Volume 407, Number 1, August III 2003
|Page(s)||249 - 257|
|Section||Interstellar and circumstellar matter|
|Published online||17 November 2003|
High resolution spectroscopy of Balmer-dominated shocks in the RCW 86, Kepler and SN 1006 supernova remnants*
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
Corresponding author: J. Sollerman, email@example.com
Accepted: 22 May 2003
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 Hα 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 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 Hα and Hβ 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
© ESO, 2003
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