Volume 449, Number 1, April I 2006
|Page(s)||349 - 358|
|Published online||16 March 2006|
VLT-UVES analysis of two giants in the bulge metal-poor globular cluster HP-1
Analysis of two giants in HP-1
Universidade de São Paulo, IAG, Rua do Matão 1226, Cidade Universitária, São Paulo 05508-900, Brazil e-mail: email@example.com
2 Universidad Catolica de Chile, Department of Astronomy & Astrophysics, Casilla 306, Santiago 22, Chile e-mail: [mzoccali;dante]@astro.puc.cl
3 Università di Padova, Dipartimento di Astronomia, Vicolo dell'Osservatorio 2, 35122 Padova, Italy e-mail: [ortolani;momany]@pd.astro.it
4 European Southern Observatory, Karl Schwarzschild Strasse 2, 85748 Garching bei München, Germany e-mail: [arenzini;lpasquin]@eso.org
5 Observatoire de Paris-Meudon, 92195 Meudon Cedex, France e-mail: Vanessa.Hill@obspm.fr
6 UCLA, Department of Physics & Astronomy, 8979 Math-Sciences Building, Los Angeles, CA 90095-1562, USA e-mail: firstname.lastname@example.org
7 Universidade Federal do Rio Grande do Sul, Departamento de Astronomia, CP 15051, Porto Alegre 91501-970, Brazil e-mail: email@example.com
8 Aryabhatta Research Institute of Observational Sciences, (ARIES) Manora Peak, NainiTal 263129, India
Accepted: 30 November 2005
Context.Metal-poor globular clusters in the bulge are important tracers of early chemical evolution. HP-1 is among the six metal-poor clusters within 5° of the Galactic center, and could be the one closest to the centerAims. The main purpose of this study is the determination of metallicity and elemental ratios. Methods.High resolution spectra of two giants of the bulge globular cluster HP-1 were obtained at the 8 m VLT UT2-Kueyen telescope with the UVES spectrograph. This is the second metal-poor globular cluster in the bulge for which a detailed abundance analysis is presented. Multiband photometry was used to derive effective temperatures.Results. The present analysis provides a metallicity [Fe/H] = . The α-elements oxygen and silicon show [ α/Fe] ≈ +0.3, whereas magnesium, calcium and titanium show solar ratios. A proper motion analysis indicates that the two stars are cluster members. Conclusions.The metallicity is unexpected for a blue Horizontal Branch (BHB) cluster. HP-1 is the first known cluster with such a high metallicity combined with a BHB and a steep Red Giant Branch (RGB). Together with NGC 6388 and NGC 6441 of it would be third with such characteristics, but it differs from them, since these two other clusters have also a populous Red HB, and a normal slope of the RGB for their metallicity, which is not the case of HP-1.
© ESO, 2006
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