V4    We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V25   We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V44   We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V88   We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V90   We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V91   We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V271  We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V272  We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V273  We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V276  We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
NV340 We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
NV341 We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
NV349 We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
NV350 We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
NV352 We estimate the pulsation parameters neglecting either the danish95 and/or the danish98 and/or the danish99 data sets, since they are noisy
V5    We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V9    We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V11   We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V56   We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V67   We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V69   We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V74   We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V106  We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V112  We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V115  We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V120  We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V130  We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V140  We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V141  We confirm the Blazhko modulations suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and Weldrake et al. 2007 (Cat. J/AJ/133/1447) and provide preliminary estimates of B- and/or V-band Blazhko amplitudes (see Table3)
V10   There is mild evidence of a period change
V24   There is mild evidence of a period change
V32   There is mild evidence of a period change
V47   There is mild evidence of a period change
V58   There is mild evidence of a period change
V64   There is mild evidence of a period change
V70   There is mild evidence of a period change
V71   There is mild evidence of a period change
V77   There is mild evidence of a period change
V81   There is mild evidence of a period change
V82   There is mild evidence of a period change
V87   There is mild evidence of a period change
V89   There is mild evidence of a period change
V95   There is mild evidence of a period change
V123  There is mild evidence of a period change
V124  There is mild evidence of a period change
V126  There is mild evidence of a period change
V131  There is mild evidence of a period change
V136  There is mild evidence of a period change
V145  There is mild evidence of a period change
V147  There is mild evidence of a period change
V153  There is mild evidence of a period change
V155  There is mild evidence of a period change
V156  There is mild evidence of a period change
V157  There is mild evidence of a period change
V158  There is mild evidence of a period change
V166  There is mild evidence of a period change
V270  There is mild evidence of a period change
V275  There is mild evidence of a period change
V289  There is mild evidence of a period change
NV340 There is mild evidence of a period change
NV346 There is mild evidence of a period change
NV347 There is mild evidence of a period change
NV353 There is mild evidence of a period change
NV354 There is mild evidence of a period change
V11   There is evidence that these variables might be affected by a phase shift. Owing to these variations, the B- and V-band mean magnitudes and amplitudes are based either on the danish95 or on the OGLE data set
V94   There is evidence that these variables might be affected by a phase shift. Owing to these variations, the B- and V-band mean magnitudes and amplitudes are based either on the danish95 or on the OGLE data set
V22   The current photometry suggests that these objects are new candidate Blazhko variables. The current data do not allow us to support the multi-modality for V261, suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and/or possible variations in the pulsation period. The variables V280 and V291 sow also evidence for a secondary modulations and/or for a phase shift
V30   The current photometry suggests that these objects are new candidate Blazhko variables. The current data do not allow us to support the multi-modality for V261, suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and/or possible variations in the pulsation period. The variables V280 and V291 sow also evidence for a secondary modulations and/or for a phase shift
V32   The current photometry suggests that these objects are new candidate Blazhko variables. The current data do not allow us to support the multi-modality for V261, suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and/or possible variations in the pulsation period. The variables V280 and V291 sow also evidence for a secondary modulations and/or for a phase shift
V94   The current photometry suggests that these objects are new candidate Blazhko variables. The current data do not allow us to support the multi-modality for V261, suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and/or possible variations in the pulsation period. The variables V280 and V291 sow also evidence for a secondary modulations and/or for a phase shift
V261  The current photometry suggests that these objects are new candidate Blazhko variables. The current data do not allow us to support the multi-modality for V261, suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and/or possible variations in the pulsation period. The variables V280 and V291 sow also evidence for a secondary modulations and/or for a phase shift
V275  The current photometry suggests that these objects are new candidate Blazhko variables. The current data do not allow us to support the multi-modality for V261, suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and/or possible variations in the pulsation period. The variables V280 and V291 sow also evidence for a secondary modulations and/or for a phase shift
V280  The current photometry suggests that these objects are new candidate Blazhko variables. The current data do not allow us to support the multi-modality for V261, suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and/or possible variations in the pulsation period. The variables V280 and V291 sow also evidence for a secondary modulations and/or for a phase shift
V291  The current photometry suggests that these objects are new candidate Blazhko variables. The current data do not allow us to support the multi-modality for V261, suggested by Kaluzny et al. 2004 (Cat. J/A+A/424/1101) and/or possible variations in the pulsation period. The variables V280 and V291 sow also evidence for a secondary modulations and/or for a phase shift
V45   Candidate Blazhko variable according to Kaluzny et al. 2004 (Cat. J/A+A/424/1101). The current light curves, based only on the other data set, are poorly sampled and do not allow us to deduce the occurrence of a Blazhko modulation
V165  Candidate Blazhko variable according to Kaluzny et al. 2004 (Cat. J/A+A/424/1101). The current light curves, based only on the other data set, are poorly sampled and do not allow us to deduce the occurrence of a Blazhko modulation
V52   The pulsation parameters are based on the other data set, since the variable is blended in all Danish data sets. Moreover, according to Navarrete et al. 2015 (Cat. 2015A&A...577A..99N), a neighboring star is located at ~0.5'' from the RRL variable
V55   Period, mean magnitudes and amplitudes are based on photometry by J. Lub and Sturch 1978PASP...90..264S
V59   Candidate Blazhko variables according to Kaluzny et al. 2004 (Cat. J/A+A/424/1101). The current light curves are well sampled, but they do not show evidence of Blazhko modulation. No firm conclusion can be reached on their Blazhko nature
V82   Candidate Blazhko variables according to Kaluzny et al. 2004 (Cat. J/A+A/424/1101). The current light curves are well sampled, but they do not show evidence of Blazhko modulation. No firm conclusion can be reached on their Blazhko nature
V97   Candidate Blazhko variables according to Kaluzny et al. 2004 (Cat. J/A+A/424/1101). The current light curves are well sampled, but they do not show evidence of Blazhko modulation. No firm conclusion can be reached on their Blazhko nature
V68   This is the brightest (V~14.24mag) and the longest-period (0.53476174 days) RRc variable. This is an interesting object worth being investigated in more detail
V73   Candidate Blazhko variable according to Martin 1938AnLei..17B...1M. The current light curves are only based on the other data set. They are poorly sampled and do not allow us to deduce the occurrence of a Blazhko modulation
V80   These stars lie outside the area covered by our images. We only provide a new estimate of the periods from the V+R band light curve by Weldrake et al. 2007 (Cat. J/AJ/133/1447). NV433 is also a candidate field variable and the current data do not allow us to address whether it is an RRL (Weldrake et al. 2007, Cat. J/AJ/133/1447; Navarrete et al. 2015A&A...577A..99N)
V177  These stars lie outside the area covered by our images. We only provide a new estimate of the periods from the V+R band light curve by Weldrake et al. 2007 (Cat. J/AJ/133/1447). NV433 is also a candidate field variable and the current data do not allow us to address whether it is an RRL (Weldrake et al. 2007, Cat. J/AJ/133/1447; Navarrete et al. 2015A&A...577A..99N)
NV411 These stars lie outside the area covered by our images. We only provide a new estimate of the periods from the V+R band light curve by Weldrake et al. 2007 (Cat. J/AJ/133/1447). NV433 is also a candidate field variable and the current data do not allow us to address whether it is an RRL (Weldrake et al. 2007, Cat. J/AJ/133/1447; Navarrete et al. 2015A&A...577A..99N)
NV433 These stars lie outside the area covered by our images. We only provide a new estimate of the periods from the V+R band light curve by Weldrake et al. 2007 (Cat. J/AJ/133/1447). NV433 is also a candidate field variable and the current data do not allow us to address whether it is an RRL (Weldrake et al. 2007, Cat. J/AJ/133/1447; Navarrete et al. 2015A&A...577A..99N)
V84   This star lies outside the area covered by our images. The pulsation parameters are based on Walraven BV-band photoelectric photometry performed by J. Lub, on UBV photoelectric photometry provided by Sturch 1978PASP...90..264S and on OGLE V-band photometry (Kaluzny et al. 1997, Cat. J/A+AS/125/343)
V142  Preliminary results concerning the mode identification of V142 indicate that it is the first radial double-mode pulsator in {omega} Cen. Note that the double-mode variables found by Olech & Moskalik 2009A&A...494L..17O are not F+FO pulsators
V168  This RRL is a candidate field variable (van Leeuwen et al. 2000, Cat. J/A+A/360/472; Bellini et al. 2009, Cat. J/A+A/493/959). On the basis of the current V-band mean magnitude we confirm its non-membership. There is mild evidence of a period change
V172  These stars lie outside the area covered by our images. The period, mean magnitude, amplitude, and epochs of maximum and minimum light have been derived from V photometry by the CATALINA survey (Drake et al. 2009, Cat. J/ApJ/696/870; Drake et al. 2013, Cat. J/ApJ/763/32; Drake et al. 2013, Cat. J/ApJ/765/154; Drake et al. 2014, Cat. J/ApJS/213/9; Torrealba et al. 2015, Cat. /MNRAS/446/2251)
NV457 These stars lie outside the area covered by our images. The period, mean magnitude, amplitude, and epochs of maximum and minimum light have been derived from V photometry by the CATALINA survey (Drake et al. 2009, Cat. J/ApJ/696/870; Drake et al. 2013, Cat. J/ApJ/763/32; Drake et al. 2013, Cat. J/ApJ/765/154; Drake et al. 2014, Cat. J/ApJS/213/9; Torrealba et al. 2015, Cat. /MNRAS/446/2251)
NV458 These stars lie outside the area covered by our images. The period, mean magnitude, amplitude, and epochs of maximum and minimum light have been derived from V photometry by the CATALINA survey (Drake et al. 2009, Cat. J/ApJ/696/870; Drake et al. 2013, Cat. J/ApJ/763/32; Drake et al. 2013, Cat. J/ApJ/765/154; Drake et al. 2014, Cat. J/ApJS/213/9; Torrealba et al. 2015, Cat. /MNRAS/446/2251)
V181  These stars lie outside the area covered by our images. On the basis of their position in the K, J-KCMD, these were classified as candidate field variable stars (Navarrete et al. 2015A&A...577A..99N)
V183  These stars lie outside the area covered by our images. On the basis of their position in the K, J-KCMD, these were classified as candidate field variable stars (Navarrete et al. 2015A&A...577A..99N)
V263  These variables have periods of 1.01215500 and 0.99992364 days and are located on the transition between RR Lyrae (RRLs) and Type II Cepheids (TIICs). The RRL-TIIC transition will be discussed in a forthcoming paper
NV366 These variables have periods of 1.01215500 and 0.99992364 days and are located on the transition between RR Lyrae (RRLs) and Type II Cepheids (TIICs). The RRL-TIIC transition will be discussed in a forthcoming paper
V281  These stars lie outside the area covered by our images. The periods, mean magnitudes, amplitudes, and epochs of maximum and minimum light have been derived from V photometry by OGLE (Kaluzny et al. 1997, Cat. J/A+AS/125/343). V283 is also a candidate field variable
V283  These stars lie outside the area covered by our images. The periods, mean magnitudes, amplitudes, and epochs of maximum and minimum light have been derived from V photometry by OGLE (Kaluzny et al. 1997, Cat. J/A+AS/125/343). V283 is also a candidate field variable
NV351 This variable on our images is heavily blended and we could not derive the mean magnitudes and amplitudes