J/MNRAS/462/1329ivo://CDS.VizieR/J/MNRAS/462/1329doi:10.26093/cds/vizier.74621329CDSMolla M.Diaz A.I.Gibson B.K.Cavichia O.Lopez-Sanchez A.-R.2024-08-16T20:18:07Z2017-10-13T12:24:31ZCDS support team

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

cds-question@unistra.frastronomical-modelsgalaxiesvisible-astronomySpiral galaxies are thought to acquire their gas through a protracted infall phase resulting in the inside-out growth of their associated discs. For field spirals, this infall occurs in the lower density environments of the cosmic web. The overall infall rate, as well as the galactocentric radius at which this infall is incorporated into the star-forming disc, plays a pivotal role in shaping the characteristics observed today. Indeed, characterizing the functional form of this spatio-temporal infall in situ is exceedingly difficult, and one is forced to constrain these forms using the present day state of galaxies with model or simulation predictions. We present the infall rates used as input to a grid of chemical evolution models spanning the mass spectrum of discs observed today. We provide a systematic comparison with alternate analytical infall schemes in the literature, including a first comparison with cosmological simulations. Identifying the degeneracies associated with the adopted infall rate prescriptions in galaxy models is an important step in the development of a consistent picture of disc galaxy formation and evolution.2016MNRAS.462.1329Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/462/1329CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/462/1329https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/462/1329http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/462/1329https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/462/1329https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/462/1329http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/462/1329GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/MNRAS/462/1329/table1Characteristics of the theoretical galaxies modeled (Table 1 in the manuscript)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMvirThe virial mass in logarithmic scale used as name for each galaxylog(solMass)meta.id;meta.mainfloatMvirThe virial mass in the protohalo of each galaxysolMassphys.massdoubleMDThe barionic mass expected in the disk at the end of the evolution as obtained from the SHMRsolMassphys.massdoubleMBThe bulge mass in each galaxysolMassphys.massdoubleRvirThe virial radius for each galaxy at the end of the evolutionkpcphys.size.radiusfloatRDThe expected scale length of the disc at the end of the evolutionkpcphys.angSize;srcfloatRoptThe expected optical radius of the disc at the end of the evolutionkpcphys.angSize;srcfloatRcarThe characteristic radius of the disc used for normalization purposeskpcphys.size.radiusfloattaucThe collapse time scale for the characteristic radiusGyrtime.scalefloatVrotThe rotation velocity at the characteristic radiuskm/sphys.veloc.rotatfloatsigma0The dispersion velocity of the bulgekm/sphys.veloc.dispersionfloatReffBThe effective radius of the bulgekpcphys.size.radiusfloatNRNumber of computed radial regions in each galaxymeta.id;obs.fieldintJ/MNRAS/462/1329/table2Mass distributions used as inputs of models (corresponding to Fig.1 of the manuscript)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMvirThe virial mass in logarithmic scale used as name for each galaxylog(solMass)meta.id;meta.mainfloatRThe galactocentric distance of each radial region (Radius)kpcpos.distance;obs.field;pos.galactocentricfloatMtotThe total mass in each radius as obtained of the rotation curvesolMassphys.massdoubleDMtotThe mass included in each radial region =Mtot(R)-Mtot(R-1)solMassphys.massdoubletau(R)The collapse time-scale for each radial regionGyrtime.scaledoubleJ/MNRAS/462/1329/table3Time evolution of infall, effective radius and mass in the disc for each galaxy as a wholerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMvirThe virial mass in logarithmic scale used as name for each galaxylog(solMass)meta.id;meta.mainfloatTimeEvolutionary time from time=0 until time=13.2GyrGyrtime.agedoubleReffThe radius where the mass of the disc reaches the half value of the total in the disc in each timekpcphys.size.radiusdoubledM/dtThe total infall rate from the protohalo over the disc in each timesolMass/yrarith.ratedoubleMDThe barionic mass in the disc in each timesolMassphys.massdoubleJ/MNRAS/462/1329/table4Time evolution of infall, and mass in the disk for each radial region of each galaxyrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMvirThe virial mass in logarithmic scale used as name for each galaxylog(solMass)meta.id;meta.mainfloatTimeEvolutionary time from time=0 until time=13.2 GyrGyrtime.agedoubleRThe galactocentric radius of each radial regionkpcpos.distance;pos.galactocentricdoubledM/dtThe infall rate from the protohalo over the disc in each time and radial regionsolMass/yrarith.ratedoubleMDThe barionic mass in each time and in each radial region of the discsolMassphys.massdoubleJ/MNRAS/462/1329/table5Relation time-redshift used in the workTimeEvolutionary timeGyrtime.agedoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzRedshift associated to each time following MacDonald (2006, Found. Phys. Lett. 19, 631)src.redshiftdoubleJ/MNRAS/462/1329/table6Parameters to the fit equations y=a+bx+cx^2^+dx^3^+ex^4^ with x=logMD of results in Fig.8 and Fig.12recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintParamParameter that it is fitted to a function of logMDstat.param;meta.modelledaParameter a for y=a+bx+cx^2^+dx^3^+ex^4^stat.fit.paramdoublebParameter b for y=a+bx+cx^2^+dx^3^+ex^4^stat.fit.paramdoublec? Parameter c for y=a+bx+cx^2^+dx^3^+ex^4^stat.fit.paramdoublenullabled? Parameter d for y=a+bx+cx^2^+dx^3^+ex^4^stat.fit.paramdoublenullablee? Parameter e for y=a+bx+cx^2^+dx^3^+ex^4^stat.fit.paramdoublenullable