EDP Sciences
Free access
Volume 374, Number 2, August I 2001
Page(s) 564 - 569
Section Stellar clusters and associations
DOI http://dx.doi.org/10.1051/0004-6361:20010753

A&A 374, 564-569 (2001)
DOI: 10.1051/0004-6361:20010753

Colour Magnitude Diagrams of the moderately metal-rich globular clusters NGC 6569 and Palomar 11

S. Ortolani1, E. Bica2 and B. Barbuy3

1  Università di Padova, Dept. di Astronomia, Vicolo dell'Osservatorio 5, 35122 Padova, Italy
    e-mail: ortolani@pd.astro.it
2  Universidade Federal do Rio Grande do Sul, Dept. de Astronomia, CP 15051, Porto Alegre 91501-970, Brazil
    e-mail: bica@if.ufrgs.br
3  Universidade de São Paulo, Dept. de Astronomia, CP 3386, São Paulo 01060-970, Brazil
    e-mail: barbuy@iagusp.usp.br

(Received 1 February 2001 / Accepted 23 May 2001 )

For the first time Colour-Magnitude Diagrams are presented for NGC 6569 and Palomar 11. NGC 6569 is a rather concentrated cluster whereas Palomar 11 is loose and sparsely populated. Cluster parameters are derived from V and I photometry. These are red Horizontal Branch globular clusters, with metallicities comparable to that of 47 Tucanae. We derive a reddening $E(B-V) \approx 0.53$ and a distance from the Sun $d_{\odot} \approx 9.8$ kpc for NGC 6569, and $E(B-V) \approx 0.35$ and $d_{\odot} \approx 13.2$ kpc for Palomar 11. NGC 6569 is located in the bulge, while Palomar 11, despite its rather high metallicity, is in the inner halo, a rare case similar to that of 47 Tucanae.

Key words: Galaxy: globular clusters: individual: NGC 6569, Palomar 11 -- stars: Hertzsprung-Russell diagram

Offprint request: B. Barbuy, barbuy@iagusp.usp.br

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© ESO 2001