Spitzer Survey of Magellanic Clouds Supernova Remnants: Dust Content in Core-Collapse Supernovae

Details Spitzer Survey of Magellanic Clouds Supernova Remnants: Dust Content in Core-Collapse Supernovae Spitzer Survey of Magellanic Clouds Supernova Remnants: Dust Content in Core-Collapse Supernovae

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4706w&link_type=abstract

American Astronomical Society Meeting 208, #47.06; Bulletin of the American Astronomical Society, Vol. 38, p.122

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We present further results from a survey of supernova remnants (SNRs) in the Magellanic Clouds using the MIPS instrument on the Spitzer Space Telescope. We have previously analyzed dust content and destruction rates in type Ia SNe; here we present morphological comparisons of several SNRs from core-collapse supernovae at infrared, X-ray (Chandra), and optical (Magellanic Clouds Emission-Line Survey, MCELS) wavelengths. Because infrared emission in SNRs is dominated by thermal emission from dust grains collisionally heated by the X-ray-emitting plasma, we can predict emission from these dust grains using parameters fixed by X-ray modeling. This combined X-ray-IR analysis provides diagnostics on plasma conditions that neither could provide on its own. Infrared flux ratios can set limits on plasma conditions, such as post-shock density, while also providing estimates of the total dust mass. We provide such an analysis here for several core-collapse SNRs. We use plane-shock models to describe the X-ray-emitting plasma, and compare observed IR color ratios to those predicted by models that incorporate a distribution of dust grain sizes and relative abundances of silicate and graphite dust grains. Since X-ray analysis also provides estimates for the total amount of gas that has been swept up by the blast wave, we also provide values for the dust-to-gas mass ratio in these remnants. Preliminary results on three of these remnants are as follows. We report total dust masses of 0.031, 0.2, and 0.022 $M_\odot$ and dust/gas ratios of 2.3$\times 10^{-4}$, 1.1$\times 10^{-3}$, and 6.4$\times 10^{-4}$ for N132D, N49B and N23, respectively. We see no dust clearly associated with ejecta. In every case we have analyzed thus far, including our earlier analysis of four type Ia remnants, we see less dust than is expected based on typically assumed global dust/gas mass ratios for the LMC. We will explore possibilities for this discrepancy.

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