Volume 469, Number 2, July II 2007
|Page(s)||529 - 537|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||24 April 2007|
Multi-color photometry of the Galactic globular cluster M 75 = NGC 6864. A new sensitive metallicity indicator and the position of the horizontal branch in UV *,**
Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Antofagasta, Chile e-mail: firstname.lastname@example.org
2 Sternberg Astronomical Institute, University Avenue 13, 119899 Moscow, Russia
3 Isaac Newton Institute of Chile, Ministerio de Educación de Chile, Casilla 8-9, Correo 9, Santiago, Chile e-mail: email@example.com, firstname.lastname@example.org
4 ESO - European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile e-mail: email@example.com
Accepted: 22 March 2007
Aims.We carry out and analyze new multi-color photometry of the Galactic globular cluster (GC) M 75 in and focus on the brighter sequences of the color–magnitude diagram (CMD), with particular emphasis on their location in U-based CMD. Specifically, we study the level both of the horizontal (HB) and red giant branches (RGB) relative to the main-sequence turnoff (TO) in the U magnitude.
Methods.Along with the presented photometry of M 75, we use our collection of photometric data on GCs belonging to the metal-poor range, [Fe/H] dex, obtained from observations with different equipment, but calibrated by standard stars situated in the observed cluster fields.
Results.We confirm our earlier finding, and extend it to a larger magnitude range. We demonstrate that expressing the difference in U magnitude between the TO point and the level of the blue HB, near its red boundary, of the metal-poor GCs observed with the EMMI camera of the NTT/ESO telescope is about 0.4–0.5 mag smaller as compared to GCs observed with the 100″ telescope and 1.3 m Warsaw telescope of the Las Campanas Observatory. At the same time, , the difference in U magnitude between the TO and RGB inflection (brightest) points, does not show such an apparent dependence on the characteristics of U filters used, but it depends on cluster metallicity. We have shown, for the first time, the dependence of the parameter on [Fe/H] and have estimated its analytical expression, by assuming a linear relation between the parameter and metallicity. Its slope, /Δ[Fe/H] ~ 1.2 mag/dex, is approximately a factor of two steeper than that of the dependence of the RGB bump position in the V magnitude on metallicity. The asymptotic giant branch (AGB) clump and features of the RGB luminosity function (LF) of M 75 are also discussed.
Key words: Galaxy: globular clusters: general / Galaxy: globular clusters: individual: M 75 / stars: population II
© ESO, 2007
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