The Globular Cluster PAL 11

Details The Globular Cluster PAL 11 The Globular Cluster PAL 11

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.5007c&link_type=abstract

American Astronomical Society, 182nd AAS Meeting, #50.07; Bulletin of the American Astronomical Society, Vol. 25, p.884

Astronomy and Astrophysics

Astronomy

2

Scientific paper

We present a color-magnitude diagram for the globular cluster Pal 11 (alpha = 19() h42() m32() s, delta =-08deg07 ' (1950), l =31.8deg , b =-15.6deg ). The cluster was observed in September 1989 and again in August 1992 using the direct CCD camera and standard B, V, and I filters on the 0.9m telescope at CTIO. From the color-magnitude diagram we determine a mean V magnitude of 17.35 for the horizontal branch (HB) and describe the morphology of the HB as a red clump of stars. These findings agree with previous investigations of the cluster. The metallicity of Pal 11 ([Fe/H]=-0.23) places it in the disk population of globular clusters which has been defined by Zinn as the clusters more metal rich than [Fe/H]=-0.8. Its distance from the galactic plane ( | Z | ga 3 kpc), however, makes it one of the most remote of the disk clusters.

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