Timing observations of rotating radio transients
Identifieur interne : 002965 ( Istex/Corpus ); précédent : 002964; suivant : 002966Timing observations of rotating radio transients
Auteurs : M. A. Mclaughlin ; A. G. Lyne ; E. F. Keane ; M. Kramer ; J. J. Miller ; D. R. Lorimer ; R. N. Manchester ; F. Camilo ; I. H. StairsSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009-12-11.
English descriptors
Abstract
We present radio timing measurements of six rotating radio transient (RRAT) sources discovered in the Parkes Multibeam Pulsar Survey. These provide four new phase‐connected timing solutions and two updated ones, making a total of seven of the original 11 reported RRATs now with high‐precision rotational and astrometric parameters. Three of these seven RRATs have magnetic fields greater than 1013 G, with spin‐down properties similar to those of the magnetars and X‐ray detected isolated neutron stars. Another two of these RRATs have long periods and large characteristic ages, and lie near the ‘death line’ for radio pulsar emission. The remaining two RRATs with timing solutions have properties typical of the bulk of the pulsar population. The new solutions offer insights into what might be responsible for the unusual emission properties. We demonstrate that the RRATs have significantly longer periods and higher magnetic fields than normal radio pulsars, and find no correlation with other spin‐down parameters. These solutions also provide precise positions, which will facilitate follow‐up studies at high energies, crucial for relating these sources with other neutron star populations.
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DOI: 10.1111/j.1365-2966.2009.15584.x
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These provide four new phase‐connected timing solutions and two updated ones, making a total of seven of the original 11 reported RRATs now with high‐precision rotational and astrometric parameters. Three of these seven RRATs have magnetic fields greater than 1013 G, with spin‐down properties similar to those of the magnetars and X‐ray detected isolated neutron stars. Another two of these RRATs have long periods and large characteristic ages, and lie near the ‘death line’ for radio pulsar emission. The remaining two RRATs with timing solutions have properties typical of the bulk of the pulsar population. The new solutions offer insights into what might be responsible for the unusual emission properties. We demonstrate that the RRATs have significantly longer periods and higher magnetic fields than normal radio pulsars, and find no correlation with other spin‐down parameters. 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Journal compilation © 2009 RAS</p></availability><date>2009</date></publicationStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a" type="main" xml:lang="en">Timing observations of rotating radio transients</title><author xml:id="author-1"><persName><forename type="first">M. A.</forename><surname>McLaughlin</surname></persName><email>maura.mclaughlin@mail.wvu.edu</email><note type="biography">http://sigproc.sourceforge.net</note><affiliation>http://sigproc.sourceforge.net</affiliation><affiliation>Department of Physics, West Virginia University, Morgantown, WV 26506, USA</affiliation><affiliation>National Radio Astronomy Observatory, Green Bank, WV 24944, USA</affiliation></author><author xml:id="author-2"><persName><forename type="first">A. G.</forename><surname>Lyne</surname></persName><affiliation>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building, Oxford Road, Manchester M13 9PL</affiliation></author><author xml:id="author-3"><persName><forename type="first">E. F.</forename><surname>Keane</surname></persName><affiliation>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building, Oxford Road, Manchester M13 9PL</affiliation></author><author xml:id="author-4"><persName><forename type="first">M.</forename><surname>Kramer</surname></persName><affiliation>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building, Oxford Road, Manchester M13 9PL</affiliation><affiliation>Max Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany</affiliation></author><author xml:id="author-5"><persName><forename type="first">J. J.</forename><surname>Miller</surname></persName><affiliation>Department of Physics, West Virginia University, Morgantown, WV 26506, USA</affiliation></author><author xml:id="author-6"><persName><forename type="first">D. R.</forename><surname>Lorimer</surname></persName><affiliation>Department of Physics, West Virginia University, Morgantown, WV 26506, USA</affiliation><affiliation>National Radio Astronomy Observatory, Green Bank, WV 24944, USA</affiliation></author><author xml:id="author-7"><persName><forename type="first">R. N.</forename><surname>Manchester</surname></persName><affiliation>ATNF‐CSIRO, PO Box 76, Epping, NSW 1710, Australia</affiliation></author><author xml:id="author-8"><persName><forename type="first">F.</forename><surname>Camilo</surname></persName><affiliation>Columbia Astrophysics Laboratory, Columbia University, 550 W. 120th Street, New York, NY 10027, USA</affiliation></author><author xml:id="author-9"><persName><forename type="first">I. H.</forename><surname>Stairs</surname></persName><affiliation>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada</affiliation></author></analytic><monogr><title level="j">Monthly Notices of the Royal Astronomical Society</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="DOI">10.1111/(ISSN)1365-2966</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2009-12-11"></date><biblScope unit="volume">400</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="1431">1431</biblScope><biblScope unit="page" to="1438">1438</biblScope></imprint></monogr><idno type="istex">BB8F3730ECC8DBD4A3D2CD1FA4F55F29D184FA5C</idno><idno type="DOI">10.1111/j.1365-2966.2009.15584.x</idno><idno type="ArticleID">MNR15584</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>2009</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>We present radio timing measurements of six rotating radio transient (RRAT) sources discovered in the Parkes Multibeam Pulsar Survey. These provide four new phase‐connected timing solutions and two updated ones, making a total of seven of the original 11 reported RRATs now with high‐precision rotational and astrometric parameters. Three of these seven RRATs have magnetic fields greater than 1013 G, with spin‐down properties similar to those of the magnetars and X‐ray detected isolated neutron stars. Another two of these RRATs have long periods and large characteristic ages, and lie near the ‘death line’ for radio pulsar emission. The remaining two RRATs with timing solutions have properties typical of the bulk of the pulsar population. The new solutions offer insights into what might be responsible for the unusual emission properties. We demonstrate that the RRATs have significantly longer periods and higher magnetic fields than normal radio pulsars, and find no correlation with other spin‐down parameters. These solutions also provide precise positions, which will facilitate follow‐up studies at high energies, crucial for relating these sources with other neutron star populations.</p></abstract><textClass xml:lang="en"><keywords scheme="keyword"><list><head>keywords</head><item><term>stars: neutron</term></item><item><term>pulsars: general</term></item><item><term>Galaxy: stellar content</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2009-12-11">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api-v5.istex.fr/document/BB8F3730ECC8DBD4A3D2CD1FA4F55F29D184FA5C/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="12003"><doi origin="wiley">10.1111/mnr.2009.400.issue-3</doi><numberingGroup><numbering type="journalVolume" number="400">400</numbering><numbering type="journalIssue" number="3">3</numbering></numberingGroup><coverDate startDate="2009-12-11">December 2009</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="22" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2009.15584.x</doi><idGroup><id type="unit" value="MNR15584"></id></idGroup><countGroup><count type="pageTotal" number="8"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2009 The Authors. 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Received 2009 August 12; in original form 2009 June 26</unparsedEditorialHistory><countGroup><count type="figureTotal" number="5"></count><count type="tableTotal" number="4"></count><count type="formulaTotal" number="90"></count><count type="referenceTotal" number="40"></count><count type="linksCrossRef" number="103"></count></countGroup><titleGroup><title type="main">Timing observations of rotating radio transients</title><title type="shortAuthors"><i>M. A. McLaughlin et al.</i></title><title type="short"><i>Timing observations of RRATs</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1 #a2" noteRef="#fn1" corresponding="yes"><personName><givenNames>M. A.</givenNames><familyName>McLaughlin</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a3"><personName><givenNames>A. G.</givenNames><familyName>Lyne</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a3"><personName><givenNames>E. F.</givenNames><familyName>Keane</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a3 #a4"><personName><givenNames>M.</givenNames><familyName>Kramer</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a1"><personName><givenNames>J. J.</givenNames><familyName>Miller</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a1 #a2"><personName><givenNames>D. R.</givenNames><familyName>Lorimer</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a5"><personName><givenNames>R. N.</givenNames><familyName>Manchester</familyName></personName></creator><creator creatorRole="author" xml:id="cr8" affiliationRef="#a6"><personName><givenNames>F.</givenNames><familyName>Camilo</familyName></personName></creator><creator creatorRole="author" xml:id="cr9" affiliationRef="#a7"><personName><givenNames>I. H.</givenNames><familyName>Stairs</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="US"><unparsedAffiliation>Department of Physics, West Virginia University, Morgantown, WV 26506, USA</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="US"><unparsedAffiliation>National Radio Astronomy Observatory, Green Bank, WV 24944, USA</unparsedAffiliation></affiliation><affiliation xml:id="a3"><unparsedAffiliation>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building, Oxford Road, Manchester M13 9PL</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="DE"><unparsedAffiliation>Max Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="AU"><unparsedAffiliation>ATNF‐CSIRO, PO Box 76, Epping, NSW 1710, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="US"><unparsedAffiliation>Columbia Astrophysics Laboratory, Columbia University, 550 W. 120th Street, New York, NY 10027, USA</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="CA"><unparsedAffiliation>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">stars: neutron</keyword><keyword xml:id="k2">pulsars: general</keyword><keyword xml:id="k3">Galaxy: stellar content</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>We present radio timing measurements of six rotating radio transient (RRAT) sources discovered in the Parkes Multibeam Pulsar Survey. These provide four new phase‐connected timing solutions and two updated ones, making a total of seven of the original 11 reported RRATs now with high‐precision rotational and astrometric parameters. Three of these seven RRATs have magnetic fields greater than 10<sup>13</sup> G, with spin‐down properties similar to those of the magnetars and X‐ray detected isolated neutron stars. Another two of these RRATs have long periods and large characteristic ages, and lie near the ‘death line’ for radio pulsar emission. The remaining two RRATs with timing solutions have properties typical of the bulk of the pulsar population. The new solutions offer insights into what might be responsible for the unusual emission properties. We demonstrate that the RRATs have significantly longer periods and higher magnetic fields than normal radio pulsars, and find no correlation with other spin‐down parameters. These solutions also provide precise positions, which will facilitate follow‐up studies at high energies, crucial for relating these sources with other neutron star populations.</p></abstract></abstractGroup></contentMeta><noteGroup><note xml:id="fn3"><label>†</label><p>Alfred P. Sloan research fellow.</p></note></noteGroup></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Timing observations of rotating radio transients</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Timing observations of RRATs</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Timing observations of rotating radio transients</title></titleInfo><name type="personal"><namePart type="given">M. A.</namePart><namePart type="family">McLaughlin</namePart><affiliation>Department of Physics, West Virginia University, Morgantown, WV 26506, USA</affiliation><affiliation>National Radio Astronomy Observatory, Green Bank, WV 24944, USA</affiliation><description>http://sigproc.sourceforge.net</description><affiliation>E-mail: maura.mclaughlin@mail.wvu.edu</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A. G.</namePart><namePart type="family">Lyne</namePart><affiliation>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building, Oxford Road, Manchester M13 9PL</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E. F.</namePart><namePart type="family">Keane</namePart><affiliation>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building, Oxford Road, Manchester M13 9PL</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Kramer</namePart><affiliation>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building, Oxford Road, Manchester M13 9PL</affiliation><affiliation>Max Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J. J.</namePart><namePart type="family">Miller</namePart><affiliation>Department of Physics, West Virginia University, Morgantown, WV 26506, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D. R.</namePart><namePart type="family">Lorimer</namePart><affiliation>Department of Physics, West Virginia University, Morgantown, WV 26506, USA</affiliation><affiliation>National Radio Astronomy Observatory, Green Bank, WV 24944, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. N.</namePart><namePart type="family">Manchester</namePart><affiliation>ATNF‐CSIRO, PO Box 76, Epping, NSW 1710, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">F.</namePart><namePart type="family">Camilo</namePart><affiliation>Columbia Astrophysics Laboratory, Columbia University, 550 W. 120th Street, New York, NY 10027, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">I. H.</namePart><namePart type="family">Stairs</namePart><affiliation>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2009-12-11</dateIssued><edition>Accepted 2009 August 19. Received 2009 August 12; in original form 2009 June 26</edition><copyrightDate encoding="w3cdtf">2009</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType><extent unit="figures">5</extent><extent unit="tables">4</extent><extent unit="formulas">90</extent><extent unit="references">40</extent></physicalDescription><abstract lang="en">We present radio timing measurements of six rotating radio transient (RRAT) sources discovered in the Parkes Multibeam Pulsar Survey. These provide four new phase‐connected timing solutions and two updated ones, making a total of seven of the original 11 reported RRATs now with high‐precision rotational and astrometric parameters. Three of these seven RRATs have magnetic fields greater than 1013 G, with spin‐down properties similar to those of the magnetars and X‐ray detected isolated neutron stars. Another two of these RRATs have long periods and large characteristic ages, and lie near the ‘death line’ for radio pulsar emission. The remaining two RRATs with timing solutions have properties typical of the bulk of the pulsar population. The new solutions offer insights into what might be responsible for the unusual emission properties. We demonstrate that the RRATs have significantly longer periods and higher magnetic fields than normal radio pulsars, and find no correlation with other spin‐down parameters. These solutions also provide precise positions, which will facilitate follow‐up studies at high energies, crucial for relating these sources with other neutron star populations.</abstract><subject lang="en"><genre>keywords</genre><topic>stars: neutron</topic><topic>pulsars: general</topic><topic>Galaxy: stellar content</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal">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>2009</date><detail type="volume"><caption>vol.</caption><number>400</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>1431</start><end>1438</end><total>8</total></extent></part></relatedItem><identifier type="istex">BB8F3730ECC8DBD4A3D2CD1FA4F55F29D184FA5C</identifier><identifier type="DOI">10.1111/j.1365-2966.2009.15584.x</identifier><identifier type="ArticleID">MNR15584</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2009 The Authors. 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