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<ri:Resource created="2022-04-05T10:41:46Z" status="active" updated="2025-06-13T15:25:00Z" 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 data for blazars 3C 279 &amp; 3C 454.3</title><shortName>J/ApJS/257/37</shortName><identifier>ivo://CDS.VizieR/J/ApJS/257/37</identifier><altIdentifier>doi:10.26093/cds/vizier.22570037</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Paliya V.S.</name></creator><creator><name>Bottcher M.</name></creator><creator><name>Gurwell M.</name></creator><creator><name>Stalin C.S.</name></creator><date role="Updated">2022-06-13T13:33:07Z</date><date role="Created">2022-04-05T10:41:46Z</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>active-galactic-nuclei</subject><subject>gamma-ray-astronomy</subject><subject>x-ray-sources</subject><subject>ultraviolet-astronomy</subject><subject>visible-astronomy</subject><subject>infrared-astronomy</subject><subject>radio-sources</subject><description>The origin of {gamma}-ray flares observed from blazars is one of the major mysteries in jet physics. We have attempted to address this problem following a novel spectral energy distribution (SED) fitting technique that explored the flaring patterns identified in the broadband SEDs of two {gamma}-ray bright blazars, 3C 279 (z=0.54) and 3C 454.3 (z=0.86), using near-simultaneous radio-to-{gamma}-ray observations. For both sources, the {gamma}-ray flux strongly correlates with the separation of the SED peaks and the Compton dominance. We propose that spectral hardening of the radiating electron population and/or enhancement of the Doppler factor can naturally explain these observations. 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