J/MNRAS/445/2385ivo://CDS.VizieR/J/MNRAS/445/2385doi:10.26093/cds/vizier.74452385CDSden Brok M.Peletier R.F.Seth A.Balcells M.Dominguez L.,Graham A.W.Carter D.Erwin P.Ferguson H.C.Goudfrooij P.Guzman R.,Hoyos C.Jogee S.Lucey J.Phillipps S.Puzia T.Valentijn E.,Kleijn G.V.Weinzirl T.2024-08-14T20:18:21Z2015-10-09T16:29:56ZCDS support team

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

cds-question@unistra.frgalaxiesphotometrystellar-associationshst-photometryWe present scaling relations between structural properties of nuclear star clusters and their host galaxies for a sample of early-type dwarf galaxies observed as part of the Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) Coma Cluster Survey. We have analysed the light profiles of 200 early-type dwarf galaxies in the magnitude range 16.0<m_F814W_<22.6mag, corresponding to -19.0<M_F814W_<-12.4mag. Nuclear star clusters are detected in 80 percent of the galaxies, thus doubling the sample of HST-observed early-type dwarf galaxies with nuclear star clusters. We confirm that the nuclear star cluster detection fraction decreases strongly towards faint magnitudes. The luminosities of nuclear star clusters do not scale linearly with host galaxy luminosity. A linear fit yields L_nuc_~L_gal_^0.57^+/-0.05. The nuclear star cluster-host galaxy luminosity scaling relation for low-mass early-type dwarf galaxies is consistent with formation by globular cluster (GC) accretion. We find that at similar luminosities, galaxies with higher Sersic indices have slightly more luminous nuclear star clusters. Rounder galaxies have on average more luminous clusters. Some of the nuclear star clusters are resolved, despite the distance of Coma. We argue that the relation between nuclear star cluster mass and size is consistent with both formation by GC accretion and in situ formation. Our data are consistent with GC inspiralling being the dominant mechanism at low masses, although the observed trend with Sersic index suggests that in situ star formation is an important second-order effect.2014MNRAS.445.2385Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/445/2385CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/411/2439 : Coma Treasury Survey. Structural parameters (Hoyos+, 2011)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/445/2385https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/445/2385http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/445/2385https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/445/2385https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/445/2385http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/445/2385GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/445/2385/tablea1 (Structural parameters of galaxies used in the paper)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/445/2385/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/445/2385/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/445/2385/tablea1?GETtext/xml+votable180.050000true195.077328.09720.005555555555555556Cone search capability for table J/MNRAS/445/2385/tablea2 (Sources excluded from the analysis)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/445/2385/tablea2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/445/2385/tablea2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/445/2385/tablea2?GETtext/xml+votable180.050000true195.055928.05330.0055555555555555566/10378-10379 10400-104012.0401237512456292e-19 2.706461185444514e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/445/2385?format=asciidefaultJ/MNRAS/445/2385/tablea1Structural parameters of galaxies used in the paperSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGalaxy name (1)meta.id;meta.maincharRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainMm[0/3] Coma membership class, 1=yes (G1)srcintF814WGalaxy F814W magnitude (AB system)magphot.mag;em.opt.Ifloate_F814Wrms uncertainty on F814WGmagstat.errorfloatn[0.4/5.9] Sersic index numberstat.fit.paramfloate_n[0.01/0.26] rms uncertainty on nstat.errorfloatF814Wn? Nuclear F814W magnitude (AB system)magphot.mag;em.opt.Ifloatnullablee_F814Wn? rms uncertainty on F814WNmagstat.errorfloatnullableFWHM[0.8/3.7]? Full width at half-maximumpixspect.line.widthfloatnullablee_FWHM[0/2.3]? rms uncertainty on FWHMpixstat.error;phys.angSizefloatnullableJ/MNRAS/445/2385/tablea2Sources excluded from the analysisTileTile number(s)meta.id;obscharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintName? Galaxy name (1)meta.id;meta.maincharMm[0/3] Coma membership class, 1=yes (G1)srcintTypeMorphological typesrc.morph.typecharcz[4684/9623]? Heliocentric redshiftkm/ssrc.redshift;pos.heliocentricfloatnullableRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainF814WF814W magnitudemagphot.mag;em.opt.IfloatNotesComments on galaxymeta.notechar