Indications of a Si-rich bilateral jet of ejecta in the Vela SNR observed with XMM-Newton

TL;DR

This study identifies a Si-rich bilateral jet of ejecta in the Vela supernova remnant, revealing a jet-counterjet structure similar to Cas A, based on detailed XMM-Newton X-ray observations of ejecta fragments.

Contribution

It provides the first evidence of a Si-rich jet-counterjet structure in the Vela SNR, indicating deeper-layer ejecta and jet-like explosion features.

Findings

Identification of a Si-rich ejecta fragment with a bowshock shape.

Detection of a symmetric Si-rich fragment opposite to the first, suggesting a jet-counterjet structure.

Similarity of the structure to the Cas A remnant's jet features.

Abstract

The Vela supernova remnant displays several ejecta, which are fragment-like features protruding beyond the front of its primary blast shock wave. They appear to be "shrapnel", bowshock-shaped relics of the supernova explosion. One of these pieces of shrapnel (A), located in the northeastern edge of the remnant, is peculiar because its X-ray spectrum exhibits a high Si abundance, in contrast to the other observed ejecta fragments, which show enhanced O, Ne, and Mg abundances. We present the analysis of another fragment located opposite to shrapnel A with respect to the center of the shell, in the southwestern boundary of the remnant, named shrapnel G. We thoroughly analyzed a dedicated XMM-Newton observation of shrapnel G by producing background-subtracted and exposure-corrected maps in different energy ranges, which we complemented with a spatially resolved spectral analysis of the X-ray emission. The fragment presents a bowshock-like shape with its anti-apex pointing to the center of the remnant. Its X-ray spectrum is best fit by a thermal plasma out of equilibrium of ionization with low O and Fe, roughly solar Ne and Mg, and a significantly high Si abundance, which is required to fit a very clear Si line at ~1.85 keV. Its chemical composition and spectral properties are compatible with those of shrapnel A, which is located on the opposite side of the remnant. As a consequence of the nucleosynthesis, pieces of Si-rich shrapnel are expected to originate in deeper layers of the progenitor star compared to ejecta with lower-Z elements. A high velocity and density contrast with respect to the surrounding ejecta are necessary to make shrapnel A and G overtake the forward shock. The line connecting shrapnel A and G crosses almost exactly the expansion center of the remnant, strongly suggesting a Si-rich jet-counterjet structure, reminiscent of that observed in the young remnant Cas A.