Spectroscopy Survey of Supernova Remnants in the Inner Galaxy

Details Spectroscopy Survey of Supernova Remnants in the Inner Galaxy Spectroscopy Survey of Supernova Remnants in the Inner Galaxy

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sptz.prop30585r&link_type=abstract

Spitzer Proposal ID #30585

Physics

Scientific paper

In the infrared, supernova remnants (SNRs) have recently been found (with GLIMPSE Legacy data covering 95 known SNRs) to comprise three major groups: molecular-line dominated, ionic-line dominated, and PAH-like. Many of the 18 IRAC-detected SNRs show molecular-line colors, indicating interactions with dense gas, for which most of the shock cooling occurs through molecular ro-vibrational lines. Such molecular SNRs have been long expected for Type II supernovae near molecular clouds, but only a few are known. Our understanding of the infrared emission from SNRs is limited with the broad-band IRAC images, because SNRs are line-dominated but with a continuum. Infrared spectroscopy is crucial to understanding physical processes such as shock physics, grain destruction and chemical processes behind strong SN shocks, and metal enrichment in interstellar gas. We propose IRS and MIPS-SED observations of 14 IRAC-detected SNRs. Our scientific goals are (i) to uncover the nature of the infrared emission of each SNR, (ii) to truly identify the SNRs that are interacting with molecular clouds, by detecting shocked H_2 emission, (iii) to study the excitation rates of H_2 lines, and shock physics, and finally, (iv) to investigate dust destruction and coupling between the dust and gas through the shocks.

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