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Catalogue and alternative designations NGC 6752


Type Globular Cluster 
Position  19 10 52, -59 59 04
Constellation Pavo
Camera and Telescope STXL11002 and 36.8 cm Ritchey Chretien
Focal Ratio F9
Exposure Details LRGB =90:90:100:100 with Baader filters

(Adapted from Wikipedia) NGC 6752 is a globular cluster in the constellation Pavo. It is the third brightest in the sky, after 47 Tucanae and Omega Centauri, and is best seen from June to October.

NGC 6752 was first identified by James Dunlop of Parramatta on 30 June 1826, who described it as an irregular bright nebula which could be resolved into a cluster of many stars, highly compressed at the centre. This corresponds with a core region densely populated with stars around 1.3 light years in diameter, which indicates it has undergone core collapse. The cluster lies around 13,000 light years distant and is one of the closer globular clusters to Earth. It also lies 17,000 light years away from the galactic centre. It belongs to Shapley–Sawyer Concentration Class VI, namely of intermediate density, and has been calculated to be 11.78 billion years old. There are a large number of binary stars in the system, as well as blue stragglers, which are likely to have been formed by collisions and mergers of smaller stars. The NASA website "Astronomy Picture of the Day" notes that it holds over 100 thousand stars in a sphere about 100 light-years in diameter.

The apparent magnitude of the cluster is 5.4, so it can be seen with the unaided eye. However this depends on good viewing conditions with a minimum of light pollution. With binoculars it can be seen to cover an area three quarters the size of the full moon. It lies 1.5 degrees east of 5th magnitude Omega Pavonis. The nearest bright star is Peacock, which lies 3.25 degrees north and 9.25 degrees east.

Six X-ray sources have been identified in the cluster's core by the Chandra X-Ray Observatory.