|Right Ascension||18 : 31.4 (h:m)
|Declination||-32 : 21 (deg:m)
|Visual Brightness||7.6 (mag)
|Apparent Dimension||9.8 (arc min)
Discovered 1780 by Charles Messier.
Globular cluster Messier 69 (M69, NGC 6637), similar to its neighbor M70, is one of the smaller and fainter globular clusters in Messier's catalog. It can just be seen in a dark night with a 7x50 or 10x50 pair of binoculars, if the observing location is not too much north. However from Paris, Messier's observing place, it is a difficult object.
M69 was discovered by Charles Messier and added to his catalog on August 31, 1780, the same night he found M70. The discovery occurred when Messier was looking for a nebulous object cataloged by Lacaille in 1751-52 as Lac I.11; he had already looked for that object in vain in 1764. Messier thought he had recovered Lacaille's object and identified M69 with Lac I.11 (NGC 6634), but this is probably a misidentification, as Glen Cozens of Australia has pointed out:
M69's spectral type has been determined as G2 or G3, and its color index is B-V = 1.01. It is one of the metal-richest globulars, meaning that its stars show a relatively high abundance of elements heavier than Helium. Nevertheless, this value is still significantly lower than that for the younger (Population I) stars like our Sun, indicating that even this globular was formed at early cosmic times when the universe contained less heavier elements, as these elements still had to be formed in the stars.
The distance of M69, about 29,700 light years, is roughly the same as that of its apparent neighbor, M70 which is at about 29,400 light years. This indicates that these two globulars happen to be physically neighbored; their mutual distance can be calculated to be as small as about 1,800 light years. In contrast, the also apparently nearby situated globular M54 is about three times as distant.
M69 is poor in variable stars: Shapley found not a single one at all, and the number of known variables is now still as low as 8, 2 of them being Mira-type variable stars with periods of about 200 days.
Last Modification: July 20, 2011