THE

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

VOLUME 35, NUMBER 3, A.D. 2008 JULY-SEPTEMBER 95.

ASTEROID LIGHTCURVE ANALYSIS AT SCT/ST-9E, or 0.35m SCT/STL-1001E. Depending on the THE PALMER DIVIDE OBSERVATORY: binning used, the scale for the images ranged from 1.2-2.5 DECEMBER 2007 – MARCH 2008 arcseconds/pixel. Exposure times were 90–240 s. Most observations were made with no filter. On occasion, e.g., when a Brian D. Warner nearly full moon was present, an R filter was used to decrease the Palmer Divide Observatory/Space Science Institute sky background noise. Guiding was used in almost all cases. 17995 Bakers Farm Rd., Colorado Springs, CO 80908 [email protected] All images were measured using MPO Canopus, which employs differential aperture to determine the values used for (Received: 6 March) analysis. Period analysis was also done using MPO Canopus, which incorporates the Fourier analysis algorithm developed by Harris (1989). Lightcurves for 17 were obtained at the Palmer Divide Observatory from December 2007 to early The results are summarized in the table below, as are individual March 2008: 793 Arizona, 1092 Lilium, 2093 plots. The data and curves are presented without comment except Genichesk, 3086 Kalbaugh, 4859 Fraknoi, 5806 when warranted. Column 3 gives the full range of dates of Archieroy, 6296 Cleveland, 6310 Jankonke, 6384 observations; column 4 gives the number of data points used in the Kervin, (7283) 1989 TX15, 7560 Spudis, (7579) 1990 analysis. Column 5 gives the range of phase angles. If there are TN1, (13578) 1993 MK, (24819) 1994 XY4, (26471) three values in the column, the phase angle reached a minimum 2000 AS152, (26916) 1996 RR2, and 2008 CN1. with the middle value being the minimum. Columns 6 and 7 give the range of values, or average if the range was relatively small, Observations of 17 asteroids were made at the Palmer Divide for the Phase Angle Bisector (PAB) longitude and latitude Observatory from December 2007 into early March 2008. One of respectively. Columns 8 and 10 give the period and amplitude of four telescopes/camera combinations was used: 0.5m Ritchey- the curve while columns 9 and 11 give the respective errors in Chretien/SBIG STL-1001E, 0.35m SCT/FLI IMG-1001E, 0.35m and magnitudes. An “(H)” follows the name of an

Date Range Data Per Amp (mm/dd) # Name Pts Phase PAB PAB (h) PE (mag) AE 2007/08 L B 793 Arizona 01/26-27 107 20.3 60.7 10.1 7.367 0.005 0.25 0.02 1092 Lilium 02/09–03/04 508 8.0,14.9 118.4 0.3 24.60 0.05 0.30 0.02 2093 Genichesk (B) 02/24-28 200 4.4,6.4 146.1 -0.8 11.028 0.006 0.24 0.02 3086 Kalbaugh (H) 01/27-02/02 248 5.6,4.2 133.0 -5.6 5.1790 0.0003 0.47 0.02 4859 Fraknoi (B) 02/06-13 304 10.4,14.1 120.0 -0.6 7.846 0.003 0.15 0.02 5806 Archieroy (H) 01/26-02/06 642 3.6,10.9 120.1 -1.5 12.163 0.011 0.45 0.02 15.65 6296 Cleveland (H) 01/11-15 462 7.9,10.2 101.1 -5.0 0.01 0.11 0.02 31.54 6310 Jankonke (H) 01/14-15 234 16.0 120.1 22.5 3.080 0.003 0.14 0.02 6384 Kervin (H) 12/29-01/13 270 8.4,15.7 90.7 12.7 3.647 0.001 0.06 0.2 7283 1989 TX15 (B) 02/24-28 181 3.4,3.7 155.8 5.2 2.6747 0.0005 0.19 0.02 7560 Spudis (H) 01/26-02/13 328 4.2,12.8 125.0 -7.5 3.5448 0.0004 0.10 0.02 7579 1990 TN1 (H) 12/18-01/05 704 15.4,20.5 75.8 20.3 18.312 0.001 1.10 0.03 13578 1993 MK (H) 12/29-01/12 257 20.2,24.0 71.9 -18.0 7.924 0.003 0.09 0.01 27.73 0.04 24819 1994 XY4 12/29-01/12 584 7.3,17.3 90.0 7.3 0.04 0.01 57.57 0.09 26471 2000 AS152 (H) 02/06-16 193 12.3,16.0 122.0 -17.2 2.687 0.001 0.20 0.02 26916 1996 RR2 (H) 12/29-01/02 342 11.4,10.8 100.3 16.6 10.324 0.003 1.05 0.03 2000 CN1 02/16-24 475 23.6,22.7 158,147 6.0,-2.8 6.0555 0.0002 1.04 0.02 Minor Planet Bulletin 35 (2008) Available on line http://www.minorplanetobserver.com/mpb/default.htm 96 in the table if it is a member of the Hungaria group or family. A the 3.54 h solution in 2008 was not as dominant though still “(B)” follows the name if the asteroid is a member of the significant. Additional data are needed to resolve the ambiguity. Baptistina family. The latter are thought to have been recently formed (160 MY) from a catastrophic collision (Bottke et al., (7579) 1990 TN1. The solution is considered unique since a half- 2007. Nature 449, 48-53) and will be targeted by PDO in the period fit shows a well-fitting monomodal curve. However, given future. the amplitude, that shorter period is not likely.

793 Arizona. This is a follow up to work by the author in early (13578) 1993 MK. Some longer periods were possible but December 2007 (Warner 2008) to determine how the shape and required tri- and multimodal curves and so were rejected as being amplitude changed with increased phase angle. The synodic highly unlikely. period, 7.367 ± 0.005 h, was about 0.03 h less than in December and the amplitude about 0.03 mag greater. Unfortunately, there are (26471) 2000 AS152. The period agrees with the posted by insufficient data from other apparitions, dense or sparse, to Behrend (2008). generate a model at this time. 2008 CN1. This Aten asteroid’s aphelion reaches just beyond the 1092 Lilium. Binzel (1987) reported a period of either 15.66 or Earth’s. It was only 0.044-0.051 AU from Earth when observed in 17.63 based on four nights of data and settled on the latter based February 2008. As might be imagined, it was moving rapidly on the overlap of data points. A search from 15-30 hours using the across the sky and so 13 different sets of comparison were 2008 data from PDO found a synodic period of 24.60 ± 0.05 h, required for the 16 February observations but only 7 for the one on which was twice as strong (0.025 versus 0.05 mag RMS fit) as the 24 February. Calibration of the multiple sets was done by a Binzel solutions. Given the considerably better RMS fit and nearly process such that the last 3-5 observations of any given set were month-long span of internally-calibrated data, I believe the 24.60 h measured again as the first few observations of the next set. This solution is the correct one. allowed matching common data points to within 0.01 mag.

2093 Genichesk. This was previously worked by Behrend et al. Acknowledgements (2008), who found a period of 11.028 h. Funding for observations at the Palmer Divide Observatory is 3086 Kalbaugh. This is follow up on work by the author in 2004 provided by NASA grant NNG06GI32G, by National Science December (Warner 2005b). The period from 2008 is virtually the Foundation grant AST-0607505, and by a Gene Shoemaker NEO same as before but the amplitude is about 0.1 mag less, likely due Grant from the Planetary Society. to the different viewing aspect. Again, there are insufficient data from other sources for a model, so additional curves are needed in References the future. Behrend, R. (2008). Observatoire de Geneve web site, 5806 Archieroy. This Hungaria was observed to complement data http://obswww.unige.ch/~behrend/page_cou.html from the author obtained in 2004 (Warner 2005a). The same period was found but the 2008 amplitude was about 0.1 mag Binzel, R.P. (1987). Icarus 72, 135-208. greater. Data from future apparitions will be needed for modeling. Warner, B.D. (2005a). Minor Planet Bulletin 32, 29-32. 6296 Cleveland. This is another Hungaria observed to complement data from previous work by the author (Warner 2006a). The Warner, B.D. (2005b). Minor Planet Bulletin 32, 54-58. synodic period for 2008 was 15.65 ± 0.01 h. However, a longer Warner, B.D. (2006a). Minor Planet Bulletin 33, 85-88. period of 31.54 h, representing a bimodal curve, cannot be ruled out. The 2006 period was 15.38 h with an amplitude of 0.20 mag. Warner, B.D., Pray, D.P., and Pravec, P. (2006b). Minor Planet Usually, that larger amplitude would tend to support to the shorter Bulletin 33, 99. period. However, the data from both apparitions had errors of ±0.03 mag or more, making a definitive solution difficult to find. Warner, B.D. (2008). Minor Planet Bulletin 35, 67-71. Complicating matters was that neither data set could be acceptably forced to fit the period of the other.

6310 Jankonke. This Hungaria was previously worked by the author in 2005 (Warner 2005b). The 2008 synodic period of 3.080 ± 0.003 h is about 0.04 h greater than the one found in 2005. However, a review of that earlier data shows it to be extremely noisy and that a solution of 3.078 h is also possible.

6384 Kervin. The results from 2008 agree with those found by Warner et al. in 2006 (Warner 2006b).

7560 Spudis. A bimodal solution of 3.5488 ± 0.0004 h was found in 2008. However, previous work by the author (Warner 2005a) found a period of 5.402 h (trimodal curve). A search for a period near that value using the most recent data found a trimodal solution at 5.740 h. Furthermore, the 2005 data decidedly favored a period in the 5-6 h range over one between 3-4 h. The strength of

Minor Planet Bulletin 35 (2008) 97

Minor Planet Bulletin 35 (2008) 98

Minor Planet Bulletin 35 (2008) 99

ASTEROID LIGHTCURVE ANALYSIS AT was given to asteroids without previously published lightcurves. THE OAKLEY OBSERVATORY – SEPTEMBER 2007 Asteroids with uncertain periods were also selected in order to potentially validate previous results. Heath Shipley, Alex Dillard, Jordan Kendall, Matthew Reichert, Jason Sauppe, Nelson Shaffer, To our knowledge, no previous observations have been reported Thomas Kleeman, Richard Ditteon for 256 Walpurga, 789 Lena, 892 Seeligeria, 1033 Simona, 1411 Rose-Hulman Institute of Technology CM 171 Brauna, 2173 Maresjev, 2976 Lautaro, 3722 Urata, 3971 5500 Wabash Ave. Voronikhin, 5615 Iskander, (8085) 1989 CD8, or (9120) 1998 Terra Haute, IN 47803 DR8. No repeatable pattern could be found for 294 Felicia, 983 [email protected] Gunila, or 3907 Kilmartin. This was due to noisy data and equipment problems. The table below contains all of the results. (Received: 31 January) Comments have been added as necessary.

408 Fama. The period was reported as “long” by Behrend (2006) Data were collected for 17 asteroids over eight nights of and by Stephens (2008) as 202.1 h. Our results gave a period of observation during the month of September 2007 at the about 12 hours, but with very low amplitude. We do not have Oakley Observatory. The asteroids were 256 Walpurga, enough data to rule out a longer period. 294 Felicia, 408 Fama, 789 Lena, 892 Seeligeria, 983 Gunila, 1033 Simona, 1411 Brauna, 2173 Maresjev, 3915 Fukushima. Our results disagree with the period of 2976 Lautaro, 3722 Urata, 3907 Kilmartin, 3915 8.4 h reported by Warner (2004). We could not make our data fit Fukushima, 3971 Voronikhin, 5615 Iskander, (8085) the 8.4 h period. 1989 CD8, and (9120) 1998 DR8. Acknowledgement

A total of 17 asteroids were observed during the nights of This research was supported in part by NASA through the 1-4, 13-15, and 17 September 2007. The observations were made American Astronomical Society’s Small Research Grant Program at the Oakley Observatory at Rose-Hulman Institute of Technology in Terre Haute, Indiana. The data that were collected References enabled us to find lightcurves for 14 asteroids. Out of those 14 lightcurves, 12 were previously unrecorded while the remaining Behrend, R. (2006). two did not agree with previously published results. http://obswww.unige.ch/~behrend/page_cou.html

Three telescopes were used throughout the eight days of Stephens, R.D. (2008). “Long Period Asteroids Observed from observation. Each telescope was a 14-inch Celestron optical tube GMARS and Santana Observatories.” Minor Planet Bulletin 35, assembly mounted on a Paramount ME. The telescopes were set 21-22. up with an STL-1001E CCD camera from Santa Barbara Instrument Group. Each CCD had a clear filter and an image scale Warner, B.D. (2004). “Rotation Rates for Asteroids 875, 926, of 1.94 arcseconds per pixel. All of the exposure times were four 1679, 1796, 3915, 4209, and 34817,” Minor Planet Bulletin 31, minutes. Images were calibrated with CCDSoft using master 19-22. twilight flats, darks, and bias frames. Processed images were measured using MPO Canopus. Asteroids were selected based on their sky position approximately one after sunset. Priority

Dates (2007) Data Period P.E. Amp. A.E. Number Name mm/dd Points (h) (h) (mag) (mag) 256 Walpurga 9/1, 9/2, 9/4 68 16.64 0.02 0.38 0.02 294 Felicia 9/13, 9/15, 9/17 23 - - 0.35 0.07 408 Fama 9/1, 9/2, 9/4, 9/15, 9/17 75 12.19 0.02 0.15 0.03 789 Lena 9/15, 9/17 42 5.85 0.05 0.5 0.01 892 Seeligeria 9/13, 9/14, 9/15, 9/17 55 15.78 0.04 0.35 0.07 983 Gunila 9/17 11 - - 0.25 0.05 1033 Simona 9/1, 9/2, 9/3, 9/4 56 10.07 0.06 0.15 0.05 1411 Brauna 9/1, 9/2, 9/3 116 4.90 0.01 0.15 0.05 2173 Maresjev 9/1, 9/2, 9/3 57 11.6 0.1 0.5 0.05 2976 Lautaro 9/1, 9/2, 9/3 49 17.41 0.08 0.16 0.01 3722 Urata 9/2, 9/4 47 5.565 0.005 0.58 0.05 3907 Kilmartin 9/13, 9/14, 9/17 25 - - 0.45 0.1 3915 Fukushima 9/1, 9/2, 9/3, 9/4 49 9.41 0.01 0.52 0.02 3971 Voronikhin 9/3 20 5.41 0.14 0.21 0.05 5615 Iskander 9/1, 9/2 76 5.415 0.011 1.05 0.1 8085 1989 CD8 9/1, 9/2, 9/3, 9/4 40 7.75 0.05 0.45 0.05 9120 1998 DR8 9/1, 9/2, 9/3 51 14.76 0.09 0.16 0.02 Minor Planet Bulletin 35 (2008) 100

Minor Planet Bulletin 35 (2008) 101

PHOTOMETRIC OBSERVATIONS OF THE NEAR EARTH ASTEROIDS 1989 UR AND 2007 XH16

Alberto Silva Betzler, Alberto Brum Novaes Projeto “Descobrindo o Céu”, (“Discovering the Sky” Project) Departamento de Fisica da Terra e do Meio Ambiente Instituto de Fisica, Universidade Federal da Bahia (IF-UFBA), Salvador, Estado da Bahia, BRAZIL [email protected]

(Received: 17 January)

The NEAs 1989 UR and 2007 XH16 were observed in November and December from Salvador, Bahia, Brazil. The synodic period of 2007 XH16 is estimated to be 3.75 ± 0.03 h, with amplitude of 0.54 ± 0.09 mag. For 1989 UR, V-R = 0.42 ± 0.05 and for 2007 XH16 V-R = 0.513 ± 0.006.

Apollo group asteroids 1989 UR and 2007 XH16 have been listed by the as Potentially Hazardous Asteroids (PHA). Observations of the two were made by Arecibo and Goldstone in November and December 2007. At that time optical photometry was requested to compliment the radar data. In response, we obtained observations of the two asteroids in December 2007 using a Meade LX-200 GPS 0.3m /f3.3 telescope and SBIG ST-7XME CCD camera. Observations were made with V and R filters to investigate the synodic period, the V-R color index, and the amplitude-phase dependency. Minor Planet Bulletin 35 (2008) 102

All images were bias, dark, and flat-field corrected. MPO Canopus Holmberg, J. Flynn, C. Portinari, L. (2006). “The colours of the v9.3.1.0 was used for photometric reductions and period searches .” MNRAS 367, 449. via Fourier analysis. In order to increase the SNR of target and stars when finding the V-R values, the images were aligned using Kidger, M. R. (2003). “Amateur CCD Photometry of : the “rregister” and “trans2” routines and then added with the How to Standardise Data”. www.astrosurf.com/comets/tecnicas/ “add2” routine of IRIS v5.52 (Buil, 2008). The b and r magnitudes MACE_photometry_proceeding.htm. of USNO A2 field stars were used for photometric calibration (Kidger, 2003; Gary, 2006). We found only a limited number that Monet et al. (2003). “USNO-B Catalogue.” Astrophys. J. 125, met our requirements of 0.3 < V-R < 0.6, as suggested by Binzel 984. (2005), V magnitudes similar to the object, and a near-solar B-V colour index (B-V = 0.654, Holmberg et al, 2006). Presumably, Pravec, P., Hergenrother, C., Whiteley, R., Šarounová, L., the cause for finding so few reference stars is the uncertainty of Kušnirák, P., Wolf, M. (2000). “Fast Rotating Asteroids the b and r magnitudes, i.e., around 0.3 mag for the USNO B 1999 TY2, 1999 SF10, and 1998 WB2.” Icarus 147, 477. catalogue (Monet et al., 2003). Zappala, V., Cellino, A., Barucci, A. M., Fulchignoni, M., 1989 UR. Observations of this asteroid were made on 16 Nov Lupishko, D. F., (1990). “An Analysis of the Amplitude-Phase 2007. Forty images of 20 s exposure in V and R were obtained. Relationship Among Asteroids.” Astron. & Astrophys. 231, 548. These were used to find a colour index of V-R = 0.42 ± 0.05. Due to poor weather conditions, we were not able to obtain sufficient data to find the period of the asteroid. Binzel et al. (2004) reported finding a period of 73.0 ± 0.5 h and a taxonomic class of S.

2007 XH16. This asteroid was observed on three nights, 21-23 December, 2007. Short exposures, 20 s, were required in order to keep the profile of the fast-moving asteroid somewhat stellar. Using 486 observations obtained on 21-22 December (Fig. 1), we found a synodic period of 3.75 ± 0.03 h. Casulli (2007) preliminarily reported a period of 4.1 h based on observations on 22 December 2007. However his data are incomplete, covering only two hours, or about one-half the estimated period. Due to large errors on 21 December, it was not possible to find a definitive relation of the amplitude versus longitude. The amplitude on 22 December was 0.54 ± 0.09 (Fig. 2). From this, the S taxonomic classification, and applying the correction for the amplitude at zero phase angle (Zappalá et al., 1990; Pravec et al., 2000), the a/b axis ratio of the asteroid is estimated to be ≥ 1.2. In addition, eighteen observations from 23 December were used to find V-R = 0.513 ± 0.006.

Acknowledgments Fig. 1. Differential lightcurve of 2007 XH16. 0% phase Thanks to The Vitae Foundation, MCT (Ministry of Science and corresponds to JD 2454456.490051, corrected for light-time technology) and the Institute of Physics of UFBA (IF-UFBA) for supporting the “Discovering the Sky” Project.

References

Benner, L.A.M., 2007, “(11500) 1989 UR Planning.” www:echo.jpl..gov/asteroids/1989UR/1989UR_planning.html

Binzel, R.P, Rivkkin, A.S., Stuary, J.D., Harris, A.W., Bus, S.J., Burbine, T.H. (2004). “Observed Spectral Properties of Near- Earth Objects: Results for Population Distribution, Source Regions, and Space Weathering Processes.” Icarus 170, 259.

Binzel, R. P. (2005). “A Simplified Method for Standard Calibration”. Minor Planet Bulletin 32, 93-95.

Buil, C., 2008, “IRIS Astronomical Image Processing Software.” www: http://astrosurf.com/buil/us/iris/iris.htm.

Casulli, S. (2007). “2007 XH16.” www:obswww.unige.ch/ ~behrend/r07x16ha.png Fig. 2. Differential lightcurve of 2007 XH16 on 22 Dec 2007. The Gary, L. B. (2006). “USNO 2.0 Download Method#5”. X-axis is + JD 2454457.0, corrected for light-time. www.brucegary.net/dummies/USNO-A2_Method.htm. Minor Planet Bulletin 35 (2008) 103

LIGHTCURVE ANALYSIS OF 3415 DANBY Acknowledgements

Brian D. Warner Funding for observations at the Palmer Divide Observatory is Palmer Divide Observatory/Space Science Institute provided by NASA grant NNG06GI32G, by National Science 17995 Bakers Farm Rd., Colorado Springs, CO 80908 Foundation grant AST-0607505, and by a 2007 Shoemaker NEO [email protected] Grant from the Planetary Society. The SBIG ST-8E used by Hunters Hill was funded by The Planetary Society under the 2005 David Higgins Gene Shoemaker NEO Grants program. The authors thank Alan Hunters Hill Observatory, Ngunnawal, Canberra 2913 Harris, Space Science Institute, and , Astronomical AUSTRALIA Institute, Czech Republic for their analysis and comments.

(Received: 5 March) References

Behrend, R. (2008). Observatoire de Geneve web site, The authors observed the main-belt asteroid 3415 Danby http://obswww.unige.ch/~behrend/page_cou.html. in November 2007 following reports that it might be binary. We found no evidence supporting a binary Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., nature but did find the lightcurve to be unusual in that it Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, has four maxima/minima pairs per rotation. We H., and Zeigler, K.W. (1989). “Photoelectric Observations of determined the synodic period to be 5.667 ± 0.001 h and Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. the lightcurve amplitude 0.13 ± 0.01 mag.

In early November 2007, Raoul Behrend put out a call for observations of 3415 Danby after initial data indicated the possibility of the asteroid being binary. The authors responded to that call and worked in collaboration. At the Palmer Divide Observatory, a 0.50-m Ritchey-Chretien and FLI-1001E were used for 180-second exposures. Hunters Hill employed a 0.35-m SCT with an SBIG ST-8E at 1x1 binning (9 µm pixels) and 180-second exposures. All images were processed with dark frames and flat fields. We used MPO Canopus for aperture photometry of the images. Period analysis was also done in Canopus, which includes an implementation of the Fourier analysis algorithm by Alan Harris (1989). We obtained five runs of data from November 9-13. Of particular note were the two runs on November 11 (UT) which, combined, went for 11 hours: 0600 to 1500 UT. The coverage was not continuous, there being a gap between 0830 and 1100 UT.

Higgins was the first to note that the initial data set that included Fig. 1. Lightcurve of 3415 Danby phased to 5.666 h. PDO data are the November 11 run could be explained with a quadramodal sessions 1, 2, and 5. Hunters Hill data are sessions 3 and 4. curve, i.e., one with four minima and maxima per rotation. There was sufficient asymmetry in the curve such that a more typical bimodal curve did not explain the data nearly as well. Low- amplitude quadramodal lightcurves are physically plausible, and, although not common, they have been seen in several asteroids in the past. Such curves can be produced by a body of unusual shape, especially if it’s observed at a non-zero phase angle. For example, a cross-section of a cube rotating around an axis parallel with its edges shows a maximum and minimum four times per cycle (Petr Pravec and Alan Harris, private communications). We further note that non-uniform can also create a lightcurve with arbitrary numbers and morphologies of extrema.

A period search using our data showed a unique solution of 5.667 ± 0.01 h and lightcurve amplitude of 0.13 ± 0.01 mag. Using a combined data set from several observers, Behrend (2008) reports a period of 5.67066 ± 0.00007 h, also with a 0.13 mag amplitude. Figure 2 shows the period spectrum of a search from 2 to 22 hours. The solutions less than 5.6 h, near 2.5 and 4.2 h, represent bimodal and trimodal fits of the data, respectively. Visual inspection of the phased plots at those periods reveals a much poorer fit of the data. Fig. 2. Period spectrum for 3415 Danby.

Minor Planet Bulletin 35 (2008) 104

PERIOD DETERMINATION FOR 168 SIBYLLA: covered in a single night. The amplitude of 0.16 +/- 0.02 A COLLABORATION TRIUMPH magnitudes requires instrumental adjustments to match lightcurve segments showing only the rising or falling sections. These may not be as reliable as determinations for shorter period 4438 Organ Mesa Loop objects in which maximum and minimum are observed on the Las Cruces, NM 88011 USA same night. [email protected] Over the large range of phase angles 1.0 to 16.1 degrees Vladimir Benishek encountered in this study, the synodic period and shape and Belgrade Astronomical Observatory amplitude of a lightcurve can change, with the amplitude often Volgina 7, 11160 Belgrade 74, SERBIA increasing with phase angle. The difficulty of accurately adjusting instrumental magnitudes over the rising and descending parts of James W. Brinsfield the lightcurve precludes accurately establishing the change in Via Capote Observatory amplitude. The two maxima retained nearly the same shape 5180 Via Capote, Thousand Oaks CA 91320 USA throughout the apparition, but significant changes in the shape of the minima were found. On 2008 Jan. 11, phase angle 16.1 (Received: 9 February Revised: 7 March) degrees, the minimum at phase 0.50 was deeper than on 2007 Nov. 15 and 17 at phase angle 1.2 degrees. Petr Pravec (2008) The synodic and amplitude of 168 considers this change as likely due to shadowing effects of Sibylla are found to be 47.009 ± 0.003 h and 0.16 ± 0.02 topographic features at increased phased angle. He also states that magnitudes, respectively. the 47 hour period is secure. An even deeper minimum at phase 0.5 was observed only on 2007 Prior to this investigation, only two lightcurve papers about 168 Oct. 16 about 23h UT at phase angle 9.7 degrees, but that part of Sibylla appear to have been published. DiMartino et al. (1994) the lightcurve was not sampled again until Nov. 15. The obtained three lightcurves in March 1991 that showed a rounded descending part of this deep minimum was unfortunately lost as minimum followed by a rapid brightening with total amplitude Sibylla passed close to a bright star. This feature seems > 0.3 magnitudes. They estimated the period to be 23.82 hours. excessively deep for a shadowing effect, but we are unable to find Wang and Gu (2003) obtained lightcurves on four consecutive a physical or instrumental cause. nights 2003 Mar. 28-31, each of which showed the magnitude increasing uniformly by about 0.2 magnitudes; they claimed a The amplitude of 0.16 magnitudes observed in 2007-2008, at 24.41 hour period. Because there were no features on their longitudes 55 to 43 degrees, is considerably smaller than those lightcurves, linking the separate sessions was difficult and subject observed by Di Martino et al. (1994) at longitude 160 degrees and to substantial error. Wang and Gu (2003) at longitude 131 degrees. Since both of these authors observed only part of the ascending branches, the actual Due to the long period, which was nearly synchronous with an amplitudes are greater than their observed ranges of 0.3 and 0.2 Earth , a collaboration was formed among the three authors. magnitudes, respectively. This indicates that longitude 49 degrees, Benishek obtained lightcurves 2007 Oct. 16, 17 at Belgrade the mean of the 2007-2008 observations, is considerably closer to Observatory with a Meade 16” LX200 GPS f/10 SC and Apogee the rotational pole. AP47p CCD. Brinsfield obtained lightcurves 2007 Dec. 2, 11, 16 at Thousand Oaks CA, USA, with a 12” Takahashi Cassegrain at prime focus, effective focal ratio f/11.5, and Alta U6 CCD. Pilcher obtained the other 20 lightcurves from 2007 Oct. 6 to 2008 Jan. 11 at Organ Mesa Observatory with a Meade 14” LX200 GPS f/11 SC and SBIG STL 1001-E CCD. Differential photometry and lightcurve construction were made with MPO Canopus. This software made much easier sharing and linking of the data by all three observers. A total of 4626 data points were binned in sets of 10 with a maximum time difference of 20 minutes to make a more readable lightcurve of only 479 points.

Observations were started 2007 Oct. 6, more than a month before opposition. By the end of October it was apparent that extrema observed on successive nights had different appearances, but those on alternate nights looked the same, and corresponding features appeared about one hour earlier on alternate nights. This indicated a period near 47 hours, twice that presumed by the earlier observers. It was desired to continue observations until full phase coverage was achieved with multiple overlap.

It is straightforward to link specific features near the maxima and Future Studies minima which are separated by up to three months. This For 168 Sibylla obtaining a reliable spin/shape model will require establishes a mean synodic period for the entire interval of a large commitment of telescope time at future oppositions. Full observation of 47.009 ± 0.003 h, which we consider reliable. The phase coverage at a single site requires observations on successive interval between minimum and maximum is greater than can be nights, or separated by an odd number of dates, to sample both Minor Planet Bulletin 35 (2008) 105 halves of the lightcurve. Both will need resampling at intervals not all long period rotators and is useful even without prediction of exceeding 8 to 12 days and continuing for a minimum of about 50 extrema. These studies are of special importance because rotation days. Differential photometry alone will suffice to obtain the statistics have become skewed as observers often fail to obtain period and shape of extrema, but as in this investigation, adjusting secure results for long period rotators. the instrumental magnitudes to match rising or falling segments may be less reliable. Acknowledgments

To overcome this limitation, it is suggested that two observers The authors thank Petr Pravec (2008) and referee Brian D. Warner separated by longitude of 5-8 hours (75-120 degrees) collaborate. (2008) for helpful advice. Their combined sessions on a single night should overlap in real time and cover a total time of at least 12 hours, the time between References successive extrema of Sibylla. As soon as an extremum is found, the known 47 hour period enables prediction of times of future Di Martino, M., Blanco, C., Riccioli, D., and De Sanctis, G. extrema. The overlapping sessions can be conducted on a night (1994). Icarus 107, 269-275. when one extremum occurs early in the session of the eastern observer and the next occurs late in the session of the western Pravec, P. (2008). personal communication observer. If the collaborating observers use the same comparison stars and identical filters, then their two combined lightcurves can Wang, X.-B. and Gu, S.-H. (2003). Earth, Moon, and Planets 93, establish the amplitude with differential photometry alone. This 275-280. method of two observers widely separated in longitude obtaining Warner, B. D. (2008). personal communication. overlapping lightcurves with identical filters is recommended for

CCD PHOTOMETRY OF SIX ASTEROIDS FROM THE The targets were selected from the list of asteroid photometry UNIVERSIDAD DE MONTERREY OBSERVATORY opportunities published by Brian Warner on his Collaborative Asteroid Lightcurve Link (CALL) website (Warner, 2007). The Pedro V. Sada selection criteria used were not stringent since we were testing the Departamento de Física y Matemáticas new imager. Some asteroids were bright, others faint, some with Universidad de Monterrey provisionally known periods, others with unknown ones, and still Av. I. Morones Prieto 4500 Pte. others were targets of opportunity. In all cases the images were Garza García, N.L., 66238 obtained unfiltered, binned 2x2, and the detector set MÉXICO to –20 C. Exposure times were 120 seconds (guided) and standard [email protected] dark-current and flat-field field corrections were applied. The image measurements and period analysis was performed using (Received: 27 February 2008) MPO Canopus (Warner, 2008).

The results for each asteroid are summarized and commented CCD photometry of six asteroids was obtained at the below. The individual plots are presented afterwards. Universidad de Monterrey Observatory during January and February 2008. The resulting synodic rotation 1292 Luce. This asteroid was observed on five nights over a four- periods and amplitudes are as follows: 1292 Luce, week interval. The resulting synodic period was 6.9541 ± 0.0002 h 6.9541 ± 0.0002 h, 0.20 ± 0.01 mag; 1303 Luthera, and the amplitude 0.20 ± 0.01 mag. The lightcurve was well 5.878 ± 0.003 h, 0.08 ± 0.01 mag; 1900 Katyusha, sampled and shows an irregular shape. The only other report for 9.4999 ± 0.0001 h, 0.72 ± 0.02 mag, 2807 Karl Marx, this asteroid corresponds to R. Behrend (2008) who reports a 8.842 ± 0.001 h, 0.40 ± 0.05 mag; 3409 Abramov, provisional period of 6.696 ± 0.216 hours from only one night of 7.791 ± 0.002 h, 0.55 ± 0.02 mag; and 9117 Aude, observations by R. Roy on February 13, 2008. 2.8156 ± 0.0001 h, 0.20 ± 0.01 mag. 1303 Luthera. This asteroid was observed on only two nights The observations reported here were made with the Meade 36-cm separated by four days in February 2008. The resulting synodic LX200GPS telescope of the Universidad de Monterrey period was 5.878 ± 0.003 h and the amplitude 0.08 ± 0.01 mag. Observatory (MPC 720). The telescope is permanently mounted in Although the amplitude was small, we are confident of the result a 6-foot fiberglass dome that has recently been automated and is since the lightcurve was well-sampled on both nights. No other operated from a nearby warm room. The CCD camera used was an reports were found for this asteroid. SBIG STL-1301E with a 1280x1024_16µm KAF-1301E/LE chip. 1900 Katyusha. This asteroid was observed on four nights over a The field-of-view is ~21.1x16.9 arcminutes with an image scale of about 1 arcseconds/pixel. This new instrument was obtained three-week interval. The resulting synodic period was 9.4999 ± thanks to a grant from the Consejo Nacional de Ciencia y 0.0001 h and the amplitude 0.72 ± 0.02 mag. The observed lightcurve was well-sampled and exhibits a nominal bimodal Tecnología of Mexico to upgrade the equipment of the observatory. With it we can now perform more efficient asteroid shape with large amplitude. This asteroid is also found on the photometry on fainter targets. These are the first results published website maintained by R. Behrend (2008). He reports a with the use of the upgraded equipment. provisional rotation period of 9.312 ± 0.096 h from one night of observations on February 11, 2005 by R. Poncy. Their lightcurve shows a magnitude variation of about 0.5 magnitudes, a bit lower than our observed amplitude from observations three later. Minor Planet Bulletin 35 (2008) 106

DeGraff and Kern (2001) also report having observed this asteroid in 2000-01, but no mention is made of their results in the abstract.

2807 Karl Marx. This asteroid was observed on three nights over a span of almost three weeks. The resulting synodic period was 8.842 ± 0.001 h and the amplitude 0.40 ± 0.05 mag. The asteroid amplitude has larger uncertainties since it was close to the magnitude limit of our system. No other reports were found for this asteroid.

3409 Abramov. This asteroid was observed on three nights over a span of only one week. It was found on the same field-of-view as 1292 Luce on January 28 and thus followed as a target of opportunity. The resulting synodic period was 7.791 ± 0.002 h and the amplitude 0.55 ± 0.02 mag. The observed lightcurve is bimodal and nearly symmetric. For this asteroid, R. Behrend (2008) reports a provisional rotation period of 8.976 ± 0.36 h from only one night of observations by R. Roy on February 13, 2008.

9117 Aude. This asteroid was observed on three nights over a span of three weeks. The resulting synodic period was 2.8156 ± 0.0001 h and the amplitude 0.20 ± 0.01 mag. The observed lightcurve is bimodal and symmetric. The short rotation period of the asteroid permitted sampling the lightcurve more than once over an observing session. For this asteroid, R. Behrend (2008) initially reported a provisional period of 2.81136 ± 0.00072 h and amplitude of 0.25 ± 0.05 mag from observations performed in 2001. He also reports a final rotation period of 2.8158 ± 0.0001 h and amplitude of 0.203 ± 0.013 mag from observations undertaken on five nights between January 9 and February 3, 2008. Behrend’s result is consistent with the one reported here within the uncertainty estimations, though his is based on more observing sessions over a larger time span, and thus should be more accurate.

Acknowledgments

We would like to thank the Consejo Nacional de Ciencia y Tecnología (CONACYT) of Mexico for the grant (Fondo Institucional, Apoyo Complementario 2006, No. 52274 – Area I) that made it possible to upgrade the equipment of the Universidad de Monterrey observatory. We also thank Brian Warner for his continuous support of the software MPO Canopus, which really makes asteroid lightcurve work much easier and enjoyable.

References

Behrend, R. (2008). “Asteroids and Comets Rotation Curves, CdR.” http://obswww.unige.ch/~behrend/page_cou.html.

DeGraff, D.R., and Kern, J.S. (2001). “Differential Photometry of Asteroids 1458, 1758, 1762, 1845, 4084, and 1900.” Bulletin of the American Astronomical Society 33, 1403.

Warner, B.D. (2007). “Collaborative Asteroid Lightcurve Link.” http://www.minorplanetobserver.com/astlc/default.htm.

Warner, B.D. (2008). MPO Software, Canopus version 9.4.0.3 Bdw Publishing, Colorado Springs, CO.

Minor Planet Bulletin 35 (2008) 107

THE PERIOD OF 2167 ERIN night; therefore, it was not possible to rule out the shorter period. Inspection of the Eau Claire data, which appeared to cover just N. Montigiani, W. Benedetti, M. Mannucci, S. Riccetti over one full rotation, indicated a period of approximately 5.8 Osservatorio Astronomico Margherita Hack, Firenze hours. When the two groups’ data were combined, a derived 50018 Scandicci (Florence) ITALY period of 5.7186 ± 0.0001 h was obtained and the 6.493 h period was shown to be inconsistent with the data. George Stecher, Lyle Ford, Kayla Lorenzen, Sarah Ulrich Department of Physics and Acknowledgements University of Wisconsin-Eau Claire Eau Claire, WI 54702-4004 USA We thank Brian D. Warner for noting that the Eau Claire group’s [email protected] result could be explained by aliasing in the Osservatorio Hack data, and for encouraging us to work together. The Eau Claire (Received: 30 January) group also thanks the Theodore Dunham Fund for Astrophysics, the National Science Foundation (award number 0519006), the University of Wisconsin-Eau Claire Office of Research and Analysis of data taken in March and April 2007 by Sponsored Programs, and the University of Wisconsin-Eau Claire groups from Osservatorio Astronomico Margherita Hack Blugold Fellow and McNair programs for financial support. and the University of Wisconsin-Eau Claire indicates a likely period of 5.7186 ± 0.0001 h for 2167 Erin. The References amplitude of the lightcurve was 0.53 ± 0.02 mag. Montigiani, N., Benedetti, W., Mannucci, M., Riccetti, S. (2007). The group from Osservatorio Astronomico Margherita Hack made measurements of 2167 Erin on nine nights in March and April 2007. Details of these measurements can be found in Montigiani (2007). The Eau Claire group used the 0.6 m “Air Force” Telescope at Hobbs Observatory near Fall Creek, Wisconsin to make measurements of the same asteroid on 20 March 2007. Sixty second images were taken in the R and V bands using Omega Optical filters and an Apogee Alta U55 camera. The images were dark-subtracted and flat-fielded. Photometric transforms were found using Landolt standard stars from the LONEOS catalog and first order extinction coefficients were determined using the modified Hardie method as described in Warner (2006). Data were analyzed using MPO Canopus version 9.3.1.0 (Warner 2007). The magnitude in R was found to vary from 14.1 to 14.7. V data were obtained at the beginning of the night but a filter slider malfunction prevented reliable V measurements later in the night. The problem occurred after the standard fields had been imaged and therefore did not affect the transforms. The Eau Claire lightcurve data can be obtained from http://www.uwec.edu/physics/asteroid/ Figure 1. Lightcurve for 2167 Erin folded with a period of Montigiani (2007) reported a period of 6.493 hours as the most 5.7186 h. The phase is referenced to JD 2454169.349297 and likely result, although a period of 5.72 hours was also consistent times have been corrected for light travel. Symbols 1–10 are the with their data. The two periods differ by about one-half asteroid Osservatorio Hack group’s data. Symbol 28 is the Eau Claire rotation per day, indicating the possibility of aliasing. The group’s R filter data. Osservatorio Hack data contained only partial rotations on each Minor Planet Bulletin 35 (2008) 108

“Lightcurve of Minor Planet 2167 Erin,” Minor Planet Bulletin, Our observations were made on 2008 January 8, generating 16 34, 111-112. CCD images. Exposures were 20s each in BVRI filters. We found B-V = 0.81 ± 0.09, V-R = 0.48 ± 0.09, and R-I = 0.56 ± 0.09. Warner, B. D. (2006). A Practical Guide to Lightcurve Photometry and Analysis. Springer, New York, NY. Having the B, V, R and I magnitudes, it was possible to obtain a four-color spectrum (Fig. 1) using standard procedures described Warner, B.D. (2007). MPO Software, Canopus version 9.3.1.0, in Bus et al (2002). The solar flux was calculated based on the Bdw Publishing, http://www.minorplanetobserver.com/ Sun’s standard magnitudes (Livingston, 2000). From the spectral curve, the lower limit of S’, associated to the “SlopeA” (Luu & Jewitt, 1990), was estimated in 60%/1000Å. Based on this, it can be suggested that 2005 WJ56 belongs to the complex of X-type COLORS OF POTENTIALLY HAZARDOUS ASTEROIDS asteroids which includes E- M- P- and X-types from Tholen 2005 WJ56 AND 2007 TU24 (1984) and Xe-, Xc-, Xk-, and X-class asteroids from the Bus & Binzel (2002) taxonomic system (Clark et al., 2004). Alberto Silva Betzler, Alberto Brum Novaes Projeto “Descobrindo o Céu”, Departamento de Física da Terra e With our asteroid’s V of 12.4 ± 0.2 on 2008 do Meio Ambiente, Instituto de Física, Universidade Federal da January 8, we calculated the reduced magnitude, H(α) = 19.9 ± Bahia (IF-UFBA), Salvador, Estado da Bahia, BRASIL 0.2. Using the H-G magnitude system (Bowell et al., 1989), our [email protected] H(α) value and G = 0.15, the H was found as 18.4 ± 0.2. This is lower that the initial estimate of 17.8 when Tony José Cruz Villa Nova, Dawinson Santos using the same value of G. This suggests a lower Associação de Astrônomos Amadores da Bahia (AAAB), for this object. Combined with the lower limit of S’, a P-type Museu Geológico da Bahia, Salvador, Estado da Bahia, BRASIL taxonomic classification for 2005 WJ56 seems more appropriate.

(Received: 17 February Revised: 24 March) Based on an analysis of 84 asteroids with well determined slope parameters, Harris (1989) concluded that C, G, B, F, P, T and D The near-Earth asteroids 2005 WJ56 and 2007 TU24 types asteroids have a mean G and albedo of 0.09 ± 0.09 and 0.06 were observed by the authors in early 2008 in Salvador, ± 0.03, respectively. Assuming these values, H was recalculated to Bahia, Brazil to determine their color indices. For 2005 be 18.3 ± 0.3. WJ56, we determined B-V = 0.81 ± 0.09, V-R = 0.48 ± 0.09 and R-I = 0.56 ± 0.09. For 2007 TU24, the V-R Bowell et al (1989) gave a relation connecting the diameter D(km) color index was estimated to be 0.41 ± 0.02. with H as: Log(D) = 3.130 – 0.5Log(p) – 0.2H (1) The near-Earth asteroids 2005 WJ56 and 2007 TU24, each with estimated diameters of < 1 km, belong to the Apollo dynamic Where p is the albedo. Using Eq. 1, we estimate the diameter of group, and were observed by Arecibo and Goldstone stations in 2005 WJ56 as 1.2 ± 0.5km. January 2008. At that time, physical observations of both objects were requested with the aim to complement the radar data. 2007 TU24. We observed the asteroid on 2008 January 31, Therefore, the “Discovering the Sky” Project carried out gathering 16 images of 20s exposure in V and R filters. All images observations using a 0.3m f/3.3 LX200 GPS Meade telescope, were corrected with bias, dark, and flat-field frames. Photometric combined with a CCD SBIG ST-7XME detector and B, V, R and I reduction was performed using MPO Canopus, v.9.3.1.0. We Bessell filters. Our goal was to estimate, if possible, the B-V, V-R found a V-R color index of 0.41 ± 0.02. and R-I color indices and the S’ reflectivity gradient of the asteroids. Acknowledgments

To improve the SNR of the asteroids and comparison stars, we Thanks to the Vitae Foundation, MCT (Ministry of Science and summed images using routines in the IRIS V. 5.52 program. Technology) and the Institute of Physics of UFBA (IF-UFBA) for Photometric calibration was done using USNO A2 stars in the supporting the “Discovering the Sky” Project. We are also grateful asteroid’s field. The USNO b and r magnitudes were converted to to B. D Warner for the detailed revision and many suggestions the equivalent B, V and R magnitudes. Only stars with near solar characteristics were used to calculate the asteroids color index. The R-I color index of the selected stars were estimated based on their relation with the B-V index as defined by Caldwell et al. (1993). 2005 WJ56 and 2007 TU24 were observed in the sequence VRVR, for V-R color index, or RRBBRRIIRRVVRR for the others filters combinations (Yoshida et al., 2004) in order to remove the effect of magnitude variation, due asteroids rotations, which affects colors objects.

2005 WJ56. According to the Tholen taxonomic system (Tholen 1984), this object can be classified as an X-type. Hamanowa & Hamanowa (2008), based on observations on 2007 December 14 and 2008 January 13, determined a synodic period of 4.379 ± 0.002 h and lightcurve amplitude of 0.151 ± 0.002 mag. Fig. 1 – Normalized Reflectivity of 2005 WJ56 (V-band) Minor Planet Bulletin 35 (2008) 109 which much improved this work. Clark, B. E., Bus, S. J., Rivkin, A. S., Shepard, M. K., and Shah, S. (2004). “Spectroscopy of X-Type Asteroids”. Astron J. 128, References 3070-3081.

Bowell, E., Hapke, B., Domingue, D., Lumme, K., Peltoniemi, J., Hamanowa, H. and Hamanowa, H., (2008. “Asteroid Lightcurve and Harris, A. W. (1989). “Application of photometric models to Data File”, http://www2.ocn.ne.jp/~hamaten/astlcdata.htm asteroids” In Asteroids II (Binzel et al., eds), University of Arizona Press, Tucson, Arizona, 524-556. Harris, A. H. (1989). “The H-G Asteroid Magnitude System: Mean Slope Parameters”. LPI, 20, 375H Bus, S. J., Vilas, F. and Barucci, M.A. (2002). “Visible- Wavelength Spectroscopy of Asteroids”. In Asteroids III (W. F. Livingston, W. C., (2000). “Sun”. In “Allen’s Astrophysical Bottke et al., eds), University of Arizona Press, Tucson, Arizona, Quantities” (A. N. Cox, ed), pp. 341. 169-182. Luu, J. X. and Jewitt, D. C. (1990). “Charge couple device of Bus. S. J. and Binzel, R. P. (2002). “Phase II of the Small Main- asteroids. 1. Near-Earth and 3:1 resonance asteroids”. Astron. J. Belt Asteroid Spectroscopic SurveyA Feature-Based Taxonomy”. 99, 1985-2011. Icarus 158, 146. Tholen, D. J. (1984). “Asteroid taxonomy from cluster analysis of Caldwell, J. A. R., Cousins, A. W. J., Ahlers, C. C., van Wamelen, photometry”. Ph D. Thesis, University of Arizona, Tucson. P., and Maritz, E. J. (1993). “Statistical Relations between the

Photometric Colors of Common Types of Stars in the UBV(RI)c, Yoshida, F., Dermawan, B., Ito, T., Sawabe, Y., Haji, M., Saito, JHK and uvby System”. SAAO Circulars 15, 1-26. R., Hirai, M., Nakamura, T., Sato, Y., Yanagisawa, T., and Malhotra, R., (2004). “Photometric Observations of a Very Young Family-Member Asteroid (832) Karin”. Publications of the Astronomical Society of Japan 56(6), 1105-1113.

LIGHTCURVE PHOTOMETRY OF NEAS 4450 , performed in about 30 minutes. Since the asteroid is a slow- (170891) 2004 TY16, 2002 RC118, AND 2007 VD12 rotator, it did not change brightness significantly over this time. After calibration and averaging two independent values, we found Albino Carbognani B-V = 0.82 ± 0.02; V-R = 0.48 ± 0.02; and Saint-Barthelemy Observatory R-I = 0.28 ± 0.02, which are typical of an S-type asteroid. When Lignan 39, 11020 Nus (Aosta), Italy using the calibrated V values and setting the slope parameter G to [email protected] 0.23 ± 0.11, the mean value for an S-type asteroid, H = 17.43 ± 0.07. Using this value and assuming a geometric albedo consistent (Received: 6 March) with the derived colors of p = 0.18 ± 0.06 (Wisniewski et al., V 1997), the mean effective diameter of 4450 Pan is 1.0 ± 0.2 km. Lightcurve periods and amplitudes are reported for Amor asteroid (170891) 2004 TY16 (P = 2.795 ± 0.002 (170891) 2004 TY16. Observations of this asteroid were h; A = 0.2 ± 0.02 mag), Amor asteroid 2002 RC118 performed between 2008 January 08-09. The lightcurve is rather (P = 9.98 ± 0.02 h; A = 0.4 ± 0.03 mag), and Apollo symmetric, having two nearly equal maximum and minimums. PHA 2007 VD12 (P = 7.418 ± 0.005 h; A = 0.6 ± 0.05 The period is 2.795 ± 0.002 h with amplitude of 0.2 mag. mag). For 4450 Pan it was not possible to establish a period, but we were able to determine color indices, 2002 RC 118. Observations were made between 2007 October 5 absolute magnitude, and diameter. A search for a and November 13. However, the lightcurve was constructed using only those observations of October 21-23, when the phase angle cometary activity of 2002 RC118 was made with negative results. was about 6.5°. The lightcurve shows a broad maximum followed by a sharper secondary maximum. The data scatter is due to moon light (0.85 phase) and to light pollution from a nearby village. The We report here results for several near-Earth asteroids (NEAs) period is 9.98 ± 0.02 h with amplitude of 0.4 mag, but the solution based on observations performed at Saint Barthelemy Observatory is not unique. An independent analysis performed by Petr Pravec, (0.81-m f/7.9 reflector and FLI 1001E CCD camera) in late 2007 Ondrejov Astronomical Institute, shows that U = 1, i.e., the period and early 2008. Photometric measurements and lightcurves were might be wrong, and so more data will be necessary to confirm or reduced and plotted by using the MPO Canopus software by BDW reject this period. The next perihelion transit of 2002 RC118 will Publishing. Differential photometry (Warner, 2006) with five be in 2012. comparison stars was used in all cases. 2007 VD12. Observations were performed between 2007 4450 Pan. Calibrated V photometry was performed between 2008 November 16-18 in response to a NASA request sent to the Minor January 19 and February 14 in collaboration with the “Photometric Planet Mailing List on November 09. The asteroid lightcurve is Survey for Asynchronous Binary Asteroids” coordinated by symmetric and convex, similar to a lightcurve for a contact binary Pravec (2005). Unfortunately, it was not possible to establish a star. The period is 7.418 ± 0.005 h with amplitude of 0.6 mag. An period. What we can say is that 4450 Pan is a slow rotator with an independent lightcurve analysis by Pravec gives a period of 7.423 amplitude of about 0.8 mag. On February 13-14, observations ± 0.005h with amplitude of 0.579 mag, in good agreement with were also taken in B, V, R and I bands. The observations were our results. This asteroid was observed by NASA Goldstone radar

Minor Planet Bulletin 35 (2008) 110 on November 26 and 27. Initial radar results show a contact with an elongation ratio of about 1.6 (Benner, 2007).

Search for Cometary Activity in 2002 RC118

2002 RC118 is on a 5.07 heliocentric orbit with perihelion at 1.28 AU and an eccentricity of 0.566. With these values, the Tisserand parameter with respect to is T = 2.86. As a general rule, but there are exceptions, the Jupiter Family Comets (JFC) have a Tisserand’s parameter between 2 and 3 while most asteroids have T > 3 (McFadden and Binzel, 2007). This puts 2002 RC118 well inside the boundary between the asteroids and Jupiter comets. Around October 22, the heliocentric distance of 2002 RC118 was 1.39 AU, close enough to the Sun to present any residual cometary activity. A search for a possible weak coma around the object was made using the images of October 21 and 22, taken unfiltered and using the technique described by Masi et al (2007). For each day, ten images with a combined total Figure 1. The H-G plot for 4450 Pan. The period is unknown, so exposure of 600 seconds were stacked with and without the V magnitude is not corrected for the rotation phase. The G compensation for the apparent motion of the object. No value is forced to 0.23 in according to asteroid type. meaningful deviation was found between the FWHM of 2002 RC118 (about 4-5 arcsec) and that of stars of similar magnitude in the same field of view.

Acknowledgments

Research on asteroids at St. Barthelemy Observatory is strongly supported by Director, Enzo Bertolini, and funded with a European Social Fund grant from the Regional Government of the Regione Autonoma della Valle d’Aosta (Italy). We also thank Petr Pravec for his independent analysis of 2002 RC118 and 2007 VD12 lightcurves and for his suggestions concerning the analysis of 4450 Pan. Figure 2. The lightcurve of (170891) 2004 TY16 shows a period of 2.795h with amplitude of 0.2 mag. References

Benner L., private communication (2007).

Masi, G., Behrend, R., Buzzi, L., Cremaschini, C., Foglia, S., Galli, G., and Tombelli, M. (2007). “Observing program ‘T3’: Finding Comets in the Asteroid Population”, Minor Planet Bulletin 34, 123-124.

McFadden, L. and Binzel, R. P. (2007). “Near-Earth Objects” in Encyclopedia of the , Second Edition, pp 283-300. Elsevier.

Pravec, P. (2005). “Photometric Survey for Asynchronous Binary Figure 3. The lightcurve of 2002 RC118 shows a period of 9.98h Asteroids” in Proceedings of the Symposium on Telescope Science with an amplitude of 0.4 mag, but the solution is not unique (The 24th Annual Conference of the Society for Astronomical (U=1). Science), B. D. Warner, D. Mais, D. A. Kenyon, J. Foote (Eds.). More information at the web address: http://www.asu.cas.cz/~asteroid/binastphotsurvey.htm

Warner, D.B. (2006). A Practical Guide to Lightcurve Photometry and Analysis. Springer, USA.

Wisniewski, W. Z., Michalowski, T. M., Harris, A. W., and McMillan, R. S. (1997). “Photometric observations of 125 asteroids”, Icarus 126, 395-449.

Figure 4. The lightcurve of 2007 VD12 shows a period of 7.418h with an amplitude of 0.6 mag.

Minor Planet Bulletin 35 (2008) 111

MINOR OBSERVER & OBSERVING NO. GENERAL REPORT OF POSITION OBSERVATIONS PLANET APERTURE (cm) PERIOD (2006) OBS. BY THE ALPO MINOR PLANETS SECTION 1 Hudgens, 38 Nov 8 2 FOR THE YEAR 2007 Pryal, 20 Nov 11-Dec 9 3

4 Bookamer, 41 Aug 17 2 Frederick Pilcher Faure-Berthet, 20 Jun 23 2 4438 Organ Mesa Loop Garrett, 3.5, 9 May 6-Sep 1 9 Pryal, 20 Jul 9-25 4 Las Cruces, NM 88011 USA 20 Massalia Bookamer, 41 Jan 28 3 (Received: 9 April) 30 Pryal, 20 Sep 9-11 4 40 Harmonia Faure, 20 Nov 12 3 Observations of positions of minor planets by members Bookamer, 41 Feb 22 3 of the Minor Planets Section in calendar year 2007 are 55 Hudgens, 38 Feb 18 2 summarized. 68 Leto Bookamer, 41 Jan 19 2

78 Diana Benishek, 41 Jan 9-15 21C During the year 2007 a total of 1557 positions of 480 different 84 Klio Pryal, 20 Dec 9 2 minor planets were reported by members of the Minor Planets 87 Sylvia Bookamer, 41 Jan 28 3 Section. Of these 188 are CCD images (denoted C). All the rest 93 Minerva Bookamer, 41 Feb 23 3 are approximate visual positions. 96 Aegle Bookamer, 41 Apr 6 3 Watson, 20 Mar 19-Apr 20 3

The summary lists minor planets in numerical order, the observer 100 Hekate Bookamer, 41 Jan 21 2 and telescope aperture (in cm), UT dates of the observations, and 125 Liberatrix Benishek, 41 Apr 13-May 13 30C the total number of observations in that period. The year is 2007 in each case. 152 Atala Hudgens, 38 Jul 16 2 Garrett, 32 Apr 21 2

168 Sibylla Benishek, 41 Oct 16-Nov 24 16C

183 Istria Bookamer, 41 Aug 17 3 Positional observations were contributed by the following Pryal, 20 Sep 11 2 observers: 210 Isabella Garrett, 32 Apr 21 2

Observer, Instrument Location Planets Positions 212 Medea Garrett, 32 Apr 21 2 214 Aschera Garrett, 32 Apr 21 2 Benishek, Vladimir Belgrade, Serbia 10 137C 41 cm Schmidt- 226 Weringia Bookamer, 41 Aug 19 3 Cassegrain+CCD Measured by Aleksandar Grbovich and Vladimir Benishek 251 Sophia Bookamer, 41 Jan 19 3

Bookamer, Richard E. Micco, Florida 127 419 255 Oppavia Bookamer, 41 Dec 30 4 41 cm reflector USA Bookamer, 41 Jun 9 3 Escalera, Eric, Cristian, Vicuna, Chile 1 2 Faure, Gerard and Harvey, 73 Oct 8 3 Christine, 30 cm Dobsonian 282 Clorinde Bookamer, 41 Jan 19 4

Faure, Gerard Col de L'Arzelier, 54 179(51C) 287 Nephthys Hudgens, 38 Mar 20 2 20 cm Celestron France 294 Felicia Bookamer, 41 Aug 18 3 Faure, Gerard, and Rayo, Col de L'Arzelier, 1 3 Jean-Michel, 35 cm France 296 Phaëtusa Hudgens, 38 Dec 31 2 Schmidt-Cassegrain 303 Josephina Harvey, 73 Feb 22 6 Faure, Gerard, and Col de L'Arzelier, 4 13 Berthet, Charly, France 327 Columbia Hudgens, 38 Feb 6 2 20 cm Celestron 342 Endymion Bookamer, 41 Oct 8 3 Garrett, Lawrence Fairfax, Vermont, 11 32 32 cm f/6 reflector USA 385 Ilmatar Watson, 20 Oct 31 2 9 cm Maksutov 35 cm binoculars 391 Ingeborg Bookamer, 41 Aug 4 3 Watson, 20 Sep 19-20 4 Harvey, G. Roger Concord, North 95 328 73 cm Newtonian Carolina, USA 398 Admete Bookamer, 41 Nov 1 3

Hudgens, Ben Stephenville, 238 509 Bookamer, 41 Dec 7 3 38 cm f/5 reflector Texas, USA and environs 445 Edna Bookamer, 41 Sep 6 3

Pryal, Jim Kanaskat, WA USA 6 18 449 Hamburga Pryal, 20 Mar 17 2 20 cm f/10 SCT 493 Griseldis Faure, 20 Aug 24 2 Watson, William W. Tonawanda, NY USA 5 15 20 cm Celestron and vicinity. Oct. 514 Armida Hudgens, 38 Feb 18 2 observations from 525 Adelaide Hudgens, 38 Jan 26 2 Portal, AZ USA 528 Rezia Bookamer, 41 Oct 11-17 5

541 Deborah Bookamer, 41 May 20 3

544 Jetta Bookamer, 41 Mar 23 3

562 Salome Bookamer, 41 Nov 29 3

575 Renate Bookamer, 41 Sep 4 3

583 Klotilde Bookamer, 41 Oct 16 2 Minor Planet Bulletin 35 (2008) 112

MINOR OBSERVER & OBSERVING NO. MINOR OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2006) OBS. PLANET APERTURE (cm) PERIOD (2006) OBS.

591 Irmgard Bookamer, 41 Mar 17 3 1032 Pafuri Bookamer, 41 Apr 21 3

609 Fulvia Bookamer, 41 Mar 24 3 1043 Beate Bookamer, 41 Jun 9 3

615 Roswitha Bookamer, 41 Apr 13 3 1044 Teutonia Bookamer, 41 Jun 5 3

632 Pyrrha Bookamer, 41 May 20 3 1064 Aethusa Bookamer, 41 Jul 9 3

650 Amalasuntha Hudgens, 38 Oct 2 2 1070 Tunica Hudgens, 38 Oct 5 2

651 Antikleia Bookamer, 41 Nov 4 3 1072 Malva Bookamer, 41 Feb 6 3

658 Asteria Faure, 20 Sep 12-13 2 1095 Tulipa Hudgens, 38 Oct 18 2

659 Nestor Hudgens, 38 Aug 12 2 1099 Figneria Bookamer, 41 Oct 8 3 Hudgens, 38 Oct 1 2 661 Cloelia Bookamer, 41 Jan 9 3 1112 Polonia Bookamer, 41 Sep 9 3 676 Melitta Benishek, 41 Jul 18 4C Bookamer, 41 Jul 9 3 1116 Catriona Bookamer, 41 Nov 19 3

698 Ernestina Bookamer, 41 Feb 16 3 1120 Cannonia Hudgens, 38 Aug 12 2

702 Alauda Benishek, 41 Jul 19-Aug 17 34C 1121 Natascha Hudgens, 38 Feb 6 2

724 Hapag Faure, 20 Sep 9 2 Bookamer, 41 Sep 13 3 Hudgens, 38 Sep 14 2 Bookamer, 41 Oct 17 3 734 Benda Bookamer, 41 Oct 10 3 1140 Crimea Bookamer, 41 Nov 6 3 741 Botolphia Bookamer, 41 Jan 21 4 1148 Rarahu Faure, 20 Jun 9-10 2 749 Malzovia Bookamer, 41 Mar 25 3 1150 Achaia Bookamer, 41 Nov 3 3 763 Cupido Hudgens, 38 Oct 12-13 2 Hudgens, 38 Nov 5 2

770 Bali Bookamer, 41 Jan 9 3 1160 Illyria Bookamer, 41 Nov 6 3

777 Gutemberga Bookamer, 41 Feb 23 3 1163 Saga Hudgens, 38 Jul 16 2

782 Montefiore Bookamer, 41 Jan 19 4 1166 Sakuntala Bookamer, 41 Jun 9 3

792 Metcalfia Bookamer, 41 Nov 4 3 1182 Ilona Bookamer, 41 Oct 10 3

793 Arizona Bookamer, 41 Nov 10 3 1186 Turnera Bookamer, 41 Jun 8 3

800 Kressmannia Bookamer, 41 Nov 5 3 1194 Aletta Faure, 20 Sep 9 2

839 Valborg Hudgens, 38 Feb 6 2 1197 Rhodesia Bookamer, 41 Dec 9 3

840 Zenobia Faure, 20 Mar 11 2 1199 Geldonia Faure, 20 Apr 6 2 Hudgens, 38 Jan 26 2 844 Leontina Bookamer, 41 Oct 9 3 1209 Pumma Hudgens, 38 Jul 16 2 856 Backlunda Bookamer, 41 Feb 9 4 1218 Aster Hudgens, 38 Mar 10 2 857 Glasenappia Bookamer, 41 Jun 8 3 1222 Tina Bookamer, 41 Sep 4 3 865 Zubaida Bookamer, 41 Jan 7 3 Hudgens, 38 Jan 8 2 1223 Neckar Faure, 20 Apr 13-14 2

886 Washingtonia Watson, 20 Nov 2-3 2 1228 Scabiosa Hudgens, 38 Feb 6 2

897 Lysistrata Bookamer, 41 Jul 10 3 1233 Kobresia Faure, 20 Apr 9 2 Faure-Berthet, 20 Jun 24 2 1237 Genevieve Bookamer, 41 Nov 27 3 900 Rosalinde Hudgens, 38 May 15 2 1240 Centenaria Bookamer, 41 Aug 5 3 907 Rhoda Bookamer, 41 Nov 6 3 1244 Deira Bookamer, 41 Mar 20 3 913 Otila Bookamer, 41 May 22 3 1263 Varsavia Bookamer, 41 Mar 9 3 914 Palisana Bookamer, 41 Jun 15 2 1274 Delportia Bookamer, 41 Apr 6 4 917 Lyka Bookamer, 41 Oct 8 3 Faure, 20 Apr 13-14 2

927 Ratisbona Bookamer, 41 Feb 22 3 1276 Ucclia Faure, 20 Apr 13-14 2

933 Susi Bookamer, 41 Jan 7 3 1282 Utopia Bookamer, 41 Jan 7 3

934 Thüringia Bookamer, 41 Sep 9 3 1302 Werra Hudgens, 38 Nov 5 2

945 Barcelona Bookamer, 41 Mar 17 3 1308 Halleria Hudgens, 38 Aug 12 2

959 Arne Bookamer, 41 Nov 8 3 1313 Berna Hudgens, 38 Nov 8 2

965 Angelica Bookamer, 41 Jan 28 3 1323 Tugela Bookamer, 41 Jan 6 4

970 Primula Bookamer, 41 Oct 28 3 1325 Inanda Bookamer, 41 Sep 6 3

971 Alsatia Bookamer, 41 Nov 11 3 1332 Marconia Bookamer, 41 Nov 3 3

1000 Piazzia Bookamer, 41 Feb 8 3 1349 Bechuana Bookamer, 41 May 21 3

1002 Olbersia Faure, 20 Sep 13 2 1360 Tarka Bookamer, 41 Mar 20 3 Faure, 20 Apr 13 2 1006 Lagrangea Bookamer, 41 Oct 15 3 Hudgens, 38 Nov 5 2 1368 Numidia Bookamer, 41 Apr 19 3

1015 Christa Bookamer, 41 Aug 18 3 1405 Sibelius Hudgens, 38 Oct 6 2

1018 Arnolda Bookamer, 41 Nov 9 3 1409 Isko Bookamer, 41 Feb 7 3

1029 La Plata Faure, 20 Mar 14 2 1418 Fayeta Bookamer, 41 Sep 12 3 Minor Planet Bulletin 35 (2008) 113

MINOR OBSERVER & OBSERVING NO. MINOR OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2006) OBS. PLANET APERTURE (cm) PERIOD (2006) OBS.

1419 Danzig Bookamer, 41 Feb 7 4 1900 Katyusha Bookamer, 41 Dec 1 3

1421 Esperanto Bookamer, 41 Apr 21 3 1903 Adzhimushkaj Hudgens, 38 Jan 8 2 Faure, 20 Apr 14 2 1907 Rudneva Hudgens, 38 Apr 13 2 1422 Strömgrenia Hudgens, 38 Nov 5 2 1910 Mikhailov Hudgens, 38 May 12 2 1426 Riviera Bookamer, 41 Feb 13 3 1911 Schubart Hudgens, 38 Jan 26 2 1432 Ethiopia Bookamer, 41 Oct 9 3 1925 Franklin-Adams Hudgens, 38 Jul 16 2 1433 Geramtina Hudgens, 38 Oct 12-13 2 1962 Dunant Hudgens, 38 Oct 10-11 2 1451 Granö Hudgens, 38 May 15 2 1978 Patrice Hudgens, 38 Aug 12 2 1457 Ankara Bookamer, 41 Apr 13 3 1985 Hopmann Hudgens, 38 Apr 19-21 3 1475 Yalta Hudgens, 38 Oct 6 2 1987 Kaplan Bookamer, 41 Aug 4 3 1482 Sebastiana Hudgens, 38 Jun 6 2 Faure, 20 Sep 8 2

1487 Boda Rayon-Faure, 35 Mar 11 2 2004 Lexell Hudgens, 38 Apr 13 2

1489 Attila Hudgens, 38 Feb 18 2 2009 Voloshina Hudgens, 38 Dec 31 2

1533 Saimaa Hudgens, 38 Feb 7 2 2010 Chebyshev Hudgens, 38 Oct 5 2

1539 Borrelly Bookamer, 41 Oct 15 3 2022 West Hudgens, 38 Oct 10-11 2

1542 Schalén Bookamer, 41 Nov 16 3 2043 Ortutay Hudgens, 38 Oct 6 2

1544 Vinterhansenia Bookamer, 41 Nov 29 3 2084 Okayama Hudgens, 38 Aug 7 2

1555 Dejan Faure, 20 Sep 8 2 2086 Newell Hudgens, 38 Jan 26 2

1586 Thiele Hudgens, 38 Jan 8 2 2088 Sahlia Hudgens, 38 Oct 6 2

1602 Indiana Faure, 20 Mar 14 2 2089 Cetacea Faure, 20 Mar 11 2 Garrett, 32 Mar 21 2 Hudgens, 38 Mar 8 2 2090 Mizuho Hudgens, 38 Oct 5 2

1605 Milankovich Bookamer, 41 Dec 30 2 2108 Otto Schmidt Hudgens, 38 Feb 18 2

1607 Mavis Bookamer, 41 Sep 8 3 2109 Dhotel Harvey, 73 Jul 23 6

1608 Muñoz Faure, 20 Sep 13 2 2111 Tselina Hudgens, 38 Nov 8 2 Hudgens, 38 Sep 9 2 2113 Ehrdni Harvey, 73 Oct 2 3 1619 Ueta Bookamer, 41 Dec 27 4 Hudgens, 38 Dec 31 2 2123 Vltava Hudgens, 38 Oct 2 2

1624 Rabe Hudgens, 38 Feb 7 2 2126 Gerasimovich Hudgens, 38 Oct 6 2

1626 Sadeya Bookamer, 41 Jan 14 4 2140 Kemorovo Hudgens, 38 Nov 5 2

1663 van den Bos Hudgens, 38 Dec 31 2 2144 Marietta Hudgens, 38 Oct 18 2

1681 Steinmetz Bookamer, 41 Feb 16 3 2167 Erin Bookamer, 41 Feb 18 3 Faure, 20 Feb 20-21 2 1686 De Sitter Hudgens, 38 Jun 6 2 2190 Coubertin Hudgens, 38 Apr 13 2 1689 Floris-Jan Bookamer, 41 Nov 12 3 2193 Jackson Hudgens, 38 Feb 22 2 1691 Oort Hudgens, 38 Oct 1 2 2195 Tengström Hudgens, 38 Aug 21 2 1696 Nurmela Faure, 20 Apr 13 2 Hudgens, 38 Mar 17 2 2250 Stalingrad Hudgens, 38 Sep 9 2

1698 Christophe Hudgens, 38 Feb 22 2 2287 Kalmykia Hudgens, 38 Aug 7 2

1705 Tapio Hudgens, 38 Aug 4 2 2290 Helffrich Hudgens, 38 Feb 22 2

1735 ITA Bookamer, 41 Feb 14 5 2306 Bauschinger Hudgens, 38 Oct 12-13 2

1736 Floirac Bookamer, 41 Oct 10 3 2320 Blarney Hudgens, 38 Oct 6 2

1741 Giclas Hudgens, 38 Nov 8 2 2347 Vinata Hudgens, 38 Nov 8 2

1752 van Herk Hudgens, 38 Aug 4 2 2378 Pannekoek Hudgens, 38 Dec 8 2

1754 Cunningham Hudgens, 38 May 14 2 2413 van de Hulst Hudgens, 38 Sep 9 2

1775 Zimmerwald Faure-Berthet, 20 Jun 23-24 2 2440 Educatio Hudgens, 38 Jul 16 2 Hudgens, 38 Jul 8 2 2445 Blazhko Bookamer, 41 Nov 16 4 1790 Volkov Hudgens, 38 Feb 6 2 Hudgens, 38 Dec 8 2

1806 Derice Bookamer, 41 Jan 14 3 2451 Dollfus Hudgens, 38 Sep 9 2 Faure, 20 Feb 20 2 2478 Tokai Hudgens, 38 Feb 22 2 1813 Imhotep Hudgens, 38 Apr 21 2 2505 Hebei Hudgens, 38 Apr 21 2 1825 Klare Hudgens, 38 Nov 8 2 2512 Tavasta Hudgens, 38 Mar 10 2 1858 Lobachevskij Hudgens, 38 Jul 16 2 2521 Heidi Hudgens, 38 Mar 8 2 1868 Thersites Faure, 20 Sep 9 2 2554 Skiff Hudgens, 38 Jul 8 2 1874 Kacivelia Hudgens, 38 Jul 8 2 2587 Gardner Harvey, 73 May 15 3 1884 Skip Bookamer, 41 Feb 8 3 Faure, 20 Feb 21 2 2612 Kathryn Hudgens, 38 Dec 31 2 Hudgens, 38 Feb 18 2 2623 Zech Faure, 20 Sep 13 2 Minor Planet Bulletin 35 (2008) 114

MINOR OBSERVER & OBSERVING NO. MINOR OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2006) OBS. PLANET APERTURE (cm) PERIOD (2006) OBS.

2630 Hermod Harvey, 73 Oct 8 3 3523 Arina Hudgens, 38 Jul 8 2

2633 Bishop Hudgens, 38 Sep 14 2 3628 Božněmcova Faure, 20 Sep 13 2

2637 Bobrovnikoff Faure, 20 Sep 13 2 3647 Dermott Hudgens, 38 Aug 21 2 Hudgens, 38 Sep 9 2 3656 Hemingway Hudgens, 38 May 14 2 2647 Sova Hudgens, 38 Oct 12-13 2 3670 Mongmanwai Hudgens, 38 Feb 17-18 2 2648 Owa Hudgens, 38 Oct 12-13 2 3687 Dzus Faure, 20 Aug 24 2 2658 Gingerich Hudgens, 38 Mar 17 3 Hudgens, 38 Sep 9 2

2687 Tortali Hudgens, 38 Oct 5 2 3689 Yeates Harvey, 73 Oct 8 3

2730 Barks Hudgens, 38 May 14 2 3767 DiMaggio Hudgens, 38 Jun 6 3

2741 Valdivia Hudgens, 38 Apr 21 2 3784 Chopin Hudgens, 38 Aug 7 2

2751 Campbell Hudgens, 38 Oct 18 2 3824 Brendalee Hudgens, 38 Nov 8 2

2752 Wu Chien-Shiung Hudgens, 38 Oct 5 2 3841 Dicicco Hudgens, 38 Oct 18 2

2760 Kacha Faure, 20 Apr 9 2 3974 Verveer Faure, 20 Mar 14 2

2776 Baikal Hudgens, 38 Jan 26 2 3986 Rozhkovskij Hudgens, 38 Feb 22 2

2783 Chernyshevskij Harvey, 73 Oct 12 3 3991 Basilevsky Hudgens, 38 Aug 6 2

2808 Belgrano Faure, 20 Apr 9 2 4066 Haapavesi Hudgens, 38 Jul 16 2

2847 Parvati Hudgens, 38 Feb 22 2 4070 Rozov Hudgens, 38 Sep 14 2

2870 Haupt Hudgens, 38 Aug 7 2 4091 Lowe Hudgens, 38 May 15 2

2896 Preiss Faure, 20 Aug 24 2 4140 Branham Hudgens, 38 Sep 9 2 Hudgens, 38 Sep 14 2 4159 Freeman Bookamer, 41 Nov 14 3 2951 Perepadin Bookamer, 41 Feb 14 3 4194 Sweitzer Harvey, 73 Apr 8 3 2959 Scholl Harvey, 73 Oct 12 3 4225 1989 BN Hudgens, 38 Aug 21 2 2988 Korhonen Hudgens, 38 Jul 8 2 4293 Masumi Hudgens, 38 Dec 8 2 3011 Chongqing Harvey, 73 Dec 11 6 4343 Tetsuya Faure, 20 Apr 9 2 3028 Zhangguoxi Benishek, 41 Apr 9 5C Hudgens, 38 Mar 10 2 Hudgens, 38 Apr 13 2 4374 Tadamori Faure, 20 Apr 6 2 3062 Wren Hudgens, 38 Aug 7 2 Hudgens, 38 Mar 10 2

3069 Heyrovsky Hudgens, 38 Aug 21 2 4388 Jürgenstock Harvey, 73 Oct 8 3 Hudgens, 38 Oct 12-13 2 3106 Morabito Hudgens, 38 Oct 18 2 4421 Kayor Hudgens, 38 Jan 8 2 3125 Hay Hudgens, 38 Jan 26 2 4440 Tchantchès Hudgens, 38 Jul 16 2 3140 Stellafane Hudgens, 38 Oct 5 2 4552 Ullacharles Hudgens, 38 Feb 17-18 2 3163 Randi Faure, 20 Sep 8-9 3 Hudgens, 38 Sep 9 2 4460 Bihoro Hudgens, 38 Aug 7 2

3166 Klondike Hudgens, 38 Apr 13-19 2 4471 Graculus Harvey, 73 Oct 11 3

3169 Ostro Hudgens, 38 Jul 16 2 4498 Shinkoyama Hudgens, 38 Aug 6 2

3200 Phaethon Bookamer, 41 Dec 9 18 4540 Oriani Hudgens, 38 Jan 26 2

3210 Lupishko Faure, 20 Mar 14 2 4563 Kahnia Hudgens, 38 Aug 12 2

3223 Forsius Bookamer, 41 Jan 21 4 4570 Runcorn Faure, 20 Apr 13 2

3233 Krišbarons Hudgens, 38 Oct 18 2 4583 Lugo Hudgens, 38 Sep 14 2

3252 Johnny Hudgens, 38 Mar 8 2 4603 Bertaud Faure, 20 Aug 18-24 4 Hudgens, 38 Sep 14 2 3275 Oberdorfer Hudgens, 38 Jun 6 2 4605 Nikitin Harvey, 73 Oct 8 3 3310 Patsy Hudgens, 38 Mar 8 2 Hudgens, 38 Oct 18 2

3310 Gantrisch Hudgens, 38 Aug 21 2 4614 Masamura Harvey, 73 Oct 11 3 Hudgens, 38 Oct 5 2 3335 Quanzhou Hudgens, 38 Dec 31 2 4618 Shakhovskoj Hudgens, 38 Oct 18 2 3345 Tarkovskij Hudgens, 38 Apr 21 2 4628 Laplace Faure, 20 Sep 9 2 3364 Zdenka Harvey, 73 May 15 3 4631 Yabu Hudgens, 38 Oct 18 2 3372 Bratijchuk Hudgens, 38 Oct 10-11 2 4650 Mori Harvey, 73 Oct 11 3 3403 Tammy Hudgens, 38 Aug 6 2 4755 Nicky Harvey, 73 Oct 8 3 3406 Omsk Hudgens, 38 May 12 2 4896 Tomoegozen Faure, 20 Aug 17-18 2 3410 Vereshchagin Hudgens, 38 Mar 8 2 Hudgens, 38 Aug 6 2

3415 Danby Hudgens, 38 Oct 13-18 3 4909 Couteau Hudgens, 38 Jul 16 2

3425 Hurukawa Hudgens, 38 Jan 26 2 4913 Wangxuan Harvey, 73 Oct 2 3 Hudgens, 38 Oct 6-7 2 3459 Bodil Harvey, 73 Oct 7 3 4925 1981 XH2 Faure, 20 Sep 8-9 4 3475 Fichte Hudgens, 38 Dec 31 2 4928 Vermeer Harvey, 73 Oct 8 3 Minor Planet Bulletin 35 (2008) 115

MINOR OBSERVER & OBSERVING NO. MINOR OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2006) OBS. PLANET APERTURE (cm) PERIOD (2006) OBS.

4948 1988 VF1 Harvey, 73 Oct 7 3 6831 1991 UM1 Hudgens, 38 Aug 7 2

4954 Eric Bookamer, 41 Sep 6 3 6875 1994 NG1 Harvey, 73 Oct 9 3 Escalera-Cristian-Faure, 30 Oct 10 2 Garrett, 32 Oct 5 3 6905 Miyazaki Bookamer, 41 Nov 9 3 Hudgens, 38 Oct 1 2 Hudgens, 38 Nov 8 2 Pryal, 20 Sep 11 3 Watson, 20 Sep 14-18 4 7055 1989 KB Harvey, 73 May 15 3

4955 Gold Harvey, 73 Oct 21 3 7134 Ikeuchisatoru Harvey, 73 May 21 3

4976 Choukyongchol Harvey, 73 Oct 7 3 7186 Tomioka Hudgens, 38 Mar 17 2

5030 Gyldenkerne Harvey, 73 Apr 8 3 7230 Lutz Harvey, 73 Oct 1 3

5053 Chladni Harvey, 73 Jan 26 3 7281 1988 RX4 Harvey, 73 Oct 12 3

5076 Lebedev-Kumach Harvey, 73 Dec 11 3 7304 Namiki Bookamer, 41 Apr 22 3 Faure, 20 Jun 9 2 5081 Sanguin Hudgens, 38 Jul 8 2 Harvey, 73 Apr 8 3 Hudgens, 38 May 12 2 5105 Westerhout Hudgens, 38 Nov 8 2 7318 Dyokov Hudgens, 38 Aug 4 2 5129 Groom Hudgens, 38 Feb 18 2 7326 Tedbunch Harvey, 73 Oct 11 3 5195 Kaendler Harvey, 73 Oct 11 3 7352 1994 CO Faure, 20 Apr 6 2 5234 Sechenov Faure, 20 Sep 9 2 7409 1990 BS Hudgens, 38 Dec 8 2 5293 Bentengahama Hudgens, 38 Dec 31 2 7517 1989 AD Harvey, 73 Oct 8 3 5331 Erimomisaki Bookamer, 41 Nov 14 4 Hudgens, 38 Nov 5 2 Hudgens, 38 Dec 8 2 7526 1993 AA Harvey, 73 Oct 1 3 5357 1992 EL Hudgens, 38 Jan 26 2 7559 Kristinemeyer Hudgens, 38 Jul 16 2 5358 1992 QH Hudgens, 38 Nov 8 2 7765 1991 AD Harvey, 73 Oct 8 3 5364 1980 RC1 Hudgens, 38 Aug 12 2 7792 1995 WZ3 Hudgens, 38 Mar 10 2 5377 Komori Harvey, 73 Feb 20 3 7802 Takiguchi Harvey, 73 Oct 8 3 5406 Jonjoseph Hudgens, 38 Mar 17 2 7870 1987 UP2 Hudgens, 38 Aug 21 2 5407 1992 AX Harvey, 73 Jan 26 3 Hudgens, 38 Feb 6 2 7930 1987 VD Hudgens, 73 Aug 6 2

5448 Siebold Faure, 20 Feb 20-21 2 8116 Jeanperrin Harvey, 73 Oct 7 3 Hudgens, 38 Feb 7 2 8197 Mizunohiroshi Harvey, 73 Oct 12 3 5484 Inoda Harvey, 73 Apr 10 3 8256 Shenzhou Harvey, 73 Oct 7 3 5508 1988 EB Hudgens, 38 Feb 7 2 8273 Apatheia Harvey, 73 Jan 27 3 5539 Limporyen Hudgens, 38 Nov 8 2 8297 Gérardfaure Faure, 20 Dec 28-29 51C 5556 1988 AL Hudgens, 38 Mar 10 2 8609 Shuvalov Hudgens, 38 Sep 14 2 5601 1991 VR Harvey, 73 Oct 8 3 8722 Schirra Harvey, 73 Oct 7 3 5625 1991 AO2 Hudgens, 38 Sep 9 2 Hudgens, 38 Sep 14 2

5626 1991 FE Harvey, 73 Jan 26 3 9149 1977 TD1 Harvey, 73 Oct 12 3

5657 1936 QE1 Harvey, 73 Oct 7 3 9601 1991 UE3 Harvey, 73 Apr 8 3

5746 1991 CK Hudgens, 38 Sep 14 2 10562 1993 UB1 Hudgens, 38 Oct 5 2

5824 Inagaki Harvey, 73 Jan 26 3 10597 1996 TR10 Hudgens, 38 Sep 14 2

5854 1992 UP Hudgens, 38 May 12 2 10701 1981 PF Hudgens, 38 Aug 21 2

5947 Bonnie Harvey, 73 May 15 3 11780 1942 TB Hudgens, 38 Oct 18 2

5995 Saint-Aignan Harvey, 73 Apr 6 3 13006 Schwaar Harvey, 73 Jan 26 6

6005 1989 BD Faure, 20 Apr 6 2 13026 1989 CX Harvey, 73 Feb 20 3 Hudgens, 38 Mar 10 2 Hudgens, 38 Feb 22 2

6028 1994 ER1 Hudgens, 38 Aug 7 2 13351 Zibeline Hudgens, 38 Apr 21 2

6091 Mitsuru Hudgens, 38 Jul 16 2 13441 2098 P-L Harvey, 73 Oct 10 3 Hudgens, 38 Oct 18 2 6103 1993 HV Harvey, 73 Oct 7 3 13497 Ronstone Hudgens, 38 Feb 22 2 6176 Horrigan Hudgens, 38 Sep 14 2 14815 Rutberg Harvey, 73 Oct 12 3 6265 1985 TW3 Hudgens, 38 Aug 6 2 14892 1991 VE5 Hudgens, 38 Jul 16 2 6420 Riheijyaya Hudgens, 38 Aug 7 2 15161 2000 FQ48 Hudgens, 38 Aug 6 2 6572 Carson Hudgens, 38 Nov 5 2 15491 1999 CW85 Harvey, 73 Oct 7 3 6603 Marycragg Harvey, 73 Apr 8 3 15549 2000 FN Garrett, 32 Jul 14 2 6618 1936 SO Hudgens, 38 Mar 17 2 Hudgens, 38 Jul 16 2

6642 1990 UE3 Harvey, 73 Dec 12 3 15779 Scottroberts Hudgens, 38 Jul 16 2

6649 Yokotatakao Hudgens, 38 Aug 21 2 15979 1978 WQ34 Harvey, 73 Jul 23 3

6724 1991 CX5 Faure, 20 Feb 20 2 16650 1993 TE3 Harvey, 73 Oct 11 3 Harvey, 73 Jan 27 3 16959 1998 QE17 Harvey, 73 Dec 11 3 Minor Planet Bulletin 35 (2008) 116

MINOR OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2006) OBS. ROTATION PERIODS AND H MAGNITUDES OF TWO MEMBERS 17075 Pankonin Harvey, 73 Oct 11 3 17583 1994 WV2 Hudgens, 38 Aug 4 2 Kathryn F. Neugent and Stephen M. Slivan 18877 Stevendodds Harvey, 73 Dec 12 3 Department of Astronomy

19251 Totziens Harvey, 73 Oct 12 3 Whitin Observatory Wellesley College 20936 4835 T-1 Hudgens, 38 Oct 5 2 106 Central Street 21652 Vasishtha Garrett, 32 Jul 14 2 Wellesley, MA 02481 22393 1994 QV Harvey, 73 Oct 7 3

23120 2000 AP50 Harvey, 73 Dec 11 3 (Received: 15 April)

23143 2000 AZ177 Harvey, 73 Oct 21 3 25332 1999 KK6 Harvey, 73 Oct 11 3 Koronis family asteroids (2268) Szmytowna and (1443) 26868 Misterrogers Hudgens, 38 Jan 26-Feb 18 7 Ruppina were observed at Whitin Observatory in Wellesley, Massachusetts during September – December 30105 2000 FO3 Hudgens, 38 Aug 12 2 2007. The lightcurve observations yield the first 31221 1998 BP26 Harvey, 73 Feb 20 4 determinations of their rotation periods, and the data 34704 2001 OS80 Harvey, 73 Jan 26 3 were also calibrated to standard V magnitudes to 34777 2001 RH Faure, 20 Feb 20 4 improve the estimates for the absolute magnitudes H and Hudgens, 38 Jan 8 2 the diameters for both objects. The steps used to 35709 1999 FR28 Harvey, 73 Oct 8 3 calibrate Szmytowna to V are discussed in some detail, 41223 1999 XD16 Garrett, 32 Oct 6 2 to demonstrate the simplified method for standard star Harvey, 73 Oct 1 3 calibration described by Binzel (2005). Hudgens, 38 Oct 6-7 2

41577 2000 SV2 Harvey, 73 Apr 8 3

42517 1993 XU1 Harvey, 73 Oct 12 3 The Koronis family asteroids are remnants of a past collision

46436 2002 LH5 Hudgens, 38 Aug 6-12 4 between two larger bodies, making the family well suited for studying the long-term results of YORP thermal effects (Slivan, 69260 1982 TJ Harvey, 73 Oct 8 3 2002; Slivan et al., 2008, Vokrouhlicky et al. 2003). YORP 71096 1999 XR136 Hudgens, 38 Nov 11 2 studies require information about asteroids’ sizes as well as their 85275 1994 LY Faure, 20 Aug 17 4 rotation rates because the rate of YORP evolution strongly Harvey, 73 Jul 23 6 depends on object size. In most cases the best estimate of an 86324 1999 WA2 Harvey, 73 Jul 23 6 asteroid’s size is based on its absolute magnitude H, which is the 86829 2000 GR146 Harvey, 73 Apr 17 6 mean V brightness at unit Earth-asteroid and Sun-asteroid 90920 1997 QM3 Harvey, 73 Oct 11 3 distances and zero solar phase angle. However, most H magnitudes are only approximately known and uncertainties on 99907 1989 VA Harvey, 73 Oct 30 6 the order of tenths of a magnitude are not uncommon. 134340 Pluto Harvey, 73 May 15 3 138127 2000 EE14 Harvey, 73 Mar 8 6 As part of an effort to determine spin properties of Koronis 153591 2001 SN263 Harvey, 73 Dec 11 3 members smaller than those previously studied, lightcurve 2003 CJ11 Benishek, 41 Apr 9 5C observations of (2268) Szmytowna and (1443) Ruppina were 2003 YV117 Harvey, 73 Feb 20 3 made during their apparitions in 2007. Both objects have Hudgens, 38 Feb 18 2 approximate H magnitudes of 11.4 (Tholen 2006) (D ~ 17 km), 2005 AD13 Faure, 20 Jun 9 4 and neither has a previously published period. This paper Harvey, 73 Jun 11 6 describes the observing program in which standard star 2006 VV2 Bookamer, 41 Mar 28-30 14 Garrett, 32 Mar 24-30 4 observations were combined with on-chip differential photometry Harvey, 73 Apr 1 6 to determine unambiguous rotation periods and more accurate Hudgens, 38 Mar 28-Apr 2 26 estimates of H for Szmytowna and Ruppina, so that they can be 2007 DS84 Benishek, 41 Apr 9 6C included in future studies of Koronis family spin properties. Faure, 20 Apr 14 12 2007 DT103 Benishek, 41 Aug 2-3 4C Observations 2007 FV42 Faure-Berthet, 20 Jun 24 7 Harvey, 73 Jun 21 Szmytowna was imaged on eleven nights over a 44-night span and 2007 LR32 Benishek, 41 Aug 2-Oct 16 14C Ruppina was imaged on four nights over a 31-night span. Table 1 2007 PU11 Harvey, 73 Oct 8 6 presents a summary of the observing circumstances. The images

2007 XH16 Harvey, 73 Dec 24 6 were taken on a 1024-pixel square Photometrics back-illuminated CCD camera with a 2 × 2 binned detector and a 1.8 arc seconds per pixel image scale on Whitin Observatory’s 0.61-m Sawyer telescope located at Wellesley College in Wellesley, Massachusetts. Each lightcurve image integration was 240 seconds in the R filter, except for a select few images taken in the V filter needed€ to determine the H magnitudes. The first (complete coverage) and second (calibrate to V magnitudes) observing principles described by Slivan et al. (2008) were followed closely. The images obtained were processed using the IRAF software Minor Planet Bulletin 35 (2008) 117 package for bias level and dark signal subtraction and twilight field flattening, as well as for measuring instrumental magnitudes using synthetic aperture photometry.

Data Reduction

To determine the rotation periods from on-chip differential photometry, light-time corrections were applied and then features were matched by inspection as described by Slivan et al. (2008). For Szmytowna, the data from September 16 span nearly 8 hours and suggest a period of about 11 hours, and there are enough lightcurves to make a definite determination of 11.26 hours. The longest span of Ruppina lightcurve covered nearly a full rotation, leading to a straightforward period determination of 5.88 hours. We next fit Fourier series models to the composite lightcurve shapes of both asteroids to refine the period results, iteratively adjusting the nightly brightness effects until the overall RMS residual was minimized. Figure 1: Extinction Diagram for (2268) Szmytowna.

In order to obtain the additional data needed to determine H magnitudes, one additional lightcurve of each object was recorded using the V filter. Unlike the R lightcurves, which were not calibrated to a standard system, the V lightcurves were observed with a standard star from Landolt (1992) using the simplified method for standard star calibration described by Binzel (2005). Prior to the observations, the “Airmass plot calculator” application at the Web site http://www.koronisfamily.com was used to determine the times at which the asteroid and its comparison star were at the same airmass as a standard star having “asteroid-like” color (precepts 1 and 2) on the night of the V observations, UT 2007 Sep 18. The graph output showed that the field’s airmass would match that of Landolt standard SA092-288 just after UT 4 h, suggesting that the rapidly alternating images of the standard and the comparison star (precept 3) should begin near UT 3:50. Based on past observations of this standard star at Whitin, an exposure time of 50 s would be used for imaging—experience has shown that it is important to determine the exposure time before Figure 2: Composite rotation lightcurve of (2268) Szmytowna. the sequence begins. To reduce the time needed to complete the One rotation period is shown with the earliest and latest 10% of calibration sequence, exposures of the comparison star field the period span repeated. The error bars shown represent the recorded during the sequence were 120 s, half the length of the estimated one-sigma uncertainty with respect to the local regular lightcurve exposures, to take advantage of the fact that the comparison star used. comparison stars are considerably brighter than the asteroid and thus can deliver sufficient signal for good photometry in a shorter time. Normally the strategy used at Whitin Observatory is to record calibration sequence images in alternating pairs and to obtain three such pairs of the standard star, but on this particular night too short an exposure time was mistakenly used for one pair, so only two pairs are available for reduction.

Figure 1 is a graph of the instrumental V magnitude of the comparison star vs. airmass for each image on which it was recorded, showing that the sky conditions were photometric during most of the observations, although there is a clear systematic dimming as the field rose above 1.5 airmasses, just after the calibration sequence was finished. In particular, the conditions seem to have been stable when the standard star was imaged, which occurred during the gaps that appear on either side of the solid dots. Recording a sequence of bracketing images of the comparison star, and using them to check how consistently the brightness of the star changes with airmass, is an essential step in Figure 3: Same as Figure 2 except displays the lightcurve of establishing confidence in the resulting calibration. For this (1443) Ruppina. particular reduction, the extinction seems to have been stable starting well before the calibration sequence, as shown by the best- fit line that is plotted with the data. This extinction solution has a photometry at Whitin, and it is clear from the graph that this slope of 0.13 mag. per airmass, which is better than usual for V solution can be used to reliably determine the apparent brightness of the comparison star at the times that the standard star was Minor Planet Bulletin 35 (2008) 118 imaged. The brightness difference between the comparison star Bowell, E., Hapke, B., Domingue, D., Lumme, K., Peltoniemi, J., and the standard star is combined with the catalog magnitude of and Harris, A.W. (1989). “Application of photometric models to the standard star to give the calibrated V magnitude of the asteroids.” In Asteroids II (Binzel, R. P., Gehrels, T., Matthews, comparison star, which then is used with the on-chip differential M. S., eds.) pp 524-556. Univ. of Arizona Press, Tucson. magnitudes of the asteroid to yield the calibrated V magnitudes of the lightcurve observations. Davis, D.R. and Neese, C., eds. (2002). Asteroid . EAR- A-5-DDR-ALBEDOS-V1.1. NASA Planetary Data System. After calibrating the lightcurve, we then followed the steps described by Slivan et al. (2008) to reduce each calibrated Lagerkvist, C.-I., Magnusson, P. (1990). “Analysis of asteroid lightcurve to unit distances, fold each with the model lightcurves lightcurves. II – Phase curves in a generalized HG-system.” using the derived period, and shift the models in brightness to best Astron. Astrophys. Suppl. Ser. 86, 119-165. match the V lightcurves. The resulting lightcurves of Szmytowna and Ruppina appear as Figures 2 and 3. Landolt, A.U. (1992). “UBVRI photometric standard stars in the magnitude range 11.5 < V < 16.0 around the celestial equator”, Finally, we used the Lumme-Bowell solar phase model and Astronomical Journal 104, 340-371. assumed G = 0.23 ± 0.11 (Lagerkvist and Magunsson, 1990) to extrapolate the mean reduced V magnitude back to zero phase Slivan, S. M. (2002). “Spin vector alignment of Koronis family angle (Bowell et al., 1989) yielding H. The results are summarized asteroids.” Nature 419, 49-51. in Table 2. Slivan et al. (2008). “Rotation Rates in the Koronis Family, Results and Discussion Complete to H ~ 11.2.” Icarus 195, 226-276

We are pleased to report that this observing program reached its Tholen, D. J. (2006). “Asteroid absolute magnitudes and slopes.” goals of determining the periods and improving the H magnitudes EAR-A-5-DDR-ASTERMAG-V10.0, NASA Planetary Data for both Szmytowna and Ruppina. Our calculated H magnitude for System. Szmytowna of 11.87 is around 0.5 magnitude fainter than the previous estimate, making it one of the faintest Koronis members Vokrouhlicky, D., Nesvorny, D., and Bottke, W.F. (2003). “The with a known period. Of the list of 41 Koronis members with vector alignments of asteroid spins by thermal torques.” Nature published periods compiled by Slivan et al. (2008), only four have 425, 147-151 H magnitudes fainter than Szmytowna. In contrast, Ruppina’s H magnitude of 11.19 is brighter than the previous estimate by 0.2 magnitude. This makes it comparable to the sample asteroids Duration studied by Slivan et al. (2008), and demonstrates the importance UT Date α (º) Filter (h) Observer(s) of obtaining accurate H magnitudes for more objects. Without (2268) Szmytowna accurate estimates, it becomes impossible to correctly identify 09 08 7.2 R 4.6 Neugent 09 14 4.8 R 4.0 Youngblood, populations for statistical studies of YORP effects. Slivan €09 16 4.1 R 7.8 Neugent, By assuming an albedo (pH) of 0.20 ± 0.07 and using the diameter Slivan 09 17 3.7 R 4.5 Neugent, equation log pH = 6.259 − 2logd − 0.4Hv (Bowell et al., 1989), improved estimates of the diameter were calculated for both Zangari 09 18 3.4 R,V 3.3 Levandowski, Ruppina (18 km) and Szmytowna (13 km). The albedo was Zangari estimated by calculating the mean and standard deviation of € 09 19 3.0 R 1.3 Levandowski, previously known albedos of 26 Koronis family members (Davis Wasser and Neese, 2002). 09 21 2.4 R 0.4 Youngblood 09 22 2.2 R 2.3 Neugent Both rotation periods are well within the wide range of values, 3 – 10 05 5.0 R 6.0 Neugent, 60 hours, known for the periods of other Koronis members Slivan (Slivan et al., 2008, Fig. 71). Szmytowna’s V-R color is also 10 15 8.9 R 6.0 Neugent, Zangari consistent with the color of other Koronis members (Slivan et al., 10 21 11.1 R 5.0 Neugent 2008, Table 4). (1443) Ruppina 11 07 9.6 R 4.8 Neugent Acknowledgements 11 08 9.3 R 3.1 Neugent 12 01 0.9 V 5.3 Neugent We would like to thank the corps of loyal observers who assisted 12 07 2.5 R 2.5 Youngblood with data collection: Kirsten Levandowski, Molly Wasser, Allison Table 1: Observing circumstances. Given for each lightcurve are Youngblood and Amanda Zangari. We would also like to thank the UT date (2007), solar phase angle, filter, lightcurve duration the Wellesley College Early Sophomore Research Program for and observers. funding this research. Object Period (h) Q H mag. V-R D(km) References (2268) 11.260±0.003 3 11.87±0.07 0.43±0.06 13±2 (1443) 5.880±0.002 3 11.19±0.03 ---- 18±3 Binzel, R.P. (2005). “A simplified method for standard star Table 2: Results determined from the observations. Given for calibration.” The Minor Planet Bulletin. 32, 93-95. each asteroid are the asteroid number, period, period reliability code Q: 3, secure – no ambiguity of period, H magnitude, V-R color and diameter.

Minor Planet Bulletin 35 (2008) 119

ASTEROID LIGHTCURVE ANALYSIS AT THE VIA some of the detailed features of the curve – presumably associated CAPOTE OBSERVATORY: FIRST QUARTER 2008 with the opposition crossing – made analyzing this data set particularly challenging. Behrend (2008) reports a period of James W. Brinsfield 9.6442 h with only partial coverage of the curve. His reported Via Capote Observatory period agrees reasonably well with the measurement obtained in 5180 Via Capote, Thousand Oaks CA 91320 this study, although the amplitude obtained here is considerably [email protected] lower than was reported by Behrend. Binzel (1983) reports a period greater than 18 h. (Received: 6 April) 1464 Armisticia. There are no previously published reports of a lightcurve for this object. Lightcurves for 13 asteroids were measured at the Via Capote Observatory from November 2007 through 1479 Inkeri. The very low apparent amplitude of the lightcurve March 2008: 1136 Mercedes (24.64 h), 1284 Latvia resulted in an ambiguous rotational period solution with a slightly (9.55 h), 1464 Armisticia (7.5 h), 1479 Inkeri (12.55 h), preferred period of 12.55 h, which is presented here. There are no 1810 Epimetheus (10.88 h), 1855 Korolev (4.65 h), published reports of a lightcurve for this object. 2284 San Juan (9.18 h), 2345 Fucik (17.12 h), 2911 Miahelena (4.2 h), 2912 Lapalma (5.71 h), 3401 1810 Epimetheus. The 10.88 h period measured in this study does Vanphilos (4.22 h), 4375 Kiyomori (6.46 h), and (7267) not agree with the period of 28.61 h reported by Pravec (2008) that 1943 DF (3.11 h). was based on a partially-covered lightcurve and assigned an uncertainty of U = 2. Both the Pravec data and the data reported Observations of the asteroids presented here were made using a here suggest a very low amplitude . Takahashi Cassigran at prime focus resulting in a focal length of 1855 Korolev. Pravec (2008) reports nearly identical results as 136 inches and a focal ratio of f/11.5. The CCD imager was an reported here. Alta U6 featuring a 1024x1024 array of 24 µ-meter pixels. The CCD was operating at a temperature of –30°C with 1x1 binning, 2284 San Juan. There are no published reports of a lightcurve for yielding an image scale of 1.43” per pixel. All images were dark this object. and flat field corrected; no other image enhancements were made. Images were measured using MPO Canopus (Bdw Publishing) 2345 Fucik. There are no published reports of a lightcurve for this using unfiltered differential photometry. The data were light-time object. corrected. Period analysis was also done with Canopus. 2911 Miahelena. This asteroid was observed on one evening with The results are summarized in the table below and include average full rotational period coverage. Binning was used here in phase angle information across the observational period. particular to smooth noisy data. There are no published reports of Individual lightcurve plots along with additional comments as a lightcurve for this object. required are also presented. In many cases, the original data were binned in sets of 2 to 5 points per bin with a maximum difference 2912 Lapalma. There are no published reports of a lightcurve for of 5 minutes between any two given points in order to make the this object. lightcurve more readable and help reduce noise. 3401 Vanphilos. Pravec (2008) reports nearly identical results as 1136 Mercedes. Only partial coverage of the curve was achieved. reported here. Behrend (2008) reports a provisionary period of 15.65 h, also with partial coverage. 4375 Kiyomori. Pravec (2008) reports nearly identical results as reported here. 1284 Latvia. The observations covered both sides of the 2008 January 10 opposition. The low apparent amplitude of the curve, (7267) 1943 DF. Pravec (2008) reports a period of 3.04 h and along with session to session changes in the relative intensity of Dates Data Per Amp # Name Phase L B PE AE (mm/dd) 2008 Points PAB PAB (h) (m) 1136 Mercedes 12/02/2007-01/13 596 17.15 55.5 -7.1 24.64 0.01 0.15 0.03 1284 Latvia 11/13/2007-02/26 1485 23,2,14 106.5 4.2 9.552 0.001 0.10 0.02 1464 Armisticia 01/14-01/15 263 9.3 89.6 1.8 7.50 0.01 0.54 0.05 1479 Inkeri 03/06-03/15 554 18.1 134.6 7.6 12.55 0.03 0.03? 0.02? 1810 Epimetheus 02/06-02/16 742 16.1 114.9 -4.2 10.88 0.02 0.03? 0.02? 1855 Korolev 03/17-03/18 260 2.5 174.2 -1.2 4.65 0.01 0.76 0.04 2284 San Juan 03/25-03/28 394 4.1 180.5 4.3 9.18 0.01 0.58 0.02 2345 Fucik 01/18-02/11 744 10.8 102 3.2 17.12 0.01 0.39 0.02 2911 Miahelena 03/24 193 4.7 189.5 7.9 4.2 0.1 0.56 0.02 2912 Lapalma 03/23-03/28 257 7.3 177.8 9.8 5.71 0.01 0.83 0.02 3401 Vanphilos 02/28-03/13 346 11.1 149.8 -7.2 4.225 0.001 0.54 0.02 4375 Kiyomori 03/17-03/18 257 3.9 174.8 5.3 6.46 0.02 0.15 0.03 (7267) 1943 DF 03/19-3/22 506 8.3 171 3.3 3.11 0.01 0.14 0.04

Minor Planet Bulletin 35 (2008) 120 amplitude of 0.20, larger than was found at this apparition.

Acknowledgments

The author wishes to thank Brian D. Warner for his ever helpful assistance with the analysis of the 1284 Latvia data set.

References

Behrend, R. (2008). Observatoire de Geneve web site, http://obswww.unige.ch/~behrend/page_cou.html

Binzel, R.P., Mulholland, J.D. (1983). Icarus 56, 519-533.

Pravec 2008w Pravec, P., Wolf, M., Sarounova, L. (2008). http://www.asu.cas.cz/~ppravec/neo.htm

Minor Planet Bulletin 35 (2008) 121

Minor Planet Bulletin 35 (2008) 122

THE ROTATIONAL PERIOD OF 1379 LOMOSONOWA algorithm developed by Harris (1989). 1370 measurements were taken of the target in support of this analysis. To make the James W. Brinsfield lightcurve plot more readable, the data have been binned in sets of Via Capote Observatory 5 with a maximum time difference of 7 minutes to make a more 5180 Via Capote, Thousand Oaks, CA 91320 readable lightcurve of only 327 data points. [email protected] Binzel (1987) reported a period of 24.71 h, but with an uncertainty David Higgins rating of 2. The table gives the average Phase Angle information Hunters Hill Observatory across the observational period. Ngunnawal, ACT, AUSTRALIA References (Received: 14 April) Binzel, R.P. (1987). Icarus 72, 135-208. Lightcurves for 1379 Lomosonowa were acquired at Via Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Capote observatory in California USA, and the Hunters Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, Hill Observatory in Australia. A synodic period of H., and Zeigler, K.W. (1989). “Photoelectric Observations of 24.488 ± 0.001 h with an amplitude of 0.63 ± 0.02 mag Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. were obtained in this collaborative effort.

Asteroid 1379 Lomosonowa lightcurves observations obtained at the Via Capote Observatory were made using either a Takahashi Cassegrain at prime focus or a 0.35 m Meade LX200 GPS SCT. The CCD imager was an Alta U6 featuring a 1024x1024 array of 24-micron pixels and operating at –30°C. All observations were made at 1x1 binning yielding an image scale of approximately 1.44” per pixel. All images were dark and flat field corrected; no other image enhancements were made. Sessions 170-172, 180, 192, and 199 were acquired at the Via Capote Observatory. Session 199 was taken with the LX200 GPS SCT. Observations obtained at Hunters Hill Observatory were made using a 0.35m Meade LX200GPS SCT. The CCD imager was an SBIG ST-8E featuring a 1530 x 1020 array of 9-micron pixels operating at a temperature of –15°C. All observations were taken at a sub-frame of 1148 x 765 pixels at 1x1 binning yielding an image scale of 1.31" per pixel. All images were dark and flat field corrected and no other image enhancements were made. Sessions 182, 183, 193, 203, and 204 were taken at the Hunters Hill Observatory.

Images were measured using MPO Canopus (Bdw Publishing). All observations were made using unfiltered differential Date Range Data photometry and all data were light time corrected. Period analysis (mm/dd) 2008 Points Phase LPAB BPAB was also done with Canopus, incorporating the Fourier analysis 02/29 – 04/07 1370 14.8 147 -5.5

Minor Planet Bulletin 35 (2008) 123

ASTERIOD LIGHTCURVE ANALYSIS AT HUNTERS HILL Apogee AP7p. Via Capote Observatory is equipped as described OBSERVATORY AND COLLABORATING STATIONS: in Brinsfield (2007). Vintage Lane observatory is equipped with a NOVEMBER 2007 – MARCH 2008 41cm Cassegrain telescope and an SBIG ST-9XE CCD. Palmer Divide observatory is equipped with a 0.5m RC telescope and an David Higgins SBIG STL-1001E CCD. Hunters Hill Observatory (E14) 7 Mawalan Street Targets were chosen either from the CALL list provided by Ngunnawal ACT 2913, Australia Warner (2008), from Binary Asteroid Photometric Survey list [email protected] provided by Dr. Petr Pravec (2005), or as specific observing requests. Results are summarised in the table below with the Petr Pravec, Peter Kusnirak and Kamil Hornoch individual plots presented at the end. Additional comments, where Ondrejov Observatory appropriate, are provided. Binary candidates and collaborative Fricova 298 targets for which Hunters Hill was not the principal observer are 25165 Ondrejov not included. Binary candidates will be reported separately by Czech Republic Pravec. The strategy is to work objects carefully for potential deviations that would indicate the presence of a . James W. Brinsfield Considerable effort was made to identify and eliminate sources of Via Capote Observatory (G69) observational errors that might corrupt the observations and lead 5180 Via Capote, Thousand Oaks CA 91320 to false attenuation events. It was particularly important to identify and eliminate data points affected by faint background stars, bad Bill Allen pixels, and cosmic ray hits. Vintage Lane Observatory 83 Vintage Lane, RD3 Blenheim, NZ . The Lightcurve Parameter list (Harris and Warner 2007) indicates that the target had been previously observed by Brian D. Warner Lagerkvist (7.0 h) and Warner (6.003 h). The data obtained in this Palmer Divide Observatory apparition did not agree with either period. Warner was contacted 17995 Bakers Farm Rd. and provided an additional 2 nights data during the current Colorado Springs, CO 80908 apparition. The combined data ruled out a 6 h period and provided (Received: 16 March Revised: 15 April) sufficient data overlap to confirm the 8.0074 h period. 443 Photographica. This target was observed by Hunters Hill (6 Lightcurves for the following asteroids were obtained at sessions) and Jim Brinsfield (1 Session). The lightcurve for this Hunters Hill Observatory and collaborating stations and target was extremely symmetrical bringing into question whether a then analysed to determine the synodic period and monomodal or bimodal curve provided the best indication of the amplitude: 332 Siri, 443 Photographica, 547 Praxedis, targets period. The monomodal RMS fit was superior to the 1650 Heckmann, 1620 Geographos, 1664 Felix, 1685 bimodal curve and the symmetry values calculated by Canopus for Toro, 1797 Schamasse, 2378 Pannekoek, 2606 Odessa, both peaks were virtually identical. However, given the target’s 2709 Sagan. 5783 Kumagaya, 6411 Tamaga, (7281) 0.24 mag amplitude, Harris advised that, although the monomodal 1988 RX4, (8828) 1988 RC7, and (24114) 1999 VV23. fit could not be ruled out, the bimodal fit was more likely. The Lightcurve Parameter list indicates that the target had been previously observed by Harris (16.0 h) and Behrend (18.190 h). Hunters Hill Observatory is equipped as described in Higgins Neither period was found to fit the data taken during this (2005). All observations for this paper were made using a clear apparition. filter with guided exposures. Ondrejov Observatory is equipped as described in Pravec et al (1998) though they have fitted a new 547 Praxedis. The Lightcurve Parameter list indicates that the

Name Date Range Session Period P.E. Amp Amp Hrs Mag Error 332 Siri 14Mar-31Mar08 6 8.0074 0.0004 0.15 0.01 443 Photographica 07Mar-16Mar08 7 19.795 0.003 0.24 0.01 547 Praxedis 16Mar-28Mar08 5 9.106 0.002 0.09 0.01 1620 Geographos 17Feb–24Feb08 5 5.2220 0.0003 1.1 0.02 1650 Heckmann 09Mar-15Mar08 4 14.893 0.005 0.16 0.02 1664 Felix 17Mar-31Mar08 5 3.3454 0.0002 0.38 0.01 1685 Toro 17Feb–01Mar08 8 10.1862 0.0006 0.6 0.02 1797 Schaumasse 12Mar-13Mar08 2 6.105 0.002 0.75 0.01 2378 Pannekoek 01Jan-05Jan08 3 5.943 0.003 0.08 0.01 2606 Odessa 15Jan–12Feb08 3 8.2426 0.0003 0.8 0.02 2709 Sagan 01Mar–03Mar08 2 5.258 0.002 0.36 0.02 5783 Kumagaya 01Mar–03Mar08 3 3.659 0.002 0.18 0.03 6411 Tamaga 26Dec-30Dec07 4 8.383 0.007 0.3 0.02 7281 1988 RX4 16Nov-19Nov07 4 16.7 0.2 0.13 0.02 8828 1988 RC7 11Nov-19Nov07 4 12.929 0.003 0.33 0.03 24114 1999 VV23 31Dec-06Jan08 5 8.244 0.002 0.26 0.03 Minor Planet Bulletin 35 (2008) 124 target had been previously observed by Cooney (9.105 h). The data obtained during the current apparition matches this period within the error margins quoted.

1620 Geographos. This target has been observed on numerous occasions in the past with the Lightcurve parameter list showing a period of 5.223 h. Geographos is a shape modelling and YORP target.

1650 Heckman. The Lightcurve Parameter list indicates that the target had been previously observed by Behrend (12.05 h). This period was found not to fit the data taken during this apparition.

1685 Toro. This target had been observed by Hunters Hill during its 2007 opposition where a period of 10.1995 + 0.0004 h was derived (Higgins 2007). The Lightcurve parameter list indicates a period of 10.196 h. Toro is a shape modelling and YORP target.

2378 Pannekoek. The Lightcurve Parameter list indicates that the target had been previously observed by Oey (11.8806 h). This period is double the period identified by Higgins.

5783 Kumagaya. This target was observed by Kamil Hornoch of Ondrejov Observatory on 1 night and by Hunters Hill Observatory on 2 nights.

(24114) 1999 VV23. The target was observed by Higgins (2 sessions), Bill Allen (2 sessions), and Kamil Hornoch (1 session).

Acknowledgements

The SBIG ST-8E used by Hunters Hill was funded by The Planetary Society under the 2005 Gene Shoemaker NEO Grants program. The work at Ondrejov was supported by the Grant Agency of the Czech Republic, Grant 205/05/0604.

References

Brinsfield, J. W. (2007), “The Rotation Periods of 872 Holda, 3028 Zhangguoxi, 3497 Innanen, 5484 Inoda, 5854 Terni and 7304 Namiki”, Minor Planet Bulletin 34, 108-110.

Harris, A.W., and Warner B.D. (2008), “Minor Planet Lightcurve Parameters”, Minor Planet Center website, http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html.

Higgins, D. (2005). “Asteroid Lightcurve Analysis at Hunters Hill Observatory and Collaborating Stations - Autumn/Winter 2005”, Minor Planet Bulletin 33, 8-11.

Higgins, D. (2007), Minor Planet Lightcurves, http://www.david- higgins.com/Astronomy/asteroid/lightcurves.htm

Pravec, P., Wolf, M., and Sarounova, L. (1998). “Lightcurves of 26 near-Earth asteroids.” Icarus 136, 124—153

Pravec, P. (2005). “Photometric Survey of Asynchronous Binary Asteroids”, http://www.asu.cas.cz/~asteroid/binastphotsurvey.htm.

Warner, B.D. (2008). CALL Website http://www.minorplanetobserver.com/astlc/default.htm.

Minor Planet Bulletin 35 (2008) 125

Minor Planet Bulletin 35 (2008) 126

ASTEROIDS OBSERVED FROM GMARS AND SANTANA OBSERVATORIES: LATE 2007 AND EARLY 2008

Robert D. Stephens Goat Mountain Astronomical Research Station (GMARS) 11355 Mount Johnson Court, Rancho Cucamonga, CA 91737 [email protected]

(Received: 27 March)

Lightcurve period and amplitude results from Santana and GMARS Observatories are reported for 2008 January to March: 1126 Otero (3.648 ± 0.002 hours and 0.70 mag.), 1488 Aura (99.7 ± 0.1 hours and 0.32 mag.), 3236 Strand (66.133 ± 0.007 hours and 0.44 mag.), 3401 Vanphilos (4.226 ± 0.001 hours and 0.50 mag.), (6823) 1988 ED1 (2.541 ± 0.001 hours and 0.10 mag.), (22275) 1982 BU (40.424 ± 0.004 hours and 0.52 mag.).

The author operates telescopes at two observatories. Santana Observatory (MPC Code 646) is located in Rancho Cucamonga, California and GMARS (Goat Mountain Astronomical Research Station, MPC G79) located at the Riverside Astronomical Society’s observing site. Details are at Stephens (2006).

All of the targets, except 1488 Aura and (6823) 1998 ED1, were selected from the Photometric Survey of Asynchronous Binary Asteroids (2006). 1488 Aura and (6823) 1998 ED1 were chosen from the list of asteroid photometry opportunities published by Brian Warner on the Collaborative Asteroid Lightcurve Link (CALL) website (Warner 2008). The author measured the images using MPO Canopus, which employs differential aperture photometry to produce the raw data. Period analysis was done using Canopus, which incorporates the Fourier analysis algorithm (FALC) developed by Harris (1989).

1126 Otero. Images were acquired using the 0.30m SCT at Santana Observatory with a SBIG STL-1001 CCD Camera. The lightcurve presented is from the author’s data set and plotted at 3.648 hours. When combined with other observers the period was calculated to be 3.64808 ± 0.00008 hours.

1488 Aura. The March 9, 2008 data was acquired using a 0.35m SCT at GMARS with a SBIG STL-1001 CCD Camera. All of the other data was acquired using the 0.30m SCT at Santana Observatory. The data were linked to an internal standard using a method developed by Warner (2007) and described by Stephens (2008) included in the latest release of Canopus.

3236 Strand. All data were obtained using the 0.35m SCT at GMARS with a SBIG STL-1001 CCD and were internally linked.

3401 Vanphilos. Images were acquired using the 0.30m SCT at

Per Asteroid Dates Phase L B PE Amp AE PAB PAB (h) 1126 Otero 2008 02/06–07 8.4,7.8 147.6,147.7 5.9,5.8 3.648 0.002 0.70 0.02 1488 Aura 2008 02/17–03/11 5.8,13.7 136.8,137.8 7.8,6.5 99.7 0.1 0.32 0.05 3236 Strand 2007 12/30–2008 02/10 11.0,1.1, 14.6 114.4,117.5 7.8,6.5 66.133 0.007 0.44 0.03 3401 Vanphilos 2008 02/12–13 4.9, 4.4 149.2 -2.7,-2.9 4.226 0.001 0.50 0.03 (6823) 1988 ED1 2007 12/14–2008 01/12 5.5,1.1, 9.4 91.5,92.2 0.8,4.0 2.541 0.001 0.10 0.06 (22275) 1982 BU 2007 12/30–2008 02/10 10.3,5.6,18.4 112.6,114.4 4.4,14.7 40.424 0.004 0.52 0.03

Minor Planet Bulletin 35 (2008) 127

Santana Observatory with a SBIG STL-1001 CCD Camera. The lightcurve presented is from the author’s data set and plotted at 4.226 hours. When combined with other observers the period was calculated to be 4.2261 ± 0.0003 hours.

(6823) 1998 ED1. Images were acquired using the 0.30m SCT at Santana Observatory with a SBIG STL-1001 CCD Camera. The period spectrum shows a possible period of 2.41 hours. However, the 2.541 hour period dominates the period spectrum and groups of nights separated by a month favors the 2.541 hour period.

(22275) 1982 BU. All of the data were obtained using a 0.35m SCT at GMARS with a SBIG ST9 CCD Camera and were internally linked.

Acknowledgements

Thanks are given to Dr. Alan Harris of the Space Science Institute, Boulder, CO, and Dr. Petr Pravec of the Astronomical Institute, Czech Republic, for their ongoing support of amateur asteroid research. Also, thanks to Brian Warner for his continuing work and enhancements to the software program MPO Canopus which makes it possible for amateur astronomers to analyze and collaborate on asteroid rotational period projects and for maintaining the CALL Web site which helps coordinate collaborative projects among amateur astronomers.

References

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., and Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.

Pravec, P. (2006). “Photometric Survey of Asynchronous Binary Asteroids.” http://www.asu.cas.cz/~asteroid/binastphotsurvey.htm.

Stephens, R.D. (2006). “Asteroid Lightcurve Photometry from Santana and GMARS Observatories – September to December 2006.” Minor Planet Bulletin 34, 31-32.

Stephens, R.D. (2008). “Long Period Asteroids Observed from GMARS and Santana Observatories.” Minor Planet Bulletin 35, 31-32.

Warner, B.D. (2007). “Initial Results from a Dedicated H-G Project.” Minor Planet Bulletin 34 113-119.

Warner, B.D. (2008) CALL web site. http://www.MinorPlanetObserver.com/astlc/default.htm.

Minor Planet Bulletin 35 (2008) 128

PART OF SIMPLE LIGHTCURVES FROM MODRA (OCTOBER 2007- FEBRUARY 2008)

Adrián Galád Modra Observatory, Department of Astronomy, Physics of the Earth, and Meteorology FMFI UK, 842 48 Bratislava, SLOVAKIA and Astronomical Institute AS CR, 251 65 Ondřejov, CZECH REPUBLIC [email protected]

(Received: 2008 April 2)

Lightcurve analysis of 1825 Klare, 4771 Hayashi, (6033) 1984 SQ4, 6905 Miyazaki, (10826) 1993 SK16, (19309) 1996 UK1, (27921) 1996 VY26, (34484) 2000 SR124, (40326) 1999 MA, and 2007 TF8 is reported. Of these, only 1825 Klare had previously reported rotation properties.

An invaluable updated version of lightcurve database with a list of references by Harris et al. (2008) comprises more than 3400 asteroids with rotational properties of various quality levels. In comparison to their previous version from just one year ago, the new one has about 600 new targets and many revised results for previously observed targets. This indicates recent rapid progress in asteroid photometry. The database seems to be huge enough even for detailed statistical purposes, only one must bear in mind several strong observational biases. They include natural preference for the brightest asteroids (closest and largest), asteroids with large lightcurve amplitude, rapid rotators, asteroids with simple lightcurves, and sometimes asteroids in special orbits (there are dedicated programs for studying specific groups and families). Moreover, despite the progress, the list of all asteroids in the database traditionally represents just less than 1% of the known population of asteroids.

It can be roughly estimated that each year about 1500 asteroids can reach magnitude 15.0, while about 4000 can reach magnitude 16.0. Most of those asteroids are from the main belt. Thus, it takes about 1.15 (for the Hilda group) up to 1.60 (for the Hungaria group) years from one opposition to another (the synodic ). Thanks to eccentricity, many usually fainter objects occasionally become so bright as well, meaning that over a span of a few years, more than 3000 different asteroids can reach magnitude 15.0 and more than 10000 can reach magnitude 16.0. From this point of view, the number of items in the current lightcurve database comprises just about all asteroids of magnitude 15.0, which is an encouraging milestone in photometry.

Number Name Dates Phases LPAB BPAB Period Amp yyyy mm/dd deg deg deg [h] [mag] 1825 Klare 2007 11/17-30 2.5,7.6 53 4 4.7431 ± 0.0001 0.71 4771 Hayashi 2007 11/01-12/15 6.1,12.6 53 5 9.801 ± 0.002 0.38 6033 1984 SQ4 2007 10/18-12/18 1.0,13.2 41 -2 35.53 ± 0.01 0.31 6905 Miyazaki 2008 01/14-26 22.2,23.4 59 6 2.7418 ± 0.0002 0.14 10826 1993 SK16 2007 11/01-30 2.6,8.1 53 5 13.835 ± 0.001 0.61 19309 1996 UK1 2007 11/01-02 1.6,2.2 41 -1 4.16 - 5.91 ? 0.06 27921 1996 VY26 2007 11/01-12/01 0.6,10.5 42 -1 18.703 ± 0.002 0.64 34484 2000 SR124 2007 10/06-20 6.8,12.4 359 -4 6.174 ± 0.001 0.8 40326 1999 MA 2007 11/28-12/15 7.5,15.1 54 4 6.481 ± 0.001 1.1 2007 TF7 2008 02/07-10 10.8,12.1 113 -3 16.53 ± 0.03 1.0 Table I. Asteroids with observation dates, minimum and maximum solar phase angles, phase angle bisector values, derived synodic rotation periods with uncertainties, and lightcurve amplitudes. Minor Planet Bulletin 35 (2008) 129

In fact, there are still many bright asteroids still missing, probably (27921) 1996 VY26. Even though it was observed near its because their lightcurves are not so simple and, of course, many favourable opposition, this asteroid was still very faint, > 17.5 other bright objects have still poorly known rotational periods. mag. Were it not for a hint of a large amplitude based on the first Hopefully, a collective effort by several observers can cope with two sessions, other sessions would not have been added. Other all these in the foreseeable future. possible periods would have a more complex lightcurve than presented here. According to proper (Knežević The asteroids presented here were observed with a 0.60-m f/5.5 and Milani, 2003) it may belong to the . If true, it is telescope and AP8p CCD-camera at Modra. More details about probably the smallest photometrically studied asteroid from that the system and data processing can be found in Galád (2008). family. Objects here were in the same field of view as other asteroids for a short time. In an attempt to derive unknown rotation properties of (34484) 2000 SR124. Its recent opposition was not favourable. the most promising cases successfully with a limited observing The rotation properties for objects fainter than magnitude 18.0 like time, further sessions dedicated to these asteroids alone could not this one could be established with the available equipment only be continuous. The results of lightcurve analysis are summarized because of the large amplitude and linked data. Proper orbital in Table I and appropriate lightcurves are in figures, in which elements (Knežević and Milani, 2003) indicate that asteroid could correction for light-travel time was applied. Most of the asteroids be a member of the . were fainter than magnitude 16.0 during observations with previously unknown rotational properties. (40326) 1999 MA. The composite lightcurve of this faint object (fainter than magnitude 17.0) was not covered fully, so its large 1825 Klare. This was the only asteroid with a previously known amplitude was not precisely determined. Low-order Fourier period. The derived rotational properties are in perfect agreement analysis does not fit the data ideally, but the rotation period could with results obtained by other authors (Pray, 2004; Clark, 2006; be derived quite precisely. Behrend, 2008; Hamanowa and Hamanowa, 2008). It was observed on four nights, three of them were consecutive. 2007 TF8. This was the faintest of all asteroids presented here, being fainter than magnitude 18.0. It was near its favorable 4771 Hayashi. The interrupted sessions mean that the uncertainty opposition, which helped lead to its recent discovery. The data for the derived rotation period and amplitude of the lightcurve was errors exceeded 0.1 mag. The rotation period was again larger than usual. However, sessions from consecutive nights were determined thanks to the large amplitude and linked observations. linked to the same magnitude level, which served as the useful In fact, a period of 12.43 h formally fits the data as well. limitation for the uncertainty. Acknowledgements (6033) 1984 SQ4. This asteroid was faint and observed in short sessions. Fortunately, there are many sessions and some data were I’m grateful to Petr Pravec, Ondřejov Observatory, Czech linked to the same magnitude level. The rotation period presented Republic, for his ALC software used in data analysis, and to Brian here seems to be the most probable value. Several others, such as D. Warner, Palmer Divide Observatory, Colorado, for his kind 20.381 h and 37.4 h, cannot be ruled out nor can others if the help with language corrections and technical advices. The work lightcurve is assumed to be more complex. was supported by the Slovak Grant Agency for Science VEGA, Grant 1/3074/06 and the Grant Agency of the Czech Republic, 6905 Miyazaki. This is one example of a bright leftover with Grant 205/05/0604. previously unknown lightcurve. However, observations were conducted two months after its recent favourable opposition. The References first short session was followed by mutually linked sessions to the same magnitude level on four consecutive nights. From the Behrend, R. (2008). dynamical point of view it belongs to the http://obswww.unige.ch/~behrend/page_cou.html (Zappalà et al., 1995). Clark, M. (2006). “Lightcurve results for 383 Janina, 899 Jokaste, (10826) 1993 SK16. The large amplitude was the leading factor 1825 Klare, 2525 O’Steen, 5064 Tanchozuru, and (17939) 1999 for the successful period determination. This object was fainter HH8.” Minor Planet Bulletin 33, 53-56. than usual in recent apparition – above magnitude 16.0. Galád, A. (2008). “Several Byproduct Targets of Photometric (19309) 1996 UK1. This asteroid was a faint target observed on Observations at Modra.” Minor Planet Bulletin 35, 17-21. just two consecutive nights. Despite the fact that the object was near favourable opposition and data were linked to the same Hamanowa, H., and Hamanowa, H. (2008). magnitude level, many possible solutions for the rotation period http://www2.ocn.ne.jp/~hamaten/astlcdata.htm are possible. The most probable values that best fit the data can be seen from the minima of a plot of the sum of square residuals Harris, A.W., Warner, B.D., and Pravec, P. (2008). versus period. The minimum is for one of several monomodal LCLIST_PUB_2008.zip, http://www.minorplanetobserver.com/ lightcurves. Several periods that formally fit as well are not so astlc/LightcurveParameters.htm. probable. Several bimodal lightcurves were found, particularly between 4.16 h and 5.91 h. From visual inspection, the best of Knežević, Z. and Milani, A. (2003). “Proper element catalogs and these bimodal composite lightcurves seems to be the one that is asteroid families.” Astronomy and Astrophysics 403, 1165-1173. plotted. However, with such a small amplitude of the lightcurve, (or at http://hamilton.dm.unipi.it/astdys/propsynth/numb.syn) this estimate is only tentative. Pray, D. P. (2004). “Lightcurve analysis of asteroids 110, 196, 776, 804, and 1825.”Minor Planet Bulletin 31, 34-36.

Minor Planet Bulletin 35 (2008) 130

Zappalà V., Bendjoya, P., Cellino, A., Farinella, P., and Froeschlé, C. (1995). “Asteroid families: Search of a 12,487-asteroid sample using two different clustering techniques.” Icarus 116, 291-314.

Minor Planet Bulletin 35 (2008) 131

Minor Planet Bulletin 35 (2008) 132

LIGHTCURVE ANALYSIS OF ASTEROIDS FROM (Warner 2007). All images were taken with clear filter. Period KINGSGROVE AND LEURA OBSERVATORIES IN THE analysis was done using MPO Canopus V9.4.0.1 and all data was 2ND HALF OF 2007 light-time corrected. All light curves were tabulated and presented without comment unless deemed necessary. Julian Oey Leura Observatory 677 Aaltje. Previous data show a period of > 10 h with U = 1 as Kingsgrove Observatory shown by Lagerkvist (1978). The current data do not considerably 94 Rawson Parade improve the solution, mainly due to background stars. Leura, NSW, 2780 AUSTRALIA [email protected] 1240 Centenaria. Di Martino (1984) and Behrend et al. (2008) made observations of this target and reported synodic periods of (Received: 15 April Revised: 20 April) 14 h and 11.2 h, respectively. Our data show a unique period of 11.2907 + 0.0007 h. The lightcurve is not typical, being tri-modal and having a deep minimum at phase 0.52. A suggestion that this Fourteen asteroids were observed from Kingsgrove and lightcurve may be associated with that of a synchronous binary Leura observatories during the second half of 2007. The asteroid was soon cleared. Unfortunately due to insufficient follow synodic periods derived were: 226 Weringia, 11.240 + up observations, the true nature was not convincingly revealed and 0.002 h; 294 Felicia, 10.4227 + 0.0007 h; 677 Aaltje, future observations may be required for its correct interpretations. 11.056 + 0.003 h; 1099 Figneria, 13.577 + 0.001 h; 1240 Centenaria, 11.2907 + 0.0007 h; 1251 Hedera, (11780) 1942 TB. No previous period determination was done on 19.9000 + 0.0002 h; 1432 Ethiopia, 9.8458 + 0.0003 h; this target. During the nights of November 10, 12, 13, and 14, the 1607 Mavis, 6.1508 + 0.0005 h; 2378 Pannekoek, asteroid was moving slowly across the sky and so the same 11.8806 + 0.0008 h; 4755 Nicky, 5.057 + 0.002 h; comparison stars were used. Despite the scarcity of data, the (11780) 1940 TB, 295 + 10 h; (30220) 2000 GP126, period is estimated to be 295 + 10 h. 3.3670 + 0.0003 h: (41223) 1999 XD16, 32.52 + 0.02 h; (143243) 2002 YA26, 7.688 + 0.003 h; (41223) 1999 XD16. This target was a Mars-crossing asteroid with no previously reported period. It was selected due to its position and brightness favourable to Southern Hemisphere Kingsgrove and Leura observatories were previously described in observers. The data were analyzed in Canopus using the new Oey et al. (2007a) and Oey (2007b) respectively. Leura Comp Star Selector module to determine the absolute magnitude Observatory used a 0.35m Schmidt-Cassegrain telescope and ST- variations in the asteroid by selecting comparison stars similar in 9XE SBIG CCD camera. The combination operates at maximum color to the target. The period derived was 32.52 + 0.02 h. binning of 1x1, providing a scale of 1.07 arcsec/pixel. At Kingsgrove Observatory, a 0.25m Schmidt- Cassegrain telescope Acknowledgement and ST-402ME SBIG CCD camera are used, providing a scale of 1.41 arcsec/pixel. Leura observatory is dedicated to asteroid I would like to thank Petr Pravec of the Ondrejov observatory for photometry work with targets selected from the Photometric his tireless leadership in the pro-am collaboration of the Survey for Asynchronous Binary Asteroid managed by Pravec Photometric Survey for Asynchronous Binary Asteroid. My (2007). Due to some surrounding conditions and the smaller thanks also to Peter Kusnirak of the Ondrejov observatory for his aperture at Kingsgrove, only relatively bright targets were assistant in deciphering 1240 Centenaria and to Brian Warner for selected. All targets reported in this paper, with the exception of providing continual improvements and support for the MPO (30220) 2000 GP126 and (143243) 2002 YA26, were from Canopus software. asteroid photometry opportunity listed in the CALL website

# Name Obs Date Range Period Amp Phase LPAB BPAB (mm/dd) 2007 (h) (mag) 226 Weringia 1 08/07–09/29 11.240 + 0.002 0.08 + 0.02 5.6,23.9 305,312 3,-3 294 Felicia 1 07/13–08/11 10.4227 + 0.0007 0.20 + 0.02 11.7,0.2,1.7 313,315 1,0 677 Aaltje 1 06/20–07/04 11.056 + 0.003 0.10 + 0.03 5.7,10.6 255 -2.5 1099 Figneria 1,2 09/25–09/28 13.577 + 0.001 0.16 + 0.02 13.7,3.5,4.3 357,359 -8,-6 1240 Centenaria 1 07/13–08/11 11.2907 + 0.0007 0.20 + 0.02 11.2,1.3,2.4 313 -4,-2 1251 Hedera 1 07/13–10/01 19.9000 + 0.0002 0.60 + 0.02 10.8,0.6,21.9 311,318 2,-1 1432 Ethiopia 1 07/18–09/13 9.8458 + 0.0003 0.40 + 0.02 30.5,10.8 347,0 -5,-10 1607 Mavis 1 09/15–09/23 6.1508 + 0.0005 0.50 + 0.03 8.5,9.6 354 -11 2378 Pannekoek 1 11/13–01/15 11.8806 + 0.0008 0.14 + 0.02 13.0,8.6,17.6 73,76 -17 4755 Nicky 1 11/13–11/19 5.057 + 0.002 0.40 + 0.03 13.9,17.1 33 -4 (11780) 1940 TB 1 10/01–11/13 295 + 10 0.80 + 0.05 8.2,7.4,21.0 13,20 -9,-12 (30220) 2000 GP126 2 07/04–07/11 3.3670 + 0.0003 0.50 + 0.05 11.4,8.1 295 8.4 (41223) 1999 XD16 1 10/01–11/10 32.52 + 0.02 0.45 + 0.05 6.8,6.1,21.6 9,18 -8,0 (143243) 2002 YA26 2 07/13–07/15 7.688 + 0.003 0.28 + 0.02 10.5,9.7 304,304 -6 Observatory code: 1: Kingsgrove Observatory; 2, Leura Observatory

Minor Planet Bulletin 35 (2008) 133 References

Behrend, R. (2008). Observatoire de Geneve web site. http://obswww.unige.ch/~behrend/page1cou.html

Di Martino, M. (1984). “Physical study of asteroids - Lightcurves and rotational periods of six asteroids”. Icarus 60, 541-546.

Lagerkvist, C. –I. (1978). “Photographic Photometry of 110 main- belt asteroids.” Astronomy and Astrophysics Supplement Series 31, 361-381

Oey, J., Világi, J., Gajdoš, Š., Kornoš, L., Galád, A. (2007a). “Light Curves Analysis of 8 Asteroids from Leura and other Collaborating Observatories”. Minor Planet Bulletin 34, 81-83.

Oey, J. (2007b). “Lightcurve Analysis of 1495 Helsinki,” Minor Planet Bulletin 34, 2.

Pravec, P. (2007). “Photometric Survey of Asynchronous Binary Asteroids.” http://www.asu.cas.cz/~asteroid/binastphotsurvey.htm

Warner, B.D. (2007). “Potential Lightcurve Targets 2007 July – September”. http://www.minorplanetobserver.com/astlc/targets_3q_2007.htm

Minor Planet Bulletin 35 (2008) 134

Minor Planet Bulletin 35 (2008) 135

PERIOD DETERMINATIONS FOR 26 , 34 CIRCE, 74 GALATEA, 143 ADRIA, 272 ANTONIA, 419 AURELIA, AND 557 VIOLETTA

Frederick Pilcher 4438 Organ Mesa Loop Las Cruces, NM 88011 USA [email protected]

(Received: 10 April)

Synodic lightcurve periods and amplitudes were determined for seven aseroids: 26 Proserpina, 13.110 ± 0.001 h, 0.14 ± 0.02 mag; 34 Circe, 12.176 ± 0.002 h, 0.17 ± 0.02 mag; 74 Galatea, 17.270 ± 0.001 h, 0.08 ± 0.01 mag with four maxima and minima per cycle; 143 Adria, 22.005 ± 0.001 h, 0.08 ± 0.02 mag with an irregular lightcurve; 272 Antonia, 3.8548 ± 0.0001 h, 0.43 ± 0.04 mag; 419 Aurelia, 16.784 ± 0.001 h, 0.07 ± 0.01 mag; 557 Violetta 5.0887 ± 0.0001 h, 0.25 ± 0.03 mag.

Seven asteroids were observed in late 2007 and early 2008 at the Organ Mesa Observatory where the equipment consists of a Meade 35 cm LX200 GPS S-C, and SBIG STL-1001E CCD camera. Exposures were 60s, unguided, and used a clear filter, except for 26 Proserpina and 419 Aurelia whose brightness required 20- and 40-second exposures, respectively. Differential photometry and lightcurve analysis were done by MPO Canopus. Because of their large number, the data points for all lightcurve were binned in sets of three with no more than 5 minutes time separation.

26 Proserpina. Harris et al. (2007) list four different periods of 6.668, 10.60, 13.06, and 13.13 h, each with reliability 2. It was the intent of this investigation to determine a unique and correct period as well as search for and eliminate all alias periods. Observations on eight nights from 2007 Dec. 24–2008 Feb. 22 achieved all of these goals. Full-phase coverage with overlap found an asymmetric bimodal lightcurve with a period of 13.110 ± 0.001 h and maximum amplitude 0.14 ± 0.02 magnitudes. No alias periods in the range from 6 to 30 hours could be found except for a quadrimodal lightcurve with full phase coverage of twice this period for which the two halves looked essentially identical, and for which the RMS residual was slightly larger. One could artificially construct a shape model greatly variant over a 90 degree rotation but almost invariant over a 180 degree rotation. The probability of this symmetry for a real asteroid is so small that it may be safely rejected. Hence I claim the 13.110 hour period is the correct one.

After this study was completed and the paper was being prepared for publication, a new lightcurve for 26 Proserpina was published by Fauerbach et al. (2008a). They found a period of 13.106 ± 0.001 h, in excellent agreement with this study, based on observations six nights from 2007 Nov. 9–Dec. 7. At the larger phase angles encountered in this pre-opposition data set, the amplitude was 0.17 ± 0.02 magnitudes. Fauerbach (2008b) kindly prepared a lightcurve that includes both his (2008a) data and those of the present study, a total of fourteen sessions 2007 Nov. 7–2008 Feb. 22, with a period of 13.110 ± 0.001 hours. Lightcurves of the Organ Mesa observations 2007 Dec. 24–2008 Feb. 22 and of the combined sessions 2007 Nov.–2008 Feb. 22 are included separately in this paper. Minor Planet Bulletin 35 (2008) 136

34 Circe. Harris et al. (2007) list a period of 12.15 h, reliability 3 and amplitude of 0.07 ± 0.01 magnitudes. Recognizing that the (secure). The purpose of this investigation was to provide synodic period varies somewhat with changing and additional data for spin/shape modeling. Observations on three at different aspect angles, I consider all of these determinations nights, 2007 Dec. 7, 25, and 30, provided full-phase coverage for consistent. an asymmetric bimodal lightcurve of period 12.176 ± 0.002 h, amplitude 0.17 ± 0.02 magnitudes. The synodic period of any 557 Violetta. Harris et al. (2007) list no previous period asteroid with fixed spin vector varies by small amounts with mean determinations. Observations on six nights from 2007 Dec. motion, aspect and obliquity angles, and the shadowing by surface 20–2008 Jan. 20 show a period of 5.0887 ± 0.0001 h and irregularities. Hence this period is not only consistent with Harris amplitude 0.25 ± 0.03 magnitudes. et al. (2007) but its small deviation provides information useful to the stated goal of spin/shape modeling. Acknowledgments

74 Galatea. Harris et al. (2007) list a period of 8.629 h, reliability The author thanks Michael Fauerbach for constructing a combined 2, based on Behrend (2008) who assumed 2 maxima and minima lightcurve of his and this author’s data for 26 Proserpina and per cycle. Observations on eleven nights from 2008 Feb. 1–Mar. encouraging its publication in this paper. 23 show a period of 17.270 ± 0.002 h with a maximum amplitude 0.08 ± 0.01 magnitudes. Unlike the case for 26 Proserpina References previously described, the lightcurve phased to 17.270 hours with four maxima and minima per cycle fit the data better than that Behrend, R., http://obswww.unige.ch/~behrend/page_cou.html. phased to a bimodal 8.635 h period in three criteria: by visual inspection alternate maxima and minima looked distinctly Fauerbach, M., Marks, S. A., and Lucas, M. P. (2008a). Minor different; the fit to the longer period had much smaller scatter of Planet Bull. 35, 44-46. individual data points; and the RMS residual to the Fourier series Fauerbach, M., (2008b): Personal communication. analysis was considerably smaller for the longer period. Particularly for small amplitude lightcurves, this example shows Harris, A. W., Warner, B. D., and Pravec, P., “Asteroid Lightcurve the importance of always examining lightcurves with periods of Data Files, Revised 20 April 2007.” twice (and 1.5 times) the bimodal value. http://www.MinorPlanetObserver.com/astlc/default.htm. 143 Adria. Harris et al. (2007) list a period of 21.89 h, reliability Harris, A. W. andYoung, J. W. (1989). Icarus 81, 314-364. 2. This is based on the most comprehensive data set preceding this investigation by Warner (2007), who published a lightcurve with Riccioli, D., Blanco, C., Di Martino, M., and De Sanctis, G. three irregularly spaced and unequal maxima and minima with a (1995). Astron. Astrophys. Suppl. Ser. 111, 297-303. maximum amplitude of 0.10 magnitudes based on observations on five nights 2006 Dec. 4–10. Behrend (2008) phased observations Riccioli, D., Blanco, C., and Cigna, M. (2001). Planetary and beginning 2005 Aug. 8 with an amplitude 0.04 magnitudes to the Space Science 49, 657-671. same period. In the current investigation observations on nine nights 2008 Jan. 11-Mar. 2 show an irregular lightcurve of one Warner, B. D. (2007). Minor Planet Bull. 34, 32-37. very shallow and two narrow deep minima with a period of 22.005 ± 0.001 h and maximum amplitude of 0.08 ± 0.02 magnitudes. The shape of the lightcurve is very different from December 2006, and, considering that the synodic period varies with aspect, the period is consistent. For objects with irregular lightcurves and small amplitudes, it is important to search diligently for alias periods. All local minima on the MPO Canopus period spectrum diagram between 10 and 44 hours were examined and none except 22.005 h produced a good fit on all nights. A lightcurve phased to 44 hours showed nearly complete phase coverage with the two halves nearly identical to each other and to the 22.005 h lightcurve. This is rejected for the same reason as previously explained for 26 Proserpina.

272 Antonia. Harris et al. (2007) list no previous period determinations. Observations on five nights from 2007 Dec. 26–2008 Jan. 22 show a period of 3.8548 ± 0.0001 h, amplitude 0.43 ± 0.04 magnitudes.

419 Aurelia. Harris and Young (1989) obtained a period of 16.709 h and amplitude 0.05 ± 0.02 magnitudes. Riccioli et al. (1995) reported a period of 16.63 ± 0.01 h and amplitude 0.18 ± 0.02 magnitudes. Riccioli et. al (2001), on the basis of full phase coverage of an asymmetric bimodal lightcurve, found a period of 16.63 ± 0.006 h and maximum amplitude 0.27 magnitudes. The current study is the densest data set published to date. Observations on nine nights 2008 Feb.17–Mar. 25 show a somewhat irregular lightcurve with a period of 16.784 ± 0.001 h

Minor Planet Bulletin 35 (2008) 137

Minor Planet Bulletin 35 (2008) 138

search routines, including the FALC routine (Harris et al 1989). Following a visual inspection of the data, periods between 5 and 10 hours were searched and several routines gave identical or near identical results with a prominent peak in the power spectrum.

The composite lightcurve for 6411 Tamaga appears to be a “normal” bi-modal curve with a synodic period of 8.352 ± 0.007 h. The peak-to-peak amplitude variation is some 0.34 mag, implying an axial ratio (assuming an equatorial observing aspect) a/b of 1.37. The lightcurve has full phase coverage and is considered a secure result. We note that this result is slightly different to that quoted by Higgins (2008), who obtained a value of 8.383 h for the synodic rotation period in December 2007 from a lightcurve (at solar phase angle 27 degrees) with two distinctly different maxima.

References

Bembrick, C.S., Richards, T., Bolt, G., Pereghy, B., Higgins, D. and Allen, W.H. (2004). “172 Baucis – A Slow Rotator”. Minor Planet Bulletin 31, 51-52.

MINOR PLANET 6411 TAMAGA GUIDE version 8 (2002). http://www.projectpluto.com

Colin Bembrick Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Mt Tarana Observatory Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, PO Box 1537, Bathurst, NSW, Australia H., and Zeigler, K. (1989). Icarus 77, 171-186. [email protected] Harris, A.W. and Warner, B.D. (2007). “Minor Planet Lightcurve Tom Richards Parameters”. Updated May 06 2007. Woodridge Observatory http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html Eltham, Victoria, Australia Higgins, D.J. (2008). http://www.davidhiggins.com/Astronomy/ Bill Allen asteroids/images/6411lc.gif Vintage Lane Observatory Blenheim, New Zealand Hurst, Guy M. (2008). “6411 Tamaga Re-visited”. The Astronomer 44, 254. Greg Bolt Craigie, WA, Australia Vanmunster, T., 2006. Peranso ver 2.0. http://www.peranso.com

(Received: 14 April) PAB PAB Phase %Phase UT Date Long Lat Angle Coverage 2008 Jan 09 113.3 -33.6 24.4 69 The synodic rotation period of the Mars crossing minor 2008 Jan 10 113.4 -33.4 24.2 132 planet 6411 Tamaga (1993 TA) was found to be 8.352 ± 2008 Jan 11 113.5 -33.2 23.9 135 0.007 h. The peak to peak variation of the bi-modal light 2008 Jan 13 113.7 -32.6 23.5 86 curve is 0.34 mag implying an axial ratio a/b of 1.37. 2008 Jan 15 113.9 -32.1 23.0 72 2008 Jan 19 114.3 -30.9 22.3 43 Table I. Aspect data for Tamaga in 2008. Minor planet 6411 Tamaga (1993 TA) was discovered by Rob McNaught at Siding Spring on 8 October, 1993. It is a Mars- crossing asteroid with a quoted diameter of 16.6 km (Guide v8, 2002). It was named in MPC 29671 (April, 1997) after the British magazine, The Astronomer, which now features the name and number of this asteroid on its cover. No rotation period data were found in the latest available lists (Harris and Warner, 2007).

Observations in 2008 were conducted from four sites: one in New Zealand and three in Australia. The locations of these sites are listed in Bembrick et al (2004). All observations were made using unfiltered differential photometry and exposures were adjusted so that 1% precision was achieved in most cases. All data were light- time corrected. The aspect data (Table I) also shows the percentage of the lightcurve observed each night. PAB is the Phase Angle Bisector. Period analyses were carried out using the Peranso software (Vanmunster, 2006), utilising a variety of period Figure 1. Composite phased lightcurve for 6411 Tamaga.

Minor Planet Bulletin 35 (2008) 139

LIGHTCURVE PHOTOMETRY OPPORTUNITIES: required but high precision work, 0.01-0.03mag, usually is. The JULY-SEPTEMBER 2008 geocentric ephemerides are for planning purposes only. The date range may not always coincide with the dates of planned radar Brian D. Warner observations. Use on-line services such as the Minor Planet Center Palmer Divide Observatory/Space Science Institute or JPL’s Horizons to generate high-accuracy topocentric 17995 Bakers Farm Rd. ephemerides. Colorado Springs, CO 80908 USA [email protected] MPC: http://cfa-www.harvard.edu/iau/mpc.html JPL: http://ssd.jpl.nasa.gov/?horizons Alan W. Harris Space Science Institute Those obtaining lightcurves in support of radar observations La Canada, CA 91011-3364 USA should contact Dr. Benner directly at the email given above.

Petr Pravec There are several web sites of particular interest for coordinating Astronomical Institute radar and optical observations. Future targets (up to 2015) can be CZ-25165 Ondrejov, CZECH REPUBLIC found at http://echo.jpl.nasa.gov/~lance/future.radar.nea.periods .html. Past radar targets can be found at http://echo. Josef Durech jpl.nasa.gov/~lance/radar.nea.periods.html This page can be used Astronomical Institute to plan optical observations for those past targets with no or Charles University in Prague poorly-known rotation periods. Obtaining a rotation period will 18000 Prague, CZECH REPUBLIC significantly improve the value of the radar data and help with 3D shape estimation. Slightly different information for Arecibo is Lance A.M. Benner given at http://www.naic.edu/~pradar/sched.shtml. For Goldstone, Jet Propulsion Laboratory additional information is available at http://echo.jpl.nasa.gov/ Pasadena, CA 91109-8099 USA asteroids/goldstone_asteroid_schedule.html. We present here four lists of “targets of opportunity” for the Once you have data and have analyzed them, it’s important that period 2008 July-September. The first list is those asteroids reaching a favorable apparition during this period, are <15m at you publish your results, if not part of a pro-am collaboration, then brightest, and have either no or poorly constrained lightcurve in the Minor Planet Bulletin. It’s also important to make the data available at least on a personal website or upon request. Note that parameters. By “favorable” we mean the asteroid is unusually brighter than at other times and, in many cases, may not be so for the lightcurve amplitude in the tables could be more, or less, than many years. The goal for these asteroids is to find a well- what’s given. Use the listing as a guide. As always, double-check your work. determined rotation rate. Don’t hesitate to solicit help from other observers at widely spread longitudes should the initial findings Changing of the Guard show that a single station may not be able to finish the job. Starting with this issue, Josef Durech takes over for Mikko The Low Phase Angle list includes asteroids that reach very low Kaasalainen as the author in charge of asteroid modeling phase angles. Getting accurate, calibrated measurements (usually opportunities. Josef has collaborated on several papers with Mikko V band) at or very near the day of opposition can provide involved asteroid modeling and is the lead of the Database of important information for those studying the “opposition effect”, Asteroid Models from Inversion Techniques (DAMIT) project at which is when objects near opposition brighten more than simple the Astronomical Institute of the Charles University, Czech geometry would predict. Republic. The DAMIT site can be found at

The third list is of those asteroids needing only a small number of http://astro.troja.mff.cuni.cz/projects/asteroids3D/web.php lightcurves to allow shape and spin axis modeling. Some asteroids have been on the list for some time, so work on them is strongly where results and the original data for a large number of asteroid encouraged so that models can be completed. For modeling work, models can be browsed and downloaded. absolute photometry is strongly recommended, meaning that data not differential magnitudes but absolute values put onto a standard Mikko is turning his attention to the “big picture”, which includes system such as Johnson V. If this is not possible or practical, working with the large surveys, e.g., Pan-STARRS, that will accurate relative photometry is also permissible. This is where all provide the sparse data needed to model thousands of asteroids in differential values are against a calibrated zero point that is not the coming years. The authors thank Mikko for all his work on necessarily on a standard system. this article as well as his efforts for encouraging asteroid lightcurve work by “backyard astronomers,” the results of which When working any asteroid, keep in mind that the best results for have been the publication of several models in recent issues of the shape and spin axis modeling come when lightcurves are obtained Minor Planet Bulletin. over a large range of phase angles within an apparition. If at all possible, try to get lightcurves not only close to opposition, but Funding for Warner and Harris in support of this article is before and after, e.g., when the phase angle is 15° or more. This provided by NASA grant NNG06GI32G and by National Science can be difficult at times but the extra effort can and will pay off. Foundation grant AST-0607505. The fourth list gives a brief ephemeris for planned radar targets. Supporting optical observations made to determine the lightcurve’s period, amplitude, and shape are needed to supplement the radar data. Reducing to standard magnitudes is not Minor Planet Bulletin 35 (2008) 140 Lightcurve Opportunities Lightcurve Opportunities (continued)

Brightest Brightest # Name Date Mag Dec U Period Amp # Name Date Mag Dec U Period Amp ------4798 Mercator 07 02.8 14.8 -24 21479 Marymartha 08 27.7 14.7 -12 2465 Wilson 07 03.7 15.0 -24 2 6.1 0.2 4269 Bogado 08 28.6 15.0 -10 15805 1994 GB1 07 04.7 14.9 -34 4139 Ul'yanin 08 29.1 15.0 -10 3880 Kaiserman 07 05.6 15.0 -17 6376 Schamp 08 29.2 14.6 - 7 7965 Katsuhiko 07 07.6 13.9 -45 27351 2000 DO73 08 29.5 14.6 -13 1836 Komarov 07 08.3 13.6 -19 5977 1992 TH1 08 30.2 14.8 -15 1598 Paloque 07 09.6 14.4 -25 3502 Huangpu 08 30.3 15.0 -12 5051 Ralph 07 11.7 15.0 -18 1428 Mombasa 08 30.4 14.2 -27 2 17.12 0.25 4919 Vishnevskaya 07 12.7 14.8 -32 5132 Maynard 08 31.4 14.7 - 7 57356 2001 QG293 07 12.7 15.0 - 9 1799 Koussevitzky 09 01.1 14.1 - 9 2 6.32 0.25 5749 1991 FV 07 14.3 14.4 -15 842 Kerstin 09 01.3 14.7 -18 1958 Chandra 07 14.8 14.2 -35 2220 Hicks 09 01.5 14.4 -12 4145 Maximova 07 15.0 14.6 -22 7638 Gladman 09 02.0 14.8 -16 1+ 15. 0.21 07 15.5 12.5 -24 2 19.67 0.20 7950 Berezov 09 02.5 15.0 -11 3494 Purple Mtn. 07 15.5 14.7 -12 3298 Massandra 09 03.1 14.9 - 3 1327 Namaqua 07 16.5 15.0 -30 848 Inna 09 03.4 14.0 - 6 2008 BT18 07 16.6 12.7 -50 224 Oceana 09 04.6 11.7 - 9 2 9.38 0.10 3761 Romanskaya 07 17.4 14.1 + 7 2 15.32 0.34 7043 Godart 09 05.3 14.1 - 6 7851 Azumino 07 18.5 14.0 -21 11434 1931 TC2 09 06.6 14.8 - 8 6670 Wallach 07 18.6 13.7 -16 09 08.9 13.5 - 9 2005 RC34 07 18.7 14.0 – 1 3619 Nash 09 09.1 14.8 - 6 90403 2003 YE45 07 19.4 15.0 +60 5614 Yakovlev 09 09.8 14.8 + 4 3543 Ningbo 07 20.2 14.8 -19 3014 Huangsushu 09 11.6 14.1 - 5 3831 Pettengill 07 21.3 14.3 -15 1410 Margret 09 12.0 14.6 - 4 5588 Jennabelle 07 22.6 15.0 -29 14480 1994 PU1 09 12.1 14.8 - 6 791 Ani 07 22.7 12.4 -15 2 16.72 0.32 7748 1987 TA 09 12.2 14.7 - 2 2644 Victor Jara 07 23.8 14.8 -24 15151 2000 EU148 09 13.0 14.9 - 6 5661 Hildebrand 07 24.5 14.3 -25 2 13.61 0.21 5985 1942 RJ 09 13.1 14.0 + 9 8195 1993 UC1 07 25.8 15.0 - 4 1137 Raissa 09 14.5 13.1 -11 1 37. 0.34 2399 Terradas 07 26.0 14.4 -15 2178 Kazakhstania 09 15.2 14.6 - 5 819 Barnardiana 07 26.0 13.3 -25 5855 Yukitsuna 09 16.0 14.3 -16 2 19.2 0.8 1754 Cunningham 07 26.9 14.5 - 9 2 4.28 0.10-0.17 4012 Geballe 09 16.7 14.9 + 6 4643 Cisneros 07 27.0 14.7 -20 3396 Muazzez 09 16.7 14.7 -11 2763 Jeans 07 27.0 13.9 -20 1170 Siva 09 16.9 14.0 -11 1 5.21 0.04 2431 Skovoroda 07 27.2 14.0 -22 4135 Svetlanov 09 17.5 14.4 + 3 6422 Akagi 07 27.9 13.9 -18 7818 Muirhead 09 17.9 15.0 -14 4446 Carolyn 07 28.0 15.0 - 9 13073 1991 RE15 09 17.9 15.0 + 2 5967 Edithlevy 07 28.3 14.9 -18 2056 Nancy 09 17.9 13.8 + 4 1 > 15.0 0.08 1233 Kobresia 07 28.3 14.1 -17 2 27.83 0.34 2000 DP107 09 18.5 14.6 +19 3 2.78 0.18 1928 Summa 07 28.4 14.6 -12 1 9.66 >0.14 2509 Chukotka 09 18.7 14.2 + 0 2616 Lesya 07 31.0 14.1 -17 1603 Neva 09 20.1 14.2 -11 2 6.42 0.22 6409 1992 VC 07 31.6 15.0 -42 4323 Hortulus 09 20.6 14.8 + 8 1420 Radcliffe 08 01.1 14.6 -14 2861 Lambrecht 09 21.1 15.0 + 0 956 Elisa 08 01.3 14.0 - 7 1 3.9 0.08 1732 Heike 09 22.1 14.6 - 7 2 3.90 0.27 08 01.8 12.3 -24 2 16.13 0.18-0.4 1010 Marlene 09 23.1 13.8 - 6 2 31.06 0.32 576 Emanuela 08 04.2 12.2 -13 2- 8.19 0.06 1707 Chantal 09 23.4 13.9 - 1 1 > 10. >0.2 4209 Briggs 08 04.3 14.8 -28 2 12.23 0.44 11015 Romanenko 09 23.4 15.0 + 0 3919 Maryanning 08 05.3 15.0 -13 85396 1996 SB7 09 24.0 14.8 + 8 2938 Hopi 08 05.6 14.9 -50 1473 Ounas 09 24.4 13.8 +15 1267 Geertruida 08 05.6 14.1 -25 2 5.50 0.5 1376 Michelle 09 25.7 13.3 - 1 2+ 6.0 0.19 3729 Yangzhou 08 06.1 14.6 -36 1 1.2 0.15 911 Agamemnon 09 27.4 14.7 +13 1 7. 0.07-0.4 11 Parthenope 08 06.6 8.7 -18 2 9.43 0.05-0.12 4169 Celsius 09 29.6 14.6 + 5 2+ 10.88 0.44 1354 Botha 08 07.9 14.5 -25 1+ 4. 0.21 1066 Lobelia 09 30.1 13.9 + 7 6690 Messick 08 09.9 14.6 -16 2631 Zhejiang 09 30.1 14.9 - 2 5122 Mucha 08 10.3 14.7 -25 164400 2005 GN59 09 30.2 13.6 +61 746 Marlu 08 10.3 13.1 -37 2 7.78 0.23 09 30.8 10.5 + 2 2- 7.16 0.07-0.15 7833 Nilstamm 08 10.6 14.9 -16 15012 1998 QS92 08 10.8 14.4 -26 2599 Veseli 08 11.6 13.7 -32 2 18.54 0.33 Low Phase Angle Opportunities 2232 Altaj 08 12.5 14.6 - 9 6320 Bremen 08 12.9 14.8 -14 # Name Date α V Dec U Period AMin AMax 7759 1990 QD2 08 13.1 14.6 -16 ------2899 Runrun Shaw 08 15.3 14.9 -19 62 Erato 07 01.5 0.43 13.3 -22 3 9.2213 0.12-0.15 9000 Hal 08 15.4 14.8 + 0 974 Lioba 07 03.0 0.89 13.5 -25 3 38.7 0.37 48902 1998 MP31 08 15.7 14.9 - 7 517 Edith 07 04.9 0.20 14.0 -22 2 9.274 0.12-0.18 2836 Sobolev 08 16.1 14.9 -20 449 Hamburga 07 05.1 0.50 13.3 -24 0.01 539 Pamina 07 06.2 0.75 12.9 -21 3 13.903 0.10 5489 Oberkochen 08 17.7 14.2 -30 412 Elisabetha 07 15.6 0.98 12.6 -24 2 19.67 0.20 32497 2000 XF18 08 19.3 15.0 - 8 534 Nassovia 07 25.0 0.80 13.7 -22 4 9.47 0.15-0.37 4671 Drtikol 08 20.0 15.0 -16 2763 Jeans 07 27.0 0.32 14.0 -20 26843 1991 UK1 08 20.4 15.0 -13 379 Huenna 07 27.1 0.75 12.3 -17 2 7.022 0.09 32479 2000 SL312 08 20.9 14.7 - 5 6422 Akagi 07 27.9 0.35 13.9 -18 6991 Chichibu 08 22.2 14.6 -15 856 Backlunda 07 31.7 0.56 13.7 -19 2 12.08 0.29 166 08 04.6 0.53 12.8 -18 3 4.715 0.13-0.35 3928 Randa 08 22.9 14.4 - 7 53 Kalypso 08 06.0 0.45 12.8 -15 2 17. 0.1 2116 Mtskheta 08 23.6 15.0 - 6 11 Parthenope 08 06.6 0.61 8.8 -18 2 9.43 0.05-0.12 31415 1999 AK23 08 24.1 14.9 - 9 1171 Rusthawelia 08 08.0 0.35 14.0 -17 3 10.98 0.26 1481 Tubingia 08 24.9 14.1 -13 1 160. 0.55 287 Nephthys 08 08.2 0.91 10.8 -14 2 7.603 0.20 2253 Espinette 08 26.0 13.2 -12 2 7.3 0.48 214 Aschera 08 12.1 0.80 12.8 -17 3 6.835 0.22 2519 Annagerman 08 26.3 14.6 -14 181 Eucharis 08 13.1 0.37 12.7 -13 3 52.23 0.05-0.15 760 Massinga 08 17.4 0.58 13.1 -15 3 10.72 0.14 1043 Beate 08 26.3 13.6 - 9 2 22.05 0.32 2253 Espinette 08 26.1 0.97 13.2 -12 2 7.3 0.48 2527 Gregory 08 27.5 14.8 - 7 1043 Beate 08 26.3 0.50 13.7 -09 2 22.05 0.32 Minor Planet Bulletin 35 (2008) 141 Low Phase Angle Opportunities (continued) (35107) 1991 VH

# Name Date α V Dec U Period AMin AMax ------This is a binary asteroid. Watch for signs of mutual events, i.e., 08 31.1 0.62 13.0 -10 3 7.80 0.15-0.20 and eclipses. 224 Oceana 09 04.7 0.69 11.8 -09 2 9.385 0.10 09 10.9 0.21 12.7 -05 2 9.96 0.30 830 Petropolitana 09 12.1 0.28 13.3 -03 DATE RA(2000) DC(2000) E.D. S.D. Mag α 58 Concordia 09 13.7 0.49 12.5 -05 3 9.895 0.10 ------1710 Gothard 09 18.2 0.29 13.9 -02 3 4.939 0.31 07/01 16 13.58 +50 56.2 0.190 1.064 15.91 70.7 1351 Uzbekistania 09 20.1 0.98 13.9 -04 2 73.9 0.34 07/11 15 52.34 +48 50.2 0.156 1.042 15.63 76.3 1062 Ljuba 09 21.0 0.83 13.8 +02 3 33.8 0.17 07/21 15 26.72 +44 29.4 0.120 1.023 15.27 83.5 1707 Chantal 09 23.3 0.45 13.9 -01 1 >10. 0.2 787 Moskva 09 24.6 0.50 12.4 +02 3 6.0556 0.47-0.60 07/31 14 48.86 +35 17.1 0.083 1.005 14.87 94.4 09 30.1 0.61 11.3 +04 4 8.752 0.04-0.44 08/10 13 41.70 +11 33.9 0.052 0.991 14.88 113.9 50 Virginia 09 30.8 0.78 10.5 +02 2 14.31 0.15 08/20 11 41.05 -32 14.6 0.050 0.981 15.75 126.7

Shape/Spin Modeling Opportunities (90403) 2003 YE45 Brightest Per Amp # Name Date Mag Dec U (h) Min Max The window of opportunity for optical observations by most ------47 Aglaja 7 10.9 11.0 -30 4 13.20 0.03-0.17 backyard telescopes is relatively short. Fortunately, the moon (full 534 Nassovia 7 25.1 13.7 -22 4 9.47 0.15-0.37 on July 18), will be waning and not interfere too much. 683 Lanzia 7 22.6 12.7 -02 3 8.630 0.12 11 Parthenope 8 06.6 8.8 -18 2 9.43 0.05-0.12 DATE RA(2000) DC(2000) E.D. S.D. Mag α 505 Cava 8 23.3 12.2 -25 3 8.1789 0.15-0.23 ------ 8 25.4 10.4 -05 4 5.978 0.05-0.24 07/15 11 57.44 +51 38.7 0.044 0.994 15.86 120.1 238 Hypatia 9 08.0 11.8 +00 4 8.86 0.12-0.15 07/20 15 53.55 +59 16.7 0.064 1.013 15.08 90.6 1917 Cuyo 9 08.0 14.5 +23 3 2.690 0.44 07/25 17 31.20 +53 18.0 0.095 1.034 15.41 76.2 64 Angelina 9 30.2 11.3 +04 4 8.752 0.04-0.44 07/30 18 08.99 +48 40.1 0.127 1.056 15.84 68.2 08/04 18 28.76 +45 24.0 0.161 1.078 16.24 63.0 Radar-Optical Opportunities

The list of potential targets is quite long this quarter and so detailed descriptions will not be provided for each one. Use the ephemerides to judge your best chances for observing. Please note that these are geocentric positions. Use the resources given above to generate updated and topocentric positions. In the ephemerides, E.D. is earth distance (AU), V is the V magnitude, and α is the phase angle.

Jean-Luc Margot is principal investigator (PI) for 1991 VH and 2000 DP107. You can contact him directly with your questions or data at [email protected].

216 Kleopatra

This has been called the “dog bone” asteroid because of its highly- elongated body with a “knobs” at each end. It’s accessible for several months.

DATE RA(2000) DC(2000) E.D. S.D. Mag α ------07/01 23 14.13 +11 26.3 1.918 2.389 11.55 24.3 07/16 23 22.22 +13 17.0 1.725 2.354 11.25 22.9 07/31 23 25.50 +14 31.0 1.552 2.319 10.92 20.2 08/15 23 23.36 +14 51.8 1.407 2.287 10.56 16.1 08/30 23 16.28 +14 05.1 1.301 2.256 10.21 11.0 09/14 23 06.35 +12 07.5 1.244 2.227 9.96 7.4 09/29 22 57.19 + 9 19.2 1.241 2.201 10.02 9.9 10/14 22 52.39 + 6 18.8 1.290 2.177 10.25 15.6 10/29 22 53.96 + 3 44.8 1.382 2.156 10.52 20.8 11/13 23 02.18 + 1 59.4 1.507 2.139 10.79 24.5

8567 1996 HW1 EDITOR ON SABBATICAL

This asteroid remains within fairly easy reach, in terms of Beginning with MPB 35-4, the MPB Editor will be on a one brightness, for several weeks. year sabbatical from his MIT teaching duties for the purpose of fully engaging in research activities. Coincident with this DATE RA(2000) DC(2000) E.D. S.D. Mag α academic sabbatical will be a one year sabbatical from the ------08/01 21 43.88 +18 05.8 0.250 1.220 14.07 31.4 editorship of the Minor Planet Bulletin. During this period, 08/16 22 30.60 +20 44.5 0.188 1.169 13.33 30.9 Brian D. Warner will serve as “Acting Editor”. Thus, authors 08/31 23 43.37 +18 40.8 0.147 1.137 12.65 27.8 are directed to submit their manuscripts to the Acting Editor 09/15 1 09.85 + 9 35.1 0.135 1.128 12.35 24.2 beginning with MPB 35-4. 09/30 2 14.92 - 1 28.4 0.155 1.141 12.66 23.9 Minor Planet Bulletin 35 (2008) 142

THE MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly journal of the Minor Planets Section of the Association of Lunar and Planetary Observers – ALPO. Beginning with volume 32, the current and most recent issues of the MPB are available on line, free of charge at http://www.minorplanetobserver.com/mpb/default.htm . Subscription information for conventional printed copies is given below.

Nonmembers are invited to join ALPO by communicating with: Matthew L. Will, A.L.P.O. Membership Secretary, P.O. Box 13456, Springfield, IL 62791-3456 ([email protected]). The Minor Planets Section is directed by its Coordinator, Prof. Frederick Pilcher, 4438 Organ Mesa Loop, Las Cruces, NM 88011 USA ([email protected]), assisted by Lawrence Garrett, 206 River Road, Fairfax, VT 05454 USA ([email protected]). Steve Larson, Lunar and Planetary Laboratory, 1629 E. University Blvd., University of Arizona, Tucson, AZ 85721 USA ([email protected]) is Scientific Advisor. The Asteroid Photometry Coordinator is Brian D. Warner, Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908 USA ([email protected]).

Brian D. Warner (address above) is the MPB Acting Editor while Dr. Richard P. Binzel is on sabbatical. The MPB is produced by Dr. Robert A. Werner, JPL MS 301-150, 4800 Oak Grove Drive, Pasadena, CA 91109 USA ([email protected]) and distributed by Derald D. Nye.

The contact for all subscriptions, contributions, address changes, etc. is:

Mr. Derald D. Nye Minor Planet Bulletin 10385 East Observatory Drive Corona de Tucson, AZ 85641-2309 USA ([email protected]) (Telephone: 520-762-5504)

Annual subscription rates for the Minor Planet Bulletin by postal delivery:

Payment Payment by by check credit card North America $24.00 $25.00 All other $34.00 $35.00

To minimize our administrative time, please consider subscribing for two years. Users of the on-line MPB who are not paid subscribers are encouraged to make a voluntary contribution of $5 or more per year. Checks or money orders should be in US dollars, drawn on a US bank, and made payable to the “Minor Planet Bulletin.” To pay by credit card, (Visa, Mastercard, or Discover) please send by mail your credit card number, your name exactly as it appears on the card, and the expiration date. Be sure to specify the desired length of your subscription. Credit card charges will be made through “Roadrunner Mkt, Corona AZ.” When sending your subscription order, be sure to include your full mailing address and an email address, if available. The numbers in the upper-right corner of your mailing label indicate the volume and issue number with which your current subscription expires.

Authors are strongly encouraged to submit their manuscripts by electronic mail ([email protected]). Electronic submissions can be formatted either using a Microsoft Word template document available at the web page given above, or else as text-only. A printed version of the file and figures must also be sent. All materials must arrive by the deadline for each issue. Visual photometry observations, positional observations, any type of observation not covered above, and general information requests should be sent to the Coordinator.

* * * * *

The deadline for the next issue (35-4) is July 15, 2008. The deadline for issue 36-1 is October 15, 2008.

Minor Planet Bulletin 35 (2008)