Detections of X-ray emissions from Type Ia Supernova 2003lx

TL;DR

This study reports the detection of X-ray emissions from supernova 2003lx, providing insights into the progenitor system's mass-loss history and the interaction between supernova debris and circumstellar medium.

Contribution

First X-ray detection of supernova 2003lx, revealing details about the progenitor's mass-loss rate and shock temperature, advancing understanding of supernova remnants.

Findings

X-ray luminosity estimated at 4.8 x 10^{41} erg/s

Shock temperature around 0.4 keV

Mass-loss rate of companion star ~10^{-4} M_sun/year

Abstract

We present a study of a young (few years old) supernova remnant 2003lx which was first discovered in X-ray through two serendipitous Swift observations in 2008 January and the corresponding merged image revealed a 7\sigma source detection at $2.1\pm1.2$ arcsec (0.9 +/- 0.5 Swift pixels) from the optical position of the supernova. The X-ray luminosity $L_x = 4.8_{-1.7}^{+1.8} \times 10^{41} erg/s of band 0.3 - 2.0 keV is estimated by a redshift z = 0.0377 power law which can infer a companion star with a mass-loss rate of \dot{M} ~ 10^{-4} M_\sun per year (with assumption of wind velocity v_w = 10 km/s) in the white dwarf binary system. Thermal Model fitting suggests the temperature of the shock wave front is kT ~ 0.4 keV which is consistent with the typical reverse shock temperate. The X-ray emission allows us to probe the interaction between the fast moving debris of the exploded star and the circumstellar medium (CSM). This in turns provides footprints of the mass-loss history of the exploded system, and may allow us to learn about the nature of the progenitor and its companion.