49 THE MINOR PLANET

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

VOLUME 31, NUMBER 3, A.D. 2004 JULY-SEPTEMBER 49.

CCD PHOTOMETRY OF ASTEROIDS 970 PRIMULA AND ideal for individuals or universities with small research 1631 KOPFF USING A REMOTE COMMERCIAL departments. TELESCOPE The targets were selected from a list of asteroid photometry Pedro V. Sada opportunities published by Brian Warner on his Collaborative Eder D. Canizales Asteroid Lightcurve Link (CALL) website (Warner, 2003). Edgar M. Armada Selection criteria included: proximity of the two asteroids to each Departamento de Física y Matemáticas other and to a nearby suitable star calibration field to save on Universidad de Monterrey telescope slewing time, asteroid declination and closeness of Av. I. Morones Prieto 4500 Pte. opposition date to dates of observation for maximum nightly Garza García, N. L., 66238 coverage, appropriate asteroid magnitude to acquire enough MÉXICO counts for a S/N of at least 100 with 1-minute V-filtered [email protected] exposures, and a high reported asteroid absolute magnitude (H- value) to target the smallest asteroid size possible. (Received: 12 February) Usable data were collected on 2003 October 28-29 and November 04-05 for both asteroids. There was an additional night of data for CCD photometry of asteroids 970 Primula and 1631 1631 Kopff on November 15. All dates are UT. Two other nights Kopff obtained remotely at Tenagra Observatories of data were obtained but were not used because most of the during October and November 2003 is reported. A images showed evidence of clouds. In total, 117 images were synodic rotation period of 2.777 ± 0.001 hours is obtained and processed for 970 Primula, and 181 for 1631 Kopff, determined from four nights of observations for Primula. using a standard Johnson V photometric filter and 1-minute The resulting rotation period for Kopff is 6.683 ± 0.001 exposure times. Of these, 112 (95.7%) were used in the final hours from five nights of observations. Both observed analysis for 970 Primula and 170 (93.9%) for 1631 Kopff. The lightcurves were nearly symmetrical with amplitudes of rest were discarded because of asteroid proximity to stars. 0.18 ± 0.02 magnitudes for Primula and 0.41 ± 0.04 for Standard bias, dark current and flat field corrections were applied. Kopff. Five stars were used in each image as magnitude comparisons for the asteroid. A nearby star field, identified from the 'LONEOS Photometric Calibration Star List' (Skiff, 2003), was observed Observations each night for magnitude calibration. Stars with known magnitudes were used to determine the magnitudes of the asteroid The observations of 970 Primula and 1631 Kopff reported here comparison stars. were made with the Tenagra II telescope at Tenagra Observatories (MPC 926). The instruments used to gather the data were a Reduction and Results computerized 0.81m (32-inch) f/7 Ritchey-Chrétien telescope with a SITe-based 1024x1024x24 µm electronic imager yielding ~0.87 Times were corrected for light travel from the asteroid to the Earth arc-seconds per pixel for a field of view of ~15'x15' (Schwartz, and were taken to be at the mid-times of the image exposures. 2003). The chip temperature is set at –45° C and the images were Relative magnitudes from night to night were uncertain as 2x2 binned for file transfer economy since previous reports had different comparison star sets were used. This was dealt with by shown no apparent effect of binning on the photometry (Ditteon et using additive constants to bring all the data into the best al. 2003). Tenagra Observatories, directed by Michael Schwartz agreement possible. However, these arbitrary magnitude shifts and assisted by Paulo Holvorcem for minor planet and comet were small (≤0.04 magnitudes). Additional magnitude shifts were studies, offers commercial telescope time with two telescopes in also used to compensate for the intrinsic magnitude variation of southern Arizona. These are fully automated instruments. An the asteroids due to their change of distance with respect to the observer only needs to send instructions on which objects to Earth, and to phase angle variations (15.2°-11.1° for 970 Primula observe, and the imaging requests from several users are sorted and 14.2°-5.3° for 1631 Kopff). and executed throughout the night. The data are stored for immediate FTP retrieval, including calibration frames. This The best-fit rotational periods for the asteroids were obtained by convenient setup saves time, travel and lodging expenses and is computing the power spectrum of the time series of data (Scargle,

Minor Planet Bulletin 31 (2004) 50

1982; Horne and Baliunas, 1986). The resulting synodic rotational period for 970 Primula from the data presented here is 2.777 ± 0.001 hours. The amplitude of the lightcurve is 0.18 ± 0.02 magnitudes (see Figure 1). For 1631 Kopff the resulting synodic rotational period was 6.683 ± 0.001 hours with an amplitude of 0.41 ± 0.04 magnitudes (see Figure 2). Both asteroids exhibited two similar maxima and minima per rotation. The time scale is given in rotational phase with the zero corresponding to 2003 November 04 at 12.0 hrs UTC (JD 2452948.0). The magnitude scale is also referenced to this epoch since it was the night that exhibited the best photometry.

This is probably the first reported rotational period for these asteroids since they are not listed in A. Harris and B. Warner’s ‘Minor Planet Lightcurve Parameters’ list (Harris and Warner, 2003).

Acknowledgments

We would like to thank R. Hernández for contributing funds for these observations. Many thanks also for M. Schwartz and P. Holvorcem, from Tenagra Observatories, Ltd., for making remote observing possible, simple, and fun; and for providing Pro Bono time for this project, which was a real ‘hands-on’ learning Figure 1: Composite lightcurve of asteroid 970 Primula derived experience for students. from 112 observations and a 2.777-hour rotation period. References

Ditteon, R., Tollefson, E., and Twarek, A. (2003). “Asteroid Photometry Using a Remote Commercial Telescope: Results for Asteroids 808, 1225, and 28753.” Minor Planet Bulletin 30, 76- 77.

Harris, A. W. and Warner, B. D. (2003). “Minor Planet Lightcurve Parameters. ” Posted on the WWW: http://cfa- www.harvard.edu/iau/lists/LightcurveDat.html (2003 December 15 update).

Horne, J. H. and Baliunas, S. L. (1986). “A Prescription for Period Analysis of Unevenly Sampled Times Series.” Astrophysical Journal 302, 757-763.

Scargle, J. D. (1982). “Studies in Astronomical Time Series Analysis. II – Statistical Aspects of Spectral Analysis of Unevenly Spaced Data.” Astrophysical Journal 263, 835-853.

Schwartz, M. (2003). “Tenagra Observatories, Ltd.” Posted on the WWW: http://www.tenagraobservatories.com/

Skiff, B. (2002). “LONEOS Photometric Calibration Star List.” Posted on the WWW: ftp://ftp.lowell.edu/pub/bas/starcats/ Figure 2: Composite lightcurve of asteroid 1631 Kopff derived loneos.phot (2003 July 15 update). from 170 observations and a 6.683-hour rotation period.

Warner, B. D. (2003). “Potential Lightcurve Targets 2003 October – December. ” Posted on the WWW: http://www .minorplanetobserver.com/astlc/default.htm

Minor Planet Bulletin 31 (2004) 51

172 BAUCIS — A SLOW ROTATOR lightcurve (particularly the minima) over the observing period of more than one month. A number of initial trials were done C.S. Bembrick between 1.5 and 2.25 days as Zeigler (1999) had listed a period of PO Box 1537, Bathurst, NSW 2795, Australia 51.25 hours. It rapidly became apparent that our data could not be [email protected] phased with that period.

T. Richards A subset of the data was compiled using the six best nights and the 8 Diosma Rd, Eltham, Vic 3095, Australia “AVE” software (Barbera 2004) was used for a period search utilizing the Phase Dispersion Minimisation (PDM) method. G. Bolt Searching between 1.0 and 2.0 days yielded a distinct minimum in 295 Camberwarra Drive, Craigie, WA 6025, Australia the “periodogram” between 1.140 and 1.143 days – and also an alias at 1.7 days. Further refinement narrowed this to 1.142 days. B. Pereghy A number of trial phase plots, gradually folding in the additional 37 Hatfield St, Blakehurst, NSW 2221, Australia data, showed that 1.1424 days (27.417 hours) was the best fit to D. Higgins the data. 7 Mawalan St, Ngunnawal, ACT 2913, Australia The phase stacked composite lightcurve for the 2003 observations W. H. Allen is displayed in Figure 1 – with arbitrary zero phase (JD 83 Vintage Lane, RD 3 Blenheim, NZ 2452852.80) to best display the data on the phase plot. Magnitudes from individual nights were adjusted by an additive (Received: 14 March) constant to give a “best fit” to the phase stack. Note the varying depths of the minima which have changed over the observing period. The overall peak-to-peak variation between extrema was Lightcurve measurements of 172 Baucis in 1985 and 0.25 magnitudes in 2003. To a first approximation (using a tri- 1999 were inconclusive in determining the period of axial ellipsoid model), this implies a ratio a/b of 1.26, where a, b rotation. However in 2003 a combined effort by and c are the semi-axes of the ellipsoid and rotation is about the Southern Hemisphere observers derived a synodic shortest axis, c. rotation period of 27.417 ± 0.013 hours. The overall variation was 0.25 magnitudes in 2003, but appears to Data from other years were then individually folded at the derived have been 0.4 in 1999 and 0.35 in 1985. period. Zeigler’s 1985 data are compatible with this period although the lightcurve is fragmentary. The total variation appears to be 0.35 magnitudes. Similarly for our unpublished 1999 data, Introduction where the overall variation appears to be 0.40 magnitudes. Both of these data sets show a deep minimum in the light curve which Minor planet 172 Baucis was discovered by A. Borrelly at could be compared to the first minimum of Figure 1. Marseilles in February, 1877. Baucis is an inner main belt, S-type asteroid with an estimated diameter of 64.5 km. The albedo is The 1989 data (Weidenschilling, et al. 1990) when phased with quoted as 0.12 and the B-V = 0.9 (Binzel et al. 1989). The latest our period produces a deep minimum (0.2 mag. in depth) not list of Harris (2003) indicates that the rotation period is probably dissimilar to the first mimimum in Figure 1 and also similar to the more than 16 hours and the lightcurve amplitude is at least 0.23 1985 data. However, 0.2 magnitudes is almost certainly not the magnitude. However, a reliability code of only one is assigned to maximum variation for that opposition as the observations sample these data. only 45% of the lightcurve. If we rely on data from 1985, 1999 and 2003, then a plot of Heliocentric Longitude vs maximum delta Baucis has been the subject of a number of investigations, magnitude suggests that the Longitude of the rotational pole lies at including six nights of photoelectric photometry by Zeigler in 55 or 235 degrees. 1985 who proposed a period of 51.25 hours (Zeigler, 1999). Weidenschilling et al. (1990) suggested a period of either 13 or 26 hours based on two single night lightcurves in 1984 and 1989. -0.3 Observations over three nights by Bembrick and Pereghy in 1999 172 Baucis (unpublished) indicated that a period near 26 hours was possible. 2003

Observations and Results -0.2 In 2003 Baucis was well placed at southerly declinations so Southern Hemisphere observers from Western Australia to New Zealand (spanning nearly 60 degrees of Longitude) undertook a Delta Mag joint observing program. The names and locations of the Aug-01 -0.1 Aug-02 observers are listed in Table I. In all, some eight nights of good Aug-03 data were acquired over a time span of 33 days. The observational Aug-06 Aug-07 circumstances are summarized in Table II, which also shows the Aug-26 Aug-29 Phase stacked with P = 1.1424 days phase coverage of the light curve on individual nights. Sep-02

0.0 Data from each night were plotted as differential instrumental 0.0 0.1 0.2 0.3 0.4 0.5 Phase0.6 0.7 0.8 0.9 1.0 magnitude vs JD. No light-time corrections were applied. Initial Figure 1. Composite lightcurve for asteroid 172 Baucis. attempts to do a quick phase stack by graphical and “eyeball” methods failed – largely due (in hindsight) to the evolution of the Minor Planet Bulletin 31 (2004) 52

Conclusions 346 HERMENTARIA – ANOTHER SLOW ROTATOR?

Minor planet 172 Baucis is a slow rotator, with a synodic rotation C. Bembrick of 27.417 ± 0.013 hours. Although observations spanned more PO Box 1537, Bathurst, NSW 2795, Australia than a month, the 2003 data when phase stacked cover only 85% [email protected] of the complete lightcurve. The overall variation was 0.25 magnitudes, but in previous years appears to have been more than B. Pereghy this, suggesting that 2003 was not an equatorial aspect. The axial 37 Hatfield St, Blakehurst, NSW 2221, Australia ratio a/b is at least 1.26 and may be as much as 1.44. For these reasons and to confirm the period, Baucis deserves observing at A. Ainsworth future oppositions. 28 Lansdowne Pde, Oatley, NSW 2223, Australia

Acknowledgements G. Bolt 295 Camberwarra Drive, Craigie, WA 6025, Australia The assistance of Alan Harris in providing original unpublished data obtained by Ken Zeigler in 1985 is gratefully acknowledged. (Received: 18 March )

References Observations of minor planet 346 Hermentaria in 2003 Barbera, R. (2004). “AVE” Analisis de Variabilidad Estelar, indicate that it has a probable synodic rotation period of version 2.51. Grup d’Estudis Astronomics. 28.43 ± 0.06 hours. The lightcurve amplitude at this http://usuarios.lycos.es/rbarbera/AVE/AveInternational.htm opposition was 0.2 magnitude, similar to that of 1998. Further work is needed to refine this suggested period. Binzel, Richard P., Gehrels, Tom and Matthews, Mildred Shapley (1989). Asteroids II. Univ. Ariz. Press, Tuscon, Arizona. Introduction

Harris, A.W. and Warner, B.D. (2003). “Minor Planet Lightcurve Minor planet 346 Hermentaria was discovered by A. Charlois at Parameters.” Updated Dec 15, 2003 & posted on http://cfa- Nice in November, 1892. It was probably named after the village www.harvard.edu/iau/lists/LightcurveDat.html of Herment in the Auvergne region of southern France. This S- type, main-belt asteroid has an estimated diameter of 110 km, and Weidenschilling, S. J., Chapman, C. R., Davis, D. R., Greenburg, albedo of 0.13 and a B-V of 0.85 (Binzel at al. 1989). In the latest R., Levy, D. H., Binzel, R. P., Vail, S. M., Magee, M., and Spaute, list of Harris and Warner (2003) the probable period is quoted as D. (1990). “Photometric Geodesy of Main-Belt Asteroids. III 19.408 hours and the lightcurve amplitude as 0.07 magnitude. A Additional Lightcurves.” Icarus 86, 402-447. reliability of 2 is assigned to these values. However, a previous suggested period of 28.33 hours is given a reliability of only 1. Zeigler, Kenneth, W. (1999). “Astronomical Research Involving Junior High and High School Students.” In the proceedings of the Hermentaria has been observed on a number of oppositions, 1999 Minor Planet Amateur/Professional Workshop (Paul Comba, including 1980 (Harris and Young, 1989), 1981 (Harris et al. Ed.), pp 70-73. 1992), 2001 and 2002 (Wang and Shi, 2002). In addition, the first three authors above have unpublished data over five nights Table I. Observer Locations — 2003 from the 1998 opposition. Largely because of the long period, the previous observations have all produced partial light curves from Observer Lat.(S) Long.(E) Alt.(m) which assumptions have been made to interpret a rotation period. C.Bembrick 33.4348 149.7576 880 T. Richards 37.7156 145.1673 100 G. Bolt 31.7906 115.7571 45 The first suggested period was 28.326 hours (Harris and Young, D. Higgins 35.1624 149.1100 655 1989), on the basis of nine nights in 1980. Two further nights of W.H.Allen 41.50 173.85 30 observations in 1981 were not inconsistent with this period (Harris et al. 1992). The 1998 data indicated that a period close to 28 hours was possible, but other periods such as 22 and 37 hours Table II. Observational Circumstances were not ruled out. On two nights in 2001 and two nights in 2002 Heliocentric Solar Phase Wang undertook observations and these were composited to Date of Lat. Long. R Phase Cover- derive a period of 19.408 hours (Wang and Shi, 2002). Obs (B°) (L°) (AU) Angle age (%) Aug 01 -4.25 307.317 2.125 4.08 40 Observations and Results Aug 02 -4.19 307.648 2.125 4.25 16 Aug 03 -4.14 307.979 2.124 4.48 22 Aug 06 -3.98 308.978 2.123 5.48 30 In 2003 Hermentaria was favourably placed at southerly Aug 07 -3.93 309.305 2.122 5.88 32 declinations – although in crowded star fields. Consequently a Aug 26 -2.88 315.625 2.114 14.70 28 Aug 29 -2.71 316.626 2.113 15.99 23 further effort was made to try to pin down the rotation period. Sep 02 -2.48 317.962 2.112 17.62 24 Due to the long period, the crowded fields and the weather constraints, only a few partial light curves were obtained in 2003. A summary of the observational circumstances is presented in Table I, which also shows the phase coverage of the lightcurve on individual nights.

Data from each night were plotted as differential magnitude vs JD. No light-time corrections were appplied. From inspection of the Minor Planet Bulletin 31 (2004) 53

-0.1 346 Hermentaria Conclusion

Minor Planet 346 Hermentaria appears to be a slow rotator, with a synodic period of 28.43 ± 0.06 hours (1.1846 days). The maximum variation in 2003 was 0.2 magnitudes, implying axial 0.0 ratio a/b = 1.2. The prevously published period of 19.408 hours (Wang and Shi, 2003) appears to us to be incorrect. However, there are still significant gaps in the phase stack and further Phase stacked with P = 28.43 hours

Delta Mag detailed observations are required to fully define the light curve 0.1 and refine the period.

Jun-07 Jun-08 2003 C. Bembrick Acknowledgements Jun-11 G. Bolt

0.2 The assistance of Dr. Alan Harris in providing reprints and e-mail 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 Phase contacts is gratefully acknowledged. Warm thanks are also extended to Dr Xiao-Bin Wang of Yunnan Observatory for Figure 1. The composite lightcurve in 2003. providing copies of her original data.

References data on individual nights the period must be >21 hours. Possible periods from our data are 35, 28.3 and 17.5 hours – where the Barbera, R. (2004). “AVE” Analisis de Variabilidad Estelar, latter is clearly too short. Our data extend over only five nights, so version 2.51. Grup d’Estudis Astronomics. the uncertainty in any period determined will be large, particularly http://usuarios.lycos.es/rbarbera/AVE/AveInternational.htm if the period is long. However, we note that our data cannot be satisfactorily phased with a 19.408 hour period (Wang, 2002). Belserene, E.P. (1988). “Rhythms of a Variable Star”. In Astronomical Computing, Sky & Telesc., 76, 288-290. Period searches using the AAVSO “TS” software yielded a possible period around 1.1 days. Similarly, searches using the Binzel, R. P., Gehrels, T. and Matthews, M. S. (1989). Asteroids discrete Fourier transform (DFT) method (Belserene, 1988) also II. Univ. Ariz. Press, Tucson, Arizona. yielded a possible period of around 1.1 days. Periods around 1.5 and 1.7 days were also found, but these were later judged to be Harris, A.W. and Warner, B. D. (2003). Minor Planet Lightcurve aliases. The “AVE” software (Barbera 2004) and the Phase Parameters. Updated Dec 15, 2003 & posted on – http://cfa- Dispersion Minimisation (PDM) method was used to test periods www.harvard.edu/iau/lists/LightcurveDat.html between 0.75 and 2.5 days. The best periods were found to lie betwen 1.175 and 1.185 days. Trial phase stacks then refined this Harris, A. W., and Young, J. W. (1989). “Asteroid Lightcurve to 1.1846 days (28.43 hours) as being the best fit to the data. This Observations from 1979-1981.” Icarus 81, 314-364. period was then used to produce the composite lightcurve in Figure 1, where the overall variation is 0.2 magnitudes. However, Harris, A. W., Young, J. W., Dockweiler, T. and Gibson, J. note there is very little overlap in the data from individual nights (1992). “Asteroid Lightcurve Observations from 1981.” Icarus and an assumption has been made that the two maxima are 95, 115-147. approximately the same size in order to align the individual nights data on the magnitude scale. Wang, Xiao-Bin and Shi, Ying. (2002). “CCD Photometry of Asteroids 38, 174, 276 and 346.” Earth, Moon and Planets 91, Original data sets from Yunnan Observatory at the 2001 and 2002 181-186. oppositions (Wang and Shi, 2002) were then examined to see if a fit could be made to our derived period. Phase stacking the two Table I. Observational Circumstances — 2003 nights of 2001 data produced a fragmentary light curve, with an overall variation of <0.1 magnitudes. The two adjacent nights of Heliocentric Solar Phase 2002 data produced a partial lightcurve with one distinct minimum Date of Lat. Long. R Phase Cover- Obs (B°) (L°) (AU) Angle age(%) and one (partial) maximum. – the overall variation being 0.1 Jun 07 0.38 269.684 2.880 7.11 17 magnitudes. We believe that the 2002 data at least are not Jun 08 0.354 269.879 2.879 6.74 27 inconsistent with our period. The unpublished 1998 data, when Jun 11 0.264 270.466 2.876 5.59 28 phased with our derived period shows a partial lightcurve with a delta magnitude of at least 0.15, but with a large gap in the phase plot of 0.4 phase. We have not attempted to combine data fom diffferent oppositions due to the low precision of our interpreted period.

We note that Harris and Young (1989), in proposing their original 28.326 hour period, suggest that the lightcurve is singly periodic – i.e. having only one maximum and one minimum per cycle. Although we have derived essentially the same period, our composite lightcurve (Figure 1) is distinctly doubly periodic.

Minor Planet Bulletin 31 (2004) 54

2003-04 WINTER OBSERVING CAMPAIGN AT ROSE- Observations and Results HULMAN INSTITUTE. RESULTS FOR 797 MONTANA, 3227 HASEGAWA, 3512 ERIEPA, 4159 FREEMAN, A total of 19 asteroids were observed during this campaign, but 5234 SECHENOV, AND (5892) 1981 YS1. lightcurves were not found for all of these asteroids. If an asteroid had a very small variation in brightness or appeared to have a Richard Ditteon period longer than about twelve hours during the first night it was Brian Hirsch observed, that asteroid was dropped from further observation. Elaine Kirkpatrick This allowed the maximum number of quality observations with Stephen Kramb limited funds. The variation in the data for 2235 Vittore and 830 Matthew Kropf Petropolitana was below 0.1 mag and 0.05 mag respectively, Joshua Meehl making these difficult targets. Asteroids 580 Selene, 673 Edda, Michael Stanfield and 1351 Uzbekistania all had variations about 0.1 mag and Eric Tollefson appeared to have periods near 32 hours or more. Asteroids 5378 Andrew Twarek Ellyett, 5392 Parker, and 6827 Wombat also had long periods Rose-Hulman Institute of Technology CM 171 (32+hours). Finally, the data on three asteroids (4618 5500 Wabash Avenue Shakhovskoj, 21282 1996 TD15, and 5426 Sharp) turned out to be Terre Haute, IN 47803 little more than noise. We encourage follow-up observations on [email protected] these 11 asteroids whose solutions are necessary so as to not bias the total statistical sample of asteroids in favor of only those (Received: 20 February) having short periods or large lightcurve amplitudes.

In addition to the successful results for 6 asteroids reported below, CCD images recorded in November and December 2003 we also successfully observed 1742 Schaifers and 2953 and January 2004 using the Tenagra 81-cm telescope Vysheslavia. These asteroids were observed for Stephen Slivan at yielded rotation period and lightcurve amplitude results MIT for pole position studies and the data have been sent to him for six asteroids: 797 Montana 4.55 ± 0.01 hr, 0.28 for future publication. mag; 3227 Hasegawa 6.536 ± 0.001 hr, 0.29 mag; 3512 Eriepa 6.7824 ± 0.0008 hr, 0.20 mag; 4159 Freeman All of our data are available upon request. 4.4021 ± 0.0008 hr, 0.35 mag; 5234 Sechenov 12.067 ± 0.006 hr, 0.22 mag; (5892) 1981 YS1 11.905 ± 0.005 797 Montana hr, 0.33 mag. We give information on eleven other asteroids that may have long periods or low amplitudes. Asteroid 797 Montana was discovered on 17 November 1914 by H. Thiele at Bergedorf. It was named after the Latin word for 'mountain village' in honor of Bergedorf (Schmadel, 1999). We Introduction and Procedures used a total of 110 images taken over three nights: 2003 November 15, 16, and 21. The data reveal a lightcurve with a 4.55 During the winter of 2003-04 seven Rose-Hulman students ± 0.01 hr period and 0.28 mag amplitude. (Hirsch, Kramb, Kropf, Meehl, Stanfield, Tollefson, and Twarek) and two professors (Ditteon and Kirkpatrick) obtained images with the 81-cm Ritchey-Chretien telescope at Tenagra Observatory in Arizona. The Tenagra telescope operates at f/7 with a CCD camera using a 1024x1024x24u SITe chip (Schwartz, 2004). Exposure times were generally 90 seconds and our images were binned 2 by 2.

Asteroids were selected for observation by using TheSky published by Software Bisque to locate asteroids that were at an elevation angle of between 20º and 30º one hour after local sunset. In addition, TheSky was set to show only asteroids between 14 and 16 mag. Bright asteroids were avoided because we pay for a minimum 60 second exposure while using this telescope. The asteroids were cross checked with Alan Harris’ list of lightcurve parameters (Harris, 2003). We tried to observe only asteroids that did not have previously reported measurements or had very uncertain published results.

Observation requests for the asteroids and Landolt reference stars were submitted by Ditteon using ASCII text files formatted for the TAO scheduling program (Schwartz, 2004). The resulting images were downloaded via ftp along with flat field, dark and bias 3227 Hasegawa frames. Standard image processing was done using MaxImDL published by Diffraction Limited. Photometric measurements and Asteroid 3227 Hasegawa was discovered on 24 February 1928 by lightcurves were prepared using MPO Canopus published by Karl Wilhelm Reinmuth at Heidelberg. It was named in honor of BDW Publishing. Ichiro Hasewaga, editor of the Yamomoto Circulars (Schmadel, 1999). A total of 86 images were taken over five nights: 2003

Minor Planet Bulletin 31 (2004) 55

December 19, 22, 25, 27, and 28. The data reveal a lightcurve with a 6.536 ± 0.001 hr period and 0.29 mag amplitude.

5234 Sechenov

Asteroid 5234 Sechenov was discovered 4 November 1989 by 3512 Eriepa L.G. Karachkina at Nauchnyj. It was named in honor of the outstanding Russian naturalist Ivan Mikhailovich Sechenov (1829- The asteroid 3512 Eriepa was discovered 8 January 1984 by J. F. 1905) (Schmadel, 1999). There were a total of 92 images Wagner at Anderson Mesa who named the asteroid after his collected over five nights: 2003 December 28, 29, 2004 January 9, hometown, Erie, Pennsylvania (Schmadel, 1999). For this 10, and 12. The apparent period of 5234 Sechenov was found to asteroid, 71 images were taken over 4 nights: 2003 December 17, be 12.067 ± 0.006 hr with 0.22 mag amplitude. However, the 18, 22, and 2004 January 9. The apparent period of 3512 Eriepa lightcurve is incomplete and we are not very confident of this was found to be 6.7824 ± 0.0008 hr with 0.20 mag amplitude. result.

4159 Freeman 5892 1981 YS1

The asteroid 4159 Freeman was discovered 5 April 1989 by E. F. The asteroid (5892) 1981 YS1 was discovered on 23 December Helin at Palomar who named the asteroid in honor of her friend 1981 at Purple Mountain Observatory in Nanking, China Ann Freeman for her birthday (Schmadel, 1999). For this asteroid (Schmadel, 1999). We used a total of 101 images collected over 67 images were taken over 3 nights: 2003 December 17, 18, and six nights: 2003 December 19, 21, 25, 27, 2004 January 10, and 23. The apparent period of 4159 Freeman was found to be 4.4021 11 in this lightcurve. The period was found to be 11.905 ± 0.005 h ± 0.0008 hr with 0.35 mag amplitude. with 0.45 mag amplitude. Here again, because the period is close to 12 hours, we are not as confident of the result as our formal uncertainty would suggest.

Minor Planet Bulletin 31 (2004) 56 Acknowledgements

This research was supported in part by NASA through the American Astronomical Society's Small Research Grant Program. Additional funds were provided by a grant from the Indiana Academy of Science. We also want to thank Michael Schwartz and Paulo Holvorcem for making remote observing with their telescope both possible and enjoyable.

References

Schwartz, M. (2004). “Tenagra Observatories, Ltd.”, http://www.tenagraobservatories.com/, last updated 11 February, 2004.

Schmadel, L. D. (1999) Dictionary of Minor Planer Names. Springer: Berlin, Germany. 4th Edition.

Harris, A. W. and Warner, B. D. “Minor Planet Lightcurve Parameters.” 2003 Dec. 15. http://cfa-www.harvard.edu/iau/ lists/LightcurveDat.html, last updated 11 February, 2004.

CCD PHOTOMETRY OF ASTEROID 12753 POVENMIRE Observations

Bruce L. Gary Asteroid 12753 was 2.0 a.u. from Earth at closest approach in 5320 E. Calle Manzana October, 2003. At that time its average V-magnitude was 17.6. Hereford, AZ 85615 An asteroid this challenging is close to the limit of amateurs using [email protected] modest equipment. It was a major learning experience for me since it was my first attempt at asteroid observing. (Received: 4 April Revised: 9 May) Nine observing sessions totaling 40 hours were conducted over a 3-month period. A Celestron 14-inch Cassegrain telescope on a Main-belt asteroid 12753 Povenmire was observed to German equatorial mount was used with a JMI Smart Focuser, a have a lightcurve period of 12.85 hours and a brightness SBIG AO-7 tip/tilt image stabilizer, SBIG CFW-8 color filter variation of 0.50 magnitude during its 2003 opposition. wheel and SBIG ST-8XE CCD. Telescope control was The lightcurve was symmetrical throughout the 3-month accomplished using MaxIm DL/CCD and MaxPoint. Image observing period, consistent with a simple shape. BVRI analysis was done using MaxIm DL. The telescope was controlled photometry measurements yield the following color from my office using 100-foot cables in buried conduit that go to a indices: V–R = 1.34 ± 0.18 (redder than the sun) and sliding roof observatory. The observing location is at an altitude R–I = 0.33 ± 0.10 (solar-like), implying a typically red, of 4650 feet, located in southern Arizona. then flattening spectral curve. The asteroid was 0.3 magnitudes fainter than predicted, suggesting H=12.8 as Because this asteroid is faint it was necessary to perform a revised absolute magnitude. background subtraction using the star field from images taken before, or after, the asteroid passed through a crowded star field. All sky photometry was used to establish a magnitude scale for V, Introduction R and I filter observations. Additional data analysis was Asteroid 12753 Povenmire is a faint main-belt object discovered performed using QuickBASIC programs written specifically for in 1993 by Eugene and Carolyn Shoemaker and named to honor this project. Quattro Pro and Excel spreadsheet programs were Hal and Katie Povenmire. Pre-discovery positions have been also used. established as far back as 1949, which enabled an accurate orbit to be determined. The closest approach to the sun is 2.238 a.u., Near opposition, when rotation-averaged brightness is unlikely to which will happen during the upcoming 2006 opposition. The change from one observing date to the next, all-sky measurements farthest distance to the sun is 3.01 a.u., which is the approximate were made of nearby standard stars from the Landolt list. geometry for the 2003 opposition. The asteroid is estimated to Extinction plots were constructed so that small brightness have a diameter of 16 km based on its brightness and an assumed corrections could be applied based on differences in the asteroid’s albedo. The absolute magnitude is given as H = 12.5 in the JPL air mass and that for the Landolt stars. CCD transformation Ephemeris, which would yield a brightest V-magnitude of 17.0 equation corrections were not applied, but they are known to be during the 2003 opposition. No information is available for small for this telescope/CCD configuration based on other brightness variation with viewing geometry since a standard value measurement programs for which transformation coefficients were for G = 0.15 is adopted in the Ephemeris. No color information is determined. available.

Minor Planet Bulletin 31 (2004) 57

Color and Lightcurve Results two nearby rotation period solutions with RMS residuals slightly higher than for the global minimum solution. The asteroid was measured to have an R–I color of +0.33 ± 0.10 magnitudes, which is approximately the same as for the sun, The data in Fig. 1 have been subjectively “zero adjusted” so that which has R–I = 0.36. The asteroid’s V–R color was unusual, each night’s magnitude plot agrees with the plot of all other being +1.34 ± 0.18. The sun has V–R = +0.37. In other words, nights. These adjustments were necessary because some the asteroid reflects less sunlight in V than R or I. If, for example, observations were not made with a V-filter. The thick trace in the the asteroid's albedo at 650 nm (R-filter) were ~15%, at 530 nm figure is a hand drawn fit that allows for slight departures from a (V-filter) it would be 6 ± 1% according to the measurements sinusoidal variation. This non-sinusoidal “hand fit” trace has a reported here. With a B filter the asteroid was undetectable, and magnitude range of 0.50 ± 0.05 magnitude. its B-magnitude was fainter than 18.2. This implies that it has an even lower albedo in B than for V. A spectrum with this shape is The two minima are compatible with the “rotating potato” typical for meteorites as well as most asteroids. The average V- lightcurve shape in which the minima are slightly “sharper” than filter brightness was consistently 0.3 magnitudes fainter than the maxima. The simplest shape that is compatible with this predicted by the JPL Ephemeris, which uses H = 12.5. Thus an lightcurve shape is an oblong spheroid with a major axis to minor improved H value of 12.8 is determined. axis length ratio of ~1.64. Lightcurves from future oppositions can be used to further model the shape. It is unlikely that the 2003 The longest observing session was 7.1 hours, and it clearly minimum brightness corresponded to the asteroid being viewed showed more than a full period of a quasi-sinusoidal variation of with its minimum possible solid angle. Hence, the length-to-width brightness, consistent with a rotation period of ~13 hours. This is ratio of 1.64 should be considered a lower limit estimate. one of the worst situations for an observer to deal with since lightcurves for closely-spaced dates will have a similar shape, and Additional details on this observing project can be found at systematic errors related to extinction, for example, could produce http://brucegary.net/POVENMIRE/ repeating brightness variation artifacts. A strategy was employed of varying the interval between observing dates in order to sample Acknowledgments the lightcurve at a variety of phases with respect to transit. I want to thank Hal Povenmire for suggesting I observe this On some dates the asteroid passed close to stars of comparable asteroid when I “spread the word” that I was looking for a brightness. Since the asteroid’s path during a typical 4.5-hour challenging asteroid project. Hal also provided ample observing session was ~2.3' arc, and my point-spread function had encouragement throughout the observing period. During this a FWHM of ~3" arc, it was possible to perform background observing project I read “the book” on asteroid lightcurves by subtraction by carefully positioning the signal aperture at the Brian Warner (2003), which saved me from many pitfalls awaiting location where the asteroid had been after it had moved away from the novice asteroid observer. the interfering star and noting the apparent “intensity” for that location. This intensity was subtracted from the intensity References measured when the asteroid was at that location, and the difference intensity was converted to a magnitude. The concept is Warner, Brian, 2003, A Practical Guide to Lightcurve Photometry straightforward, but implementing it is tedious. Also for each and Analysis, BDW Publishing, Colorado Springs, CO. observing session one or more “check stars” were measured and plotted versus time. In every case the check star was constant, or varied with a linear drift by an amount that was small (<0.1 magnitude) compared with the asteroid’s variation (0.5 magnitude).

A rotation period search was conducted using a program written in QuickBASIC specifically for this task. The program allowed the user to specify an initial period and increment, and for each candidate period a least squares fit was obtained assuming a sinusoidal variation with a fitted phase and amplitude. The sinusoidal shape appeared to be a good first-order assumption based on individual observing sessions. Because observations spanned 3 months period change increments had to be as small as 0.0005 hours in order to avoid “missing” the RMS residual global minimum. Within this analysis, allowance was not made for the changing Earth-asteroid viewing angle. This neglect was judged acceptable given that this angle changed by only 11 degrees during the 3-month observing period (owing to the 2.05 to 2.33 a.u. distance to the asteroid).

The best solution from the “brute force” parameter search program is period = 12.854 ± 0.001 hours, phase for the sinusoidal component = 2003 October 4.550 UT, and sinusoidal amplitude Figure 1. Lightcurve for 12753 Povenmire assembled from 9 (1/2 of peak-to-peak) = 0.227 magnitudes. The RMS residual for observing dates using the QuickBASIC program’s least squares this solution is 0.119 magnitude. A Bayesian analysis rules out solution for rotation period (12.854 hours).

Minor Planet Bulletin 31 (2004) 58

LIGHTCURVE PHOTOMETRY OF ASTEROIDS minutes each. Images were taken at 2.5-minute intervals. A total 306, 1508, 3223, 3270 AND 3712 of 369 observations were used in the solution.

Robert A. Koff Figure 1 shows the resulting lightcurve. The zero point of the 980 Antelope Drive West curve is J.D. 2452708.70506. The synodic period was determined Bennett, CO 80102 to be 8.736 hours with a formal error of ± 0.001 hours. The [email protected] amplitude was 0.34 ± 0.02 magnitude.

(Received: 10 April)

Asteroid photometry measurements in 2003 and early 2004 from Antelope Hills Observatory yield the following lightcurve period and amplitude results: 306 Unitas 8.736±0.001 hr and 0.34±0.02 m, 1508 Kemi 9.196±0.001 hr and 0.34±0.02 m, 3223 Forsius 2.343±0.001 hr and 0.26±0.02 m, 3270 Dudley 4.047±0.001 hr and 0.40±0.03 m, 3712 Kraft 9.341±0.001 hr and 1.20±0.03 m.

Equipment and Procedure

In 2002, Antelope Hills Observatory was established as a replacement for Thornton Observatory, MPC code 713. The new observatory, MPC code H09, is located near Bennett, Colorado at an elevation of 1740 meters. The equipment and instrumentation of Antelope Hills Observatory have been detailed in a previous paper (Koff, 2004). Figure 1. Lightcurve of 306 Unitas, based on a period of 8.736 Targets were selected from the “Potential Lightcurve Targets” on hours. Ordinate is relative magnitude the CALL website (Warner, 2002), and further refined based on their magnitude and position in the sky. Targets were selected for (1508) Kemi which no lightcurve data had been previously reported. (Harris, 2003). Targets were further refined to include Mars-crossing Kemi, a nearly Mars-crossing asteroid, was discovered October 21, asteroids, including those with reported but uncertain periods. In 1938 by H. Alikoski at Turku. It is approximately 26 km in addition, asteroid 306 Unitas was included to obtain data for shape diameter. The perihelion is 1.61 AU, and the aphelion is 3.92 AU. modeling purposes. Period determinations have been previously reported for this object. According to the report by Harris (2003), Holliday in 1995 The images were obtained in unfiltered light. All images were reported a period of 11.36 hours, while Sarneczky in 1999 reported calibrated with dark frames and flat field frames. The differential a period of 9.15 hours. Dr. Harris lists the period of this object at photometry was measured using the program “Canopus” by Brian 9.15, but with an uncertainty value of 2. Observations were Warner, which uses aperture photometry. Magnitudes were calculated using reference stars from the USNO A–2.0 catalog. Comparison stars differed from night-to-night due to movement of the asteroid. Lightcurves were prepared using “Canopus”, based on the method developed by Dr. Alan Harris (Harris et al, 1989). This program allows compensation for night-to-night comparison star variation by manually shifting individual night's magnitude scales to obtain a best fit.

Observations and Results

(306) Unitas

Unitas is a main-belt asteroid, and was discovered March 1, 1891, by E. Millosevich at Rome. It is an S-class asteroid, of approximately 49 km diameter. This object was previously observed by H. Childers at the University of Iowa in November, 2001 (CALL, 2004). At that time, a period of 8.74 hours ± 0.02 hours was determined. Observations were undertaken at Antelope Hills in 2003 to help in the effort to model this object. Observations were made on three nights during the period from March 9, 2003 to April 1, 2003. During the period of the investigation, the phase angle increased from 13.24 degrees to 19.29 degrees. Exposure times for this investigation were two Figure 2. Lightcurve of 1508 Kemi, based on a period of 9.196 hours. Ordinate is relative magnitude Minor Planet Bulletin 31 (2004) 59 undertaken to resolve the period. Images were taken at 2.5-minute intervals. A total of 488 observations were used in the solution. Observations were made on three nights during the period from February 18, 2004 to March 29, 2004. During the period of the Figure 4 shows the resulting lightcurve. The zero point of the investigation, the phase angle dropped from 22.8 degrees to 21.0 curve is J.D. 2453042.63917. The synodic period was determined degrees, then increased to 21.64 degrees. Exposure times for this to be 4.047 hours with a formal error of ± 0.001 hours. The investigation were two minutes each. Images were taken at 2.5- maximum amplitude was 0.40 ± 0.03 magnitude. The amplitude minute intervals. A total of 508 observations were used in the dropped steadily during the period of the investigation to a solution. Figure 2 shows the resulting lightcurve. The zero point minimum of 0.26 ± 0.02 magnitude. Efforts to obtain further of the curve is J.D. 2453053.89037. The synodic period was observations failed due to weather and the dimming of the object. determined to be 9.196 hours with a formal error of ± 0.001 hours. The maximum amplitude was measured at 0.34 ± 0.02 magnitude.

(3223) Forsius

Forsius, a main-belt asteroid, was discovered September 7, 1942 by Y. Vaisala at Turku. It is approximately 24 km in diameter. No lightcurve data are previously reported for this object (Harris, 2003). Observations were made on four nights from January 30, 2003 to February 11, 2003. During the interval of the investigation, the phase angle dropped from 13.0 degrees to 7.4 degrees. Exposure times for this investigation were two minutes each. Images were taken at 2.5-minute intervals. A total of 288 observations were used in the solution.

Figure 3 shows the resulting lightcurve. The zero point of the curve is J.D. 2452681.82830. The synodic period was determined to be 2.343 hours with a formal error of ± 0.001 hours. The amplitude was 0.26±0.02 mag. The mean measured magnitude was 13.8, which should be considered an instrumental magnitude.

Figure 4. Lightcurve of 3270 Dudley, based on a period of 4.047 hours. Ordinate is relative magnitude

(3712) Kraft

Kraft, a main-belt asteroid, was discovered December 22, 1984 by E. A. Harlan and A. R. Klemola at Mount Hamilton. It is approximately 31 km in diameter. No lightcurve data are previously reported for this object (Harris, 2003). Observations were made on 4 nights from November 30, 2002 to January 21,

Figure 3. Lightcurve of 3223 Forsius, based on a period of 2.343 hours. Ordinate is relative magnitude

(3270) Dudley

Dudley is a Mars-crossing asteroid, discovered February 18, 1982 by C. Shoemaker and S. Bus at Palomar. It is approximately eight km in diameter. The perihelion is 1.44 AU and the aphelion is 2.86 AU. No lightcurve data are previously reported for this object (Harris, 2003). Observations were made on four nights from February 7-26, 2004. During the period of the investigation, the phase angle increased from 12.18 degrees to 19.00 degrees. Exposure times for this investigation were two minutes each. Figure 5. Lightcurve of 3712 Kraft, based on a period of 9.341 hours. Ordinate is relative magnitude.

Minor Planet Bulletin 31 (2004) 60

2003, during which the phase angle dropped from 20.61 degrees to References a minimum of 0.65 degrees at opposition on January 7.9, 2003, and then increased to 8.74 degrees. Exposure times were two minutes Harris, A. W., Young, J. W., Bowell, E., Martin, L. J., Millis, R. each. Images were taken at 2.5-minute intervals. A total of 556 L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J., observations were used in the solution. Debehogne, H., and Zeigler, K. W. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, Figure 5 shows the resulting lightcurve. The zero point of the 171-186. curve is J.D. 2542614.98095. The synodic period was determined to be 9.341 hours with a formal error of ± 0.001 hours. The Harris, A. W. (2003). “Minor Planet Lightcurve Parameters”, On amplitude was 1.20 ± 0.03 magnitude. The mean measured the Minor Planet Center website: http://cfa-www.harvard magnitude was 14.7, which should be considered an instrumental .edu/iau/lists/LightcurveDat.html, or on the CALL website: magnitude. http://www.MinorPlanetObserver.com/astlc/default.htm

Acknowledgments Koff, R. A. (2004). “Lightcurve Photometry of Mars-Crossing Asteroids 1474 Beira and 3674 Erbisbuhl”. The Minor Planet Many thanks to Brian Warner for his continuing work on the Bulletin 31, 33-34. CALL website and the program “Canopus”, which has made it possible for amateurs to analyze and share lightcurve data. Warner, B. D. (2002), “Potential Lightcurve Targets”, on the CALL website, http://www.MinorPlanetObserver.com/astlc/ default.htm

PHOTOMETRY OF 966 MUSCHI, 1567 ALIKOSKI, Results AND 2331 PARVULESCO 966 Muschi Robert D. Stephens 11355 Mount Johnson Court Discovered November 9, 1921 by W. Badde at Bergedorf, Muschi Rancho Cucamonga, CA 91737 USA is a main-belt asteroid with an estimated radius of 12 km. Muschi [email protected] is the nickname of the wife of the discoverer. Five hundred four observations over three sessions between March 4 and 19, 2004 (Received: 30 March Revised: 3 April) were used to derive the synodic rotational period of 5.355 ± 0.01 hours with an amplitude of 0.31 ± 0.04 magnitude. Table I gives the phase angles during the observing run. Results for the following asteroids (lightcurve period and amplitude) observed from Santana Observatory during the period January to March 2004 are reported: 966 Muschi (5.355 ± 0.01 hours and 0.31 mag.), 1567 Alikoski (16.405 ± 0.01 hours and 0.16 mag.), 2331 Parvulesco (32.03 ± 0.02 hours and 0.50 mag.

Santana Observatory (MPC Code 646) is located in Rancho Cucamonga, California at an elevation of 400 meters and is operated by Robert D. Stephens. Temporarily, a 0.35 meter SCT operating at F/11 with an SBIG ST1001E CCD camera was used for these observations. This telescope is on a Paramount ME jointly owned with Glenn Malcolm and is being tested before delivery to a new observatory at a remote location. Further details can be obtained at the author’s web site.

Aperture photometry was done using the software program “Canopus” developed by Brian Warner and including the Fourier analysis routine developed by Alan Harris (Harris et al, 1989). Figure 1: Lightcurve of 966 Muschi based upon a derived period This program allows combining data from different observers and of 5.355 ± 0.01 hours. Zero phase is equal to 2453081.850860 JD adjusting the zero points to compensate for different equipment (corrected for light-time). and comparison stars. It also adjusts for light-time differences between observations. All observations were unfiltered. Dark Table I: Observing circumstances for 966 Muschi frames and flat fields were used to calibrate the images. Further information on the methods and capabilities of “Canopus” can be Phase PAB PAB Number Date found in Warner (2003) Angle (Long.) (Lat.) Observations 2004/3/18 8.7 181.8 17.9 186 All of the asteroids were selected from the “CALL” web site “List of Potential Lightcurve Targets” (Warner 2004). 2004/3/18 8.6 181.9 17.9 165 2004/3/19 8.5 181.9 17.9 153

Minor Planet Bulletin 31 (2004) 61 1567 Alikoski 2331 Parvulesco

Alikoski is a main-belt asteroid discovered April 22, 1941 by Y. Discovered March 12, 1936 by E. Delporte at Uccle, Parvulesco is Väisälä at Turku. It has an estimated radius of 34 km and is a member of the Nysas family. It is named for in memory of the named in honor of Heikki A. Alikoski, assistant to the discoverer Romanian professor Constantin Parvvulesco (1890-1945). It also from 1937 to 1956 and observer and discoverer of minor planets. honors his daughter, Carina Parbulesco who, as a professor of Seven hundred thirty nine observations over four sessions between astronomy at San Mateo College, California, has made March 12 and 16, 2004 were used to derive the synodic rotational contributions in stellar and galactic dynamics. Six hundred ninety period of 16.405 ± 0.01 hours with an amplitude of 0.16 ± 0.02 seven observations over nine sessions between January 29 and magnitude. Table II gives the phase angles during the observing February 13, 2004 were used to derive the synodic rotational run. period of 32.03 ± 0.02 hours with an amplitude of 0.50 ± 0.04 magnitude. Table III gives the phase angles during the observing run.

Table III: Observing circumstances for 2331 Parulesco

Phase PAB PAB Number Date Angle (Long.) (Lat.) Observations 2004/1/29 5.3 134.5 -4.8 69 2004/1/30 4.9 134.6 -4.8 92 2004/2/01 4.1 134.8 -4.8 56 2004/2/02 3.8 134.9 -4.9 82 2004/2/08 4.1 135.4 -5.0 56 2004/2/09 4.5 135.5 -5.0 116 2004/2/11 5.4 135.7 -5.0 49 2004/2/12 5.9 135.8 -5.0 102

Figure 2: Lightcurve of 1567 Alikoski based upon a derived 2004/2/13 6.5 135.9 -5.1 75 period of 16.405 ± 0.01 hours. Zero phase is equal to 2453080.680183 JD (corrected for light-time). Acknowledgements Table II: Observing circumstances for 1567 Alikoski Many thanks to Brian Warner for his continuing work and Phase PAB PAB Number enhancements to the software program “Canopus” which makes it Date Angle (Long.) (Lat.) Observations possible for amateur astronomers to analyze and collaborate on 2004/3/12 7.4 177.9 17.8 147 asteroid rotational period projects and for maintaining the CALL Web site which helps coordinate collaborative projects between 2004/3/14 7.2 177.9 17.7 157 amateur astronomers. 2004/3/15 7.1 177.9 17.7 215 References 2004/3/16 7.1 177.9 17.7 220 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, 40, 60, 261, and 863.” Icarus 77, p. 171-186.

Schmadel, L. D. (1999) “Dictionary of Minor Planet Names, 4th Edition.” Springer.

Stephens, R. D. (2004). http://home.earthlink.net/~rdstephens/ default.htm.

Warner, B. (2003). “Lightcurve Analysis for Asteroids 436 Patricia, 3155 Lee, 4254 Kamel, 5940 Feliksobolev, (16558) 1991 VQ2, and (45656) 2000 EE45.” Minor Planet Bulletin 30, 21-24.

Warner, B. (2004). “Potential Lightcurve Targets”. http://www.minorplanetobserver.com/astlc.targets. Figure 3: Lightcurve of 2331 Parvulesco based upon a derived period of 32.03 ± 0.02 hours. Zero phase is equal to 2453034.986312 JD (corrected for light-time).

Minor Planet Bulletin 31 (2004) 62

GENERAL REPORT OF POSITION OBSERVATIONS OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES BY THE ALPO MINOR PLANETS SECTION FOR THE YEAR 2003 13 Egeria Bookamer, 41 Nov 13 2 18 Melpomene Bookamer, 41 Feb 10 3 Frederick Pilcher 41 Daphne Arlia, 15 Feb 6-22 9P Illinois College Jacksonville, IL 62650 USA 61 Danaë Bookamer, 41 May 2 3 65 Cybele Faure, 20 Nov 11-12 7C (Received: 23 April) 78 Diana Bookamer, 41 Mar 20 3

85 Io Hudgens, 35 Sep 21 2

Observations of positions of minor planets by members 93 Minerva Watson, 20 Apr 25-May 5 3 of the Minor Planets Section in calendar year 2003 are summarized. 99 Dike Garrett, 32 Jun 3-7 3 117 Lomia Garrett, 32 Mar 17 2

131 Vala Hudgens, 35 Oct 17-19 4 During the year 2003 a total of 1404 positions of 366 different minor planets were reported by members of the Minor Planets 142 Polana Bookamer, 41 Feb 5 4 Section. Of these 46 are CCD images (denoted C) and 65 are 156 Xanthippe Bookamer, 41 Jan 31 4 precise photographic measurements (denoted P). All the rest are Garrett, 32 Feb 25 2 approximate visual positions. All of the numbered minor planets 163 Erigone Watson, 20 Feb 21-27 2 were observed at positions agreeing within errors of measurement 191 Kolga Bookamer, 41 Feb 24 3 with those predicted from their published ephemerides. 192 Nausikaa Arlia, 15 May 27-Jun 8 9P The summary lists minor planets in numerical order, the observer 219 Thusnelda Hudgens, 35 Nov 20 2 and telescope aperture (in cm), UT dates of the observations, and 227 Philosophia Bookamer, 41 Feb 11 4 the total number of observations in that period. The year is 2003 228 Agathe Hudgens, 35 Oct 15 2 in each case. 245 Vera Bookamer, 41 Nov 11 4

247 Eukrate Garrett, 32 May 20 2

273 Atropos Bookamer, 41 Mar 4 3 Positional observations were contributed by the following 275 Sapientia Garrett, 32 Mar 24-25 2 observers: 279 Thule Hudgens, 35 Oct 15-16 2

Observer, Instrument Location Planets 286 Iclea Garrett, 32 Aug 24 2 Positions 295 Theresia Bookamer, 41 Dec 15 4

Arlia, Saverio Buenos Aires 5 65P 299 Thora Hudgens, 25 Jun 7-20 3 15 cm f/6 reflector Argentina 306 Unitas Garrett, 32 Mar 24-25 2 Bookamer, Richard E. Micco, Florida 39 148 41 cm reflector, USA 312 Pierretta Hudgens, 35 Nov 20 2 314 Rosalia Bookamer, 41 Oct 30 4 Faure, Gerard Col de L'Arzelier, 97 263 (38C) 20 cm Celestron, France 321 Florentina Garrett, 32 Aug 23 2

Faure, Gerard, and Rayon, Col de L'Arzelier, 2 5 330 Adalberta Faure, 20 Feb 21 2 Jean-Michel, 20 cm France Celestron, 35 cm 340 Eduarda Bookamer, 41 Jan 31 4 Garrett, 32 Feb 20 2 reflector 342 Endymion Hudgens, 35 Oct 19 2 Garrett, Lawrence Fairfax, Vermont, 35 75 32 cm f/6 reflector USA 347 Pariana Bookamer, 41 Feb 12 3

Harvey, G. Roger Concord, North 110 376 350 Ornamenta Bookamer, 41 Feb 2 3 74 cm Newtonian Carolina, USA 360 Carlova Garrett, 32 Jun 7 2

Hudgens, Ben Stephenville, 144 453 366 Vincentina Bookamer, 41 Feb 25 3 25 cm Dobsonian Texas, USA Garrett, 32 Feb 25 2 33 cm Dobsonian 35 cm Dobsonian 377 Campania Hudgens, 25 Aug 29 2 383 Janina Faure, 20 Oct 21 2 Jardine, Don, and Pleasant Plains, 3 12 (8C) Pilcher, Frederick Illinois, USA 387 Aquitania Bookamer, 41 Feb 20 2 25 cm Cassegrain + CCD 35 cm Cassegrain 394 Arduina Hudgens, 25 May 28 2 405 Thia Faure, 20 Aug 1 10C Watson, William W. Tonawanda, NY USA 3 7 20 cm Celestron 411 Xanthe Bookamer, 41 May 2 4

416 Vaticana Bookamer, 41 May 2 3

417 Suevia Bookamer, 41 Feb 20 3

426 Hippo Watson, 20 Feb 21-27 2

442 Eichsfeldia Bookamer, 41 Feb 19 3

Minor Planet Bulletin 31 (2004) 63

OBSERVER & OBSERVING NO. OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES

446 Aeternitas Garrett, 32 Feb 25 2 868 Lova Garrett, 32 Aug 28 2 Hudgens, 25 Aug 29 2 449 Hamburga Bookamer, 41 May 24 3 871 Amneris Bookamer, 41 Mar 28 3 450 Brigitta Hudgens, 25 Aug 29 2 Hudgens, 35 Apr 5 2

483 Seppina Bookamer, 41 Feb 26 3 875 Nymphe Hudgens, 25 Jun 20 2

494 Virtus Garrett, 32 Feb 20 2 890 Waltraut Faure, 20 May 30 2

515 Athalia Faure, 20 Nov 19 4 903 Nealley Hudgens, 25 Mar 8-9 2 Garrett, 32 Nov 23 2 Hudgens, 35 Nov 20 2 921 Jovita Faure, 20 May 23-31 7 Garrett, 32 Jun 7 2 516 Amherstia Arlia, 15 Jun 22-31 24P Hudgens, 25 May 28 2

517 Edith Hudgens, 35 Sep 21 2 922 Schlutia Faure, 20 Nov 18 2 Hudgens, 35 Oct 17-19 4 522 Helga Hudgens, 25 May 28 2 937 Bethgea Hudgens, 25 Jun 7 2 526 Jena Bookamer, 41 Feb 20 3 957 Camelia Bookamer, 41 Mar 6 3 532 Herculina Hudgens, 35 Oct 22-23 2 970 Primula Faure, 20 Nov 19 2 557 Violetta Hudgens, 35 Dec 20 2 Hudgens, 35 Nov 20 2

574 Reginhild Hudgens, 35 Sep 22-27 2 973 Aralia Bookamer, 41 Mar 24 3

576 Emanuela Garrett, 32 Aug 24 2 992 Swasey Faure, 20 Feb 22 3

584 Semiramis Arlia, 15 Sep 10-24 18P 995 Sternberga Hudgens, 25 May 28 2

593 Titania Bookamer, 41 Feb 11 4 1007 Pawlowia Hudgens, 35 Sep 27 2

595 Polyxena Garrett, 20 May 20 2 1010 Marlene Faure, 20 Oct 21 2

614 Pia Hudgens, 35 Sep 27 2 1033 Simona Hudgens, 35 Dec 24 2

630 Euphemia Hudgens, 35 Nov 20 2 1041 Asta Hudgens, 35 Oct 20 2

641 Agnes Hudgens, 35 Oct 1-15 3 1046 Edwin Faure, 20 Feb 8 2

646 Kastalia Faure, 20 Nov 19 2 1048 Feodosia Bookamer, 41 Apr 2 4 Garrett, 20 May 20 2 650 Amalasuntha Faure, 20 Aug 26-27 2 1057 Tynka Hudgens, 35 Oct 16-17 2 653 Berenike Bookamer, 41 Feb 21 3 1062 Ljuba Hudgens, 35 Oct 15 2 663 Gerlinde Bookamer, 41 Feb 12 5 1086 Nata Bookamer, 41 Mar 5 3 683 Lanzia Garrett, 32 Aug 29 2 1087 Arabis Bookamer, 41 Mar 10 4 684 Hildburg Hudgens, 25 Apr 5 2 1101 Clematis Faure, 20 Jun 29 2 707 Steïna Hudgens, 35 Oct 15 2 1132 Hollandia Faure, 20 May 23-30 3 708 Raphaela Bookamer, 41 Mar 24 3 1136 Mercedes Hudgens, 35 Dec 14-18 2 739 Mandeville Bookamer, 41 Feb 5 3 1149 Volga Faure, 20 Aug 26 2 746 Marlu Faure, 20 Jul 30 2 Hudgens, 35 Oct 15 2 1157 Arabia Faure, 20 Jul 29 2 Garrett, 32 Aug 23 2 774 Armor Garrett, 32 Nov 16 2 Hudgens, 25 Aug 18-19 2 Hudgens, 35 Oct 24 2 1160 Illyria Faure, 20 Nov 19 2 775 Lumière Hudgens, 33 Feb 10-11 2 Hudgens, 35 Nov 20 2

779 Nina Arlia, 15 Sep 3-18 5P 1165 Imprinetta Faure, 20 Sep 19-20 2

794 Irenaea Garrett, 32 Aug 24 2 1166 Sakuntala Faure, 20 Jul 18-19 4

801 Helwerthia Faure, 20 Feb 22 2 1179 Mally Harvey, 73 Mar 31 3

808 Merxia Bookamer, 41 Feb 10 4 1180 Rita Hudgens, 25 May 28 2

811 Nauheima Hudgens, 25 Jun 7 2 1225 Ariane Faure, 20 Feb 21-22 2

825 Tanina Hudgens, 25 Jul 29-30 2 1226 Golia Hudgens, 25 Dec 24 2

837 Schwarzschilda Garrett, 32 Aug 24 2 1232 Cortusa Faure, 20 May 30 2 Hudgens, 25 Aug 29 2 1243 Pamela Hudgens, 25 May 28 2 842 Kerstin Faure, 20 Nov 19 2 Hudgens, 35 Nov 27-29 2 1270 Datura Hudgens, 35 Sep 27 2

847 Agnia Garrett, 32 Aug 24 2 1271 Isergina Hudgens, 35 Oct 23 2

852 Wladilena Bookamer, 41 Mar 28 3 1280 Baillauda Hudgens, 35 Oct 24 2

855 Newcombia Faure, 20 May 23 2 1298 Nocturna Faure, 20 Jul 29 2

861 Aïda Garrett, 32 Aug 23 2 1299 Mertona Hudgens, 35 Nov 20 2

863 Benkoela Bookamer, 41 Feb 25 3 1314 Paula Hudgens, 35 Dec 24 2

864 Aase Faure, 20 Aug 27 2 1385 Gelria Faure, 20 Jun 21-Jul 18 4 Hudgens, 35 Sep 27 2

Minor Planet Bulletin 31 (2004) 64

OBSERVER & OBSERVING NO. OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES

1387 Kama Faure, 20 Nov 18 2 1903 Adzhimushkaj Faure, 20 May 29 2 Hudgens, 35 Oct 19 2 1930 Lucifer Faure, 20 Sep 19 2 1396 Outeniqua Faure, 20 May 29-30 2 Hudgens, 25 Sep 3 2 Hudgens, 25 Apr 5 2 1935 Lucerna Hudgens, 35 Oct 23 2 1398 Donnera Faure, 20 Jul 28-29 2 1952 Hesburgh Hudgens, 35 Nov 20 2 1403 Idelsonia Faure, 20 Jun 30 2 1958 Chandra Hudgens, 35 Sep 27 3 1409 Isko Hudgens, 25 Mar 8-9 3 1982 Cline Faure, 20 Oct 21 2 1410 Margret Hudgens, 35 Oct 24 3 Hudgens, 35 Oct 17-24 5

1416 Renauxa Hudgnes, 35 Oct 16-17 2 2014 Vasilevskis Hudgens, 25 Jul 18-22 3

1432 Ethiopia Faure, 20 Jun 21-22 2 2021 Poincaré Faure, 20 Oct 21 2

1436 Salonta Hudgens, 35 Dec 24 2 2036 Sheragul Faure, 20 Jul 29 2 Hudgens, 25 Aug 18-19 2 1461 Jean-Jacques Hudgens, 35 Dec 20-21 2 2054 Gawain Harvey, 73 Jan 11 3 1474 Beira Hudgens, 35 Sep 27-Oct 1 2 2064 Thomsen Faure and Rayon, 20 Jul 6 3 1494 Savo Hudgens, 35 Nov 20 2 Garrett, 32 Aug 24 2 Hudgens, 25 Aug 18-19 2 1499 Pori Faure, 20 Jul 28-29 2 Hudgens, 25 Jul 29-30 2 2074 Shoemaker Harvey, 73 Oct 3 3 Hudgens, 35 Oct 19 2 1501 Baade Faure, 20 Oct 21 2 2078 Nanking Hudgens, 25 Sep 3 2 1503 Kuopio Hudgens, 33 Feb 10-11 2 2094 Magnitka Faure, 20 May 30 2 1507 Vaasa Faure, 20 Sep 19 2 Garrett, 32 Aug 29 2 2134 Dennispalm Hudgens, 25 Mar 24 2 Hudgens, 25 Aug 28-29 2 2141 Simferopol Hudgens, 35 Oct 24 2 1514 Ricouxa Hudgens, 25 Jun 20 2 2159 Kukkamäki Faure, 20 Aug 26-27 2 1520 Imatra Garrett, 32 Aug 29 2 Hudgens, 25 Sep 3 2 2167 Erin Hudgens, 25 Mar 8-9 2

1523 Pieksämäki Jardine, Pilcher, 25 Apr 2 4C 2171 Kiev Harvey, 73 Apr 24 3

1544 Vinterhansenia Hudgens, 35 Oct 16-17 2 2180 Marjaleena Hudgens, 35 Oct 24 2

1555 Dejan Garrett, 32 Nov 23 2 2216 Kerch Faure, 20 Jul 29 2 Hudgens, 35 Nov 20 2 2235 Vittore Faure, 20 Nov 19 2 1560 Strattonia Faure, 20 Jul 28-29 2 2262 Mitidika Hudgens, 25 Sep 3 2 1564 Srbija Hudgens, 35 Oct 15 2 2271 Kiso Faure, 20 Aug 26 2 1590 Tsiolkovskaja Hudgens, 25 Jul 18-22 4 Hudgens, 25 Aug 29 2

1594 Danjon Faure, 20 Jun 21 2 2316 Jo-Ann Hudgens, 25 Apr 18-19 2 Hudgens, 25 Jun 7 2 2358 Bahner Hudgens, 35 Oct 24 2 1595 Tanga Hudgens, 25 Jun 7 2 2448 Sholokhov Hudgens, 33 Feb 10-11 2 1596 Itzigsohn Faure, 20 Nov 19 2 2502 Nummela Harvey, 73 Jan 6 3 1603 Neva Faure, 20 Jul 29-30 2 2525 O'Steen Faure, 20 Oct 21 3 1606 Jekhovsky Faure, 20 Sep 19 2 Garrett, 32 Aug 24 2 2543 Machado Faure, 20 Nov 19 2 Hudgens, 25 Aug 29 2 Harvey, 73 Oct 30 3

1615 Bardwell Faure, 20 Nov 18 2 2580 Smilevskia Hudgens, 35 Oct 18 2 Hudgens, 35 Oct 18 2 2617 Jiangxi Faure, 20 Nov 19 2 1622 Chacornac Hudgens, 35 Sep 27-Oct 1 2 2675 Tolkien Hudgens, 35 Oct 23 2 1625 The NORC Faure, 20 May 23-30 2 Hudgens, 25 Mar 24 2 2697 Albina Faure, 20 Nov 19 2 Hudgens, 35 Oct 24 2 1635 Bohrmann Hudgens, 35 Sep 27-Oct 1 3 2741 Valdivia Faure, 20 May 30 2 1640 Nemo Faure, 20 Nov 18 2 2791 Paradise Faure, 20 Feb 23 3 1646 Rosseland Hudgens, 35 Dec 20 2 Hudgens, 33 Feb 10-11 2

1675 Simonida Faure, 20 Nov 19 2 2795 Lepage Harvey, 73 Nov 1 3

1699 Honkasalo Faure, 20 May 30 2 2803 Vilho Harvey, 73 Jan 6 3

1732 Heike Hudgens, 35 Oct 24 2 2831 Stevin Hudgens, 25 Sep 3 3

1742 Schaifers Hudgens, 35 Oct 23 2 2931 Mayakovsky Harvey, 73 Nov 1 3

1746 Brouwer Hudgens, 35 Oct 18 2 2938 Hopi Harvey, 73 Nov 23 3

1793 Zoya Hudgens, 35 Dec 24 2 2950 Rousseau Harvey, 73 Jan 11 3

1799 Koussevitzky Hudgens, 35 Oct 19-23 3 2997 Cabrera Harvey, 73 Oct 3 3

1803 Zwicky Faure, 20 Feb 21-22 3 3019 Kulin Harvey, 73 Jan 2 3

1824 Haworth Hudgens, 35 Oct 23 2 3041 Webb Harvey, 73 Dec 21 3 Minor Planet Bulletin 31 (2004) 65

OBSERVER & OBSERVING NO. OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES

3106 Morabito Faure, 20 Feb 22 2 5378 Ellyett Harvey, 73 Dec 1 3

3178 Yoshitsune Faure, 20 Feb 21 2 5381 Sekhmet Harvey, 73 May 13 6

3223 Forsius Faure, 20 Feb 22 2 5394 Jurgens Harvey, 73 Dec 28 3 Hudgens, 25 Mar 8-9 2 5426 Sharp Harvey, 73 Dec 28 3 3401 Vanphilos Faure, 20 Sep 19-20 3 5522 De Rop Harvey, 73 Dec 21 3 3507 Vilas Hudgens, 25 Jun 20 2 5606 Muramatsu Harvey, 73 Mar 11 3 3509 Sanshui Harvey, 73 Oct 23 3 Hudgens, 35 Oct 23 2 5625 1991 AO2 Harvey, 73 Dec 1 3

3544 Borodino Faure, 20 Jul 28-29 2 5630 Billschaefer Harvey, 73 Mar 11 3 Garrett, 32 Aug 24 2 Hudgens, 25 Jul 30 2 5681 Bakulev Harvey, 73 Sep 20 3

3577 Putilin Harvey, 73 Jan 6-11 3 5827 Letunov Harvey, 73 Dec 1 3

3589 Loyola Harvey, 73 Dec 28 3 5892 1981 YS1 Harvey, 73 Oct 30 3 Hudgens, 35 Nov 20 2 3590 Holst Harvey, 73 Dec 28 3 6023 Tsuyashima Harvey, 73 Dec 1 3 3628 Boˇznˇemcová Hudgens, 35 Oct 17-18 2 6091 1991 RO6 Harvey, 73 Dec 28 3 3674 Erbisbühl Hudgens, 35 Dec 24 2 6244 Okamoto Faure, 20 Nov 19 2 3700 Geowilliams Hudgens, 35 Dec 20-21 2 Harvey, 73 Nov 1 3

3712 Kraft Jardine, Pilcher, 25 Jan 7 4C 6354 Vangelis Faure, 20 Feb 22 2

3738 Ots Faure, 20 May 29-30 2 6386 1989 NK1 Harvey, 73 Sep 20 3 Hudgens, 35 Oct 22-23 2 3767 DiMaggio Faure, 20 Jul 18 3 6406 1992 MJ Harvey, 73 Nov 1 3 3811 Karma Hudgens, 35 Dec 24 3 6418 Hanamigahara Harvey, 73 Nov 1 3 3855 Pasasymphonia Hudgens, 35 Oct 17 2 6475 Refugium Faure, 20 Jul 29 2 3929 Carmelmaria Harvey, 73 Nov 1 3 6572 Carson Harvey, 73 Oct 30 3 3936 Elst Faure, 20 Jul 29-Aug 2 14,12C 6649 Yokotatakao Hudgens, 25 Aug 28-29 2 3953 Perth Harvey, 73 Oct 23 3 6808 Plantin Harvey, 73 Mar 25 3 3974 Verveer Hudgens, 25 Apr 5 2 6821 Ranevskaja Faure, 20 Nov 18 2 3990 Heimdal Hudgens, 25 Oct 19 2 6905 Miyazaki Harvey, 73 Dec 21 3 3997 Taga Harvey, 73 Dec 16 3 6926 1994 RO11 Harvey, 73 Nov 1 3 4092 Tyr Harvey, 73 Sep 20 3 6955 Ekaterina Faure, 20 Aug 26-27 2 4159 Freeman Faure, 20 Nov 19 2 7186 Tomioka Harvey, 73 Jan 11 3 4209 Briggs Harvey, 73 Sep 20 3 7234 1986 QV3 Hudgens, 35 Oct 21-23 2 4289 Biwako Hudgens, 35 Dec 14-18 2 7288 1991 FE1 Harvey, 73 Dec 1 3 4297 Eichhorn Hudgens, 25 Aug 29 2 7369 Gavrilin Faure, 20 Nov 18 4 4331 Hubbard Harvey, 73 Apr 23 3 Harvey, 73 Oct 30 3

4381 Uenohara Harvey, 73 Jun 1 3 7554 Johnspencer Harvey, 73 Apr 1 3

4477 1983 SB Harvey, 73 Nov 1 3 7631 Vokrouhlicky´ Harvey, 73 Nov 30-Dec 1 3

4481 Herbelin Harvey, 73 Oct 23 3 7680 Cari Harvey, 73 Nov 1 3

4508 Takatsuki Harvey, 73 Apr 25 3 7829 Jaroff Harvey, 73 Dec 28 3

4513 Louvre Harvey, 73 Oct 30 3 7887 1993 SU2 Harvey, 73 Jan 2 3

4523 MIT Harvey, 73 Mar 25 3 8077 Hoyle Harvey, 73 Jan 11 3

4625 Shchedrin Harvey, 73 Oct 30 3 8146 Jimbell Harvey, 73 Jan 6 3

4683 Veratar Harvey, 73 Jan 11 3 8297 Gérardfaure Faure, 20 Aug 2 6C

4822 Karge Harvey, 73 Oct 30 3 8373 Stephengould Hudgens, 35 Dec 24 2

4848 Tutenchamum Harvey, 73 Jan 11 3 8444 Popovich Faure, 20 Aug 26-27 2 Hudgens, 25 Aug 29 2 4941 1986 UA Harvey, 73 Oct 30 3 8693 Matsuki Harvey, 73 Oct 3 3 5081 1976 WC1 Harvey, 73 Mar 8 3 8736 1997 AD7 Hudgens, 35 Oct 15-16 2 5090 Wyeth Harvey, 73 Dec 21 3 8828 1988 RC7 Harvey, 73 Sep 20 3 5105 Westerhout Harvey, 73 Dec 2 3 Hudgens, 35 Sep 27 2

5133 Phillipadams Hudgens, 25 Sep 3 2 8904 1995 VY Faure, 20 Oct 21 2

5192 Yabuki Harvey, 73 Apr 1 3 9117 Aude Harvey, 73 Dec 1 3

5230 Asahina Harvey, 73 Mar 25 3 9219 1995 WO8 Faure, 20 May 29 2

5234 Sechenov Harvey, 73 Oct 30 3 9871 1992 DG1 Harvey, 73 Apr 1 3 Minor Planet Bulletin 31 (2004) 66

OBSERVER & OBSERVING NO. OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES PLANET APERTURE (cm) PERIOD (2003) OBS. NOTES

9992 1997 TG19 Hudgens, 25 Jun 20 2 65803 1996 GT Faure, 20 Nov 18 3 Garrett, 32 Nov 16 3 10826 1998 SK16 Harvey, 73 Jul 25 3 Harvey, 73 Nov 22 6 Hudgens, 35 Nov 22 4 11230 1999 JV57 Harvey, 73 Oct 30 3 66063 1998 RO1 Faure, 20 Sep 19 3 Harvey, 73 Sep 20 6 11483 1988 BC4 Faure, 20 Aug 2 3C 66959 1999 XO35 Harvey, 73 Dec 1 4 12193 1979 EL Hudgens, 35 Dec 18-20 2 69230 Hermes Bookamer, 41 Oct 27-30 22 12808 1996 AF1 Harvey, 73 Dec 1 3 Faure, 20 Oct 21 5 Garrett, 32 Oct 25 5 13249 Marcallen Harvey, 73 Nov 1 3 Harvey, 73 Oct 21 6 Hudgens, 35 Oct 17-19 5 13856 1999 XZ105 Hudgens, 35 Nov 20 2 Jardine, Pilcher, 35 Oct 24-30 4

13860 Neely Harvey, 73 Jul 6 3 70411 1999 SF3 Harvey, 73 Dec 16 3 Hudgens, 35 Dec 18-20 2 14699 2000 AV239 Harvey, 73 Dec 1 3 72569 2001 EC13 Harvey, 73 Dec 16 3 16975 1998 YX29 Harvey, 73 Apr 1 3 1978 CA Faure, 20 Feb 21 6 17919 1999 GC8 Harvey, 73 Jul 25 3 Harvey, 73 Mar 8 6

17939 1999 HH8 Faure, 20 Aug 26 2 1990 OS Faure, 20 Nov 18-19 3 Harvey, 73 Nov 23 6 18181 2000 QD34 Harvey, 73 Mar 8 3 1997 AE12 Faure, 20 Aug 27 3 19127 Olegfremov Harvey, 73 Sep 20 3 Hudgens, 35 Sep 27-Oct 1 2 1997 CZ5 Hudgens, 35 Dec 18-20 2

20446 1999 JB80 Harvey, 73 Sep 23 3 1998 TU3 Faure and Rayon, 35 Aug 24 2

21652 1999 OQ2 Garrett, 32 Aug 29 2 1998 XB Harvey, 73 Nov 30 6 Harvey, 73 Jul 25 3 Hudgens, 25 Aug 29 2 2001 CL42 Harvey, 73 Oct 3 6

24029 1999 RT198 Harvey, 73 Nov 9 3 2003 AL18 Faure, 20 Feb 8 4

26121 1992 BX Harvey, 73 Jan 6 3 2003 FG Harvey, 73 Apr 1 6

28913 2000 OT Harvey, 73 Jan 11 3 2003 UV11 Harvey, 73 Oct 30 6

34817 2001 SE116 Faure, 20 Jul 28 3 2003 UC20 Harvey, 73 Nov 23 6 Harvey, 73 Jul 25 3 2003 WX153 Harvey, 73 Dec 21 6 35107 1991 VH Faure, 20 Feb 9 4 Saverio Arlia, Buenos Aires, Argentina, with a 15 cm f/6 Newtonian, obtained 40 37274 2000 XO42 Faure, 20 Sep 19 2 astrometric photographs in calendar 2002 which were omitted from the 2002 report Harvey, 73 Aug 27 3 Hudgens, 25 Aug 29 2 due to a communication problem. We apologize for this omission and report them here. 40267 1999 GJ4 Harvey, 73 Feb 12 6 71 Niobe Arlia, 15 2002 Mar 21-24 4P 52340 1992 SY Faure, 20 Feb 23 4 Harvey, 73 Feb 24 6 230 Athamantis Arlia, 15 2002 Mar 2-24 17P

52387 1993 OM7 Harvey, 73 Jan 5 6 532 Herculina Arlia, 15 2002 Aug 10-Sep 8 19P

PHOTOMETRY OF 374 BURGUNDIA The facility is located fifteen miles east of Moorhead, Minnesota, and is adjacent to the Buffalo River State Park. Data were W.E. Worman collected on the nights of August 8, 1999, August 9, 1999, August Sherry Fieber 11, 1999, August 13, 1999, and August 14, 1999. (The dates on Kiernan Hulet the graph are one day later as they are universal time.) Dept. of Physics and Astronomy Minnesota State University Moorhead The Paul Feder Observatory has a sixteen-inch computer Moorhead, MN 56563 controlled DFM telescope with an associated Photometrics Star 1 [email protected] CCD camera. The CCD camera was used to collect data. 142 images were taken of 374 Burgundia over the five nights. Of (Received: 26 March) these 124 were used in the analysis. The others were discarded because the sky clouded over. 374 Burgundia was observed for five nights using CCD The exposures were two minutes long, and were generally Photometry during the month of August 1999. The separated by ten minutes. A filter was not used when taking the period of rotation is 6.972 ± 0.007 hours, and the exposures. Dark current and flat field corrections were made to lightcurve had an amplitude of 0.176 ± 0.011 magnitude. the data. Five stars were selected as magnitude standards for each image, but on the night of August 11, 1999 four stars were used. Observations The magnitudes of the comparison stars were taken from the Guide 7 program (Hubble Guide Star Catalog). A least squares fit Observations of 374 Burgundia were made at the Paul Feder was done and the relation between the magnitudes and the log of Observatory, which is located on the Buffalo River site of the total count determined from this relationship. A circular Minnesota State University Moorhead Regional Science Center. aperture of thirteen-pixel diameter was used and an equal sized Minor Planet Bulletin 31 (2004) 67 region of nearby background was used for the background LIGHTCURVE ANALYSIS FOR NUMBERED ASTEROIDS correction. 301, 380, 2867, 8373, 25143, AND 31368

Results Brian D. Warner Palmer Divide Observatory Times were corrected for the time it takes the light to travel from 17995 Bakers Farm Rd. the asteroid to the earth, and were taken at the center times for the Colorado Springs, CO 80908 image. Lightcurves were plotted for the four nights of usable data. [email protected] Relative magnitudes from night to night were uncertain as different comparison stars were used. This was dealt with by (Received: 21 March) using additive constants for the third–fifth night magnitudes to bring them into agreement with the second. A single lightcurve for the four nights was then least squares fit with a Fourier series Lightcurves results from Palmer Divide Observatory are including ten harmonics. The additive constants and the period presented for six numbered asteroids observed in early were adjusted so the fit minimized the square of the residual. The 2004. The following synodic periods and lightcurve resulting values were a period of 6.972 ± 0.007 hours. The amplitudes were determined: 301 Bavaria 12.24±0.01h additive constant for the third night was 0.38, for the fourth night and 0.25±0.02m; 380 Fiducia 13.69±0.01h and was –0.35, and for the fifth night was 0.12. The standard 0.20±0.02m; 2867 Steins 6.05±0.01h and 0.30±0.03m; deviation of the residuals was 0.023 magnitudes, which should be 8373 Stephengould 4.435±0.005h and 0.24±0.03m; 25143 good measure of the uncertainty in the relative magnitudes. The Itokawa 12.09±0.01h and 0.70±0.03m; (31368) 1998 last two points for the night August 15 (phase 0.45 and 0.47) look WW23 14.860±0.005h and 0.21±0.02m. low. They were taken when the sky background level was increasing with the approach of dawn (3:50 and 4:00 AM CDT) Equipment and Procedures and may have larger uncertainties than the other points. The high points around the same phase (about 0.5) were the first four The asteroid lightcurve program at the Palmer Divide Observatory observations on August 10. We have checked and not found any has been previously described in detail (Warner 2003) so only a error. It is conceivable that the lightcurve may actually have been summary is provided now. The main instrument at the changing with time in that region. Observatory is a 0.5m f/8.1 Ritchey-Chretien telescope using a Finger Lakes Instruments IMG camera with Kodak KAF-1001E A period of 6.972 ± 0.007 hours was found, and the third-fifth chip. A second instrument also in use was a 0.3m f/9.3 Schmidt- night was translated to fall on the second night of data to give the Cassegrain using an SBIG ST-9E camera. For this set of composite lightcurve shown in Figure 1. The time scale is given asteroids, only the 0.5m scope was used. phase. There are two maxima per period. The amplitude of the light curve is 0.176 ± 0.011 magnitude. The uncertainty in the Initial targets are determined by referring to the list of lightcurves amplitude was determined from the least squares fit to the Fourier maintained by Dr. Alan Harris (Harris 2003), with additions made series using the standard deviation of the mean for nine points by the author to include findings posted in subsequent issues of each in the vicinities of the maximum and the minimum. the Minor Planet Bulletin. In addition, reference is made to the Collaborative Asteroid Lightcurve Link (CALL) web site The standard magnitudes given on the graph must be considered to maintained by the author (http://www.MinorPlanetObserver.com/ be uncertain by ± 0.40 magnitudes, while relative magnitudes are astlc/default.htm) where researchers can post their findings uncertain by about ± 0.023 magnitudes. The phase angles during pending publication. MPO Canopus, a custom software package observations varied between 9.5 degrees and 10.6 degrees. written by the author, is used to measure the images. It uses aperture photometry with derived magnitudes determined by calibrating images against field or, preferably, standard stars. Raw instrumental magnitudes are used for period analysis, which is included in the program. The routine is a conversion of an original FORTRAN code developed by Alan Harris (Harris et al, 1989).

Note: in the following, the orbital elements are taken from the IAU MPCORB data file available at the Minor Planet Center web site (ftp://cfa-ftp.harvard.edu/pub/MPCORB/). The date of osculation for the elements was 2453200.5. The Phase Angle Bisector (PAB) was previously described (Warner 2004).

Results

301 Bavaria

J. Palisa discovered Bavaria, also known as 1928 DH1, 1951 FD, and 1952 OF, from Vienna on 1890 November 16. Named in Figure 1. Lightcurve for 374 Burgundia assuming a synodic period commemoration of the 1891 August meeting of the of 6.972 hours. The V magnitude scale is approximate owing to Astronomische Gesellschanft in Munich (the capital of Bavaria), the typical 0.4 mag. uncertainty of the Hubble Guide Star Catalog. the asteroid is a member of the Liberatrix family. Kosai (1979) puts Bavaria in his group 30, which includes more than 100

Minor Planet Bulletin 31 (2004) 68 members such as 26 Proserpina, 34 Circe, 88 Thisbe, in addition to the family namesake, 125 Liberatrix. Bavaria’s primary orbital elements are: semi-major axis, 2.724AU; inclination, 4.895°; and eccentricity, 0.0662. The IRAS survey (Tedesco 1989) gives a diameter of 54.32±3.3km and albedo of 0.0546±0.007.

This asteroid was picked partly for being one of those few asteroids numbered less than 1,000 that had either no or a poorly established set of lightcurve parameters. Observations were made over five sessions from 2004, January 15 through January 25. 468 data points were used in the lightcurve analysis, which gave a synodic period of 12.24±0.01h and an amplitude of 0.25±0.02m. Figure 1 shows the data phased against this period.

DATE Phase PAB 2004 Angle Long Lat 01/15 7.7 95.1 -4.2 01/18 8.8 95.1 -4.1 01/19 9.2 95.1 -4.1 01/22 10.2 95.2 -4.1 01/25 11.2 95.2 -4.0

Figure 2. The lightcurve for 380 Fiducia phased against a synodic period of 13.69±0.01h. The amplitude is 0.20±0.02m.

2867 Steins

Discovered by N.S. Chernykh at Nauchnyj on 1969 November 4, Steins is named after Karlis Augustovich Steins, the former director of the Latvian University Astronomical Observatory who was well known for his work on cometary cosmogony. The asteroid was selected after the announcement that it would be one of two targets for the Rosetta mission in 2008. Planning for such mission flybys often requires having at least some information about the target’s spin rate and, if possible, pole orientation. Unfortunately, 2004 was the “worst” apparition in the current decade, based on maximum brightness. A much better opportunity awaits Southern Hemisphere observers in 2005.

Other information on Steins is wanting. Using its H value of 12.90, the estimated diameter based on Harris (2003) indicates a diameter of 8km, if one assumes an albedo of 0.18. The principal Figure 1. The lightcurve for 301 Bavaria. The synodic period is elements are: semi-major axis, 2.364AU; inclination, 9.944°; and 12.24±0.01h and the amplitude 0.25±0.02m. eccentricity, 0.1455. The asteroid has also carried the

designations 1954 QL, 1969 VC, 1979 FJ4, 1980 VV1, and 1980 380 Fiducia WB.

Fiducia was discovered by A. Chrolis at Nice on 1894 January 8. Steins was observed on four successive nights, starting on 2004 It has carried the designations 1933 CA, 1945 VH, and 1975 LX March 17. The magnitude was approximately 16.5 at the time and in addition to its Latin name for “confidence.” The IRAS survey so the resulting data was noisier (low SNR) than usually preferred. (Tedesco 1989) states a diameter of 73.2±2.8km and albedo of Figure 3 shows the plot of data, binned 3x3, meaning three 0.0563. Just as with 301 Bavaria, Kosai (1979) places Fiducia in consecutive data points were averaged to find a single value, his group 30. The principal elements are: semi-major axis: providing that the maximum time span between any two 2.681AU; inclination, 6.154°; and eccentricity, 0.1130. observations was less than three minutes. The time-interval test assures that a value isn’t found by combining points that may be The asteroid was observed 2004 March 8 through March 13, with well separated in phase location. The binning provided some only March 11 excluded. Some 820 data points were used in the “smoothing” of the data so that period analysis could be more period analysis, which showed a lightcurve period of 13.69±0.01h readily performed. The synodic period is 6.05±0.01h and the and amplitude of 0.20±0.02m. Figure 2 shows the data phased to amplitude of the curve is 0.30±0.03m. that period. DATE Phase PAB DATE Phase PAB 2004 Angle Long Lat 2004 Angle Long Lat 03/17 7.4 166.0 11.9 03/08 8.8 145.4 6.1 03/18 7.7 166.0 11.9 03/09 9.2 145.4 6.1 03/19 8.0 166.0 11.9 03/10 9.5 145.4 6.1 03/20 8.4 166.0 11.8 03/12 10.2 145.4 6.2 03/13 10.5 145.4 6.2 Minor Planet Bulletin 31 (2004) 69

among family members may be a sign of the YORP effect, the period of 1362 Griqua is 6.907h with an amplitude of 0.25m (Bembrick 2002).

DATE Phase PAB 2004 Angle Long Lat 01/09 19.3 98.5 20.4 01/10 20.1 98.5 21.0 01/11 20.9 98.5 21.6 01/12 21.8 98.5 22.3 01/13 22.6 98.6 22.9

Figure 3. The lightcurve for 2867 Steins. The data is phased against a synodic period of 6.05±0.01h. The amplitude is 0.30±0.03m.

8373 Stephengould

This asteroid is named after Stephen Jay Gould (1941-2003) who is probably best known for his series of articles in Natural History in which he expressed his views on evolution. Along with Niles Eldredge, he developed the idea of “punctuated equilibrium”. C. S. Shoemaker found the asteroid on New Year’s Day 1992. Being the second asteroid found in the new year, it was given the Figure 4. The lightcurve for 8373 Stephengould. The synodic designation 1992 AB. period is 4.435±0.005h with an amplitude of 0.24±0.03m.

Using the H value of 13.8 from the MPCORB database, a formula 25143 Itokawa provided by Harris (2003), gives a diameter of 10km – assuming This asteroid was selected for as a result of a call for observations the albedo is approximately 0.18. The primary elements are: from D. Vokrouhlicky, M. Kaasalinen, and others (Vokrouhlicky semi-major axis, 3.282AU; inclination, 40.782°; and eccentricity, 2004). The authors stated their belief that careful observations of 0.5541. These elements put Stephengould in a small group of the asteroid could help prove the YORP effect by the fact that the asteroids headed by 1362 Griqua that appear to be in a stable 2:1 spin rate of Itokawa was gradually slowing down. This could be libration with Jupiter. There are about ten members in this group. demonstrated by plotting the curve obtained in 2004 against a predicted curve based on the accurate sidereal period found in This was a very fortuitous catch of the asteroid. Almost all the apparitions through 2050 have it in the range of magnitude 19 to 2001. If the prediction was correct, coincident maxima would be out of phase by about 8%, or one hour. Itokawa is also the 21. About every six years, usually late one year and early the planned destination for the Japanese MUSES-C sample return next, it comes within 1.0 AU of Earth and then 14th to 15th mission, now enroute. magnitude. The 2004 apparition happened to be the closest approach the asteroid makes through 2050 (at 0.650 AU). Despite being near the observational limit for PDO (about 18th Observations were made in five sessions from 2004 January 9 magnitude using the Clear filter), data of reasonable quality (about 0.05m scatter) was obtained on the nights of 2004 January 23 and through 13, with two of the sessions being on the same date, 24. Using the Clear to Visual method mentioned previously, the January 10. The definition of a session at the Palmer Divide Observatory is a set of observations that use the same set of asteroid was found to be about 17.8 on the two nights. Figure 5 shows the phased data of 178 points against a period of comparison stars on the same night through the same filter. In the 12.09±0.01h. The curve has an amplitude of 0.70±0.03m. The case of January 10, the asteroid was moving fast enough that the original set of comparison stars could not be used throughout the period agrees well with the sidereal period found in 2001 of 12.132h (Kaasalainen 2003). night. A method developed by the author and Robert D. Stephens of Santana Observatory, CA, allows clear filter observations to be The initial indication after the two nights as analyzed by converted reasonably close to the Johnson V band. The data were Kaasalainen (2004), was that the data supported the prediction of a transformed using this technique with the result that overlapping slowing spin axis rate. However, Petr Pravec (2004) pointed out observations matched to an internal precision of 0.02m or better. that other factors may have contributed to the phase shift and that additional study was needed. A call for additional observations A total of 268 data points used in the analysis gave a synodic was issued to the amateur community, which will be accompanied period of 4.435±0.005h with an amplitude of 0.24±0.03m (see Figure 4). For comparison, since spin axis rate and orientation Minor Planet Bulletin 31 (2004) 70 by radar observations planned by Steve Ostro et al at Arecibo, Puerto Rico, in mid-2004.

The primary orbital elements for the asteroid are: semi-major axis, 1.323AU; inclination, 1.728°; and eccentricity, 0.2795.

DATE Phase PAB 2004 Angle Long Lat 01/23 5.0 125.0 3.3 01/24 4.4 125.1 3.3

Figure 6. A phased lightcurve for (31368) 1998 WW23 using a synodic period of 14.860±0.005. The amplitude is 0.21±0.02.

Acknowledgments

Thanks go to Dr. Alan Harris of the Space Science Institute for making available the source code to his Fourier Analysis program and his continuing support and advice. I also thank Robert D. Stephens of Santana Observatory, Rancho Cucamonga, for his on- going advice and support. Figure 5. A phased lightcurve for 25143 Itokawa using a synodic References period of 12.09±0.01h. The amplitude is 0.70±0.03m. Harris, A. W., Young, J. W., Bowell, E., Martin, L.. J., Millis, R. (31368) 1998 WW 23 L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J., Debehogne, H., and Zeigler, K. W., (1989). “Photoelectric Discovered on 1998 November 25 by the LINEAR survey, this Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, asteroid has an estimated diameter of 22km (Harris 2003). The 171-186. primary elements are: semi-major axis, 2.914AU; inclination, 15.219; and eccentricity, 0.2587. These make 1998 WW a 23 Harris, Alan W. (2003). “Minor Planet Lightcurve Parameters”, member of the main belt with no apparent attachment to a special On Minor Planet Center web site: http://cfa- group or family. The 2004 apparition was one of the best through www.harvard.edu/iau/lists/LightcurveDat.html 2050 for this asteroid. Most years the asteroid stays well below th 15 magnitude but in March every five years (at least through Kaasalainen, Mikko (2004) private communications. 2050), it almost brightens into the 14s and so becomes an easier target for amateur equipment. Kozai, Y., (1979). “The dynamical evolution of the Hirayama family.” In Asteroids (T. Geherels, Ed.) pp. 334-358. Univ of Observations were made in four sessions in the period between Arizona Press, Tucson. 2004 January 18 and February 14. The first two sessions in January seemed to favor a period near 24 hours, so it was decided Pravec, Petr (2004) private communications. to wait a week or two before re-observing the asteroid. This would allow the data to migrate along the curve enough to get a Schmadel, L. (1999). Dictionary of Minor Planet Names, 4th significantly different portion of the curve. Weather and travel edition. Springer-Verlag, Heidelberg, Germany. prevented additional observations until mid-February. The Clear to Visual technique previously mentioned was used to calibrate the Tedesco, E. F., Tholen, D. J., and Zellner, B. (1989). “UBV colors data for period analysis, which involved 389 data points and found and IRAS alebedos and diameters”. In Asteroids II (R.P. Binzel, a period of 14.860±0.005h with an amplitude of 0.21±0.02m. T. Gehrels, and M.S. Matthews, Eds.) pp. 1090-1138. Univ. of Figure 6 shows the data phased against this period. Arizona Press, Tucson.

DATE Phase PAB 2004 Angle Long Lat Warner, B. D. (2003). “Lightcurve Analysis for [Several] 01/18 19.3 156.1 15.9 Asteroids”, Minor Planet Bulletin 30, 21-24. 01/25 17.6 157.2 16.6 02/13 12.7 159.3 18.5 Warner, B. D. (2004). “Lightcurve analysis for Numbered 02/14 12.5 159.3 18.5 Asteroids 1351, 1589, 2778, 5076, 5892, and 6386”, Minor Planet Bulletin, 31, 29-32. Minor Planet Bulletin 31 (2004) 71

ROTATIONAL PERIODS OF ASTEROIDS arisen. Being present was also a good opportunity to roughly 1165 IMPRINETTA, 1299 MERTONA, judge the quality of the data and to make any changes if necessary. 1645 WATERFIELD, 1833 SHMAKOVA, 2313 ARUNA, In some cases an asteroid was abandoned to obtain a better AND (13856) 1999 XZ105 lightcurve for the other two. It was thought impractical to do more than three asteroids per session otherwise the time resolution Andy Monson would be too poor to construct a quality lightcurve in only 2-3 Department of Physics and Astronomy sessions. At least seven bias and dark frames were taken at the Minnesota State University beginning of each run once the operating temperature was 141 Trafton Science Center N. reached. They were each median combined in MIRA and used to Mankato, MN 56001 correct each raw image. A master flat was created using a number [email protected] of unprocessed raw images from each field throughout the night. The pointing accuracy of the telescope throughout the night was Dr. Steven Kipp excellent, however with the large image scale individual stars in Department of Physics and Astronomy each field were not aligned, thus a median of a large number of Minnesota State University raw images where stars didn’t line up produced a good flat field. 141 Trafton Science Center N. Aperture photometry was performed on the asteroid and stars in Mankato, MN 56001 each field using MIRA. The data were then copied into Excel [email protected] where comparisons were made between all the stars in a field to find five that showed the most stable magnitude difference (Received: 16 February Revised: 9 March) throughout the session. With the first image in the series representing the zero-point, the five chosen stars were compared to the asteroid in that field to construct a differential lightcurve. We report rotation lightcurve periods for six asteroids The data were then transferred into the FORTRAN program, with previously unknown values: 1165 Imprinetta FALC, Harris et al. (1989), where the period was found. 7.9374±0.0016 hr, 1299 Mertona 4.977±0.003 hr, 1645 Waterfield 4.861±0.002 hr, 1833 Shmakova Observations and Results 3.934±0.003 hr, 2313 Aruna 8.900±0.003 hr, and (13856) 1999 XZ105 4.4475±0.0055 hr. We also list six 1165 Imprinetta asteroids for which data were insufficient to yield period results at this time. This asteroid was observed on the nights of September 27th, 29th and October 1st. There is not a complete lightcurve due to the six- hour sessions and approximate eight hour period, thus each night Introduction and Procedures the same portion of the lightcurve was observed. The period was th In this paper a method for obtaining multiple asteroid observations found using a 4 order Fourier fit and found to be 7.9374±0.0016 at our site is discussed. Using previously developed methods of hr. The observed amplitude appears to be about 0.20 magnitudes. Independent observations by Menke (2004) during October 15th- data reduction Uzpen and Kipp (2003), the periods of the observed th asteroids were determined. 19 of Imprinetta yielded a similar period of 8.107±0.020 hr and an amplitude of 0.20±0.04. The selected asteroids were observed using the 51-cm DFM Cassegrain telescope at Andreas Observatory at Minnesota State University, Mankato. An f/6.3 focal reducer was mounted at the focus of the telescope to yield a 6.8'x10.2' field of view with the SBIG ST-8E CCD camera and color filter wheel. A Johnson R filter was used for all observations in this article because the chip is most sensitive in the red part of the spectrum. The chip was binned 3x3 to increase the count rate and also to reduce download time. The field of view offered far fewer comparison stars than Uzpen and Kipp (2003), who used a faster but smaller aperture Schmidt, however exposure times were cut and image scale was greatly improved. With exposure times of 90-120 seconds for 14th and 15th magnitude, respectively, it became possible to slew between multiple targets in a single session and still have enough data points for each target to construct a reasonable lightcurve. Three asteroids were chosen from the CALL website (Warner 2003) to be observed each session. Each asteroid was individually 1299 Mertona chosen based on brightness and proximity to enough comparison stars. Ideally asteroids were chosen as close together as possible Mertona was observed on the nights of November 20th, 28th and so that the pointing accuracy of telescope would not be affected 29th. The period was found to be 4.977±0.003 hr with an between multiple slew commands. The telescope was cycled amplitude of 0.55 magnitudes. through each field throughout the session. There was typically a 6 minute gap between exposures on a single asteroid yielding around 60 data points for a six hour session. In practice however, weather and fatigue cut most observing runs to four hours. Although the telescope is capable of automation it was preferred that someone was present to solve any problems that may have Minor Planet Bulletin 31 (2004) 72 2313 Aruna

Asteroid Aruna was observed in conjunction with asteroid Waterfield and found to have a period of 8.900±0.003 hr and a large amplitude of 0.8 magnitudes.

1645 Waterfield

Asteroid Waterfield was observed on the nights of October 17th and 18th. It was also observed independently by Willis et al. (2003) on October 16th and 17th. The period found by Willis was 4.87±0.01 hr which is consistent with our value of 4.861±0.002 hr (13856) 1999 XZ105 with a mean amplitude of 0.20 magnitudes. This asteroid was observed in conjunction with asteroid Mertona and found to have a period of 4.4475±0.0055 hr with an amplitude of 0.5 magnitudes.

1833 Shmakova

This asteroid was observed on the night of August 11th. It was satisfactorily determined to have a period of 3.934±0.003 hr with Other Asteroid Observations only the one night of observation. The observed amplitude was 0.38 magnitudes. In addition to our reported results, Table I lists other asteroids that have been observed in our program. At present, we have insufficient data to determine their periods. It is possible some of these objects may have low lightcurve amplitudes or long periods, making them somewhat difficult targets for rotation lightcurve period solutions.

Acknowledgements

We would like to thank Brian Uzpen for his pioneering work on asteroid rotation lightcurves at Andreas Observatory. We would also like to thank Brain Warner for maintaining the Collaborative Asteroid Lightcurve Link (CALL) and Dr. Alan Harris for the FALC program.

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. (1989). “Photoelectric

Minor Planet Bulletin 31 (2004) 73

Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, Observations and Analysis 171-186. The images were obtained using the 1.8-meter Vatican Advanced Menke, John. (2003). “Submitted Lightcurve parameters,” on the Technology Telescope at Mt. Graham International Observatory. Collaborative Asteroid Lightcurve Link: http://www The Harris R filter was used for most of the frames with exposure .minorplanetobserver.com/astlc/default.htm times that ranged from 90-120 seconds. Additionally, on Jan 28, BVRI sequences were obtained. The observational circumstances Warner, B.D. (2003). Collaborative Asteroid Lightcurve Link are given in Table I. This table includes the UT date of mid- (CALL) web site. http://www.minorplanetobserver.com/astlc/ observation, geocentric ecliptic longitudes and latitudes, solar default.htm phase angle, and mean R magnitudes, reduced to unit heliocentric and geocentric distances. The observations were performed in the Willis, S., Divoky, M., Spitler, L., Staab, M. (2003). “Submitted Milky Way region. Therefore, although seeing conditions that Lightcurve parameters,” on the Collaborative Asteroid Lightcurve were of order 1" or better made this feasible, frequent gaps in the Link: http://www.minorplanetobserver .com/astlc/default.htm data exist due to the fact that either Tabei was obscured by field stars in the images, or the primary target, Celle, was obscured, and Uzpen, B., and Kipp, S. (2003). “Rotational Periods of Asteroids hence, no frames were taken. 34, 239, 759, and 963.” The Minor Planet Bulletin 30, 59-61. The images were processed and aperture photometry was performed using IRAF (Tody, 1993). Differential magnitudes were calculated between Tabei and an ensemble of 5 comparison Table I. stars yielding typical errors on the order of 0.005 mag. The Observations of Asteroids with too little data (at present) occasional larger errors were due primarily to contamination by for rotational lightcurve period solutions. nearby field stars. The BVRI sequences taken on Jan 28 were calibrated using Landolt (1992) standards that were observed the # Name Date same night. The R magnitudes for Jan 29 were similarly 634 Ute 2003-7-1 calibrated using images taken of the comparison star field later in 370 Modestia 2003-8-2 1499 Pori 2003-8-4 the run on the photometric nights of Jan 30 and Feb 1. 1775 Zimmerwald 2003-8-4 1775 Zimmerwald 2003-8-13 Lightcurves were generated for the two nights using the 1775 Zimmerwald 2003-8-14 4092 Tyr 2003-9-29 heliocentric and geocentric distance corrected R magnitudes. 4092 Tyr 2003-10-1 These data were analyzed using the standard technique described 1930 Lucifer 2003-10-1 3990 Heimdal 2003-10-17 by Harris and Lupishko (1989) and Harris, et al (1989). The 3990 Heimdal 2003-10-18 resulting composite lightcurve using a period of 5.862 ± 0.001 1589 Fanatica 2003-12-1 hours is shown in Figure 1 and displays an amplitude of 0.43 mag. The analysis of two BVRI color sequences from Jan 28 yielded the following observed (not corrected for solar colors) color indices PHOTOMETRY OF MINOR PLANET 6897 TABEI for 6897 Tabei: B–V=0.908±0.010, V–R=0.477±0.010, and V–I=0.889±0.010. William H. Ryan Magdalena Ridge Observatory, Acknowledgements New Mexico Institute of Mining and Technology Socorro, NM 87801 This work is supported by NASA Planetary Astronomy Grant [email protected] NAG5-8734 and is based on observations with the VATT: the Alice P. Lennon telescope and the Thomas J. Bannan Astrophysics (Received: 29 March) Facility.

The minor planet 6897 Tabei was observed for two nights in January 2003 using the 1.8-meter Vatican Advanced Technology Telescope. The observed R lightcurves indicated a rotational period of 5.862 ± 0.001 hours and an amplitude of 0.43 mag. BVRI data taken on Jan 28 yielded the following color indices: B–V=0.908±0.010, V–R=0.477±0.010, and V–I=0.889 ± 0.010.

Since 1999, a photometric study of the Vesta family of asteroids has been undertaken in order to gain more insight to their collisional origin (Ryan, et al., 2000). During the course of this project, the binary system 3782 Celle was discovered (Ryan, et al., 2004). In January 2003, 6897 Tabei, the subject of this note, was observed for two nights in images taken by the author while collecting additional data on Celle. Figure 1. Composite lightcurve for 6897 TabeiCCD

Minor Planet Bulletin 31 (2004) 74

References Proceedings of the 32nd Meeting of the DPS, Pasadena, Calif, BAAS, 32, 1002. Harris, A. W. and Lupishko, D. F. (1989). “Photometric lightcirve observation and reduction techniques.” In Asteroids II (R. P. Ryan, W. H., Ryan, E. V., and Martinez, C. T. and Stewart, L. Binzel, M. Matthews, and T. Gehrels, eds.) pp 39-53. Univ. (2003). “(3782) Celle”, IAU Circular No. 8128 Arizona Press, Tucson. Ryan, W. H., Ryan, E. V., and Martinez, C. T. (2004). “3782 Harris, A. W., Young, J. W., Bowell, E., Martin, L. J., Millis, R. Celle: Discovery of a Binary System within the Vesta Family of L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J., Asteroids”, submitted to Planetary and Space Science Debehogne, H, and Zeigler, K. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, Tody, D. (1993). “IRAF in the Nineties”. In Astronomical Data 171-186. Analysis Software and Systems II, A.S.P Conference Ser., Vol 52, eds. Hanisch, R.J., Brissenden, R.J.V., and Barnes, J., 173. Landolt, A.U. (1992). “UBVRI photometric standard stars in the magnitude range 11.5

THE MINOR PLANET OBSERVER: Flying somewhere between Denver and Atlanta, I was amazed to BEING IN THE DARK IS NOT ALL BAD see all the unprotected lighting. In some places, where I thought there should be hundreds of square miles of black landscape there Brian Warner were, instead, hundreds of unshielded mercury vapor lights dotting Palmer Divide Observatory the scene. It seemed at times that the only way to tell the end of a 17995 Bakers Farm Rd. town and the beginning of “countryside” was the color of the Colorado Springs, CO 80908 lights: purplish mercury vapor for the latter and orange-tinted [email protected] sodium vapor for the former. In those earlier days of flying, I easily imagined myself in one of the many vast dark locations Last February, I had the pleasure and privilege to attend a below, armed with a large scope and camera. On this trip, I was workshop at the Arecibo Observatory in Puerto Rico. It had been hard-pressed to find a spot that wasn’t affected by at least one set a long time since I had taken a trip by air, even longer since I did of lights. Flying into Atlanta itself was fascinating in its own way. so at night. Years ago, I did more such traveling and remembered I could see the shadow of my hand against the seatback, cast by how I’d particularly like to fly at night. The Earth seems much the galaxy of sodium lights shining through the window. different then, especially at 30,000 feet (9200m). The details of the landscape disappear and so all that’s left to guide you are the It continues to confound me when one of my neighbors talks about lights of one small town to the next to the next and so on to the big what they like about country living is all the stars that can be seen city down the road. I would trace the lights in each town, finding and then have them go turn on their uncovered lighting and drown the main street (more lights) and parks (black squares amidst a those stars in a sea of artificial light. There have been many sprinkle of diamonds). On Friday and Saturday nights in the fall, studies done that show that uncovered, glaring lights are less of a especially over some states, it was easy to see which town had a security guard than well-conceived, covered lighting. That idea football game going (or several). The stadium would light up the just doesn’t seem to sink in with many. The goal seems to be a sky and surrounding landscape and could be seen for miles. I literal 24-hour day, the sun notwithstanding. Efforts at light always wondered who was playing and what was the score. I pollution control do sometimes succeed. Other times, as with a wondered who was driving along those small town streets. How recent attempt by a legislator in my state, those efforts are met many re-enactments of “American Graffiti” were taking place with derision, contempt, or bursts of laughter. each night? Even though I was interested in astronomy in those days, my thoughts never turned to those of light pollution and Those of us involved in astronomy, particularly those who are at wasted electricity. This trip, they were. I supposed it was in large the scope (even if not quite literally given the automation available part because I have become so much more active in observing these days), need to find ways to make the case for controlled (asteroid lightcurves) and the encroachment of housing lighting without making it an all or nothing debate. That only development on my once mostly isolated neighborhood. My night widens the gap before understanding and acceptance can take sky is rapidly brightening, more than it should even considering place. The International Dark Sky Association the housing growth due to a number of unprotected porch lights. (http://www.darksky.org/) is a good starting point for formulating Fortunately, there are no streetlights in the neighborhood – yet. ideas and plans that can help save the night sky. This is one case There is an elementary school that does have hooded lights. I’m where being a little selfish and saving something for ourselves hard pressed to tell those lights are on, even though they are only yields returns for everyone. two blocks away. It’s the two porch lights across the street, lighting up the sky almost as much as the entire city of Colorado I mentioned a trip to Arecibo at the start. While certainly for Springs about 20 miles to the south. When the neighbor leaves pleasure it was for more formal reasons. In early February, the those lights off, the limiting magnitude to the south improves Observatory hosted the “Asteroid Dynamics Workshop” where for dramatically. three days updates on developments in YORP effect and rubble pile theories were presented. The latter had a humorous post

Minor Planet Bulletin 31 (2004) 75 script when a few days afterwards it was announced by two U.S. marching orders and left with directions from 13 generals, each scientists that a 55-gallon drum full of M&M candy helped show telling me to go a different way.” For example, there was that non-spherical particles can pack together more efficiently than continuing work on asteroids whose spin rate is believed to have spherical. I wonder if we’ll soon see an asteroid made of M&M been altered by the YORP effect. That applies to, among others, candy on a web site. Will those modeling software packages the Koronis family, long-studied by Steve Slivan, and the Karin include a special option, allowing the user to select plain, peanut, family, believed to be only 6MY old. It’s important to see how or almond? the members of this family have or have not been affected by YORP. Add getting additional lightcurves for Mikko I was privileged to attend this meeting, thanks to an invitation Kaasalainen’s shape modeling candidates and using Sloan Digital from the committee, and to get a guided tour of the facility, Sky Survey results to confirm whether or not asteroids change including a trip to the platform suspended 500 feet (152m) above color during a rotational cycle or help confirm theories on galaxy the surface of the dish. Words can’t really do justice to the formation by observing certain fainter stars to see if they are observatory, nor can most pictures (one needs a very wide-angle members of the RR Lyrae class (someone managed to sneak in lens). When standing at the visitor’s center viewing area, the variable stars at an asteroid workshop). massive radar dome and platform seem just out of arm’s reach, yet they are 500 feet away. Being on the platform was not as scary as Those are just some of the projects. There are many more. I thought it might be. Walking down the catwalk to the visitor’s What’s on the CALL site alone could occupy many observers full- center was another matter entirely. Enclosed or not, it’s a bit time for many years. Add the many other projects already known frightening. and those yet to be, not just involving asteroids – the AAVSO would love to hear from qualified CCD photometrists, and there I was able to give a talk to the group of professionals that touted should be no doubt that there is more than enough for any amateur the growing number of skilled amateurs and how they can help (or professional) to do. “Observers! Start your telescopes!” Clear acquire the data professionals need to prove and develop their (and darker) Skies! work. As I mentioned more than once, “I arrived looking for

LIGHTCURVE PHOTOMETRY OPPORTUNITIES This can be very challenging work but, like any other, can reap JULY – SEPTEMBER 2004 considerable rewards. Towards the goal of getting some observers interested in this field, now facilitated by equipment and resources Brian D. Warner readily available these days, here are some considerations to be Palmer Divide Observatory keep in mind. 17995 Bakers Farm Rd. Colorado Springs, CO 80908 First, sample the lightcurve at several different phase angles. The minimum recommendation is about every factor of 1.5 in phase Mikko Kaasalainen angle, e.g., 1.0 (or less), 1.5, 2, 3, 5, 8, 12, 18, and 24 degrees is a Rolf Nevanlinna Institute good starting sequence. If at all possible, try to cover both sides of P.O. Box 4 (Yliopistonkatu 5, room 714) minimum phase angle. The reason is that some asteroids show a FIN-00014 University of Helsinki, Finland different phase relationship on either side of minimum, 44 Nysa being one of the first found to show this trait. Next, if the phase Alan W. Harris angle is less than 1°, sample every night and as thoroughly as Space Science Institute possible. In this case, oversampling the curve is definitely 4603 Orange Knoll Ave. preferred so as to “beat down the noise.” La Canada, CA 91011-3364 It is best to do the highest density reference lightcurve (remember, Petr Pravec you need to find the V magnitude for the average value of the Astronomical Institute lightcurve) on nights a bit off the zero phase angle time. This is CZ-25165 Ondrejov because the phase angle effect, especially if there is a spike near Czech Republic 0°, can distort the lightcurve on a time scale comparable to the [email protected] rotation period. In this case, you can’t separate the phase angle effect from the lightcurve over a single cycle of the curve. Sometime ago, when one of the authors (Harris) wrote this article with V. Zappala, the list of lightcurve opportunities included not If possible, the data should be reduced to standard V magnitudes only targets with no or poorly known lightcurve parameters but those that were going to reach very small phase angles (indicated since the H–G values are based on that band. Regardless of the with ‘PHA’ at the time; those initials have since taken on an color band in which you observe, absolute calibration between entirely different meaning in asteroid work). The study of nights over the entire run is essential. lightcurves when the phase angle is less than 7°, and particularly when less than 1°, is important for studies involving the so-called From here on, the list of opportunities will include objects “opposition effect” and “opposition spike.” The former is a non- reaching a particularly low phase angle (<7°). We’ll continue to linear change in brightness as the object approaches opposition. list targets of opportunity for shape/spin modeling as well. Never The latter is an even more dramatic non-linear change when the let it be said that there’s not enough to keep everyone busy! phase angle is very small. Besides helping develop theories about You’ll find a more complete list of lightcurve opportunities for the why these effects occur, the data from small phase angle current and recent quarters on the CALL web site. observations can be used to refine the H-G phase relation used to (http://www.MinorPlanetObserver.com/astlc/ default.htm). Be predict asteroid magnitudes. sure to check the link on the CALL site to planned radar

Minor Planet Bulletin 31 (2004) 76 observations. Optical observations are often needed to support the THE MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly radar work. The complete list for low phase angle opportunities journal of the Minor Planets Section of the Association of Lunar and Planetary Observers. The Minor Planets Section is directed by its for 2004 is also available, covering asteroids <16.0 and <1.5°. Coordinator, Prof. Frederick Pilcher, Department of Physics, Illinois College, Jacksonville, IL 62650 USA ([email protected]), assisted by Lightcurve Opportunities Lawrence Garrett, 206 River Road, Fairfax, VT 05454 USA ([email protected]). Richard Kowalski, 7630 Conrad St., Brightest Zephyrhills, FL 33544-2729 USA (qho@bitnik. com) is Associate # Name Date V Dec Per. Amp Coordinator for Observation of NEO’s, and Steve Larson, Lunar and 1386 Storeria 7 03.1 14.2 + 1 Planetary Laboratory, 1629 E. 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Electronic submissions can be formatted either using a Microsoft Word template document Note that the amplitude in the table just above could be more, or available at the web page just given, or else as text-only. A printed version less, that what’s given. Use the listing as a guide and double- of the file and figures must also be sent. All materials must arrive by the check your work. deadline for each issue. We regret that diskettes cannot be returned. Visual photometry observations, positional observations, any type of observation not covered above, and general information requests should be sent to the Coordinator.

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The deadline for the next issue (31-4) is July 15, 2004. The deadline for issue 32-1 is October 15, 2004.

Minor Planet Bulletin 31 (2004)