DPS 2001 meeting, November 2001
Session 20. Comet Posters
Displayed, 9:00am Tuesday - 3:00pm Saturday, Highlighted, Wednesday, November 28, 2001, 10:30am-12:30pm, French Market Exhibit Hall

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[20.03] CCD Spectroscopy and Photometry of the DS1 Flyby Target P/Borrelly.

M. D. Hicks, B.J. Buratti (JPL/Caltech), D. Esqueda, E. Ha (CalState LA), R.P. Pass III (Draper Labortory)

In support of the Deep Space 1 encounter with the comet P/Borrelly on Sep 23 2001, we have been engaged in a vigorous campaign of ground-based observations on telescopes ranging in aperture from 10 inches (for rough R-magnitudes) to 200 (for medium resolution spectrophotometry). We present our preliminary analysis and discuss our results in the context of the successful DS1 flyby.

On the nights of July 26 and Sep 16-17 we obtained long-slit spectrograms of the comet at the Palomar 200-inch using the facility ``Double Spec'' with a resolution of ~3 angstrom and a wavelength range between ~0.38 and 0.90 micron. We can compute the production rates of H2O, CN, C2, C3, and NH2. We shall compare the production rate ratios of Borrelly to values obtained in previous apparitions and to the ensemble of comets.

Our broad-band photometry of the coma began ias soon as the comet was availible from our latitude in early July and continued until a few days before encounter. The R-band magnitudes where converted to a dust production rate through the Afrho formalism. The astrometry was reduced and submitted to to MPC and the JPL Solar System Dynamics group throughout the apparition. The astrometry obtained at the P200 on Sep 16 proved especially helpful to mission planners, due to its high spatial resolution and nearly perpendicular point of view from the DS1 line of sight. The photometric data was collected by an ecclectic mix of professionals, undergraduate students, and a dedicated amatuer observer.

This work was funded by NASA, with the stipend for the student observers coming from the NASA/NSF CURE program.

The author(s) of this abstract have provided an email address for comments about the abstract: hicksm@galah.jpl.nasa.gov

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