The dust and cold gas content of local star-forming galaxies.

We use dust masses (M _dust) derived from far-infrared data and molecular gas masses (M _mol) based on CO luminosity to calibrate proxies based on a combination of the galaxy Balmer decrement, disc inclination, and gas metallicity. We use such proxies to estimate M _dust and M _mol in the local SDSS sample of star-forming galaxies (SFGs). We study the distribution of M _dust and M _mol along and across the main sequence (MS) of SFGs. We find that M _dust and M _mol increase rapidly along the MS with increasing stellar mass (M _*), and more marginally across the MS with increasing SFR (or distance from the relation). The dependence on M _* is sub-linear for both M _dust and M _mol. Thus, the fraction of dust (f _dust) and molecular gas mass (f _mol) decreases monotonically towards large M _*. The star formation efficiency (SFE, inverse of the molecular gas depletion time) depends strongly on the distance from the MS and it is constant along the MS. As nearly all galaxies in the sample are central galaxies, we estimate the dependence of f _dust and f _gas on the host halo mass and find a tight anticorrelation. As the region where the MS is bending is numerically dominated by massive haloes, we conclude that the bending of the MS is due to a lower availability of molecular gas mass in massive haloes rather than a lower efficiency in forming stars. [ABSTRACT FROM AUTHOR]