The properties of the T8.5p dwarf Ross 458C
Identifieur interne : 006301 ( Main/Exploration ); précédent : 006300; suivant : 006302The 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 ; D. J. Pinfield ; C. G. Tinney [Australie] ; F. Allard [France] ; M. S. Marley [États-Unis] ; H. R. A. Jones ; D. N. Murray ; M. Ishii [États-Unis] ; A. Day-Jones ; J. Gomes ; Z. H. ZhangSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-07-11.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
- Age, Bolometric, Bolometric correction, Brown dwarf stars, 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, Infrared photometry, Infrared spectra, Infrared spectroscopy, Irac, Irac photometry, Johnson apps, Leggett, Low-mass stars, Luminosity, Marley, Metallicity, Methane opacities, Mnras, Model grid, Model sets, Model spectra, Models, Monthly notices, Near infrared spectrum, 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
Affiliations:
- Allemagne, Australie, France, Royaume-Uni, États-Unis
- Basse-Saxe, Californie, Hawaï, Nouveau-Mexique
- Göttingen
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Zhang</name><affiliation><wicri:noCountry code="subField">9AB</wicri:noCountry></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>Age</term><term>Bolometric</term><term>Bolometric correction</term><term>Brown dwarf stars</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>Infrared photometry</term><term>Infrared spectra</term><term>Infrared spectroscopy</term><term>Irac</term><term>Irac photometry</term><term>Johnson apps</term><term>Leggett</term><term>Low-mass stars</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>Models</term><term>Monthly notices</term><term>Near infrared spectrum</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="Pascal" xml:lang="fr"><term>Age</term><term>Etoile faible masse</term><term>Modèle</term><term>Naine brune</term><term>Opacité</term><term>Photométrie IR</term><term>Spectre IR</term><term>Spectre IR proche</term><term>Spectrométrie IR</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><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>France</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Basse-Saxe</li><li>Californie</li><li>Hawaï</li><li>Nouveau-Mexique</li></region><settlement><li>Göttingen</li></settlement></list><tree><noCountry><name sortKey="Day Ones, A" sort="Day Ones, A" uniqKey="Day Ones A" first="A." last="Day-Jones">A. Day-Jones</name><name sortKey="Gomes, J" sort="Gomes, J" uniqKey="Gomes J" first="J." last="Gomes">J. Gomes</name><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><name sortKey="Lucas, P W" sort="Lucas, P W" uniqKey="Lucas P" first="P. W." last="Lucas">P. W. Lucas</name><name sortKey="Murray, D N" sort="Murray, D N" uniqKey="Murray D" first="D. N." last="Murray">D. N. Murray</name><name sortKey="Pinfield, D J" sort="Pinfield, D J" uniqKey="Pinfield D" first="D. J." last="Pinfield">D. J. Pinfield</name><name sortKey="Zhang, Z H" sort="Zhang, Z H" uniqKey="Zhang Z" first="Z. H." last="Zhang">Z. H. Zhang</name></noCountry><country name="Royaume-Uni"><noRegion><name sortKey="Burningham, Ben" sort="Burningham, Ben" uniqKey="Burningham B" first="Ben" last="Burningham">Ben Burningham</name></noRegion></country><country name="États-Unis"><region name="Hawaï"><name sortKey="Leggett, S K" sort="Leggett, S K" uniqKey="Leggett S" first="S. K." last="Leggett">S. K. Leggett</name></region><name sortKey="Homeier, D" sort="Homeier, D" uniqKey="Homeier D" first="D." last="Homeier">D. Homeier</name><name sortKey="Ishii, M" sort="Ishii, M" uniqKey="Ishii M" first="M." last="Ishii">M. Ishii</name><name sortKey="Marley, M S" sort="Marley, M S" uniqKey="Marley M" first="M. S." last="Marley">M. S. Marley</name></country><country name="Allemagne"><region name="Basse-Saxe"><name sortKey="Saumon, D" sort="Saumon, D" uniqKey="Saumon D" first="D." last="Saumon">D. Saumon</name></region></country><country name="Australie"><noRegion><name sortKey="Tinney, C G" sort="Tinney, C G" uniqKey="Tinney C" first="C. G." last="Tinney">C. G. Tinney</name></noRegion></country><country name="France"><noRegion><name sortKey="Allard, F" sort="Allard, F" uniqKey="Allard F" first="F." last="Allard">F. Allard</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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