Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ascl.soft02022p&link_type=abstract
Astrophysics Source Code Library, record ascl:1102.022
Astronomy and Astrophysics
Astrophysics
Scientific paper
Ultraviolet photons from O and B stars strongly influence the structure and emission spectra of the interstellar medium. The UV photons energetic enough to ionize hydrogen (h? > 13.6 eV) will create the H II region around the star, but lower energy UV photons escape. These far-UV photons (6 eV < h? < 13.6 eV) are still energetic enough to photodissociate molecules and to ionize low ionization-potential atoms such as carbon, silicon, and sulfur. They thus create a photodissociation region (PDR) just outside the H II region. In aggregate, these PDRs dominates the heating and cooling of the neutral interstellar medium. As part of the Web Infrared Tool Shed (WITS {http://dustem.astro.umd.edu}) we have developed a web tool, called the PDR Toolbox, that allows users to determine the physical parameters of a PDR from a set of spectral line observations. Typical observations of both Galactic and extragalactic PDRs come from ground-based millimeter and submillimeter telescopes such as CARMA or the CSO, or space-based telescopes such as Spitzer, ISO, SOFIA, and Herschel. Given a set of observations of spectral line intensities, PDR Toolbox will compute best-fit FUV incident intensity and cloud density based on our published models of PDR emission.
Pound Marc William
Wolfire Mark G.
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