# A Detailed Archival CHANDRA Study of the Young Core-Collapse Supernova Remnant 1E 0102.2-7219 in the Small Magellanic Cloud

## TL;DR

This study uses deep archival Chandra data to analyze the spatial and chemical structure of the supernova remnant 1E 0102.2-7219, revealing detailed ejecta distribution, abundance ratios, and insights into its explosion and progenitor.

## Contribution

It provides the first detailed spatially resolved spectral analysis of 1E 0102.2-7219, revealing asymmetries in ejecta distribution and constraining the remnant's age, energy, and progenitor characteristics.

## Key findings

- Ejecta extend further in west and southwest directions.
- Abundance ratios suggest a 40 solar mass progenitor.
- Estimated age of the remnant is up to 3500 years.

## Abstract

We present an archival Chandra study of the O-rich supernova remnant (SNR) 1E 0102.2-7219 in the Small Magellanic Cloud. Based on the deep $\sim$ 265 ks archival Chandra data we performed a detailed spatially resolved spectral analysis of 1E 0102.2-7219. Our aim is to reveal the spatial and chemical structures of this remnant in unprecedented details. Radial profiles of O, Ne and Mg abundances based on our analysis of regional spectra extracted along nine different azimuthal directions of 1E 0102.2-7219 suggest the contact discontinuity at $\sim$ 5-5.5 pc from the geometric center of the X-ray emission of the SNR. We find that the metal-rich ejecta gas extends further outward in west and southwest than in other directions of the SNR. The average O/Ne, O/Mg and Ne/Mg abundance ratios of the ejecta are in plausible agreement with the nucleosynthesis products from the explosion of a $\sim 40 M_\odot$ progenitor. We estimate an upper limit on the Sedov age of $\sim 3500$ yr and explosion energy of $\sim 1.8\times10^{51}$ erg for 1E 0102.2-7219. We discuss the implications of our results on the geometrical structure of the remnant, its circumstellar medium and the nature of the progenitor star. Our results do not fit with a simple picture of the reverse-shocked emission from a spherical shell-like ejecta gas with a uniformly-distributed metal abundance and a power-law density along the radius of the SNR.