J/MNRAS/466/2570ivo://CDS.VizieR/J/MNRAS/466/2570doi:10.26093/cds/vizier.74662570CDSBelfiore F.Maiolino R.Maraston C.Emsellem E.Bershady M.A.,Masters K.L.Bizyaev D.Boquien M.Brownstein J.R.Bundy K.,Diamond-Stanic A.M.Drory N.Heckman T.M.Law D.R.Malanushenko O.,Oravetz A.Pan K.Roman-Lopes A.Thomas D.Weijmans A.-M.,Westfall K.B.Yan R.2024-08-17T20:17:45Z2019-11-27T14:28:31ZCDS support team

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

cds-question@unistra.frgalaxiesredshiftedgalaxy-classification-systemsvisible-astronomysloan-photometryUsing spatially resolved spectroscopy from SDSS-IV MaNGA we have demonstrated that low ionization emission-line regions (LIERs) in local galaxies result from photoionization by hot evolved stars, not active galactic nuclei, hence tracing galactic region hosting old stellar population where, despite the presence of ionized gas, star formation is no longer occurring. LIERs are ubiquitous in both quiescent galaxies and in the central regions of galaxies where star formation takes place at larger radii. We refer to these two classes of galaxies as extended LIER (eLIER) and central LIER (cLIER) galaxies, respectively. cLIERs are late-type galaxies primarily spread across the green valley, in the transition region between the star formation main sequence and quiescent galaxies. These galaxies display regular disc rotation in both stars and gas, although featuring a higher central stellar velocity dispersion than star-forming galaxies of the same mass. cLIERs are consistent with being slowly quenched inside-out; the transformation is associated with massive bulges, pointing towards the importance of bulge growth via secular evolution. eLIERs are morphologically early types and are indistinguishable from passive galaxies devoid of line emission in terms of their stellar populations, morphology and central stellar velocity dispersion. Ionized gas in eLIERs shows both disturbed and disc-like kinematics. When a large-scale flow/rotation is observed in the gas, it is often misaligned relative to the stellar component. These features indicate that eLIERs are passive galaxies harbouring a residual cold gas component, acquired mostly via external accretion. Importantly, quiescent galaxies devoid of line emission reside in denser environments and have significantly higher satellite fraction than eLIERs. Environmental effects thus represent the likely cause for the existence of line-less galaxies on the red sequence.2017MNRAS.466.2570Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/466/2570CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/435/2835 : Morphological types from Galaxy Zoo 2 (Willett+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/466/2570https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/466/2570http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/466/2570https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/466/2570https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/466/2570http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/466/2570GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/466/2570/tableb (Identifiers and fundamental properties (table B1) and Photometric and morphological properties (table B2) of the galaxy used in this work)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/466/2570/tableb?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/466/2570/tableb?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/466/2570/tableb?GETtext/xml+votable180.050000true259.1747130656.927791940.0055555555555555565/1279 1382 1389 1450 1599 1638-1639 1641 1644 1646 1685 1728 1793 1808 2737 2758 3099 5801 6/5463 5469-5471 5492-5494 5523 5526-5527 5532-5533 5535 5552 5563-5565 5567 5717 5719 5738-5739 5741-5743 5757-5759 5797-5799 5804-5806 5808 5810 5816 5819 5825 5828 5841 5844-5846 5857 5859 5862 5865 5867-5868 5870 5888-5890 6367 6385 6387 6389-6391 6393 6395 6541 6543 6547 6560 6571-6574 6580 6582-6583 6588-6589 6591 6916-6917 6928-6930 6932-6933 7169 7185-7186 7215 7224-7226 7230 7236-7237 7301 7308-7309 7311 7313-7315 7318 7320 7323 9880 9882-9883 9893 9895 9904-9906 10092-10093 10095 10179-10180 10182 10267 10270-10271 10292-10293 10312 10336 10689-10692 10694-10696 10698 10701 10704 10707-10708 10710 10712-10713 10716 10855 10857 10859 10861-10863 10866-10867 10872-10874 10926-10927 10934 10937 10939-10941 10957 10962-10963 10978 11023 11036-11037 11045 12375 12380-12381 12383 12387 12390-12391 12395 12552 12554 19380 19382-19383 19387 19389-19390 19432 23182-23183 23194 23201 23216 23218https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/466/2570?format=asciiOpticaldefaultJ/MNRAS/466/2570/tablebIdentifiers and fundamental properties (table B1) and Photometric and morphological properties (table B2) of the galaxy used in this workNSANSA ID (1)meta.idintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMaNGAMaNGA ID (NN-NNNNN)meta.id;meta.maincharRAJ2000NSA right ascension (J2000) (1)degpos.eq.ra;meta.mainDEJ2000NSA declination (J2000) (1)degpos.eq.dec;meta.mainzNSA redshift (1)src.redshiftfloatPlateMaNGA platemeta.noteintIFUMaNGA ifudesignmeta.idintlogM*NSA Log of stellar mass, from K-correction, {omega}_M_=0.3, H_0_=70log(solMass)phys.massfloatlogSFR? MaNGA star formation rate, calculated following Appendix Alog(solMass.yr**-1)meta.idfloatnullablen_logSFR[i] i for infinitymeta.notecharReNSA, Sersic effective radiusarcsecphys.angSizefloatClassMaNGA Emission line class, from LIER Paper I (Belfiore et al., 2016MNRAS.461.3111B) (2)meta.code.classcharb/aNSA, Sersic b/a axis ratiophys.angSize;arith.ratiofloatnNSA, Sersic n indexstat.fit.paramfloatphiNSA, Sersic position angledegpos.posAngfloatR90/R50NSA, Concentration index, C=R_90_/R_50_meta.code;spect.indexfloatGZPdiscGalaxy Zoo 2, p_disc, from Willet et al., 2013, Cat. J/MNRAS/435/2835src.class.starGalaxyfloatsigma*? MaNGA, stellar velocity dispersion within 0.5Rekm/sphys.veloc.dispersionfloatnullableNUV-rNSA, NUV-r colour indexmagphot.color;em.UV;em.optfloatu-rNSA, u-r colour indexmagphot.colorfloatg-rNSA, g-r colour indexmagphot.color;em.opt.B;em.opt.RfloatSimbadSimbad column added by the CDSmeta.ref.urlchar