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Figure 3
Figure 3: CMD for NGC 288 showing evidence of two populations, and models incorporating different metallicities, helium fraction, and age. The best fit model has an age difference of Δ Age = 1.5 Gyr. Image reproduced by permission from Roh et al. [412], copyright by IOP.

Matthew J. Benacquista and Jonathan M. B. Downing, "Relativistic Binaries in Globular Clusters",
Living Rev. Relativity, 16 (2013), 4, doi:10.12942/lrr-2013-4, URL (accessed <date>): http://www.livingreviews.org/lrr-2013-4.
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