J/MNRAS/471/59ivo://CDS.VizieR/J/MNRAS/471/59doi:10.26093/cds/vizier.74710059CDSLani C.Netzer H.Lutz D.2024-08-17T20:20:40Z2020-07-03T13:56:56ZCDS support team

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

cds-question@unistra.fractive-galactic-nucleiquasarsspectral-energy-distributionWe present a new analysis of the Palomar-Green quasar sample based on Spitzer and Herschel observations. (i) Assuming polycyclic aromatic hydrocarbon (PAH)-based star formation luminosities (L_SF_) similar to Symeonidis et al. (S16, 2016MNRAS.459..257S), we find mean and median intrinsic active galactic nucleus (AGN) spectral energy distributions (SEDs). These, in the far-infrared (FIR), appear hotter and significantly less luminous than the S16 mean intrinsic AGN SED. The differences are mostly due to our normalization of the individual SED that properly accounts for a small number of very FIR-luminous quasars. Our median, PAH-based SED represents ~6 per cent increase on the 1-243{mu}m luminosity of the extended Mor & Netzer (EM12, 2012MNRAS.420..526M) torus SED, while S16 find a significantly larger difference. It requires large-scale dust with T~20-30K, which, if optically thin and heated by the AGN, would be outside the host galaxy. (ii) We also explore the black hole and stellar mass growths, using L_SF_ estimates from fitting Herschel/PACS observations after subtracting the EM12 torus contribution. We use rough estimates of stellar mass, based on scaling relations, to divide our sample into groups: on, below and above the star formation main sequence (SFMS). Objects on the SFMS show a strong correlation between star formation luminosity and AGN bolometric luminosity, with a logarithmic slope of ~0.7. Finally, we derive the relative duty cycles of this and another sample of very luminous AGN at z=2-3.5. Large differences in this quantity indicate different evolutionary pathways for these two populations characterized by significantly different black hole masses.2017MNRAS.471...59Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/471/59CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJ/269/352 : Quasar evolution (Schmidt+, 1983)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/471/59https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/471/59http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/471/59https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/471/59https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/471/59http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/471/59GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/471/59/table1 (Quantities for our PG QSOs sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/471/59/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/471/59/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/471/59/table1?GETtext/xml+votable180.050000true1.581320.20290.0055555555555555566/4215 4506 5091 5244 5437 5481 5576 5687 5731 6028 7246 7998 8017 8071 8299 8528 8636 8641 8845 8881 8893 8906 8927 8941 9018 9181 9194 9262 9959 10039 10162 10217 10269 10472 10691 10694 10709 11217 11354 11388 11668 11829 11924 12317 12380 12632 17819 18127 18918 19287 19315 19416 19433 19567 19700 19730 19746 19767 19883 19932 25403 25735 25742 25965 26310 26509 26736 26859 26902 27023 27025 27227 27293 27349 27580 27720 27848 27862 28060 28164 28356 28471 31650 44785 44988https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/471/59?format=asciidefaultJ/MNRAS/471/59/table1Quantities for our PG QSOs samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameNamemeta.id;meta.maincharn_NameNote on Name (1)meta.notecharONameOther Namemeta.idcharRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainzRedshiftsrc.redshiftfloatlogL5100Uncorrected for host galaxy contamination which, in our sample, we estimate to be typically ~20 per centlog(1e-07W)phys.luminosity;em.optfloatlogMBHBlack hole masslog(solMass)phys.massfloatlogL5um5um luminositylog(1e-07W)phys.luminosity;em.IRfloate_logL5umrms uncertainty on logL5umlog(1e-07W)stat.errorfloatlogLSF? Star formation luminositylog(1e-07W)phys.luminosityfloatnullablee_logLSF? rms uncertainty on logLSFlog(1e-07W)stat.errorfloatnullableLoc[0/2]? Location w.r.t. SFMS (2)meta.codeintnullableTemp[1/3]? Choice of EM12 template (3)meta.id;stat.fitintnullableJ/MNRAS/471/59/tabled1Data for the intrinsic AGN SEDs considered in our workrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaRest wavelengthumem.wlfloatlamndaLl1Extended EM12- median ({lambda}L_{lambda}_, arbitrary units)stat.fit.paramfloatlambdaLl1-25Extended EM12- 25th percentile ({lambda}L_{lambda}_, arbitrary units)stat.fit.paramfloatlambdaLl1-75Extended EM12- 75th percentile ({lambda}L_{lambda}_, arbitrary units)stat.fit.paramfloatlambdaLl2? PAH-based median intrinsic AGN SED for full PG sample ({lambda}L_{lambda}_, arbitrary units)stat.fit.paramdoublenullablelambdaLl2-25? PAH-based 25th percentile for full PG sample ({lambda}L_{lambda}_, arbitrary units)stat.fit.paramdoublenullablelambdaLl2-75? PAH-based 75th percentile for full PG sample ({lambda}L_{lambda}_, arbitrary units)stat.fit.paramdoublenullablelambdaLl3? PAH-based median intrinsic AGN SED for the top 1 sigma sources (lambdaL_{lambda}_, arbitrary units)stat.fit.paramdoublenullable