Volume 474, Number 2, November I 2007
|Page(s)||541 - 547|
|Section||Interstellar and circumstellar matter|
|Published online||28 August 2007|
Radio and X-ray images of the SNR G18.8+0.3 interacting with molecular clouds
National Astronomical Observatories, CAS, Beijing 100012, PR China e-mail: email@example.com
2 Department of Physics & Astronomy, University of Calgary, Calgary, Alberta T2N 1N4, Canada
3 Department of Astronomy, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01003, USA
Accepted: 20 August 2007
New HI images from the VLA Galactic Plane Survey (VGPS) show clear absorption features associated with the supernova remnant (SNR) G18.8+0.3. High-resolution 13CO images reveal that molecular clouds overlap the radio filaments of G18.8+0.3. The 13CO emission spectrum over the full velocity range in the direction of G18.8+0.3 shows two molecular components with high brightness-temperature and three molecular components with low brightness-temperature, all with respective HI absorption. This implies that these clouds are in front of G18.8+0.3. In the HI images, the highest velocity absorption feature seen against the continuum image of G18.8+0.3 is at 129 km s-1, which corresponds to the tangent point in this direction. This yields a lower distance limit of 6.9 kpc for G18.8+0.3. Absence of absorption at negative velocities gives an upper distance limit of 15 kpc. The broadened profile at km s-1 in the 13CO emission spectra is a strong indicator of a possible SNR/CO cloud interaction. Thus, G18.8+0.3 is likely to be at the distance of about 12 kpc. The upper mass limit and mean density of the giant CO cloud at km s-1 are ~ and ~ cm-3. We find an atomic hydrogen column density in front of G18.8+0.3 of cm-2. The ROSAT PSPC observations show a diffuse X-ray enhancement apparently associated with part of the radio shell of G18.8+0.3. Assuming an association, the unabsorbed flux is erg cm-2 s-1, suggesting an intrinsic luminosity of erg s-1 for G18.8+0.3.
Key words: ISM: supernova remnants / galaxies: ISM / galaxies: kinematics and dynamics / ISM: structure
© ESO, 2007
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