It is about 29,400[4]light years away from Earth and around 6,500 light-years[11] from the Galactic Center. It is roughly the same size and luminosity as its neighbour in space, M69.[12] M70 has a very small core radius of 0.22 ly (0.068 pc)[13] and a half-light radius of 182.0 ly (55.80 pc).[14] This cluster has undergone core collapse, leaving it centrally concentrated[15] with the luminosity distribution following a power law.[11]
There are two distinct stellar populations in the cluster, with each displaying unique abundance abundances. These likely represent different generations of stars.[16] Five known variable stars lie within the broadest radius, the tidal radius, of it, all of which are RR Lyrae variables.[8][17] The cluster may have two blue stragglers near the core.[11]
↑Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin849 (849): 11–14, Bibcode: 1927BHarO.849...11S.
↑Djorgovski, S. (January 1993), "Physical Parameters of Galactic Globular Clusters", in Djorgovski, S. G.; Meylan, G., Structure and Dynamics of Globular Clusters. Proceedings of a Workshop held in Berkeley, California, July 15–17, 1992, to Honor the 65th Birthday of Ivan King, 50, San Francisco, California: Astronomical Society of the Pacific, pp. 373, ISBN978-0937707692, Bibcode: 1993ASPC...50..373D.
↑Forbes, Duncan A. et al. (October 2008), "Uniting old stellar systems: from globular clusters to giant ellipticals", Monthly Notices of the Royal Astronomical Society389 (4): 1924–1936, doi:10.1111/j.1365-2966.2008.13739.x, Bibcode: 2008MNRAS.389.1924F.
↑Pryor, Carlton et al. (August 1989), "Mass-to-light ratios for globular clusters. I - The centrally concentrated clusters NGC 6624, M28 (NGC 6626), and M70 (NGC 6681)", Astronomical Journal98: 596–610, doi:10.1086/115160, Bibcode: 1989AJ.....98..596P.
↑O'Malley, Erin M. et al. (September 2017), "High-resolution Spectroscopic Abundances of Red Giant Branch Stars in NGC 6681", The Astrophysical Journal846 (1): 15, doi:10.3847/1538-4357/aa7b72, 23, Bibcode: 2017ApJ...846...23O.
↑Clement, Christine M. et al. (November 2001), "Variable Stars in Galactic Globular Clusters", The Astronomical Journal122 (5): 2587–2599, doi:10.1086/323719, Bibcode: 2001AJ....122.2587C.
↑On the southernmost line of the main (teapot) asterism; its declination means it will not rise (above the horizon) above the 58th parallel north and will need the observer to be as much as a further fifteen degrees of latitude south for detailed, little distorted observation