AustralieFrV1, Main, Exploration, bibRecord, 005D40

Deep search for companions to probable young brown dwarfs VLT/NACO adaptive optics imaging using IR wavefront sensing

Identifieur interne : 005D40 ( Main/Exploration ); précédent : 005D39; suivant : 005D41

Deep search for companions to probable young brown dwarfs VLT/NACO adaptive optics imaging using IR wavefront sensing

Auteurs : G. Chauvin [France, Allemagne] ; J. Faherty [Chili, États-Unis] ; A. Boccaletti [France] ; K. Cruz [États-Unis] ; A.-M. Lagrange [France] ; B. Zuckerman [États-Unis] ; M. S. Bessell [Australie] ; J.-L. Beuzit [France] ; M. Bonnefoy [Allemagne] ; C. Dumas [Chili] ; P. Lowrance [États-Unis] ; D. Mouillet [France] ; I. Song [États-Unis]

Source :

Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.

RBID : Pascal:13-0063981

Descripteurs français

Pascal (Inist)
- Naine brune, Optique adaptative, Front onde, Age, Source ponctuelle, Photométrie, Rapport masse, Propriété physique, Système dynamique, Modèle, Binaire serrée, Traitement image.

English descriptors

KwdEn :
- Adaptive optics, Age, Brown dwarf stars, Close binary stars, Dynamical systems, Image processing, Mass ratio, Models, Photometry, Physical properties, Point sources, Wave front.

Abstract

Aims. We have obtained high contrast images of four nearby, faint, and very low mass objects 2MASS J04351455-1414468, SDSS J044337.61+000205.1, 2MASSJ06085283-2753583 and 2MASS J06524851-5741376 (hereafter 2MASS0435-14, SDSS0443+00, 2MASS0608-27 and 2MASS0652-57), identified in the field as probable isolated young brown dwarfs. Our goal was to search for binary companions down to the planetary mass regime. Methods. We used the NAOS-CONICA adaptive optics instrument (NACO) and its unique capability to sense the wavefront in the near-infrared to acquire sharp images of the four systems in K_s, with a field of view of 28" x 28". Additional J and L' imaging and follow-up observations at a second epoch were obtained for 2MASS0652-57. Results. With a typical contrast ΔK_s = 4.0-7.0 mag, our observations are sensitive down to the planetary mass regime considering a minimum age of 10 to 120 Myr for these systems. No additional point sources are detected in the environment of 2MASS0435-14, SDSS0443+00 and 2MASS0608-27 between 0.1-12" (i.e. about 2 to 250 AU at 20 pc). 2MASS0652-57 is resolved as a ∼230 mas binary. Follow-up observations reject a background contaminate, resolve the orbital motion of the pair, and confirm with high confidence that the system is physically bound. The J, K_s and L' photometry suggest a q ∼ 0.7-0.8 mass ratio binary with a probable semi-major axis of 5-6 AU. Among the four systems, 2MASS0652-57 is probably the less constrained in terms of age determination. Further analysis would be necessary to confirm its youth. It would then be interesting to determine its orbital and physical properties to derive the system's dynamical mass and to test evolutionary model predictions.

Affiliations:

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Le document en format XML

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<author><name sortKey="Mouillet, D" sort="Mouillet, D" uniqKey="Mouillet D" first="D." last="Mouillet">D. Mouillet</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>UJF-Grenoblel/CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble UMR 5274</s1>
<s2>38041 Grenoble</s2>
<s3>FRA</s3>
<sZ>1 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>12 aut.</sZ>
</inist:fA14>
<country>France</country>
<wicri:noRegion>38041 Grenoble</wicri:noRegion>
<placeName><settlement type="city">Grenoble</settlement>
<region type="region" nuts="2">Auvergne-Rhône-Alpes</region>
<region type="old region" nuts="2">Rhône-Alpes</region>
</placeName>
</affiliation>
</author>
<author><name sortKey="Song, I" sort="Song, I" uniqKey="Song I" first="I." last="Song">I. Song</name>
<affiliation wicri:level="1"><inist:fA14 i1="11"><s1>Department of Physics & Astronomy, University of Georgia</s1>
<s2>Athens, GA 30602-2451</s2>
<s3>USA</s3>
<sZ>13 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
<wicri:noRegion>Athens, GA 30602-2451</wicri:noRegion>
</affiliation>
</author>
</analytic>
<series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title>
<title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title>
<idno type="ISSN">0004-6361</idno>
<imprint><date when="2012">2012</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title>
<title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title>
<idno type="ISSN">0004-6361</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Adaptive optics</term>
<term>Age</term>
<term>Brown dwarf stars</term>
<term>Close binary stars</term>
<term>Dynamical systems</term>
<term>Image processing</term>
<term>Mass ratio</term>
<term>Models</term>
<term>Photometry</term>
<term>Physical properties</term>
<term>Point sources</term>
<term>Wave front</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Naine brune</term>
<term>Optique adaptative</term>
<term>Front onde</term>
<term>Age</term>
<term>Source ponctuelle</term>
<term>Photométrie</term>
<term>Rapport masse</term>
<term>Propriété physique</term>
<term>Système dynamique</term>
<term>Modèle</term>
<term>Binaire serrée</term>
<term>Traitement image</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">Aims. We have obtained high contrast images of four nearby, faint, and very low mass objects 2MASS J04351455-1414468, SDSS J044337.61+000205.1, 2MASSJ06085283-2753583 and 2MASS J06524851-5741376 (hereafter 2MASS0435-14, SDSS0443+00, 2MASS0608-27 and 2MASS0652-57), identified in the field as probable isolated young brown dwarfs. Our goal was to search for binary companions down to the planetary mass regime. Methods. We used the NAOS-CONICA adaptive optics instrument (NACO) and its unique capability to sense the wavefront in the near-infrared to acquire sharp images of the four systems in K<sub>s</sub>
, with a field of view of 28" x 28". Additional J and L' imaging and follow-up observations at a second epoch were obtained for 2MASS0652-57. Results. With a typical contrast ΔK<sub>s</sub>
 = 4.0-7.0 mag, our observations are sensitive down to the planetary mass regime considering a minimum age of 10 to 120 Myr for these systems. No additional point sources are detected in the environment of 2MASS0435-14, SDSS0443+00 and 2MASS0608-27 between 0.1-12" (i.e. about 2 to 250 AU at 20 pc). 2MASS0652-57 is resolved as a ∼230 mas binary. Follow-up observations reject a background contaminate, resolve the orbital motion of the pair, and confirm with high confidence that the system is physically bound. The J, K<sub>s</sub>
 and L' photometry suggest a q ∼ 0.7-0.8 mass ratio binary with a probable semi-major axis of 5-6 AU. Among the four systems, 2MASS0652-57 is probably the less constrained in terms of age determination. Further analysis would be necessary to confirm its youth. It would then be interesting to determine its orbital and physical properties to derive the system's dynamical mass and to test evolutionary model predictions.</div>
</front>
</TEI>
<affiliations><list><country><li>Allemagne</li>
<li>Australie</li>
<li>Chili</li>
<li>France</li>
<li>États-Unis</li>
</country>
<region><li>Auvergne-Rhône-Alpes</li>
<li>Bade-Wurtemberg</li>
<li>District de Karlsruhe</li>
<li>Rhône-Alpes</li>
</region>
<settlement><li>Grenoble</li>
<li>Heidelberg</li>
</settlement>
</list>
<tree><country name="France"><region name="Auvergne-Rhône-Alpes"><name sortKey="Chauvin, G" sort="Chauvin, G" uniqKey="Chauvin G" first="G." last="Chauvin">G. Chauvin</name>
</region>
<name sortKey="Beuzit, J L" sort="Beuzit, J L" uniqKey="Beuzit J" first="J.-L." last="Beuzit">J.-L. Beuzit</name>
<name sortKey="Boccaletti, A" sort="Boccaletti, A" uniqKey="Boccaletti A" first="A." last="Boccaletti">A. Boccaletti</name>
<name sortKey="Lagrange, A M" sort="Lagrange, A M" uniqKey="Lagrange A" first="A.-M." last="Lagrange">A.-M. Lagrange</name>
<name sortKey="Mouillet, D" sort="Mouillet, D" uniqKey="Mouillet D" first="D." last="Mouillet">D. Mouillet</name>
</country>
<country name="Allemagne"><region name="Bade-Wurtemberg"><name sortKey="Chauvin, G" sort="Chauvin, G" uniqKey="Chauvin G" first="G." last="Chauvin">G. Chauvin</name>
</region>
<name sortKey="Bonnefoy, M" sort="Bonnefoy, M" uniqKey="Bonnefoy M" first="M." last="Bonnefoy">M. Bonnefoy</name>
</country>
<country name="Chili"><noRegion><name sortKey="Faherty, J" sort="Faherty, J" uniqKey="Faherty J" first="J." last="Faherty">J. Faherty</name>
</noRegion>
<name sortKey="Dumas, C" sort="Dumas, C" uniqKey="Dumas C" first="C." last="Dumas">C. Dumas</name>
</country>
<country name="États-Unis"><noRegion><name sortKey="Faherty, J" sort="Faherty, J" uniqKey="Faherty J" first="J." last="Faherty">J. Faherty</name>
</noRegion>
<name sortKey="Cruz, K" sort="Cruz, K" uniqKey="Cruz K" first="K." last="Cruz">K. Cruz</name>
<name sortKey="Cruz, K" sort="Cruz, K" uniqKey="Cruz K" first="K." last="Cruz">K. Cruz</name>
<name sortKey="Lowrance, P" sort="Lowrance, P" uniqKey="Lowrance P" first="P." last="Lowrance">P. Lowrance</name>
<name sortKey="Song, I" sort="Song, I" uniqKey="Song I" first="I." last="Song">I. Song</name>
<name sortKey="Zuckerman, B" sort="Zuckerman, B" uniqKey="Zuckerman B" first="B." last="Zuckerman">B. Zuckerman</name>
</country>
<country name="Australie"><noRegion><name sortKey="Bessell, M S" sort="Bessell, M S" uniqKey="Bessell M" first="M. S." last="Bessell">M. S. Bessell</name>
</noRegion>
</country>
</tree>
</affiliations>
</record>

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Deep search for companions to probable young brown dwarfs VLT/NACO adaptive optics imaging using IR wavefront sensing

Deep search for companions to probable young brown dwarfs VLT/NACO adaptive optics imaging using IR wavefront sensing

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