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The Minor Planet Bulletin Published an Article on Analysis THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 34, NUMBER 2, A.D. 2007 APRIL-JUNE 27. THE ROTATION PERIOD OF 2651 KAREN Colin Bembrick Mt Tarana Observatory PO Box 1537, Bathurst, NSW 2795, Australia [email protected] Bill Allen Vintage Lane Observatory 83 Vintage Lane, RD3, Blenheim, New Zealand (Received: 6 January) 2651 Karen was observed over 4 nights in 2006. The synodic period was determined as 6.3227 ± 0.0037 hr. The peak to peak amplitude was approximately 0.3 mag, implying an axial ratio (a/b) of 1.32 References Bembrick, C.S., Richards, T., Bolt, G., Pereghy, B., Higgins, D. Minor planet 2651 Karen (1949 QD) was discovered by E. and Allen, W.H. (2004). “172 Baucis – A Slow Rotator”. Minor Johnson in August 1949 at Johannesburg. This is an outer main Planet Bulletin, 31, 51-52. belt asteroid with a diameter of 39.7 km (GUIDE ver 8). The latest list of rotational parameters (Harris & Warner, 2006) has no GUIDE version 8 (2002). http://www.projectpluto.com quoted period. Harris, A.W. and Warner, B.D. (2006). “Minor Planet Lightcurve The observations of Karen in 2006 were conducted from two sites Parameters”. Updated March 14, 2006. – one in New Zealand and one in Australia. The locations of these http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html sites are listed in Bembrick et al (2004). All observations were made using unfiltered differential photometry and all data were Harris, A.W., Young, J.W., Bowell, E., Martin, L. J., Millis, R. L., light time corrected. The aspect data (Table I) also shows the Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J.,Debehogne, percentage of the light curve observed each night. PAB is the H, and Zeigler, K. (1989). “Photoelectric Observations of Phase Angle Bisector. Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. Period analysis was carried out using the “Peranso” software Vanmunster, T. (2006). Peranso ver 2.0. http://www.peranso.com (Vanmunster 2006). Various routines available in Peranso were utilised, including the “FALC” routine based on Harris et al (1989). Due to the noisy lightcurve and the relatively short observing span, a definitive period was not obvious. The derived period appears to be the best fit to the data, but other periods at 12.7 and 9.5 hours cannot be ruled out entirely. The final analysis UT Date PAB PAB Phase %Phase determined a period of 6.3227 ± 0.0037 hr which was used to Long Lat Angle Coverage 2006 Oct 26 32.6 -25.6 15.8 38 compile the composite light curve with the arbitrary zero phase 2006 Oct 27 32.7 -25.7 15.9 49 maximum at JD 2454034.666 (see Figure 1). The peak to peak 2006 Oct 30 33.0 -25.6 16.0 47 variation in the lightcurve implies an axial ratio (a/b) of 1.32. Full 2006 Nov 09 34.2 -25.4 17.2 110 phase coverage was achieved but the noisy light curve could bear checking. Table I. Aspect data for Karen in 2006. Minor Planet Bulletin 34 (2007) Available on line http://www.minorplanetobserver.com/mpb/default.htm 28 FIRST PERIOD DETERMINATION FOR Finally, we should mention a third possible solution of 9.72 ± 0.01 ASTEROID 1564 SRBIJA hr. This solution has just slightly larger RMS uncertainty than the preceding two, and it does not exhibit the bimodal shape. Maryanne Angliongto and Milan Mijic Interestingly enough, there is only a moderately weak signal at Department of Physics and Astronomy twice the period, but much stronger local minima in the noise California State University, Los Angeles spectrum at three times the period, or 29 hours. We suspect that 5151 State University Dr., Los Angeles, CA 90032 this solution is likely an alias, but we cannot be certain of that. [email protected], [email protected] More data is needed to verify these findings. For now, we may (Received: 2 December) adopt the 29.64 ± 0.02 hr as the tentative value for the period. This lightcurve is displayed in Figure 1. The estimated amplitude is 0.38 ± 0.02 mag, consistent for all three solutions. Lightcurve measurement of 1564 Srbija performed April – June 2006 yielded a tentative synodic rotation period Acknowledgements of 29.64 ± 0.02 hr. We would like to thank Jim Young and Ron Wodaski for their assistance during the observing sessions at TMO and BBO, Our observations of 1564 Srbija were carried out at three respectively, and Brian Warner for his helpful and timely locations: 3 nights at JPL Table Mountain Observatory (TMO) in responses to questions related to Canopus. Wrightwood, CA; 4 nights at Blackbird Observatory (BBO) in Cloudcroft, NM; and 2 nights at El Dorado Hills Observatory References (EDHO) in El Dorado Hills, CA. In total, we had 15 sessions with 95 data points. The table shows the observation dates for each Harris, A. W., Young, J. W., Bowell, E., Martin, L. J., Millis, observatory, equipment used, bands measured, and range of R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J., observed phase angle. All images were dark subtracted and flat- Debehogne, H., and Zeigler, K. W. (1989). “Photoelectric fielded before measuring using MPO Canopus by Bdw Publishing. Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. We used MPO Canopus for differential aperture photometry of all images. Data were corrected by light travel time from the asteroid to the Earth, and times are for mid-exposure. Adjustments were made to the differential magnitudes in order to eliminate causes of magnitude fluctuation not related to the rotation, such as changing observing conditions and phase angle between nights. We also used Canopus to determine the period, using a Fourier analysis routine written by Alan Harris (1989). At the time of observation, the asteroid was of magnitude 16.5- 17.3, and it was a few months after opposition, setting by midnight or earlier. It was a particularly difficult target for the 0.3m EDHO telescope with the resulting low signal causing an excessively large magnitude error. The minimal proper motion of the asteroid on May 26 enabled us to increase the signal by adding consecutive images in groups of three, thus decreasing the error. We could not use this technique with the June 26 EDHO data, so we did not include them in the period determination. This brings our data set down to 85 points, with only slight changes in values for the period, but within the formal uncertainty of the harmonic analysis. The value of 29.64 ± 0.02 hr emerged as the preferred rotation Figure 1. The lightcurve of 1564 Srbija phased to a period of period, characterized by the classical bimodal shape of the 29.64 hrs. lightcurve, low RMS deviation between observed and modeled magnitudes, and strong signal at half-period of 14.79 ±0.01 hours. The next strongest period candidate is 18.29 ± 0.01 hr. The secondary minimum appears to be much shallower, but we cannot be certain of that since our data coverage is very sparse in that region. This solution also has a moderately strong signal at half the period. Dates (2006) Location Telescope Camera Band Phase Angle April 25, May 3, 17 TMO 0.6m f/16 1024x1024 24µm B,V,R 6.3 - 11.6 May 25, 27, 29, 30 BBO 0.5m f/8.3 R-C SBIG STL-11000 C,Red 12.9 - 13.7 May 26, June 26 EDHO 0.3m LX200 f/4 SBIG ST-7 R 13.1 - 15.6 Table 1. Minor Planet Bulletin 34 (2007) 29 LIGHTCURVE OF MINOR PLANET 2006RZ photometric studies. Thanks also to Ellen Howell and Mike Nolan at Arecibo Observatory for their assistance and openness. Gary A. Vander Haagen Stonegate Observatory References 825 Stonegate Road, Ann Arbor, MI 48103 [email protected] Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, (Received: 16 November) H., and Zeigler, K.W., (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. Analysis of lightcurves of 2006 RZ spanning 10 days Nolan, M., (2006). “Scheduled Arecibo Radar Asteroid from September 25, 2006 through October 4, 2006 with Observations, Future Observations”. http://www.naic.edu/ 973 data points produced an indeterminate rotation ~pradar/sched.shtml period. The most prominent periods were 4.967 hrs and 5.540 hrs with an amplitude of 0.20 ± 0.04 mag. Vannmunster, T. (2006), Peranso Period Analysis Software, Astrometric data was also submitted to the Minor Planet Peranso version 2.10, CBABelgium, http://users.skynet.be/ Center for the same time period. fa079980/peranso/index.htm Warner, B.D. (2006). MPO Software, Canopus version 9.2.0.0, Minor Planet 2006 RZ was listed as a radar target for Arecibo Bdw Publishing, http://minorplanetobserver.com/ (Nolan 2006) requesting astrometric and photometric data prior to the targeting dates of October 1, 7, and 9, 2006. Astrometric and photometric data were collected using a 36 cm Celestron C-14, a SBIG ST-10XME camera, and clear filter at Stonegate Observatory. The image scale was 1.4 arc-seconds per pixel and camera temperature held at –15C for all measurements. All images were collected unguided. Data were collected on every available clear night from September 25 through October 4, 2006, resulting in 9 data sets. 2006 RZ ranged from 2 arc-second/minute sky motion and 17th mag.
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