14.88   13.74   12.932   12.367   12.230     16.32       0.02                       -2.10
  NGC 5024-50371                 15.64   14.56   13.35   12.574   11.973   11.878     16.32       0.02                       -2.10
  NGC 5466-9951                  15.90   14.97   13.92   13.092   12.551   12.472     16.02       0.00                       -1.98
  NGC 5466-1344                  15.67   14.67   13.58   12.725   12.153   12.056     16.02       0.00                       -1.98
  NGC 5466-10186                 15.56   14.62   13.55   12.712   12.137   12.107     16.02       0.00                       -1.98
  M3-C41303-2217                 14.86   13.75   12.58   11.698   11.118   10.969     15.07       0.01              -1.37$\pm$0.05
  M13-III-18                     13.94   12.74   11.51   10.601   9.928    9.830      14.33       0.02              -1.43$\pm$0.05
  \[table:phot\]                                                                                          
  ----------------------------- ------- ------- ------- -------- -------- -------- ----------- ---------- ------------------------

Spectroscopic Stellar Parameters {#sec:aspcapref}
--------------------------------

. These models were run with MOOG to compute initial line abundances from EW measurements. Revised values of $\mathrm{T}_{\mathrm{eff}}$ and , and new microturbulence values were found. $\mathrm{T}_{\mathrm{eff}}$ is adjusted in small increments to find the best fit to the [Fe$\;$[Roman[1]{}]{}]{} line abundances when plotted against the excitation potential ($\chi$). Simultaneously the microturbulence is adjusted such that there is no dependence between $\log\epsilon$([Fe$\;$[Roman[1]{}]{}]{}) and the reduced EWs. This process is repeated until the final slopes in [Fe$\;$[Roman[1]{}]{}]{} vs $\chi$ and reduced EW were $<$ 0.004. These spectroscopic parameters are listed in Table \[table:inputParam\] Also included in the table are the derived stellar parameters from the APOGEE Stellar Parameters and Chemical Abundance Pipeline 