The cluster has an apparent magnitude of 9.67 and lies at a distance of 33,600 light years from Earth. It has the designation NGC 4590 in the New General Catalogue.
Messier 68 occupies an area of 11 arc minutes, which corresponds to a spatial diameter of 106 light years. It is easily visible in 10×50 binoculars and best observed in medium or large telescopes.
In binoculars, the cluster appears as a faint patch of light and one needs at least a 4-inch telescope to resolve the brightest stars.
6-inch instruments resolve the cluster’s outer regions and halo, which has an apparent diameter of 12 arc minutes. Large telescopes resolve stars throughout the cluster, including the core.
Messier 68 can be found 3.5 degrees southeast of Kraz, Beta Corvi, one of the stars that form the rectangle of the constellation Corvus. The best time of year to observe the cluster from southern latitudes is during the spring. It stays very low above the southern horizon for northern observers and is not an easy target.
Messier 68 lies in the direction opposite to the galactic centre and may have come from another galaxy, one of the dwarf satellites absorbed by the Milky Way in the distant past. The stars in M68 are very old and metal-poor compared to the typical stars found in the Milky Way. As the cluster is about 11.2 billion years old, the brightest stars have long burned out, leaving only dim, old members. With a density classification of X, M68 is one of the less concentrated globulars.
Messier 68 has a mass of 223,000 solar masses and is probably home to more than 100,000 stars, of which at least 2,000 are visible.
The cluster contains at least 42 variable stars and about 250 giants with an absolute magnitude greater than zero. The clusters Messier 3 and Messier 13 have about twice as many. M68 has an overall spectral type A6 and has 25 stars brighter than magnitude 14.8. The single brightest star in the cluster has a visual magnitude of 12.6. M68 is approaching us at 112 km/s.
Messier 68 was one of Charles Messier’s original discoveries. The French astronomer found the cluster and catalogued it on April 9, 1780. He described it as a “nebula without stars below Corvus & Hydra,” adding that “it is very faint, very difficult to see with the refractors; near it is star of sixth magnitude.”
William Herschel was the first to resolve individual stars in the cluster in 1786. He offered the following description: “A beautiful cluster of stars, extremely rich, and so compressed that most of the stars are blended together; it is near 3′ broad and about 4′ long, but chiefly round, and there are very few scattered stars about.”
John Herschel catalogued the cluster as h 3404 in 1836 and later added it to the General Catalogue as GC 3128. He described M68 as a “globular cluster; irregularly round; gradually brighter toward the middle; diameter in RA = 12…15 sec [3.0 .. 3.75′]. All clearly resolved into stars of 12 m; very loose and ragged at the borders.”
Admiral William Henry Smyth wrongly credited Messier’s friend and colleague Pierre Méchain for the discovery of M68, and a number of sources have picked up the error. Smyth observed the cluster in April 1837 and wrote:
A large round nebula on Hydra‘s body, under Corvus, discovered in 1780 by Méchain. In 1786, Sir William Herschel’s powerful 20-foot reflector resolved it into a rich cluster of small stars, so compressed that most of the components are blended together. It is about 3′ broad, and 4′ long; and he estimated that its profundity may be of the 344th order. It is posited nearly mid-way between two small stars, one in the np [NW] and the other in the sf [SE] quadrant, a line between which would bisect the nebula. It is very pale, but so mottled that a patient scrutiny leads to the inference, that it has assumed a spherical figure in obedience to attractive forces. Differentiated with Beta Corvi, from which it bears south by east, within 3 deg distance.
|Designations: Messier 68, M68, NGC 4590, GCl 20, C 1236-264, HD 110032, MWSC 2059|
|Features: Relatively metal poor|
|Right ascension: 12h 39m 27.98s|
|Distance: 33,600 light years (10,300 parsecs)|
|Age: 11.2 billion years|
|Number of stars: >100,000|
|Apparent magnitude: +9.67|
|Apparent dimensions: 11′|
|Radius: 53 light years|