J/A+A/639/A51ivo://CDS.VizieR/J/A+A/639/A51doi:10.26093/cds/vizier.36390051CDSIwasawa K.Comastri A.Vignali C.Gilli R.Lanzuisi G.Brandt W .N.,Tozzi P.Brusa M.Carrera F.J.Ranalli P.Mainieri V.,Georgantopoulos I.Puccetti S.Paolillo M.2020-09-01T10:23:35Z2020-07-06T06:51:31ZCDS support team

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

cds-question@unistra.frx-ray-sourcesredshiftedline-intensitiesspectroscopyWe present X-ray spectra of 185 bright sources detected in the XMM-Newton deep survey of the Chandra Deep Field South, combining the three EPIC cameras. The 2-10keV flux limit of the sample is 2x10^-15^erg/s/cm^2^. The sources are distributed over a redshift range of z=0.1-3.8. Eleven new X-ray redshift measurements are included. A spectral analysis was performed using a simple model to obtain absorbing column densities, rest-frame 2-10keV luminosities and Fe K line properties of 180 sources at z>0.4. Obscured AGN are found to be more abundant toward higher redshifts. Using the XMM-Newton data alone, seven Compton-thick AGN candidates are identified, which makes the Compton-thick AGN fraction to be ~=4%. An exploratory spectral inspection method with two rest-frame X-ray colours and an Fe line strength indicator is introduced and tested against the results from spectral fitting. This method works reasonably well to characterise a spectral shape and can be useful for a pre-selection of Compton-thick AGN candidates.We found six objects exhibiting broad Fe K lines out of 21 unobscured AGN of best data quality, implying a detection rate of 30%. Five redshift spikes, each of which has more than six sources, are identified in the redshift distribution of the X-ray sources. Contrary to the overall trend, the sources at the two higher-redshift spikes at z=1.61 and z=2.57 have puzzlingly low obscuration.2020A&A...639A..51Ihttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/639/A51CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/MNRAS/436/3759 : ECDFS sources optical/IR counterparts (Bonzini+, 2013)J/ApJS/224/15 : Improved 2Ms and 250ks Chandra catalogs (Xue+, 2016)J/ApJS/228/2 : Chandra Deep Field-South survey: 7Ms sources (Luo+, 2017)J/A+A/555/A42 : The XMM-CDFS catalogues (Ranalli+, 2013)J/A+A/556/A114 : Obscured AGNs in XMM deep survey in CDF-SJ/A+A/574/A49 : XMMOMCDFS catalogue (Antonucci+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/639/A51https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/639/A51http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/639/A51https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/639/A51https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/639/A51http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/639/A51GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapX-raydefaultJ/A+A/639/A51/table1Properties of 185 XMM-CDFS sourcese_S/M? Uncertainty of S/Mstat.errorfloatnullablee_H/M? Uncertainty of H/Mstat.errorfloatnullableRfe? Fe K line strength indicatorspect.line.intensityfloatnullablee_Rfe? Uncertainty of Rfestat.errorfloatnullableSNe310? Signal-to-noise indicator of spectral data in the rest-frame 3-10keV bandstat.snrfloatnullableb_EW? The 68% lower bound of EWkeVspect.line.eqWidth;stat.minfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintspShow the 0.5-7keV spectrummeta.ref.urlcharPIDXMM-CDFS source identification numbermeta.id;phys.atmol.numberintzRedshiftsrc.redshiftfloatztypeRedshift type (1)meta.codecharr_zReference for the adopted redshift (2)meta.ref;pos.frameintlogNHLogarithmic of absorbing column densitylog(cm**-2)phys.columnDensityfloatb_logNHThe 68% lower bound of NHlog(cm**-2)phys.columnDensity;stat.minfloatB_logNHThe 68% upper bound of NHlog(cm**-2)phys.columnDensity;stat.maxfloatlogLXobsLogarithmic of rest-frame 2-10keV luminosity as observedlog(1e-07W)phys.luminosity;em.X-ray.mediumfloatlogLXcorLogarithmic of rest-frame 2-10keV luminosity corrected for absorptionlog(1e-07W)phys.luminosity;em.X-ray.mediumfloatD90[0/1]? Fe K line detection flag with threshold of the 90% significance (0: no detection/1 detection)meta.codeintnullableD68[0/1]? Fe K line detection flag with threshold of the 68% significance (0: nodetection/1: detection)meta.codeintnullableEline? Adopted Fe K line energykeVphys.energyfloatnullableEW? Equivalent width of Fe K linekeVspect.line.eqWidthfloatnullableB_EW? The 68% upper bound of EWkeVspect.line.eqWidth;stat.maxfloatnullableS/M? Rest-frame X-ray colour S/M=(2-5keV)/(5-9keV)phot.color;em.X-rayfloatnullableH/M? Rest-frame X-ray colour H/M=(9-14keV)/(5-9keV)phot.color;em.X-rayfloatnullableL17? Chandra source identification number in Luo et al., 2017, Cat. J/ApJS/228/2, [LBX2017] NNNN in Simbadmeta.idintnullableX16? Chandra source identification number in Xue et al., 2016, Cat. J/ApJS/224/15 (3)meta.idcharRID? Radio source identification number in Bonzini et al., 2013, Cat. J/MNRAS/436/3759, [MBF2013] in Simbad (4)meta.idintnullable