V01  V1, V8, V10, V20, V86; these stars located around the cluster RGB tip are 
V01   classified as LPVs. They are saturated in all the HST frames and in the 
V01   Subaru 180s long exposures. Only the TNG and Subaru frames with texp=30s 
V01   were used to derive their light curves and pulsation properties.
V02  this RRab is about 1mag brighter than the HB, and being at the center of 
V02   the cluster it is likely contaminated by companion stars which also may 
V02   cause the bumpy light curves from 0.2 to 0.6 in phase.
V08  V1, V8, V10, V20, V86; these stars located around the cluster RGB tip are 
V08   classified as LPVs. They are saturated in all the HST frames and in the 
V08   Subaru 180s long exposures. Only the TNG and Subaru frames with texp=30s 
V08   were used to derive their light curves and pulsation properties.
V10  V1, V8, V10, V20, V86; these stars located around the cluster RGB tip are 
V10   classified as LPVs. They are saturated in all the HST frames and in the 
V10   Subaru 180s long exposures. Only the TNG and Subaru frames with texp=30s 
V10   were used to derive their light curves and pulsation properties.
V20  V1, V8, V10, V20, V86; these stars located around the cluster RGB tip are 
V20   classified as LPVs. They are saturated in all the HST frames and in the 
V20   Subaru 180s long exposures. Only the TNG and Subaru frames with texp=30s 
V20   were used to derive their light curves and pulsation properties.
V27  data from the TNG set are very scattered. The Fourier analysis gives 
V27   several aliases which makes it difficult to define the period. The star 
V27   was also observed by Baade (1935ApJ....82..396B). The three sets of data 
V27   (this paper, Baade, and PR, Pinto & Rosini, 1977A&AS...28..427P) are not 
V27   phased by the same period, probably because the period changed from 
V27   P=0.35184-days by Baade, to P=0.34896-days by PR, to the value 
V27   P=0.34519-days inferred from our data.
V37  there is a shift in magnitude between Subaru and TNG light curves; we used 
V37   both data sets to define the period, but only the Subaru data to derive 
V37   mean magnitudes and amplitudes.
V39  double-mode RR Lyrae star with period ratio P1/P0=0.745. In Table 2, we 
V39   report the pulsation characteristics of the first-overtone (FO) pulsation;
V39   the pulsation characteristics of the fundamental mode are P_F_=0.54621d, 
V39   A_V_=0.347mag, A_B_=0.454mag, and A_I_=0.305mag.
V44  this star is very bright and is saturated in the HST frames and in the 
V44   Subaru 180s exposures; only the TNG images and the Subaru frames with 
V44   texp=30s could be used to derive its pulsation properties. The star has 
V44   P~0.9-days and rather small amplitudes. According to the position on the 
V44   CMD, V44 falls in the region of LPVs.
V45  the star is very close to the cluster center. The Subaru data provide a 
V45   V amplitude larger than do the TNG data. In Table 2, we have reported the 
V45   visual amplitude inferred from the Subaru data; the amplitude of the TNG 
V45   data is A_V_>0.416mag.
V46  the star is in the central part of the cluster and likely contaminated by 
V46   other stars. We have used only the Subaru data because these are less 
V46   scattered than the TNG observations.
V54  the star, classified as first-overtone RR Lyrae, has small amplitudes 
V54   likely because it is contaminated by two companion stars.
V62  the star is contaminated by a very luminous source. The Subaru data are 
V62   not usable and the TNG data are very scattered.
V65  V65, V71, V79, V76; these stars are in the central part of the cluster. 
V65   There are systematic shifts among TNG, Subaru, and HST data sets of the 
V65   four stars likely due to crowding and blending effects. All three data 
V65   sets were used to estimate the periods, but only the Subaru data to 
V65   derive average magnitudes and amplitudes.
V70  there is a shift in magnitude between TNG and Subaru data sets for the 
V70   star. In the present analysis, we used only the TNG data which produce a 
V70   smoother light curve.
V71  V65, V71, V79, V76; these stars are in the central part of the cluster. 
V71   There are systematic shifts among TNG, Subaru, and HST data sets of the 
V71   four stars likely due to crowding and blending effects. All three data 
V71   sets were used to estimate the periods, but only the Subaru data to 
V71   derive average magnitudes and amplitudes.
V76  V65, V71, V79, V76; these stars are in the central part of the cluster. 
V76   There are systematic shifts among TNG, Subaru, and HST data sets of the 
V76   four stars likely due to crowding and blending effects. All three data 
V76   sets were used to estimate the periods, but only the Subaru data to 
V76   derive average magnitudes and amplitudes.
V79  V65, V71, V79, V76; these stars are in the central part of the cluster. 
V79   There are systematic shifts among TNG, Subaru, and HST data sets of the 
V79   four stars likely due to crowding and blending effects. All three data 
V79   sets were used to estimate the periods, but only the Subaru data to 
V79   derive average magnitudes and amplitudes.
V80  the star is near a very bright source. Only the TNG data set was used since
V80   it produced smoother light curves.
V83  the star is in the blue straggler region and is tentatively classified as a
V83   SX Phoenicis variable. However, with a period of about 0.14-days it 
V83   significantly deviates from the SX Phe period-luminosity (PL) relation 
V83   (see Figure 13).
V86  V1, V8, V10, V20, V86; these stars located around the cluster RGB tip are 
V86   classified as LPVs. They are saturated in all the HST frames and in the 
V86   Subaru 180s long exposures. Only the TNG and Subaru frames with texp=30s 
V86   were used to derive their light curves and pulsation properties.
V87  binary system. In Table 2, we list the most probable period inferred for 
V87   the star by the Lomb periodogram since it gives less scatter than the 
V87   period inferred from the Fourier analysis (P=0.184716-days, A_V_=1.199mag,
V87   A_B_=0.166mag, and A_V_>0.265mag).
V89  the star has very small amplitudes for a c-type RR Lyrae. It lies very 
V89   close to the edge of the frames and this may partially explain the 
V89   anomalous amplitudes.