XMM-Newton Large Program on SN1006 - II: Thermal Emission

TL;DR

This study uses advanced spatially resolved X-ray spectroscopy to analyze the thermal emission of SN1006, revealing detailed distributions of elements, ionization states, and evidence for asymmetric explosion and ejecta heating processes.

Contribution

It introduces improved spectral analysis tools and provides detailed spatial mapping of thermal emission, ejecta composition, and ionization in SN1006, highlighting asymmetries and element origins.

Findings

Different elements have distinct spatial distributions.

Fe-rich ejecta is confined to a small shell-like region.

Ejecta patterns suggest an asymmetric explosion.

Abstract

Based on the XMM-Newton large program on SN1006 and our newly developed spatially resolved spectroscopy tools (Paper~I), we study the thermal emission from ISM and ejecta of SN1006 by analyzing the spectra extracted from 583 tessellated regions dominated by thermal emission. With some key improvements in spectral analysis as compared to Paper~I, we obtain much better spectral fitting results with less residuals. The spatial distributions of the thermal and ionization states of the ISM and ejecta show different features, which are consistent with a scenario that the ISM (ejecta) is heated and ionized by the forward (reverse) shock propagating outward (inward). Different elements have different spatial distributions and origins, with Ne mostly from the ISM, Si and S from the ejecta, and O and Mg from both ISM and ejecta. Fe L-shell lines are only detected in a small shell-like region SE to the center of SN1006, indicating that most of the Fe-rich ejecta has not yet or just recently been reached by the reverse shock. The overall ejecta abundance patterns for most of the heavy elements, except for Fe and sometimes S, are consistent with typical Type~Ia SN products. The NW half of the SNR interior probably represents a region with turbulently mixed ISM and ejecta, so has enhanced emission from O, Mg, Si, S, lower ejecta temperature, and a large diversity of ionization age. In addition to the asymmetric ISM distribution, an asymmetric explosion of the progenitor star is also needed to explain the asymmetric ejecta distribution.