Sign on
ADS Classic is now deprecated. It will be completely retired in October 2019. This page will automatically redirect to the new ADS interface at that point.

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Printable Article (PDF/Postscript)
· Scanned Article (GIF)
· Table of Contents
· References in the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Results of the NaCo Large Program: probing the occurrence of exoplanets and brown dwarfs at wide orbit
Authors:
Vigan, A.; Chauvin, G.; Bonavita, M.; Desidera, S.; Bonnefoy, M.; Mesa, D.; Beuzit, J.-L.; Augereau, J.-C.; Biller, B.; Boccaletti, A.; Brugaletta, E.; Buenzli, E.; Carson, J.; Covino, E.; Delorme, P.; Eggenberger, A.; Feldt, M.; Hagelberg, J.; Henning, T.; Lagrange, A.-M.; Lanzafame, A.; Ménard, F.; Messina, S.; Meyer, M.; Montagnier, G.; Mordasini, C.; Mouillet, D.; Moutou, C.; Mugnier, L.; Quanz, S. P.; Reggiani, M.; Ségransan, D.; Thalmann, C.; Waters, R.; Zurlo, A.
Affiliation:
AA(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France. ), AB(UJF-Grenoble 1 / CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France), AC(INAF - Osservatorio Astronomico di Padova, Vicolo dell' Osservatorio 5, 35122, Padova, Italy), AD(INAF - Osservatorio Astronomico di Padova, Vicolo dell' Osservatorio 5, 35122, Padova, Italy), AE(Max Planck Instiute für Astronomy, Königsthul 17, D-69117 Heidelberg, Germany), AF(INAF - Osservatorio Astronomico di Padova, Vicolo dell' Osservatorio 5, 35122, Padova, Italy), AG(UJF-Grenoble 1 / CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France), AH(UJF-Grenoble 1 / CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France), AI(Max Planck Instiute für Astronomy, Königsthul 17, D-69117 Heidelberg, Germany), AJ(LESIA, Observatoire de Paris, CNRS, University Pierre et Marie Curie Paris 6; University Denis Diderot Paris 7, 5 place Jules Janssen, 92195 Meudon, France), AK(INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy), AL(Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland), AM(College of Charleston, Department of Physics & Astronomy, USA), AN(INAF - Osservatorio Astronomico di Napoli, Salita Moiariello 16, 80131 Napoli, Italy), AO(UJF-Grenoble 1 / CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France), AP(UJF-Grenoble 1 / CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France), AQ(Max Planck Instiute für Astronomy, Königsthul 17, D-69117 Heidelberg, Germany), AR(Geneva Observatory, Univ. of Geneva, Chemin des Mailettes 51, 1290, Versoix, Switzerland), AS(Max Planck Instiute für Astronomy, Königsthul 17, D-69117 Heidelberg, Germany), AT(UJF-Grenoble 1 / CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France), AU(INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy), AV(UJF-Grenoble 1 / CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France), AW(INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy), AX(Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland), AY(Observatoire de Haute-Provence, CNRS/OAMP, 04870 Saint-Michel-l'Observatoire, France), AZ(Max Planck Instiute für Astronomy, Königsthul 17, D-69117 Heidelberg, Germany), BA(UJF-Grenoble 1 / CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France), BB(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France. ), BC(Onera - The French Aerospace Lab, 92322, Chatillon, France), BD(Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland), BE(Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland), BF(Geneva Observatory, Univ. of Geneva, Chemin des Mailettes 51, 1290, Versoix, Switzerland), BG(University of Amsterdam, Postbus 94249, 1090 GE, Amsterdam, The Netherlands), BH(University of Amsterdam, Postbus 94249, 1090 GE, Amsterdam, The Netherlands), BI(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France. )
Publication:
Exploring the Formation and Evolution of Planetary Systems, Proceedings of the International Astronomical Union, IAU Symposium, Volume 299, pp. 17-20
Publication Date:
01/2014
Origin:
CUP
Keywords:
instrumentation: adaptive optics, instrumentation: high angular resolution, stars: imaging, methods: statistical,
Abstract Copyright:
(c) 2014: Copyright © International Astronomical Union 2013
DOI:
10.1017/S1743921313007680
Bibliographic Code:
2014IAUS..299...17V

Abstract

Over the past decade, a growing number of deep imaging surveys have started to provide meaningful constraints on the population of extrasolar giant planets at large orbital separation. Primary targets for these surveys have been carefully selected based on their age, distance and spectral type, and often on their membership to young nearby associations where all stars share common kinematics, photometric and spectroscopic properties. The next step is a wider statistical analysis of the frequency and properties of low mass companions as a function of stellar mass and orbital separation. In late 2009, we initiated a coordinated European Large Program using angular differential imaging in the H band (1.66 mum) with NaCo at the VLT. Our aim is to provide a comprehensive and statistically significant study of the occurrence of extrasolar giant planets and brown dwarfs at large (5-500 AU) orbital separation around ~150 young, nearby stars, a large fraction of which have never been observed at very deep contrast. The survey has now been completed and we present the data analysis and detection limits for the observed sample, for which we reach the planetary-mass domain at separations of >~50 AU on average. We also present the results of the statistical analysis that has been performed over the 75 targets newly observed at high-contrast. We discuss the details of the statistical analysis and the physical constraints that our survey provides for the frequency and formation scenario of planetary mass companions at large separation.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints