The Nature of Shocks in Supernova Remnants 3C 396, Kes 69 and G346.6-0.2 revealed by Spitzer

Details The Nature of Shocks in Supernova Remnants 3C 396, Kes 69 and G346.6-0.2 revealed by Spitzer The Nature of Shocks in Supernova Remnants 3C 396, Kes 69 and G346.6-0.2 revealed by Spitzer

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21111501h&link_type=abstract

American Astronomical Society, AAS Meeting #211, #115.01; Bulletin of the American Astronomical Society, Vol. 39, p.944

Astronomy and Astrophysics

Astronomy

Scientific paper

Infrared emission from interacting supernova remnants is rich in atomic fine-structure and molecular rovibrational lines which allows a detailed characterization of the shock conditions present. With Spitzer IRS and MIPS-SED we have obtained sensitive, high spatial resolution spectroscopy between 5.2 and 95 microns for 14 interacting remnants in the Galactic plane. We present the first detections of collisionally excited molecular hydrogen from three supernova remnants in our survey: 3C 396, Kes 69 and G346.6-0.2. For Kes 69 and G346.6-0.2 bright emission from H2 pure rotational lines and [O I] 63 microns is detected. This confirms a slow, non-dissociative shock interaction with nearby molecular clouds first suggested by nearby OH(1720 MHz) maser detections. In contrast, bright atomic fine-structure lines dominate emission from the shell of 3C 396 giving clear evidence for an ionic shock, though H2 lines are also detected. Interestingly, peak emission from ionic lines appears offset from that of molecular lines demonstrating the variation of physical conditions across the shock front. For these three remnants we analyze the excitation of the observed H2 S(0)-S(7) lines to determine gas temperature and density as well as discriminate between shock models. Evidence for shock processing of dust and PAHs is also considered.

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