EDP Sciences
AMBER: Instrument description and first astrophysical results
Press Release
Free Access
Issue
A&A
Volume 464, Number 1, March II 2007
AMBER: Instrument description and first astrophysical results
Page(s) 55 - 58
DOI https://doi.org/10.1051/0004-6361:20065719
Published online 12 September 2006


A&A 464, 55-58 (2007)
DOI: 10.1051/0004-6361:20065719

Constraining the wind launching region in Herbig Ae stars: AMBER/VLTI spectroscopy of HD 104237

E. Tatulli1, A. Isella1, 2, A. Natta1, L. Testi1, A. Marconi1, F. Malbet3, P. Stee4, R.G. Petrov5, F. Millour3, 5, A. Chelli3, G. Duvert3, P. Antonelli4, U. Beckmann6, Y. Bresson4, M. Dugué4, S. Gennari1, L. Glück3, P. Kern3, S. Lagarde4, E. Le Coarer3, F. Lisi1, K. Perraut3, P. Puget3, F. Rantakyrö7, S. Robbe-Dubois5, A. Roussel4, G. Weigelt6, G. Zins3, M. Accardo1, B. Acke3, 8, K. Agabi5, E. Altariba3, B. Arezki3, E. Aristidi5, C. Baffa1, J. Behrend6, T. Blöcker6, S. Bonhomme4, S. Busoni1, F. Cassaing9, J.-M. Clausse4, J. Colin4, C. Connot6, A. Delboulbé3, A. Domiciano de Souza5, 4, T. Driebe6, P. Feautrier3, D. Ferruzzi1, T. Forveille3, E. Fossat5, R. Foy10, D. Fraix-Burnet3, A. Gallardo3, E. Giani1, C. Gil3, 11, A. Glentzlin4, M. Heiden6, M. Heininger6, O. Hernandez Utrera3, K.-H. Hofmann6, D. Kamm4, M. Kiekebusch7, S. Kraus6, D. Le Contel4, J.-M. Le Contel4, T. Lesourd12, B. Lopez4, M. Lopez12, Y. Magnard3, G. Mars4, G. Martinot-Lagarde12, 4, P. Mathias4, P. Mège3, J.-L. Monin3, D. Mouillet3, 13, D. Mourard4, E. Nussbaum6, K. Ohnaka6, J. Pacheco4, C. Perrier3, Y. Rabbia4, S. Rebattu4, F. Reynaud14, A. Richichi15, A. Robini5, M. Sacchettini3, D. Schertl6, M. Schöller7, W. Solscheid6, A. Spang4, P. Stefanini1, M. Tallon10, I. Tallon-Bosc10, D. Tasso4, F. Vakili5, O. von der Lühe16, J.-C. Valtier4, M. Vannier5, 7, 17, and N. Ventura3

1  INAF-Osservatorio Astrofisico di Arcetri, Istituto Nazionale di Astrofisica, Largo E. Fermi 5, 50125 Firenze, Italy
2  Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria 16, 20133 Milano, Italy
3  Laboratoire d'Astrophysique de Grenoble, UMR 5571 Université Joseph Fourier/CNRS, BP 53, 38041 Grenoble Cedex 9, France
4  Laboratoire Gemini, UMR 6203 Observatoire de la Côte d'Azur/CNRS, BP 4229, 06304 Nice Cedex 4, France
5  Laboratoire Universitaire d'Astrophysique de Nice, UMR 6525 Université de Nice - Sophia Antipolis/CNRS, Parc Valrose, 06108 Nice Cedex 2, France
6  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
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 29 May 2006 / Accepted 26 June 2006 )

Abstract
Aims.We investigate the origin of the ${\rm Br}\gamma$ emission of the Herbig Ae star HD 104237 on Astronomical Unit (AU) scales.
Methods.Using AMBER/VLTI at a spectral resolution $\mathcal{R}=1500$ we spatially resolve the emission in both the ${\rm Br}\gamma$ line and the adjacent continuum.
Results.The visibility does not vary between the continuum and the ${\rm Br}\gamma$ line, even though the line is strongly detected in the spectrum, with a peak intensity 35% above the continuum. This demonstrates that the line and continuum emission have similar size scales. We assume that the K-band continuum excess originates in a "puffed-up" inner rim of the circumstellar disk, and discuss the likely origin of  ${\rm Br}\gamma$.
Conclusions.We conclude that this emission most likely arises from a compact disk wind, launched from a region 0.2-0.5 AU from the star, with a spatial extent similar to that of the near infrared continuum emission region, i.e., very close to the inner rim location.


Key words: stars: individual: HD 104237 -- stars: pre-main sequence -- technique: interferometric



© ESO 2007

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