X-ray Emission from Strongly Asymmetric Circumstellar Material in the Remnant of Kepler's Supernova

TL;DR

This study uses X-ray and infrared observations combined with hydrodynamic simulations to analyze the asymmetric circumstellar material in Kepler's supernova remnant, revealing a disk-like distribution likely from a binary system with an AGB star.

Contribution

The paper introduces a statistical technique to isolate CSM X-ray emission and presents hydrodynamic simulations supporting a disk-shaped CSM distribution in Kepler's supernova remnant.

Findings

CSM distribution aligns with 24 μm infrared emission.

Evidence suggests a disk-like CSM distribution in the remnant.

Kepler's supernova originated from a binary system with an AGB star.

Abstract

Kepler's supernova remnant resulted from a thermonuclear explosion, but is interacting with circumstellar material (CSM) lost from the progenitor system. We describe a statistical technique for isolating X-ray emission due to CSM from that due to shocked ejecta. Shocked CSM coincides well in position with 24 $\mu$m emission seen by {\sl Spitzer}. We find most CSM to be distributed along the bright north rim, but substantial concentrations are also found projected against the center of the remnant, roughly along a diameter with position angle $\sim 100^\circ$. We interpret this as evidence for a disk distribution of CSM before the SN, with the line of sight to the observer roughly in the disk plane. We present 2-D hydrodynamic simulations of this scenario, in qualitative agreement with the observed CSM morphology. Our observations require Kepler to have originated in a close binary system with an AGB star companion.