Messier 62 or M62, also known as NGC 6266, is a globular cluster of stars in the equatorialconstellation of Ophiuchus. It was discovered on June 7, 1771 by Charles Messier, then added to his catalogue in 1779. M62 is at a distance of about from Earth and from the Galactic center. It is among the ten most massive and luminous globular clusters in the Milky Way, showing an integrated absolute magnitude of –9.18. The cluster has an estimated mass of and a mass-to-light ratio of in the V band. It has a projected ellipticity of 0.01, meaning is it essentially spherical. The density profile of the cluster members suggests it has not yet undergone core collapse. It has a core radius of, a half-mass radius of, and a half-light radius of. The stellar density at the core is per cubic parsec. It has a tidal radius of. The cluster shows at least two distinct populations of stars, which most likely represent two separate episodes of star formation. Of the main sequence stars in the cluster, are from the first generation and from the second. The second generation is polluted by materials released by the first. In particular, the abundances of helium, carbon, magnesium, aluminium, and sodium differ between the two populations. Indications are this is an Oosterhoff type I, or "metal-rich" system. A 2010 study identified 245 variable stars in the cluster's field, of which 209 are RR Lyrae variables, four are Type II Cepheids, 25 are long period variables, and one is an eclipsing binary. The cluster may prove to be the galaxy's richest in terms of RR Lyrae variables. It has six binary millisecond pulsars, including one that is displaying eclipsing behavior from gas streaming off its companion. There are multiple X-ray sources, including 50 within the half-mass radius. 47 blue straggler candidates have been identified, formed from the merger of two stars in a binary system, and these are preferentially concentrated near the core region. It is hypothesized that this cluster may be host to an intermediate mass black hole, and it is considered particularly suitable for searching for such an object. Examination of the proper motion of stars within of the core does not require an IMBH to explain. However, simulations can not rule out an IMBH with a mass of a few thousand. Based upon radial velocity measurements within an arcsecond of the core, Kiselev et al. made the claim that there is an IMBH with a mass in the range.
