\begin{table}%t3 \caption{\label{table-Prot}Photometric periods and ancillary data are presented, resulting from the light-curve analysis of variable stars detected in the Lowell M~34 fields.} \par %\centering { \begin{tabular}{lrrrrl} \hline\hline \noalign{\smallskip} Internal\tablefootmark{a} ~~ & Data\tablefootmark{b} & Sigma Clipped\tablefootmark{c} & Period & $B-V_{o}$\tablefootmark{d} & Mem\tablefootmark{e} \\ Identifier & Epochs & StdDev [mag] & [days] & & \\ \hline F3\_0172-lIlVsV & 53/54/59 & 0.00883/0.01010/0.01190 & $ 8.0 \pm 1.0 $ & 0.811 & Y;Ys \\ F3\_0176-lIlVsIsV & 53/54/58/59 & 0.04275/0.06460/0.04313/0.06427 & $ 2.780 \pm 0.005$ & 0.818 & Y;Ys \\ F3\_0215-lIlVsIsV & 52/54/58/59 & 0.01121/0.01722/0.01439/0.02020 & $ 7.47 \pm 0.11 $ & 0.874 & Y;Ys \\ F3\_0258-lIlVsV & 53/54/58 & 0.01182/0.01250/0.01457 & $11.0 \pm 1.0 $ & 0.947 & Y;Ys \\ F3\_0306-lIsIsV & 53/58/59 & 0.01886/0.01809/0.02081 & $1.1435 \pm 0.0007$ & 0.991 & Y;Yb \\ F3\_0320-lIlVsV & 52/54/58 & 0.00898/0.01023/0.01430 & $ 8.511 \pm 0.001 $ & 1.046 & Y; \\ F3\_0383-lIlV & 52/54 & 0.00776/0.00937 & $ 9.5 \pm 0.4 $ & 1.160 & Y;Ys \\ F3\_0430-lV & 54 & 0.01253 & $10.5 \pm 1.0 $ & 1.239 & Y;Ys \\ F3\_0469-lIlVsIsV & 52/54/57/57 & 0.01344/0.01745/0.01768/0.02225 & $12.9 \pm 0.3 $ & 1.283 & Y; \\ F3\_0485-lIlV & 52/54 & 0.01040/0.01393 & $12.0 \pm 1.0 $ & 1.285 & Y; \\ F3\_0487-lIlV & 53/54 & 0.01076/0.01388 & $ 8.4 \pm 0.6 $ & 1.278 & Y; \\ F3\_0600-lIlV & 53/54 & 0.01263/0.02503 & $ 7.44 \pm 0.05 $ & 1.452 & Y; \\ F3\_0664-lI & 52 & 0.01077 & $10.5 \pm 1.0 $ & 1.441 & Y; \\ F4\_0136-sIsV & 60/60 & 0.01457/0.01794 & $ 2.87 \pm 0.03 $ & 0.544 & Y;Ys \\ F4\_0169-lIlVsIsV & 55/42/60/59 & 0.01275/0.01297/0.01094/0.01429 & $ 3.81 \pm 0.08 $ & 0.598 & Y;Ys \\ F4\_0194-sIsV & 60/60 & 0.00817/0.00889 & $ 2.20 \pm 0.03 $ & 0.652 & Y;Ys \\ F4\_0234-lIlVsV & 54/55/60 & 0.00692/0.00984/0.01014 & $ 5.56 \pm 0.07 $ & 0.698 & Y;Ys \\ F4\_0303-lIlVsIsV & 55/55/60/60 & 0.00800/0.00941/0.00839/0.00978 & $ 7.4 \pm 0.3 $ & 0.767 & Y;Ys \\ F4\_0317-lIlVsIsV & 55/55/59/60 & 0.01701/0.02159/0.01698/0.02167 & $ 6.8 \pm 0.1 $ & 0.805 & Y;Ys \\ F4\_0327-lVsV & 55/60 & 0.01471/0.01406 & $ 7.6 \pm 1.1 $ & 0.813 & Y;Ys \\ F4\_0335-lIlVsIsV & 55/55/60/60 & 0.01538/0.01953/0.01601/0.02032 & $ 0.89 \pm 0.02 $ & 0.790 & Y;Yb \\ F4\_0450-lIlVsIsV & 54/55/60/60 & 0.00985/0.01181/0.01264/0.01368 & $ 8.00 \pm 0.21 $ & 0.895 & Y;Ys \\ F4\_0667-lIlVsV & 54/55/59 & 0.01122/0.01819/0.02028 & $ 7.97 \pm 0.05 $ & 1.030 & Y;Yb \\ F4\_0695-lI & 54 & 0.00748 & $ 4.3 \pm 0.5 $ & 1.086 & Y;Ys \\ F4\_0730-lIlVsIsV & 55/55/60/59 & 0.02944/0.04619/0.03109/0.04695 & $ 8.41 \pm 0.10 $ & 1.051 & Y; \\ F4\_0736-lIlVsIsV & 55/55/60/60 & 0.01875/0.02715/0.02022/0.02911 & $ 0.786 \pm 0.001$ & 1.008 & Y;Yb \\ F4\_0803-lVsI & 55/60 & 0.01435/0.01416 & $12.6 \pm 0.7 $ & 1.164 & Y;Ys \\ F4\_0804-lIlVsIsV & 55/55/60/60 & 0.02568/0.04152/0.02448/0.04239 & $ 4.95 \pm 0.04 $ & 1.106 & Y; \\ F4\_0852-lIlVsIsV & 55/55/59/60 & 0.01547/0.02368/0.01624/0.02564 & $0.879 \pm 0.002$ & 1.155 & Y;Yb \\ F4\_0942-lIlVsV & 54/55/60 & 0.00942/0.01300/0.02362 & $ 9.4 \pm 0.3 $ & 1.198 & Y; \\ F4\_1007-lIlV & 55/55 & 0.00774/0.01177 & $15 \pm 2 $ & 1.440 & Y; \\ F4\_1020-lIlVsIsV & 55/55/60/59 & 0.01344/0.01846/0.01568/0.02528 & $ 8.6 \pm 0.4 $ & 1.260 & Y; \\ F4\_1055-lIlVsIsV & 55/55/60/60 & 0.01427/0.02542/0.02233/0.02664 & $ 6.80 \pm 0.15 $ & 1.272 & Y; \\ F4\_1147-lV & 55 & 0.01883 & $ 0.589 \pm 0.001 $ & 1.336 & Y; \\ F4\_1315-lIlV & 54/54 & 0.01429/0.01913 & $12.2 \pm 0.5 $ & 1.371 & Y; \\ F4\_1357-lIlV & 55/55 & 0.01197/0.01973 & $ 9.4 \pm 0.2 $ & 1.380 & Y; \\ F4\_1369-lIlV & 53/53 & 0.01886/0.02578 & $11.85 \pm 0.13 $ & 1.443 & Y; \\ F4\_1392-lIlV & 55/55 & 0.01496/0.02385 & $ 6.5 \pm 0.5 $ & 1.434 & Y; \\ F4\_1566-lIlV & 55/54 & 0.01920/0.03248 & $11.2 \pm 0.1 $ & 1.479 & Y; \\ F4\_1617-lV & 52 & 0.03379 & $ 7.3 \pm 0.5 $ & 1.500 & Y; \\ F4\_1793-lIlV & 55/53 & 0.02221/0.04966 & $ 7.5 \pm 0.6 $ & 1.323 & Y; \\ F4\_1925-lV$^{f}$ & 44 & 0.09210 & $12.7 \pm 2.0 $ & 1.507 & Y; \\ F4\_2226-lI$^{f}$ & 55 & 0.02681 & $ 6.0 \pm 0.5 $ & 1.555 & Y; \\ \hline F3\_0071-sIsV & 58/59 & 0.02052/0.02502 & $ 3.014 \pm 0.008 $ & 0.977 & N; \\ F3\_0121-lVsV & 54/59 & 0.00851/0.00881 & $ 8.4 \pm 0.2 $ & 1.178 & N; \\ F3\_0163-lIsIsV & 53/58/59 & 0.00814/0.00943/0.00935 & $14 \pm 2 $ & 0.830 & Y;N \\ F3\_0165-lI & 52 & 0.01089 & $12 \pm 1 $ & 0.795 & Y;N \\ F3\_0388-lIlVsIsV & 53/54/58/59 & 0.01534/0.02141/0.01715/0.02448 & $11.59 \pm 0.01 $ & 0.905 & N; \\ F3\_0413-lIlVsIsV & 53/54/58/59 & 0.01640/0.02417/0.01909/0.02982 & $ 5.45 \pm 0.08 $ & 1.073 & Y;N \\ F3\_0437-lIlVsV & 53/54/59 & 0.00859/0.01134/0.01563 & $ 9.7 \pm 0.4 $ & 0.577 & N; \\ F3\_0692-lIlV & 53/54 & 0.01886/0.02686 & $ 0.3368 \pm 0.0001$ & 0.787 & N; \\ F3\_2310-lIlV & 52/54 & 0.02667/0.02846 & $ 2.991 \pm 0.008 $ & - - - & \\ F4\_0167-lIlVsI & 54/55/59 & 0.01321/0.01091/0.00961 & $ 9.2 \pm 0.9 $ & 0.868 & N; \\ F4\_0404-lIlVsV & 55/55/60 & 0.01099/0.01419/0.01461 & $ 6.6 \pm 0.3 $ & 0.782 & Y;N \\ F4\_0515-lIlVsV & 55/55/60 & 0.00886/0.00957/0.01239 & $ 8.2 \pm 0.1 $ & 0.833 & N; \\ \hline \end{tabular}} \tablefoot {\tablefoottext{a}{Internal Identifiers are the same as those detailed in Table~\ref{table-identifier}. Designations indicating exposure time and filter choice for a given light-curve are annotated. For instance, {lI} represents {\em long-I}, for light-curves derived from long exposures in the $I$-filter. Thus, {lIlVsIsV} represents four independent light-curves created from image sequences of 400~s, $I$-filter; 600~s, $V$-filter; 40~s, $I$-filter and 60~s, $V$-filter, respectively (namely, long-I, long-V, short-I \& short-V).}\\ \tablefoottext{b}{Number of photometric data points in each light-curve, derived from each target's image series, in a given filter and exposure time sequence.} \\ \tablefoottext{c}{For each target's light-curve, in a filter+exposure combination, standard deviations of the differential magnitudes are provided. The time series files for each target were sigma-clipped to eliminate outliers. A $\Delta$-magnitude for each light-curve can be determined by multiplying these standard deviations by~2$\sqrt2$ (strictly speaking this is only true for perfectly sinusoidal variations).} \\ \tablefoottext{d}{$E_{B-V}$~= 0.07 is adopted; Canterna et~al. (\cite{Cant79}).} \\ \tablefoottext{e}{Abridged cluster membership criteria are reproduced from Table~\ref{table-identifier}, with format Photometric; Kinematic (s-single, b-binary).} \\ \tablefoottext{f}{$B-V$ colours are determined using a field star $V-I$ to $B-V$ relationship (Caldwell et~al. \cite{Cald93}), assuming $E_{V-I}$~$=$ $1.25$~$\times$ $E_{B-V}$, and $E_{B-V}$~=~0.07.}} \end{table}