Decarli, RobertoWalter, FabianAravena, M.Carilli, C LBouwens, Rychard Johnda Cunha, ElisabeteDaddi, E.Elbaz, DavidRiechers, DominikSmail, Ian2018-11-292018-11-290004-637Xhttp://hdl.handle.net/1885/152279We study the molecular gas properties of high-z galaxies observed in the ALMA Spectroscopic Survey (ASPECS) that targets an ~1 arcmin2 region in the Hubble Ultra Deep Field (UDF), a blind survey of CO emission (tracing molecular gas) in the 3 and 1 mm bands. Of a total of 1302 galaxies in the field, 56 have spectroscopic redshifts and correspondingly well-defined physical properties. Among these, 11 have infrared luminosities ${L}_{\mathrm{IR}}\gt {10}^{11}$ ${L}_{\odot }$, i.e., a detection in CO emission was expected. Out of these, 7 are detected at various significance in CO, and 4 are undetected in CO emission. In the CO-detected sources, we find CO excitation conditions that are lower than those typically found in starburst/sub-mm galaxy/QSO environments. We use the CO luminosities (including limits for non-detections) to derive molecular gas masses. We discuss our findings in the context of previous molecular gas observations at high redshift (star formation law, gas depletion times, gas fractions): the CO-detected galaxies in the UDF tend to reside on the low-${L}_{\mathrm{IR}}$ envelope of the scatter in the ${L}_{\mathrm{IR}}\mbox{--}{L}_{\mathrm{CO}}^{\prime }$ relation, but exceptions exist. For the CO-detected sources, we find an average depletion time of ~1 Gyr, with significant scatter. The average molecular-to-stellar mass ratio (${M}_{{\rm{H}}2}$/M *) is consistent with earlier measurements of main-sequence galaxies at these redshifts, and again shows large variations among sources. In some cases, we also measure dust continuum emission. On average, the dust-based estimates of the molecular gas are a factor ~2–5× smaller than those based on CO. When we account for detections as well as non-detections, we find large diversity in the molecular gas properties of the high-redshift galaxies covered by ASPECSapplication/pdf201610.3847/1538-4357/833/1/702018-11-29