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|Title:||The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits. I. Sample definition and characterization||Authors:||DESIDERA, Silvano
Schlieder, J. E.
ALCALA', JUAN MANUEL
Beuzit, J. L.
GIRARDI, Leo Alberto
Lagrange, A. M.
Lanzafame, Alessandro Carmelo
Zaidi, C. M.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||573||First Page:||A126||Abstract:||Context. Young, close stars are ideal targets for searching planets using the direct imaging technique. The determination of stellar parameters is crucial for the interpretation of imaging survey results, particularly since the luminosity of substellar objects has a strong dependence on system age. Aims: We have conducted a large program with NaCo at the VLT to search for planets and brown dwarfs in wide orbits around 86 stars. A large fraction of the targets observed with NaCo were poorly investigated in the literature. We performed a study to characterize the fundamental properties (age, distance, and mass) of the stars in our sample. To improve target age determinations, we compiled and analyzed a complete set of age diagnostics. Methods: We measured spectroscopic parameters and age diagnostics using dedicated observations acquired with FEROS and CORALIE spectrographs at La Silla Observatory. We also made extensive use of archival spectroscopic data and the results that are available in the literature. Additionally, we exploited photometric time-series, which are available in ASAS and Super-WASP archives, to derive a rotational period for a large fraction of our program stars. Results: We provided updated characterization of all the targets observed in the VLT NaCo Large program, a survey designed to probe the occurrence of exoplanets and brown dwarfs in wide orbits. The median distance and age of our program stars are 64 pc and 100 Myr, respectively. Nearly all the stars have masses between 0.70 and 1.50, with a median value of 1.01 . The typical metallicity is close to solar with a dispersion that is smaller than that of samples usually observed in radial velocity surveys. Several stars are confirmed or proposed here to be members of close young moving groups. Eight spectroscopic binaries are identified. Based on observations collected at La Silla and Paranal Observatory, ESO (Chile) using FEROS, HARPS, and NaCo; with the CORALIE echelle spectrograph mounted on the 1.2 m Swiss telescope at La Silla Observatory; and on the All Sky Automated Survey (ASAS) photometric data. Tables 1-4, 6, 8 and Appendices are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201323168/olm">http://www.aanda.org</A>Tables 9-12 and D.1 are only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://18.104.22.168) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/573/A126">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/573/A126||Acknowledgments:||Based on observations collected at La Silla and Paranal Observatory, ESO (Chile): Programs 70.D-0081A, 072.D-0021, 072.C-0393, 074.D-0016, 074.A-9002, 074.A-9020, 076.C-0578, 076.A-9013, 077.C-0138, 077.D-0525, 081.A-9005, 082.A-9007, 083.A-9003, 083.A-9011, 083.A-9013, 084.A-9004, 084.A-9011 (FEROS), 072.C-0488, 074.C-0037, 075.C-0689, 076.C-0010, 077.C-0012, 077.D-0085, 077.C-0295, 079.C-0046, 079.C-0170, 080.D-0151, 080.C-0712, 080.C-0664, 081.D-0008, 081.C-0779, 082.C-0390, 184.C-0815 (HARPS), 184.C-0157 (NaCo). Based on data obtained from the ESO Science Archive Facility. This research has made use of the SIMBAD database and Vizier services, operated at CDS, Strasbourg, France and of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. We have used data from the WASP public archive in this research. The WASP consortium comprises of the University of Cambridge, Keele University, University of Leicester, The Open University, The Queen’s University Belfast, St. Andrews University and the Isaac Newton Group. Funding for WASP comes from the consortium universities and from the UK’s Science and Technology Facilities Council. We thank the SACY team for providing reduced spectra of NaCo-LP targets from their archive. We thank the SOPHIE Consortium for providing unpublished activity measurements. We thank L. Pastori for providing the CES spectra of HD 16699 A and B. We thank B. Mason for providing astrometric data for individual objects collected in the Washington Double Star Catalog. We acknowledge partial support from PRIN-INAF 2010 “Planetary systems at young ages and the interactions with their active host stars”. JC was supported by the US National Science Foundation under Award No. 1009203.||URI:||http://hdl.handle.net/20.500.12386/23971||URL:||http://arxiv.org/abs/1405.1559v1
|Appears in Collections:||1.01 Articoli in rivista|
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