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10 × 10 arcmin 2 gray-scale map of an R reference image of the globular cluster M53. Sixteen confirmed SX Phe stars are labeled by their respective designations given in Table 6. The image was scaled so that to only mark the positions of the stars. The cross marks the center of the cluster. The cluster size is ∼ 13 , thus we can be confident that most detected variables belong to the cluster. North is up, east to the left. 

10 × 10 arcmin 2 gray-scale map of an R reference image of the globular cluster M53. Sixteen confirmed SX Phe stars are labeled by their respective designations given in Table 6. The image was scaled so that to only mark the positions of the stars. The cross marks the center of the cluster. The cluster size is ∼ 13 , thus we can be confident that most detected variables belong to the cluster. North is up, east to the left. 

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Figure 1. 10 × 10 arcmin 2 gray-scale map of an R reference image of...
Figure 2. Top panel: changes of the FWHM of four Stetson's (2001)...
Table 2 Equatorial Coordinates (α, δ) of known Variables V61-V70
Figure 3. 7 
+15 Table 3 Revised Periods for Previously known Short-period Variables in M53
A photometric survey for short-periodic variables in globular clusters NGC5024
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  • Jan 2011
We are presenting the results of a commissioning campaign to observe Galactic globular clusters for the search of microlensing events. We have observed the cluster NGC5024 in March 2010. Light curves were obtained for 9,600 stars, out of which we identified 60 known variables and revised periods of some of short-periodic variables. We identify abou...
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Context 1
... gray-scale map of an R CCD image (reference frame, RF) is shown in Figure 1. It shows an area of about 5. 5 × 5. 5 of the total observed field. ...
Context 2
... SX7, SX20, SX12, SX13, SX15, and SX23 located to the right and below the fundamental P − L line, though undoubtedly variable (see their light curves in Figure 10), are most probably not SX Phe type. However, since their periods exceed 0.1 days, we cannot truly determine their nature. ...
Context 3
... thus confirm SX Phe-type fundamental mode pulsations for 10 new variables (namely, SX2, SX3, SX4, SX8, SX10, SX11, SX14, SX21, SX22, SX25) and probable higher pulsation mode for 5 new variables: SX6, SX9_1, SX16, SX17, and SX24. The phase and time-domain light curves of all 21 stars are shown in Figure 10 and their parameters are given in Table 6. The positions of 15 confirmed SX Phe stars on the CCD image are given in Figure 1. ...
Context 4
... phase and time-domain light curves of all 21 stars are shown in Figure 10 and their parameters are given in Table 6. The positions of 15 confirmed SX Phe stars on the CCD image are given in Figure 1. ...
Context 5
... tentatively classify the variable candidates with a charac- teristic shape of a light curve as RR Lyrae variables (Clement et al. 2001). The light curves of these 14 RR Lyrae candidates are shown in Figure 11. The equatorial coordinates (α, δ) of these stars, mean brightness in R, and a possible variability type are given in Table 7. ...
Context 6
... each star we provide designation, equatorial coordinates (α, δ), mean brightness in R, rough estimate of the period, range of variability Δr, epoch of light-minimum T = JD − 2, 455, 280 and in the Notes we present a possible variability type or BSS match. The phase and time-domain curves are presented in Figure 12. ...
Context 7
... have found 27 more stars that show definite light variations, but which are also impossible to classify due to the short span of our observations and their possible long periods and irregular nature. Their variability, however, is undoubtful judging from their light curves ( Figure 13). The equatorial coordinates and standard R magnitudes of these variables are presented in Table 9. ...