Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21348806w&link_type=abstract
American Astronomical Society, AAS Meeting #213, #488.06; Bulletin of the American Astronomical Society, Vol. 41, p.463
Astronomy and Astrophysics
Astronomy
Scientific paper
We present results from {\it Spitzer} Cycle 5 IRS observations of 3 young supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). We have obtained complete mapping in the long wavelength, low-resolution modules of 0509-67.5 (0509), 0519-69.0 (0519), and 0509-68.7 (N103B), as well as pointed staring observations with the short wavelength, low-resolution module for knots in N103B. This work follows up on previously published photometric images of these SNRs with {\it Spitzer}. These objects all have ages determined by optical light echoes, and 0509 has recently been confirmed as type Ia from its echo. All 3 objects are detected in IRS, and show a clearly rising continuum which we attribute to warm dust. 0509 and 0519 show no line emission, whereas N103B has lines from Ne and Fe, and evidence for a silicate dust feature around 18 $\mu$m. We use plane-shock dust models which incorporate a distribution of dust grain sizes and relative abundances of silicate and graphite grains relevant to the LMC to model observed continuum. Dust models depend on these parameters as well as plasma temperature, remnant age, and density. We include effects of thermal sputtering of grains, including enhancements of sputtering for small grains. We use information about these remnants derived from both optical and X-ray studies to determine relevant parameters, regarding plasma density as a free parameter. Post-shock density in 0519 is $\sim 18$ cm$^{-3}$. For 0509, spectral differences resulting from different dust temperatures can be seen between the brigther half and fainter half of the remnant. This implies a density gradient in the pre-shock gas. Our inferred densities are $\sim 4$ and $\sim 0.75$ cm$^{-3}$ for the bright and faint parts, respectively. These densities are in reasonable agreement with recent hydrodynamic modeling of the X-ray spectrum by Badenes et al. (2008, ApJ, 680, 1149)
Blair William Patrick
Borkowski Kazimierz J.
Ghavamian Parviz
Hendrick Sean Patrick
Long Knox S.
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