J/MNRAS/454/2050ivo://CDS.VizieR/J/MNRAS/454/2050doi:10.26093/cds/vizier.74542050CDSFogarty L.M.R.Scott N.Owers M.S.Croom S.M.Bekki K.,Houghton R.C.W.van de Sande J.D'Eugenio F.Cecil G.N.Colless M.M.,Bland-Hawthorn J.Brough S.Cortese L.Davies R.L.Jones D.H.,Pracy M.Allen J.T.Bryant J.J.Goodwin M.Green A.W.,Konstantopoulos I.S.Lawrence J.S.Lorente N.P.F.Richards S.,Sharp R.G.2024-08-15T20:15:53Z2016-09-15T15:00:36ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxiescatalogsgalaxy-classification-systemsWe present the SAMI Pilot Survey, consisting of integral field spectroscopy of 106 galaxies across three galaxy clusters, Abell 85, Abell 168 and Abell 2399. The galaxies were selected by absolute magnitude to have Mr<-20.25mag. The survey, using the Sydney-AAO Multi-object Integral field spectrograph (SAMI), comprises observations of galaxies of all morphological types with 75 per cent of the sample being early-type galaxies (ETGs) and 25 per cent being late-type galaxies (LTGs). Stellar velocity and velocity dispersion maps are derived for all 106 galaxies in the sample. The {lambda}_R_ parameter, a proxy for the specific stellar angular momentum, is calculated for each galaxy in the sample. We find a trend between {lambda}_R_ and galaxy concentration such that LTGs are less concentrated higher angular momentum systems, with the fast-rotating ETGs (FRs) more concentrated and lower in angular momentum. This suggests that some dynamical processes are involved in transforming LTGs to FRs, though a significant overlap between the {lambda}_R_ distributions of these classes of galaxies implies that this is just one piece of a more complicated picture. We measure the kinematic misalignment angle, {Psi}, for the ETGs in the sample, to probe the intrinsic shapes of the galaxies. We find the majority of FRs (83 per cent) to be aligned, consistent with them being oblate spheroids (i.e. discs). The slow rotating ETGs (SRs), on the other hand, are significantly more likely to show kinematic misalignment (only 38 per cent are aligned). This confirms previous results that SRs are likely to be mildly triaxial systems.2015MNRAS.454.2050Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/454/2050CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/454/2050https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/454/2050http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/454/2050https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/454/2050https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/454/2050http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/454/2050GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/454/2050/tablea1 (The 106 galaxies in the SAMI Pilot Survey)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/454/2050/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/454/2050/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/454/2050/tablea1?GETtext/xml+votable180.050000true9.7782083-8.79952780.0055555555555555566/17236-17237 17239 17920 18009 18011 18605 18607 18618 18949 18960https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/454/2050?format=asciiOpticaldefaultJ/MNRAS/454/2050/tablea1The 106 galaxies in the SAMI Pilot SurveyepsEllipticitysrc.ellipticityfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeqGalaxy sequential numbermeta.recordintGalaxyGalaxy name (JHHMMSS.ss+DDMMSS.s)meta.id;meta.maincharn_Galaxy[*] note on eps and PA (1)meta.notecharClusterCluster sample the galaxy belongs to (ABELLNNNN)src.samplecharMemb[0/1] shows whether the galaxy was deemed to be a cluster member (1) or not (0)meta.code.memberintRMAGAbsolute R magnitude from NYU-VAGC (Blanton et al., 2005AJ....129.2562B)magphys.magAbs;em.opt.RfloatPAphotPhotometric position angledegpos.posAngfloatPAkinKinematic position angledegpos.posAngfloatPsiMisalignment angledeginstr.offsetfloatlambdaR{lambda}_R_ parameter, proxy for the specific stellar angular momentumstat.fit.paramfloate_lambdaRrms uncertainty on lambdaRstat.errorfloatClassKinematic classification for the ETGs and morphological classification for the LTGssrc.classcharRadFiducial radius at which {lambda}R was measured (Re or Re/2)stat.fit.paramchar_RAPosition from galaxy name (right ascension part)degpos.eq.ra;meta.main_DEPosition from galaxy name (declination part)degpos.eq.dec;meta.main