PDR-Produced HI in Star-Forming Regions of M33

Details PDR-Produced HI in Star-Forming Regions of M33 PDR-Produced HI in Star-Forming Regions of M33

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.1502h&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #15.02; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

We report our latest findings on the volume densities of molecular hydrogen in Giant Molecular Clouds (GMCs) associated with photodissociation regions (PDRs) in the nearby galaxy M33, using HI continuum, FUVand metallicity data.
The morphology of the atomic hydrogen distribution is similar to what is expected for PDRs, since the HI is seen surrounding bright FUV sources. Potential PDRs that we detect, in which dissociating photons dominate the radiation field, have sizes in the order of 100 parsec. Complexes of young, hot stars are responsible for these PDRs. They create a 'blanket' of photodissociated HI.
The balance equation governing the photodissociation process needs the ultraviolet luminosity incident on the surface of the GMC and the local dust-to-gas ratio together with the HI column density in order to calculate the volume density of molecular hydrogen.
Verification of the PDR scheme that we are testing depends ciritically on the spatial resolution of the M33 data. At a resolution in the order of 20-30pc we expect to see a PDR morphology. Earlier results for M81 and M83 had the right resolution to apply our method, but lacked the spatial resolution to truly discern any structure.
We used M33 radio data kindly provided by David Thilker and Robert Braun and publicly available Galex UV data.
This work is funded by STScI's Director's Discretionary Research Fund.

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