2011MNRAS.415...61S

We study the relation between molecular gas and star formation in a volume-limited sample of 222 galaxies from the COLD GASS survey, with measurements of the CO(1–0) line from the IRAM 30-m telescope. The galaxies are at redshifts 0.025 < z < 0.05 and have stellar masses in the range 10.0 < log M_{Ux2605}/M_☉< 11.5. The IRAM measurements are complemented by deep Arecibo H I observations and homogeneous Sloan Digital Sky Survey and GALEX photometry. A reference sample that includes both ultraviolet (UV) and far-infrared data is used to calibrate our estimates of star formation rates from the seven optical/UV bands. The mean molecular gas depletion time-scale [{img}] for all the galaxies in our sample is 1 Gyr; however, {img} increases by a factor of 6 from a value of ∼0.5 Gyr for galaxies with stellar masses of ∼10¹⁰ M_☉ to ∼3 Gyr for galaxies with masses of a few {x}10¹¹ M_☉. In contrast, the atomic gas depletion time-scale remains constant at a value of around 3 Gyr. This implies that in high-mass galaxies, molecular and atomic gas depletion time-scales are comparable, but in low-mass galaxies, the molecular gas is being consumed much more quickly than the atomic gas. The strongest dependences of {img} are on the stellar mass of the galaxy [parametrized as {img}], and on the specific star formation rate (sSFR). A single {img} versus sSFR relation is able to fit both `normal' star-forming galaxies in our COLD GASS sample and more extreme starburst galaxies (luminous infrared galaxies and ultraluminous infrared galaxies), which have {img} yr. Normal galaxies at z = 1–2 are displaced with respect to the local galaxy population in the {img} versus sSFR plane and have molecular gas depletion times that are a factor of 3–5 times longer at a given value of sSFR due to their significantly larger gas fractions.