A Deep Chandra Observation of Oxygen-Rich Supernova Remnant B0049-73.6 in the Small Magellanic Cloud

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$M_{\odot }$ progenitor. The central ring-like (in projection) ejecta nebula extends to $\sim$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 $\sim$17000 yr and an explosion energy of $E_0$ $\sim 1.7\times 10^{51}$ erg for B0049-73.6. We place a stringent upper limit on the 2-7 keV band luminosity of $L_X\sim$ 8.5 $\times 10^{31}$ erg s${}^{-1}$ for the embedded compact stellar remnant at the center of B0049-73.6.

10 pages (ApJ emulator style), 2 tables, 4 figures, Accepted by ApJ

References in corpus (2)

• A Physical Relationship Between Electron-Proton Temperature Equilibration and Mach Number in Fast Collisionless Shocks
• A Half-Megasecond Chandra Observation of the Oxygen-Rich Supernova Remnant G292.0+1.8

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