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A&A Supplement series, Vol. 127, January II 1998, 167-179

Received October 11, 1995; accepted April 29, 1997

V, I CCD photometry of metal-rich globular clusters:
NGC 6528gif

T. Richtler tex2html_wrap1552 - E.K. Grebel tex2html_wrap1554 - A. Subramaniam tex2html_wrap1556 - R. Sagar tex2html_wrap1558

Send offprint request: T. Richtler, Bonn

tex2html_wrap1560  Sternwarte der Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany
tex2html_wrap1562  Indian Institute of Astrophysics, 560034 Bangalore, India,
tex2html_wrap1564  Astronomisches Institut der Universität Würzburg, Am Hubland, D-97074 Würzburg, Germany
tex2html_wrap1566  Uttar Pradesh State Observatory, Naini Tal, India


We present CCD photometry in V and I for the metal-rich globular cluster NGC 6528. A comparison with previous photometry reveals discrepancies of the order 0.1 to 0.2 mag in V, emphasizing the need for independent photometry. As found previously, the giant branch (or the asymptotic giant branch, which cannot be distinguished) of the cluster extends to V-I = 7. Population synthesis in V-I must take these red stars into account in order to understand integrated red colours of bulge populations. Currently available theoretical isochrones do not reproduce the shape of the RGB/AGB. The derivation of reliable values for reddening, distance and metallicity of NGC 6528 is hampered by uncertainties in the extrapolation to high metallicity, which dominate the absolute error rather than the photometric uncertainty does. Together with other properties (old age derived from HST data, high radial velocity), this object is more likely a member of the bulge than of the disk population.gif

keywords: Galaxy: globular clusters: general; individual: NGC 6528 -- galaxy abundances -- stars: late-type -- HR diagram

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