J/A+A/635/A129ivo://CDS.VizieR/J/A+A/635/A129doi:10.26093/cds/vizier.36350129CDSKrajnovic D.Ural U.Kuntschner H.Goudfrooij P.Wolfe M.,Cappellari M.Davies R.de Zeeuw P.T.Duc P.-A.Emsellem E.Karick A.,McDermid R.M.Mei S.Naab T.2021-05-11T14:57:41Z2020-03-19T06:12:29ZCDS support team

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

cds-question@unistra.frgalaxiescatalogschemical-abundancesWe study the evidence for a diversity of formation processes in early-type galaxies by presenting the first complete volume-limited sample of slow rotators with both integral-field kinematics from the ATLAS^3D^ Project and high spatial resolution photometry from the Hubble Space Telescope. Analysing the nuclear surface brightness profiles of 12 newly imaged slow rotators, we classify their light profiles as core-less, and place an upper limit to the core size of about 10 pc. Considering the full magnitude and volume-limited ATLAS^3D^ sample, we correlate the presence or lack of cores with stellar kinematics, including the proxy for the stellar angular momentum ({lambda}_Re_) and the velocity dispersion within one half-light radius ({sigma}_e_), stellar mass, stellar age, {alpha}-element abundance, and age and metallicity gradients. More than half of the slow rotators have core-less light profiles, and they are all less massive than 10^11^M_{sun}_. Core-less slow rotators show evidence for counter-rotating flattened structures, have steeper metallicity gradients, and a larger dispersion of gradient values ({Delta}[Z/H]=-0.42+/-0.18) than core slow rotators ({Delta}[Z/H]=-0.23+/-0.07). Our results suggest that core and core-less slow rotators have different assembly processes, where the former, as previously discussed, are the relics of massive dissipation-less merging in the presence of central supermassive black holes. Formation processes of core-less slow rotators are consistent with accretion of counter-rotating gas or gas-rich mergers of special orbital configurations, which lower the final net angular momentum of stars, but support star formation. We also highlight core fast rotators as galaxies that share properties of core slow rotators (i.e. cores, ages, {sigma}_e_, and population gradients) and core-less slow rotators (i.e. kinematics, {lambda}_Re_, mass, and larger spread in population gradients). Formation processes similar to those for core-less slow rotators can be invoked to explain the assembly of core fast rotators, with the distinction that these processes form or preserve cores.2020A&A...635A.129Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/635/A129CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)J/MNRAS/448/3484 : ATLAS3D Project. XXX (McDermid+, 2015)J/MNRAS/433/2812 : ATLAS3D project. XXIII. (Krajnovic+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/635/A129https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/635/A129http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/635/A129https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/635/A129https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/635/A129http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/635/A129GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/635/A129/tableb1 (Metallicity and age gradients for ATLAS^3D^ sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/635/A129/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/635/A129/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/635/A129/tableb1?GETtext/xml+votable180.050000true146.4722333-0.26912220.0055555555555555565/4581 6941 6/664 697 2145 2374 4439 4447 4565 4807 4829 4840 4869 4930 4989 5021 5075 5125 5134 5182 5196 5198 5288 5398 5429 5474 5599 5608 5745 5773 5975 5999 6012 6082 6087 6089-6090 6093 6097 6099 6103 6162 7214 7287 7355 7374 7385 7424 7442 7460 7560 8193 8195-8197 8208 8228 8533 9186 10454 10501 10523 10551 10616 10637 10714 10720 10739 10845 10924 10980 11026 11246 11253 11418 11435 11443 11457 11776 11791 11800 11824 13336 13401 15056 15204 17744 17761 18002 18209 18269 18755 18766 19442 20014 20070 20101 22740 22914 23177-23178 25571 25893 25907 25979 26055 26065 26125 26149 26157 26166 26173 26210 26285 26307 26313 26316 26361-26362 26530 26542 27079 27135 27186 27199 27255 27367 27480 27515 27518 27578 27582 27595 27604 27669 27671 27712-27714 27718-27720 27722-27723 27728 27734-27736 27738-27739 27743 27755 27758 27773-27774 27802 27857 27861 27905 27907-27908 27913-27915 27921 27931 27936 27938 27944 27946 28033 28037-28038 28045 28142 28200 28221 28264 28300 28311 28362 28491 28495 28524 28538 28601 28653 31340 31404 31418 31453-31454 31499 31624 32168-32169 32482 32539 36819 36831 40952https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/635/A129?format=asciidefaultJ/A+A/635/A129/tableb1Metallicity and age gradients for ATLAS^3D^ samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyName of the galaxymeta.id;meta.maincharD[Z/H]Metallicity gradient as defined by Eq.1 (1)arith.grad;phys.abund.Zfloate_D[Z/H]Uncertainty on the gradient obtained from weighted linear regression fits to the metallicity profilesstat.error;src.redshiftfloatDAgeAge gradient as defined by Eq.1 (1)arith.grad;time.agefloate_DAgeUncertainty on the gradient obtained from weighted linear regression fits to the age profilesstat.errorfloatHST[0/2]? HST flag (2)meta.codeintnullableSimbadSimbad column added by the CDSmeta.ref.urlchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main