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Issue A&A
Volume 407, Number 1, August III 2003
Page(s) 249 - 257
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20030839



A&A 407, 249-257 (2003)
DOI: 10.1051/0004-6361:20030839

High resolution spectroscopy of Balmer-dominated shocks in the RCW 86, Kepler and SN 1006 supernova remnants

J. Sollerman1, P. Ghavamian2, 3, P. Lundqvist1 and R. C. Smith4, 3

1  Stockholm Observatory, Department of Astronomy, AlbaNova, 106 91 Stockholm, Sweden
2  Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Rd., Piscataway, NJ 08854-8019, USA
3  Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories, CTIO is operated by AURA, Inc. under contract to the National Science Foundation
4  Cerro Tololo Inter-American Observatory, Casilla 603, Chile

(Received 25 March 2003 / Accepted 22 May 2003)

Abstract
We report results from high resolution optical spectroscopy of three non-radiative galactic supernova remnants, RCW 86, Kepler's supernova remnant and SN 1006. We have measured the narrow component H $\alpha$ line widths in Balmer-dominated filaments in RCW 86 and SN 1006, as well as the narrow component width in a Balmer-dominated knot in Kepler's SNR. The narrow component line widths measured in RCW 86 and Kepler's SNR show FWHM of 30-40 km s -1, similar to what has been seen in other Balmer-dominated remnants. Of the remnants in our sample, SN 1006 is the fastest shock (~3000 km s -1). The narrow component H $\alpha$ and H $\beta$ lines in this remnant have a FWHM of merely 21 km s -1. Comparing the narrow component widths measured in our sample with those measured in other remnants shows that the width of the narrow component does not correlate in a simple way with the shock velocity. The implications for the pre-heating mechanism responsible for the observed line widths are discussed.


Key words: ISM: supernova remnants -- shock waves -- ISM: individual objects: SN 1006 -- ISM: individual objects: RCW 86 -- ISM: individual objects: Kepler

Offprint request: J. Sollerman, jesper@astro.su.se

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