Issue |
A&A
Volume 580, August 2015
|
|
---|---|---|
Article Number | A75 | |
Number of page(s) | 13 | |
Section | Catalogs and data | |
DOI | https://doi.org/10.1051/0004-6361/201526248 | |
Published online | 05 August 2015 |
The Gaia-ESO Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities⋆,⋆⋆
1
Astrophysics Group, Keele University,
Keele,
Staffordshire
ST5 5BG,
UK
e-mail:
r.j.jackson@keele.ac.uk
2
Institute of Astronomy, University of Cambridge,
Madingley Road, Cambridge,
CB3 0HA,
UK
3
Moscow MV Lomonosov State University, Sternberg Astronomical
Institute, 119992
Moscow,
Russia
4
INAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi
5, 50125
Florence,
Italy
5
Research School of Astronomy & Astrophysics, Australian
National University, Cotter
Road, Weston Creek,
ACT
2611,
Australia
6
Rudolf Peierls Centre for Theoretical Physics, Keble
Road, Oxford,
OX1 3NP,
UK
7
GEPI, Observatoire de Paris, CNRS, Université Paris
Diderot, 5 place Jules
Janssen, 92190
Meudon,
France
8
Centre for Astrophysics Research, STRI, University of
Hertfordshire, College Lane
Campus, Hatfield
AL10 9AB,
UK
9
Lund Observatory, Department of Astronomy and Theoretical
Physics, Box 43,
221 00
Lund,
Sweden
10
Institute of Astronomy, University of Edinburgh,
Blackford Hill, Edinburgh
EH9 3HJ,
UK
11
INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento
1, 90134
Palermo,
Italy
12
Departamento de Física, Ingeniería de Sistemas y Teoría de la
Señal,
Universidad de Alicante, Apdo.
99, 03080
Alicante,
Spain
13
ESA, ESTEC, Keplerlaan 1, Po Box
299
2200 AG,
Noordwijk, The
Netherlands
14
Max-Planck Institut für Astronomie, Königstuhl 17, 69117
Heidelberg,
Germany
15
INAF–Padova Observatory, Vicolo dell’Osservatorio 5, 35122
Padova,
Italy
16
Instituto de Astrofísica de Andalucía-CSIC,
Apdo. 3004, 18080
Granada,
Spain
17
Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain
18
Universidad de La Laguna, Dept. Astrofísica, 38206,
La Laguna, Tenerife,
Spain
19
Royal Observatory of Belgium, Ringlaan 3, 1180
Brussels,
Belgium
20
INAF–Osservatorio Astronomico di Bologna, via Ranzani
1, 40127
Bologna,
Italy
21
Department of Physics and Astronomy, Uppsala
University, Box
516, 751 20
Uppsala,
Sweden
22
Dipartimento di Fisica e Astronomia, Sezione Astrofisica,
Università di Catania, via S. Sofia
78, 95123
Catania,
Italy
23
ASI Science Data Center, Via del Politecnico SNC,
00133
Roma,
Italy
24
Laboratoire Lagrange (UMR 7293), Université de Nice-Sophia
Antipolis, CNRS, Observatoire de la Côte d’Azur, CS 34229, 06304
Nice Cedex 4,
France
25
Department for Astrophysics, Nicolaus Copernicus Astronomical Center, ul. Rabiańska
8, 87–100
Toruń,
Poland
26
Institut d’Astronomie et d’Astrophysique, Université libre de
Brussels, Boulevard du
Triomphe, 1050
Brussels,
Belgium
27
Instituto de Física y Astronomiía, Universidad de
Valparaiíso, Chile
28
European Southern Observatory, Alonso de Cordova 3107 Vitacura, Santiago de Chile,
Chile
29
INAF–Osservatorio Astrofisico di Catania, via S. Sofia
78, 95123
Catania,
Italy
30
Astrophysics Research Institute, Liverpool John Moores
University, 146 Brownlow
Hill, Liverpool
L3 5RF,
UK
31
Departamento de Ciencias Físicas, Universidad Andrés
Bello, República 220,
837-0134
Santiago,
Chile
32
Millennium Institute of Astrophysics, Av. Vicuña Mackenna 4860, 782-0436 Macul,
Santiago,
Chile
33
Pontificia Universidad Católica de Chile,
Av. Vicuña Mackenna 4860, 782-0436
Macul, Santiago,
Chile
34
Instituto de Astrofísica e Ciências do Espaço, Universidade do
Porto, CAUP, Rua das
Estrelas, 4150-762
Porto,
Portugal
Received: 2 April 2015
Accepted: 25 May 2015
Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very Large Telescope.
Aims. A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (vsini) for representative samples of Galactic stars, which will complement information obtained by the Gaia astrometry satellite.
Methods. We present an analysis to empirically quantify the size and distribution of uncertainties in RV and vsini using spectra from repeated exposures of the same stars.
Results. We show that the uncertainties vary as simple scaling functions of signal-to-noise ratio (S/N) and vsini, that the uncertainties become larger with increasing photospheric temperature, but that the dependence on stellar gravity, metallicity and age is weak. The underlying uncertainty distributions have extended tails that are better represented by Student’s t-distributions than by normal distributions.
Conclusions. Parametrised results are provided, which enable estimates of the RV precision for almost all GES measurements, and estimates of the vsini precision for stars in young clusters, as a function of S/N, vsini and stellar temperature. The precision of individual high S/N GES RV measurements is 0.22–0.26 km s-1, dependent on instrumental configuration.
Key words: stars: kinematics and dynamics / open clusters and associations: general
Based on observations collected with the FLAMES spectrograph at VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia- ESO Large Public Survey (188.B-3002).
Full Table 2 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/580/A75
© ESO, 2015
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