Testing the fragmentation limit in the Upper Sco association
Identifieur interne : 001D78 ( Istex/Corpus ); précédent : 001D77; suivant : 001D79Testing the fragmentation limit in the Upper Sco association
Auteurs : N. Lodieu ; N. C. Hambly ; P. D. Dobbie ; N. J. G. Cross ; L. Christensen ; E. L. Martin ; L. ValdivielsoSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-12-21.
English descriptors
- KwdEn :
- April, Arcsec, Baraffe, Brown dwarf, Candidate members, Central region, Cluster sequence, Colour, Colours, Constraint, Data reduction, Deep survey, Deg2, Deg2 area, Dobbie, Doublet, Dwarf, Dwarf candidates, Error bars, Fragmentation limit, Hambly, Imaging, Imaging survey, Jameson, Joint project, Kingdom telescope, Large telescope, Last column, Lodieu, Lter, Lters, Mass function, Median, Methane, Methane candidates, Methane colour, Methane imaging, Methane photometry, Methane survey, Mnras, Monthly notices, Msun, Open squares, Optical counterparts, Photometric, Photometric candidate, Photometric candidates, Photometric error bars, Photometric selection, Photometry, Pixel, Preibisch, Preibisch zinnecker, Proper motion, Proper motions, Quasar, Right ascension, Second epoch, Service mode, Slesnick, Spectral type, Spectral types, Spectroscopic, Spectroscopic members, Spectroscopically, Spie, Substellar, Telescope, Ukidss, Ukirt, Usco, Various diagrams, Weather conditions, Wfcam, Wircam, Zapatero osorio, Zinnecker.
- Teeft :
- April, Arcsec, Baraffe, Brown dwarf, Candidate members, Central region, Cluster sequence, Colour, Colours, Constraint, Data reduction, Deep survey, Deg2, Deg2 area, Dobbie, Doublet, Dwarf, Dwarf candidates, Error bars, Fragmentation limit, Hambly, Imaging, Imaging survey, Jameson, Joint project, Kingdom telescope, Large telescope, Last column, Lodieu, Lter, Lters, Mass function, Median, Methane, Methane candidates, Methane colour, Methane imaging, Methane photometry, Methane survey, Mnras, Monthly notices, Msun, Open squares, Optical counterparts, Photometric, Photometric candidate, Photometric candidates, Photometric error bars, Photometric selection, Photometry, Pixel, Preibisch, Preibisch zinnecker, Proper motion, Proper motions, Quasar, Right ascension, Second epoch, Service mode, Slesnick, Spectral type, Spectral types, Spectroscopic, Spectroscopic members, Spectroscopically, Spie, Substellar, Telescope, Ukidss, Ukirt, Usco, Various diagrams, Weather conditions, Wfcam, Wircam, Zapatero osorio, Zinnecker.
Abstract
We present the results of a deep (J∼ 21 at 5σ) infrared photometric survey of a 0.95‐deg2 area in the central region of the Upper Sco association. The photometric observations consist of a deep Y+J‐band image obtained with the Wide Field Camera on the United Kingdom Infra‐Red Telescope (UKIRT) with part coverage in Z complemented by the methane ON and OFF imaging survey conducted with the Wide‐field InfraRed Camera on the Canada–France–Hawaii Telescope. We have selected five potential T‐type objects belonging to the Upper Sco association on the basis of their blue methane colours and their J− CH4 off colours. We have also identified a sample of seven to eight Upper Sco member candidates bridging the gap between known cluster M types and our new T‐type candidates. These candidates were selected based on their positions in various colour–magnitude diagrams, and they follow the sequence of known Upper Sco members identified in the UKIRT Infrared Deep Sky Survey Galactic Clusters Survey. We present additional membership constraints using proper motion estimates from the multiple epochs available with us. We also present optical and near‐infrared spectra obtained with the X‐Shooter spectrograph on the Very Large Telescope for five L‐type candidates covering the 0.6–2.5 m wavelength range, none of which is confirmed as a young brown dwarf. We discuss the lack of detection of new candidate members as well as the possible turn‐down in the Upper Sco mass function as we are approaching the fragmentation limit.
Url:
DOI: 10.1111/j.1365-2966.2011.19651.x
Links to Exploration step
ISTEX:9CD17C38DE39F0E609976BB06609591924717BA8Le document en format XML
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members</term><term>Spectroscopically</term><term>Spie</term><term>Substellar</term><term>Telescope</term><term>Ukidss</term><term>Ukirt</term><term>Usco</term><term>Various diagrams</term><term>Weather conditions</term><term>Wfcam</term><term>Wircam</term><term>Zapatero osorio</term><term>Zinnecker</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>April</term><term>Arcsec</term><term>Baraffe</term><term>Brown dwarf</term><term>Candidate members</term><term>Central region</term><term>Cluster sequence</term><term>Colour</term><term>Colours</term><term>Constraint</term><term>Data reduction</term><term>Deep survey</term><term>Deg2</term><term>Deg2 area</term><term>Dobbie</term><term>Doublet</term><term>Dwarf</term><term>Dwarf candidates</term><term>Error bars</term><term>Fragmentation limit</term><term>Hambly</term><term>Imaging</term><term>Imaging survey</term><term>Jameson</term><term>Joint project</term><term>Kingdom telescope</term><term>Large telescope</term><term>Last column</term><term>Lodieu</term><term>Lter</term><term>Lters</term><term>Mass function</term><term>Median</term><term>Methane</term><term>Methane candidates</term><term>Methane colour</term><term>Methane imaging</term><term>Methane photometry</term><term>Methane survey</term><term>Mnras</term><term>Monthly notices</term><term>Msun</term><term>Open squares</term><term>Optical counterparts</term><term>Photometric</term><term>Photometric candidate</term><term>Photometric candidates</term><term>Photometric error bars</term><term>Photometric selection</term><term>Photometry</term><term>Pixel</term><term>Preibisch</term><term>Preibisch zinnecker</term><term>Proper motion</term><term>Proper motions</term><term>Quasar</term><term>Right ascension</term><term>Second epoch</term><term>Service mode</term><term>Slesnick</term><term>Spectral type</term><term>Spectral types</term><term>Spectroscopic</term><term>Spectroscopic members</term><term>Spectroscopically</term><term>Spie</term><term>Substellar</term><term>Telescope</term><term>Ukidss</term><term>Ukirt</term><term>Usco</term><term>Various diagrams</term><term>Weather conditions</term><term>Wfcam</term><term>Wircam</term><term>Zapatero osorio</term><term>Zinnecker</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present the results of a deep (J∼ 21 at 5σ) infrared photometric survey of a 0.95‐deg2 area in the central region of the Upper Sco association. The photometric observations consist of a deep Y+J‐band image obtained with the Wide Field Camera on the United Kingdom Infra‐Red Telescope (UKIRT) with part coverage in Z complemented by the methane ON and OFF imaging survey conducted with the Wide‐field InfraRed Camera on the Canada–France–Hawaii Telescope. We have selected five potential T‐type objects belonging to the Upper Sco association on the basis of their blue methane colours and their J− CH4 off colours. We have also identified a sample of seven to eight Upper Sco member candidates bridging the gap between known cluster M types and our new T‐type candidates. These candidates were selected based on their positions in various colour–magnitude diagrams, and they follow the sequence of known Upper Sco members identified in the UKIRT Infrared Deep Sky Survey Galactic Clusters Survey. We present additional membership constraints using proper motion estimates from the multiple epochs available with us. We also present optical and near‐infrared spectra obtained with the X‐Shooter spectrograph on the Very Large Telescope for five L‐type candidates covering the 0.6–2.5 m wavelength range, none of which is confirmed as a young brown dwarf. We discuss the lack of detection of new candidate members as well as the possible turn‐down in the Upper Sco mass function as we are approaching the fragmentation limit.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>usco</json:string><json:string>photometric</json:string><json:string>methane</json:string><json:string>lodieu</json:string><json:string>mnras</json:string><json:string>photometry</json:string><json:string>spectroscopic</json:string><json:string>fragmentation limit</json:string><json:string>colour</json:string><json:string>ukidss</json:string><json:string>april</json:string><json:string>quasar</json:string><json:string>hambly</json:string><json:string>arcsec</json:string><json:string>pixel</json:string><json:string>colours</json:string><json:string>monthly notices</json:string><json:string>mass function</json:string><json:string>wircam</json:string><json:string>doublet</json:string><json:string>wfcam</json:string><json:string>photometric candidates</json:string><json:string>deep survey</json:string><json:string>baraffe</json:string><json:string>lter</json:string><json:string>spie</json:string><json:string>deg2</json:string><json:string>proper motion</json:string><json:string>preibisch</json:string><json:string>lters</json:string><json:string>substellar</json:string><json:string>ukirt</json:string><json:string>dobbie</json:string><json:string>spectroscopically</json:string><json:string>methane colour</json:string><json:string>slesnick</json:string><json:string>zinnecker</json:string><json:string>msun</json:string><json:string>spectral type</json:string><json:string>dwarf candidates</json:string><json:string>methane survey</json:string><json:string>zapatero osorio</json:string><json:string>spectroscopic members</json:string><json:string>imaging survey</json:string><json:string>data reduction</json:string><json:string>central region</json:string><json:string>last column</json:string><json:string>median</json:string><json:string>deg2 area</json:string><json:string>methane candidates</json:string><json:string>cluster sequence</json:string><json:string>methane photometry</json:string><json:string>optical counterparts</json:string><json:string>right ascension</json:string><json:string>photometric candidate</json:string><json:string>photometric selection</json:string><json:string>proper motions</json:string><json:string>spectral types</json:string><json:string>jameson</json:string><json:string>dwarf</json:string><json:string>imaging</json:string><json:string>photometric error bars</json:string><json:string>error bars</json:string><json:string>brown dwarf</json:string><json:string>open squares</json:string><json:string>weather conditions</json:string><json:string>joint project</json:string><json:string>candidate members</json:string><json:string>large telescope</json:string><json:string>service mode</json:string><json:string>preibisch zinnecker</json:string><json:string>methane imaging</json:string><json:string>various diagrams</json:string><json:string>second epoch</json:string><json:string>kingdom telescope</json:string><json:string>constraint</json:string><json:string>telescope</json:string></teeft></keywords><author><json:item><name>N. Lodieu</name><affiliations><json:string>Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, E‐38200 La Laguna, Tenerife, Spain</json:string><json:string>Departamento de Astrofísica, Universidad de La Laguna (ULL), E‐38205 La Laguna, Tenerife, Spain</json:string><json:string>Based on observations made with the United Kingdom Infra‐Red Telescope, Canada–France–Hawaii Telescope and Very Large Telescope.E‐mail:</json:string><json:string>E-mail: nlodieu@iac.es</json:string></affiliations></json:item><json:item><name>N. C. Hambly</name><affiliations><json:string>Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</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>N. J. G. Cross</name><affiliations><json:string>Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</json:string></affiliations></json:item><json:item><name>L. Christensen</name><affiliations><json:string>Excellence Cluster Universe, Technische Universität München, Bolzmanstrasse 2, 85748 Garching bei München, Germany</json:string></affiliations></json:item><json:item><name>E. L. Martin</name><affiliations><json:string>CSIC‐INTA Centro de Astrobiología, Ctra. Ajalvir km 4, 28850, Torrejón de Ardoz, Madrid, Spain</json:string></affiliations></json:item><json:item><name>L. Valdivielso</name><affiliations><json:string>Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, E‐38200 La Laguna, Tenerife, Spain</json:string><json:string>Departamento de Astrofísica, Universidad de La Laguna (ULL), E‐38205 La Laguna, Tenerife, Spain</json:string><json:string>Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Plaza San Juan, 1, E‐44001 Teruel, Spain</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>techniques: photometric</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>techniques: spectroscopic</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>surveys</value></json:item><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>stars: luminosity function, mass function</value></json:item></subject><articleId><json:string>MNR19651</json:string></articleId><arkIstex>ark:/67375/WNG-W3LNHCV6-2</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We present the results of a deep (J∼ 21 at 5σ) infrared photometric survey of a 0.95‐deg2 area in the central region of the Upper Sco association. The photometric observations consist of a deep Y+J‐band image obtained with the Wide Field Camera on the United Kingdom Infra‐Red Telescope (UKIRT) with part coverage in Z complemented by the methane ON and OFF imaging survey conducted with the Wide‐field InfraRed Camera on the Canada–France–Hawaii Telescope. We have selected five potential T‐type objects belonging to the Upper Sco association on the basis of their blue methane colours and their J− CH4 off colours. We have also identified a sample of seven to eight Upper Sco member candidates bridging the gap between known cluster M types and our new T‐type candidates. These candidates were selected based on their positions in various colour–magnitude diagrams, and they follow the sequence of known Upper Sco members identified in the UKIRT Infrared Deep Sky Survey Galactic Clusters Survey. We present additional membership constraints using proper motion estimates from the multiple epochs available with us. We also present optical and near‐infrared spectra obtained with the X‐Shooter spectrograph on the Very Large Telescope for five L‐type candidates covering the 0.6–2.5 m wavelength range, none of which is confirmed as a young brown dwarf. 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(2007a)</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-W3LNHCV6-2</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></categories><publicationDate>2011</publicationDate><copyrightDate>2011</copyrightDate><doi><json:string>10.1111/j.1365-2966.2011.19651.x</json:string></doi><id>9CD17C38DE39F0E609976BB06609591924717BA8</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/9CD17C38DE39F0E609976BB06609591924717BA8/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/9CD17C38DE39F0E609976BB06609591924717BA8/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/9CD17C38DE39F0E609976BB06609591924717BA8/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Testing the fragmentation limit in the Upper Sco association</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2011 The Authors. 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E‐mail: nlodieu@iac.es</affiliation></author><author xml:id="author-0001"><persName><forename type="first">N. C.</forename><surname>Hambly</surname></persName><affiliation>Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</affiliation></author><author xml:id="author-0002"><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-0003"><persName><forename type="first">N. J. G.</forename><surname>Cross</surname></persName><affiliation>Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</affiliation></author><author xml:id="author-0004"><persName><forename type="first">L.</forename><surname>Christensen</surname></persName><affiliation>Excellence Cluster Universe, Technische Universität München, Bolzmanstrasse 2, 85748 Garching bei München, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">E. L.</forename><surname>Martin</surname></persName><affiliation>CSIC‐INTA Centro de Astrobiología, Ctra. 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The photometric observations consist of a deep <hi rend="italic">Y</hi>+<hi rend="italic">J</hi>‐band image obtained with the Wide Field Camera on the United Kingdom Infra‐Red Telescope (UKIRT) with part coverage in <hi rend="italic">Z</hi> complemented by the methane ON and OFF imaging survey conducted with the Wide‐field InfraRed Camera on the Canada–France–Hawaii Telescope. We have selected five potential T‐type objects belonging to the Upper Sco association on the basis of their blue methane colours and their <hi rend="italic">J</hi>− CH<hi rend="subscript">4 off</hi> colours. We have also identified a sample of seven to eight Upper Sco member candidates bridging the gap between known cluster M types and our new T‐type candidates. These candidates were selected based on their positions in various colour–magnitude diagrams, and they follow the sequence of known Upper Sco members identified in the UKIRT Infrared Deep Sky Survey Galactic Clusters Survey. We present additional membership constraints using proper motion estimates from the multiple epochs available with us. We also present optical and near‐infrared spectra obtained with the X‐Shooter spectrograph on the Very Large Telescope for five L‐type candidates covering the 0.6–2.5 <graphic url="equation/MNR_19651_mu1.gif" rend="inline image"></graphic>m wavelength range, none of which is confirmed as a young brown dwarf. 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Lodieu et al.</i></title><title type="short"><i>Testing the fragmentation limit in the USco</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1 #a2" corresponding="yes"><personName><givenNames>N.</givenNames><familyName>Lodieu</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a3"><personName><givenNames>N. C.</givenNames><familyName>Hambly</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a4"><personName><givenNames>P. D.</givenNames><familyName>Dobbie</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a3"><personName><givenNames>N. J. 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The photometric observations consist of a deep <i>Y</i>+<i>J</i>‐band image obtained with the Wide Field Camera on the United Kingdom Infra‐Red Telescope (UKIRT) with part coverage in <i>Z</i> complemented by the methane ON and OFF imaging survey conducted with the Wide‐field InfraRed Camera on the Canada–France–Hawaii Telescope. We have selected five potential T‐type objects belonging to the Upper Sco association on the basis of their blue methane colours and their <i>J</i>− CH<sub>4 off</sub> colours. We have also identified a sample of seven to eight Upper Sco member candidates bridging the gap between known cluster M types and our new T‐type candidates. These candidates were selected based on their positions in various colour–magnitude diagrams, and they follow the sequence of known Upper Sco members identified in the UKIRT Infrared Deep Sky Survey Galactic Clusters Survey. We present additional membership constraints using proper motion estimates from the multiple epochs available with us. We also present optical and near‐infrared spectra obtained with the X‐Shooter spectrograph on the Very Large Telescope for five L‐type candidates covering the 0.6–2.5 <inlineGraphic alt="inline image" location="equation/MNR_19651_mu1.gif" href=""></inlineGraphic>m wavelength range, none of which is confirmed as a young brown dwarf. We discuss the lack of detection of new candidate members as well as the possible turn‐down in the Upper Sco mass function as we are approaching the fragmentation limit.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Testing the fragmentation limit in the Upper Sco association</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Testing the fragmentation limit in the USco</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Testing the fragmentation limit in the Upper Sco association★</title></titleInfo><name type="personal"><namePart type="given">N.</namePart><namePart type="family">Lodieu</namePart><affiliation>Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, E‐38200 La Laguna, Tenerife, Spain</affiliation><affiliation>Departamento de Astrofísica, Universidad de La Laguna (ULL), E‐38205 La Laguna, Tenerife, Spain</affiliation><affiliation>Based on observations made with the United Kingdom Infra‐Red Telescope, Canada–France–Hawaii Telescope and Very Large Telescope.E‐mail:</affiliation><affiliation>E-mail: nlodieu@iac.es</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">N. C.</namePart><namePart type="family">Hambly</namePart><affiliation>Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</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">N. J. G.</namePart><namePart type="family">Cross</namePart><affiliation>Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L.</namePart><namePart type="family">Christensen</namePart><affiliation>Excellence Cluster Universe, Technische Universität München, Bolzmanstrasse 2, 85748 Garching bei München, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E. L.</namePart><namePart type="family">Martin</namePart><affiliation>CSIC‐INTA Centro de Astrobiología, Ctra. Ajalvir km 4, 28850, Torrejón de Ardoz, Madrid, Spain</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L.</namePart><namePart type="family">Valdivielso</namePart><affiliation>Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, E‐38200 La Laguna, Tenerife, Spain</affiliation><affiliation>Departamento de Astrofísica, Universidad de La Laguna (ULL), E‐38205 La Laguna, Tenerife, Spain</affiliation><affiliation>Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Plaza San Juan, 1, E‐44001 Teruel, Spain</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">2011-12-21</dateIssued><edition>Accepted 2011 August 18. Received 2011 August 18; in original form 2011 July 8</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">6</extent><extent unit="tables">9</extent><extent unit="formulas">20</extent><extent unit="references">82</extent><extent unit="linksCrossRef">199</extent></physicalDescription><abstract lang="en">We present the results of a deep (J∼ 21 at 5σ) infrared photometric survey of a 0.95‐deg2 area in the central region of the Upper Sco association. The photometric observations consist of a deep Y+J‐band image obtained with the Wide Field Camera on the United Kingdom Infra‐Red Telescope (UKIRT) with part coverage in Z complemented by the methane ON and OFF imaging survey conducted with the Wide‐field InfraRed Camera on the Canada–France–Hawaii Telescope. We have selected five potential T‐type objects belonging to the Upper Sco association on the basis of their blue methane colours and their J− CH4 off colours. We have also identified a sample of seven to eight Upper Sco member candidates bridging the gap between known cluster M types and our new T‐type candidates. These candidates were selected based on their positions in various colour–magnitude diagrams, and they follow the sequence of known Upper Sco members identified in the UKIRT Infrared Deep Sky Survey Galactic Clusters Survey. We present additional membership constraints using proper motion estimates from the multiple epochs available with us. We also present optical and near‐infrared spectra obtained with the X‐Shooter spectrograph on the Very Large Telescope for five L‐type candidates covering the 0.6–2.5 m wavelength range, none of which is confirmed as a young brown dwarf. We discuss the lack of detection of new candidate members as well as the possible turn‐down in the Upper Sco mass function as we are approaching the fragmentation limit.</abstract><note type="content">*</note><subject lang="en"><genre>keywords</genre><topic>techniques: photometric</topic><topic>techniques: spectroscopic</topic><topic>surveys</topic><topic>brown dwarfs</topic><topic>stars: low‐mass</topic><topic>stars: luminosity function, mass function</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>418</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>2604</start><end>2617</end><total>14</total></extent></part></relatedItem><identifier type="istex">9CD17C38DE39F0E609976BB06609591924717BA8</identifier><identifier type="ark">ark:/67375/WNG-W3LNHCV6-2</identifier><identifier type="DOI">10.1111/j.1365-2966.2011.19651.x</identifier><identifier type="ArticleID">MNR19651</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2011 The Authors. 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