Methane band and Spitzer mid‐IR imaging of L and T dwarf candidates in the Pleiades
Identifieur interne : 002151 ( Istex/Corpus ); précédent : 002150; suivant : 002152Methane band and Spitzer mid‐IR imaging of L and T dwarf candidates in the Pleiades
Auteurs : S. L. Casewell ; R. F. Jameson ; M. R. Burleigh ; P. D. Dobbie ; M. Roy ; S. T. Hodgkin ; E. MorauxSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-04-11.
English descriptors
- KwdEn :
- 2mass, Allard, Baraffe, Bihain, Bolometric luminosity, Bouvier, Brown dwarf, Burgasser, Casewell, Cluster members, Colour, Colours, Cond, Cond models, Dwarf, Dwarf candidates, Dwarf regime, Dwarf sequence, Effective temperature, Effective temperatures, Evolutionary models, Imaging, Irac, Kirkpatrick, Leggett, Lower gravity, Lower temperature, Lter, Luminosity, Methane, Methane absorption, Methane colour index, Mnras, Monthly notices, Niri, Photometric, Photometry, Pixel, Pleiades, Proper motions, Saumon marley, Spectral class, Spectral type, Spectral types, Spitzer, Spitzer imaging, Spitzer irac, Stauffer, Total luminosity, Zapatero osorio.
- Teeft :
- 2mass, Allard, Baraffe, Bihain, Bolometric luminosity, Bouvier, Brown dwarf, Burgasser, Casewell, Cluster members, Colour, Colours, Cond, Cond models, Dwarf, Dwarf candidates, Dwarf regime, Dwarf sequence, Effective temperature, Effective temperatures, Evolutionary models, Imaging, Irac, Kirkpatrick, Leggett, Lower gravity, Lower temperature, Lter, Luminosity, Methane, Methane absorption, Methane colour index, Mnras, Monthly notices, Niri, Photometric, Photometry, Pixel, Pleiades, Proper motions, Saumon marley, Spectral class, Spectral type, Spectral types, Spitzer, Spitzer imaging, Spitzer irac, Stauffer, Total luminosity, Zapatero osorio.
Abstract
We present Spitzer observations at [3.6] and [4.5] μm together with the methane short (1.58 μm) − methane long (1.69 μm) colour for three cool dwarfs in the Pleiades, PLZJ23, PLZJ93 and PLZJ100. We determine the effective temperatures of PLZJ23 and PLZJ93 to be ≈1200 and ≈1100 K. From the broad‐band photometry we place an upper limit of 1100 K on the effective temperature of PLZJ100 but lack the data required to determine the value more precisely. These temperatures are in the T dwarf regime, yet the methane colours indicate no methane is present. We attribute this to youth/low gravity in line with theoretical expectations. However, we find even less methane is present than predicted by the models. PLZJ23 and PLZJ93 are also very bright in the [3.6] μm waveband (PLZJ100 is not measured) compared to field brown dwarfs which can also be explained by this lack of methane. The definition of the T spectral class is the appearance of methane absorption, so strictly, via this definition, PLZJ93 and PLZJ100 cannot be described as T dwarfs. The colours of these two objects are, however, not compatible with those of L dwarfs. Thus we have a classification problem and cannot assign these objects a (photometric) spectral type.
Url:
DOI: 10.1111/j.1365-2966.2010.18044.x
Links to Exploration step
ISTEX:AFAD10993B6701AB35B7C74265A8EE5F834F5085Le document en format XML
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We determine the effective temperatures of PLZJ23 and PLZJ93 to be ≈1200 and ≈1100 K. From the broad‐band photometry we place an upper limit of 1100 K on the effective temperature of PLZJ100 but lack the data required to determine the value more precisely. These temperatures are in the T dwarf regime, yet the methane colours indicate no methane is present. We attribute this to youth/low gravity in line with theoretical expectations. However, we find even less methane is present than predicted by the models. PLZJ23 and PLZJ93 are also very bright in the [3.6] μm waveband (PLZJ100 is not measured) compared to field brown dwarfs which can also be explained by this lack of methane. The definition of the T spectral class is the appearance of methane absorption, so strictly, via this definition, PLZJ93 and PLZJ100 cannot be described as T dwarfs. The colours of these two objects are, however, not compatible with those of L dwarfs. Thus we have a classification problem and cannot assign these objects a (photometric) spectral type.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>methane</json:string><json:string>pleiades</json:string><json:string>colour</json:string><json:string>colours</json:string><json:string>lter</json:string><json:string>methane absorption</json:string><json:string>photometry</json:string><json:string>mnras</json:string><json:string>effective temperature</json:string><json:string>spectral type</json:string><json:string>spitzer</json:string><json:string>casewell</json:string><json:string>niri</json:string><json:string>burgasser</json:string><json:string>baraffe</json:string><json:string>2mass</json:string><json:string>stauffer</json:string><json:string>cond</json:string><json:string>allard</json:string><json:string>pixel</json:string><json:string>monthly notices</json:string><json:string>irac</json:string><json:string>bihain</json:string><json:string>photometric</json:string><json:string>dwarf</json:string><json:string>leggett</json:string><json:string>evolutionary models</json:string><json:string>spitzer imaging</json:string><json:string>brown dwarf</json:string><json:string>bouvier</json:string><json:string>kirkpatrick</json:string><json:string>dwarf candidates</json:string><json:string>spectral types</json:string><json:string>cond models</json:string><json:string>lower gravity</json:string><json:string>zapatero osorio</json:string><json:string>luminosity</json:string><json:string>effective temperatures</json:string><json:string>methane colour index</json:string><json:string>cluster members</json:string><json:string>proper motions</json:string><json:string>spectral class</json:string><json:string>spitzer irac</json:string><json:string>total luminosity</json:string><json:string>lower temperature</json:string><json:string>dwarf sequence</json:string><json:string>bolometric luminosity</json:string><json:string>dwarf regime</json:string><json:string>saumon marley</json:string><json:string>imaging</json:string></teeft></keywords><author><json:item><name>S. L. Casewell</name><affiliations><json:string>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</json:string><json:string>E-mail: slc25@star.le.ac.uk</json:string></affiliations></json:item><json:item><name>R. F. Jameson</name><affiliations><json:string>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</json:string></affiliations></json:item><json:item><name>M. R. Burleigh</name><affiliations><json:string>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</json:string></affiliations></json:item><json:item><name>P. D. Dobbie</name><affiliations><json:string>Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia</json:string></affiliations></json:item><json:item><name>M. Roy</name><affiliations><json:string>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</json:string></affiliations></json:item><json:item><name>S. T. Hodgkin</name><affiliations><json:string>CASU, Institute of Astronomy, University of Cambridge, Maddingley Road, Cambridge CB3 0HA</json:string></affiliations></json:item><json:item><name>E. Moraux</name><affiliations><json:string>Laboratoire d'Astrophysique, Observatoire de Grenoble, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>brown dwarfs</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stars: low‐mass</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>open clusters and associations: individual: Pleiades</value></json:item></subject><articleId><json:string>MNR18044</json:string></articleId><arkIstex>ark:/67375/WNG-G3F0G0VJ-3</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We present Spitzer observations at [3.6] and [4.5] μm together with the methane short (1.58 μm) − methane long (1.69 μm) colour for three cool dwarfs in the Pleiades, PLZJ23, PLZJ93 and PLZJ100. We determine the effective temperatures of PLZJ23 and PLZJ93 to be ≈1200 and ≈1100 K. From the broad‐band photometry we place an upper limit of 1100 K on the effective temperature of PLZJ100 but lack the data required to determine the value more precisely. These temperatures are in the T dwarf regime, yet the methane colours indicate no methane is present. We attribute this to youth/low gravity in line with theoretical expectations. However, we find even less methane is present than predicted by the models. PLZJ23 and PLZJ93 are also very bright in the [3.6] μm waveband (PLZJ100 is not measured) compared to field brown dwarfs which can also be explained by this lack of methane. The definition of the T spectral class is the appearance of methane absorption, so strictly, via this definition, PLZJ93 and PLZJ100 cannot be described as T dwarfs. The colours of these two objects are, however, not compatible with those of L dwarfs. Thus we have a classification problem and cannot assign these objects a (photometric) spectral type.</abstract><qualityIndicators><score>9.4</score><pdfWordCount>7296</pdfWordCount><pdfCharCount>38659</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>8</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>200</abstractWordCount><abstractCharCount>1234</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>Methane band and Spitzer mid‐IR imaging of L and T dwarf candidates in the Pleiades</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>412</volume><issue>3</issue><pages><first>2071</first><last>2078</last><total>8</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2011</json:string><json:string>1121</json:string><json:string>2007</json:string><json:string>1800</json:string><json:string>1100</json:string><json:string>1200</json:string></date><geogName></geogName><orgName><json:string>National Science Foundation</json:string><json:string>United Kingdom Infrared Telescope</json:string><json:string>Astronomy, Inc.</json:string><json:string>National Research Council</json:string><json:string>Australian Research Council</json:string><json:string>Ministerio de Ciencia</json:string><json:string>Jet Propulsion Laboratory, California Institute of Technology</json:string><json:string>Institute of Astronomy, University of Cambridge, Maddingley Road, Cambridge CB</json:string><json:string>University of Leicester</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>E. 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(2006)</json:string><json:string>Burgasser et al. 2002</json:string><json:string>Bouvier et al. 2008</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-G3F0G0VJ-3</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 biologiques et medicales</json:string><json:string>3 - sciences biologiques fondamentales et appliquees. psychologie</json:string></inist></categories><publicationDate>2011</publicationDate><copyrightDate>2011</copyrightDate><doi><json:string>10.1111/j.1365-2966.2010.18044.x</json:string></doi><id>AFAD10993B6701AB35B7C74265A8EE5F834F5085</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/AFAD10993B6701AB35B7C74265A8EE5F834F5085/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/AFAD10993B6701AB35B7C74265A8EE5F834F5085/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/AFAD10993B6701AB35B7C74265A8EE5F834F5085/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Methane band and <hi rend="italic">Spitzer</hi> mid‐IR imaging of L and T dwarf candidates in the Pleiades</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</licence></availability><date type="published" when="2011-04-11"></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">Methane band and <hi rend="italic">Spitzer</hi> mid‐IR imaging of L and T dwarf candidates in the Pleiades</title><title level="a" type="short">Methane and Spitzer imaging of the Pleiades</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">S. L.</forename><surname>Casewell</surname></persName><affiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</affiliation><affiliation>E‐mail: slc25@star.le.ac.uk</affiliation></author><author xml:id="author-0001"><persName><forename type="first">R. F.</forename><surname>Jameson</surname></persName><affiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</affiliation></author><author xml:id="author-0002"><persName><forename type="first">M. R.</forename><surname>Burleigh</surname></persName><affiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</affiliation></author><author xml:id="author-0003"><persName><forename type="first">P. D.</forename><surname>Dobbie</surname></persName><affiliation>Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">M.</forename><surname>Roy</surname></persName><affiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</affiliation></author><author xml:id="author-0005"><persName><forename type="first">S. T.</forename><surname>Hodgkin</surname></persName><affiliation>CASU, Institute of Astronomy, University of Cambridge, Maddingley Road, Cambridge CB3 0HA</affiliation></author><author xml:id="author-0006"><persName><forename type="first">E.</forename><surname>Moraux</surname></persName><affiliation>Laboratoire d'Astrophysique, Observatoire de Grenoble, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France<address><country key="FR"></country></address></affiliation></author><idno type="istex">AFAD10993B6701AB35B7C74265A8EE5F834F5085</idno><idno type="ark">ark:/67375/WNG-G3F0G0VJ-3</idno><idno type="DOI">10.1111/j.1365-2966.2010.18044.x</idno><idno type="unit">MNR18044</idno><idno type="toTypesetVersion">file:MNR.MNR18044.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.2011.412.issue-3</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">412</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="2071">2071</biblScope><biblScope unit="page" to="2078">2078</biblScope><biblScope unit="page-count">8</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-04-11"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>We present <hi rend="italic">Spitzer</hi> observations at [3.6] and [4.5] μm together with the methane short (1.58 μm<emph><span>) − methane</span></emph> long (1.69 μm) colour for three cool dwarfs in the Pleiades, PLZJ23, PLZJ93 and PLZJ100. We determine the effective temperatures of PLZJ23 and PLZJ93 to be ≈1200 and <emph><span>≈1100</span></emph> K. From the broad‐band photometry we place an upper limit of 1100 K on the effective temperature of PLZJ100 but lack the data required to determine the value more precisely. These temperatures are in the T dwarf regime, yet the methane colours indicate no methane is present. We attribute this to youth/low gravity in line with theoretical expectations. However, we find even less methane is present than predicted by the models.</p><p>PLZJ23 and PLZJ93 are also very bright in the [3.6] μm waveband (PLZJ100 is not measured) compared to field brown dwarfs which can also be explained by this lack of methane.</p><p>The definition of the T spectral class is the appearance of methane absorption, so strictly, via this definition, PLZJ93 and PLZJ100 cannot be described as T dwarfs. The colours of these two objects are, however, not compatible with those of L dwarfs. Thus we have a classification problem and cannot assign these objects a (photometric) spectral type.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">brown dwarfs</term><term xml:id="k2">stars: low‐mass</term><term xml:id="k3">open clusters and associations: individual: Pleiades</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/AFAD10993B6701AB35B7C74265A8EE5F834F5085/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="04103"><doi origin="wiley">10.1111/mnr.2011.412.issue-3</doi><numberingGroup><numbering type="journalVolume" number="412">412</numbering><numbering type="journalIssue" number="3">3</numbering></numberingGroup><coverDate startDate="2011-04-11">April 2011</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="52" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2010.18044.x</doi><idGroup><id type="unit" value="MNR18044"></id></idGroup><countGroup><count type="pageTotal" number="8"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</copyright><eventGroup><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.4.8 mode:FullText" date="2011-04-04"></event><event type="publishedOnlineEarlyUnpaginated" date="2011-01-19"></event><event type="firstOnline" date="2011-01-19"></event><event type="publishedOnlineFinalForm" date="2011-04-04"></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="2071">2071</numbering><numbering type="pageLast" number="2078">2078</numbering></numberingGroup><correspondenceTo>
E‐mail: <email>slc25@star.le.ac.uk</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR18044.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2010 November 17. Received 2010 November 4; in original form 2010 September 17</unparsedEditorialHistory><countGroup><count type="figureTotal" number="8"></count><count type="tableTotal" number="3"></count><count type="formulaTotal" number="162"></count><count type="referenceTotal" number="55"></count><count type="linksCrossRef" number="128"></count></countGroup><titleGroup><title type="main">Methane band and <i>Spitzer</i> mid‐IR imaging of L and T dwarf candidates in the Pleiades</title><title type="shortAuthors"><i>S. L. Casewell et al.</i></title><title type="short"><i>Methane and Spitzer imaging of the Pleiades</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>S. 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T.</givenNames><familyName>Hodgkin</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a4"><personName><givenNames>E.</givenNames><familyName>Moraux</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1"><unparsedAffiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="AU"><unparsedAffiliation>Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a3"><unparsedAffiliation>CASU, Institute of Astronomy, University of Cambridge, Maddingley Road, Cambridge CB3 0HA</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="FR"><unparsedAffiliation>Laboratoire d'Astrophysique, Observatoire de Grenoble, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">brown dwarfs</keyword><keyword xml:id="k2">stars: low‐mass</keyword><keyword xml:id="k3">open clusters and associations: individual: Pleiades</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>We present <i>Spitzer</i> observations at [3.6] and [4.5] μm together with the methane short (1.58 μm<span type="mathematics">) − methane</span> long (1.69 μm) colour for three cool dwarfs in the Pleiades, PLZJ23, PLZJ93 and PLZJ100. We determine the effective temperatures of PLZJ23 and PLZJ93 to be ≈1200 and <span type="mathematics">≈1100</span> K. From the broad‐band photometry we place an upper limit of 1100 K on the effective temperature of PLZJ100 but lack the data required to determine the value more precisely. These temperatures are in the T dwarf regime, yet the methane colours indicate no methane is present. We attribute this to youth/low gravity in line with theoretical expectations. However, we find even less methane is present than predicted by the models.</p><p>PLZJ23 and PLZJ93 are also very bright in the [3.6] μm waveband (PLZJ100 is not measured) compared to field brown dwarfs which can also be explained by this lack of methane.</p><p>The definition of the T spectral class is the appearance of methane absorption, so strictly, via this definition, PLZJ93 and PLZJ100 cannot be described as T dwarfs. The colours of these two objects are, however, not compatible with those of L dwarfs. Thus we have a classification problem and cannot assign these objects a (photometric) spectral type.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Methane band and Spitzer mid‐IR imaging of L and T dwarf candidates in the Pleiades</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Methane and Spitzer imaging of the Pleiades</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Methane band and Spitzer mid‐IR imaging of L and T dwarf candidates in the Pleiades</title></titleInfo><name type="personal"><namePart type="given">S. L.</namePart><namePart type="family">Casewell</namePart><affiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</affiliation><affiliation>E-mail: slc25@star.le.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. F.</namePart><namePart type="family">Jameson</namePart><affiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M. R.</namePart><namePart type="family">Burleigh</namePart><affiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P. D.</namePart><namePart type="family">Dobbie</namePart><affiliation>Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Roy</namePart><affiliation>Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. T.</namePart><namePart type="family">Hodgkin</namePart><affiliation>CASU, Institute of Astronomy, University of Cambridge, Maddingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E.</namePart><namePart type="family">Moraux</namePart><affiliation>Laboratoire d'Astrophysique, Observatoire de Grenoble, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, 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">2011-04-11</dateIssued><edition>Accepted 2010 November 17. Received 2010 November 4; in original form 2010 September 17</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">8</extent><extent unit="tables">3</extent><extent unit="formulas">162</extent><extent unit="references">55</extent><extent unit="linksCrossRef">128</extent></physicalDescription><abstract lang="en">We present Spitzer observations at [3.6] and [4.5] μm together with the methane short (1.58 μm) − methane long (1.69 μm) colour for three cool dwarfs in the Pleiades, PLZJ23, PLZJ93 and PLZJ100. We determine the effective temperatures of PLZJ23 and PLZJ93 to be ≈1200 and ≈1100 K. From the broad‐band photometry we place an upper limit of 1100 K on the effective temperature of PLZJ100 but lack the data required to determine the value more precisely. These temperatures are in the T dwarf regime, yet the methane colours indicate no methane is present. We attribute this to youth/low gravity in line with theoretical expectations. However, we find even less methane is present than predicted by the models. PLZJ23 and PLZJ93 are also very bright in the [3.6] μm waveband (PLZJ100 is not measured) compared to field brown dwarfs which can also be explained by this lack of methane. The definition of the T spectral class is the appearance of methane absorption, so strictly, via this definition, PLZJ93 and PLZJ100 cannot be described as T dwarfs. The colours of these two objects are, however, not compatible with those of L dwarfs. Thus we have a classification problem and cannot assign these objects a (photometric) spectral type.</abstract><subject lang="en"><genre>keywords</genre><topic>brown dwarfs</topic><topic>stars: low‐mass</topic><topic>open clusters and associations: individual: Pleiades</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>412</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>2071</start><end>2078</end><total>8</total></extent></part></relatedItem><identifier type="istex">AFAD10993B6701AB35B7C74265A8EE5F834F5085</identifier><identifier type="ark">ark:/67375/WNG-G3F0G0VJ-3</identifier><identifier type="DOI">10.1111/j.1365-2966.2010.18044.x</identifier><identifier type="ArticleID">MNR18044</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 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/AFAD10993B6701AB35B7C74265A8EE5F834F5085/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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