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<ri:Resource created="2014-11-05T12:41:54Z" 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>MgII and FeII flux of the blazar 3C 454.3</title><shortName>J/ApJ/763/L36</shortName><identifier>ivo://CDS.VizieR/J/ApJ/763/L36</identifier><altIdentifier>doi:10.26093/cds/vizier.17639036</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Leon-Tavares J.</name></creator><creator><name>Chavushyan V.</name></creator><creator><name>Patino-Alvarez V.</name></creator><creator><name>Valtaoja E.,Arshakian T.G.</name></creator><creator><name>Popovic L.C.</name></creator><creator><name>Tornikoski M.</name></creator><creator><name>Lobanov A.</name></creator><creator><name>Carraminana A.,Carrasco L.</name></creator><creator><name>Lahteenmaki A.</name></creator><date role="Updated">2017-06-20T13:17:17Z</date><date role="Created">2014-11-05T12:41:54Z</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>spectroscopy</subject><subject>ultraviolet-astronomy</subject><subject>quasars</subject><description>We report the detection of a statistically significant flare-like event in the MgII {lambda}2800 emission line of 3C 454.3 during the outburst of autumn 2010. The highest levels of emission line flux recorded over the monitoring period (2008-2011) coincide with a superluminal jet component traversing through the radio core. This finding crucially links the broad emission line fluctuations to the non-thermal continuum emission produced by relativistically moving material in the jet and hence to the presence of broad-line region clouds surrounding the radio core. If the radio core were located at several parsecs from the central black hole, then our results would suggest the presence of broad-line region material outside the inner parsec where the canonical broad-line region is envisaged to be located. We briefly discuss the implications of broad emission line material ionized by non-thermal continuum in the context of virial black hole mass estimates and gamma-ray production mechanisms.</description><source format="bibcode">2013ApJ...763L..36L</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/763/L36</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/J/other/RMxAA/48.9">J/other/RMxAA/48.9 : MOJAVE/2cm AGN sample spectros. atlas (Torrealba+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/545/A113">J/A+A/545/A113 : MOJAVE IX. Core shift effects (Pushkarev+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/754/23">J/ApJ/754/23 : Blazar mm + {gamma}-ray luminosities (Leon-Tavares+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/712/405">J/ApJ/712/405 : Multiwavelength obs. of 3C 454.3 III. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>JD</name><description>Julian Date of observation; JD-2450000</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>MgII</name><description>[1.05/1.82] Flux of MgII 280nm line (1)</description><unit>1e-16W.m**-2</unit><ucd>phot.flux;em.UV.200-300nm;spect.line</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_MgII</name><description>[0.01/0.2] Error in MgII (1)</description><unit>1e-16W.m**-2</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>FeII</name><description>[1.3/8] Flux of FeII (1)</description><unit>1e-16W.m**-2</unit><ucd>phot.flux</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_FeII</name><description>Error in FeII (1)</description><unit>1e-16W.m**-2</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>UVcont</name><description>[0.5/8] Flux of UV continuum at 300nm (2)</description><unit>1e-16W.m**-2.nm**-1</unit><ucd>phot.flux</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_UVcont</name><description>Error in UV3000 (2)</description><unit>1e-16W.m**-2.nm**-1</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column></table></schema></tableset></ri:Resource>