Post-Perihelion HST Observations of Comet Hale-Bopp

Details Post-Perihelion HST Observations of Comet Hale-Bopp Post-Perihelion HST Observations of Comet Hale-Bopp

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...191.8802w&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #88.02; Bulletin of the American Astronomical Society, Vol. 29, p.1356

Astronomy and Astrophysics

Astronomy

Scientific paper

Observations of comet Hale-Bopp with HST resumed on 27 Aug 1997 (at r=2.476 AU and Delta =2.989 AU) following a 10 month hiatus during which time the comet was in the HST solar avoidance zone. The observations executed flawlessly using the newly-installed Space Telescope Imaging Spectrograph (STIS). The STIS CCD was used to image the comet, and useful spectroscopy was performed between 2100-3190 Angstroms using the G230LB and G230MB gratings. The morphology of the images closely resembled that obtained at similar heliocentric distances pre-perihelion (i.e., ``porcupine'' appearance), but the dust production rate was slightly lower post-perihelion. From the observed emission in the OH(0,0) band, we derived a preliminary value for the water production rate of ~ 3 x 10(29) molecules s(-1) , which is comparable to the pre-perihelion value. The 2-dim nature of the STIS data allowed us to map the spatial distribution of the OH emission, and the ~ 6 Angstroms resolution of the G230MB grating permits a detailed examination of the OH excitation. Preliminary analysis indicates that a conventional vectorial model can reproduce the observed OH spatial distribution. Emissions from CS and the OH(1,0) band were observed in the G230LB data. The next HST observations of Hale-Bopp are scheduled for Nov 1997, and the final observations in our program will probably take place in mid-Feb 1998.

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