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Identifying Multiple Populations in M71 Using CN

  • Authors: Jeffrey M. Gerber, Eileen D. Friel, and Enrico Vesperini

2020 The Astronomical Journal 159 50.

  • Provider: AAS Journals

Caption: Figure 1.

Left Panel: CMD for M71 using B and V photometry from Cudworth (1985 and private communication). Stars shown have an 85% or higher probability of being cluster members based on their proper motions Cudworth (1985 and private communication). Stars in our sample are indicated as large filled circles for RGB, red stars for AGB, and blue squares for HB. Three stars determined to be M giants are shown as green triangles. Stars with Na and/or O measurements are circled (Sneden et al. 1994; Ramírez & Cohen 2002; Carretta et al. 2009a, 2009b; Cordero et al. 2015). Right Panel: CMD for M71 using V photometry from Cudworth (1985 and private communication) and Ks photometry from 2MASS (Skrutskie et al. 2006). Symbols are the same as the left panel.

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