A deep Chandra observation of oxygen-rich supernova remnant B0049-73.6 in the Small Magellanic cloud

Andrew Schenck, Sangwook Park, David N. Burrows, John P. Hughes, Jae Joon Lee, Koji Mori

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Abstract

We report on the initial results from our deep Chandra observation (450 ks) of O-rich supernova remnant (SNR) B0049-73.6 in the Small Magellanic Cloud. We detect small metal-rich ejecta features extending out to the outermost boundary of B0049-73.6, which were not seen in the previous data with a shorter exposure. The central nebula is dominated by emission from reverse-shocked ejecta material enriched in O, Ne, Mg, and Si. O-rich ejecta distribution is relatively smooth throughout the central nebula. In contrast, the Si-rich material is highly structured. These results suggest that B0049-73.6 was produced by an asymmetric core-collapse explosion of a massive star. The estimated abundance ratios among these ejecta elements are in plausible agreement with the nucleosynthesis products from the explosion of a 13-15 M progenitor. The central ring-like (in projection) ejecta nebula extends to ∼9 pc from the SNR center. This suggests that the contact discontinuity may be located at a further distance from the SNR center than the previous estimate. We estimate the Sedov age of ∼17,000 yr and an explosion energy of E 0 ∼1.7 × 1051 erg for B0049-73.6. We place a stringent upper limit on the 2-7 keV band luminosity of LX ∼ 8.5 × 1031 erg s-1 for the embedded compact stellar remnant at the center of B0049-73.6.

Original languageEnglish (US)
Article number50
JournalAstrophysical Journal
Volume791
Issue number1
DOIs
StatePublished - Aug 10 2014

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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