Observations of the Shoemaker-Levy 9 L Impact from Palomar

Details Observations of the Shoemaker-Levy 9 L Impact from Palomar Observations of the Shoemaker-Levy 9 L Impact from Palomar

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.2243m&link_type=abstract

American Astronomical Society, DPS meeting #28, #22.43; Bulletin of the American Astronomical Society, Vol. 28, p.1149

Astronomy and Astrophysics

Astronomy

Scientific paper

We present observations taken with SpectroCam-10, a mid-infrared imaging spectrometer mounted on the 200-inch Hale telescope at Palomar, of the Shoemaker-Levy 9 L impact site on its first jovian rotation. While conditions were cloudy and we did not observe continuously throughout the L impact, we did obtain images at several cloud-free times, with filters centered at 4.5 mu m, 7.9 mu m, 8.8 mu m and 10.3 mu m. Low resolution ({lambda /{bigtriangleup lambda }}~ 100) spectra in the 8-14 mu m region were obtained ~ 25 and ~ 85 minutes after the L impact. A broad emission feature from 8.0-11.5 mu m in both spectra is interpreted as warm silicate emission similar to that seen from Palomar after the R impact [Nicholson et al., GRL 22, 1617 (1995)]. A fit using the standard Draine & Lee [Ap. J. 285, 89 (1984)] silicate dust emissivity indicates optically thin dust with a temperature T~350 K for the first spectrum. A fit to a 2:1 poly-HCN/silicate mixture [Wilson and Sagan, preprint (1996)] does not match this spectrum as well. In our second spectrum, the flux longward of 11.5 mu m is twice that of the silicate model, possibly due to C_2 H_6 emission. Images at 10.3 mu m at t_impact+22, 31, and 77 minutes show the bright oval-shaped L site at high emission angle and ~ 3" in diameter. Those at t_impact+2:22 hrs and at +2:44 hours hours show more clearly the familiar crescent shape of the splashback region. At t_impact+3:41 hours the arc is still present, but an unresolved spot appears within it. This ``core'' feature is not seen at 7.9 mu m, which senses stratospheric emission, and we therefore interpret it as emission from deeper (upwelling?) warm gas.

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