Mid-infrared interferometry of the massive young stellar object NGC 3603 - IRS 9A
Identifieur interne : 007735 ( Main/Exploration ); précédent : 007734; suivant : 007736Mid-infrared interferometry of the massive young stellar object NGC 3603 - IRS 9A
Auteurs : S. Vehoff [Allemagne, Chili] ; C. A. Hummel [Allemagne] ; J. D. Monnier [États-Unis] ; P. Tuthill [Australie] ; D. E. A. Nürnberger [Chili] ; R. Siebenmorgen [Allemagne] ; O. Chesneau [France] ; W. J. Duschl [Allemagne, États-Unis]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2010.
Descripteurs français
- Pascal (Inist)
- Interférométrie IR, Objet stellaire jeune, Modèle géométrique, Etoile O, Etoile B, Observation interférométrique, Densité spectrale énergie, Distribution brillance, Transfert radiatif, Largeur équivalente, Multiplicité, Diamètre, Visibilité, Modèle sphérique, Matière circumstellaire, Etoile premier type, Formation stellaire.
English descriptors
- KwdEn :
- B stars, Brightness distribution, Circumstellar matter, Diameter, Early type stars, Equivalent width, Geometrical model, Infrared interferometry, Interferometric observation, Multiplicity, O stars, Radiative transfer, Spectral energy distribution, Spherical model, Star formation, Visibility, Young stellar object.
Abstract
Context. Very few massive young stellar objects (MYSO) have been studied in the infrared at high angular resolution due to their rarity and large associated extinction. We present observations and models for one of these MYSO candidates, NGC 3603 IRS 9A. Aims. Our goal is to investigate with infrared interferometry the structure of IRS 9A on scales as small as 200 AU, exploiting the fact that a cluster of O and B stars has blown away much of the obscuring foreground dust and gas. Methods. Observations in the N-band were carried out with the MIDI beam combiner attached to the VLTI, providing spatial information on scales of about 25-95 milli-arcsec (mas). Additional interferometric observations which probe the structure of IRS 9A on larger scales were performed with an aperture mask installed in the T-ReCS instrument of Gemini South. The spectral energy distribution (SED) is constrained by the MIDI N-band spectrum and by data from the Spitzer Space Telescope. Our efforts to model the structure and SED of IRS 9A range from simple geometrical models of the brightness distribution to one- and two-dimensional radiative transfer computations. Results. The target is resolved by T-ReCS, with an equivalent (elliptical) Gaussian width of 330 mas by 280 mas (2300 AU by 2000 AU). Despite this fact, a warm compact unresolved component was detected by MIDI which is possibly associated with the inner regions of a flattened dust distribution. Based on our interferometric data, no sign of multiplicity was found on scales between about 200 AU and 700 AU projected separation. A geometric model consisting of a warm (1000 K) ring (400 AU diameter) and a cool (140 K) large envelope provides a good fit to the data. No single model fitting all visibility and photometric data could be found, with disk models performing better than spherical models. Conclusions. While the data are clearly inconsistent with a spherical dust distribution they are insufficient to prove the existence of a disk but rather hint at a more complex dust distribution.
Affiliations:
- Allemagne, Australie, Chili, France, États-Unis
- Bade-Wurtemberg, District de Karlsruhe, Nouvelle-Galles du Sud, Schleswig-Holstein
- Heidelberg, Kiel, Sydney
- Université de Sydney
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Vehoff</name><affiliation wicri:level="3"><inist:fA14 i1="01"><s1>Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ></inist:fA14><country>Allemagne</country><placeName><region type="land" nuts="1">Bade-Wurtemberg</region><region type="district" nuts="2">District de Karlsruhe</region><settlement type="city">Heidelberg</settlement></placeName></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001</s1><s2>Santiago</s2><s3>CHL</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Chili</country><wicri:noRegion>Santiago</wicri:noRegion></affiliation></author><author><name sortKey="Hummel, C A" sort="Hummel, C A" uniqKey="Hummel C" first="C. A." last="Hummel">C. A. Hummel</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>European Organization for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>2 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching bei München</wicri:noRegion><wicri:noRegion>Karl-Schwarzschild-Str. 2</wicri:noRegion><wicri:noRegion>85748 Garching bei München</wicri:noRegion></affiliation></author><author><name sortKey="Monnier, J D" sort="Monnier, J D" uniqKey="Monnier J" first="J. D." last="Monnier">J. D. Monnier</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Department of Astronomy, University of Michigan</s1><s2>Ann Arbor, MI 48109</s2><s3>USA</s3><sZ>3 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Ann Arbor, MI 48109</wicri:noRegion></affiliation></author><author><name sortKey="Tuthill, P" sort="Tuthill, P" uniqKey="Tuthill P" first="P." last="Tuthill">P. Tuthill</name><affiliation wicri:level="4"><inist:fA14 i1="05"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ></inist:fA14><country>Australie</country><placeName><settlement type="city">Sydney</settlement><region type="état">Nouvelle-Galles du Sud</region></placeName><orgName type="university">Université de Sydney</orgName></affiliation></author><author><name sortKey="Nurnberger, D E A" sort="Nurnberger, D E A" uniqKey="Nurnberger D" first="D. E. A." last="Nürnberger">D. E. A. Nürnberger</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001</s1><s2>Santiago</s2><s3>CHL</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Chili</country><wicri:noRegion>Santiago</wicri:noRegion></affiliation></author><author><name sortKey="Siebenmorgen, R" sort="Siebenmorgen, R" uniqKey="Siebenmorgen R" first="R." last="Siebenmorgen">R. Siebenmorgen</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>European Organization for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>2 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching bei München</wicri:noRegion><wicri:noRegion>Karl-Schwarzschild-Str. 2</wicri:noRegion><wicri:noRegion>85748 Garching bei München</wicri:noRegion></affiliation></author><author><name sortKey="Chesneau, O" sort="Chesneau, O" uniqKey="Chesneau O" first="O." last="Chesneau">O. Chesneau</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Observatoire de la Côte d'Azur, Dpt. Gemini-CNRS-UMR 6203, Avenue Copernic</s1><s2>06130 Grasse</s2><s3>FRA</s3><sZ>7 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>06130 Grasse</wicri:noRegion><wicri:noRegion>Avenue Copernic</wicri:noRegion><wicri:noRegion>06130 Grasse</wicri:noRegion></affiliation></author><author><name sortKey="Duschl, W J" sort="Duschl, W J" uniqKey="Duschl W" first="W. J." last="Duschl">W. J. Duschl</name><affiliation wicri:level="3"><inist:fA14 i1="07"><s1>Institut für Theoretische Physik und Astrophysik der Christian-Albrechts-Universität zu Kiel, Leibnizstr. 15</s1><s2>24118 Kiel</s2><s3>DEU</s3><sZ>8 aut.</sZ></inist:fA14><country>Allemagne</country><placeName><region type="land" nuts="2">Schleswig-Holstein</region><settlement type="city">Kiel</settlement></placeName></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Steward Observatory, The University of Arizona, 933 N. Cherry Ave.</s1><s2>Tucson, AZ 85721</s2><s3>USA</s3><sZ>8 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Tucson, AZ 85721</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="2010">2010</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>B stars</term><term>Brightness distribution</term><term>Circumstellar matter</term><term>Diameter</term><term>Early type stars</term><term>Equivalent width</term><term>Geometrical model</term><term>Infrared interferometry</term><term>Interferometric observation</term><term>Multiplicity</term><term>O stars</term><term>Radiative transfer</term><term>Spectral energy distribution</term><term>Spherical model</term><term>Star formation</term><term>Visibility</term><term>Young stellar object</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Interférométrie IR</term><term>Objet stellaire jeune</term><term>Modèle géométrique</term><term>Etoile O</term><term>Etoile B</term><term>Observation interférométrique</term><term>Densité spectrale énergie</term><term>Distribution brillance</term><term>Transfert radiatif</term><term>Largeur équivalente</term><term>Multiplicité</term><term>Diamètre</term><term>Visibilité</term><term>Modèle sphérique</term><term>Matière circumstellaire</term><term>Etoile premier type</term><term>Formation stellaire</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Context. Very few massive young stellar objects (MYSO) have been studied in the infrared at high angular resolution due to their rarity and large associated extinction. We present observations and models for one of these MYSO candidates, NGC 3603 IRS 9A. Aims. Our goal is to investigate with infrared interferometry the structure of IRS 9A on scales as small as 200 AU, exploiting the fact that a cluster of O and B stars has blown away much of the obscuring foreground dust and gas. Methods. Observations in the N-band were carried out with the MIDI beam combiner attached to the VLTI, providing spatial information on scales of about 25-95 milli-arcsec (mas). Additional interferometric observations which probe the structure of IRS 9A on larger scales were performed with an aperture mask installed in the T-ReCS instrument of Gemini South. The spectral energy distribution (SED) is constrained by the MIDI N-band spectrum and by data from the Spitzer Space Telescope. Our efforts to model the structure and SED of IRS 9A range from simple geometrical models of the brightness distribution to one- and two-dimensional radiative transfer computations. Results. The target is resolved by T-ReCS, with an equivalent (elliptical) Gaussian width of 330 mas by 280 mas (2300 AU by 2000 AU). Despite this fact, a warm compact unresolved component was detected by MIDI which is possibly associated with the inner regions of a flattened dust distribution. Based on our interferometric data, no sign of multiplicity was found on scales between about 200 AU and 700 AU projected separation. A geometric model consisting of a warm (1000 K) ring (400 AU diameter) and a cool (140 K) large envelope provides a good fit to the data. No single model fitting all visibility and photometric data could be found, with disk models performing better than spherical models. Conclusions. While the data are clearly inconsistent with a spherical dust distribution they are insufficient to prove the existence of a disk but rather hint at a more complex dust distribution.</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>Bade-Wurtemberg</li><li>District de Karlsruhe</li><li>Nouvelle-Galles du Sud</li><li>Schleswig-Holstein</li></region><settlement><li>Heidelberg</li><li>Kiel</li><li>Sydney</li></settlement><orgName><li>Université de Sydney</li></orgName></list><tree><country name="Allemagne"><region name="Bade-Wurtemberg"><name sortKey="Vehoff, S" sort="Vehoff, S" uniqKey="Vehoff S" first="S." last="Vehoff">S. Vehoff</name></region><name sortKey="Duschl, W J" sort="Duschl, W J" uniqKey="Duschl W" first="W. J." last="Duschl">W. J. Duschl</name><name sortKey="Hummel, C A" sort="Hummel, C A" uniqKey="Hummel C" first="C. A." last="Hummel">C. A. Hummel</name><name sortKey="Siebenmorgen, R" sort="Siebenmorgen, R" uniqKey="Siebenmorgen R" first="R." last="Siebenmorgen">R. Siebenmorgen</name></country><country name="Chili"><noRegion><name sortKey="Vehoff, S" sort="Vehoff, S" uniqKey="Vehoff S" first="S." last="Vehoff">S. Vehoff</name></noRegion><name sortKey="Nurnberger, D E A" sort="Nurnberger, D E A" uniqKey="Nurnberger D" first="D. E. A." last="Nürnberger">D. E. A. Nürnberger</name></country><country name="États-Unis"><noRegion><name sortKey="Monnier, J D" sort="Monnier, J D" uniqKey="Monnier J" first="J. D." last="Monnier">J. D. Monnier</name></noRegion><name sortKey="Duschl, W J" sort="Duschl, W J" uniqKey="Duschl W" first="W. J." last="Duschl">W. J. Duschl</name></country><country name="Australie"><region name="Nouvelle-Galles du Sud"><name sortKey="Tuthill, P" sort="Tuthill, P" uniqKey="Tuthill P" first="P." last="Tuthill">P. Tuthill</name></region></country><country name="France"><noRegion><name sortKey="Chesneau, O" sort="Chesneau, O" uniqKey="Chesneau O" first="O." last="Chesneau">O. Chesneau</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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