Other
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21114104d&link_type=abstract
American Astronomical Society, AAS Meeting #211, #141.04; Bulletin of the American Astronomical Society, Vol. 39, p.991
Other
Scientific paper
Molecular line diagnostics provide new insight into the OH megamaser (OHM) phenomenon, suggesting a dense gas trigger for OHMs. We identify three physical properties that differentiate OHM hosts from other starburst galaxies: (1) OHMs have the highest mean molecular gas densities among starburst galaxies, (2) OHM hosts are a distinct population in the nonlinear part of the IR-CO relation, (3) OHM hosts have exceptionally high dense molecular gas fractions. OH absorbers and kilomasers generally follow the linear IR-CO relation and are uniformly distributed in dense gas fraction and L(HCN), demonstrating that OHMs form independent of OH abundance. The fraction of non-OHMs with high mean densities and high dense gas fractions constrains beaming to be a minor effect: OHM emission solid angle must exceed 2π steradians. IR luminosity does not appear to dictate OHM formation; both star formation and OHM activity are consequences of tidal density enhancements accompanying galaxy interactions. OHM fraction in starbursts is likely due to the fraction of mergers experiencing a temporal spike in tidally-driven density enhancement. OHMs are thus signposts marking the most intense, compact, and unusual modes of star formation in the local universe. Future high redshift OHM surveys can now be interpreted in a star formation and galaxy evolution context, indicating both the merging rate of galaxies and the burst contribution to star formation.
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