Cavity of Molecular Gas Associated with Supernova Remnant 3C 397

Details Cavity of Molecular Gas Associated with Supernova Remnant 3C 397 Cavity of Molecular Gas Associated with Supernova Remnant 3C 397

2010-01-13

arxiv.org/abs/1001.2204v3

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

ApJ in press, 11 pages, 8 figures and 2 tables. A list of Galactic SNRs in physical contact with molecular clouds is included;

Scientific paper

3C 397 is a radio and X-ray bright Galactic supernova remnant (SNR) with an unusual rectangular morphology. Our CO observation obtained with the Purple Mountain Observatory at Delingha reveals that the remnant is well confined in a cavity of molecular gas, and embedded at the edge of a molecular cloud (MC) at the local standard of rest systemic velocity of ~32 km/s. The cloud has a column density gradient increasing from southeast to northwest, perpendicular to the Galactic plane, in agreement with the elongation direction of the remnant. This systemic velocity places the cloud and SNR 3C 397 at a kinematic distance of ~10.3 kpc. The derived mean molecular density (~10-30 cm^-3) explains the high volume emission measure of the X-ray emitting gas. A 12CO line broadening of the ~32 km/s component is detected at the westmost boundary of the remnant, which provides direct evidence of the SNR-MC interaction and suggests multi-component gas there with dense (~10^4 cm^-3) molecular clumps. We confirm the previous detection of a MC at ~38 km/s to the west and south of the SNR and argue, based on HI self-absorption, that the cloud is located in the foreground of the remnant. A list of Galactic SNRs presently known and suggested to be in physical contact with environmental MCs is appended in this paper.

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