rating of ‘1’ definitely merits additional

Asteroid (5892) 1981 YS1 was discovered from Purple Mountain observations. A rating of ‘3’ can probably be passed over in lieu of Observatory on 1981 Dec. 23. The approximate diameter (Harris more deserving targets. A ‘4’ rating is ambiguous. While it does 2003) is 6km. Warner (2003) previously reported a synodic indicate a pole solution has been reported, the period may still be period of 10.60±0.02h and amplitude of 0.26±0.03 mag. In a in error. Again, this is where examination of the literature can help subsequent issue of the Minor Planet Bulletin (Ditteon 2003), a make or break the case for additional work. Even when the period period of 11.905±0.005h and amplitude of 0.33 mag. were is well known, one can check if there is a pole solution wanting reported. See those previous articles for the lightcurve plots. The only a few more observations. In short, truly needless duplication second article prompted Warner to contact Ditteon to arrange for of effort is relatively rare and, as been shown above, duplicate an exchange of data to see if combining the two sets could resolve work can lead to improved and more certain results. the discrepancy. This was made easier by the fact both authors were using the same MPO Canopus data analysis program, which allows importing data from other observers into the common data files used for period analysis.

While this was happening, an email was sent to Dr. Alan Harris of Space Science Institute for his analysis. His reply, without having the data in hand and based only on reviewing the published lightcurves, eventually proved to be correct (Harris 2003a):

“I immediately noticed that all [Ditteon sessions] except for the very last day of observation (January 11) are separated by multiples of 2 days, or 48 hours. So the period assumes 4 cycles in close to 48 hours, specifically 47.62 hours. Because the curve is so symmetrical, we could think of 8 half-cycles in 47.62 hours in looking for aliases. If I take [the Warner] period of 10.59 hours and divide that into 47.62 hours, I get 4.4967 cycles! It appears to me that [Ditteon] picked up the alias of 4.0 cycles in 47.62 hours instead of the correct 4.5 cycles per 47.62 hours, which would yield a period of 10.58 hours. If this hypothesis is correct, I’ll bet the last day (January 11) has so few data points that it was unable to reveal the half-cycle ambiguity error. If [there had been] Figure 1. The combined data lightcurve for (5892) 1981 YS1. The enough data on the odd days, I’m sure that the alias solution synodic period is 10.59±0.02h and amplitude is 0.27±0.03m. would go away.”

Minor Planet Bulletin 32 (2005) 18

The authors want to thank Dr. Harris for his continuing and and no light-time corrections have been applied. Data were invaluable support and insights. plotted as instrumental differential magnitude vs JD and initial graphical analysis was carried out. References For 265 Anna, some 14 extrema observed during March 2004 Ditteon et al. (2003). “2003-04 Winter Observing Campaign at yielded an initial period of 11.700 hours. Analysis was then Roese-Hulman Institute. Results for 797 Montana, 3227 performed using the AVE software (Barbera, 2004) and the Phase Hasegawa, 3512 Eriepa, 4159 Freeman, 5234 Sechenov, and Dispersion Minimisation (PDM) technique. Periods between 0.35 (5892) 1981 YS1”, Minor Planet Bulletin 31, 54-56. and 1.2 days were searched and a distinct minimum on the periodogram occurred at 0.486 days. This was then refined further Harris, A. W. (2003). “Minor Planet Lightcurve Parameters”, On by trial phase stacks – finally yielding a period of 0.487 days or Minor Planet Center web site: http://cfa- 11.681 ± 0.006 hours. Using this period and a zero phase epoch of www.harvard.edu/iau/lists/LightcurveDat.html JD 2453083.96 the data were phase stacked as shown in Figure 1. An additive constant was applied to match the magnitudes on Harris, A. W. (2003a). Private communication. different nights. The lightcurve variation is 0.48 magnitudes. Using a tri-axial ellipsoid model, this implies an axial ratio a/b of Warner, B. D. (2003), “Lightcurve Analysis for Numbered 1.55 – a significantly non-spherical shape – possibly a good Asteroids 1351, 1589, 2278, 5076, 5892, and 6386”, Minor Planet candidate for shape modelling. The high value of the variation Bulletin 31, 36-39. suggests that this asteroid was at near-equatorial aspect at this opposition. As all phases of the rotation were observed with a good density of points, we believe this is a secure result.

PERIOD DETERMINATIONS For 1584 Fuji, some 11 extrema observed in February 2004 were FOR 265 ANNA AND 1584 FUJI used in the initial graphical analysis, yielding a period of 14.89 hours. The AVE software and the PDM method were then C. S. Bembrick employed to search periods between 0.3 and 0.85 days. The PO Box 1537, Bathurst, NSW 2795, Australia periodogram showed a large distinct minimum at 0.620 days [email protected] (14.880 ± 0.013 hours) and a secondary minimum at 0.310 days. The latter was judged to be an alias as the phase stack produced a G. Bolt single maximum and minimum. The data were phase stacked 295 Camberwarra Drive, Craigie, WA 6025, Australia using the above period and a zero phase epoch of JD 2453047.049 (Figure 2). For the final lightcurve the individual night (Received: 15 July Revised: 18 July) lightcurves were adjusted by an additive constant. The lightcurve amplitude is 0.17 magnitudes. This variation implies an axial ratio Minor planets 265 Anna and 1584 Fuji were observed a/b of 1.17, however, the previously reported variation of 0.3 from two sites widely separated in longitude. The magnitudes suggests a higher ratio at more equatorial aspects. former was observed over 12 nights (22 rotations) and Almost all phases of the rotation were observed with a high the latter over 15 nights (23 rotations). Unfiltered CCD density of points yielding a secure result. photometry yielded a synodic rotation period of 11.681 ± 0.006 hours for Anna and a period of 14.880 ± 0.013 References hours for Fuji. The amplitudes are 0.48 and 0.17, Barbera, R. (2004). “AVE” Analisis de Variabilidad Estelar, respectively. version 2.51. Grup Estudis Astronomics. http://usuarios.lycos.es/rbarbera/AVE/AveInternational.htm Introduction Harris, A. W. and Warner, B. D. (2003). “Minor Planet Lightcurve Minor planet 265 Anna was discovered in 1887 by J. Palisa at Parameters.” Updated Dec 15, 2003 and posted on Vienna Observatory. No previously published lightcurves have http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html been found for this main-belt asteroid and no data are listed in the tabulations of Harris and Warner (2003). Its diameter is quoted as Warner, B. D., Kaasalainen, M., Harris, A. W., and Pravec, P. 30 km and the albedo as 0.054. Minor planet 1584 Fuji was (2004). Asteroid Photometry Opportunities January – March discovered in 1927 by O. Oikama at Tokyo and named after the 2004. Minor Planet Bulletin 31, 27. highest mountain in Japan. This main-belt, S-type asteroid is one of the Phocaea group with an albedo of 0.13 and a B-V of 0.89. There are no previously published lightcurves, but the asteroid is listed in the tabulations of Harris and Warner (2003), where its period is noted as possibly 10 hours with an amplitude of 0.3 magnitudes. The diameter is quoted as 25 km. Both of these asteroids were chosen from the lists published in the Minor Planet Bulletin (e.g. Warner, et al., 2004).

Observations and Results

In early 2004 both these minor planets were favorably placed for southern observers. Unfiltered CCD photometry was employed

Minor Planet Bulletin 32 (2005) 19

0.5 0.9 265 Anna 1584 Fuji

0.6 Feb-11 Feb-12 Feb-14 Feb-15 Feb-17 0.7 1.0 Feb-18 Feb-19 Feb-20 Feb-22 0.8 Feb-25 Delta Mag Delta Mag Mar-19 0.9 1.1 Mar-22 Mar-24 Mar-27 1.0 Mar-29 Period = 11.681 hours Mar-30 Period = 14.880 hours

1.1 1.2 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 Phase Phase Figure 1. Composite lightcurve – 265 Anna in March 2004. Figure 2. Composite lightcurve – 1584 Fuji in February 2004.

THE MINOR PLANET OBSERVER: noise and dropped a few images where clouds had rolled in. The DATA AND MORE DATA! net result is shown below.

Brian Warner Palmer Divide Observatory 17995 Bakers Farm Rd. Colorado Springs, CO 80908 [email protected]

The oft-heard phrase in asteroid photometry is “More Data!” Asteroids do not always give up their secrets easily with the initial runs of data showing the promise of finding a period (or none) and the subsequent runs only confusing the issue. If a “normal” curve suddenly displays something unusual, say an unexpected dip, the urge is think “binary”. It’s a temptation difficult to ignore. However, good science says that the proof is not in the pudding but in multiple observations for which there is no explanation other than the data represents something physically real. Note that the dip is gone. Measuring the images with a second set comparisons and not using some “bad” images gave a much different result! Is it the true result? Mostly likely it is. Another rule to remember is that the less complicated answer is usually the best answer. A binary asteroid, while not as rare as once thought, is also not that common. When in doubt, check and double check. If after that you still have something, then you can quote the famous fictional detective, Sherlock Holmes: “When you have exhausted all other possibilities, then whatever remains, no matter how improbable, must be the truth.”

SAPC and OLAF

For sometime, it’s been the hope of Mikko Kaasalainen of the University of Helsinki to get an on-line database of asteroid lightcurve data established. The Uppsala system was a bit The plot above shows the data that I acquired over three nights for cumbersome and hasn’t been updated for some time. Toward that (18108) 2000 NT5 when phased against a period of 2.9h. My goal of an easy to use site, I’ve worked with Dr. Kaasalainen to immediate thought was that I’d caught a binary event (the “dip” at develop something that allows observers to upload text files for 0.5 phase). Was it real? I sent the data to Petr Pravec at Ondrejov use by other researchers. The Standard Asteroid Photometry Observatory in the Czech Republic and asked if he might be able Catalog (SAPC) can be found at to observe the asteroid. He set Peter Kusnirak on the task and then sent me the resulting data. In the meantime, I also remeasured my http://www.minorplanetobserver.com/sapc/default.htm images, using a different set of comparison stars for the one session that showed the anomalous behavior, even though the This is a very basic site but it’s a beginning. The problem is that plots for the comparisons didn’t show anything wrong. In the it’s not overly formal and its lifetime is whatever I can support. second set, I used some brighter comparisons to cut down the Should I suddenly inherit millions, my inclinations may change!

Minor Planet Bulletin 32 (2005) 20

This is where something more permanent might be preferred and encouraged to give special attention to those which lie near the that is being developed. It’s called the “Online Archiving Facility” limit of their equipment. (OLAF) and is part of the Small Bodies Node of NASA’s Planetary Data System. OLAF may be found at 1862 Apollo has close approaches in pairs; that in 2005 November while outbound from the Sun will be followed by another http://dorothy.as.arizona.edu/olaf/index.html comparably close and bright in 2007 April-May on its following inbound journey. (5660) 1974 MA is brighter 2005 July 28 at I’ve tried uploading data to OLAF and found it a bit daunting. magnitude 14.5 than until the year 2036 when the next close However, it’s the plan and hopes of those developing the site to approach under comparable observing conditions occurs. (6611) make the site a little easier to use and, more important, provide the 1993 VW in late April is making its brightest at magnitude 13.3 necessary training and support to make using the site as efficient and closest at 0.086 AU approach until the 22nd century. (22753) as possible. One possibility is a presentation at the Society for 1998 WT is brighter in early March at magnitude 14.3 and closer Astronomical Sciences meeting at Big Bear in May 2005. Others at 0.079 AU than until March 2040. will occur before then. Something very important about the OLAF database is that professionals will review it and so data on it will These lists have been prepared by an examination of the maximum carry additional weight. elongation circumstances of minor planets computed by the author for all years through 2060 with a full perturbation program written So, which do you use? I’ve been in contact with one of the by Dr. John Reed, and to whom he expresses his thanks. Elements designers of the site, Mark Sykes, about how data from MPO are from EMP 1992, except that for all minor planets for which Canopus could be readily uploaded to OLAF so that the data meet new or improved elements have been published subsequently in the more stringent formatting requirements. It appears this may the Minor Planet Ciculars or in electronic form, the newer not be too difficult and so those who can supply data with a elements have been used. Planetary positions are from the JPL minimum of two or three columns (JD, magnitude, [error]), DE-200 ephemeris, courtesy of Dr. E. Myles Standish. Dr. Reed's wouldn’t have too much trouble. If you want to make your data ephemeris generating program, a list of minor planet elements, and easily available now, then use SAPC. If you want to work through the JPL planetary ephemeris are freeware which may be obtained OLAF now and save the steps of uploading again in the future, try from the author by sending a 100 Megabyte zip disk and stamped, to use it now. addressed return mailer. They cannot be downloaded directly over the Internet. The main point is that having actual observations available is important to those doing spin axis and other work. It’s difficult to Any objects whose brightest magnitudes near the time of do that work when the only way to get actual data points is to scan maximum elongation vary by at least 2.0 in this interval and in in a low resolution plot and try to determine X/Y values. It’s 2005 will be within 0.3 of the brightest occuring, or vary by at possible to get rough results but certainly not high precision. Of least 3.0 and in 2005 will be within 0.5 of the brightest occuring; course, you want to be careful about uploading your data in that and which are visual magnitude 14.5 or brighter, are included. For once you do, it becomes public domain. Some might prefer to wait objects brighter than visual magnitude 13.5, which are within the until the results have been published. That’s fine, too, just as long range of a large number of observers, these standards have been as it’s available at some point. This is all parallel to submitting relaxed somewhat to include a larger number of objects. astrometry to the Minor Planet Center. Fortunately, there is a Magnitudes have been computed from the updated magnitude central clearinghouse for astrometry. There is not for photometry. parameters published in MPC28104-28116, on 1996 Nov. 25, or There should be and, in the end, it needs to be in the hands of more recently in the Minor Planet Circulars. those who can manage it for the long-term (and have LOTS of data storage capabilities!). Oppositions may be in right ascension or in celestial longitude. Here we use still a third representation, maximum elongation from the Sun, instead of opposition. Though unconventional, it has the advantage that many close approaches do not involve actual MINOR PLANETS AT UNUSUALLY FAVORABLE opposition to the Sun near the time of minimum distance and ELONGATIONS IN 2005 greatest brightness and are missed by an opposition-based program. Other data are also provided according to the following Frederick Pilcher tabular listings: Minor planet number, date of maximum Illinois College elongation from the Sun in format yyyy/mm/dd, maximum Jacksonville, IL 62650 USA elongation in degrees, right ascension on date of maximum elongation, declination on date of maximum elongation, both in (Received: 13 October) J2000 coordinates, date of minimum or brightest magnitude in format yyyy/mm/dd, minimum magnitude, date of minimum distance in format yyyy/mm/dd, and minimum distance in AU. A list is presented of minor planets which are much brighter than usual at their 2005 apparitions. Very close Users should note that when the maximum elongation is about approaches of four Apollo type minor planets: 1862 177° or greater, the minimum magnitude is sharply peaked due to Apollo, (5660) 1974 MA, (6611) 1993 VW, and (22753) enhanced brightening near zero phase angle. Even as near as 10 1998 WT, are the highlights of the year. days before or after minimum magnitude the magnitude is generally about 0.4 greater. This effect takes place in greater time The minor planets in the lists which follow will be much brighter interval for smaller maximum elongations. There is some interest at their 2005 apparitions than at their average distances at in very small minimum phase angles. For maximum elongations maximum elongation. Many years may pass before these minor E near 180° at Earth distance ∆ an approximate formula for the minimum phase angle is =(180-E)/(∆+1). planets will be again as bright as in 2005. Observers are α α Minor Planet Bulletin 32 (2005) 21 Table 1. Numerical Sequence of Favorable Elongations Planet Max Elon D Max E RA Dec Min Mag D Mag Min Dist D Min Dist 2199 2005/06/19 164.1° 17h49m - 7° 2005/06/20 14.5 2005/06/24 0.812 2243 2005/09/19 173.2° 23h54m - 7° 2005/09/18 14.1 2005/09/12 0.841 Planet Max Elon D Max E RA Dec Min Mag D Mag Min Dist D Min Dist 2375 2005/07/14 179.4° 19h33m -22° 2005/07/14 14.4 2005/07/06 1.879 2464 2005/12/07 178.6° 4h53m +23° 2005/12/07 14.5 2005/12/08 1.513 2 2005/03/21 168.9° 12h29m + 8° 2005/03/20 7.1 2005/03/15 1.368 2474 2005/05/31 176.9° 16h37m -18° 2005/05/31 13.8 2005/06/01 1.092 3 2005/12/09 155.1° 5h13m - 1° 2005/12/07 7.7 2005/12/04 1.063 14 2005/05/18 172.0° 15h47m -11° 2005/05/17 9.1 2005/05/13 1.278 2544 2005/03/12 143.0° 10h59m -33° 2005/03/17 14.5 2005/03/21 0.952 19 2005/11/04 179.4° 2h39m +14° 2005/11/04 8.9 2005/11/02 1.064 2731 2005/06/19 160.5° 17h49m - 3° 2005/06/20 14.3 2005/06/21 1.595 42 2005/07/18 170.3° 20h 6m -30° 2005/07/19 9.2 2005/07/23 0.917 2757 2005/10/16 179.6° 1h26m + 9° 2005/10/16 14.5 2005/10/20 1.618 2794 2005/11/02 165.6° 2h10m +28° 2005/11/02 14.5 2005/11/02 0.936 57 2005/11/05 170.1° 2h57m + 6° 2005/11/05 10.9 2005/11/05 1.798 2839 2005/10/28 178.3° 2h14m +11° 2005/10/28 13.6 2005/10/29 0.899 60 2005/12/21 173.0° 5h58m +16° 2005/12/21 9.9 2005/12/23 0.985 69 2005/02/21 172.5° 10h 8m + 3° 2005/02/21 10.4 2005/02/18 1.578 3875 2005/08/28 174.3° 22h38m -14° 2005/08/28 13.9 2005/08/24 0.798 70 2005/06/08 169.2° 17h 6m -33° 2005/06/09 10.7 2005/06/14 1.232 3895 2005/02/10 170.0° 9h13m + 6° 2005/02/10 14.5 2005/02/13 0.960 90 2005/07/09 177.8° 19h15m -24° 2005/07/09 11.7 2005/07/11 1.682 3901 2005/05/28 156.7° 16h 9m -44° 2005/05/27 14.5 2005/05/26 0.929 3925 2005/09/23 172.4° 0h14m - 6° 2005/09/23 14.2 2005/09/23 1.558 101 2005/09/10 178.5° 23h13m - 3° 2005/09/10 10.6 2005/09/07 1.222 3998 2005/11/02 172.2° 2h24m +22° 2005/11/03 14.5 2005/11/08 0.917 126 2005/09/04 176.4° 22h57m -10° 2005/09/04 11.5 2005/09/04 1.176 129 2005/05/06 158.4° 15h18m + 4° 2005/05/08 10.0 2005/05/10 1.307 4049 2005/07/07 179.3° 19h 8m -23° 2005/07/07 14.3 2005/07/13 1.308 145 2005/01/27 162.8° 9h 7m +34° 2005/01/27 11.1 2005/01/27 1.333 4121 2005/11/11 177.6° 3h 7m +19° 2005/11/11 14.5 2005/10/31 1.145 146 2005/06/09 177.8° 17h 9m -20° 2005/06/09 11.3 2005/06/08 1.549 4132 2005/09/25 170.3° 0h34m - 6° 2005/09/27 13.5 2005/10/06 0.939 4324 2005/10/15 165.0° 0h56m +22° 2005/10/15 14.5 2005/10/17 1.076 161 2005/07/18 162.5° 20h 9m -38° 2005/07/19 11.5 2005/07/20 1.071 4384 2005/08/05 178.6° 21h 4m -18° 2005/08/05 14.5 2005/08/10 1.241 164 2005/12/12 176.6° 5h22m +26° 2005/12/12 11.1 2005/11/29 1.188 181 2005/01/09 161.5° 7h 4m + 4° 2005/01/08 11.3 2005/01/08 1.566 4577 2005/12/02 175.9° 4h36m +26° 2005/12/03 14.1 2005/12/12 1.043 222 2005/05/22 178.8° 15h59m -19° 2005/05/22 12.5 2005/05/25 1.701 4768 2005/08/11 178.7° 21h25m -16° 2005/08/11 14.3 2005/08/14 1.486 269 2005/06/17 169.9° 17h45m -13° 2005/06/18 11.6 2005/06/19 1.060 4875 2005/06/20 173.3° 17h53m -16° 2005/06/20 14.3 2005/06/22 0.837 4894 2005/06/26 178.8° 18h22m -22° 2005/06/26 14.4 2005/07/03 0.785 284 2005/05/23 177.5° 16h 4m -18° 2005/05/23 11.6 2005/06/01 0.933 5176 2005/09/09 164.2° 23h39m -19° 2005/09/10 13.9 2005/09/12 0.876 288 2005/05/08 172.4° 15h11m - 9° 2005/05/08 12.3 2005/05/05 1.204 305 2005/01/08 172.8° 7h17m +15° 2005/01/08 12.0 2005/01/08 1.549 5567 2005/10/04 178.9° 0h40m + 5° 2005/10/04 13.7 2005/09/27 1.471 315 2005/08/14 178.1° 21h32m -12° 2005/08/14 14.4 2005/08/15 0.859 5660 2005/07/15 128.7° 22h47m + 1° 2005/07/28 14.5 2005/07/31 0.188 326 2005/04/17 175.6° 13h46m - 6° 2005/04/18 11.3 2005/04/26 1.049 5847 2005/09/27 165.1° 23h52m +15° 2005/09/28 14.0 2005/09/30 0.796 5852 2005/06/05 177.3° 16h53m -19° 2005/06/05 14.5 2005/06/06 1.156 381 2005/07/22 178.0° 20h 3m -18° 2005/07/22 12.2 2005/07/19 1.947 5994 2005/10/25 179.5° 1h57m +12° 2005/10/25 14.5 2005/10/16 1.396 382 2005/04/15 168.5° 13h17m -20° 2005/04/16 12.2 2005/04/18 1.592 384 2005/12/29 172.4° 6h39m +30° 2005/12/29 12.3 2005/12/28 1.291 6364 2005/08/25 171.2° 22h25m -19° 2005/08/24 14.4 2005/08/21 1.065 386 2005/10/12 160.1° 1h51m - 9° 2005/10/12 10.7 2005/10/12 1.433 6611 2005/05/15 150.0° 13h29m -10° 2005/04/30 13.3 2005/04/24 0.086 397 2005/11/02 176.3° 2h23m +18° 2005/11/02 11.2 2005/10/26 1.050 7353 2005/07/18 169.8° 19h52m -31° 2005/07/18 14.5 2005/07/22 1.177 7534 2005/08/05 172.1° 21h12m -24° 2005/08/04 14.3 2005/08/01 0.718 409 2005/05/24 179.2° 16h 8m -20° 2005/05/24 10.3 2005/05/25 1.383 8400 2005/10/16 154.9° 2h 3m -14° 2005/10/15 14.4 2005/10/14 1.143 418 2005/11/15 176.7° 3h20m +21° 2005/11/15 12.4 2005/11/12 1.346 437 2005/09/07 163.9° 22h38m + 8° 2005/09/05 11.9 2005/09/01 0.824 13918 2005/07/28 178.1° 20h31m -20° 2005/07/28 14.4 2005/07/28 1.037 448 2005/11/04 178.4° 2h36m +17° 2005/11/04 14.0 2005/10/28 1.851 14276 2005/10/26 179.4° 2h 1m +12° 2005/10/26 14.0 2005/10/22 0.866 465 2005/03/28 172.9° 12h18m - 9° 2005/03/29 12.9 2005/04/03 1.526 14835 2005/11/11 175.1° 2h55m +21° 2005/11/10 14.4 2005/11/02 0.796 16403 2005/10/23 178.1° 1h53m + 9° 2005/10/23 13.8 2005/10/21 0.849 481 2005/12/13 175.6° 5h23m +27° 2005/12/13 11.3 2005/12/10 1.355 22753 2005/02/18 172.0° 10h 5m + 3° 2005/03/02 14.3 2005/03/08 0.079 498 2005/07/29 171.0° 20h48m -27° 2005/07/30 11.2 2005/08/03 1.100 503 2005/11/22 178.5° 3h51m +18° 2005/11/22 11.8 2005/11/26 1.382 27973 2005/10/01 173.4° 0h37m - 3° 2005/10/01 14.5 2005/10/08 0.932 519 2005/08/01 160.9° 21h10m -36° 2005/08/02 12.2 2005/08/05 1.367 28017 2005/09/10 168.6° 22h58m + 5° 2005/09/14 14.3 2005/09/27 0.743 532 2005/01/16 175.8° 7h57m +24° 2005/01/16 8.9 2005/01/22 1.526 29769 2005/07/16 172.6° 19h51m -28° 2005/07/16 14.2 2005/07/20 1.175 34706 2005/12/06 176.2° 4h53m +26° 2005/12/07 14.2 2005/12/20 0.461 560 2005/01/01 178.8° 6h46m +21° 2005/01/01 13.2 2005/01/02 1.338 629 2005/12/06 176.6° 4h51m +19° 2005/12/06 13.5 2005/12/09 1.754 686 2005/10/04 154.7° 23h47m +26° 2005/09/30 11.9 2005/09/24 1.016 694 2005/11/11 179.3° 3h 7m +18° 2005/11/11 11.2 2005/10/29 1.116 696 2005/09/22 161.1° 23h32m +17° 2005/09/25 12.5 2005/09/28 1.534 Table 2. Temporal Sequence of Favorable Elongations

712 2005/11/28 173.5° 4h23m +15° 2005/11/28 10.5 2005/11/25 1.116 778 2005/01/28 174.5° 8h50m +23° 2005/01/28 12.8 2005/01/24 1.522 Planet Max Elon D Max E RA Dec Min Mag D Mag Min Dist D Min Dist 785 2005/04/20 162.9° 14h11m + 4° 2005/04/20 11.7 2005/04/20 1.048 786 2005/06/24 178.7° 18h13m -24° 2005/06/24 12.2 2005/06/20 1.760 560 2005/01/01 178.8° 6h46m +21° 2005/01/01 13.2 2005/01/02 1.338 810 2005/08/17 179.0° 21h44m -12° 2005/08/17 13.6 2005/08/20 0.796 2075 2005/01/01 164.1° 6h22m + 8° 2005/01/01 14.5 2005/01/03 0.843 305 2005/01/08 172.8° 7h17m +15° 2005/01/08 12.0 2005/01/08 1.549 814 2005/12/24 177.1° 6h15m +26° 2005/12/24 11.9 2005/12/14 1.551 181 2005/01/09 161.5° 7h 4m + 4° 2005/01/08 11.3 2005/01/08 1.566 834 2005/05/12 175.2° 15h22m -13° 2005/05/12 12.7 2005/05/18 1.598 532 2005/01/16 175.8° 7h57m +24° 2005/01/16 8.9 2005/01/22 1.526 850 2005/06/13 163.8° 17h27m - 7° 2005/06/13 13.2 2005/06/13 1.630 910 2005/05/11 179.8° 15h12m -18° 2005/05/11 13.2 2005/05/14 1.490 1021 2005/01/16 179.4° 7h51m +21° 2005/01/16 11.5 2005/01/05 1.330 950 2005/04/01 170.8° 13h 3m + 3° 2005/03/31 13.6 2005/03/30 1.026 1708 2005/01/24 169.8° 8h16m + 9° 2005/01/23 14.3 2005/01/16 1.205 145 2005/01/27 162.8° 9h 7m +34° 2005/01/27 11.1 2005/01/27 1.333 951 2005/11/12 176.5° 3h 4m +21° 2005/11/12 12.7 2005/11/07 0.863 778 2005/01/28 174.5° 8h50m +23° 2005/01/28 12.8 2005/01/24 1.522 953 2005/05/22 173.6° 15h54m -26° 2005/05/23 13.3 2005/05/29 1.415 3895 2005/02/10 170.0° 9h13m + 6° 2005/02/10 14.5 2005/02/13 0.960 960 2005/08/01 174.4° 20h42m -12° 2005/08/02 14.4 2005/08/05 0.894 986 2005/08/03 164.6° 21h20m -31° 2005/08/05 13.1 2005/08/08 1.656 22753 2005/02/18 172.0° 10h 5m + 3° 2005/03/02 14.3 2005/03/08 0.079 1021 2005/01/16 179.4° 7h51m +21° 2005/01/16 11.5 2005/01/05 1.330 69 2005/02/21 172.5° 10h 8m + 3° 2005/02/21 10.4 2005/02/18 1.578 2544 2005/03/12 143.0° 10h59m -33° 2005/03/17 14.5 2005/03/21 0.952 1052 2005/09/25 170.5° 0h25m - 7° 2005/09/26 13.8 2005/09/28 0.960 2 2005/03/21 168.9° 12h29m + 8° 2005/03/20 7.1 2005/03/15 1.368 1056 2005/08/12 172.9° 21h41m -21° 2005/08/12 13.0 2005/08/11 0.825 465 2005/03/28 172.9° 12h18m - 9° 2005/03/29 12.9 2005/04/03 1.526 1083 2005/12/27 177.3° 6h24m +26° 2005/12/27 14.1 2005/12/29 0.937 1139 2005/10/14 170.6° 0h52m +15° 2005/10/15 12.5 2005/10/23 0.522 950 2005/04/01 170.8° 13h 3m + 3° 2005/03/31 13.6 2005/03/30 1.026 1153 2005/06/12 177.7° 17h22m -25° 2005/06/12 13.5 2005/06/19 0.911 382 2005/04/15 168.5° 13h17m -20° 2005/04/16 12.2 2005/04/18 1.592 326 2005/04/17 175.6° 13h46m - 6° 2005/04/18 11.3 2005/04/26 1.049 1196 2005/07/20 170.2° 20h15m -29° 2005/07/21 13.2 2005/07/27 1.362 785 2005/04/20 162.9° 14h11m + 4° 2005/04/20 11.7 2005/04/20 1.048 1227 2005/07/10 154.7° 19h37m -47° 2005/07/11 13.9 2005/07/12 1.670 1715 2005/04/28 179.5° 14h23m -13° 2005/04/28 13.2 2005/05/05 0.859 1324 2005/05/29 171.7° 16h17m -29° 2005/05/30 14.0 2005/06/03 0.843 1358 2005/07/06 175.8° 19h 2m -26° 2005/07/06 14.2 2005/07/09 1.074 129 2005/05/06 158.4° 15h18m + 4° 2005/05/08 10.0 2005/05/10 1.307 1407 2005/12/08 177.6° 4h58m +25° 2005/12/07 12.9 2005/11/28 1.207 288 2005/05/08 172.4° 15h11m - 9° 2005/05/08 12.3 2005/05/05 1.204 910 2005/05/11 179.8° 15h12m -18° 2005/05/11 13.2 2005/05/14 1.490 1431 2005/08/20 166.4° 22h25m -24° 2005/08/20 13.9 2005/08/21 1.147 834 2005/05/12 175.2° 15h22m -13° 2005/05/12 12.7 2005/05/18 1.598 1438 2005/09/19 176.9° 23h41m + 1° 2005/09/19 14.3 2005/09/20 1.424 6611 2005/05/15 150.0° 13h29m -10° 2005/04/30 13.3 2005/04/24 0.086 1500 2005/09/17 173.2° 23h51m - 8° 2005/09/18 14.5 2005/09/23 0.889 1506 2005/06/15 166.4° 17h43m - 9° 2005/06/15 13.5 2005/06/18 0.915 14 2005/05/18 172.0° 15h47m -11° 2005/05/17 9.1 2005/05/13 1.278 1543 2005/09/04 160.2° 22h28m +11° 2005/08/31 13.7 2005/08/24 0.837 222 2005/05/22 178.8° 15h59m -19° 2005/05/22 12.5 2005/05/25 1.701 953 2005/05/22 173.6° 15h54m -26° 2005/05/23 13.3 2005/05/29 1.415 1578 2005/12/31 179.4° 6h41m +23° 2005/12/31 14.3 2005/12/28 2.054 284 2005/05/23 177.5° 16h 4m -18° 2005/05/23 11.6 2005/06/01 0.933 1609 2005/07/17 172.8° 20h 1m -27° 2005/07/18 12.5 2005/07/24 1.004 409 2005/05/24 179.2° 16h 8m -20° 2005/05/24 10.3 2005/05/25 1.383 1648 2005/07/31 179.6° 20h42m -17° 2005/07/31 13.6 2005/07/23 0.838 1662 2005/10/29 173.2° 2h 5m +19° 2005/10/29 13.9 2005/10/28 1.279 3901 2005/05/28 156.7° 16h 9m -44° 2005/05/27 14.5 2005/05/26 0.929 1671 2005/12/03 172.2° 4h43m +14° 2005/12/03 13.6 2005/12/01 0.935 1324 2005/05/29 171.7° 16h17m -29° 2005/05/30 14.0 2005/06/03 0.843 2474 2005/05/31 176.9° 16h37m -18° 2005/05/31 13.8 2005/06/01 1.092 1687 2005/12/28 179.5° 6h27m +23° 2005/12/28 13.6 2005/12/23 1.713 5852 2005/06/05 177.3° 16h53m -19° 2005/06/05 14.5 2005/06/06 1.156 1708 2005/01/24 169.8° 8h16m + 9° 2005/01/23 14.3 2005/01/16 1.205 70 2005/06/08 169.2° 17h 6m -33° 2005/06/09 10.7 2005/06/14 1.232 1715 2005/04/28 179.5° 14h23m -13° 2005/04/28 13.2 2005/05/05 0.859 1771 2005/11/18 170.6° 3h42m +10° 2005/11/18 13.5 2005/11/16 1.587 146 2005/06/09 177.8° 17h 9m -20° 2005/06/09 11.3 2005/06/08 1.549 1821 2005/07/07 179.0° 19h 8m -23° 2005/07/07 14.5 2005/07/07 0.881 1153 2005/06/12 177.7° 17h22m -25° 2005/06/12 13.5 2005/06/19 0.911 850 2005/06/13 163.8° 17h27m - 7° 2005/06/13 13.2 2005/06/13 1.630 1862 2005/12/01 161.8° 4h 6m +39° 2005/11/13 13.3 2005/11/06 0.075 2019 2005/06/14 178.2° 17h34m -21° 2005/06/14 13.1 2005/06/17 0.861 1902 2005/08/16 161.6° 22h13m -30° 2005/08/16 14.0 2005/08/16 2.107 1506 2005/06/15 166.4° 17h43m - 9° 2005/06/15 13.5 2005/06/18 0.915 1937 2005/06/28 172.0° 18h36m -31° 2005/06/29 13.9 2005/07/02 1.023 2006 2005/11/07 172.8° 2h42m +23° 2005/11/07 14.1 2005/11/03 0.903 269 2005/06/17 169.9° 17h45m -13° 2005/06/18 11.6 2005/06/19 1.060 2016 2005/10/21 179.6° 1h43m +10° 2005/10/21 14.5 2005/10/16 1.588 2199 2005/06/19 164.1° 17h49m - 7° 2005/06/20 14.5 2005/06/24 0.812 2731 2005/06/19 160.5° 17h49m - 3° 2005/06/20 14.3 2005/06/21 1.595 2019 2005/06/14 178.2° 17h34m -21° 2005/06/14 13.1 2005/06/17 0.861 4875 2005/06/20 173.3° 17h53m -16° 2005/06/20 14.3 2005/06/22 0.837 2034 2005/10/20 177.4° 1h39m +13° 2005/10/21 14.5 2005/10/26 0.971 786 2005/06/24 178.7° 18h13m -24° 2005/06/24 12.2 2005/06/20 1.760 2044 2005/11/21 173.1° 3h49m +26° 2005/11/22 14.0 2005/11/30 0.689 2075 2005/01/01 164.1° 6h22m + 8° 2005/01/01 14.5 2005/01/03 0.843 4894 2005/06/26 178.8° 18h22m -22° 2005/06/26 14.4 2005/07/03 0.785 2099 2005/11/01 179.5° 2h28m +14° 2005/11/01 14.6 2005/10/26 0.496 1937 2005/06/28 172.0° 18h36m -31° 2005/06/29 13.9 2005/07/02 1.023 1358 2005/07/06 175.8° 19h 2m -26° 2005/07/06 14.2 2005/07/09 1.074 1821 2005/07/07 179.0° 19h 8m -23° 2005/07/07 14.5 2005/07/07 0.881 4049 2005/07/07 179.3° 19h 8m -23° 2005/07/07 14.3 2005/07/13 1.308

Minor Planet Bulletin 32 (2005) 22

Planet Max Elon D Max E RA Dec Min Mag D Mag Min Dist D Min Dist LIGHTCURVE PHOTOMETRY OPPORTUNITIES 90 2005/07/09 177.8° 19h15m -24° 2005/07/09 11.7 2005/07/11 1.682 1227 2005/07/10 154.7° 19h37m -47° 2005/07/11 13.9 2005/07/12 1.670 JANUARY-MARCH 2005 2375 2005/07/14 179.4° 19h33m -22° 2005/07/14 14.4 2005/07/06 1.879 5660 2005/07/15 128.7° 22h47m + 1° 2005/07/28 14.5 2005/07/31 0.188 29769 2005/07/16 172.6° 19h51m -28° 2005/07/16 14.2 2005/07/20 1.175 Brian D. Warner 1609 2005/07/17 172.8° 20h 1m -27° 2005/07/18 12.5 2005/07/24 1.004 Palmer Divide Observatory 42 2005/07/18 170.3° 20h 6m -30° 2005/07/19 9.2 2005/07/23 0.917 161 2005/07/18 162.5° 20h 9m -38° 2005/07/19 11.5 2005/07/20 1.071 17995 Bakers Farm Rd. 7353 2005/07/18 169.8° 19h52m -31° 2005/07/18 14.5 2005/07/22 1.177 1196 2005/07/20 170.2° 20h15m -29° 2005/07/21 13.2 2005/07/27 1.362 Colorado Springs, CO 80908

381 2005/07/22 178.0° 20h 3m -18° 2005/07/22 12.2 2005/07/19 1.947 13918 2005/07/28 178.1° 20h31m -20° 2005/07/28 14.4 2005/07/28 1.037 498 2005/07/29 171.0° 20h48m -27° 2005/07/30 11.2 2005/08/03 1.100 Mikko Kaasalainen 1648 2005/07/31 179.6° 20h42m -17° 2005/07/31 13.6 2005/07/23 0.838 Rolf Nevanlinna Institute 519 2005/08/01 160.9° 21h10m -36° 2005/08/02 12.2 2005/08/05 1.367 P.O. Box 68 (Gustaf Hallstromin katu 2b, room A422) 960 2005/08/01 174.4° 20h42m -12° 2005/08/02 14.4 2005/08/05 0.894 986 2005/08/03 164.6° 21h20m -31° 2005/08/05 13.1 2005/08/08 1.656 FIN-00014 University of Helsinki 4384 2005/08/05 178.6° 21h 4m -18° 2005/08/05 14.5 2005/08/10 1.241 7534 2005/08/05 172.1° 21h12m -24° 2005/08/04 14.3 2005/08/01 0.718 Finland 4768 2005/08/11 178.7° 21h25m -16° 2005/08/11 14.3 2005/08/14 1.486

1056 2005/08/12 172.9° 21h41m -21° 2005/08/12 13.0 2005/08/11 0.825 315 2005/08/14 178.1° 21h32m -12° 2005/08/14 14.4 2005/08/15 0.859 Alan W. Harris 1902 2005/08/16 161.6° 22h13m -30° 2005/08/16 14.0 2005/08/16 2.107 Space Science Institute 810 2005/08/17 179.0° 21h44m -12° 2005/08/17 13.6 2005/08/20 0.796 1431 2005/08/20 166.4° 22h25m -24° 2005/08/20 13.9 2005/08/21 1.147 4603 Orange Knoll Ave. 6364 2005/08/25 171.2° 22h25m -19° 2005/08/24 14.4 2005/08/21 1.065 La Canada, CA 91011-3364 3875 2005/08/28 174.3° 22h38m -14° 2005/08/28 13.9 2005/08/24 0.798 126 2005/09/04 176.4° 22h57m -10° 2005/09/04 11.5 2005/09/04 1.176 1543 2005/09/04 160.2° 22h28m +11° 2005/08/31 13.7 2005/08/24 0.837 437 2005/09/07 163.9° 22h38m + 8° 2005/09/05 11.9 2005/09/01 0.824 Petr Pravec

5176 2005/09/09 164.2° 23h39m -19° 2005/09/10 13.9 2005/09/12 0.876 Astronomical Institute 101 2005/09/10 178.5° 23h13m - 3° 2005/09/10 10.6 2005/09/07 1.222 28017 2005/09/10 168.6° 22h58m + 5° 2005/09/14 14.3 2005/09/27 0.743 CZ-25165 Ondrejov 1500 2005/09/17 173.2° 23h51m - 8° 2005/09/18 14.5 2005/09/23 0.889 Czech Republic 1438 2005/09/19 176.9° 23h41m + 1° 2005/09/19 14.3 2005/09/20 1.424 [email protected] 2243 2005/09/19 173.2° 23h54m - 7° 2005/09/18 14.1 2005/09/12 0.841 696 2005/09/22 161.1° 23h32m +17° 2005/09/25 12.5 2005/09/28 1.534 3925 2005/09/23 172.4° 0h14m - 6° 2005/09/23 14.2 2005/09/23 1.558 1052 2005/09/25 170.5° 0h25m - 7° 2005/09/26 13.8 2005/09/28 0.960 This article has gone through many changes over the years. Going 4132 2005/09/25 170.3° 0h34m - 6° 2005/09/27 13.5 2005/10/06 0.939 back to 1975 and volume 3 (the earliest that could be found on the 5847 2005/09/27 165.1° 23h52m +15° 2005/09/28 14.0 2005/09/30 0.796 27973 2005/10/01 173.4° 0h37m - 3° 2005/10/01 14.5 2005/10/08 0.932 ADS in a quick search), only visual photometry was mentioned in 686 2005/10/04 154.7° 23h47m +26° 2005/09/30 11.9 2005/09/24 1.016 the article by Derek Wallentine and Alain Porter. It was in MPB 5567 2005/10/04 178.9° 0h40m + 5° 2005/10/04 13.7 2005/09/27 1.471 386 2005/10/12 160.1° 1h51m - 9° 2005/10/12 10.7 2005/10/12 1.433 10-1, 1983 January-March, that author Harris first presented a list 1139 2005/10/14 170.6° 0h52m +15° 2005/10/15 12.5 2005/10/23 0.522 of photoelectric photometry opportunities, where he provided not 4324 2005/10/15 165.0° 0h56m +22° 2005/10/15 14.5 2005/10/17 1.076 2757 2005/10/16 179.6° 1h26m + 9° 2005/10/16 14.5 2005/10/20 1.618 only a general list of potential targets but ten day ephemerides. 8400 2005/10/16 154.9° 2h 3m -14° 2005/10/15 14.4 2005/10/14 1.143 2034 2005/10/20 177.4° 1h39m +13° 2005/10/21 14.5 2005/10/26 0.971 Back then, personal computers were just coming to the fore and

2016 2005/10/21 179.6° 1h43m +10° 2005/10/21 14.5 2005/10/16 1.588 ephemeris programs were not so many or so sophisticated. Author 16403 2005/10/23 178.1° 1h53m + 9° 2005/10/23 13.8 2005/10/21 0.849 5994 2005/10/25 179.5° 1h57m +12° 2005/10/25 14.5 2005/10/16 1.396 Warner remembers using his Radio Shack Model I taking a couple 14276 2005/10/26 179.4° 2h 1m +12° 2005/10/26 14.0 2005/10/22 0.866 2839 2005/10/28 178.3° 2h14m +11° 2005/10/28 13.6 2005/10/29 0.899 of minutes to do orbit calculations that took hours on a programmable calculator. On today’s computers, it’s a few 1662 2005/10/29 173.2° 2h 5m +19° 2005/10/29 13.9 2005/10/28 1.279 2099 2005/11/01 179.5° 2h28m +14° 2005/11/01 14.6 2005/10/26 0.496 milliseconds. 397 2005/11/02 176.3° 2h23m +18° 2005/11/02 11.2 2005/10/26 1.050 2794 2005/11/02 165.6° 2h10m +28° 2005/11/02 14.5 2005/11/02 0.936 3998 2005/11/02 172.2° 2h24m +22° 2005/11/03 14.5 2005/11/08 0.917 Even in the early days, low phase angle observations were 19 2005/11/04 179.4° 2h39m +14° 2005/11/04 8.9 2005/11/02 1.064 448 2005/11/04 178.4° 2h36m +17° 2005/11/04 14.0 2005/10/28 1.851 encouraged. Due to a lack of interest, special note of asteroids 57 2005/11/05 170.1° 2h57m + 6° 2005/11/05 10.9 2005/11/05 1.798 2006 2005/11/07 172.8° 2h42m +23° 2005/11/07 14.1 2005/11/03 0.903 reaching low phase angles was dropped but, as noted in the past 694 2005/11/11 179.3° 3h 7m +18° 2005/11/11 11.2 2005/10/29 1.116 Minor Planet Bulletin, such notices have made a comeback. We 4121 2005/11/11 177.6° 3h 7m +19° 2005/11/11 14.5 2005/10/31 1.145 14835 2005/11/11 175.1° 2h55m +21° 2005/11/10 14.4 2005/11/02 0.796 highlight them again because they provide some unique 951 2005/11/12 176.5° 3h 4m +21° 2005/11/12 12.7 2005/11/07 0.863 opportunities to contribute some important data to asteroid studies, 418 2005/11/15 176.7° 3h20m +21° 2005/11/15 12.4 2005/11/12 1.346 1771 2005/11/18 170.6° 3h42m +10° 2005/11/18 13.5 2005/11/16 1.587 beyond the already important work of finding the periods for more 2044 2005/11/21 173.1° 3h49m +26° 2005/11/22 14.0 2005/11/30 0.689 difficult targets (long period, low amplitude, etc.) and getting 503 2005/11/22 178.5° 3h51m +18° 2005/11/22 11.8 2005/11/26 1.382 712 2005/11/28 173.5° 4h23m +15° 2005/11/28 10.5 2005/11/25 1.116 higher quality curves to fill in the small gaps and so allow shape 1862 2005/12/01 161.8° 4h 6m +39° 2005/11/13 13.3 2005/11/06 0.075 4577 2005/12/02 175.9° 4h36m +26° 2005/12/03 14.1 2005/12/12 1.043 and pole modeling to be tried on a given asteroid.

1671 2005/12/03 172.2° 4h43m +14° 2005/12/03 13.6 2005/12/01 0.935 629 2005/12/06 176.6° 4h51m +19° 2005/12/06 13.5 2005/12/09 1.754 34706 2005/12/06 176.2° 4h53m +26° 2005/12/07 14.2 2005/12/20 0.461 The main “tricks” for working asteroids at their smallest phase 2464 2005/12/07 178.6° 4h53m +23° 2005/12/07 14.5 2005/12/08 1.513 1407 2005/12/08 177.6° 4h58m +25° 2005/12/07 12.9 2005/11/28 1.207 angle is having the event be when it’s dark, the asteroid is up, the skies are clear, and the full moon isn’t five degrees away. After 3 2005/12/09 155.1° 5h13m - 1° 2005/12/07 7.7 2005/12/04 1.063 164 2005/12/12 176.6° 5h22m +26° 2005/12/12 11.1 2005/11/29 1.188 that, it’s all “skittles and beer” as the old saying goes. Actually, 481 2005/12/13 175.6° 5h23m +27° 2005/12/13 11.3 2005/12/10 1.355 60 2005/12/21 173.0° 5h58m +16° 2005/12/21 9.9 2005/12/23 0.985 it’s not but you have no control over those aspects, so all you can 814 2005/12/24 177.1° 6h15m +26° 2005/12/24 11.9 2005/12/14 1.551 do is hope the Fates are in your favor. 1083 2005/12/27 177.3° 6h24m +26° 2005/12/27 14.1 2005/12/29 0.937 1687 2005/12/28 179.5° 6h27m +23° 2005/12/28 13.6 2005/12/23 1.713 384 2005/12/29 172.4° 6h39m +30° 2005/12/29 12.3 2005/12/28 1.291 1578 2005/12/31 179.4° 6h41m +23° 2005/12/31 14.3 2005/12/28 2.054 You need to get one good time series to define the lightcurve accurately. This is so that partial coverage on other nights to define the phase curve can be accurately related to one another. Next, you need observations at a large phase angle, well outside the 7° range, before and after opposition to remove the aspect variation of brightness from the phase angle variation. Finally, to maximize your efforts, a good and adequate sampling of phase angles can be had by observing at factors of two. For example, observe when the phase angle is near zero, 1°, 2°, 4°, 8°, 16°, and Minor Planet Bulletin 32 (2005) 23 as large as possible. You don’t have to hit these values exactly, or Lightcurve Opportunities even closely, just try to avoid gaps of more than a factor of two in phase angle. More is better but this serves as a minimum Brightest # Name Date Mag Dec U Per. Amp. sampling. ------2075 Martinez 1 01.7 14.5 + 9 0 Unfortunately, especially at large phase angles, the asteroid may 6838 Okuda 1 06.6 14.7 + 7 0 181 Eucharis 1 08.8 11.3 + 4 2 >24. 0.15 fade one or two magnitudes in the process. You’ll have to make 2647 Sova 1 08.2 14.2 +23 0 sure to maintain the quality of the data throughout. This can be 305 Gordonia 1 09.0 12.0 +15 2 16.2 0.16 difficult when using a filter, which is another requirement since 752 Sulamitis 1 09.7 12.7 +26 1 10. 0.04 2463 Sterpin 1 11.1 14.7 + 0 0 the absolute values you provide for H/G determination must be on 6161 Vojno-Yasenetsky 1 19.7 14.9 +15 0 a standard system. V is preferred but R will do as well. You just 4006 Sandler 1 21.6 14.9 +19 0 1708 Polit 1 23.1 14.3 + 9 0 need to be sure to indicate which band was being used. 42600 1997 YF10 1 23.1 14.8 +27 0 4706 1988 DR 1 23.0 15.0 + 6 0 Our concentration of late on low phase angle work doesn’t mean 1936 Lugano 1 26.4 14.1 + 7 0 1815 Beethoven 1 29.6 14.6 +19 0 you should forsake all other asteroids. In fact, there is considerable 1454 Kalevala 2 01.9 14.7 +23 0 interplay among the three lists. Phase work requires at least one 16955 1998 KU48 2 03.7 14.7 +28 0 good light curve, which is required for pole/shape modeling. 1483 Hakoila 2 03.3 14.1 +23 0 3895 Earhart 2 10.7 14.5 + 6 0 Whatever your concentration, you’re putting important 1559 Kustaanheimo 2 28.4 13.8 + 7 0 information into the overall data pool. Thanks in part to some 22753 1998 WT 3 02.0 14.3 + 2 2 <11. MPB readers, the list of pole/shape candidates maintained by 1927 Suvanto 3 03.5 14.6 +22 0 1630 Milet 3 03.0 14.5 +13 0 author Kaasalainen shrank a little in 2004. There are several good 5878 Charlene 3 11.1 14.6 + 8 0 candidates this quarter and we strongly encourage pursuit of those. 3445 Pinson 3 12.6 15.0 - 3 0 2103 Laverna 3 12.0 14.2 - 7 0 2544 Gubarev 3 17.8 14.5 -34 ? In the last issue we gave some tips about how to approach 30825 1990 TG1 3 18.5 13.4 - 8 0 lightcurve work. We’d like to add one more. As has often been 1924 Horus 3 23.9 14.7 - 2 ? said in science, “the lack of results can be just important as actual 3617 Eicher 3 24.7 14.7 - 1 0 329 Svea 3 27.7 12.6 + 1 1 15. 0.26 results.” If you work an asteroid but the period can't be resolved 5692 Shirao 3 28.8 14.7 - 1 2 2.86 0.16 after some reasonable attempt or the first attempt shows that 465 Alekto 3 29.2 12.9 -10 2 8.61 0.1 getting a reasonable result may take more time and effort than you 950 Ahrensa 3 31.8 13.6 + 3 0 can afford, consider publishing the results anyway, even if only summary by way of likely minimums. There are several entries in Low Phase Angle Opportunities the lightcurve list maintained by Harris and Warner where the period is listed as “>X” or “long” and the amplitude is given only # Name Date PhA V Dec as a minimum. This can be useful information in statistical studies ------560 Delila 01 01.3 0.50 13.2 +22 and when someone else starts planning an observing program. In 779 Nina 01 02.5 0.23 12.2 +24 science, the “eighth sin” is “caching”, i.e., keeping seemingly 379 Huenna 01 09.8 0.63 13.4 +20 useless data in the proverbial dusty filing cabinet when brining it 657 Gunlod 01 13.0 0.60 13.9 +23 8 Flora 01 14.6 0.32 8.4 +22 out may provide a critical link to other existing data. 1021 Flammario 01 16.1 0.03 11.5 +21 618 Elfriede 01 18.9 0.92 12.9 +24 868 Lova 01 19.4 0.21 13.3 +21 149 Medusa 01 26.1 0.44 12.8 +18 115 Thyra 01 27.2 0.30 9.8 +19 383 Janina 01 28.1 0.77 13.8 +20 52 Europa 02 02.7 0.35 9.9 +18 133 Cyrene 02 06.7 0.08 12.2 +16 171 Ophelia 02 07.6 0.90 11.9 +18 830 Petropolitana 02 08.0 0.67 13.4 +17 622 Esther 02 08.8 0.24 12.9 +14 130 Elektra 02 14.1 0.06 11.7 +13 112 Iphigenia 02 16.6 0.11 13.3 +12 1069 Planckia 02 17.9 0.85 13.0 +14 231 Vindobona 02 18.1 0.97 13.3 +15 1559 Kustaanheimo 02 28.4 0.59 13.8 +07 169 Zelia 03 02.5 0.81 12.9 +09 218 Bianca 03 12.3 0.16 11.5 +04 477 Italia 03 17.9 0.72 13.9 +03 431 Nephele 03 19.4 0.65 13.7 +03 209 Dido 03 22.2 0.04 12.3 -01 104 Klymene 03 23.2 0.84 12.7 +02 501 Urhixidur 03 23.4 0.78 13.9 -04 339 Dorothea 03 24.0 0.73 13.7 +01 308 Polyxo 03 29.0 0.27 11.7 -03 29 Amphitrite 03 30.4 0.84 9.2 -06 186 Celuta 03 30.8 0.78 12.2 -02 444 Gyptis 03 31.4 0.43 12.2 -05

Minor Planet Bulletin 32 (2005) 24

Shape/Spin Modeling Opportunities THE MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly journal of the Minor Planets Section of the Association of Lunar and Brightest Per Planetary Observers – ALPO. Beginning with volume 32, the current and # Name Date Mag Dec (h) Amp. U most recent issues of the MPB are available on line, free of charge at ------http://www.minorplanetobserver.com/mpb/default.htm. Subscription 30 Urania 1 01. 9.9 +25 13.686 0.11-0.45 3 40 Harmonia 1 01. 11.2 +04 8.910 0.15-0.36 4 information for conventional printed copies is given below. 80 Sappho 1 01. 11.1 +11 14.030 0.1 -0.40 3 238 Hypatia 1 01. 12.3 +04 8.86 0.12-0.15 4 Nonmembers are invited to join ALPO by communicating with: Matthew 283 Emma 1 01. 13.2 +30 6.888 0.31 3 L. Will, A.L.P.O. Membership Secretary, P.O. Box 13456, Springfield, IL 324 Bamberga 1 01. 11.0 -03 29.43 0.07 3 62791-3456 ([email protected]). The Minor Planets Section is 423 Diotima 1 01. 11.9 +29 4.775 0.06-0.18 4 directed by its Coordinator, Prof. Frederick Pilcher, Department of 505 Cava 1 01. 12.6 +04 8.1789 0.23 3 944 Hidalgo 1 01. 14.4 +46 10.063 0.35-0.60 3 Physics, Illinois College, Jacksonville, IL 62650 USA 377 Campania 1 02.5 12.3 +13 8.507 0.16 3 ([email protected]), assisted by Lawrence Garrett, 206 River Road, 804 Hispania 1 13.0 12.4 +39 14.840 0.19-0.23 2 Fairfax, VT 05454 USA ([email protected]). Richard Kowalski, 114 Kassandra 1 16.1 11.2 +15 10.758 0.25 3 7630 Conrad St., Zephyrhills, FL 33544-2729 USA ([email protected]) is 59 Elpis 1 26.3 11.7 +10 13.69 0.1 3 Associate Coordinator for Observation of NEO’s, and Steve Larson, Lunar 110 Lydia 2 06.5 11.9 +24 10.927 0.10-0.20 3 487 Venetia 2 10.0 11.8 +21 13.28 0.05-0.30 2 and Planetary Laboratory, 1629 E. University Blvd., University of 196 Philomela 2 21.9 11.0 +20 8.343 0.07-0.37 4 Arizona, Tucson, AZ 85721 USA ([email protected]) is Scientific 83 Beatrix 2 25.0 11.3 +16 10.16 0.18-0.27 4 Advisor. The Asteroid Photometry Coordinator is Brian D. Warner, 218 Bianca 3 12.3 11.5 +04 6.337 0.11-0.24 4 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, 776 Berbericia 3 17.8 12.6 +24 7.668 0.13-0.21 2 CO 80908 USA ([email protected]).

Note that the amplitude in the table just above could be more, or The Minor Planet Bulletin is edited by Dr. Richard P. Binzel, MIT 54-410, less, than what’s given. Use the listing as a guide and double- Cambridge, MA 02139 USA ([email protected]), produced by Dr. Robert A. check your work. Also, if the date is ‘1 01.’ Or ’12 31. ‘, i.e., there Werner, JPL MS 301-150, 4800 Oak Grove Drive, Pasadena, CA 91109 is no value after the decimal, it means that the asteroid reaches its USA (robert.a.werner@jpl.nasa.gov), and distributed by Derald D. Nye. brightest just as the year begins (it gets dimmer all year) or it The contact for all subscriptions, contributions, address changes, etc. is: reaches its brightest at the end of the year (it gets brighter all year). Mr. Derald D. Nye Minor Planet Bulletin Go to the CALL site at 10385 East Observatory Drive http://www.MinorPlanetObserver.com/astlc/default.htm Corona de Tucson, AZ 85641-2309 USA for a more complete listing of potential lightcurve targets, ([email protected]) (Telephone: 520-762-5504) including links to those for shape/pole modeling and low phase angles. Annual subscription rates for the Minor Planet Bulletin by postal delivery:

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Minor Planet Bulletin 32 (2005)