Aravena, ManuelBoogaard, LeindertGonzalez-Lopez, J.Decarli, RobertoWalter, FabianCarilli, C LSmail, IanWeiss, AAssef, Roberto J.Bauer, Franz Erikda Cunha, Elisabete2022-07-202022-07-200004-637Xhttp://hdl.handle.net/1885/269810We present a characterization of the physical properties of a sample of 35 securely detected, dusty galaxies in the deep ALMA 1.2 mm image obtained as part of the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS) Large Program. This sample is complemented by 26 additional sources identified via an optical/infrared source positional prior. Using their well-characterized spectral energy distributions, we derive median stellar masses and star formation rates (SFR) of $4.8\times {10}^{10}\,{M}_{\odot }$ and 30 M ☉ yr−1, respectively, and interquartile ranges of (2.4-11.7) x 1010 M ☉ and 20-50 M ☉ yr−1. We derive a median spectroscopic redshift of 1.8 with an interquartile range 1.1-2.6, significantly lower than submillimeter galaxies detected in shallower, wide-field surveys. We find that 59% +- 13%, 6% +- 4%, and 34% +- 9% of our sources are within, above, and below+-0.4 dex from the SFR-stellar-mass relation or main sequence (MS), respectively. The ASPECS galaxies closely follow the SFR-molecular gas mass relation and other previously established scaling relations, confirming a factor of five increase of the gas-to-stellar-mass ratio from z = 0.5 to 2.5 and a mild evolution of the gas depletion timescales with a typical value of 0.7 Gyr at z = 1-3. ASPECS galaxies located significantly below the MS, a poorly exploited parameter space, have low gas-to-stellar-mass ratios of ~0.1-0.2 and long depletion timescales >1 Gyr. Galaxies along the MS dominate the cosmic density of molecular gas at all redshifts. Systems above the MS have an increasing contribution to the total gas reservoirs from z < 1 to z = 2.5, while the opposite is found for galaxies below the MS.M.A. has been supported by the grant “CONICYT + PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG190030” and “CONICYT+PCI+REDES 190194.” J.G.-L. acknowledges partial support from ALMA-CONICYT project 31160033. F.W. and M.N. acknowledge funding from the ERC Advanced Grant “Cosmic Gas.” F.E.B. acknowledges support from CONICYT grants CATA-Basal AFB-170002 (FEB), FONDECYT Regular 1190818 (FEB), 1200495 (FEB), and Chile’s Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). T.D.-S. acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT project 1151239. D.R. acknowledges support from the National Science Foundation under grant Nos. AST-1614213 and AST-1910107 and from the Alexander von Humboldt Foundation through a Humboldt Research Fellowship for Experienced Researchers. I.R.S. acknowledges support from STFC (ST/P000541/1). L.H.I. acknowledges support from JSPS KAKENHI grant No. JP19K23462. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: 2016.1.00324. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.application/pdfen-AU© 2020. The American Astronomical SocietyGalaxy evolutionGalaxy quenchingSubmillimeter astronomyHigh-redshift galaxies202010.3847/1538-4357/ab99a22021-08-01