High resolution infrared spectroscopy of comet 2P/Encke: Application to future observations of comets 9P/Tempel 1 and 21P/Giacobini-Zinner.

Details High resolution infrared spectroscopy of comet 2P/Encke: Application to future observations of comets 9P/Tempel 1 and 21P/Giacobini-Zinner. High resolution infrared spectroscopy of comet 2P/Encke: Application to future observations of comets 9P/Tempel 1 and 21P/Giacobini-Zinner.

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004dps....36.2309d&link_type=abstract

American Astronomical Society, DPS meeting #36, #23.09; Bulletin of the American Astronomical Society, Vol. 36, p.1122

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Observations of comets with ground-based high-resolution infrared spectroscopy have retrieved a wealth of information on volatile abundances in bright long-period comets, but have achieved only limited success in characterizing the chemistry of fainter short-period comets. Recent advances in ground-based instrumentation, such as the high-resolution cross-dispersed NIRSPEC spectrometer at the Keck 2 Observatory, have permitted the in-depth study of fainter comets. We present volatile production rates and relative abundances for several molecules in comet 2P/Encke on three dates (UT November 4.3, 5.3, and 6.3, 2003) using NIRSPEC. Analysis of ro-vibrational lines of H2O and HCN suggest low gas rotational temperatures ( ˜ 20-30 K) on these dates.
Observations of 2P/Encke with NIRSPEC yielded molecular lines with high signal-to-noise ratios. These data were used to assess the feasibility of detecting molecular species in two Jupiter-family comets available in the spring of 2005: 21P/Giacobini-Zinner (G-Z) and 9P/Tempel 1. G-Z is the prototypical C2 depleted comet, and prospects for detecting possible parents C2H2 and C2H6 (as well as other volatile species) will be explored. 9P/Tempel 1 is the target of the Deep Impact Mission. We will discuss prospects for determining pre-impact molecular abundances, and detecting changes in volatile abundances post-impact.
This work was supported by the NASA Planetary Atmospheres and Planetary Astronomy Programs, and the Keck PI Data Analysis Fund.

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