An X-Ray Study of Supernova Remnant N49 and Soft Gamma-Ray Repeater 0526-66 in the Large Magellanic Cloud

We report on the results from our deep Chandra observation (120 ks) of the supernova remnant (SNR) N49 and soft gamma-ray repeater (SGR) 0526–66 in the Large Magellanic Cloud. We firmly establish the detection of an ejecta "bullet" beyond the southwestern boundary of N49. The X-ray spectrum of the bullet is distinguished from that of the main SNR shell, showing significantly enhanced Si and S abundances. We also detect an ejecta feature in the eastern shell, which shows metal overabundances similar to those of the bullet. If N49 was produced by a core-collapse explosion of a massive star, the detected Si-rich ejecta may represent explosive O-burning or incomplete Si-burning products from deep interior of the SN. On the other hand, the observed Si/S abundance ratio in the ejecta may favor Type Ia origin for N49. We refine the Sedov age of N49, τ Sed ∼ 4800 yr, with the explosion energy E 0 ∼ 1.8 × 10 51 erg. Our blackbody (BB) + power law (PL) model for the quiescent X-ray emission from SGR 0526–66 indicates that the PL photon index (Γ ∼ 2.5) is identical to that of PSR 1E1048.1–5937, the well-known candidate transition object between anomalous X-ray pulsars and SGRs. Alternatively, the two-component BB model implies X-ray emission from a small ( R ∼ 1 km) hot spot(s) ( kT ∼ 1 keV) in addition to emission from the neutron star's cooler surface ( R ∼ 10 km, kT ∼ 0.4 keV). There is a considerable discrepancy in the estimated column toward 0526–66 between BB+PL and BB+BB model fits. Discriminating these spectral models would be crucial to test the long-debated physical association between N49 and 0526–66.