Probing the Shocked and Photoionized Ejecta in the Oxygen-Rich Supernova Remnant G292.0+1.8

Details Probing the Shocked and Photoionized Ejecta in the Oxygen-Rich Supernova Remnant G292.0+1.8 Probing the Shocked and Photoionized Ejecta in the Oxygen-Rich Supernova Remnant G292.0+1.8

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop.3598g&link_type=abstract

Spitzer Proposal ID #3598

Computer Science

Scientific paper

Of the known Galactic supernova remnants, G292.0+1.8 is the only object known to exhibit all the expected characteristics of a core-collapse SN: O-rich X-ray and optical emission from stellar ejecta, a recently discovered active pulsar and associated pulsar wind nebula, and evidence for circumstellar wind interaction. We propose IRS spectroscopy of the bright spur of shocked O-rich ejecta seen in in the optical images of G292.0+1.8 to study the nucleosynthesis products (O,Ne,...,Fe) from both hydrostatic evolution and explosive nucleosynthesis in the massive progenitor star. Recent X-ray observations suggest that only the outermost (hydrostatic product) layers have passed through the reverse shock. However, we have detected [S II] optical emission from the spur in G292.0+1.8 which may have originated in the deeper ejecta layers. The benefit of observations in the mid-IR is that nearly all of the ejecta species produce emission lines in this band, and interstellar extinction is negligible. This makes Spitzer observations the best way to bridge the gap in our understanding between the optical and X-ray results. Comparing our data with the predictions from Type II SN models we can constrain the mass of the progenitor and measure the degree of mixing between different ejecta species, critical information for understanding both the role of core collapse SNe in seeding the ISM with metals and the nature of the supernova explosion itself. We also propose a deep IRS staring observation of the center of G292.0+1.8 to detect Fe VI 19.6 micron emission from unshocked, photoionized iron. The search for Fe emission both here and in the radiative shocks will help constrain the poorly known amount of iron expelled in the SN explosion and the amount contained in the newly formed neutron star.

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