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A&A 483, L13-L16 (2008)
DOI: 10.1051/0004-6361:200809641
Letter
Gas and dust in the inner disk of the Herbig Ae star MWC 758
A. Isella1, 2, E. Tatulli1, 3, A. Natta1, and L. Testi1, 41 Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy
2 California Institute of Technology, MC 105-24, 1200 East California Blvd., Pasadena CA 91125, USA
e-mail: isella@astro.caltech.edu
3 Laboratoire d'Astrophysique de Grenoble, UMR 5571, Université Joseph Fourier/CNRS, BP 53, 38041 Grenoble Cedex 9, France
4 ESO, Karl-Schwarschild Strasse 2, 85748 Garching bei München, Germany
(Received 24 February 2008 / Accepted 25 March 2008)
Abstract
We investigate the origin of the near-infrared emission of the Herbig Ae star MWC 758 on sub-astronomical unit (AU) scales using spectrally dispersed low resolution
(R = 35) AMBER/VLTI interferometric observations in the H (1.7 
m) and K (2.2 m) bands.
We find that the K band visibilities and closure phases are consistent with the presence of a dusty
disk inner rim located at the dust evaporation distance (0.4 AU) while the bulk of the H band emission
arises within 0.1 AU from the central star. Comparing the observational results
with theoretical model predictions, we suggest that the H band emission is dominated by an hot gaseous
accretion disk.
Key words: accretion, accretion disks -- techniques: interferometric -- stars: planetary systems: protoplanetary disks
© ESO 2008