J/A+A/623/A122ivo://CDS.VizieR/J/A+A/623/A122doi:10.26093/cds/vizier.36230122CDSPilyugin L.S.Grebel E.K.Zinchenko I.A.Nefedyev Y.A.Vilchez J.M.2019-11-05T07:50:03Z2019-10-02T12:34:33ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsgalaxy-classification-systemschemical-abundancesWe derive rotation curves, surface brightness profiles, and oxygen abundance distributions for 147 late-type galaxies using the publicly available spectroscopy obtained by the MaNGA survey. Changes of the central oxygen abundance (O/H)_0_, the abundance at the optical radius (O/H)_R25_, and the abundance gradient with rotation velocity V_rot_ were examined for galaxies with rotation velocities from 90km/s to 350km/s. We find that each relation shows a break at V_rot_^*^~200km/s. The central (O/H)_0_ abundance increases with rising V_rot_ and the slope of the (O/H)_0_-V_rot_ relation is steeper for galaxies with V_rot_<=V_rot_^*^. The mean scatter of the central abundances around this relation is 0.053 dex. The relation between the abundance at the optical radius of a galaxy and its rotation velocity is similar; the mean scatter in abundances around this relation is 0.081 dex. The radial abundance gradient expressed in dex/kpc flattens with the increase of the rotation velocity. The slope of the relation is very low for galaxies with V_rot_>=V_rot_^*^. The abundance gradient expressed in dex/R_25_ is roughly constant for galaxies with V_rot_<=V_rot_^*^, flattens towards V_rot_^*^, and then again is roughly constant for galaxies with V_rot_>=V_rot_^*^. The change of the gradient expressed in terms of dex/h_d_ (where h_d_ is the disc scale length), in terms of dex/R_e,d_ (where R_e,d_ is the disc effective radius), and in terms of dex/R_e,g_ (where R_e,g_ is the galaxy effective radius) with rotation velocity is similar to that for gradient in dex/R_25_. The relations between abundance characteristics and other basic parameters (stellar mass, luminosity, and radius) are also considered.2019A&A...623A.122Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/623/A122CatalogResearchIsServedByTAP VizieR generic servicerelated-tohttps://www.sdss.org/surveys/manga : MaNGA Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/623/A122https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/623/A122http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/623/A122https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/623/A122https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/623/A122http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/623/A122GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/623/A122/tablea1Properties of our MaNGA galaxiesNameMaNGA number, NNNN NNNNNmeta.id;meta.maincharVrotMaximum value of the rotation velocity within the optical radiuskm/sphys.veloc.rotat;stat.maxfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDistGalaxy distanceMpcpos.distance;pos.heliocentricfloatPAPosition angle of the major axisdegpos.posAngfloatinclGalaxy inclination angledegsrc.orbital.inclinationfloatlogMspSpectroscopic stellar maslog(solMass)phys.massfloatlogLBLuminosity in B bandlog(solLum)phys.luminosity;em.opt.BfloatR25Optical radiuskpcphys.size.radiusfloathdDisc scale lengthkpcphys.angSize;srcfloat12+log(O/H)0Central oxygen abundancephys.abundfloat12+log(O/H)R25Oxygen abundance at the optical radiusphys.abundfloatNANumber of points (spaxels) with a measured rotation velocitymeta.numberintNBNumber of points used in derivation of the final rotation curvemeta.numberint