J/A+A/644/A144ivo://CDS.VizieR/J/A+A/644/A144doi:10.26093/cds/vizier.36440144CDSDonevski D.Lapi A.Malek K.Liu D.Gomez-Guijarro C.Dave R.,Kraljic K.Pantoni L.Man A.Fujimoto S.Feltre A.Pearson W.Li Q.,NarayananD.2021-02-19T07:33:32Z2020-12-14T08:03:36ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiescatalogsmillimeter-astronomyphotometrysubmillimeter-astronomyThe dust-to-stellar mass ratio (M_dust_/M*) is a crucial yet poorly constrained quantity to understand the complex physical processes involved in the production of dust, metals and stars in galaxy evolution. In this work we explore trends of M_dust_/M* with different physica parameters using observations of 300 massive, dusty star-forming galaxies detected with ALMA up to z~5. Additionally, we interpret our findings with different models of dusty galaxy formation. We find that M_dust_/M* evolves with redshift, stellar mass, specific star formation rate and integrated dust size, differently for main sequence and starburst galaxies. In both galaxy populations M_dust_/M* increases until z~2 followed by a roughly flat trend towards higher redshifts, suggesting efficient dust growth in the distant universe. We confirm that the inverse relation between M_dust_/M* and M* holds up to z~5 and can be interpreted as an evolutionary transition from early to late starburst phases. We demonstrate that M_dust_/M* in starbursts reflects the increase in molecular gas fraction with redshift, and attains the highest values for sources with the most compact dusty star-formation. The state-of-the-art cosmological simulations that include self-consistent dust growth, broadly reproduce the evolution of M_dust_/M* in main sequence galaxies, but underestimate it in starbursts. The latter is found to be linked to lower gas-phase metallicities and longer dust growth timescales relative to observations. Phenomenological models based on the main-sequence/starburst dichotomy and analytical models that include recipes for rapid metal enrichment are consistent with our observations. Therefore, our results strongly suggest that high M_dust_/M* is due to rapid dust grain growth in metal enriched interstellar medium. This work highlights multifold benefits of using M_dust_/M* as a diagnostic tool for: (1) disentangling main sequence and starburst galaxies up to z~5; (2) probing the evolutionary phase of massive objects; and (3) refining the treatment of the dust life cycle in simulations.2020A&A...644A.144Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/644/A144CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJS/244/40 : A3COSMOS. I. ALMA continuum photometry catalogs (Liu+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/644/A144https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/644/A144http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/644/A144https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/644/A144https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/644/A144http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/644/A144GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/644/A144/table3 (List of selected DSFGs and their physical properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/644/A144/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/644/A144/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/644/A144/table3?GETtext/xml+votable180.050000true150.1752.3530.0055555555555555565/6814 6/27245 27247 27344https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/644/A144?format=asciiMillimeterdefaultJ/A+A/644/A144/table3List of selected DSFGs and their physical propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceIDSource name (as in HELP database, HELP_JHHMMSS.sss)meta.id;meta.datasetcharRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainzSource observed redshiftsrc.redshiftfloatlogMsSource stellar mass (log scale)log(solMass)phys.massfloate_logMsUncertainty on source logMs (log scale)log(solMass)stat.errorfloatlogLIRInfrared luminosity integrated over 8-1000um (log scale)log(solLum)phys.luminosity;em.IRfloate_logLIRUncertainty on source logLIR (log scale)log(solLum)stat.errorfloatlogMdSource dust mass (log scale)log(solMass)phys.massfloate_logMdUncertainty on source logMd (log scale)log(solMass)stat.errorfloatSalmaALMA flux estimation at nu frequency (1)mJyphot.flux.density;em.radiofloate_SalmaUncertainty on ALMA fluxmJystat.errorfloatnuObserved ALMA frequencyGHzem.freqfloatA3CDisplay the A3COSMOS data (Liu et al., 2019, Cat. J/ApJS/244/40)meta.ref.urlchar