2025MNRAS.542..409B

Radio observations have shown that G190.9-2.2 is a barrel-shaped, low surface brightness supernova remnant (SNR), with a large angular size and a shell-type morphology. In this work, we present the first comprehensive optical investigation of the SNR G190.9-2.2, aiming to determine its physical characteristics based on imaging and spectroscopic observations obtained with the 1-m Turkish Telescope (T100) and 1.5-m Russian-Turkish Telescope (RTT150). The H $\alpha$ and [S II] images show sharp, long, and curved filamentary structures within the southern radio shell of the SNR. The presence of forbidden line emission ([O III], [O I], [N II], and [S II]) from the SNR indicates that there is strong cooling behind the shock front. [S II]/H $\alpha$ line ratios measured from both long-slit spectra and imaging analysis support the interpretation that the emission originates from a shock-heated gas. We estimate that the electron density ranges from 17 to 1899 cm$^{-3}$, based on the [S II] $\lambda$6716/$\lambda$6731 line ratio. The [O III] $\lambda$5007/H $\beta$ ratio suggests the presence of relatively slow shocks with velocities $V_{\rm s}$ $\sim$ 80 km s$^{-1}$. Both the optical morphology and the spectra of G190.9-2.2 are consistent with radiative shocks. Significant variations in physical parameters, including electron density, pre-shock density, and extinction, were observed across the studied regions, indicating a highly inhomogeneous ambient medium.