Optical Emission Associated with the Galactic Supernova Remnant G179.0+2.6

TL;DR

This study presents optical imaging and spectroscopy of the large Galactic supernova remnant G179.0+2.6, revealing dominant [O III] emission indicative of shock velocities above 100 km/s and unusual properties for an old remnant.

Contribution

First detailed optical emission analysis of G179.0+2.6 showing high [O III]/H-alpha ratios and shock velocities, expanding understanding of its physical state and properties.

Findings

Dominant [O III] emission indicates shock velocities >100 km/s.

High [O III]/H-alpha ratio suggests low-density ambient ISM.

Remnant exhibits properties similar to young supernova remnants.

Abstract

Narrow passband optical images of the large Galactic supernova remnant G179.0+2.6 reveal a faint but nearly complete emission shell dominated by strong [O III] 4959,5007 A line emission. The remnant's optical emission, which consists of both diffuse and filamentary features, is brightest along its southern and northeastern limbs. Deep H-alpha images detect little coincidence emission indicating an unusually high [O III]/H-alpha emission ratio for such a large and apparently old remnant. Low-dispersion optical spectra of several regions confirm large [O III]/H-alpha line ratios with typical values around 10. The dominance of [O III] emission for the majority of the remnant's optical filaments suggests shock velocities above 100 km/s are present throughout most of the remnant, likely reflecting a relatively low density ambient ISM. The remnant's unusually strong [O III] emission adds to the remnant's interesting set of properties which include a thick radio emission shell, radial polarization of its radio emission like that typically seen in young supernova remnants, and an unusually slow-rotating gamma-ray pulsar with a characteristic spin-down age ~50 kyr.