against the best matching template spectrum from the full grid.

As described in Paper I we also take $BV$ photometry for stars in the field of this cluster from @Kalirai.01, $K_{S}$ photometry from 2MASS [@Skrutskie.06] and we transform our $ri$ photometry to $I_{C}$ using a transformation based on the $I_{C}$ photometry from @Nilakshi.02.

Catalog of Candidate Cluster Members with Measured Rotation Periods
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Selection of Rotational Variables {#sec:rotsel}
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In Paper II we selected 1445 periodic variable stars using the Lomb-Scargle [L-S; @Lomb.76; @Scargle.82; @Press.89; @Press.92], phase-binning analysis of variance [AoV; @Schwarzenberg-Czerny.89; @Devor.05] and box-fitting least squares [BLS; @Kovacs.02] algorithms. From this catalog we will now select a population of probable cluster member, rotational variables. To do this we follow the procedure for selecting candidate photometric cluster members described in Paper I. For each star we determine the $g,r,i,B,V$ point within the fiducial cluster main sequences, generated by eye, that has a minimum $\chi^{2}$ deviation from the observed $g,r,i,B,V$ values for the star. We then select as candidate cluster members stars with $\chi^{2} < 150$ in $g,r,i$ and $\chi^{2} < 250$ in $B,V$ for $B-V < 1.38$ and $V < 20$ or $\chi^{2} < 150$ in $B,V$ for other stars. 