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Radio sources in the 2dF Galaxy Redshift Survey – II. Local radio luminosity functions for AGN and star-forming galaxies at 1.4 GHz

Identifieur interne : 000896 ( Main/Corpus ); précédent : 000895; suivant : 000897

Radio sources in the 2dF Galaxy Redshift Survey – II. Local radio luminosity functions for AGN and star-forming galaxies at 1.4 GHz

Auteurs : Elaine M. Sadler ; Carole A. Jackson ; Russell D. Cannon ; Vincent J. Mcintyre ; Tara Murphy ; Joss Bland-Hawthorn ; Terry Bridges ; Shaun Cole ; Matthew Colless ; Chris Collins ; Warrick Couch ; Gavin Dalton ; Roberto De Propris ; Simon P. Driver ; George Efstathiou ; Richard S. Ellis ; Carlos S. Frenk ; Karl Glazebrook ; Ofer Lahav ; Ian Lewis ; Stuart Lumsden ; Steve Maddox ; Darren Madgwick ; Peder Norberg ; John A. Peacock ; Bruce A. Peterson ; Will Sutherland ; Keith Taylor

Source :

RBID : ISTEX:A9758DBD73B9A1040271D6C86D9C2EB336EDF1F5

English descriptors

Abstract

We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS), covering an effective area of 325deg2 (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications – the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4GHz for both active and star-forming galaxies, and derive a local star formation density of .

Url:
DOI: 10.1046/j.1365-8711.2002.04998.x

Links to Exploration step

ISTEX:A9758DBD73B9A1040271D6C86D9C2EB336EDF1F5

Le document en format XML

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<name sortKey="Couch, Warrick" sort="Couch, Warrick" uniqKey="Couch W" first="Warrick" last="Couch">Warrick Couch</name>
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<name sortKey="Couch, Warrick" sort="Couch, Warrick" uniqKey="Couch W" first="Warrick" last="Couch">Warrick Couch</name>
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<name sortKey="Dalton, Gavin" sort="Dalton, Gavin" uniqKey="Dalton G" first="Gavin" last="Dalton">Gavin Dalton</name>
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<name sortKey="De Propris, Roberto" sort="De Propris, Roberto" uniqKey="De Propris R" first="Roberto" last="De Propris">Roberto De Propris</name>
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</affiliation>
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<name sortKey="Driver, Simon P" sort="Driver, Simon P" uniqKey="Driver S" first="Simon P." last="Driver">Simon P. Driver</name>
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<name sortKey="Efstathiou, George" sort="Efstathiou, George" uniqKey="Efstathiou G" first="George" last="Efstathiou">George Efstathiou</name>
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<name sortKey="Frenk, Carlos S" sort="Frenk, Carlos S" uniqKey="Frenk C" first="Carlos S." last="Frenk">Carlos S. Frenk</name>
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<name sortKey="Lahav, Ofer" sort="Lahav, Ofer" uniqKey="Lahav O" first="Ofer" last="Lahav">Ofer Lahav</name>
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<name sortKey="Lumsden, Stuart" sort="Lumsden, Stuart" uniqKey="Lumsden S" first="Stuart" last="Lumsden">Stuart Lumsden</name>
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<name sortKey="Taylor, Keith" sort="Taylor, Keith" uniqKey="Taylor K" first="Keith" last="Taylor">Keith Taylor</name>
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<front>
<div type="abstract">We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS), covering an effective area of 325deg2 (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications – the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4GHz for both active and star-forming galaxies, and derive a local star formation density of .</div>
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<sup>9</sup>
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</contrib>
<contrib contrib-type="author">
<name>
<surname>Efstathiou</surname>
<given-names>George</given-names>
</name>
<xref ref-type="aff" rid="a10">
<sup>10</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Ellis</surname>
<given-names>Richard S.</given-names>
</name>
<xref ref-type="aff" rid="a11">
<sup>11</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Frenk</surname>
<given-names>Carlos S.</given-names>
</name>
<xref ref-type="aff" rid="a5">
<sup>5</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Glazebrook</surname>
<given-names>Karl</given-names>
</name>
<xref ref-type="aff" rid="a12">
<sup>12</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Lahav</surname>
<given-names>Ofer</given-names>
</name>
<xref ref-type="aff" rid="a10">
<sup>10</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Lewis</surname>
<given-names>Ian</given-names>
</name>
<xref ref-type="aff" rid="a3">
<sup>3</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Lumsden</surname>
<given-names>Stuart</given-names>
</name>
<xref ref-type="aff" rid="a13">
<sup>13</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Maddox</surname>
<given-names>Steve</given-names>
</name>
<xref ref-type="aff" rid="a14">
<sup>14</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Madgwick</surname>
<given-names>Darren</given-names>
</name>
<xref ref-type="aff" rid="a10">
<sup>10</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Norberg</surname>
<given-names>Peder</given-names>
</name>
<xref ref-type="aff" rid="a5">
<sup>5</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Peacock</surname>
<given-names>John A.</given-names>
</name>
<xref ref-type="aff" rid="a15">
<sup>15</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Peterson</surname>
<given-names>Bruce A.</given-names>
</name>
<xref ref-type="aff" rid="a2">
<sup>2</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Sutherland</surname>
<given-names>Will</given-names>
</name>
<xref ref-type="aff" rid="a8">
<sup>8</sup>
</xref>
</contrib>
<contrib contrib-type="author">
<name>
<surname>Taylor</surname>
<given-names>Keith</given-names>
</name>
<xref ref-type="aff" rid="a11">
<sup>11</sup>
</xref>
</contrib>
<aff id="a1">
<label>
<sup>1</sup>
</label>
School of Physics, University of Sydney, NSW 2006, Australia</aff>
<aff id="a2">
<label>
<sup>2</sup>
</label>
Research School of Astronomy and Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia</aff>
<aff id="a3">
<label>
<sup>3</sup>
</label>
Anglo-Australian Observatory, PO Box 296, Epping, NSW 2121, Australia</aff>
<aff id="a4">
<label>
<sup>4</sup>
</label>
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 2121, Australia</aff>
<aff id="a5">
<label>
<sup>5</sup>
</label>
Department of Physics, South Road, Durham DH1 3LE</aff>
<aff id="a6">
<label>
<sup>6</sup>
</label>
Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Birkenhead L14 1LD</aff>
<aff id="a7">
<label>
<sup>7</sup>
</label>
Department of Astrophysics, University of New South Wales, Sydney, NSW 2052, Australia</aff>
<aff id="a8">
<label>
<sup>8</sup>
</label>
Department of Physics, Keble Road, Oxford OX1 3RH</aff>
<aff id="a9">
<label>
<sup>9</sup>
</label>
School of Physics and Astronomy, North Haugh, St Andrews, Fife KY6 9SS</aff>
<aff id="a10">
<label>
<sup>10</sup>
</label>
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</aff>
<aff id="a11">
<label>
<sup>11</sup>
</label>
Department of Astronomy, Caltech, Pasadena, CA 91125, USA</aff>
<aff id="a12">
<label>
<sup>12</sup>
</label>
Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218-2686, USA</aff>
<aff id="a13">
<label>
<sup>13</sup>
</label>
Department of Physics, University of Leeds, Woodhouse Lane, Leeds LS2 9JT</aff>
<aff id="a14">
<label>
<sup>14</sup>
</label>
School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD</aff>
<aff id="a15">
<label>
<sup>15</sup>
</label>
Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</aff>
</contrib-group>
<author-notes>
<corresp id="cor1">
<label>
<sup></sup>
</label>
E-mail:
<email>ems@physics.usyd.edu.au</email>
</corresp>
</author-notes>
<pub-date pub-type="ppub">
<day>1</day>
<month>1</month>
<year>2002</year>
</pub-date>
<volume>329</volume>
<issue>1</issue>
<fpage>227</fpage>
<lpage>245</lpage>
<history>
<date date-type="received">
<day>20</day>
<month>8</month>
<year>2001</year>
</date>
<date date-type="accepted">
<day>4</day>
<month>9</month>
<year>2001</year>
</date>
</history>
<permissions>
<copyright-statement>© 2002 RAS</copyright-statement>
<copyright-year>2002</copyright-year>
</permissions>
<abstract>
<title>Abstract</title>
<p>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS), covering an effective area of 325deg
<sup>2</sup>
(about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications – the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range
<inline-graphic mimetype="image" xlink:href="329-1-227-eq001.tif"></inline-graphic>
to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4GHz for both active and star-forming galaxies, and derive a local star formation density of
<inline-graphic mimetype="image" xlink:href="329-1-227-eq002.tif"></inline-graphic>
<inline-graphic mimetype="image" xlink:href="329-1-227-eq003.tif"></inline-graphic>
.</p>
</abstract>
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<title>Keywords</title>
<kwd>galaxies: active</kwd>
<kwd>galaxies: luminosity function, mass function</kwd>
<kwd>galaxies: starburst</kwd>
<kwd>radio continuum: galaxies</kwd>
</kwd-group>
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<namePart type="given">Elaine M.</namePart>
<namePart type="family">Sadler</namePart>
<affiliation>School of Physics, University of Sydney, NSW 2006, Australia</affiliation>
<affiliation>E-mail: ems@physics.usyd.edu.au</affiliation>
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<namePart type="given">Carole A.</namePart>
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<name type="personal">
<namePart type="given">Russell D.</namePart>
<namePart type="family">Cannon</namePart>
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<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Vincent J.</namePart>
<namePart type="family">McIntyre</namePart>
<affiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 2121, Australia</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Tara</namePart>
<namePart type="family">Murphy</namePart>
<affiliation>School of Physics, University of Sydney, NSW 2006, Australia</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Joss</namePart>
<namePart type="family">Bland-Hawthorn</namePart>
<affiliation>Anglo-Australian Observatory, PO Box 296, Epping, NSW 2121, Australia</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Terry</namePart>
<namePart type="family">Bridges</namePart>
<affiliation>Anglo-Australian Observatory, PO Box 296, Epping, NSW 2121, Australia</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Shaun</namePart>
<namePart type="family">Cole</namePart>
<affiliation>Department of Physics, South Road, Durham DH1 3LE</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Matthew</namePart>
<namePart type="family">Colless</namePart>
<affiliation>Research School of Astronomy and Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Chris</namePart>
<namePart type="family">Collins</namePart>
<affiliation>Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Birkenhead L14 1LD</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Warrick</namePart>
<namePart type="family">Couch</namePart>
<affiliation>Department of Astrophysics, University of New South Wales, Sydney, NSW 2052, Australia</affiliation>
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<roleTerm type="text">author</roleTerm>
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</name>
<name type="personal">
<namePart type="given">Gavin</namePart>
<namePart type="family">Dalton</namePart>
<affiliation>Department of Physics, Keble Road, Oxford OX1 3RH</affiliation>
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<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Roberto</namePart>
<namePart type="family">de Propris</namePart>
<affiliation>Department of Astrophysics, University of New South Wales, Sydney, NSW 2052, Australia</affiliation>
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<roleTerm type="text">author</roleTerm>
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<name type="personal">
<namePart type="given">Simon P.</namePart>
<namePart type="family">Driver</namePart>
<affiliation>School of Physics and Astronomy, North Haugh, St Andrews, Fife KY6 9SS</affiliation>
<role>
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<name type="personal">
<namePart type="given">George</namePart>
<namePart type="family">Efstathiou</namePart>
<affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
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<name type="personal">
<namePart type="given">Richard S.</namePart>
<namePart type="family">Ellis</namePart>
<affiliation>Department of Astronomy, Caltech, Pasadena, CA 91125, USA</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
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<name type="personal">
<namePart type="given">Carlos S.</namePart>
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<affiliation>Department of Physics, South Road, Durham DH1 3LE</affiliation>
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<name type="personal">
<namePart type="given">Ian</namePart>
<namePart type="family">Lewis</namePart>
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<role>
<roleTerm type="text">author</roleTerm>
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</name>
<name type="personal">
<namePart type="given">Stuart</namePart>
<namePart type="family">Lumsden</namePart>
<affiliation>Department of Physics, University of Leeds, Woodhouse Lane, Leeds LS2 9JT</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
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</name>
<name type="personal">
<namePart type="given">Steve</namePart>
<namePart type="family">Maddox</namePart>
<affiliation>School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Darren</namePart>
<namePart type="family">Madgwick</namePart>
<affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
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</name>
<name type="personal">
<namePart type="given">Peder</namePart>
<namePart type="family">Norberg</namePart>
<affiliation>Department of Physics, South Road, Durham DH1 3LE</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
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</name>
<name type="personal">
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<name type="personal">
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<abstract>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS), covering an effective area of 325deg2 (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications – the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4GHz for both active and star-forming galaxies, and derive a local star formation density of .</abstract>
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