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Title:
Spitzer Spectral Line Mapping of Supernova Remnants. I. Basic Data and Principal Component Analysis
Authors:
Neufeld, David A.; Hollenbach, David J.; Kaufman, Michael J.; Snell, Ronald L.; Melnick, Gary J.; Bergin, Edwin A.; Sonnentrucker, Paule
Affiliation:
AA(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AB(NASA Ames Research Center, Moffett Field, CA 94035.), AC(Department of Physics, San Jose State University, 1 Washington Square, San Jose, CA 95192.), AD(Department of Astronomy, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01003.), AE(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.), AF(Department of Astronomy, University of Michigan, 825 Dennison Building, Ann Arbor, MI 48109.), AG(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.)
Publication:
The Astrophysical Journal, Volume 664, Issue 2, pp. 890-908. (ApJ Homepage)
Publication Date:
08/2007
Origin:
UCP
ApJ Keywords:
ISM: Abundances, ISM: Clouds, ISM: Molecules, Molecular Processes, Shock Waves
DOI:
10.1086/518857
Bibliographic Code:
2007ApJ...664..890N

Abstract

We report the results of spectroscopic mapping observations carried out toward small (1'×1') regions within the supernova remnants W44, W28, IC 443, and 3C 391 using the Infrared Spectrograph (IRS) of the Spitzer Space Telescope. These observations, covering the 5.2-37 μm spectral region, have led to the detection of a total of 15 fine-structure transitions of Ne+, Ne++, Si+, P+, S, S++, Cl+, Fe+, and Fe++; the S(0)-S(7) pure rotational lines of molecular hydrogen; and the R(3) and R(4) transitions of hydrogen deuteride. In addition to these 25 spectral lines, the 6.2, 7.7, 8.6, 11.3, and 12.6 μm PAH emission bands were also observed. Most of the detected line transitions have proven strong enough to map in several sources, providing a comprehensive picture of the relative distribution of the various line emissions observable in the Spitzer IRS bandpass. A principal component analysis of the spectral-line maps reveals that the observed emission lines fall into five distinct groups, each of which may exhibit a distinct spatial distribution: (1) lines of S and H2(J>2) (2) the H2 S(0) line; (3) lines of ions with appearance potentials less than 13.6 eV; (4) lines of ions with appearance potentials greater than 13.6 eV, not including S++; (5) lines of S++. Lines of group 1 likely originate in molecular material subject to a slow, nondissociative shock that is driven by the overpressure within the supernova remnant, and lines in groups 3-5 are associated primarily with dissociative shock fronts with a range of (larger) shock velocities. The H2 S(0) line shows a low-density diffuse emission component and, in some sources, a shock-excited component.
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