J/MNRAS/496/3668ivo://CDS.VizieR/J/MNRAS/496/3668doi:10.26093/cds/vizier.74963668CDSDe Looze I.Lamperti I.Saintonge A.Relano M.Smith M.W.L.,Clark C.J.R.Wilson C.D.Decleir M.Jones A.P.Kennicutt R.C.,Accurso G.Brinks E.Bureau M.Cigan P.Clements D.L.De Vis P.,Fanciullo L.Gao Y.Gear W.K.Ho L.C.Hwang H.S.Michalowski M.J.,Lee J.C.Li C.Lin L.Liu T.Lomaeva M.Pan H.-A.Sargent M.,Williams T.Xiao T.Zhu M.2025-05-22T20:16:03Z2023-10-12T15:31:32ZCDS support team

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

cds-question@unistra.frgalaxiesinterstellar-mediumastronomical-modelsinfrared-astronomyScaling laws of dust, HI gas, and metal mass with stellar mass, specific star formation rate, and metallicity are crucial to our understanding of the build-up of galaxies through their enrichment with metals and dust. In this work, we analyse how the dust and metal content varies with specific gas mass (M_HI_/M_*_) across a diverse sample of 423 nearby galaxies. The observed trends are interpreted with a set of Dust and Element evolUtion modelS (DEUS) - including stellar dust production, grain growth, and dust destruction - within a Bayesian framework to enable a rigorous search of the multidimensional parameter space. We find that these scaling laws for galaxies with -1.0~<logM_HI_/M_*_~<0 can be reproduced using closed-box models with high fractions (37-89 per cent) of supernova dust surviving a reverse shock, relatively low grain growth efficiencies ({epsilon}=30-40), and long dust lifetimes (1-2Gyr). The models have present-day dust masses with similar contributions from stellar sources (50-80 per cent) and grain growth (20-50 per cent). Over the entire lifetime of these galaxies, the contribution from stardust (>90 per cent) outweighs the fraction of dust grown in the interstellar medium (<10 per cent). Our results provide an alternative for the chemical evolution models that require extremely low supernova dust production efficiencies and short grain growth time-scales to reproduce local scaling laws, and could help solving the conundrum on whether or not grains can grow efficiently in the interstellar medium.2020MNRAS.496.3668Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/496/3668CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/496/3668https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/496/3668http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/496/3668https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/496/3668https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/496/3668http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/496/3668GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/496/3668/tablea1 (Overview of the dust masses inferred for the JINGLE, HRS, HAPLESS, HiGH and KINGFISH galaxies considered in the scaling relations presented in this work)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/496/3668/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/496/3668/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/496/3668/tablea1?GETtext/xml+votable180.050000true199.070091125.40520280.0055555555555555565/2593-2594 2610 6486 6/764 2320 3506 4105 4439 4447 5124 5164 5172 5181 5183 5190 5200 5241 5244 5247 5332 5336 5342 5440 5492 5629 5715 5751 5799 5966-5967 5975-5978 5981-5982 5999 6001 6011 6037 6087 7241 7602 7604 7607 7624 7769 7799 7956 8106 8235 8320 8330 8359 10253 10259 10264 10267 10269 10271 10282 10285-10286 10289-10294 10296-10297 10302 10336 10342 10345-10346 10351 10368 10371 10380-10381 10383-10385 10389 10391 10393-10398 10400-10402 10404 10415 10421-10423 10434 10439 10444-10445 10454 10466 10475 10592 10632 10684 10761 10841 10901 10990 11010 11434-11435 11457 11961 13522 15592 16441 17594 17612 18398 21845 21847 21849 21852-21854 21879 25083 25575 25581 25596-25597 25599 25775 25788 25918-25919 25933 25935 25958-25961 25964-25966 25971-25972 25974 25976 25980 25997 26005 26051 26065 26068 26088 26090 26119 26128 26174-26175 26214 26217 26222 26253-26255 26260 26265 26271 26275-26276 26279 26282 26286 26290-26291 26294 26301-26303 26308-26309 26317-26318 26320 26323 26330-26331 26336 26338 26344 26346 26351 26365 26377 26388 26432 26472 26528 26537 26960 26965-26967 26969 26971 26992 26996 27030 27130 27279 27300 27303 27305 27324 27514 27555 27603 27606 27648 27650 27653-27654 27656 27712-27713 27715 27718-27719 27724 27727-27728 27731 27736 27741 27750 27757 27761 27763 27814 27823 27830 27841 27855 27857 27860-27862 27889 27907 27909 27914 27918 27926 27934 27937 27941 27948 27955 28015 28033 28035 28037-28038 28054 28056 28118 28123 28126-28127 28141 28162 28167 28170 28191 28201 28208 28213 28220 28234 28258 28264 28294 28299 28304 28348 28404 28416 28496 28508 28529 28538 28643 28651 34404 34471 35993 36194 36974 38390 40959 43420 43845https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/496/3668?format=asciiInfrareddefaultJ/MNRAS/496/3668/tablea1Overview of the dust masses inferred for the JINGLE, HRS, HAPLESS, HiGH and KINGFISH galaxies considered in the scaling relations presented in this workrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGalaxy name (2)meta.id;meta.maincharlogMdustLogarithm of the median dust masslog(solMass)phys.mass;stat.medianfloate_logMdustLower error on logMdust (16th percentile)log(solMass)stat.errorfloatE_logMdustUpper error on logMdust (84th percentile)log(solMass)stat.error;stat.maxfloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainSampleGalaxy sample (1)srccharSimbadNameSimbad column added by the CDSmeta.idcharnullable