All Figures

$\begin{figure} \par\includegraphics[height=8.5cm,width=8.5cm]{H4299_fig1.eps} \end{figure}$ Figure 1: Composite/cropped frame showing the central (K-band) field of M 3 with the two AO guide stars, S1 and S2, and relevant RR Lyrae stars marked. North (N) and East (E) directions are included.
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In the text

$\begin{figure} \par\includegraphics[height=8.8cm,width=3.7cm,angle=-90]{H4299_fig2.ps} \end{figure}$ Figure 2: Difference between the intensity weighted ensemble average K-band photometry from this work and DG as a function of K-band magnitude. The RR Lyrae stars in common between the two data sets are marked with open circles. The circled outlier may be a false measurement due to stellar crowding.
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In the text

$\begin{figure} \par\includegraphics[height=8.8cm,width=5cm,angle=270]{H4299_fig3.ps} \end{figure}$ Figure 3: $\sigma _{K}$ is plotted as a function of mean $K_{\rm PC1}$ magnitude. Top: stars in common with the DG K-band data with at least two data points. The five known RR Lyrae stars in common are marked with open circles in both plots at $K\sim 15$ ; the circled point at about K=12.4 is an outlier in Fig. 2 and may be a false measurement due to stellar crowding. Bottom: stars in the PC1 region with at least two data points. Nine known variable stars (tabulated in Table 2) are marked with open circles.
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In the text

$\begin{figure} \par\includegraphics[height=6.8cm,width=5.5cm,angle=-90]{H4299_fig4.ps}\end{figure}$ Figure 4: K-band zero point offset assessment. ( $V_{\rm 555}$ , $V_{\rm 555}-K_{\rm PC1}$ ) CMD (squares) where $K_{\rm PC1}$ magnitudes have been shifted to match the lower end of the RGB fiducial ridgeline (dot-dashed/thick) deduced from the work of Ferraro et al. (2002; referred to hereafter as F00) taking a distance modulus of 15.0. The Cohen et al. (1978; referred to hereafter as C78) giant branch data (asterisks and diamonds) has been considered for the purpose of zero point validation; taking the C78 data as comprising asymptotic giant branch (AGB) stars at V > 13.5, the 2nd order polynomial/least squares fit to the C78 data (excluding the outliers (diamonds) falls within $\pm$ 0.05 mag of the apparent AGB stars in the K $_{\rm PC1}$ data. A $\pm$ 0.1 K-band magnitude envelope (dotted) has been included for convenience. See the final paragraph of Sect. 2.1 for more information.
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In the text

$\begin{figure} \par\includegraphics[height=14cm,width=15cm,angle=-90]{H4299_fig5.ps} \end{figure}$ Figure 5: Linear least squares fit to the K-band magnitude / period data (solid). The dotted lines form the 1 $\sigma$ envelope of the linear least squares fit to the data. Coefficient errors of the general relation a Log $P_{\rm o} + b$ , arising from the line fitting are given in parentheses. Top-left: diamonds and triangles mark the RRab- and RRc-type RR Lyrae stars respectively. Top-right: DG data shifted by -0.1 mag to match the $K_{\rm PC1}$ data (zero pointed to match C78), with no J96 offset applied as the epoch is unavailable. The open square marks an outlying star; it is V215 (K=15.87 mag in the DG data and is not in the $K_{\rm PC1}$ data). Bottom: outer region data. Z = 0.0003, 0.0007, 0.0011 and 0.0015 tracks are overlaid (from upper to lower tracks). Data points marked with open circles are the Blazhko (irregular) stars and one RRd-type RR Lyrae star. See text in Sect. 2.3 for further information.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,width=8.5cm]{H4299_fig1.eps} \end{figure}$	Figure 1: Composite/cropped frame showing the central (K-band) field of M 3 with the two AO guide stars, S1 and S2, and relevant RR Lyrae stars marked. North (N) and East (E) directions are included.
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$\begin{figure} \par\includegraphics[height=8.8cm,width=3.7cm,angle=-90]{H4299_fig2.ps} \end{figure}$	Figure 2: Difference between the intensity weighted ensemble average K-band photometry from this work and DG as a function of K-band magnitude. The RR Lyrae stars in common between the two data sets are marked with open circles. The circled outlier may be a false measurement due to stellar crowding.
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