Scaling Relations between Gas and Star Formation in Nearby Galaxies
Abstract
High resolution, multi-wavelength maps of a sizeable set of nearby galaxies have made it possible to study how the surface densities of HI, H2 and star formation rate (SigmaHI, SigmaH2, SigmaSFR) relate on scales of a few hundred parsecs. At these scales, individual galaxy disks are comfortably resolved, making it possible to assess gas-SFR relations with respect to environment within galaxies. SigmaH2, traced by CO intensity, shows a strong correlation with SigmaSFR and the ratio between these two quantities, the molecular gas depletion time, appears to be constant at about 2Gyr in large spiral galaxies. Within the star-forming disks of galaxies, SigmaSFR shows almost no correlation with SigmaHI. In the outer parts of galaxies, however, SigmaSFR does scale with SigmaHI, though with large scatter. Combining data from these different environments yields a distribution with multiple regimes in Sigmagas - SigmaSFR space. If the underlying assumptions to convert observables to physical quantities are matched, even combined datasets based on different SFR tracers, methodologies and spatial scales occupy a well define locus in Sigmagas - SigmaSFR space.