Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 358599.0, MPI für Astronomie / Publikationen_mpia
Warm molecular hydrogen in the Spitzer SINGS galaxy sample
Authors:Roussel, H.; Helou, G.; Hollenbach, D. J.; Draine, B. T.; Smith, J. D.; Armus, L.; Schinnerer, E.; Walter, F.; Engelbracht, C. W.; Thornley, M. D.; Kennicutt, R. C.; Calzetti, D.; Dale, D. A.; Murphy, E. J.; Bot, C.
Date of Publication (YYYY-MM-DD):2007
Title of Journal:The Astrophysical Journal
Volume:669
Start Page:959
End Page:981
Audience:Not Specified
Abstract / Description:Results on the properties of warm molecular hydrogen in 57 normal galaxies are derived from measurements of H2 rotational transitions, obtained as part of SINGS. This study extends previous extragalactic surveys of emission lines of H2 to fainter and more common systems (LFIR=107-6×1010 Lsolar). The 17 mum S(1) transition is securely detected in the nuclear regions of 86% of galaxies with stellar masses above 109.5 Msolar. The derived column densities of warm H2 (T>=100 K), although averaged over kiloparsec-scale areas, are commensurate with values observed in resolved photodissociation regions. They amount to between 1% and >30% of the total H2. The power emitted in the three lowest energy transitions is on average 30% of the power of the bright [Si II] cooling line (34.8 mum) and about 4×10-4 of the total infrared power for star-forming galaxies, which is consistent with excitation in PDRs. The fact that the H2 line intensities scale tightly with the aromatic band emission, even though the average radiation field intensity varies by a factor of 10, can also be understood if both tracers originate predominantly in PDRs, either dense or diffuse. Many of the 25 LINER/Seyfert targets strongly depart from the rest of the sample, in having warmer excited H2 and excess H2 rotational power with respect to the dust emission. We propose a threshold in H2-to-aromatic band power ratios, allowing the identification of low-luminosity AGNs by an excess H2 excitation. A dominant contribution from shock heating is favored in these objects. Finally, we detect in nearly half the star-forming targets nonequilibrium ortho-to-para ratios, consistent with the effects of FUV pumping combined with incomplete ortho-para thermalization, or possibly nonequilibrium photodissociation fronts.
Free Keywords:Galaxies: ISM; Infrared: Galaxies; Infrared: ISM; ISM: Lines and Bands; ISM: Molecules; Surveys
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2007ApJ...669..959R
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.