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Metallicity distribution of ω Cen Red Giants based on the Strömgren m1 metallicity index

Published online by Cambridge University Press:  01 December 2006

A. Calamida
Affiliation:
INAF-Osservatorio Astronomico di Roma, Via Frascati 33, 00040, Monte Porzio Catone, Italy email: calamida@mporzio.astro.it Universita' di Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Rome, Italy
G. Bono
Affiliation:
INAF-Osservatorio Astronomico di Roma, Via Frascati 33, 00040, Monte Porzio Catone, Italy email: calamida@mporzio.astro.it
L. M. Freyhammer
Affiliation:
Centre for Astrophysics, University of Central Lancashire, Preston PR1 2HE, UK
F. Grundahl
Affiliation:
Institute of Physics and Astronomy, Aarhus University, Ny Munkegade, 8000 Aarhus C, Denmark
C. E. Corsi
Affiliation:
INAF-Osservatorio Astronomico di Roma, Via Frascati 33, 00040, Monte Porzio Catone, Italy email: calamida@mporzio.astro.it
P. B. Stetson
Affiliation:
DAO, HIA-NRC, 5071 W. Saanich Road, Victoria, BC V9E 2E7, Canada
R. Buonanno
Affiliation:
Universita' di Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Rome, Italy
M. Hilker
Affiliation:
ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany
T. Richtler
Affiliation:
Universidad de Concepcion, Departamento de Fisica, Casilla 106-C, Concepcion, Chile
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Abstract

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We adopted uvby Strömgren photometry to investigate the metallicity distribution of ω Cen Red Giant (RG) stars. We provided a new empirical calibration of the Strömgren m1≡(v − b) − (b − y) metallicity index based on cluster stars. The new calibration has been applied to a sample of ω Cen RGs. The shape of the estimated metallicity distribution is clearly asymmetric, with a sharp cut-off at low metallicities ([Fe/H] < −2.0) and a metal-rich tail up to [Fe/H] ∼ 0.0. Two main metallicity peaks have been identified, around [Fe/H]≈ −1.9 and −1.3 dex, and a metal-rich shoulder at ≈ −0.2 dex.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

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