J/A+A/641/A168ivo://CDS.VizieR/J/A+A/641/A168doi:10.26093/cds/vizier.36410168CDSNanni A.Burgarella D.Theule P.Cote B.Hirashita H.2022-03-10T07:07:07Z2020-09-25T07:24:19ZCDS support team

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

cds-question@unistra.frastronomical-modelsgalaxiesinterstellar-mediumThe chemical enrichment in the interstellar medium (ISM) of galaxies is regulated by several physical processes: star birth and death, grain formation and destruction, and galactic inflows and outflows. Understanding such processes and their relative importance is essential to following galaxy evolution and the chemical enrichment through the cosmic epochs, and to interpreting current and future observations. Despite the importance of such topics, the contribution of different stellar sources to the chemical enrichment of galaxies, for example massive stars exploding as Type II supernovae (SNe) and low-mass stars, as well as the mechanisms driving the evolution of dust grains, such as for example grain growth in the ISM and destruction by SN shocks, remain controversial from both observational and theoretical viewpoints. In this work, we revise the current description of metal and dust evolution in the ISM of local low-metallicity dwarf galaxies and develop a new description of Lyman-break galaxies (LBGs) which are considered to be their high-redshift counterparts in terms of star formation, stellar mass, and metallicity. Our goal is to reproduce the observed properties of such galaxies, in particular (i) the peak in dust mass over total stellar mass (sMdust) observed within a few hundred million years; and (ii) the decrease in sMdust at a later time. We fitted spectral energy distribution (SED) of dwarf galaxies and LBGs with the 'Code Investigating GALaxies Emission' (CIGALE), through which the total stellar mass, dust mass, and star formation rate are estimated. For some of the dwarf galaxies considered, the metal and gas content are available from the literature. We computed different prescriptions for metal and dust evolution in these systems (e.g. different initial mass functions for stars, dust condensation fractions, SN destruction, dust accretion in the ISM, and inflow and outflow efficiency), and we fitted the properties of the observed galaxies through the predictions of the models. Only some combinations of models are able to reproduce the observed trend and simultaneously fit the observed properties of the galaxies considered. In particular, we show that (i) a top-heavy initial mass function that favours the formation of massive stars and a dust condensation fraction for Type II SNe of around 50% or more help to reproduce the peak of sMdust observed after ~100Myr from the beginning of the baryon cycle for both dwarf galaxies and LBGs; (ii) galactic outflows play a crucial role in reproducing the observed decline in sMdust with age and are more efficient than grain destruction from Type II SNe both in local galaxies and at high-redshift; (iii) a star formation efficiency (mass of gas converted into stars) of a few percent is required to explain the observed metallicity of local dwarf galaxies; and (iv) dust growth in the ISM is not necessary in order to reproduce the values of sMdust derived for the galaxies under study, and, if present, the effect of this process would be erased by galactic outflows.2020A&A...641A.168Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/641/A168CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/641/A168https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/641/A168http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/641/A168https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/641/A168https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/641/A168http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/641/A168GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/641/A168/table3 (Physical properties of 31 DGS and 18 LBGs)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/641/A168/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/641/A168/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/641/A168/table3?GETtext/xml+votable180.050000true161.343291755.96038890.0055555555555555566/333 684 3389 5950 6011 6046 6419 7281 7946 10399 10431 10481 10587 10811 10970 11137 11177-11178 11382 17683 17692 18198 19934 20283 20388 23468 23470 23476 23495 23508 23531 23549 24204 24696 25594 25659 26971 27258 28448 29718 35243 35935 36756 40124 43874https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/641/A168?format=asciidefaultJ/A+A/641/A168/table3Physical properties of 31 DGS and 18 LBGsSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of the galaxymeta.id;meta.maincharchi2Averaged residual given by Eq. 15stat.fit.residualdoubleMSilPredicted mass of silicate dust normalised for the final stellar mass (=1Msun at 13x10^9^yr)phys.massdoublee_MSilUncertainty of predicted mass of silicate duststat.errordoubleMCarPredicted mass of carbon dust normalised for the final stellar mass (=1Msun at 13x10^9^yr)phys.massdoublee_MCarUncertainty of predicted mass of carbon duststat.errordoubleMironPredicted mass of iron dust normalised for the final stellar mass (=1 Msun at 13x10^9^yr)phys.massdoublee_MironUncertainty of predicted mass of iron duststat.errordoublefcondDust condensation fraction for SNe IIphys.mass;arith.ratiodoublee_fcondUncertainty on dust condensation fraction for SNe IIstat.errordoubleMgasInitial mass of baryons normalised for final stellar mass (=1Msun at 13x10^9^yr)phys.massdoublee_MgasUncertainty of initial mass of baryonsstat.errordoublealphaSlope of the top-heavy Initial Mass Function in Eq. 3stat.fit.paramdoublee_alphaUncertainty of slope of the top-heavy IMFstat.error;pos.eq.radoubleMsweptMass of gas swept-up by a SN event in Eq. 8stat.fit.paramdoublee_MsweptUncertainty of Msweptstat.errordoublefdustoutFraction of circumgalactic dust over the totalphys.mass;arith.ratiodoublee_fdustoutUncertainty of circumgalactic dust over the totalstat.errordoublefgasoutFraction of circumgalactic gas over the totalphys.mass;arith.ratiodoublee_fgasoutUncertainty of circumgalactic gas over the totalstat.errordoublefdoutSNRatio between dust ejected by the galactic outflow and total ejected and destroyed by SN shocksphys.mass;arith.ratiodoublee_fdoutSNUncertainty of ratio between the dust ejected by galactic outflow and total ejected and destroyed by SN shocksstat.errordoubleTypeType of galaxy (DGS or LBG)src.classchar_RAPositions from Simbad except lgb10 (right ascension part)degpos.eq.ra;meta.mainnullable_DEPositions from Simbad except lgb10 (declination part)degpos.eq.dec;meta.mainnullable