The properties of the T8.5p dwarf Ross 458C
Identifieur interne : 004438 ( PascalFrancis/Curation ); précédent : 004437; suivant : 004439The properties of the T8.5p dwarf Ross 458C
Auteurs : Ben Burningham [Royaume-Uni] ; S. K. Leggett [États-Unis] ; D. Homeier [États-Unis] ; D. Saumon [Allemagne] ; P. W. Lucas [Royaume-Uni] ; D. J. Pinfield [Royaume-Uni] ; C. G. Tinney [Australie] ; F. Allard [France] ; M. S. Marley [États-Unis] ; H. R. A. Jones [Royaume-Uni] ; D. N. Murray [Royaume-Uni] ; M. Ishii [États-Unis] ; A. Day-Jones [Chili] ; J. Gomes [Royaume-Uni] ; Z. H. Zhang [Royaume-Uni]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.
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- Pascal (Inist)
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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.
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<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">The properties of the T8.5p dwarf Ross 458C</title><author><name sortKey="Burningham, Ben" sort="Burningham, Ben" uniqKey="Burningham B" first="Ben" last="Burningham">Ben Burningham</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Leggett, S K" sort="Leggett, S K" uniqKey="Leggett S" first="S. K." last="Leggett">S. K. Leggett</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Gemini Observatory, 670 N. 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A." last="Jones">H. R. A. Jones</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Ishii, M" sort="Ishii, M" uniqKey="Ishii M" first="M." last="Ishii">M. Ishii</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Subaru Telescope, 650 North A'ohoku Place</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>12 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Day Jones, A" sort="Day Jones, A" uniqKey="Day Jones A" first="A." last="Day-Jones">A. Day-Jones</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Universidad de Chile, Camino el Observatorio # 1515</s1><s2>Santiago, Casilla</s2><s3>CHL</s3><sZ>13 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author><author><name sortKey="Gomes, J" sort="Gomes, J" uniqKey="Gomes J" first="J." last="Gomes">J. Gomes</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0320606</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0320606 INIST</idno><idno type="RBID">Pascal:11-0320606</idno><idno type="wicri:Area/PascalFrancis/Corpus">001B06</idno><idno type="wicri:Area/PascalFrancis/Curation">004438</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">The properties of the T8.5p dwarf Ross 458C</title><author><name sortKey="Burningham, Ben" sort="Burningham, Ben" uniqKey="Burningham B" first="Ben" last="Burningham">Ben Burningham</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Leggett, S K" sort="Leggett, S K" uniqKey="Leggett S" first="S. K." last="Leggett">S. K. Leggett</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Gemini Observatory, 670 N. A'ohoku Place</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>2 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Homeier, D" sort="Homeier, D" uniqKey="Homeier D" first="D." last="Homeier">D. Homeier</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Los Alamos National Laboratory, PO Box 1663, MS F663</s1><s2>Los Alamos, NM 87545</s2><s3>USA</s3><sZ>3 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Saumon, D" sort="Saumon, D" uniqKey="Saumon D" first="D." last="Saumon">D. Saumon</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Institut fur Astrophysik, Georg-August-Universitat, Friedrich-Hund-Platz 1</s1><s2>37077 Gottingen</s2><s3>DEU</s3><sZ>4 aut.</sZ></inist:fA14><country>Allemagne</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="05"><s1>School of Physics, The University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>7 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Allard, F" sort="Allard, F" uniqKey="Allard F" first="F." last="Allard">F. Allard</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>CRAL (UMR 5574 CNRS), Ecole Normale Superieure</s1><s2>69364 Lyon</s2><s3>FRA</s3><sZ>8 aut.</sZ></inist:fA14><country>France</country></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 wicri:level="1"><inist:fA14 i1="07"><s1>NASA Ames Research Center, Mail Stop 245-3</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>9 aut.</sZ></inist:fA14><country>États-Unis</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Ishii, M" sort="Ishii, M" uniqKey="Ishii M" first="M." last="Ishii">M. Ishii</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Subaru Telescope, 650 North A'ohoku Place</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>12 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Day Jones, A" sort="Day Jones, A" uniqKey="Day Jones A" first="A." last="Day-Jones">A. Day-Jones</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Universidad de Chile, Camino el Observatorio # 1515</s1><s2>Santiago, Casilla</s2><s3>CHL</s3><sZ>13 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author><author><name sortKey="Gomes, J" sort="Gomes, J" uniqKey="Gomes J" first="J." last="Gomes">J. Gomes</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Age</term><term>Brown dwarf stars</term><term>Infrared photometry</term><term>Infrared spectra</term><term>Infrared spectroscopy</term><term>Low-mass stars</term><term>Models</term><term>Near infrared spectrum</term><term>Opacity</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Spectrométrie IR</term><term>Photométrie IR</term><term>Age</term><term>Spectre IR proche</term><term>Modèle</term><term>Spectre IR</term><term>Opacité</term><term>Naine brune</term><term>Etoile faible masse</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 T<sub>eff</sub> = 695 ± 60 K, log g = 4.0-4.7 and an inferred mass of 5-20M<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 f<sub>sed</sub> = 2 and we briefly discuss the influence of condensate clouds on T dwarf spectra.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>414</s2></fA05><fA06><s2>4</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The properties of the T8.5p dwarf Ross 458C</s1></fA08><fA11 i1="01" i2="1"><s1>BURNINGHAM (Ben)</s1></fA11><fA11 i1="02" i2="1"><s1>LEGGETT (S. K.)</s1></fA11><fA11 i1="03" i2="1"><s1>HOMEIER (D.)</s1></fA11><fA11 i1="04" i2="1"><s1>SAUMON (D.)</s1></fA11><fA11 i1="05" i2="1"><s1>LUCAS (P. W.)</s1></fA11><fA11 i1="06" i2="1"><s1>PINFIELD (D. J.)</s1></fA11><fA11 i1="07" i2="1"><s1>TINNEY (C. G.)</s1></fA11><fA11 i1="08" i2="1"><s1>ALLARD (F.)</s1></fA11><fA11 i1="09" i2="1"><s1>MARLEY (M. S.)</s1></fA11><fA11 i1="10" i2="1"><s1>JONES (H. R. A.)</s1></fA11><fA11 i1="11" i2="1"><s1>MURRAY (D. N.)</s1></fA11><fA11 i1="12" i2="1"><s1>ISHII (M.)</s1></fA11><fA11 i1="13" i2="1"><s1>DAY-JONES (A.)</s1></fA11><fA11 i1="14" i2="1"><s1>GOMES (J.)</s1></fA11><fA11 i1="15" i2="1"><s1>ZHANG (Z. H.)</s1></fA11><fA14 i1="01"><s1>Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="02"><s1>Gemini Observatory, 670 N. A'ohoku Place</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>2 aut.</sZ></fA14><fA14 i1="03"><s1>Los Alamos National Laboratory, PO Box 1663, MS F663</s1><s2>Los Alamos, NM 87545</s2><s3>USA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>Institut fur Astrophysik, Georg-August-Universitat, Friedrich-Hund-Platz 1</s1><s2>37077 Gottingen</s2><s3>DEU</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>School of Physics, The University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>7 aut.</sZ></fA14><fA14 i1="06"><s1>CRAL (UMR 5574 CNRS), Ecole Normale Superieure</s1><s2>69364 Lyon</s2><s3>FRA</s3><sZ>8 aut.</sZ></fA14><fA14 i1="07"><s1>NASA Ames Research Center, Mail Stop 245-3</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>9 aut.</sZ></fA14><fA14 i1="08"><s1>Subaru Telescope, 650 North A'ohoku Place</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>12 aut.</sZ></fA14><fA14 i1="09"><s1>Universidad de Chile, Camino el Observatorio # 1515</s1><s2>Santiago, Casilla</s2><s3>CHL</s3><sZ>13 aut.</sZ></fA14><fA20><s1>3590-3598</s1></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000190477460630</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0320606</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>USA</s0></fA66><fC01 i1="01" l="ENG"><s0>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 T<sub>eff</sub> = 695 ± 60 K, log g = 4.0-4.7 and an inferred mass of 5-20M<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 f<sub>sed</sub> = 2 and we briefly discuss the influence of condensate clouds on T dwarf spectra.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Spectrométrie IR</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Infrared spectroscopy</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Photométrie IR</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Infrared photometry</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Fotometría IR</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Age</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Age</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Edad</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Spectre IR proche</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Near infrared spectrum</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Espectro IR próximo</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Modèle</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Models</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Modelo</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Spectre IR</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Infrared spectra</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Opacité</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Opacity</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Naine brune</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Brown dwarf stars</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Etoile faible masse</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Low-mass stars</s0><s5>34</s5></fC03><fN21><s1>220</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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|wiki= Wicri/Asie
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|texte= The properties of the T8.5p dwarf Ross 458C
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