Volume 573, January 2015
|Number of page(s)||13|
|Section||Galactic structure, stellar clusters and populations|
|Published online||08 January 2015|
Astrophysics Research Institute, Liverpool John Moores
146 Brownlow Hill,
2 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
3 ASI Science Data Center, Via del Politecnico SNC, 00133 Roma, Italy
4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
5 INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Florence, Italy
6 Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, 221 00 Lund, Sweden
7 Astrophysics Group, Research Institute for the Environment, Physical Sciences and Applied Mathematics, Keele University, Keele, Staffordshire ST5 5BG, UK
8 INAF – Padova Observatory, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
9 Instituto de Astrofísica de Andalucía-CSIC, Apdo. 3004, 18080 Granada, Spain
10 Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain
11 Universidad de La Laguna, Dept. Astrofísica, 38206, La Laguna, Tenerife, Spain
12 INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
13 Moscow MV Lomonosov State University, Sternberg Astronomical Institute, 119992 Moscow, Russia
14 Laboratoire Lagrange (UMR 7293), Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, CS 34229, 06304 Nice Cedex 4, France
15 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile
Received: 20 September 2014
Accepted: 14 November 2014
The Gaia-ESO survey is a large public spectroscopic survey aimed at investigating the origin and formation history of our Galaxy by collecting spectroscopy of representative samples (about 105 Milky Way stars) of all Galactic stellar populations, in the field and in clusters. The survey uses globular clusters as intra- and inter-survey calibrators, deriving stellar atmospheric parameters and abundances of a significant number of stars in clusters, along with radial velocity determinations. We used precise radial velocities of a large number of stars in seven globular clusters (NGC 1851, NGC 2808, NGC 4372, NGC 4833, NGC 5927, NGC 6752, and NGC 7078) to validate pipeline results and to preliminarily investigate the cluster internal kinematics. Radial velocity measurements were extracted from FLAMES/GIRAFFE spectra processed by the survey pipeline as part of the second internal data release of data products to ESO. We complemented our sample with ESO archival data obtained with different instrument configurations. Reliable radial velocity measurements for 1513 bona fide cluster star members were obtained in total. We measured systemic rotation, estimated central velocity dispersions, and present velocity dispersion profiles of all the selected clusters, providing the first velocity dispersion curve and the first estimate of the central velocitydispersion for the cluster NGC 5927. Finally, we explore the possible link between cluster kinematics and other physical parameters. The analysis we present here demonstrates that Gaia-ESO survey data are sufficiently accurate to be used in studies of kinematics of stellar systems and stellar populations in the Milky Way.
Key words: globular clusters: general
Full Table 3 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/573/A115
Based on data products from observations made with ESO telescopes at the La Silla Paranal Observatory under programme 188.B-3002 (the public Gaia-ESO spectroscopic survey, PIs Gilmore & Randich) and on the archive data of the programmes 62.N-0236, 63.L-0439, 65.L-0561, 68.D-0212, 68.D-0265, 69.D-0582, 064.L-0255, 065.L-0463, 071.D-0205, 073.D-0211, 073.D-0695, 075.D-0492, 077.D-0246, 077.D-0652, 079.D-0645, 080.B-0489, 080.D-0106, 081.D-0253, 082.B-0386, 083.B-0083, 083.D-0208, 083.D-0798, 085.D-0205, 086.D-0141, 088.A-9012, 088.B-0403, 088.B-0492, 088.D-0026, 088.D-0519, 089.D-0038, 164.O-0561, 386.D-0086.
© ESO, 2015
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