Volume 430, Number 2, February I 2005
|Page(s)||561 - 566|
|Section||Interstellar and circumstellar matter|
|Published online||20 January 2005|
An alternate estimate of the mass of dust in Cassiopeia A
European Southern Observatory, K-Schwarzschild-Strasse 2, 85748 Garching, Germany e-mail: firstname.lastname@example.org
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Accepted: 28 September 2004
Recent observations of sub-millimeter continuum emission toward supernova remnants (SNR) have raised the question of whether such emission is caused by dust within the SNR itself or along the line-of-sight. Here we make a comparison of the image of sub-mm emission from dust with the integrated line emission from interstellar toward the SNR Cassiopeia A based on existing data. The cm and mm synchrotron emission from Cas A has a rather symmetric, ring-like structure whereas both the sub-mm continuum and interstellar line emission are located mostly toward the south of the SNR. There is positional agreement for 3 of 6 maxima found in line and sub-mm continuum emission, with the weakest feature near the center of Cas A and the other two features near the southeast and west edges of the SNR. For these three maxima, a comparison of masses determined from dust and data shows good agreement if we use the 450 μm dust absorption coefficient typical for diffuse clouds. There is also good agreement between the sub-mm dust temperature and the gas kinetic temperature from CO and . For the remaining sub-mm continuum peaks, one is outside the forward shock of the SNR. For the other two, one was not mapped in 13CO; for the other there is no 13CO emission. absorption covers all of Cas A, but the column density may be too small to account for the sub-mm dust emission. Thus it is possible that one, or perhaps two of these sub-mm continuum peaks are located inside the SNR. From lower resolution maps in CO lines, the SE and W features are the edges of extended clouds. Toward the cloud centers, the CO emission is more intense, but there appears to be less sub-mm dust emission. The differences between CO and sub-mm images may be caused a combination of the techniques used to produce the sub-mm maps and changes in cloud properties from center to edge.
Key words: stars: supernovae: individual: Cassiopia A / submillimeter / radio lines: ISM / galaxies: abundances / ISM: dust, extinction
© ESO, 2005
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