First optical identification of the SRG/eROSITA-detected supernova remnant G 116.6-26.1 I. Preliminary results

TL;DR

This paper reports the first optical detection of the supernova remnant G 116.6-26.1, confirming its nature through imaging, spectral analysis, and shock diagnostics, and indicating it is a mature SNR at high Galactic latitude.

Contribution

It provides the first optical identification and detailed spectral analysis of G 116.6-26.1, confirming its supernova remnant status and characterizing its shock properties and evolutionary stage.

Findings

Optical filaments match X-ray, radio, and UV maps.

Line ratio [S II]/Hα exceeds 0.4, confirming shock excitation.

Estimated shock velocity is 70-100 km/s.

Abstract

The supernova remnant (SNR) candidate G 116.6-26.1 is one of the few high Galactic latitude ($|b| > 15^o$) remnants detected so far in several wavebands. It was discovered recently in the SRG/eROSITA all-sky X-ray survey and displays also a low-frequency weak radio signature. In this study, we report the first optical detection of G 116.6-26.1 through deep, wide-field and higher resolution narrowband imaging in $\rm H\alpha$, [S II] and [O III] light. The object exhibits two major and distinct filamentary emission structures in a partial shell-like formation. The optical filaments are found in excellent positional match with available X-ray, radio and UV maps, can be traced over a relatively long angular distance (38' and 70') and appear unaffected by any strong interactions with the ambient interstellar medium. We also present a flux-calibrated, optical emission spectrum from a single location, with Balmer and several forbidden lines detected, indicative of emission from shock excitation in a typical evolved SNR. Confirmation of the most likely SNR nature of G 116.6-26.1 is provided from the observed value of the line ratio $\rm [S\, II] / H\alpha = 0.56 \pm 0.06$, which exceeds the widely accepted threshold 0.4, and is further strengthened by the positive outcome of several diagnostic tests for shock emission. Our results indicate an approximate shock velocity range $70-100\, km\, s^{-1}$ at the spectroscopically examined filament, which, when combined with the low emissivity in $\rm H\alpha$ and other emission lines, suggest that G 116.6-26.1 is a SNR at a mature evolutionary stage.