J/A+A/671/A34ivo://CDS.VizieR/J/A+A/671/A34doi:10.26093/cds/vizier.36710034CDSSaccheo I.Bongiorno A.Piconcelli E.Testa V.Bischetti M.Bisogni S.,Bruni G.Cresci G.Feruglio C.Fiore F.Grazian A.Luminari A.,Lusso E.Mainieri V.Maiolino R.Marconi A.Ricci F.Tombesi F.,Travascio A.Vietri G.Vignali C.Zappacosta L.La Franca F.2023-08-25T10:46:54Z2023-03-02T09:03:20ZCDS support team

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

cds-question@unistra.frquasarsvisible-astronomysloan-photometryinfrared-photometryradio-sourcesx-ray-sourcesHyper-luminous Quasi-Stellar Objects (QSOs) represent the ideal laboratory to investigate Active Galactic Nuclei (AGN) feedback mechanism since their formidable energy release causes powerful winds at all scales and thus the maximum feedback is expected. We aim at deriving the mean Spectral Energy Distribution (SED) of a sample of 85 WISE-SDSS Selected Hyper-luminous (WISSH) quasars. Since the SED provides a direct way to investigate the AGN structure, our goal is to understand if quasars at the bright end of the luminosity function have peculiar properties compared to the bulk of the population. We built a mean intrinsic SED after correcting for the dust extinction, absorption and emission lines and intergalactic medium absorption. We also derived bolometric, IR band and monochromatic luminosities together with bolometric corrections at lambda=5100{AA} and 3 micron. We define a new relation for the 3 micron bolometric correction. We find that the mean SED of hyper-luminous WISSH QSOs is different from that of less luminous sources, i.e. a relatively lower X-ray emission and a near and mid IR excess which can be explained assuming a larger dust contribution. WISSH QSOs have stronger emission from both warm and very hot dust, the latter being responsible for shifting the typical dip of the AGN SED from 1.3 to 1.1 micron. We also derived the mean SEDs of two sub-samples created according to the presence of Broad Absorption Lines and equivalent width of CIV line. We confirm that BALs are X-ray weak and that they have a reddened UV-optical continuum. We also find that BALs tend to have stronger emission from the hot dust component. This analysis suggests that hyper-luminous QSOs have a peculiar SED compared to less luminous objects. It is therefore critical to use SED templates constructed exclusively from very bright quasars samples when dealing with particularly luminous sources.2023A&A...671A..34Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/671/A34CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/635/A157 : QSO J1538+0855 MUSE datacube (Travascio+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/671/A34https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/671/A34http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/671/A34https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/671/A34https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/671/A34http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/671/A34GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap3.2031150387835462e-22 6.090060298487514e-19X-rayOpticalInfraredRadiodefaultJ/A+A/671/A34/table2Photometric data of the WISSH sampleW1magWISE W1-band (3.4um) magnitudemagphot.mag;em.IR.3-4umfloate_W1magrms uncertainty on W1-band magnitudemagstat.error;phot.magfloatW2magWISE W2-band (4.6um) magnitudemagphot.mag;em.IR.4-8umfloate_W2magrms uncertainty on W2-band magnitudemagstat.error;phot.magfloatW3magWISE W3-band (12um) magnitudemagphot.flux.density;em.IR.8-15umfloate_W3magrms uncertainty on W3-band magnitudemagstat.error;phot.magdoubleW4magWISE W4-band (22um) magnitudemagphot.flux.density;em.IR.15-30umfloate_W4magrms uncertainty on W4-band magnitudemagstat.error;phot.magdoubleS250? Herschel/SPIRE 250um-band magnitudemagphot.flux.density;em.mm.750-1500GHzfloatnullablee_S250? rms uncertainty on 250um-band magnitudemagstat.errorfloatnullableS350? Herschel/SPIRE 350um-band magnitudemagphot.flux.density;em.mm.750-1500GHzfloatnullablee_S350? rms uncertainty on 350um-band magnitudemagstat.errorfloatnullableS500? Herschel/SPIRE 500um-band magnitudemagphot.flux.density;em.mm.400-750GHzfloatnullablee_S500? rms uncertainty on 500um-band magnitudemagstat.errorfloatnullableBandJVLA? JVLA observed continuum frequencyGHzem.freq;spect.continuumfloatnullableFJVLA? JVLA continuum fluxmJyphot.flux.density;em.radiofloatnullablee_FJVLA? rms uncertainty on JVLA measured fluxmJystat.errorfloatnullablelogL(2-10)? Chandra/XMM integrated 2-10Kev luminositylog(mW.m**-2)phys.luminosity;em.X-rayfloatnullableGamma? X-ray photon indexmeta.code;spect.indexfloatnullableIDID of each targetmeta.id;meta.maincharBand? ALMA/NOEMA observed continuum frequencyGHzem.freq;spect.continuumfloatnullableFlux? ALMA/NOEMA continuum fluxmJyphot.flux.density;em.radiofloatnullablee_Flux? rms uncertainty on ALMA/NOEMA measured fluxmJystat.error;phot.fluxfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintumagSDSS u-band magnitudemagphot.mag;em.opt.Ufloate_umagrms uncertainty on u-band magnitudemagstat.error;phot.magfloatgmagSDSS g-band magnitudemagphot.mag;em.opt.Bfloate_gmagrms uncertainty on g-band magnitudemagstat.error;phot.magfloatrmagSDSS r-band magnitudemagphot.mag;em.opt.Rfloate_rmagrms uncertainty on r-band magnitudemagstat.error;phot.magfloatimagSDSS i-band magnitudemagphot.mag;em.opt.Ifloate_imagrms uncertainty on i-band magnitudemagstat.error;phot.magfloatzmagSDSS z-band magnitudemagphot.mag;em.opt.Ifloate_zmagrms uncertainty on z-band magnitudemagstat.error;phot.magfloatJmag2MASS/TNG J-band magnitudemagphot.mag;em.IR.Kfloate_Jmagrms uncertainty on J-band magnitudemagstat.error;phot.magfloatHmag2MASS/TNG H-band magnitudemagphot.mag;em.IR.Hfloate_Hmagrms uncertainty on H-band magnitudemagstat.error;phot.magfloatKmag2MASS/TNG K-band magnitudemagphot.mag;em.IR.Kfloate_Kmagrms uncertainty on K-band magnitudemagstat.error;phot.magfloatJ/A+A/671/A34/table3Bolometric and monochromatic luminosities for WISSH QSOsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDID of each targetmeta.id;meta.maincharLbolBolometric luminosity1e-07Wphys.luminosityfloate_LbolLower uncertainty on Lbol1e-07Wstat.errorfloatE_LbolUpper uncertainty on Lbol1e-07Wstat.error;stat.maxfloatL25002500{AA} monochromatic luminosity1e-07Wphys.luminosityfloate_L2500rms uncertainty on 2500{AA} luminosity1e-07Wstat.errorfloatL51005100{AA} monochromatic luminosity1e-07Wphys.luminosityfloate_L5100rms uncertainty on 5100{AA} luminosity1e-07Wstat.errorfloatL300003um monochromatic luminosity1e-07Wphys.luminosityfloate_L30000rms uncertainty on 3um luminosity1e-07Wstat.errorfloatE(B-V)E(B-V) colour excessmagphot.color.excessfloatJ/A+A/671/A34/table4Derived mean SEDs of WISSH QSOsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintloglambdaWavelength0.1nmem.wlfloatlogmeanMean SED (lambdaL_lambda_) of the full WISSH sample (in erg/s)log(1e-07W)phot.fluxfloats_logmeanrms uncertainty on the mean SED (lambdaL_lambda_) of the full samplelog(1e-07W)stat.errorfloatlogBAL? Mean SED (lambdaL_lambda_) of the BAL subsample (in erg/s)log(1e-07W)phot.fluxfloatnullables_logBAL? rms uncertainty on the mean SED (lambdaL_lambda_) of the BAL subsamplelog(1e-07W)stat.error;instr.det.noise;stat.meanfloatnullablelogNonBAL? Mean SED (lambdaL_lambda_) of the non-BAL subsample (in erg/s)log(1e-07W)phot.fluxfloatnullables_logNonBAL? rms uncertainty on the mean SED (lambdaL_lambda_) of the non-BAL subsamplelog(1e-07W)stat.error;instr.det.noise;stat.meanfloatnullablelogWeak? Mean SED (lambdaL_lambda_) of the CIV weak subsample (in erg/s)log(1e-07W)phot.fluxfloatnullables_logWeak? rms uncertainty on the mean SED (lambdaL_lambda_) of the CIV weak subsamplelog(1e-07W)stat.error;instr.det.noise;stat.meanfloatnullablelogNonWeak? Mean SED (lambdaL_lambda_) of the non-CIV weak subsample (in erg/s)log(1e-07W)phot.fluxfloatnullables_logNonWeak? rms uncertainty on the mean SED (lambdaL_lambda_) of the non-CIV weak subsamplelog(1e-07W)stat.error;instr.det.noise;stat.meanfloatnullable