Reference : A near-infrared interferometric survey of debris disc stars. II. CHARA/FLUOR observat...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/18133
A near-infrared interferometric survey of debris disc stars. II. CHARA/FLUOR observations of six early-type dwarfs
English
Absil, Olivier mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
di Folco, E. [Observatoire Astronomique de l'Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland]
Mérand, A. [Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3969, Atlanta, Georgia 30302-3965, USA]
Augereau, J.-C. [LAOG - UMR 5571, CNRS and Université Joseph Fourier, BP 53, 38041 Grenoble, France]
Coudé Du Foresto, V. [LESIA - UMR 8109, CNRS and Observatoire de Paris-Meudon, 5 place J. Janssen, 92195 Meudon, France]
Defrère, Denis [Université de Liège - ULg > Département d'Astrophysique, Géophysique et Océanographie > > >]
Kervella, P. [LESIA - UMR 8109, CNRS and Observatoire de Paris-Meudon, 5 place J. Janssen, 92195 Meudon, France]
Aufdenberg, J. P. [Physical Sciences Department, Embry-Riddle Aeronautical University, Daytona Beach, FL 32114, USA]
Desort, M. [LAOG - UMR 5571, CNRS and Université Joseph Fourier, BP 53, 38041 Grenoble, France]
Ehrenreich, D. [LAOG - UMR 5571, CNRS and Université Joseph Fourier, BP 53, 38041 Grenoble, France]
Lagrange, A.-M. [LAOG-UMR 5571, CNRS and Université Joseph Fourier, BP 53, 38041 Grenoble, France]
Montagnier, G. [Observatoire Astronomique de l'Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland ; LAOG-UMR 5571, CNRS and Université Joseph Fourier, BP 53, 38041 Grenoble, France]
Olofsson, J. [LAOG-UMR 5571, CNRS and Université Joseph Fourier, BP 53, 38041 Grenoble, France]
Ten Brummelaar, T. A. [Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3969, Atlanta, Georgia 30302-3965, USA]
McAlister, H. A. [Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3969, Atlanta, Georgia 30302-3965, USA]
Sturmann, J. [Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3969, Atlanta, Georgia 30302-3965, USA]
Sturmann, L. [Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3969, Atlanta, Georgia 30302-3965, USA]
Turner, N. H. [Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3969, Atlanta, Georgia 30302-3965, USA]
1-Sep-2008
Astronomy and Astrophysics
EDP Sciences
487
1041-1054
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] stars: fundamental parameters ; circumstellar matter ; binaries: close ; methods: observational ; techniques: interferometric
[en] Aims. We aim at directly detecting the presence of optically thin circumstellar dust emission within the terrestrial planetary zone around main sequence stars known to harbour cold debris discs. The present study focuses on a sample of six bright A- and early F-type stars. Methods: High-precision interferometric observations have been obtained in the near-infrared K band with the FLUOR instrument installed on the CHARA Array. The measured squared visibilities are compared to the expected visibility of the stellar photospheres based on theoretical photospheric models taking into account rotational distortion. We search for potential visibility reduction at short baselines, a direct piece of evidence for resolved circumstellar emission. Results: Our observations bring to light the presence of resolved circumstellar emission around one of the six target stars (zeta Aql) at the 5sigma level. The morphology of the emission source cannot be directly constrained because of the sparse spatial frequency sampling of our interferometric data. Using complementary adaptive optics observations and radial velocity measurements, we find that the presence of a low-mass companion is a likely origin for the excess emission. The potential companion is characterised by a K-band contrast of four magnitudes. It has a most probable mass of about 0.6~Msun and is expected to orbit between about 5.5 AU and 8 AU from its host star assuming a purely circular orbit. Nevertheless, by adjusting a physical debris disc model to the observed Spectral Energy Distribution of the zeta Aql system, we also show that the presence of hot dust within 10 AU from zeta Aql, producing a total thermal emission equal to 1.69 ± 0.31% of the photospheric flux in the K band, is another viable explanation for the observed near-infrared excess. Our re-interpretation of archival near- to far-infrared photometric measurements shows however that cold dust is not present around zeta Aql at the sensitivity limit of the IRS and MIPS instruments onboard Spitzer, and urges us to remove zeta Aql from the category of bona fide debris disc stars. Conclusions: The hot debris disc around Vega (Absil et al. 2006) currently remains our only secure resolved detection within the context of this survey, with six genuine early-type debris disc stars observed so far. Further observations will be needed to assess whether zeta Aql also belongs to this hot debris disc category. Partly based on observations collected at the European Southern Observatory, La Silla, Chile, under program IDs 073.C-0733, 077.C-0295 and 080.C-0712.
Researchers
http://hdl.handle.net/2268/18133
10.1051/0004-6361:200810008
http://adsabs.harvard.edu/abs/2008A%26A...487.1041A
http://de.arxiv.org/abs/0806.4936

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