First optical detection from the supernova remnant G 15.1-1.6

TL;DR

This study presents the first optical detection of supernova remnant G 15.1-1.6, revealing filamentary shock-heated gas structures and correlating optical, radio, and infrared emissions, with estimates of shock velocities and remnant distance.

Contribution

First optical imaging and spectroscopic analysis of G 15.1-1.6, identifying shock-heated filaments and correlating multi-wavelength data to characterize the remnant.

Findings

Optical filaments correlate with radio emission.

Shock velocities estimated at ~100 km/s.

Distance to remnant estimated at ≥2.2 kpc.

Abstract

Deep optical CCD images of the supernova remnant G 15.1-1.6 were obtained and filamentary and diffuse emission has been discovered. The images, taken in the emission lines of Halpha+[N II], [S II] and [O III], reveal filamentary and diffuse structures all around the remnant. The radio emission at 4850 MHz in the same area is found to be well correlated with the brightest optical filaments. The IRAS 60 micron emission may also be correlated with the optical emission but to a lesser extent. The flux calibrated images suggest that the optical emission originates from shock-heated gas ([S II]/Halpha > 0.4), while there is a possible HII region ([S II]/Halpha ~0.3) contaminating the supernova remnant's emission to the east. Furthermore, deep long-slit spectra were taken at two bright filaments and also show that the emission originates from shock heated gas. An [O III] filamentary structure has also been detected further to the west but it lies outside the remnant's boundaries and possibly is not associated to it. The [O III] flux suggests shock velocities into the interstellar "clouds" ~100 km/s, while the [S II] 6716/6731 ratio indicates electron densities up to ~250 cm^{-3}. Finally, the Halpha emission has been measured to be between 2 to 7 x 10^{-16} erg/s/cm^2/arcsec^2, while the lower limit to the distance is estimated at 2.2 kpc.