an estimate of the stellar mass, the surface gravity can be determined.

Optical photometry comes from the Stetson database[^9] and the infrared photometry comes from 2MASS [@b22 see Table \[table:phot\]]. Typical errors for both photometric sources are $\sim0.02$ mag. Reddening values are from the Harris catalogue; typical reddening errors are 10%. Distance moduli are from the Harris catalogue as determined from the horizontal branch magnitude (taken from @b23 for NGC 5024 and from @b24 for NGC 5466). The uncertainty in the distance moduli are 0.1 mag. Input metallicities are taken from the literature: either from direct Fe measurements or from the average cluster metallicity (see Table \[table:phot\]). Assuming the RGB mass is roughly equivalent to the main sequence turnoff (MSTO) mass, an input stellar mass of $0.8M_{\odot}$ is taken from the MSTO of the isochrone fits of NGC 5024/5466 [@b25][^10]. The isochrone with the larger age uncertainty is NGC 5466 ($\sigma = 0.75$ Gyr, reflecting a larger intrinsic scatter in its CMD), resulting in a maximum turnoff mass uncertainty of $\Delta M_\mathrm{{turnoff}}~=~3\%$.

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  ----------------------------- ------- ------- ------- -------- -------- -------- ----------- ---------- ------------------------
                                                                                                          
  (r)[2-7]{} (r)[8-10]{} Star      B       V       I       J        H        K      $(m-M)_V$   $E(B-V)$    Initial \[Fe/H\] (dex)
  NGC 5024-22254                 15.92   