J/A+A/473/105ivo://CDS.VizieR/J/A+A/473/105doi:10.26093/cds/vizier.34730105CDSMateos S.Barcons X.Carrera F.J.Page M.J.Ceballos M.T.Hasinger G.,Fabian A.C.2017-11-28T13:21:10Z2008-07-21T13:55:06ZCDS support team

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

cds-question@unistra.frx-ray-sourcesactive-galactic-nucleiThis paper presents the results of a study of X-ray spectral and flux variability on time scales from months to years, of the 123 brightest objects (including 46 type-1 AGN and 28 type-2 AGN) detected with XMM-Newton in the Lockman Hole field. We detected flux variability with a significance >=3{sigma} in ~50% of the objects, including 68+/-11% and 48+/-15% among our samples of type-1 and type-2 AGN. However we found that the fraction of sources with best quality light curves that exhibit flux variability on the time scales sampled by our data is >=80%, i.e the great majority of the AGN population may actually vary in flux on long time scales. The mean relative intrinsic amplitude of flux variability was found to be ~0.15 although with a large dispersion in measured values, from ~0.1 to ~0.65. The flux variability properties of our samples of AGN (fraction of variable objects and amplitude of variability) do not significantly depend on the redshift or X-ray luminosity of the objects and seem to be similar for the two AGN types. Using a broad band X-ray colour we found that the fraction of sources showing spectral variability with a significance >=3{sigma} is ~40% i.e. less common than flux variability. Spectral variability was found to be more common in type-2 AGN than in type-1 AGN with a significance of more than 99%. This result is consistent with the fact that part of the soft emission in type-2 AGN comes from scattered radiation, and this component is expected to be much less variable than the hard component. The observed flux and spectral variability properties of our objects and especially the lack of correlation between flux and spectral variability in most of them cannot be explained as being produced by variability of one spectral component alone, for example changes in Gamma associated with changes in the mass accretion rate, or variability in the amount of X-ray absorption. At least two spectral components must vary in order to explain the X-ray variability of our objects.2007A&A...473..105Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/473/105CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/393/425 : Spectral analysis of Lockman Hole (Mainieri+, 2002)J/A+A/444/79 : XMM observations of Lockman Hole brightest AGNs (Mateos+, 2005)J/A+A/479/283 : XMM observations of the Lockman Hole (Brunner+, 2008)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/473/105https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/473/105http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/473/105https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/473/105https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/473/105http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/473/105GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/473/105/table4 (Summary of detection of X-ray variability in Lockman Hole sources)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/473/105/table4?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/473/105/table4?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/473/105/table4?GETtext/xml+votable180.050000true163.2577557.25019170.0055555555555555566/6069 6090 6112https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/473/105?format=asciiX-raydefaultJ/A+A/473/105/table4Summary of detection of X-ray variability in Lockman Hole sourcesz? Redshiftsrc.redshiftfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint[MBC2005]Source sequential numbermeta.recordintRDS? X-ray source ROSAT number (RDS NNN)meta.id.crossintnullableRDSOOptical source ROSAT number (RDS NNNA)meta.id.crosscharRAJ2000Right ascension (J2000.0) (1)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0) (1)pos.eq.dec;meta.mainAGN[1,2]? AGN class from optical spectroscopymeta.code.classintnullableModelBest fit spectral model (2)stat.param;meta.modelledcharl_SFluxLimit on SFluxmeta.code.errorcharSFlux? Significance of detection of flux variability%stat.fit.goodnessfloatnullablel_SSpecLimit on SSpecmeta.code.errorcharSSpec? Significance of detection of spectral variability%stat.fit.goodnessfloatnullablel_sigmaLimit on sigmameta.code.errorcharsigma? Intrinsic amplitude of flux variabilitysrc.var.amplitudefloatnullablee_sigma? Low error bar of sigmastat.errorfloatnullableE_sigma? High error bar of sigmastat.error;stat.maxfloatnullableSimbadSimbad column added by the CDSchar