Far-Ultraviolet Cooling Features of the Antlia Supernova Remnant

TL;DR

This study uses far-ultraviolet observations to analyze the emission features of the Antlia supernova remnant, revealing insights into its structure and the processes occurring within it.

Contribution

It provides the first detailed far-ultraviolet spectral analysis of the Antlia supernova remnant, highlighting the distribution of emission lines and their implications for remnant morphology.

Findings

C IV emission is clumpy and nearly constant with radius.

C III emission varies radially, peaking at half the radius.

Edge regions show increased C IV to C III ratio, indicating evaporating cloudlets.

Abstract

We present far-ultraviolet observations of the Antlia supernova remnant obtained with Far-ultraviolet IMaging Spectrograph (FIMS, also called SPEAR). The strongest lines observed are C IV 1548,1551 and C III 977. The C IV emission of this mixed-morphology supernova remnant shows a clumpy distribution, and the line intensity is nearly constant with radius. The C III 977 line, though too weak to be mapped over the whole remnant, is shown to vary radially. The line intensity peaks at about half the radius, and drops at the edge of the remnant. Both the clumpy distribution of C IV and the rise in the C IV to C III ratio towards the edge suggest that central emission is from evaporating cloudlets rather than thermal conduction in a more uniform, dense medium.