Astronomy and Astrophysics – Astronomy
Scientific paper
May 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.1801r&link_type=abstract
American Astronomical Society, 192nd AAS Meeting, #18.01; Bulletin of the American Astronomical Society, Vol. 30, p.844
Astronomy and Astrophysics
Astronomy
Scientific paper
We present Infrared Space Observatory spectroscopy of a site in the supernova remnant 3C 391, where the blast wave is impacting a dense clump in a giant molecular cloud. The complete wavelength ranges of 40--190 (LWS) and 5--17 (CAM) mu m were observed, as well as narrow ranges centered on 26 and 34.8 (SWS) mu m. Atomic fine-structure lines were detected from (in order of atomic number): C(+) , N(+) , N(++) , O(0) , O(++) , Ne(+) , Ne(++) , Si(+) , P(+) , Ar(+) , and Fe(+) . The presence of a wide range of abundant ions indicates a strong, dissociative (J-type) shock into the lower-density portions of the cloud. The [P II] line at 60.6 mu m is the first known astronomical detection. We discuss the likelihood of this detection in terms of the atomic structure and interstellar abundance of phosphorus. Molecular rotational lines were detected from H_2, CO, OH, and H_2O. All lines arise from low-lying energy levels, consistent with collisional excitation in the dense and warm post-shock gas. Together with millimeter-wave lines of CO, CS, and HCO(+) , the infrared molecular lines are more consistent with a C-type or partially dissociative shock into a region of very high preshock density. The presence of both J-type and C-type shocks in this small region show that the pre-shock medium had a wide range of densities: dense pre-shock clumps (10(5) cm(-3) ) lead to the shock-excited molecular lines, while a more tenuous medium (10(3) cm(-3) ) leads to the shock-excited atomic fine-structure lines.
Reach William T.
Rho Jeonghee
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