Imaging and spectroscopy of the faint remnant G 114.30.3

¹ University of Crete, Physics Department, PO Box 2208, 710 03 Heraklion, Crete, Greece
² Foundation for Research and Technology-Hellas, PO Box 1527, 711 10 Heraklion, Crete, Greece

Corresponding author: F. Mavromatakis, fotis@physics.uoc.gr

Received: 14 November 2001
Accepted: 18 December 2001

Abstract

We present the first calibrated CCD images of the faint supernova remnant G 114.3+0.3 in the emission lines of [ ], [ ], H ] and [ ]. The deep low ionization CCD images reveal diffuse emission in the south and central areas of the remnant. These are correlated with areas of intense radio emission, while estimates of the [ ]/Hα ratio suggest that the detected emission originates from shock heated gas. In the medium ionization image of [ ] we discovered a thin filament in the south matching very well the outer radio contours. This filament is not continuous over its total extent but shows variations in the intensity, mainly in the south–west, suggesting inhomogeneous interstellar clouds. Deep long–slit spectra were also taken along the [ ] filament clearly identifying the observed emission as emission from shock heated gas. The Hα emission is a few times 10^-17 erg s^-1 cm^-2 arcsec^-2, while the variations seen in the [ ] flux suggest shock velocities into the interstellar clouds around or below 100 km s^-1. The sulfur line ratio approaches the low density limit, implying electron densities less than ~500 cm^-3.