Optical observations of the galactic supernova remnants G59.5+0.1, G84.9+0.5 and G67.7+1.8

Details Optical observations of the galactic supernova remnants G59.5+0.1, G84.9+0.5 and G67.7+1.8 Optical observations of the galactic supernova remnants G59.5+0.1, G84.9+0.5 and G67.7+1.8

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008ap%26ss.318..207g&link_type=abstract

Astrophysics and Space Science, Volume 318, Issue 3-4, pp. 207-214

Astronomy and Astrophysics

Astrophysics

1

Galactic Supernova Remnants: G59.5+0.1, G84.9+0.5, G67.7+1.8, Ccd Image, Longslit Spectra

Scientific paper

We present here the optical CCD observations and long slit spectra of the galactic supernova remnants G59.5+0.1, G84.9+0.5 and G67.7+1.8, the first two being observed for the first time. The observations were carried out with the 1.5 m Russian-Turkish joint Telescope (RTT150) at TÜBİTAK National Observatory (TUG). The images were taken with H α, [SII] and their continuum filters. After subtracting the continuum from H α and [SII], [SII]/H α ratio is obtained. The average ratio is found to be 0.41 for G59.5+0.1 and 0.44 for G84.9+0.5, in a very good agreement with the ratios obtained from the optical spectra, namely 0.46 and 0.40, respectively, indicating that these remnants are close to, or interacting with, HII regions. G59.5+0.1 and G84.9+0.5 remnants show diffuse-shell morphology while G67.7+1.8 shows arc-shell morphology. From the emission lines of the spectra, the electron density N e , pre-shock density n c , explosion energy E, interstellar extinction E(B-V), and neutral hydrogen column density N(HI) are calculated and shock velocity V s is estimated for these remnants.

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