# Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-Collapse Supernova Remnant G292.0+1.8

## TL;DR

This study provides detailed high-resolution X-ray maps of the shocked ejecta and circumstellar medium in the supernova remnant G292.0+1.8, revealing the distribution of elements and insights into the explosion dynamics.

## Contribution

First Chandra detection of Fe-rich ejecta and detailed spatial mapping of element distributions in G292.0+1.8, enhancing understanding of supernova explosion asymmetries.

## Key findings

- Fe-rich ejecta detected for the first time in G292.
- Ejecta enriched in O, Ne, Mg, Si, S, Fe mapped spatially.
- Ejecta distribution suggests asymmetric explosion and pulsar kick origin.

## Abstract

G292.0+1.8 (G292) is a young ($\sim$3000 yr), Galactic textbook-type core-collapse supernova remnant (CCSNR). It is characterized by X-ray, optical and infrared emission from ejecta and circumstellar medium (CSM) features, and contains a pulsar (PSR J1124-5916) and pulsar wind nebula that have been observed in X-rays and radio. Previous studies have revealed a complex, dynamically evolving, oxygen-rich remnant, a striking relic from the explosion of a massive star. Here, using our deep (530 ks) $\textit{Chandra}$ ACIS data, we present high spatial-resolution maps (based on a regional grid size of a few arcsec) of the shocked CSM and metal-rich ejecta in G292. We make the first $\textit{Chandra}$-detection of Fe-rich ejecta in G292. We identify the X-ray counterpart of the northern equatorial belt, a component of a ring-like CSM structure identified earlier in the infrared band. We show the detailed spatial distributions of ejecta enriched in O, Ne, Mg, Si, S and Fe. We find that the bulk of the Si, S and Fe-rich X-ray-emitting ejecta are located in the northwestern hemisphere of the remnant, opposite to the pulsar's projected angular displacement to the southeast from the SNR's center. This suggests that the pulsar's kick may have originated from gravitational and hydrodynamic forces during an asymmetric explosion, rather than from anisotropic neutrino emission. Based on abundance ratios and our estimated CSM and ejecta masses, we constrain the progenitor mass to 13 M$_{\odot}$ $\lesssim$ M $\lesssim$ 30 M$_{\odot}$