The properties of the T8.5p dwarf Ross 458C
Identifieur interne : 002A98 ( Istex/Corpus ); précédent : 002A97; suivant : 002A99The properties of the T8.5p dwarf Ross 458C
Auteurs : Ben Burningham ; S. K. Leggett ; D. Homeier ; D. Saumon ; P. W. Lucas ; D. J. Pinfield ; C. G. Tinney ; F. Allard ; M. S. Marley ; H. R. A. Jones ; D. N. Murray ; M. Ishii ; A. Day-Jones ; J. Gomes ; Z. H. ZhangSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-07-11.
English descriptors
- KwdEn :
- Bolometric, Bolometric correction, Burgasser, Burningham, Carbon species, Chemical effects, Cloudless models, Condensate, Condensate cloud model, Condensate clouds, Condensate opacity, Dispersion direction, Dust opacity, Dwarf, Dwarf ross, Effective temperature, Emergent spectra, Equal reduction rate, Evolutionary models, Full chemical equilibrium, Goldman, Grid, Irac, Irac photometry, Johnson apps, Leggett, Luminosity, Marley, Metallicity, Methane opacities, Mnras, Model grid, Model sets, Model spectra, Monthly notices, Opacity, Photometry, Ross, Saumon, Saumon marley, Saumon marley model, Saumon marley model grid, Saumon marley model grids, Saumon marley models, Schlaufman laughlin, Settl, Settl bolometric correction, Settl model grid, Settl models, Solar metallicity, Spectral regions, Spectral type, Spectrum, Spie conf, Statistic, Subaru telescope, Systematic effects, Target spectrum, Total luminosity, Ukidss, Upper layers, Various model spectra, Wfcam, Wfcam photometry, Whilst.
- Teeft :
- Bolometric, Bolometric correction, Burgasser, Burningham, Carbon species, Chemical effects, Cloudless models, Condensate, Condensate cloud model, Condensate clouds, Condensate opacity, Dispersion direction, Dust opacity, Dwarf, Dwarf ross, Effective temperature, Emergent spectra, Equal reduction rate, Evolutionary models, Full chemical equilibrium, Goldman, Grid, Irac, Irac photometry, Johnson apps, Leggett, Luminosity, Marley, Metallicity, Methane opacities, Mnras, Model grid, Model sets, Model spectra, Monthly notices, Opacity, Photometry, Ross, Saumon, Saumon marley, Saumon marley model, Saumon marley model grid, Saumon marley model grids, Saumon marley models, Schlaufman laughlin, Settl, Settl bolometric correction, Settl model grid, Settl models, Solar metallicity, Spectral regions, Spectral type, Spectrum, Spie conf, Statistic, Subaru telescope, Systematic effects, Target spectrum, Total luminosity, Ukidss, Upper layers, Various model spectra, Wfcam, Wfcam photometry, Whilst.
Abstract
We present near‐infrared photometry and spectroscopy, and warm‐Spitzer IRAC photometry of the young very cool T dwarf Ross 458C, which we have typed as T8.5p. By applying the fiducial age constraints (≤1 Gyr) imposed by the properties of the active M dwarf Ross 458A, we have used these data to determine that Ross 458C has Teff= 695 ± 60 K, log g= 4.0–4.7 and an inferred mass of 5–20MJ. We have compared fits of the near‐infrared spectrum and IRAC photometry to the BT Settl and Saumon & Marley model grids, and have found that both sets provide best fits that are consistent with our derived properties, whilst the former provide a marginally closer match to the data for all scenarios explored here. The main difference between the model grids arises in the 4.5‐μm region, where the BT Settl models are able to better predict the flux through the IRAC filter, suggesting that non‐equilibrium effects on the CO–CO2 ratio are important for shaping the mid‐infrared spectra of very cool T dwarfs. We have also revisited the issue of the dust opacity in the spectra of Ross 458C that was raised by Burgasser et al. We have found that the BT Settl models which also incorporate a condensate cloud model provide a better match to the near‐infrared spectrum of this target than the Saumon & Marley model with fsed= 2 and we briefly discuss the influence of condensate clouds on T dwarf spectra.
Url:
DOI: 10.1111/j.1365-2966.2011.18664.x
Links to Exploration step
ISTEX:E47AE8FD303E68C63A9AF1ACF24EF3E5C46CECDALe document en format XML
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K." last="Leggett">S. K. Leggett</name><affiliation><mods:affiliation>Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720, USA</mods:affiliation></affiliation></author><author><name sortKey="Homeier, D" sort="Homeier, D" uniqKey="Homeier D" first="D." last="Homeier">D. Homeier</name><affiliation><mods:affiliation>Los Alamos National Laboratory, PO Box 1663, MS F663, Los Alamos, NM 87545, USA</mods:affiliation></affiliation></author><author><name sortKey="Saumon, D" sort="Saumon, D" uniqKey="Saumon D" first="D." last="Saumon">D. Saumon</name><affiliation><mods:affiliation>Institut fur Astrophysik, Georg‐August‐Universitat, Friedrich‐Hund‐Platz 1, 37077 Gottingen, Germany</mods:affiliation></affiliation></author><author><name sortKey="Lucas, P W" sort="Lucas, P W" uniqKey="Lucas P" first="P. W." last="Lucas">P. W. Lucas</name><affiliation><mods:affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</mods:affiliation></affiliation></author><author><name sortKey="Pinfield, D J" sort="Pinfield, D J" uniqKey="Pinfield D" first="D. J." last="Pinfield">D. J. Pinfield</name><affiliation><mods:affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</mods:affiliation></affiliation></author><author><name sortKey="Tinney, C G" sort="Tinney, C G" uniqKey="Tinney C" first="C. G." last="Tinney">C. G. Tinney</name><affiliation><mods:affiliation>School of Physics, The University of New South Wales, Sydney, NSW 2052, Australia</mods:affiliation></affiliation></author><author><name sortKey="Allard, F" sort="Allard, F" uniqKey="Allard F" first="F." last="Allard">F. Allard</name><affiliation><mods:affiliation>CRAL (UMR 5574 CNRS), Ecole Normale Superieure, 69364 Lyon Cedex 07, France</mods:affiliation></affiliation></author><author><name sortKey="Marley, M S" sort="Marley, M S" uniqKey="Marley M" first="M. S." last="Marley">M. S. Marley</name><affiliation><mods:affiliation>NASA Ames Research Center, Mail Stop 245‐3, Moffett Field, CA 94035, USA</mods:affiliation></affiliation></author><author><name sortKey="Jones, H R A" sort="Jones, H R A" uniqKey="Jones H" first="H. R. A." last="Jones">H. R. A. Jones</name><affiliation><mods:affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</mods:affiliation></affiliation></author><author><name sortKey="Murray, D N" sort="Murray, D N" uniqKey="Murray D" first="D. N." last="Murray">D. N. Murray</name><affiliation><mods:affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</mods:affiliation></affiliation></author><author><name sortKey="Ishii, M" sort="Ishii, M" uniqKey="Ishii M" first="M." last="Ishii">M. Ishii</name><affiliation><mods:affiliation>Subaru Telescope, 650 North A'ohoku Place, Hilo, HI 96720, USA</mods:affiliation></affiliation></author><author><name sortKey="Day Ones, A" sort="Day Ones, A" uniqKey="Day Ones A" first="A." last="Day-Jones">A. Day-Jones</name><affiliation><mods:affiliation>Universidad de Chile, Camino el Observatorio # 1515, Santiago, Chile, Casilla 36‐D</mods:affiliation></affiliation></author><author><name sortKey="Gomes, J" sort="Gomes, J" uniqKey="Gomes J" first="J." last="Gomes">J. Gomes</name><affiliation><mods:affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</mods:affiliation></affiliation></author><author><name sortKey="Zhang, Z H" sort="Zhang, Z H" uniqKey="Zhang Z" first="Z. H." last="Zhang">Z. H. Zhang</name><affiliation><mods:affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">414</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="3590">3590</biblScope><biblScope unit="page" to="3598">3598</biblScope><biblScope unit="page-count">9</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-07-11">2011-07-11</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Bolometric</term><term>Bolometric correction</term><term>Burgasser</term><term>Burningham</term><term>Carbon species</term><term>Chemical effects</term><term>Cloudless models</term><term>Condensate</term><term>Condensate cloud model</term><term>Condensate clouds</term><term>Condensate opacity</term><term>Dispersion direction</term><term>Dust opacity</term><term>Dwarf</term><term>Dwarf ross</term><term>Effective temperature</term><term>Emergent spectra</term><term>Equal reduction rate</term><term>Evolutionary models</term><term>Full chemical equilibrium</term><term>Goldman</term><term>Grid</term><term>Irac</term><term>Irac photometry</term><term>Johnson apps</term><term>Leggett</term><term>Luminosity</term><term>Marley</term><term>Metallicity</term><term>Methane opacities</term><term>Mnras</term><term>Model grid</term><term>Model sets</term><term>Model spectra</term><term>Monthly notices</term><term>Opacity</term><term>Photometry</term><term>Ross</term><term>Saumon</term><term>Saumon marley</term><term>Saumon marley model</term><term>Saumon marley model grid</term><term>Saumon marley model grids</term><term>Saumon marley models</term><term>Schlaufman laughlin</term><term>Settl</term><term>Settl bolometric correction</term><term>Settl model grid</term><term>Settl models</term><term>Solar metallicity</term><term>Spectral regions</term><term>Spectral type</term><term>Spectrum</term><term>Spie conf</term><term>Statistic</term><term>Subaru telescope</term><term>Systematic effects</term><term>Target spectrum</term><term>Total luminosity</term><term>Ukidss</term><term>Upper layers</term><term>Various model spectra</term><term>Wfcam</term><term>Wfcam photometry</term><term>Whilst</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Bolometric</term><term>Bolometric correction</term><term>Burgasser</term><term>Burningham</term><term>Carbon species</term><term>Chemical effects</term><term>Cloudless models</term><term>Condensate</term><term>Condensate cloud model</term><term>Condensate clouds</term><term>Condensate opacity</term><term>Dispersion direction</term><term>Dust opacity</term><term>Dwarf</term><term>Dwarf ross</term><term>Effective temperature</term><term>Emergent spectra</term><term>Equal reduction rate</term><term>Evolutionary models</term><term>Full chemical equilibrium</term><term>Goldman</term><term>Grid</term><term>Irac</term><term>Irac photometry</term><term>Johnson apps</term><term>Leggett</term><term>Luminosity</term><term>Marley</term><term>Metallicity</term><term>Methane opacities</term><term>Mnras</term><term>Model grid</term><term>Model sets</term><term>Model spectra</term><term>Monthly notices</term><term>Opacity</term><term>Photometry</term><term>Ross</term><term>Saumon</term><term>Saumon marley</term><term>Saumon marley model</term><term>Saumon marley model grid</term><term>Saumon marley model grids</term><term>Saumon marley models</term><term>Schlaufman laughlin</term><term>Settl</term><term>Settl bolometric correction</term><term>Settl model grid</term><term>Settl models</term><term>Solar metallicity</term><term>Spectral regions</term><term>Spectral type</term><term>Spectrum</term><term>Spie conf</term><term>Statistic</term><term>Subaru telescope</term><term>Systematic effects</term><term>Target spectrum</term><term>Total luminosity</term><term>Ukidss</term><term>Upper layers</term><term>Various model spectra</term><term>Wfcam</term><term>Wfcam photometry</term><term>Whilst</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present near‐infrared photometry and spectroscopy, and warm‐Spitzer IRAC photometry of the young very cool T dwarf Ross 458C, which we have typed as T8.5p. By applying the fiducial age constraints (≤1 Gyr) imposed by the properties of the active M dwarf Ross 458A, we have used these data to determine that Ross 458C has Teff= 695 ± 60 K, log g= 4.0–4.7 and an inferred mass of 5–20MJ. We have compared fits of the near‐infrared spectrum and IRAC photometry to the BT Settl and Saumon & Marley model grids, and have found that both sets provide best fits that are consistent with our derived properties, whilst the former provide a marginally closer match to the data for all scenarios explored here. The main difference between the model grids arises in the 4.5‐μm region, where the BT Settl models are able to better predict the flux through the IRAC filter, suggesting that non‐equilibrium effects on the CO–CO2 ratio are important for shaping the mid‐infrared spectra of very cool T dwarfs. We have also revisited the issue of the dust opacity in the spectra of Ross 458C that was raised by Burgasser et al. We have found that the BT Settl models which also incorporate a condensate cloud model provide a better match to the near‐infrared spectrum of this target than the Saumon & Marley model with fsed= 2 and we briefly discuss the influence of condensate clouds on T dwarf spectra.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>settl</json:string><json:string>saumon</json:string><json:string>marley</json:string><json:string>photometry</json:string><json:string>mnras</json:string><json:string>burningham</json:string><json:string>wfcam</json:string><json:string>settl models</json:string><json:string>metallicity</json:string><json:string>burgasser</json:string><json:string>model spectra</json:string><json:string>grid</json:string><json:string>opacity</json:string><json:string>saumon marley models</json:string><json:string>condensate</json:string><json:string>bolometric</json:string><json:string>ukidss</json:string><json:string>monthly notices</json:string><json:string>irac</json:string><json:string>goldman</json:string><json:string>spectral type</json:string><json:string>whilst</json:string><json:string>statistic</json:string><json:string>irac photometry</json:string><json:string>model sets</json:string><json:string>evolutionary models</json:string><json:string>settl model grid</json:string><json:string>leggett</json:string><json:string>luminosity</json:string><json:string>saumon marley</json:string><json:string>condensate clouds</json:string><json:string>dwarf ross</json:string><json:string>solar metallicity</json:string><json:string>target spectrum</json:string><json:string>systematic effects</json:string><json:string>saumon marley model</json:string><json:string>condensate opacity</json:string><json:string>bolometric correction</json:string><json:string>effective temperature</json:string><json:string>spie conf</json:string><json:string>dwarf</json:string><json:string>ross</json:string><json:string>spectrum</json:string><json:string>johnson apps</json:string><json:string>cloudless models</json:string><json:string>wfcam photometry</json:string><json:string>total luminosity</json:string><json:string>spectral regions</json:string><json:string>model grid</json:string><json:string>settl bolometric correction</json:string><json:string>emergent spectra</json:string><json:string>condensate cloud model</json:string><json:string>schlaufman laughlin</json:string><json:string>saumon marley model grids</json:string><json:string>methane opacities</json:string><json:string>chemical effects</json:string><json:string>carbon species</json:string><json:string>full chemical equilibrium</json:string><json:string>equal reduction rate</json:string><json:string>dispersion direction</json:string><json:string>subaru telescope</json:string><json:string>various model spectra</json:string><json:string>saumon marley model grid</json:string><json:string>upper layers</json:string><json:string>dust opacity</json:string></teeft></keywords><author><json:item><name>Ben Burningham</name><affiliations><json:string>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</json:string><json:string>E-mail: B.Burningham@herts.ac.uk</json:string></affiliations></json:item><json:item><name>S. K. Leggett</name><affiliations><json:string>Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720, USA</json:string></affiliations></json:item><json:item><name>D. Homeier</name><affiliations><json:string>Los Alamos National Laboratory, PO Box 1663, MS F663, Los Alamos, NM 87545, USA</json:string></affiliations></json:item><json:item><name>D. Saumon</name><affiliations><json:string>Institut fur Astrophysik, Georg‐August‐Universitat, Friedrich‐Hund‐Platz 1, 37077 Gottingen, Germany</json:string></affiliations></json:item><json:item><name>P. W. Lucas</name><affiliations><json:string>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</json:string></affiliations></json:item><json:item><name>D. J. Pinfield</name><affiliations><json:string>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</json:string></affiliations></json:item><json:item><name>C. G. Tinney</name><affiliations><json:string>School of Physics, The University of New South Wales, Sydney, NSW 2052, Australia</json:string></affiliations></json:item><json:item><name>F. Allard</name><affiliations><json:string>CRAL (UMR 5574 CNRS), Ecole Normale Superieure, 69364 Lyon Cedex 07, France</json:string></affiliations></json:item><json:item><name>M. S. Marley</name><affiliations><json:string>NASA Ames Research Center, Mail Stop 245‐3, Moffett Field, CA 94035, USA</json:string></affiliations></json:item><json:item><name>H. R. A. Jones</name><affiliations><json:string>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</json:string></affiliations></json:item><json:item><name>D. N. Murray</name><affiliations><json:string>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</json:string></affiliations></json:item><json:item><name>M. Ishii</name><affiliations><json:string>Subaru Telescope, 650 North A'ohoku Place, Hilo, HI 96720, USA</json:string></affiliations></json:item><json:item><name>A. Day‐Jones</name><affiliations><json:string>Universidad de Chile, Camino el Observatorio # 1515, Santiago, Chile, Casilla 36‐D</json:string></affiliations></json:item><json:item><name>J. Gomes</name><affiliations><json:string>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</json:string></affiliations></json:item><json:item><name>Z. H. Zhang</name><affiliations><json:string>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</json:string></affiliations></json:item></author><subject><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></subject><articleId><json:string>MNR18664</json:string></articleId><arkIstex>ark:/67375/WNG-FG10GQL0-S</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We present near‐infrared photometry and spectroscopy, and warm‐Spitzer IRAC photometry of the young very cool T dwarf Ross 458C, which we have typed as T8.5p. By applying the fiducial age constraints (≤1 Gyr) imposed by the properties of the active M dwarf Ross 458A, we have used these data to determine that Ross 458C has Teff= 695 ± 60 K, log g= 4.0–4.7 and an inferred mass of 5–20MJ. We have compared fits of the near‐infrared spectrum and IRAC photometry to the BT Settl and Saumon & Marley model grids, and have found that both sets provide best fits that are consistent with our derived properties, whilst the former provide a marginally closer match to the data for all scenarios explored here. The main difference between the model grids arises in the 4.5‐μm region, where the BT Settl models are able to better predict the flux through the IRAC filter, suggesting that non‐equilibrium effects on the CO–CO2 ratio are important for shaping the mid‐infrared spectra of very cool T dwarfs. We have also revisited the issue of the dust opacity in the spectra of Ross 458C that was raised by Burgasser et al. We have found that the BT Settl models which also incorporate a condensate cloud model provide a better match to the near‐infrared spectrum of this target than the Saumon & Marley model with fsed= 2 and we briefly discuss the influence of condensate clouds on T dwarf spectra.</abstract><qualityIndicators><score>9.856</score><pdfWordCount>6952</pdfWordCount><pdfCharCount>36062</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>9</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>238</abstractWordCount><abstractCharCount>1391</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>The properties of the T8.5p dwarf Ross 458C</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>414</volume><issue>4</issue><pages><first>3590</first><last>3598</last><total>9</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2009</json:string><json:string>2011</json:string></date><geogName></geogName><orgName><json:string>Chile, Casilla</json:string><json:string>University of New South Wales</json:string><json:string>University of Hertfordshire</json:string><json:string>Chile, Camino</json:string><json:string>Argentina, Australia, Brazil, Canada, Chile, the United Kingdom</json:string><json:string>Los Alamos National Laboratory, PO Box</json:string><json:string>Ames Research Center, Mail Stop</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>B.Burningham</json:string><json:string>Sky Survey</json:string><json:string>F. Allard</json:string><json:string>D. N. Murray</json:string><json:string>G. Tinney</json:string><json:string>D. Saumon</json:string><json:string>S. K. Leggett</json:string><json:string>D. J. Pin</json:string><json:string>In</json:string><json:string>P. W. Lucas</json:string><json:string>Of</json:string><json:string>S. Marley</json:string><json:string>D. Homeier</json:string><json:string>Ben Burningham</json:string><json:string>By</json:string><json:string>A. Day-Jones</json:string><json:string>H. R. A. Jones</json:string><json:string>Z. H. Zhang</json:string><json:string>Adam Burgasser</json:string></persName><placeName><json:string>United States of America</json:string><json:string>Germany</json:string><json:string>Australia</json:string><json:string>Hilo</json:string><json:string>Strasbourg</json:string><json:string>HI</json:string><json:string>Ireland</json:string><json:string>France</json:string><json:string>Cambridge</json:string><json:string>Lyon</json:string></placeName><ref_url><json:string>http://www.browndwarfs.org/spexprism</json:string><json:string>http://ssc.spitzer.caltech.edu/irac/dh/</json:string></ref_url><ref_bibl><json:string>Zhang et al. 2010</json:string><json:string>Burgasser et al. (2010)</json:string><json:string>Leggett et al. 2010</json:string><json:string>Saumon & Marley 2008</json:string><json:string>Allard et al.</json:string><json:string>Cushing et al. (2008)</json:string><json:string>Casali et al. 2007</json:string><json:string>Jordi (2008)</json:string><json:string>Murray et al. 2011</json:string><json:string>Tokunaga, Simons & Vacca 2002</json:string><json:string>Burningham et al. 2010b</json:string><json:string>Leggett et al. (2010)</json:string><json:string>Burgasser et al. 2006</json:string><json:string>Burningham et al 2010</json:string><json:string>Cushing et al. 2008</json:string><json:string>Lodieu et al. 2007</json:string><json:string>Burningham et al. (2010b)</json:string><json:string>Littlefair et al. 2007</json:string><json:string>Allard, Homeier & Freytag 2010</json:string><json:string>Burgasser et al.</json:string><json:string>Hodapp et al. 2003</json:string><json:string>Day-Jones et al. 2008</json:string><json:string>Scholz et al. 2003</json:string><json:string>Saumon et al. (2006, 2007)</json:string><json:string>King et al. 2010</json:string><json:string>Burgasser et al. (2006)</json:string><json:string>Kobayashi et al. 2000</json:string><json:string>Burningham et al. 2008, 2009, 2010a</json:string><json:string>Irwin et al. 2004</json:string><json:string>Burningham et al. 2009</json:string><json:string>Goldman et al. 2010</json:string><json:string>McLean et al. 2006</json:string><json:string>B. Burningham et al.</json:string><json:string>Burningham et al. (2008)</json:string><json:string>Marley (2008)</json:string><json:string>West et al. (2008)</json:string><json:string>West et al. 2008</json:string><json:string>Burningham et al. 2008</json:string><json:string>Becklin 2005</json:string><json:string>Borysow et al. (2003)</json:string><json:string>Nidever et al. (2002)</json:string><json:string>Baraffe et al. 2003</json:string><json:string>Goldman et al. (2010)</json:string><json:string>Stassun, Mathieu & Valenti 2006</json:string><json:string>Burningham et al. (2009)</json:string><json:string>Hambly et al. 2008</json:string><json:string>Day-Jones et al. 2011</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-FG10GQL0-S</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences exactes et technologie</json:string><json:string>3 - terre, ocean, espace</json:string><json:string>4 - geophysique externe</json:string></inist></categories><publicationDate>2011</publicationDate><copyrightDate>2011</copyrightDate><doi><json:string>10.1111/j.1365-2966.2011.18664.x</json:string></doi><id>E47AE8FD303E68C63A9AF1ACF24EF3E5C46CECDA</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/E47AE8FD303E68C63A9AF1ACF24EF3E5C46CECDA/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/E47AE8FD303E68C63A9AF1ACF24EF3E5C46CECDA/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/E47AE8FD303E68C63A9AF1ACF24EF3E5C46CECDA/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">The properties of the T8.5p dwarf Ross 458C</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="2011-07-11"></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">The properties of the T8.5p dwarf Ross 458C</title><title level="a" type="short">Ross 458C</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">Ben</forename><surname>Burningham</surname></persName><affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</affiliation><affiliation>E‐mail: B.Burningham@herts.ac.uk</affiliation></author><author xml:id="author-0001"><persName><forename type="first">S. K.</forename><surname>Leggett</surname></persName><affiliation>Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">D.</forename><surname>Homeier</surname></persName><affiliation>Los Alamos National Laboratory, PO Box 1663, MS F663, Los Alamos, NM 87545, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">D.</forename><surname>Saumon</surname></persName><affiliation>Institut fur Astrophysik, Georg‐August‐Universitat, Friedrich‐Hund‐Platz 1, 37077 Gottingen, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">P. 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By applying the fiducial age constraints (≤1 Gyr) imposed by the properties of the active M dwarf Ross 458A, we have used these data to determine that Ross 458C has <emph><span><hi rend="italic">T</hi><hi rend="subscript">eff</hi>= 695 ± 60</span></emph> K, <emph><span>log <hi rend="italic">g</hi>= 4.0–4.7</span></emph> and an inferred mass of 5–20<hi rend="italic">M</hi><hi rend="subscript">J</hi>. We have compared fits of the near‐infrared spectrum and IRAC photometry to the BT Settl and Saumon & Marley model grids, and have found that both sets provide best fits that are consistent with our derived properties, whilst the former provide a marginally closer match to the data for all scenarios explored here. The main difference between the model grids arises in the 4.5‐μm region, where the BT Settl models are able to better predict the flux through the IRAC filter, suggesting that non‐equilibrium effects on the CO–CO<hi rend="subscript">2</hi> ratio are important for shaping the mid‐infrared spectra of very cool T dwarfs. We have also revisited the issue of the dust opacity in the spectra of Ross 458C that was raised by Burgasser et al. We have found that the BT Settl models which also incorporate a condensate cloud model provide a better match to the near‐infrared spectrum of this target than the Saumon & Marley model with <emph><span><hi rend="italic">f</hi><hi rend="subscript">sed</hi>= 2</span></emph> and we briefly discuss the influence of condensate clouds on T dwarf spectra.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">surveys</term><term xml:id="k2">brown dwarfs</term><term xml:id="k3">stars: low‐mass</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/E47AE8FD303E68C63A9AF1ACF24EF3E5C46CECDA/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="07104"><doi origin="wiley">10.1111/mnr.2011.414.issue-4</doi><numberingGroup><numbering type="journalVolume" number="414">414</numbering><numbering type="journalIssue" number="4">4</numbering></numberingGroup><coverDate startDate="2011-07-11">July 2011</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="63" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2011.18664.x</doi><idGroup><id type="unit" value="MNR18664"></id></idGroup><countGroup><count type="pageTotal" number="9"></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:3.1.6 mode:FullText" date="2012-08-22"></event><event type="publishedOnlineEarlyUnpaginated" date="2011-05-04"></event><event type="publishedOnlineFinalForm" date="2011-07-01"></event><event type="firstOnline" date="2011-05-04"></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="3590">3590</numbering><numbering type="pageLast" number="3598">3598</numbering></numberingGroup><correspondenceTo>
E‐mail: <email>B.Burningham@herts.ac.uk</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR18664.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2011 March 6. Received 2011 February 21; in original form 2010 November 26</unparsedEditorialHistory><countGroup><count type="figureTotal" number="7"></count><count type="tableTotal" number="3"></count><count type="formulaTotal" number="138"></count><count type="referenceTotal" number="48"></count><count type="linksCrossRef" number="124"></count></countGroup><titleGroup><title type="main">The properties of the T8.5p dwarf Ross 458C</title><title type="shortAuthors"><i>B. Burningham et al.</i></title><title type="short"><i>Ross 458C</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Ben</givenNames><familyName>Burningham</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2"><personName><givenNames>S. K.</givenNames><familyName>Leggett</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a3"><personName><givenNames>D.</givenNames><familyName>Homeier</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a4"><personName><givenNames>D.</givenNames><familyName>Saumon</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a1"><personName><givenNames>P. 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A'ohoku Place, Hilo, HI 96720, USA</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="US"><unparsedAffiliation>Los Alamos National Laboratory, PO Box 1663, MS F663, Los Alamos, NM 87545, USA</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="DE"><unparsedAffiliation>Institut fur Astrophysik, Georg‐August‐Universitat, Friedrich‐Hund‐Platz 1, 37077 Gottingen, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="AU"><unparsedAffiliation>School of Physics, The University of New South Wales, Sydney, NSW 2052, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="FR"><unparsedAffiliation>CRAL (UMR 5574 CNRS), Ecole Normale Superieure, 69364 Lyon Cedex 07, France</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="US"><unparsedAffiliation>NASA Ames Research Center, Mail Stop 245‐3, Moffett Field, CA 94035, USA</unparsedAffiliation></affiliation><affiliation xml:id="a8" countryCode="US"><unparsedAffiliation>Subaru Telescope, 650 North A'ohoku Place, Hilo, HI 96720, USA</unparsedAffiliation></affiliation><affiliation xml:id="a9" countryCode="CL"><unparsedAffiliation>Universidad de Chile, Camino el Observatorio # 1515, Santiago, Chile, Casilla 36‐D</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">surveys</keyword><keyword xml:id="k2">brown dwarfs</keyword><keyword xml:id="k3">stars: low‐mass</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>We present near‐infrared photometry and spectroscopy, and warm‐<i>Spitzer</i> IRAC photometry of the young very cool T dwarf Ross 458C, which we have typed as T8.5p. By applying the fiducial age constraints (≤1 Gyr) imposed by the properties of the active M dwarf Ross 458A, we have used these data to determine that Ross 458C has <span type="mathematics"><i>T</i><sub>eff</sub>= 695 ± 60</span> K, <span type="mathematics">log <i>g</i>= 4.0–4.7</span> and an inferred mass of 5–20<i>M</i><sub>J</sub>. We have compared fits of the near‐infrared spectrum and IRAC photometry to the BT Settl and Saumon & Marley model grids, and have found that both sets provide best fits that are consistent with our derived properties, whilst the former provide a marginally closer match to the data for all scenarios explored here. The main difference between the model grids arises in the 4.5‐μm region, where the BT Settl models are able to better predict the flux through the IRAC filter, suggesting that non‐equilibrium effects on the CO–CO<sub>2</sub> ratio are important for shaping the mid‐infrared spectra of very cool T dwarfs. We have also revisited the issue of the dust opacity in the spectra of Ross 458C that was raised by Burgasser et al. We have found that the BT Settl models which also incorporate a condensate cloud model provide a better match to the near‐infrared spectrum of this target than the Saumon & Marley model with <span type="mathematics"><i>f</i><sub>sed</sub>= 2</span> and we briefly discuss the influence of condensate clouds on T dwarf spectra.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>The properties of the T8.5p dwarf Ross 458C</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Ross 458C</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>The properties of the T8.5p dwarf Ross 458C</title></titleInfo><name type="personal"><namePart type="given">Ben</namePart><namePart type="family">Burningham</namePart><affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</affiliation><affiliation>E-mail: B.Burningham@herts.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. K.</namePart><namePart type="family">Leggett</namePart><affiliation>Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Homeier</namePart><affiliation>Los Alamos National Laboratory, PO Box 1663, MS F663, Los Alamos, NM 87545, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Saumon</namePart><affiliation>Institut fur Astrophysik, Georg‐August‐Universitat, Friedrich‐Hund‐Platz 1, 37077 Gottingen, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P. W.</namePart><namePart type="family">Lucas</namePart><affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D. J.</namePart><namePart type="family">Pinfield</namePart><affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C. G.</namePart><namePart type="family">Tinney</namePart><affiliation>School of Physics, The University of New South Wales, Sydney, NSW 2052, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">F.</namePart><namePart type="family">Allard</namePart><affiliation>CRAL (UMR 5574 CNRS), Ecole Normale Superieure, 69364 Lyon Cedex 07, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M. S.</namePart><namePart type="family">Marley</namePart><affiliation>NASA Ames Research Center, Mail Stop 245‐3, Moffett Field, CA 94035, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">H. R. A.</namePart><namePart type="family">Jones</namePart><affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D. N.</namePart><namePart type="family">Murray</namePart><affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Ishii</namePart><affiliation>Subaru Telescope, 650 North A'ohoku Place, Hilo, HI 96720, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Day‐Jones</namePart><affiliation>Universidad de Chile, Camino el Observatorio # 1515, Santiago, Chile, Casilla 36‐D</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Gomes</namePart><affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Z. H.</namePart><namePart type="family">Zhang</namePart><affiliation>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB</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">2011-07-11</dateIssued><edition>Accepted 2011 March 6. Received 2011 February 21; in original form 2010 November 26</edition><copyrightDate encoding="w3cdtf">2011</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">7</extent><extent unit="tables">3</extent><extent unit="formulas">138</extent><extent unit="references">48</extent><extent unit="linksCrossRef">124</extent></physicalDescription><abstract lang="en">We present near‐infrared photometry and spectroscopy, and warm‐Spitzer IRAC photometry of the young very cool T dwarf Ross 458C, which we have typed as T8.5p. By applying the fiducial age constraints (≤1 Gyr) imposed by the properties of the active M dwarf Ross 458A, we have used these data to determine that Ross 458C has Teff= 695 ± 60 K, log g= 4.0–4.7 and an inferred mass of 5–20MJ. We have compared fits of the near‐infrared spectrum and IRAC photometry to the BT Settl and Saumon & Marley model grids, and have found that both sets provide best fits that are consistent with our derived properties, whilst the former provide a marginally closer match to the data for all scenarios explored here. The main difference between the model grids arises in the 4.5‐μm region, where the BT Settl models are able to better predict the flux through the IRAC filter, suggesting that non‐equilibrium effects on the CO–CO2 ratio are important for shaping the mid‐infrared spectra of very cool T dwarfs. We have also revisited the issue of the dust opacity in the spectra of Ross 458C that was raised by Burgasser et al. We have found that the BT Settl models which also incorporate a condensate cloud model provide a better match to the near‐infrared spectrum of this target than the Saumon & Marley model with fsed= 2 and we briefly discuss the influence of condensate clouds on T dwarf spectra.</abstract><subject lang="en"><genre>keywords</genre><topic>surveys</topic><topic>brown dwarfs</topic><topic>stars: low‐mass</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>414</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>3590</start><end>3598</end><total>9</total></extent></part></relatedItem><identifier type="istex">E47AE8FD303E68C63A9AF1ACF24EF3E5C46CECDA</identifier><identifier type="ark">ark:/67375/WNG-FG10GQL0-S</identifier><identifier type="DOI">10.1111/j.1365-2966.2011.18664.x</identifier><identifier type="ArticleID">MNR18664</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/E47AE8FD303E68C63A9AF1ACF24EF3E5C46CECDA/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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