Recent studies of nearby spiral galaxies suggest that photodissociation regions (PDRs) are capable of producing much of the observed H I in galaxy disks. In that case, measurements of the observed H I column density and the far-ultraviolet (FUV) photon flux responsible for the photodissociation process provide a new probe of the volume density of the local underlying molecular hydrogen. We develop the method and apply it to the giant Scd spiral galaxy M101 (NGC 5457). The H I column density and amount of FUV emission have been measured for a sample of 35 candidate PDRs located throughout the disk of M101 using the Very Large Array and the Ultraviolet Imaging Telescope. We find that, after correction for the best-estimate gradient of metallicity in the interstellar medium (ISM) of M101 and for the extinction of the ultraviolet emission, molecular gas with a narrow range of density from 30-1000 cm-3 is found near star-forming regions at all radii in the disk of M101 out to a distance of 12' ≈ 26 kpc, close to the photometric limit of R25 ≈ 135. In this picture, the ISM is virtually all molecular in the inner parts of M101. The strong decrease of the H I column density in the inner disk of the galaxy at RG 10 kpc is a consequence of a strong increase in the dust-to-gas ratio there, resulting in an increase of the H2 formation rate on grains and a corresponding disappearance of hydrogen in its atomic form.
展开▼
