J/A+A/694/A235ivo://CDS.VizieR/J/A+A/694/A235doi:10.26093/cds/vizier.36940235CDSJiang Y.Li J.-T.Tan Q.-H.Ji L.Bregman J.N.Wang Q.D.Wang J.-F.,Lu L.-Y.Jiang X.-J.2025-05-21T20:01:47Z2025-02-18T09:13:32ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsco-line-emissioninterstellar-mediumradio-sourcesMolecular gas, as the fuel for star formation, and its relationship with atomic gas are crucial for understanding how galaxies regulate their star forming (SF) activities. We conducted IRAM 30m observations of 23 nearby spiral galaxies from the CHANG-ES project to investigated the distribution of molecular gas and the Kennicutt-Schmidt law. Combining these results with atomic gas masses from previous studies, we aim to investigate the scaling relations that connect the molecular and atomic gas masses with stellar masses and the baryonic Tully-Fisher relation. Based on spatially resolved observations of the three CO lines, we calculated the total molecular gas masses, the ratios between different CO lines, and derived physical parameters such as temperature and optical depth. The median line ratios for nuclear/disk regions are 8.6/6.1 (^12^CO/^13^CO(1-0)) and 0.53/0.39 (^12^CO(2-1/1-0)). Molecular gas mass derived from ^13^CO is correlated but systematically lower than that from ^12^CO. Most galaxies follow the spatially resolved SF scaling relation with a median gas depletion timescale of approximately 1Gyr, while a few exhibit shorter timescales of approximately 0.1Gyr. The molecular-to-atomic gas mass ratio correlates strongly with stellar mass, consistent with previous studies. Galaxies with lower stellar masses show an excess of atomic gas, indicating less efficient conversion to molecular gas. Most galaxies tightly follow the baryonic Tully-Fisher relation, but NGC 2992 and NGC 4594 deviate from the relation due to different physical factors. We find that the ratio of the cold gas (comprising molecular and atomic gas) to the total baryon mass decreases with the gravitational potential of the galaxy, as traced by rotation velocity, which could be due to gas consumption in SF or being heated to the hot phase.2025A&A...694A.235Jhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/694/A235CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/694/A235https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/694/A235http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/694/A235https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/694/A235https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/694/A235http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/694/A235GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/694/A235/table2 (IRAM 30m observation log)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/694/A235/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/694/A235/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/694/A235/table2?GETtext/xml+votable180.050000true128.326625-22.96575830.0055555555555555566/5067 5504 5587 5639 5995 6037 6081 7550 7584 10674 10888 10979 10986 11000 26175 26221 26223 27246 27861 31321 40410 40432 40514 40520 44026 45054https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/694/A235?format=asciiRadiodefaultJ/A+A/694/A235/table1Parameters of the galaxiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSimbadSimbad column added by the CDSmeta.ref.urlcharGalaxyGalaxy namemeta.id;meta.maincharDistDistance is obtained from Vargas et al. (2019ApJ...881...26V)Mpcpos.distancefloatMtypeThe morphological type code (1)meta.code;src.morph.typefloate_MtypeThe morphological type code errormeta.notefloatVrotThe maximum atomic gas rotation velocity (2)km/sphys.veloc.rotat;stat.maxfloatDiamDiameter derived from 22um data by Wiegert et al. (2015AJ....150...81W, Cat. J/AJ/150/81)kpcpos.distancefloatM*The stellar mass (3)1e+10solMassphys.massfloate_M*The stellar mass error1e+10solMassstat.errorfloatMHIThe total atomic gas mass (4)1e+10solMassphys.massfloatr_MHIThe source of the HI flux, the detailed calculation methods are summarized in Sect. 4.1. (5)meta.ref;pos.framecharSFR? The revised star formation rate (6)solMass/yrphys.SFRfloatnullablee_SFR? The revised star formation rate errorsolMass/yrstat.error;phys.SFRfloatnullableSSFR? The surface density of SFR (7)0.001solMass.yr**-1.kpc**-2src.densityfloatnullablee_SSFR? The surface density of SFR error0.001solMass.yr**-1.kpc**-2stat.errorfloatnullableJ/A+A/694/A235/table2IRAM 30m observation logTexp12COThe total on-source integration time at each position for the ^12^CO(1-0) (2)mintime.expofloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName, NGCNNNN-NN or UGCNNNNN-NN (1)meta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainDate1Observation datetime.epoch;obsnullableDate2Observation datetime.epoch;obsnullableDate3Observation datetime.epoch;obsnullabletau225GHzThe average opacity at 225GHz during observation datesphys.absorption.coefffloatNobsThe total number of observation scans at each position, each scan having an effective on-source integration time of 9.8 minutesmeta.numberintTexp13COThe total on-source integration time at each position for the ^13^CO(1-0) (2)mintime.expofloatTexpCO21The total on-source integration time at each position for the ^12^CO(2-1) (2)mintime.expofloatrms12COThe root mean square for the ^12^CO(1-0) (2)mkstat.errorfloatrms13COThe root mean square for the ^13^CO(1-0) (2)mkstat.errorfloatrmsCO21The root mean square for the ^12^CO(2-1) (2)mkstat.errorfloatJ/A+A/694/A235/table3Observed and derived parameters of the CO linesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDist? The projection distance to the minor axis of the galaxykpcpos.distancefloatnullableI12COThe integrated line intensity of ^12^CO(1-0) (1)K.km/sphot.flux.densityfloate_I12CO? The integrated line intensity of ^12^CO(1-0) error (1)K.km/sstat.errorfloatnullablev012CO? The centroid velocity of ^12^CO(1-0)km/sspect.dopplerVelocfloatnullableE_v012CO? The centroid velocity of ^12^CO(1-0) error (upper value)km/sstat.error;stat.maxfloatnullablee_v012CO? The centroid velocity of ^12^CO(1-0) error (lower value)km/sstat.errorfloatnullableI13COThe integrated line intensity of ^13^CO(1-0) (1)K.km/sphot.flux.densityfloate_I13CO? The integrated line intensity of ^13^CO(1-0) error (1)K.km/sstat.errorfloatnullablev013CO? The centroid velocity of ^13^CO(1-0)km/sspect.dopplerVelocfloatnullableE_v013CO? The centroid velocity of ^13^CO(1-0) error (upper value)km/sstat.error;stat.maxfloatnullablee_v013CO? The centroid velocity of ^13^CO(1-0) error (lower value)km/sstat.errorfloatnullableICO21The integrated line intensity of ^12^CO(2-1) (1)K.km/sphot.flux.densityfloate_ICO21? The integrated line intensity of ^12^CO(2-1) error (1)K.km/sstat.errorfloatnullablev0CO21? The centroid velocity of ^12^CO(2-1)km/sspect.dopplerVelocfloatnullableE_v0CO21? The centroid velocity of ^12^CO(2-1) error (upper value)km/sstat.error;stat.maxfloatnullablee_v0CO21? The centroid velocity of ^12^CO(2-1) error (lower value)km/sstat.errorfloatnullableR12CO/13CO? The intensity line ratios of ^12^CO/^13^CO(1-0) (2)spect.line.intensity;arith.ratiofloatnullableNameName, NGCNNNN-NN or UGCNNNNN-NNmeta.id;meta.maincharE_R12CO/13CO? The intensity line ratios of ^12^CO/^13^CO (1-0) error (upper value) (2)stat.error;stat.maxfloatnullablee_R12CO/13CO? The intensity line ratios of ^12^CO/^13^CO (1-0) error (lower value) (2)stat.errorfloatnullableRCO21/CO10? The intensity line ratio of ^12^CO(2-1)/^12^CO(1-0) (2)spect.line.intensity;arith.ratiofloatnullableE_RCO21/CO10? The intensity line ratio of ^12^CO(2-1)/^12^CO(1-0) error (upper value) (2)stat.error;stat.maxfloatnullablee_RCO21/CO10? The intensity line ratio of ^12^CO(2-1)/^12^CO(1-0) error (lower value) (2)stat.errorfloatnullableTau13CO? The optical depth derived under LTEphys.absorption.opticalDepthfloatnullableE_Tau13CO? The optical depth derived under LTE error (upper value)stat.error;stat.maxfloatnullablee_Tau13CO? The optical depth derived under LTE error (lower value)stat.errorfloatnullableTkin? The kinetic temperature derived under LTEKphys.temperaturefloatnullableE_Tkin? The kinetic temperature derived under LTE error (upper value)Kstat.error;stat.maxfloatnullablee_Tkin? The kinetic temperature derived under LTE error (lower value)Kstat.errorfloatnullablel_I12COLimit flag on I12COmeta.code.errorcharl_I13COLimit file on I13COmeta.code.errorcharl_ICO21Limit flag on ICO21meta.code.errorcharl_R12CO/13COLimit flag on R12CO/13COmeta.code.errorcharl_RCO21/CO10Limit flag on RCO21/CO10meta.code.errorcharl_Tau13COLimit flag on Tau13cometa.code.errorchar