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A&A 464, 43-53 (2007)
DOI: 10.1051/0004-6361:20053924

Disk and wind interaction in the young stellar object MWC 297 spatially resolved with AMBER/VLTI

F. Malbet¹, M. Benisty¹, W.-J. de Wit¹, S. Kraus², A. Meilland³, F. Millour^{1, 4}, E. Tatulli^{1, 5}, J.-P. Berger¹, O. Chesneau³, K.-H. Hofmann², A. Isella^{5, 6}, A. Natta⁵, R.G. Petrov⁴, T. Preibisch², P. Stee³, L. Testi⁵, G. Weigelt², P. Antonelli³, U. Beckmann², Y. Bresson³, A. Chelli¹, M. Dugué³, G. Duvert¹, S. Gennari⁵, L. Glück¹, P. Kern¹, S. Lagarde³, E. Le Coarer¹, F. Lisi⁵, K. Perraut¹, P. Puget¹, F. Rantakyrö⁷, S. Robbe-Dubois⁴, A. Roussel³, G. Zins¹, M. Accardo⁵, B. Acke^{1, 8}, K. Agabi⁴, E. Altariba¹, B. Arezki¹, E. Aristidi⁴, C. Baffa⁵, J. Behrend², T. Blöcker², S. Bonhomme³, S. Busoni⁵, F. Cassaing⁹, J.-M. Clausse³, J. Colin³, C. Connot², A. Delboulbé¹, A. Domiciano de Souza^{4, 3}, T. Driebe², P. Feautrier¹, D. Ferruzzi⁵, T. Forveille¹, E. Fossat⁴, R. Foy¹⁰, D. Fraix-Burnet¹, A. Gallardo¹, E. Giani⁵, C. Gil^{1, 11}, A. Glentzlin³, M. Heiden², M. Heininger², O. Hernandez Utrera¹, D. Kamm³, M. Kiekebusch⁷, D. Le Contel³, J.-M. Le Contel³, T. Lesourd¹², B. Lopez³, M. Lopez¹², Y. Magnard¹, A. Marconi⁵, G. Mars³, G. Martinot-Lagarde^{12, 3}, P. Mathias³, P. Mège¹, J.-L. Monin¹, D. Mouillet^{1, 13}, D. Mourard³, E. Nussbaum², K. Ohnaka², J. Pacheco³, C. Perrier¹, Y. Rabbia³, S. Rebattu³, F. Reynaud¹⁴, A. Richichi¹⁵, A. Robini⁴, M. Sacchettini¹, D. Schertl², M. Schöller⁷, W. Solscheid², A. Spang³, P. Stefanini⁵, M. Tallon¹⁰, I. Tallon-Bosc¹⁰, D. Tasso³, F. Vakili⁴, O. von der Lühe¹⁶, J.-C. Valtier³, M. Vannier^{4, 7, 17}, and N. Ventura<sup>1

1</sup>  Laboratoire d'Astrophysique de Grenoble, UMR 5571 Université Joseph Fourier/CNRS, BP 53, 38041 Grenoble Cedex 9, France
    e-mail: Fabien.Malbet@obs.ujf-grenoble.fr
²  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
³  Laboratoire Gemini, UMR 6203 Observatoire de la Côte d'Azur/CNRS, BP 4229, 06304 Nice Cedex 4, France
⁴  Laboratoire Universitaire d'Astrophysique de Nice, UMR 6525 Université de Nice - Sophia Antipolis/CNRS, Parc Valrose, 06108 Nice Cedex 2, France
⁵  INAF-Osservatorio Astrofisico di Arcetri, Istituto Nazionale di Astrofisica, Largo E. Fermi 5, 50125 Firenze, Italy
⁶  Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria 16, 20133 Milano, Italy
⁷  European Southern Observatory, Casilla 19001, Santiago 19, Chile
⁸  Instituut voor Sterrenkunde, KU-Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
⁹  ONERA/DOTA, 29 av de la Division Leclerc, BP 72, 92322 Chatillon Cedex, France
¹⁰  Centre de Recherche Astronomique de Lyon, UMR 5574 Université Claude Bernard/CNRS, 9 avenue Charles André, 69561 Saint Genis Laval Cedex, France
¹¹  Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
¹²  Division Technique INSU/CNRS UPS 855, 1 place Aristide Briand, 92195 Meudon Cedex, France
¹³  Laboratoire Astrophysique de Toulouse, UMR 5572 Université Paul Sabatier/CNRS, BP 826, 65008 Tarbes Cedex, France
¹⁴  IRCOM, UMR 6615 Université de Limoges/CNRS, 123 avenue Albert Thomas, 87060 Limoges Cedex, France
¹⁵  European Southern Observatory, Karl Schwarzschild Strasse 2, 85748 Garching, Germany
¹⁶  Kiepenheuer Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany
¹⁷  Departamento de Astronomia, Universidad de Chile, Chile

(Received 26 July 2005/ Accepted 11 October 2005 )

Abstract
The young stellar object MWC 297 is an embedded B1.5Ve star exhibiting strong hydrogen emission lines and a strong near-infrared continuum excess. This object has been observed with the VLT interferometer equipped with the AMBER instrument during its first commissioning run. AMBER/VLTI is currently the only near infrared interferometer that can observe spectrally dispersed visibilities. MWC 297 has been spatially resolved in the continuum with a visibility of 0.50^+0.08_-0.10 as well as in the Br emission line where the visibility decreases to . This change in the visibility with wavelength can be interpreted by the presence of an optically thick disk responsible for the visibility in the continuum and of a stellar wind traced by the Br emission line and whose apparent size is 40% larger. We validate this interpretation by building a model of the stellar environment that combines a geometrically thin, optically thick accretion disk model consisting of gas and dust, and a latitude-dependent stellar wind outflowing above the disk surface. The continuum emission and visibilities obtained from this model are fully consistent with the interferometric AMBER data. They agree also with existing optical, near-infrared spectra and other broad-band near-infrared interferometric visibilities. We also reproduce the shape of the visibilities in the Br line as well as the profile of this line obtained at an higher spectral resolution with the VLT/ISAAC spectrograph, and those of the H and H lines. The disk and wind models yield a consistent inclination of the system of approximately 20°. A picture emerges in which MWC 297 is surrounded by an equatorial flat disk that is possibly still accreting and an outflowing wind that has a much higher velocity in the polar region than at the equator. The AMBER/VLTI unique capability of measuring spectral visibilities therefore allows us for the first time to compare the apparent geometry of a wind with the disk structure in a young stellar system.

Key words: accretion, accretion disks -- techniques: interferometric -- stars: pre-main sequence -- planetary systems: protoplanetary disks -- stars: emission-line, Be -- stars: individual: MWC297

© ESO 2007

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