EDP Sciences
Free access
Volume 388, Number 1, June II 2002
Page(s) 355 - 362
Section Diffuse matter in space
DOI http://dx.doi.org/10.1051/0004-6361:20020511

A&A 388, 355-362 (2002)
DOI: 10.1051/0004-6361:20020511

Deep optical observations of G 65.3+5.7

F. Mavromatakis1, P. Boumis1, J. Papamastorakis1, 2 and J. Ventura1

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

(Received 12 February 2002 / Accepted 3 April 2002 )

We present the first CCD mosaic of the supernova remnant G 65.3+5.7 in the optical emission lines of [ $\ion{O}{ii}$ ] and [ $\ion{O}{iii}$ ]. The new images reveal several diffuse and filamentary structures both inside and outside the extent of the remnant as defined by its X-ray and radio emission. The medium ionization line of [ $\ion{O}{iii}$ ]5007 Å provides the sharpest view to the system, while the remnant appears less filamentary in the emission line of [ $\ion{O}{ii}$ ]. There are significant morphological differences between the two images strongly suggesting the presence of incomplete shock structures. Deep long-slit spectra were taken at several different positions of G 65.3+5.7. All spectra originate from shock heated gas, while the majority of them is characterized by large [ $\ion{O}{iii}$ ]/H $\beta$ ratios. The sulfur line ratios indicate electron densities below ~200 cm -3, while estimates of the shock velocities lie in the range of 90-140 km s -1. Finally, the observed variations of the H $\alpha$/H $\beta$ ratios may reflect the presence of intrinsic absorption affecting the optical spectra.

Key words: ISM: general -- ISM: supernova remnants -- ISM: individual objects: G 65.3+5.7

Offprint request: F. Mavromatakis, fotis@physics.uoc.gr

SIMBAD Objects

© ESO 2002