First detailed optical spectroscopic observations of the supernova remnants G107.7-5.1 and G150.3+4.5

TL;DR

This study provides detailed optical spectroscopic analysis of supernova remnants G107.7-5.1 and G150.3+4.5, confirming their shock-excited nature and deriving physical conditions, with implications for their gamma-ray properties.

Contribution

First detailed optical spectroscopic observations of these SNRs, confirming their shock excitation and analyzing their physical conditions with new spectral data.

Findings

Both SNRs are shock-excited with shock velocities >100 km/s.

Spectral line ratios indicate varying electron densities and dust extinction.

Remnants show similar spectral properties and gamma-ray characteristics.

Abstract

We present optical spectroscopic observations of the supernova remnants (SNRs) G107.7$-$5.1 and G150.3+4.5, each spanning nearly 3 degree. Both remnants were recently examined in the optical band through a deep H$\alpha$ and [OIII] emission-line imaging survey, which led to the discovery of G107.7$-$5.1. Using long-slit spectra obtained with the 1.5-m Russian-Turkish Telescope (RTT150), we investigate the physical conditions of the pre-shock and post-shock gas in the optical filamentary regions of the SNRs. The SNR nature of G107.7$-$5.1 is confirmed by the measured [SII]/H$\alpha$ and [NII]/H$\alpha$ ratios, which range from 0.56 to 0.86 and from 0.7 to 1.4, respectively. A similar conclusion is reached for G150.3+4.5, where the observed [SII]/H$\alpha$ (0.43-0.92) and [NII]/H$\alpha$ (0.49-1.29) ratios likewise support a shock-excitation origin. Further confirmation of the shock-excited nature of both SNRs comes from their consistency with recent diagnostic diagrams based on multiple emission-line ratios. The [OIII]/H$\beta$ line ratios measured in both remnants indicate shocks with complete recombination zones and are consistent with shock velocities of $\gtrsim$100 km s$^{-1}$. The electron densities ($n_{\rm e}$), derived from the [SII] $\lambda$6716/$\lambda$6731 line ratios, exhibit substantial variation in the spectra of both SNRs. Additionally, extinction variations observed across the remnants suggest the presence of significant dust structures along the line of sight. We conclude that these two remnants display remarkable similarities across multiple diagnostic spectral properties, consistent with previous reports indicating comparable GeV gamma-ray characteristics.