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<ri:Resource created="2012-03-27T15:51:13Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>X-ray variability of AGN</title><shortName>J/A+A/536/A84</shortName><identifier>ivo://CDS.VizieR/J/A+A/536/A84</identifier><altIdentifier>doi:10.26093/cds/vizier.35360084</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Vagnetti F.</name></creator><creator><name>Turriziani S.</name></creator><creator><name>Trevese D.</name></creator><date role="Updated">2012-04-13T17:41:38Z</date><date role="Created">2012-03-27T15:51:13Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>surveys</subject><subject>active-galactic-nuclei</subject><subject>x-ray-sources</subject><description>The X-ray variability of the active galactic nuclei (AGN) has been most often investigated with studies of individual, nearby sources, and only a few ensemble analyses have been applied to large samples in wide ranges of luminosity and redshift. We aim to determine the ensemble variability properties of two serendipitously selected AGN samples extracted from the catalogues of XMM-Newton and Swift, with redshift between ~0.2 and ~4.5, and X-ray luminosities, in the 0.5-4.5keV band, between ~10^43^erg/s and ~10^46^erg/s. We used the structure function (SF), which operates in the time domain, and allows for an ensemble analysis even when only a few observations are available for individual sources and the power spectral density (PSD) cannot be derived. The SF is also more appropriate than fractional variability and excess variance, because these parameters are biased by the duration of the monitoring time interval in the rest-frame, and therefore by cosmological time dilation.</description><source format="bibcode">2011A&amp;A...536A..84V</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/536/A84</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/IX/41">IX/41 : XMM-Newton Serendipitous Source Cat. 2XMMi-DR3 (XMM-SSC, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/260">VII/260 : The 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