Reference : An Interferometric Study of the Fomalhaut Inner Debris Disk. I. Near-Infrared Detection ...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/25278
An Interferometric Study of the Fomalhaut Inner Debris Disk. I. Near-Infrared Detection of Hot Dust with VLTI/VINCI
English
Absil, Olivier mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Mennesson, Bertrand [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA]
Le Bouquin, Jean-Baptiste [European Southern Observatory, Casilla 19001, Santiago 19, Chile]
Di Folco, Emmanuel [LESIA-UMR 8109, CNRS and Observatoire de Paris-Meudon, 5 place J. Janssen, F-92195 Meudon, France]
Kervella, Pierre [LESIA-UMR 8109, CNRS and Observatoire de Paris-Meudon, 5 place J. Janssen, F-92195 Meudon, France]
Augereau, Jean-Charles [LAOG-UMR 5571, CNRS and Université Joseph Fourier, BP 53, F-38041 Grenoble, France]
10-Oct-2009
Astrophysical Journal
University of Chicago Press
704
150-160
Yes (verified by ORBi)
International
0004-637X
Chicago
IL
[en] circumstellar matter ; stars: individual: Fomalhaut ; techniques: interferometric
[en] The innermost parts of dusty debris disks around main-sequence stars are currently poorly known due to the high contrast and small angular separation with their parent stars. Using near-infrared interferometry, we aim to detect the signature of hot dust around the nearby A4 V star Fomalhaut, which has already been suggested to harbor a warm dust population in addition to a cold dust ring located at about 140 AU. Archival data obtained with the VINCI instrument at the VLTI are used to study the fringe visibility of the Fomalhaut system at projected baseline lengths ranging from 4 m to 140 m in the K band. A significant visibility deficit is observed at short baselines with respect to the expected visibility of the sole stellar photosphere. This is interpreted as the signature of resolved circumstellar emission, producing a relative flux of 0.88% ± 0.12% with respect to the stellar photosphere. While our interferometric data cannot directly constrain the morphology of the excess emission source, complementary data from the literature allow us to discard an off-axis point-like object as the source of circumstellar emission. We argue that the thermal emission from hot dusty grains located within 6 AU from Fomalhaut is the most plausible explanation for the detected excess. Our study also provides a revised limb-darkened diameter for Fomalhaut (theta_LD = 2.223 ± 0.022 mas), taking into account the effect of the resolved circumstellar emission. Based on observations made with ESO Telescopes at the Paranal Observatory (public VINCI commissioning data).
Researchers
http://hdl.handle.net/2268/25278
10.1088/0004-637X/704/1/150
http://adsabs.harvard.edu/abs/2009ApJ...704..150A
http://www.iop.org/EJ/abstract/0004-637X/704/1/150/ - Copyright The American Astronomical Society (AAS) and IOP Publishing Limited 2009
http://de.arxiv.org/abs/0908.3133

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