J/MNRAS/446/4039ivo://CDS.VizieR/J/MNRAS/446/4039doi:10.26093/cds/vizier.74464039CDSErwin P.Saglia R.P.Fabricius M.Thomas J.Nowak N.Rusli S.,Bender R.Vega Beltran J.C.Beckman J.E.2024-08-14T20:19:19Z2017-11-13T11:20:02ZCDS support team

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

cds-question@unistra.frgalaxiesspectroscopyradial-velocitygalaxy-kinematicsWe present an analysis of nine S0-Sb galaxies which have (photometric) bulges consisting of two distinct components. The outer component is a flattened, kinematically cool, disc-like structure: a 'discy pseudo-bulge'. Embedded inside is a rounder, kinematically hot spheroidal structure: a `classical bulge'. This indicates that pseudo-bulges and classical bulges are not mutually exclusive phenomena: some galaxies have both. The discy pseudo-bulges almost always consist of an exponential disc (scalelengths=125-870 pc, mean size ~440 pc) with one or more disc-related subcomponents: nuclear rings, nuclear bars, and/or spiral arms. They constitute 11-59 percent of the galaxy stellar mass (mean PB/T=0.33), with stellar masses ~7x10^9^-9x10^10^ M_{sun}_. The classical-bulge components have Sersic indices of 0.9-2.2, effective radii of 25-430 pc and stellar masses of 5x10^8^-3x10^10^ M_{sun}_; they are usually <10 percent of the galaxy's stellar mass (mean B/T=0.06). The classical bulges do show rotation, but are clearly kinematically hotter than the discy pseudo-bulges. Dynamical modelling of three systems indicates that velocity dispersions are isotropic in the classical bulges and equatorially biased in the discy pseudo-bulges. In the mass-radius and mass-stellar mass density planes, classical-bulge components follow sequences defined by ellipticals and (larger) classical bulges. Discy pseudo-bulges also fall on this sequence; they are more compact than large-scale discs of similar mass. Although some classical bulges are quite compact, they are as a class clearly distinct from nuclear star clusters in both size and mass; in at least two galaxies they coexist with nuclear clusters. Since almost all the galaxies in this study are barred, they probably also host boxy/peanut-shaped bulges (vertically thickened inner parts of bars). NGC 3368 shows isophotal evidence for such a zone just outside its discy pseudo-bulge, making it a clear case of a galaxy with all three types of 'bulge'.2015MNRAS.446.4039Ehttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/446/4039CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/136/773 : Structure of classical bulges and pseudobulges (Fisher+, 2008)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/446/4039https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/446/4039http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/446/4039https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/446/4039https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/446/4039http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/446/4039GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/446/4039/galaxy (List of galaxy)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/446/4039/galaxy?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/446/4039/galaxy?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/446/4039/galaxy?GETtext/xml+votable180.050000true141.077287534.513377780.0055555555555555566/4989 27766https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/446/4039?format=asciiOpticaldefaultJ/MNRAS/446/4039/galaxyList of galaxyrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGalaxy Namemeta.id;meta.maincharRAJ2000Simbad Hour of Right Ascension (J2000)pos.eq.ra;meta.mainDEJ2000Simbad Degree of Declination (J2000)pos.eq.dec;meta.mainSimbadSimbad column added by the CDSmeta.ref.urlcharJ/MNRAS/446/4039/tableb2Major-axis stellar kinematics for NGC 2859 and NGC 4371recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNGC[2859/4371] Galaxy namemeta.id;meta.mainintPA[85/92] Position angle of the telescopedegpos.posAngintRad[] Radius along the major axisarcsecphys.angSizefloatRVRadial velocitykm/sphys.veloc;pos.heliocentricfloate_RVUncertainty in RVkm/sstat.errorfloatsigmaVelocity dispersionkm/sphys.veloc.dispersionfloate_sigmaUncertainty in sigmakm/sstat.errorfloath3Gauss-Hermite coefficient h_3_stat.fit.paramfloate_h3Uncertainty in h3stat.errorfloath4Gauss-Hermite coefficient h_4_stat.fit.paramfloate_h4Uncertainty in h4stat.errorfloat