Deep search for companions to probable young brown dwarfs VLT/NACO adaptive optics imaging using IR wavefront sensing
Identifieur interne : 005182 ( PascalFrancis/Curation ); précédent : 005181; suivant : 005183Deep 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.
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- Pascal (Inist)
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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 Ks, 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 ΔKs = 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, Ks 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.
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Bonnefoy</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Max Planck Institute for Astronomy, Konigstuhl 17</s1><s2>69117 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Dumas, C" sort="Dumas, C" uniqKey="Dumas C" first="C." last="Dumas">C. Dumas</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>European Southern Observatory</s1><s2>Casilla 19001, Santiago</s2><s3>CHL</s3><sZ>10 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author><author><name sortKey="Lowrance, P" sort="Lowrance, P" uniqKey="Lowrance P" first="P." last="Lowrance">P. Lowrance</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><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></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></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">13-0063981</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 13-0063981 INIST</idno><idno type="RBID">Pascal:13-0063981</idno><idno type="wicri:Area/PascalFrancis/Corpus">000C82</idno><idno type="wicri:Area/PascalFrancis/Curation">005182</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Deep search for companions to probable young brown dwarfs VLT/NACO adaptive optics imaging using IR wavefront sensing</title><author><name sortKey="Chauvin, G" sort="Chauvin, G" uniqKey="Chauvin G" first="G." last="Chauvin">G. Chauvin</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></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Max Planck Institute for Astronomy, Konigstuhl 17</s1><s2>69117 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Faherty, J" sort="Faherty, J" uniqKey="Faherty J" first="J." last="Faherty">J. Faherty</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Departmento de Astronomia, Universidad de Chile, Casilla 36-D</s1><s2>Santiago</s2><s3>CHL</s3><sZ>2 aut.</sZ></inist:fA14><country>Chili</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street</s1><s2>New York, NY 10024</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Boccaletti, A" sort="Boccaletti, A" uniqKey="Boccaletti A" first="A." last="Boccaletti">A. Boccaletti</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>3 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Cruz, K" sort="Cruz, K" uniqKey="Cruz K" first="K." last="Cruz">K. Cruz</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street</s1><s2>New York, NY 10024</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Department of Physics & Astronomy, Hunter College, City University of New York, 695 Park Avenue</s1><s2>New York, NY 10065</s2><s3>USA</s3><sZ>4 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Lagrange, A M" sort="Lagrange, A M" uniqKey="Lagrange A" first="A.-M." last="Lagrange">A.-M. Lagrange</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></affiliation></author><author><name sortKey="Zuckerman, B" sort="Zuckerman, B" uniqKey="Zuckerman B" first="B." last="Zuckerman">B. Zuckerman</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Department of Physics & Astronomy and Center for Astrobiology, University of California: Los Angeles, Box 951562</s1><s2>CA 90095</s2><s3>USA</s3><sZ>6 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Bessell, M S" sort="Bessell, M S" uniqKey="Bessell M" first="M. S." last="Bessell">M. S. Bessell</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Research School of Astronomy and Astrophysics Institute of Advance Studies, Australian National University: Cotter Road, Weston Creek</s1><s2>Canberra, ACT 2611</s2><s3>AUS</s3><sZ>7 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Beuzit, J L" sort="Beuzit, J L" uniqKey="Beuzit J" first="J.-L." last="Beuzit">J.-L. Beuzit</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></affiliation></author><author><name sortKey="Bonnefoy, M" sort="Bonnefoy, M" uniqKey="Bonnefoy M" first="M." last="Bonnefoy">M. Bonnefoy</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Max Planck Institute for Astronomy, Konigstuhl 17</s1><s2>69117 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Dumas, C" sort="Dumas, C" uniqKey="Dumas C" first="C." last="Dumas">C. Dumas</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>European Southern Observatory</s1><s2>Casilla 19001, Santiago</s2><s3>CHL</s3><sZ>10 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author><author><name sortKey="Lowrance, P" sort="Lowrance, P" uniqKey="Lowrance P" first="P." last="Lowrance">P. Lowrance</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><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></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></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><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>548</s2></fA05><fA06><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Deep search for companions to probable young brown dwarfs VLT/NACO adaptive optics imaging using IR wavefront sensing</s1></fA08><fA11 i1="01" i2="1"><s1>CHAUVIN (G.)</s1></fA11><fA11 i1="02" i2="1"><s1>FAHERTY (J.)</s1></fA11><fA11 i1="03" i2="1"><s1>BOCCALETTI (A.)</s1></fA11><fA11 i1="04" i2="1"><s1>CRUZ (K.)</s1></fA11><fA11 i1="05" i2="1"><s1>LAGRANGE (A.-M.)</s1></fA11><fA11 i1="06" i2="1"><s1>ZUCKERMAN (B.)</s1></fA11><fA11 i1="07" i2="1"><s1>BESSELL (M. S.)</s1></fA11><fA11 i1="08" i2="1"><s1>BEUZIT (J.-L.)</s1></fA11><fA11 i1="09" i2="1"><s1>BONNEFOY (M.)</s1></fA11><fA11 i1="10" i2="1"><s1>DUMAS (C.)</s1></fA11><fA11 i1="11" i2="1"><s1>LOWRANCE (P.)</s1></fA11><fA11 i1="12" i2="1"><s1>MOUILLET (D.)</s1></fA11><fA11 i1="13" i2="1"><s1>SONG (I.)</s1></fA11><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></fA14><fA14 i1="02"><s1>Max Planck Institute for Astronomy, Konigstuhl 17</s1><s2>69117 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="03"><s1>Departmento de Astronomia, Universidad de Chile, Casilla 36-D</s1><s2>Santiago</s2><s3>CHL</s3><sZ>2 aut.</sZ></fA14><fA14 i1="04"><s1>Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street</s1><s2>New York, NY 10024</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="06"><s1>Department of Physics & Astronomy, Hunter College, City University of New York, 695 Park Avenue</s1><s2>New York, NY 10065</s2><s3>USA</s3><sZ>4 aut.</sZ></fA14><fA14 i1="07"><s1>Department of Physics & Astronomy and Center for Astrobiology, University of California: Los Angeles, Box 951562</s1><s2>CA 90095</s2><s3>USA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="08"><s1>Research School of Astronomy and Astrophysics Institute of Advance Studies, Australian National University: Cotter Road, Weston Creek</s1><s2>Canberra, ACT 2611</s2><s3>AUS</s3><sZ>7 aut.</sZ></fA14><fA14 i1="09"><s1>European Southern Observatory</s1><s2>Casilla 19001, Santiago</s2><s3>CHL</s3><sZ>10 aut.</sZ></fA14><fA14 i1="10"><s1>Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>11 aut.</sZ></fA14><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></fA14><fA20><s2>A33.1-A33.5</s2></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000506265070280</s5></fA43><fA44><s0>0000</s0><s1>© 2013 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>13-0063981</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>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.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Naine brune</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Brown dwarf stars</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Optique adaptative</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Adaptive optics</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Front onde</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Wave front</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Age</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Age</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Edad</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Source ponctuelle</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Point sources</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Photométrie</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Photometry</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Rapport masse</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Mass ratio</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Relación masa</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Propriété physique</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Physical properties</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Système dynamique</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Dynamical systems</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Modèle</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Models</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Modelo</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Binaire serrée</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Close binary stars</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Traitement image</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Image processing</s0><s5>37</s5></fC03><fN21><s1>042</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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|texte= Deep search for companions to probable young brown dwarfs VLT/NACO adaptive optics imaging using IR wavefront sensing
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