Discovery of optical emission associated with the supernova remnant G107.5-1.5

TL;DR

This study reports the first optical imaging and spectroscopic detection of emission from supernova remnant G107.5-1.5, revealing shock-heated gas and ionized regions with varying densities.

Contribution

First optical detection and analysis of emission from SNR G107.5-1.5, identifying shock-heated and ionized gas regions with detailed spectroscopic measurements.

Findings

Optical diffuse and filamentary emission detected from G107.5-1.5.

Shock-heated gas confirmed by [SII]/Hα ratios > 0.5.

Electron densities estimated at ~2400 cm$^{-3}$ in dense regions.

Abstract

We present the first results from an imaging and a spectroscopic survey of the optical emission associated with supernova remnant (SNR) G107.5$-$1.5. We discovered optical diffuse and filamentary emission from G107.5$-$1.5 using the 1.5-m and 1-m telescopes. The optical emission from the North East (NE) and North West (NW) regions show the diffuse structure, while the South East (SE) and East (E) regions show filamentary structure. From long-slit spectra, we found [SII]/H$\alpha$ $>$ 0.5 for the SE and E regions, which supports the origin of the emission being from shock-heated gas. The average [SII]/H$\alpha$ ratio is found to be $\sim$0.4 and $\sim$0.3 for the NW and NE regions, respectively, indicating that the optical emission is coming from ionized gas in an HII region. From the ratios of [SII]$\lambda\lambda$ 6716/6731, we estimate an average electron density of $\sim$2400 cm$^{-3}$ for the NW region, which can be attributed to the dense ionized gas. The average [SII]$\lambda\lambda$ 6716/6731 ratios are $\sim$1.25 and $\sim$1.15 for the SE and E regions, respectively, which are indicative of low electron density.