| Issue |
A&A
Volume 374, Number 2, August I 2001
|
|
|---|---|---|
| Page(s) | 564 - 569 | |
| Section | Galactic structure, stellar clusters, and populations | |
| DOI | https://doi.org/10.1051/0004-6361:20010753 | |
| Published online | 15 August 2001 | |
Colour Magnitude Diagrams of the moderately metal-rich globular clusters NGC 6569 and Palomar 11 *
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
Corresponding author: B. Barbuy, 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 
and a distance
from the Sun 
kpc for NGC 6569, and
and
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
© ESO, 2001
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