This cluster is about 12.67[8] billion years old with two distinct stellar populations; the second generation is only around 10 million years younger than the first.[3] It lies approximately 13 kly (4 kpc) from theGalactic Center and 1.6 kly (0.5 kpc) from thegalactic plane.[11] The orbital motion of this cluster through theMilky Way suggests it is a member of thebulge ordisk population.[12] It is relatively metal-rich for an object of this class,[3] having ametallicity of –0.70.[8] The core radius is49.8″[3] and thetidal radius is10.5″.[7]
^abShapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters",Harvard College Observatory Bulletin,849 (849):11–14,Bibcode:1927BHarO.849...11S.
^abcdeLibralato, Mattia; et al. (March 2019), "The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. XVIII. Proper-motion Kinematics of Multiple Stellar Populations in the Core Regions of NGC 6352",The Astrophysical Journal,873 (2): 12,arXiv:1902.02787,Bibcode:2019ApJ...873..109L,doi:10.3847/1538-4357/ab0551,S2CID119222605, 109.
^abJohnston, H. M.; et al. (May 1996), "ROSAT observations of ten globular clusters with large core radii.",Astronomy and Astrophysics,309:116–122,Bibcode:1996A&A...309..116J.
^Fullton, L. K.; et al. (August 1995), "A VIC Color-Magnitude Diagram of the Globular Cluster NGC 6352 From Hubble Space Telescope Planetary Camera Observations",Astronomical Journal,110: 652,Bibcode:1995AJ....110..652F,doi:10.1086/117552.
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