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P. A. Taylor, J.-L. Margot, P. D. Nicholson, D. B. Campbell (Cornell University), R. F. Jurgens, S. J. Ostro, L. A. M. Benner, J. D. Giorgini (Jet Propulsion Laboratory), M. C. Nolan, E. S. Howell, A. A. Hine (Arecibo Observatory), C. Magri (University of Maine at Farmington), R. S. Hudson (Washington State University)
We present a preliminary shape model for asteroid 54509 (2000 PH5) using radar data inversion. Our results build upon the dynamical and physical characterization of this object from radar observations made at Goldstone in July 2001 and Arecibo Observatory in July 2004 (Taylor et al., BAAS 36, 2004). We search a grid of spin pole positions to find the optimal shape and spin state of the asteroid based on datasets consisting of 100+ continuous wave spectra, with 0.5 or 1 Hz frequency resolution, and 200+ delay-Doppler images, with 0.5 Hz frequency resolution and range resolutions of 7.5 or 15 meters. We will present our best model for the shape and spin state at the meeting.
By the time of the meeting, we anticipate that our shape model will benefit from observations scheduled for July 2005 with the Arecibo telescope. During the upcoming observations, 2000 PH5 will be more than 50 degrees from its position during the 2004 observations, and the object will move approximately 15 degrees across the sky in three days. Sky motion and different viewing geometries are important factors in resolving the north-south and prograde-retrograde spin pole ambiguities. Including the continuous wave spectra and delay-Doppler images from the July 2005 observations will further constrain both the shape and spin state of asteroid 2000 PH5.
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Bulletin of the American Astronomical Society, 37 #3
© 2004. The American Astronomical Soceity.