J/A+A/561/A140ivo://CDS.VizieR/J/A+A/561/A140doi:10.26093/cds/vizier.35610140CDSBusch G.Zuther J.Valencia-S. M.Moser L.Fischer S.Eckart A.,Scharwachter J.Gadotti D.A.Wisotzki L.2017-11-06T12:23:24Z2014-01-28T07:29:10ZCDS support team

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

cds-question@unistra.frquasarsactive-galactic-nucleiseyfert-galaxiesinfrared-photometryRecognizing the properties of the host galaxies of quasi-stellar objects (QSOs) is essential to understand the suspected coevolution of central supermassive black holes (BHs) and their host galaxies. We selected a subsample of the Hamburg/ESO survey for bright UV-excess QSOs, containing only the 99 nearest QSOs with redshift z<=0.06, that are close enough to allow detailed structural analysis. From this "low-luminosity type-1 QSO sample", we observed 20 galaxies and performed aperture photometry and bulge-disk-bar-AGN-decomposition with BUDDA on near-infrared J, H, K band images. From the photometric decomposition of these 20 objects and visual inspection of images of another 26, we find that ~50% of the hosts are disk galaxies and most of them (86%) are barred. Stellar masses, calculated from parametric models based on inactive galaxy colors, range from 2x10^9^M_{sun}_ to 2x10^11^M_{sun}_. Black hole masses measured from single epoch spectroscopy range from 1x10^6^M_{sun}_ to 5x10^8^M_{sun}_. In comparison to higher luminosity QSO samples, LLQSOs tend to have lower stellar and BH masses. Also, in the effective radius vs. mean surface-brightness projection of the fundamental plane, they lie in the transition area between luminous QSOs and "normal" galaxies. This can be seen as further evidence that they can be pictured as a "bridge" between the local Seyfert population and luminous QSOs at higher redshift. Eleven low-luminosity QSOs for which we have reliable morphological decompositions and BH mass estimations lie below the published BH mass vs. bulge luminosity relations for inactive galaxies. This could be partially explained by bulges of active galaxies containing much younger stellar populations than bulges of inactive galaxies. Also, one could suspect that their BHs are undermassive. This might hint at the growth of the host spheroid to precede that of the BH.2014A&A...561A.140Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/561/A140CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/561/A140https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/561/A140http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/561/A140https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/561/A140https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/561/A140http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/561/A140GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/561/A140/qsos (The observed galaxies, and their BUDDA fit parameters J, H and K bands)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/561/A140/qsos?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/561/A140/qsos?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/561/A140/qsos?GETtext/xml+votable180.050000true9.8158333-51.28390.0055555555555555566/16694 18001 18683 19077 24941 25051 25619 25661 25735 34845 35001 36015 36619 44722 44971 45852 46709 46831 46873 46988https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/561/A140?format=asciiInfrareddefaultJ/A+A/561/A140/qsosThe observed galaxies, and their BUDDA fit parameters J, H and K bandszRedshiftsrc.redshiftfloatID[5/89] ID number in LLQSO samplemeta.idintprimaryNameHamburg/ESO survey name (HEHHMM+DDMM)meta.id;meta.maincharprimaryRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainBmagB_J_ nuclear magnitudemagphot.mag;em.opt.Bfloatn_Bmag[a] a: magnitude from NEDmeta.notecharBMAGAbsolute B_J_ nuclear magnitudemagphys.magAbsfloatn_BMAG[a] a: magnitude from NEDmeta.notecharJseeSeeing in the J bandarcsecinstr.obsty.seeingfloatHseeSeeing in the H bandarcsecinstr.obsty.seeingfloatKseeSeeing in the K bandarcsecinstr.obsty.seeingfloatJskySky deviation in the J bandmag.arcsec**-2stat.stdev;phot.mag.sb;em.IR.JfloatHskySky deviation in the H bandmag.arcsec**-2stat.stdev;phot.mag.sb;em.IR.HfloatKskySky deviation in the K bandmag.arcsec**-2stat.stdev;phot.mag.sb;em.IR.KfloatSimbadSimbad column added by the CDSmeta.ref.urlcharNEDSimbad column added by the CDSmeta.ref.urlcharmu0(J)? Central surface brightness of diskmag.arcsec**-2phot.mag.sbfloatnullableh(J)? Scale length of diskarcsecsrc.morph.scLengthfloatnullablemue(J)? Effective surface brightness of bulgemag.arcsec**-2phot.mag.sbfloatnullablere(J)? Effective radius of bulgearcsecphys.angSizefloatnullablen(J)? Sersic index of bulgestat.fit.paramfloatnullableB/T(J)? Bulge-to-total fractionphys.luminosity;arith.ratiofloatnullableD/T(J)? Disk-to-total fractionphys.luminosity;arith.ratiofloatnullableBar/T(J)? Bar-to-total fractionphys.luminosity;arith.ratiofloatnullableA/T(J)? AGN-to-total fractionphys.luminosity;arith.ratiofloatnullablemu0(H)? Central surface brightness of diskmag.arcsec**-2phot.mag.sbfloatnullableh(H)? Scale length of diskarcsecsrc.morph.scLengthfloatnullablemue(H)? Effective surface brightness of bulgemag.arcsec**-2phot.mag.sbfloatnullablere(H)? Effective radius of bulgearcsecphys.angSizefloatnullablen(H)? Sersic index of bulgestat.fit.paramfloatnullableB/T(H)? Bulge-to-total fractionphys.luminosity;arith.ratiofloatnullableD/T(H)? Disk-to-total fractionphys.luminosity;arith.ratiofloatnullableBar/T(H)? Bar-to-total fractionphys.luminosity;arith.ratiofloatnullableA/T(H)? AGN-to-total fractionphys.luminosity;arith.ratiofloatnullablemu0(K)? Central surface brightness of diskmag.arcsec**-2phot.mag.sbfloatnullableh(K)? Scale length of diskarcsecsrc.morph.scLengthfloatnullablemue(K)? Effective surface brightness of bulgemag.arcsec**-2phot.mag.sbfloatnullablere(K)? Effective radius of bulgearcsecphys.angSizefloatnullablen(K)? Sersic index of bulgestat.fit.paramfloatnullableB/T(K)? Bulge-to-total fractionphys.luminosity;arith.ratiofloatnullableD/T(K)? Disk-to-total fractionphys.luminosity;arith.ratiofloatnullableBar/T(K)? Bar-to-total fractionphys.luminosity;arith.ratiofloatnullableA/T(K)? AGN-to-total fractionphys.luminosity;arith.ratiofloatnullableInstInstrumentmeta.id;instrchar