AustralieFrV1, Istex, Corpus, bibRecord, 001A26

X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213

Identifieur interne : 001A26 ( Istex/Corpus ); précédent : 001A25; suivant : 001A27

X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213

Auteurs : M. E. Bell ; T. Tzioumis ; P. Uttley ; R. P. Fender ; P. Arévalo ; E. Breedt ; I. Mchardy ; D. E. Calvelo ; O. Jamil ; E. Körding

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-02-11.

RBID : ISTEX:8B40C620A40D05F69CB1F0C860A7194D684BA528

English descriptors

Abstract

We present the results of a ∼3 yr campaign to monitor the low‐luminosity active galactic nucleus (LLAGN) NGC 7213 in the radio (4.8 and 8.4 GHz) and X‐ray bands (2–10 keV). With a reported X‐ray Eddington ratio of 7 × 10−4LEdd, NGC 7213 can be considered to be comparable to a hard‐state black hole X‐ray binary. We show that a weak correlation exists between the X‐ray and radio light curves. We use the cross‐correlation function to calculate a global time‐lag between events in the X‐ray and radio bands to be 24 ± 12 d lag (8.4 GHz radio lagging X‐ray) and 40 ± 13 d lag (4.8 GHz radio lagging X‐ray), respectively. The radio–radio light curves are extremely well correlated with a lag of 20.5 ± 12.9 d (4.8 GHz lagging 8.4 GHz). We explore the previously established scaling relationship between core radio and X‐ray luminosities and black hole mass LR∝M0.6‐0.8L0.6X, known as the ‘Fundamental Plane of black hole activity’, and show that NGC 7213 lies very close to the best‐fitting ‘global’ correlation for the plane as one of the most‐luminous LLAGNs. With a large number of quasi‐simultaneous radio and X‐ray observations, we explore for the first time the variations of a single AGN with respect to the Fundamental Plane. Although the average radio and X‐ray luminosities for NGC 7213 are in good agreement with the Plane, we show that there is intrinsic scatter with respect to the Plane for the individual data points.

Url:

https://api.istex.fr/document/8B40C620A40D05F69CB1F0C860A7194D684BA528/fulltext/pdf

DOI: 10.1111/j.1365-2966.2010.17692.x

Links to Exploration step

ISTEX:8B40C620A40D05F69CB1F0C860A7194D684BA528

Le document en format XML

<record><TEI wicri:istexFullTextTei="biblStruct"><teiHeader><fileDesc><titleStmt><title xml:lang="en">X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213</title>
<author><name sortKey="Bell, M E" sort="Bell, M E" uniqKey="Bell M" first="M. E." last="Bell">M. E. Bell</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
<affiliation><mods:affiliation>E-mail: meb1w07@soton.ac.uk</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Tzioumis, T" sort="Tzioumis, T" uniqKey="Tzioumis T" first="T." last="Tzioumis">T. Tzioumis</name>
<affiliation><mods:affiliation>Australia Telescope National Facility, CSIRO, Marsfield, NSW 2122, Australia</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Uttley, P" sort="Uttley, P" uniqKey="Uttley P" first="P." last="Uttley">P. Uttley</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Fender, R P" sort="Fender, R P" uniqKey="Fender R" first="R. P." last="Fender">R. P. Fender</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Arevalo, P" sort="Arevalo, P" uniqKey="Arevalo P" first="P." last="Arévalo">P. Arévalo</name>
<affiliation><mods:affiliation>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Strasse 1, 85741 Garching, Germany</mods:affiliation>
</affiliation>
<affiliation><mods:affiliation>Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Breedt, E" sort="Breedt, E" uniqKey="Breedt E" first="E." last="Breedt">E. Breedt</name>
<affiliation><mods:affiliation>Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Mchardy, I" sort="Mchardy, I" uniqKey="Mchardy I" first="I." last="Mchardy">I. Mchardy</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Calvelo, D E" sort="Calvelo, D E" uniqKey="Calvelo D" first="D. E." last="Calvelo">D. E. Calvelo</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Jamil, O" sort="Jamil, O" uniqKey="Jamil O" first="O." last="Jamil">O. Jamil</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Kording, E" sort="Kording, E" uniqKey="Kording E" first="E." last="Körding">E. Körding</name>
<affiliation><mods:affiliation>AIM/CEA Saclay and University Paris Diderot, l'Orme des Merisers, F‐91219 Gif‐sur‐Yvette CEDEX, France</mods:affiliation>
</affiliation>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">ISTEX</idno>
<idno type="RBID">ISTEX:8B40C620A40D05F69CB1F0C860A7194D684BA528</idno>
<date when="2011" year="2011">2011</date>
<idno type="doi">10.1111/j.1365-2966.2010.17692.x</idno>
<idno type="url">https://api.istex.fr/document/8B40C620A40D05F69CB1F0C860A7194D684BA528/fulltext/pdf</idno>
<idno type="wicri:Area/Istex/Corpus">001A26</idno>
<idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001A26</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title level="a" type="main">X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213</title>
<author><name sortKey="Bell, M E" sort="Bell, M E" uniqKey="Bell M" first="M. E." last="Bell">M. E. Bell</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
<affiliation><mods:affiliation>E-mail: meb1w07@soton.ac.uk</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Tzioumis, T" sort="Tzioumis, T" uniqKey="Tzioumis T" first="T." last="Tzioumis">T. Tzioumis</name>
<affiliation><mods:affiliation>Australia Telescope National Facility, CSIRO, Marsfield, NSW 2122, Australia</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Uttley, P" sort="Uttley, P" uniqKey="Uttley P" first="P." last="Uttley">P. Uttley</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Fender, R P" sort="Fender, R P" uniqKey="Fender R" first="R. P." last="Fender">R. P. Fender</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Arevalo, P" sort="Arevalo, P" uniqKey="Arevalo P" first="P." last="Arévalo">P. Arévalo</name>
<affiliation><mods:affiliation>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Strasse 1, 85741 Garching, Germany</mods:affiliation>
</affiliation>
<affiliation><mods:affiliation>Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Breedt, E" sort="Breedt, E" uniqKey="Breedt E" first="E." last="Breedt">E. Breedt</name>
<affiliation><mods:affiliation>Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Mchardy, I" sort="Mchardy, I" uniqKey="Mchardy I" first="I." last="Mchardy">I. Mchardy</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Calvelo, D E" sort="Calvelo, D E" uniqKey="Calvelo D" first="D. E." last="Calvelo">D. E. Calvelo</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Jamil, O" sort="Jamil, O" uniqKey="Jamil O" first="O." last="Jamil">O. Jamil</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Kording, E" sort="Kording, E" uniqKey="Kording E" first="E." last="Körding">E. Körding</name>
<affiliation><mods:affiliation>AIM/CEA Saclay and University Paris Diderot, l'Orme des Merisers, F‐91219 Gif‐sur‐Yvette CEDEX, France</mods:affiliation>
</affiliation>
</author>
</analytic>
<monogr></monogr>
<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title>
<idno type="ISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<imprint><biblScope unit="vol">411</biblScope>
<biblScope unit="issue">1</biblScope>
<biblScope unit="page" from="402">402</biblScope>
<biblScope unit="page" to="410">410</biblScope>
<biblScope unit="page-count">9</biblScope>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<date type="published" when="2011-02-11">2011-02-11</date>
</imprint>
<idno type="ISSN">0035-8711</idno>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><idno type="ISSN">0035-8711</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accretion</term>
<term>Accretion rate</term>
<term>Accurate measurement</term>
<term>Agns</term>
<term>Archival</term>
<term>Archival data points</term>
<term>Archival observations</term>
<term>Archival points</term>
<term>Atca</term>
<term>Atca monitoring</term>
<term>Australia telescope</term>
<term>Average location</term>
<term>Baseline</term>
<term>Bhxrb</term>
<term>Bhxrb sample</term>
<term>Bhxrbs</term>
<term>Black hole</term>
<term>Black hole activity</term>
<term>Black hole mass</term>
<term>Blandford konigl</term>
<term>Bottom panel</term>
<term>Cent threshold</term>
<term>Centroid</term>
<term>Confidence centroid</term>
<term>Correlation ceofficient</term>
<term>Data point</term>
<term>Data points</term>
<term>Dcfmax</term>
<term>Discrete function</term>
<term>Edelson krolik</term>
<term>Ejection events</term>
<term>Energy range</term>
<term>Erg</term>
<term>Falcke</term>
<term>Fender</term>
<term>Flux values</term>
<term>Fundamental plane</term>
<term>Gallo</term>
<term>Halpern filippenko</term>
<term>Internal shock model</term>
<term>Light curve</term>
<term>Light curves</term>
<term>Llagn</term>
<term>Llagn sample</term>
<term>Local level</term>
<term>Localized shocks</term>
<term>Luminosity</term>
<term>Many orders</term>
<term>Middle panel</term>
<term>Mnras</term>
<term>Monthly notices</term>
<term>Nandra pounds</term>
<term>Other forms</term>
<term>Plasmon model</term>
<term>Pooley</term>
<term>Pooley fender</term>
<term>Power spectrum</term>
<term>Radio bands</term>
<term>Radio data</term>
<term>Radio data points</term>
<term>Radio flux</term>
<term>Radio light curves</term>
<term>Radio loudness</term>
<term>Radio loudness parameter</term>
<term>Radio luminosities</term>
<term>Radio points</term>
<term>Radio variability</term>
<term>Random light curves</term>
<term>Rding</term>
<term>Same source</term>
<term>Scatter</term>
<term>Seyfert galaxies</term>
<term>Show evidence</term>
<term>Softer state</term>
<term>Solid line</term>
<term>Spectral index</term>
<term>Spectral indices</term>
<term>Tting</term>
<term>Tting parameters</term>
<term>Turner pounds</term>
<term>Variability</term>
<term>Weak correlation</term>
</keywords>
<keywords scheme="Teeft" xml:lang="en"><term>Accretion</term>
<term>Accretion rate</term>
<term>Accurate measurement</term>
<term>Agns</term>
<term>Archival</term>
<term>Archival data points</term>
<term>Archival observations</term>
<term>Archival points</term>
<term>Atca</term>
<term>Atca monitoring</term>
<term>Australia telescope</term>
<term>Average location</term>
<term>Baseline</term>
<term>Bhxrb</term>
<term>Bhxrb sample</term>
<term>Bhxrbs</term>
<term>Black hole</term>
<term>Black hole activity</term>
<term>Black hole mass</term>
<term>Blandford konigl</term>
<term>Bottom panel</term>
<term>Cent threshold</term>
<term>Centroid</term>
<term>Confidence centroid</term>
<term>Correlation ceofficient</term>
<term>Data point</term>
<term>Data points</term>
<term>Dcfmax</term>
<term>Discrete function</term>
<term>Edelson krolik</term>
<term>Ejection events</term>
<term>Energy range</term>
<term>Erg</term>
<term>Falcke</term>
<term>Fender</term>
<term>Flux values</term>
<term>Fundamental plane</term>
<term>Gallo</term>
<term>Halpern filippenko</term>
<term>Internal shock model</term>
<term>Light curve</term>
<term>Light curves</term>
<term>Llagn</term>
<term>Llagn sample</term>
<term>Local level</term>
<term>Localized shocks</term>
<term>Luminosity</term>
<term>Many orders</term>
<term>Middle panel</term>
<term>Mnras</term>
<term>Monthly notices</term>
<term>Nandra pounds</term>
<term>Other forms</term>
<term>Plasmon model</term>
<term>Pooley</term>
<term>Pooley fender</term>
<term>Power spectrum</term>
<term>Radio bands</term>
<term>Radio data</term>
<term>Radio data points</term>
<term>Radio flux</term>
<term>Radio light curves</term>
<term>Radio loudness</term>
<term>Radio loudness parameter</term>
<term>Radio luminosities</term>
<term>Radio points</term>
<term>Radio variability</term>
<term>Random light curves</term>
<term>Rding</term>
<term>Same source</term>
<term>Scatter</term>
<term>Seyfert galaxies</term>
<term>Show evidence</term>
<term>Softer state</term>
<term>Solid line</term>
<term>Spectral index</term>
<term>Spectral indices</term>
<term>Tting</term>
<term>Tting parameters</term>
<term>Turner pounds</term>
<term>Variability</term>
<term>Weak correlation</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We present the results of a ∼3 yr campaign to monitor the low‐luminosity active galactic nucleus (LLAGN) NGC 7213 in the radio (4.8 and 8.4 GHz) and X‐ray bands (2–10 keV). With a reported X‐ray Eddington ratio of 7 × 10−4LEdd, NGC 7213 can be considered to be comparable to a hard‐state black hole X‐ray binary. We show that a weak correlation exists between the X‐ray and radio light curves. We use the cross‐correlation function to calculate a global time‐lag between events in the X‐ray and radio bands to be 24 ± 12 d lag (8.4 GHz radio lagging X‐ray) and 40 ± 13 d lag (4.8 GHz radio lagging X‐ray), respectively. The radio–radio light curves are extremely well correlated with a lag of 20.5 ± 12.9 d (4.8 GHz lagging 8.4 GHz). We explore the previously established scaling relationship between core radio and X‐ray luminosities and black hole mass LR∝M0.6‐0.8L0.6X, known as the ‘Fundamental Plane of black hole activity’, and show that NGC 7213 lies very close to the best‐fitting ‘global’ correlation for the plane as one of the most‐luminous LLAGNs. With a large number of quasi‐simultaneous radio and X‐ray observations, we explore for the first time the variations of a single AGN with respect to the Fundamental Plane. Although the average radio and X‐ray luminosities for NGC 7213 are in good agreement with the Plane, we show that there is intrinsic scatter with respect to the Plane for the individual data points.</div>
</front>
</TEI>
<istex><corpusName>wiley</corpusName>
<keywords><teeft><json:string>mnras</json:string>
<json:string>fundamental plane</json:string>
<json:string>bhxrbs</json:string>
<json:string>data points</json:string>
<json:string>agns</json:string>
<json:string>archival</json:string>
<json:string>atca</json:string>
<json:string>falcke</json:string>
<json:string>bhxrb</json:string>
<json:string>gallo</json:string>
<json:string>centroid</json:string>
<json:string>dcfmax</json:string>
<json:string>monthly notices</json:string>
<json:string>llagn</json:string>
<json:string>erg</json:string>
<json:string>tting</json:string>
<json:string>pooley</json:string>
<json:string>black hole mass</json:string>
<json:string>bhxrb sample</json:string>
<json:string>rding</json:string>
<json:string>radio bands</json:string>
<json:string>luminosity</json:string>
<json:string>radio data points</json:string>
<json:string>radio light curves</json:string>
<json:string>radio variability</json:string>
<json:string>light curve</json:string>
<json:string>bottom panel</json:string>
<json:string>black hole activity</json:string>
<json:string>baseline</json:string>
<json:string>light curves</json:string>
<json:string>archival points</json:string>
<json:string>fender</json:string>
<json:string>halpern filippenko</json:string>
<json:string>australia telescope</json:string>
<json:string>random light curves</json:string>
<json:string>middle panel</json:string>
<json:string>pooley fender</json:string>
<json:string>cent threshold</json:string>
<json:string>archival data points</json:string>
<json:string>atca monitoring</json:string>
<json:string>data point</json:string>
<json:string>black hole</json:string>
<json:string>radio data</json:string>
<json:string>solid line</json:string>
<json:string>llagn sample</json:string>
<json:string>accretion</json:string>
<json:string>weak correlation</json:string>
<json:string>softer state</json:string>
<json:string>ejection events</json:string>
<json:string>power spectrum</json:string>
<json:string>correlation ceofficient</json:string>
<json:string>confidence centroid</json:string>
<json:string>show evidence</json:string>
<json:string>local level</json:string>
<json:string>many orders</json:string>
<json:string>accurate measurement</json:string>
<json:string>seyfert galaxies</json:string>
<json:string>tting parameters</json:string>
<json:string>turner pounds</json:string>
<json:string>nandra pounds</json:string>
<json:string>radio flux</json:string>
<json:string>flux values</json:string>
<json:string>same source</json:string>
<json:string>spectral index</json:string>
<json:string>internal shock model</json:string>
<json:string>blandford konigl</json:string>
<json:string>plasmon model</json:string>
<json:string>localized shocks</json:string>
<json:string>accretion rate</json:string>
<json:string>energy range</json:string>
<json:string>radio luminosities</json:string>
<json:string>spectral indices</json:string>
<json:string>average location</json:string>
<json:string>radio loudness</json:string>
<json:string>radio points</json:string>
<json:string>discrete function</json:string>
<json:string>archival observations</json:string>
<json:string>edelson krolik</json:string>
<json:string>other forms</json:string>
<json:string>radio loudness parameter</json:string>
<json:string>scatter</json:string>
<json:string>variability</json:string>
</teeft>
</keywords>
<author><json:item><name>M. E. Bell</name>
<affiliations><json:string>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</json:string>
<json:string>E-mail: meb1w07@soton.ac.uk</json:string>
</affiliations>
</json:item>
<json:item><name>T. Tzioumis</name>
<affiliations><json:string>Australia Telescope National Facility, CSIRO, Marsfield, NSW 2122, Australia</json:string>
</affiliations>
</json:item>
<json:item><name>P. Uttley</name>
<affiliations><json:string>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</json:string>
</affiliations>
</json:item>
<json:item><name>R. P. Fender</name>
<affiliations><json:string>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</json:string>
</affiliations>
</json:item>
<json:item><name>P. Arévalo</name>
<affiliations><json:string>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Strasse 1, 85741 Garching, Germany</json:string>
<json:string>Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile</json:string>
</affiliations>
</json:item>
<json:item><name>E. Breedt</name>
<affiliations><json:string>Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL</json:string>
</affiliations>
</json:item>
<json:item><name>I. McHardy</name>
<affiliations><json:string>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</json:string>
</affiliations>
</json:item>
<json:item><name>D. E. Calvelo</name>
<affiliations><json:string>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</json:string>
</affiliations>
</json:item>
<json:item><name>O. Jamil</name>
<affiliations><json:string>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</json:string>
</affiliations>
</json:item>
<json:item><name>E. Körding</name>
<affiliations><json:string>AIM/CEA Saclay and University Paris Diderot, l'Orme des Merisers, F‐91219 Gif‐sur‐Yvette CEDEX, France</json:string>
</affiliations>
</json:item>
</author>
<subject><json:item><lang><json:string>eng</json:string>
</lang>
<value>accretion, accretion discs</value>
</json:item>
<json:item><lang><json:string>eng</json:string>
</lang>
<value>techniques: interferometric</value>
</json:item>
<json:item><lang><json:string>eng</json:string>
</lang>
<value>galaxies: active</value>
</json:item>
</subject>
<articleId><json:string>MNR17692</json:string>
</articleId>
<arkIstex>ark:/67375/WNG-2MJ1GNZR-W</arkIstex>
<language><json:string>eng</json:string>
</language>
<originalGenre><json:string>article</json:string>
</originalGenre>
<abstract>We present the results of a ∼3 yr campaign to monitor the low‐luminosity active galactic nucleus (LLAGN) NGC 7213 in the radio (4.8 and 8.4 GHz) and X‐ray bands (2–10 keV). With a reported X‐ray Eddington ratio of 7 × 10−4LEdd, NGC 7213 can be considered to be comparable to a hard‐state black hole X‐ray binary. We show that a weak correlation exists between the X‐ray and radio light curves. We use the cross‐correlation function to calculate a global time‐lag between events in the X‐ray and radio bands to be 24 ± 12 d lag (8.4 GHz radio lagging X‐ray) and 40 ± 13 d lag (4.8 GHz radio lagging X‐ray), respectively. The radio–radio light curves are extremely well correlated with a lag of 20.5 ± 12.9 d (4.8 GHz lagging 8.4 GHz). We explore the previously established scaling relationship between core radio and X‐ray luminosities and black hole mass LR∝M0.6‐0.8L0.6X, known as the ‘Fundamental Plane of black hole activity’, and show that NGC 7213 lies very close to the best‐fitting ‘global’ correlation for the plane as one of the most‐luminous LLAGNs. With a large number of quasi‐simultaneous radio and X‐ray observations, we explore for the first time the variations of a single AGN with respect to the Fundamental Plane. Although the average radio and X‐ray luminosities for NGC 7213 are in good agreement with the Plane, we show that there is intrinsic scatter with respect to the Plane for the individual data points.</abstract>
<qualityIndicators><score>9.844</score>
<pdfWordCount>7988</pdfWordCount>
<pdfCharCount>42123</pdfCharCount>
<pdfVersion>1.4</pdfVersion>
<pdfPageCount>9</pdfPageCount>
<pdfPageSize>595.274 x 782.286 pts</pdfPageSize>
<refBibsNative>true</refBibsNative>
<abstractWordCount>237</abstractWordCount>
<abstractCharCount>1430</abstractCharCount>
<keywordCount>3</keywordCount>
</qualityIndicators>
<title>X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213</title>
<genre><json:string>article</json:string>
</genre>
<host><title>Monthly Notices of the Royal Astronomical Society</title>
<language><json:string>unknown</json:string>
</language>
<doi><json:string>10.1111/(ISSN)1365-2966</json:string>
</doi>
<issn><json:string>0035-8711</json:string>
</issn>
<eissn><json:string>1365-2966</json:string>
</eissn>
<publisherId><json:string>MNR</json:string>
</publisherId>
<volume>411</volume>
<issue>1</issue>
<pages><first>402</first>
<last>410</last>
<total>9</total>
</pages>
<genre><json:string>journal</json:string>
</genre>
</host>
<namedEntities><unitex><date><json:string>2011</json:string>
<json:string>1000</json:string>
</date>
<geogName></geogName>
<orgName><json:string>Australia Accepted</json:string>
<json:string>ATCA</json:string>
<json:string>Department of Physics, University of Warwick, Gibbet Hill Road, Coventry</json:string>
<json:string>National Facility</json:string>
<json:string>Australia Telescope</json:string>
<json:string>Australia Telescope Compact Array</json:string>
<json:string>Telescope National Facility, CSIRO, Mars</json:string>
</orgName>
<orgName_funder></orgName_funder>
<orgName_provider></orgName_provider>
<persName><json:string>Paul O’Neill</json:string>
<json:string>Anthony Rushton</json:string>
<json:string>I. McHardy</json:string>
<json:string>E. Breedt</json:string>
<json:string>P. Fender</json:string>
<json:string>Kirpal</json:string>
<json:string>Paris Diderot</json:string>
<json:string>O. Jamil</json:string>
<json:string>Andres Bello</json:string>
<json:string>D. E. Calvelo</json:string>
<json:string>Sadie Jones</json:string>
<json:string>P. Ar</json:string>
<json:string>P. Uttley</json:string>
<json:string>Sera Markoff</json:string>
<json:string>Ray Flux</json:string>
<json:string>Jane Turner</json:string>
<json:string>Although</json:string>
<json:string>E. Bell</json:string>
</persName>
<placeName><json:string>Terashima</json:string>
<json:string>Australia</json:string>
<json:string>Chile</json:string>
<json:string>Santiago</json:string>
<json:string>Gif-sur-Yvette</json:string>
<json:string>Compton</json:string>
<json:string>France</json:string>
</placeName>
<ref_url></ref_url>
<ref_bibl><json:string>M. E. Bell et al.</json:string>
<json:string>Gallo et al. (2006)</json:string>
<json:string>Peterson et al. (1998)</json:string>
<json:string>Bignall et al. (2004)</json:string>
<json:string>Hameed et al. 2001</json:string>
<json:string>Rees 1978</json:string>
<json:string>Spada et al. 2001</json:string>
<json:string>Nandra & Pounds 1994</json:string>
<json:string>Maccarone, Gallo & Fender 2003</json:string>
<json:string>Kellermann et al. 1989</json:string>
<json:string>Fender et al. 2007</json:string>
<json:string>Slee et al. 1994</json:string>
<json:string>Falcke et al. (2004)</json:string>
<json:string>Xue & Cui 2007</json:string>
<json:string>Fender et al. 1999</json:string>
<json:string>Turner & Pounds 1989</json:string>
<json:string>Bianchi et al. (2008)</json:string>
<json:string>Falcke, Markoff & Bower 2009</json:string>
<json:string>Jonker et al. 2010</json:string>
<json:string>Peterson et al. 1998</json:string>
<json:string>Calvelo et al. 2010</json:string>
<json:string>Blank, Harnett & Jones 2005</json:string>
<json:string>Marscher et al. 2002</json:string>
<json:string>Panessa et al. (2007)</json:string>
<json:string>McHardy et al. 2006</json:string>
<json:string>Halpern & Filippenko 1984</json:string>
<json:string>Russell et al. 2009</json:string>
<json:string>Dunn et al. 2010</json:string>
<json:string>Koratkar & Gaskell 1991</json:string>
<json:string>Thean et al. 2001</json:string>
<json:string>van der Laan 1966</json:string>
<json:string>Starling et al. 2005</json:string>
<json:string>Falcke et al. 2004</json:string>
<json:string>Merloni et al. 2003</json:string>
<json:string>Felten 1967</json:string>
<json:string>Blank et al. 2005</json:string>
<json:string>Falcke et al. 2009</json:string>
<json:string>Gallo 2007</json:string>
<json:string>Turner et al. 2001</json:string>
<json:string>Casella et al. (2010)</json:string>
<json:string>Bianchi et al. 2008</json:string>
<json:string>Breedt et al. 2009</json:string>
<json:string>Blank et al. (2005)</json:string>
<json:string>Mellon (2002)</json:string>
<json:string>Tzioumis 1997</json:string>
<json:string>Corbel et al. (2003)</json:string>
<json:string>Starling et al. (2005)</json:string>
<json:string>Bransford et al. 1998</json:string>
<json:string>Mirabel et al. 1998</json:string>
<json:string>Pooley & Fender 1997</json:string>
<json:string>Blandford & Konigl 1979</json:string>
<json:string>Bianchi et al. 2003, 2008</json:string>
</ref_bibl>
<bibl></bibl>
</unitex>
</namedEntities>
<ark><json:string>ark:/67375/WNG-2MJ1GNZR-W</json:string>
</ark>
<categories><wos><json:string>1 - science</json:string>
<json:string>2 - astronomy & astrophysics</json:string>
</wos>
<scienceMetrix><json:string>1 - natural sciences</json:string>
<json:string>2 - physics & astronomy</json:string>
<json:string>3 - astronomy & astrophysics</json:string>
</scienceMetrix>
<scopus><json:string>1 - Physical Sciences</json:string>
<json:string>2 - Earth and Planetary Sciences</json:string>
<json:string>3 - Space and Planetary Science</json:string>
<json:string>1 - Physical Sciences</json:string>
<json:string>2 - Physics and Astronomy</json:string>
<json:string>3 - Astronomy and Astrophysics</json:string>
</scopus>
<inist><json:string>1 - sciences appliquees, technologies et medecines</json:string>
<json:string>2 - sciences exactes et technologie</json:string>
<json:string>3 - terre, ocean, espace</json:string>
<json:string>4 - astronomie</json:string>
</inist>
</categories>
<publicationDate>2011</publicationDate>
<copyrightDate>2011</copyrightDate>
<doi><json:string>10.1111/j.1365-2966.2010.17692.x</json:string>
</doi>
<id>8B40C620A40D05F69CB1F0C860A7194D684BA528</id>
<score>1</score>
<fulltext><json:item><extension>pdf</extension>
<original>true</original>
<mimetype>application/pdf</mimetype>
<uri>https://api.istex.fr/document/8B40C620A40D05F69CB1F0C860A7194D684BA528/fulltext/pdf</uri>
</json:item>
<json:item><extension>zip</extension>
<original>false</original>
<mimetype>application/zip</mimetype>
<uri>https://api.istex.fr/document/8B40C620A40D05F69CB1F0C860A7194D684BA528/fulltext/zip</uri>
</json:item>
<istex:fulltextTEI uri="https://api.istex.fr/document/8B40C620A40D05F69CB1F0C860A7194D684BA528/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213</title>
</titleStmt>
<publicationStmt><authority>ISTEX</authority>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<availability><licence>© 2010 The Authors Monthly Notices of the Royal Astronomical Society © 2010 RAS</licence>
</availability>
<date type="published" when="2011-02-11"></date>
</publicationStmt>
<notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note>
<note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note>
</notesStmt>
<sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213</title>
<title level="a" type="short">NGC 7213: X‐ray and radio variability</title>
<author xml:id="author-0000" role="corresp"><persName><forename type="first">M. E.</forename>
<surname>Bell</surname>
</persName>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
<affiliation>E‐mail: meb1w07@soton.ac.uk</affiliation>
</author>
<author xml:id="author-0001"><persName><forename type="first">T.</forename>
<surname>Tzioumis</surname>
</persName>
<affiliation>Australia Telescope National Facility, CSIRO, Marsfield, NSW 2122, Australia<address><country key="AU"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0002"><persName><forename type="first">P.</forename>
<surname>Uttley</surname>
</persName>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
</author>
<author xml:id="author-0003"><persName><forename type="first">R. P.</forename>
<surname>Fender</surname>
</persName>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
</author>
<author xml:id="author-0004"><persName><forename type="first">P.</forename>
<surname>Arévalo</surname>
</persName>
<affiliation>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Strasse 1, 85741 Garching, Germany<address><country key="DE"></country>
</address>
</affiliation>
<affiliation>Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile<address><country key="CL"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0005"><persName><forename type="first">E.</forename>
<surname>Breedt</surname>
</persName>
<affiliation>Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL</affiliation>
</author>
<author xml:id="author-0006"><persName><forename type="first">I.</forename>
<surname>McHardy</surname>
</persName>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
</author>
<author xml:id="author-0007"><persName><forename type="first">D. E.</forename>
<surname>Calvelo</surname>
</persName>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
</author>
<author xml:id="author-0008"><persName><forename type="first">O.</forename>
<surname>Jamil</surname>
</persName>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
</author>
<author xml:id="author-0009"><persName><forename type="first">E.</forename>
<surname>Körding</surname>
</persName>
<affiliation>AIM/CEA Saclay and University Paris Diderot, l'Orme des Merisers, F‐91219 Gif‐sur‐Yvette CEDEX, France<address><country key="FR"></country>
</address>
</affiliation>
</author>
<idno type="istex">8B40C620A40D05F69CB1F0C860A7194D684BA528</idno>
<idno type="ark">ark:/67375/WNG-2MJ1GNZR-W</idno>
<idno type="DOI">10.1111/j.1365-2966.2010.17692.x</idno>
<idno type="unit">MNR17692</idno>
<idno type="toTypesetVersion">file:MNR.MNR17692.pdf</idno>
</analytic>
<monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title>
<idno type="pISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<idno type="book-DOI">10.1111/(ISSN)1365-2966</idno>
<idno type="book-part-DOI">10.1111/mnr.2011.411.issue-1</idno>
<idno type="product">MNR</idno>
<idno type="publisherDivision">ST</idno>
<imprint><biblScope unit="vol">411</biblScope>
<biblScope unit="issue">1</biblScope>
<biblScope unit="page" from="402">402</biblScope>
<biblScope unit="page" to="410">410</biblScope>
<biblScope unit="page-count">9</biblScope>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<date type="published" when="2011-02-11"></date>
</imprint>
</monogr>
</biblStruct>
</sourceDesc>
</fileDesc>
<profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head>
<p>We present the results of a ∼3 yr campaign to monitor the low‐luminosity active galactic nucleus (LLAGN) NGC 7213 in the radio (4.8 and 8.4 GHz) and X‐ray bands (2–10 keV). With a reported X‐ray Eddington ratio of <emph><span>7 × 10<hi rend="superscript">−4</hi>
<hi rend="italic">L</hi>
<hi rend="subscript">Edd</hi>
</span>
</emph>
, NGC 7213 can be considered to be comparable to a hard‐state black hole X‐ray binary. We show that a weak correlation exists between the X‐ray and radio light curves. We use the cross‐correlation function to calculate a global time‐lag between events in the X‐ray and radio bands to be 24 ± 12 d lag (8.4 GHz radio lagging X‐ray) and <emph><span>40 ± 13</span>
</emph>
 d lag (4.8 GHz radio lagging X‐ray), respectively. The radio–radio light curves are extremely well correlated with a lag of 20.5 ± 12.9 d (4.8 GHz lagging 8.4 GHz). We explore the previously established scaling relationship between core radio and X‐ray luminosities and black hole mass <emph><span><hi rend="italic">L</hi>
<hi rend="subscript">R</hi>
∝<hi rend="italic">M</hi>
<hi rend="superscript">0.6‐0.8</hi>
<hi rend="italic">L</hi>
<hi rend="superscript">0.6</hi>
<hi rend="subscript">X</hi>
</span>
</emph>
, known as the ‘Fundamental Plane of black hole activity’, and show that NGC 7213 lies very close to the best‐fitting ‘global’ correlation for the plane as one of the most‐luminous LLAGNs. With a large number of quasi‐simultaneous radio and X‐ray observations, we explore for the first time the variations of a single AGN with respect to the Fundamental Plane. Although the average radio and X‐ray luminosities for NGC 7213 are in good agreement with the Plane, we show that there is intrinsic scatter with respect to the Plane for the individual data points.</p>
</abstract>
<textClass><keywords xml:lang="en"><term xml:id="k1">accretion, accretion discs</term>
<term xml:id="k2">techniques: interferometric</term>
<term xml:id="k3">galaxies: active</term>
</keywords>
<keywords rend="tocHeading1"><term>Papers</term>
</keywords>
</textClass>
<langUsage><language ident="en"></language>
</langUsage>
</profileDesc>
</teiHeader>
</istex:fulltextTEI>
<json:item><extension>txt</extension>
<original>false</original>
<mimetype>text/plain</mimetype>
<uri>https://api.istex.fr/document/8B40C620A40D05F69CB1F0C860A7194D684BA528/fulltext/txt</uri>
</json:item>
</fulltext>
<metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration>
<istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName>
<publisherLoc>Oxford, UK</publisherLoc>
</publisherInfo>
<doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi>
<issn type="print">0035-8711</issn>
<issn type="electronic">1365-2966</issn>
<idGroup><id type="product" value="MNR"></id>
<id type="publisherDivision" value="ST"></id>
</idGroup>
<titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title>
</titleGroup>
</publicationMeta>
<publicationMeta level="part" position="02101"><doi origin="wiley">10.1111/mnr.2011.411.issue-1</doi>
<numberingGroup><numbering type="journalVolume" number="411">411</numbering>
<numbering type="journalIssue" number="1">1</numbering>
</numberingGroup>
<coverDate startDate="2011-02-11">February 2011</coverDate>
</publicationMeta>
<publicationMeta level="unit" type="article" position="36" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2010.17692.x</doi>
<idGroup><id type="unit" value="MNR17692"></id>
</idGroup>
<countGroup><count type="pageTotal" number="9"></count>
</countGroup>
<titleGroup><title type="tocHeading1">Papers</title>
</titleGroup>
<copyright>© 2010 The Authors Monthly Notices of the Royal Astronomical Society © 2010 RAS</copyright>
<eventGroup><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.4.4 mode:FullText" date="2011-01-21"></event>
<event type="publishedOnlineEarlyUnpaginated" date="2010-11-23"></event>
<event type="firstOnline" date="2010-11-23"></event>
<event type="publishedOnlineFinalForm" date="2011-01-21"></event>
<event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-03"></event>
<event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event>
</eventGroup>
<numberingGroup><numbering type="pageFirst" number="402">402</numbering>
<numbering type="pageLast" number="410">410</numbering>
</numberingGroup>
<correspondenceTo>
E‐mail: <email>meb1w07@soton.ac.uk</email>
</correspondenceTo>
<linkGroup><link type="toTypesetVersion" href="file:MNR.MNR17692.pdf"></link>
</linkGroup>
</publicationMeta>
<contentMeta><unparsedEditorialHistory>Accepted 2010 September 10. Received 2010 September 9; in original form 2010 July 1</unparsedEditorialHistory>
<countGroup><count type="figureTotal" number="7"></count>
<count type="tableTotal" number="2"></count>
<count type="formulaTotal" number="101"></count>
<count type="referenceTotal" number="58"></count>
<count type="linksCrossRef" number="128"></count>
</countGroup>
<titleGroup><title type="main">X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213</title>
<title type="shortAuthors"><i>M. E. Bell et al.</i>
</title>
<title type="short"><i>NGC 7213: X‐ray and radio variability</i>
</title>
</titleGroup>
<creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>M. E.</givenNames>
<familyName>Bell</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr2" affiliationRef="#a2"><personName><givenNames>T.</givenNames>
<familyName>Tzioumis</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr3" affiliationRef="#a1"><personName><givenNames>P.</givenNames>
<familyName>Uttley</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr4" affiliationRef="#a1"><personName><givenNames>R. P.</givenNames>
<familyName>Fender</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr5" affiliationRef="#a3 #a4"><personName><givenNames>P.</givenNames>
<familyName>Arévalo</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr6" affiliationRef="#a5"><personName><givenNames>E.</givenNames>
<familyName>Breedt</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr7" affiliationRef="#a1"><personName><givenNames>I.</givenNames>
<familyName>McHardy</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr8" affiliationRef="#a1"><personName><givenNames>D. E.</givenNames>
<familyName>Calvelo</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr9" affiliationRef="#a1"><personName><givenNames>O.</givenNames>
<familyName>Jamil</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr10" affiliationRef="#a6"><personName><givenNames>E.</givenNames>
<familyName>Körding</familyName>
</personName>
</creator>
</creators>
<affiliationGroup><affiliation xml:id="a1"><unparsedAffiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a2" countryCode="AU"><unparsedAffiliation>Australia Telescope National Facility, CSIRO, Marsfield, NSW 2122, Australia</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a3" countryCode="DE"><unparsedAffiliation>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Strasse 1, 85741 Garching, Germany</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a4" countryCode="CL"><unparsedAffiliation>Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a5"><unparsedAffiliation>Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a6" countryCode="FR"><unparsedAffiliation>AIM/CEA Saclay and University Paris Diderot, l'Orme des Merisers, F‐91219 Gif‐sur‐Yvette CEDEX, France</unparsedAffiliation>
</affiliation>
</affiliationGroup>
<keywordGroup xml:lang="en"><keyword xml:id="k1">accretion, accretion discs</keyword>
<keyword xml:id="k2">techniques: interferometric</keyword>
<keyword xml:id="k3">galaxies: active</keyword>
</keywordGroup>
<abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title>
<p>We present the results of a ∼3 yr campaign to monitor the low‐luminosity active galactic nucleus (LLAGN) NGC 7213 in the radio (4.8 and 8.4 GHz) and X‐ray bands (2–10 keV). With a reported X‐ray Eddington ratio of <span type="mathematics">7 × 10<sup>−4</sup>
<i>L</i>
<sub>Edd</sub>
</span>
, NGC 7213 can be considered to be comparable to a hard‐state black hole X‐ray binary. We show that a weak correlation exists between the X‐ray and radio light curves. We use the cross‐correlation function to calculate a global time‐lag between events in the X‐ray and radio bands to be 24 ± 12 d lag (8.4 GHz radio lagging X‐ray) and <span type="mathematics">40 ± 13</span>
 d lag (4.8 GHz radio lagging X‐ray), respectively. The radio–radio light curves are extremely well correlated with a lag of 20.5 ± 12.9 d (4.8 GHz lagging 8.4 GHz). We explore the previously established scaling relationship between core radio and X‐ray luminosities and black hole mass <span type="mathematics"><i>L</i>
<sub>R</sub>
∝<i>M</i>
<sup>0.6‐0.8</sup>
<i>L</i>
<sup>0.6</sup>
<sub>X</sub>
</span>
, known as the ‘Fundamental Plane of black hole activity’, and show that NGC 7213 lies very close to the best‐fitting ‘global’ correlation for the plane as one of the most‐luminous LLAGNs. With a large number of quasi‐simultaneous radio and X‐ray observations, we explore for the first time the variations of a single AGN with respect to the Fundamental Plane. Although the average radio and X‐ray luminosities for NGC 7213 are in good agreement with the Plane, we show that there is intrinsic scatter with respect to the Plane for the individual data points.</p>
</abstract>
</abstractGroup>
</contentMeta>
</header>
</component>
</istex:document>
</istex:metadataXml>
<mods version="3.6"><titleInfo lang="en"><title>X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213</title>
</titleInfo>
<titleInfo type="abbreviated" lang="en"><title>NGC 7213: X‐ray and radio variability</title>
</titleInfo>
<titleInfo type="alternative" contentType="CDATA" lang="en"><title>X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213</title>
</titleInfo>
<name type="personal"><namePart type="given">M. E.</namePart>
<namePart type="family">Bell</namePart>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
<affiliation>E-mail: meb1w07@soton.ac.uk</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">T.</namePart>
<namePart type="family">Tzioumis</namePart>
<affiliation>Australia Telescope National Facility, CSIRO, Marsfield, NSW 2122, Australia</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">P.</namePart>
<namePart type="family">Uttley</namePart>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">R. P.</namePart>
<namePart type="family">Fender</namePart>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">P.</namePart>
<namePart type="family">Arévalo</namePart>
<affiliation>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Strasse 1, 85741 Garching, Germany</affiliation>
<affiliation>Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">E.</namePart>
<namePart type="family">Breedt</namePart>
<affiliation>Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">I.</namePart>
<namePart type="family">McHardy</namePart>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">D. E.</namePart>
<namePart type="family">Calvelo</namePart>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">O.</namePart>
<namePart type="family">Jamil</namePart>
<affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">E.</namePart>
<namePart type="family">Körding</namePart>
<affiliation>AIM/CEA Saclay and University Paris Diderot, l'Orme des Merisers, F‐91219 Gif‐sur‐Yvette CEDEX, France</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<typeOfResource>text</typeOfResource>
<genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre>
<originInfo><publisher>Blackwell Publishing Ltd</publisher>
<place><placeTerm type="text">Oxford, UK</placeTerm>
</place>
<dateIssued encoding="w3cdtf">2011-02-11</dateIssued>
<edition>Accepted 2010 September 10. Received 2010 September 9; in original form 2010 July 1</edition>
<copyrightDate encoding="w3cdtf">2011</copyrightDate>
</originInfo>
<language><languageTerm type="code" authority="rfc3066">en</languageTerm>
<languageTerm type="code" authority="iso639-2b">eng</languageTerm>
</language>
<physicalDescription><extent unit="figures">7</extent>
<extent unit="tables">2</extent>
<extent unit="formulas">101</extent>
<extent unit="references">58</extent>
<extent unit="linksCrossRef">128</extent>
</physicalDescription>
<abstract lang="en">We present the results of a ∼3 yr campaign to monitor the low‐luminosity active galactic nucleus (LLAGN) NGC 7213 in the radio (4.8 and 8.4 GHz) and X‐ray bands (2–10 keV). With a reported X‐ray Eddington ratio of 7 × 10−4LEdd, NGC 7213 can be considered to be comparable to a hard‐state black hole X‐ray binary. We show that a weak correlation exists between the X‐ray and radio light curves. We use the cross‐correlation function to calculate a global time‐lag between events in the X‐ray and radio bands to be 24 ± 12 d lag (8.4 GHz radio lagging X‐ray) and 40 ± 13 d lag (4.8 GHz radio lagging X‐ray), respectively. The radio–radio light curves are extremely well correlated with a lag of 20.5 ± 12.9 d (4.8 GHz lagging 8.4 GHz). We explore the previously established scaling relationship between core radio and X‐ray luminosities and black hole mass LR∝M0.6‐0.8L0.6X, known as the ‘Fundamental Plane of black hole activity’, and show that NGC 7213 lies very close to the best‐fitting ‘global’ correlation for the plane as one of the most‐luminous LLAGNs. With a large number of quasi‐simultaneous radio and X‐ray observations, we explore for the first time the variations of a single AGN with respect to the Fundamental Plane. Although the average radio and X‐ray luminosities for NGC 7213 are in good agreement with the Plane, we show that there is intrinsic scatter with respect to the Plane for the individual data points.</abstract>
<subject lang="en"><genre>keywords</genre>
<topic>accretion, accretion discs</topic>
<topic>techniques: interferometric</topic>
<topic>galaxies: active</topic>
</subject>
<relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title>
</titleInfo>
<genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre>
<identifier type="ISSN">0035-8711</identifier>
<identifier type="eISSN">1365-2966</identifier>
<identifier type="DOI">10.1111/(ISSN)1365-2966</identifier>
<identifier type="PublisherID">MNR</identifier>
<part><date>2011</date>
<detail type="volume"><caption>vol.</caption>
<number>411</number>
</detail>
<detail type="issue"><caption>no.</caption>
<number>1</number>
</detail>
<extent unit="pages"><start>402</start>
<end>410</end>
<total>9</total>
</extent>
</part>
</relatedItem>
<identifier type="istex">8B40C620A40D05F69CB1F0C860A7194D684BA528</identifier>
<identifier type="ark">ark:/67375/WNG-2MJ1GNZR-W</identifier>
<identifier type="DOI">10.1111/j.1365-2966.2010.17692.x</identifier>
<identifier type="ArticleID">MNR17692</identifier>
<accessCondition type="use and reproduction" contentType="copyright">© 2010 The Authors Monthly Notices of the Royal Astronomical Society © 2010 RAS</accessCondition>
<recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource>
<recordOrigin>Blackwell Publishing Ltd</recordOrigin>
</recordInfo>
</mods>
<json:item><extension>json</extension>
<original>false</original>
<mimetype>application/json</mimetype>
<uri>https://api.istex.fr/document/8B40C620A40D05F69CB1F0C860A7194D684BA528/metadata/json</uri>
</json:item>
</metadata>
<serie></serie>
</istex>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/Istex/Corpus

HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 001A26 | SxmlIndent | more

HfdSelect -h $EXPLOR_AREA/Data/Istex/Corpus/biblio.hfd -nk 001A26 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
   |flux=    Istex
   |étape=   Corpus
   |type=    RBID
   |clé=     ISTEX:8B40C620A40D05F69CB1F0C860A7194D684BA528
   |texte=   X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213
}}

This area was generated with Dilib version V0.6.33.
Data generation: Tue Dec 5 10:43:12 2017. Site generation: Tue Mar 5 14:07:20 2024

	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.

Serveur d'exploration sur les relations entre la France et l'Australie

X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213

X‐ray and radio variability in the low‐luminosity active galactic nucleus NGC 7213

Source :

English descriptors

Abstract

Links to Exploration step

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri