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<ri:Resource created="2023-05-03T09:05:59Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" 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/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>Multiwavelength light curves of PG 1553+113</title><shortName>J/ApJ/922/222</shortName><identifier>ivo://CDS.VizieR/J/ApJ/922/222</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Huang S.</name></creator><creator><name>Yin H.</name></creator><creator><name>Hu S.</name></creator><creator><name>Chen Xu</name></creator><creator><name>Jiang Y.</name></creator><creator><name>Alexeeva S.</name></creator><creator><name>Wang Y.</name></creator><date role="Updated">2024-05-14T08:41:28Z</date><date role="Created">2023-05-03T09:05:59Z</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>bl-lacertae-objects</subject><subject>gamma-ray-astronomy</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><subject>ultraviolet-astronomy</subject><subject>x-ray-sources</subject><subject>radio-sources</subject><subject>black-holes</subject><description>Blazar PG 1553+113 is thought to be a host of supermassive black hole binary system. A 2.2yr quasi-periodicity in the {gamma}-ray light curve was detected, possibly a result of jet precession. Motivated by the previous studies based on the {gamma}-ray data, we analyzed the X-ray light curve and spectra observed during 2012-2020. The 2.2yr quasi-periodicity might be consistent with the main-flare recurrence in the X-ray light curve. When a weak rebrightening in the {gamma}-ray was observed, a corresponding relatively strong brightening in the X-ray light curve can be identified. The harder- when-brighter tendency in both X-ray main and weak flares was shown, as well as a weak softer-when-brighter behavior for the quiescent state. We explore the possibility that the variability in the X-ray band can be interpreted with two-jet precession scenario. Using the relation between jets and accretion disks, we derive the primary black hole mass ~3.47x10^8^M_{sun}_ and mass of the secondary one ~1.40x10^8^M_{sun}_, and their mass ratio ~0.41.</description><source format="bibcode">2021ApJ...922..222H</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/922/222</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>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/B/swift">B/swift : Swift Master Catalog (HEASARC, 2004-)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/B/xmm">B/xmm : XMM-Newton Obs. 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