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The supernova remnant (SNR) candidate G 116.6-26.1 is one of the few highGalactic 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 displaysalso a low-frequency weak radio signature. In this study, we report the firstoptical detection of G 116.6-26.1 through deep, wide-field and higherresolution narrowband imaging in $\rm H\alpha$, [S II] and [O III] light. Theobject exhibits two major and distinct filamentary emission structures in apartial shell-like formation. The optical filaments are found in excellentpositional match with available X-ray, radio and UV maps, can be traced over arelatively long angular distance (38' and 70') and appear unaffected by anystrong interactions with the ambient interstellar medium. We also present aflux-calibrated, optical emission spectrum from a single location, with Balmerand several forbidden lines detected, indicative of emission from shockexcitation in a typical evolved SNR. Confirmation of the most likely SNR natureof 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 threshold0.4, and is further strengthened by the positive outcome of several diagnostictests for shock emission. Our results indicate an approximate shock velocityrange $70-100\, km\, s^{-1}$ at the spectroscopically examined filament, which,when combined with the low emissivity in $\rm H\alpha$ and other emissionlines, suggest that G 116.6-26.1 is a SNR at a mature evolutionary stage.

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