I work as part of a collaboration which aims to study the variable stars in Galactic globular clusters. We routinely discover new variables in the crowded central regions of these clusters using difference image analysis (DIA) and we analyse the variable star light curves in order to study the properties of the variables themselves and of the clusters in which they reside. Below I list our variable star discoveries for the clusters that we have studied. The clusters are listed in alpha-numerical order. The information on our own discoveries is up to date as of 01/02/2018. With regards to subsequent discoveries by other investigators, I have not updated this information since 01/02/2018.

• NGC104 (47 Tucanae): Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    EM1 : Semi-regular variable
    EM2 : Semi-regular variable
    EM3 : Semi-regular variable
    EM4 : Semi-regular variable
    EM5 : Long-period irregular variable
    EM6 : Long-period irregular variable
    EM7 : Unclassified
  
  
  • We reclassified WF2-V34 as a long-period irregular variable.
  
  
  • We reclassified LW11 as a semi-regular variable.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC288: Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2013):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We did not discover any new variable stars, although we can be sure that there are no more RR Lyrae stars that are cluster members in the field of view of our study.
  
  
  • Our data are on CDS.

  
  Since our above publication:
  
  

  • Martinazzi et al. (2015) discovered the new variables:
    
    V11 : SX Phe
    V12 : SX Phe
    
    These two variables are of very low amplitude.
  
  
  • Lee et al. (2016) discovered the new variable:
    
    V13 : SX Phe

  
  
  


• NGC1904 (M79): Click for details...
  
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  Our variable star discoveries from Kains et al. (2012):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variable:
    
    V14 : RR1
  
  
  • We classified V7 as a long-period irregular variable.
  
  
  • We speculated that V9 could be a RR01 (double mode) variable.
  
  
  • Our data are on CDS.

  
  Since our above publication:
  
  

  • Kopacki (2015) discovered the new variables:
    
    V15 : RR1
    V16 : SX Phe
    V17 : SX Phe
    V18 : SX Phe
    V19 : Long-period irregular variable
    V20 : Long-period irregular variable
    V21 : Long-period irregular variable
    V22 : Long-period irregular variable
    V23 : Long-period irregular variable
    V24 : Long-period irregular variable
    V25 : Long-period irregular variable
    V26 : Long-period irregular variable
    V27 : Long-period irregular variable
    V28 : Long-period irregular variable
    V29 : SX Phe
    V30 : SX Phe
    V31 : W UMa eclipsing binary
    V32 : Unclassified
    V33 : Long-period irregular variable
    V34 : Long-period irregular variable
    
    A number of these variables are outside the field-of-view of our previous study.
  
  
  • Kopacki (2015) reclassified V7 as a Population II Cepheid (W Virginis).
  
  
  • Kopacki (2015) classified V8 as a semi-regular variable. This star was saturated in our data.

  
  
  


• NGC4147: Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2004):
  
  

  • We used DAOPhot to perform PSF photometry on the CCD images in order to extract the light curves. For the variable star search, we used the version of DanDIA described in Bramich et al. (2005) to perform difference image analysis.
  
  
  • We discovered the new variable:
    
    V18 : Tentatively classified as RR0
  
  
  • We reported that V5 and V15, previously thought to be variable, are in fact non-variable.
  
  
  • We classified V16 as RR1.
  
  
  • Our data are on CDS.

  
  Since our above publication:
  
  

  • Stetson et al. (2005) discovered the new variable:
    
    V19 : RR1
  
  
  • Stetson et al. (2005) found that V18 is non-variable.

  
  
  


• NGC4590 (M68): Click for details...
  
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  Our variable star discoveries from Kains et al. (2015):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V49 : SX Phe
    V50 : SX Phe
    V51 : SX Phe
    V52 : SX Phe
  
  
  • We confirmed the variability of the standard star S28 (Walker 1994) and we assigned the name V53. The type of variability of this star remains unknown.
  
  
  • We confirmed that V40, V41 and V42 are non-variable stars.
  
  
  • We did not detect any variability above the noise in our light curves for the nine stars claimed to be variable by Sariya et al. (2014).
  
  
  • We are sure that there are no more RR Lyrae stars that are cluster members in the field of view of our study.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC5024 (M53): Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2011):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V91 : RR1
    V92 : RR1
    V93 : SX Phe
    V94 : SX Phe
    V95 : SX Phe
    V96 : SX Phe
    V97 : SX Phe
    V98 : SX Phe
    V99 : SX Phe
    V100 : SX Phe
    V101 : SX Phe
    V102 : SX Phe
    V103 : SX Phe
    V104 : SX Phe
    V105 : SX Phe
  
  
  • We reported that V81, V82 and V83, previously thought to be variable, are in fact non-variable.
  
  
  • We announced the variable star candidates S1, S2, S3, S4 and S5.
  
  
  • Our data are on CDS.

  
  Our variable star discoveries from our follow-up paper Arellano Ferro et al. (2012):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We concluded that the rate of incidence of the Blazhko effect in this cluster is at least 37% and 66% for the RR0 and RR1 variables, respectively.
  
  
  • Our data are on CDS.

  
  Since our above publications:
  
  

  • Safonova & Stalin (2011) presented 74 candidate variable stars in NGC5024.

  
  We followed up on the results presented in the Safonova & Stalin (2011) paper. We made the following variable star discoveries in Bramich et al. (2012):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We confirmed the variability and classification of three of the Safonova & Stalin (2011) variable star candidates:
    
    V106 : SX Phe
    V107 : SX Phe
    V108 : SX Phe
  
  
  • We tentatively confirmed the variable nature of the Safonova & Stalin (2011) variable star candidates W11 and SX12.
  
  
  • We discovered the new variable:
    
    V109 : Semi-regular variable
  
  
  • We found that 10 of the Safonova & Stalin (2011) variable star candidates are already known variables and that 54 candidates are false positive detections.
  
  
  • Our data are on CDS.

  
  Since our last publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC5053: Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2010):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We announced the variable star candidates BS4, BS5, BS19, BS22, BS23, BS25, BS28, BS29, BS30, BS31 and NV1.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC5139 (Omega Centauri): Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V457 : Unclassified
    V458 : Long-period irregular variable
    V459 : Long-period irregular variable
  
  
  • Our data are on CDS.

  
  Since our above publication:
  
  

  • Lebzelter & Wood (2016) discovered the new variables:
    
    LW1 : Long-period irregular variable
    LW2 : Long-period irregular variable
    LW3 : Long-period irregular variable
    LW4 : Long-period irregular variable
    LW5 : Long-period irregular variable
    LW6 : Long-period irregular variable
    LW7 : Long-period irregular variable
    LW8 : Long-period irregular variable
    LW9 : Long-period irregular variable
    LW10 : Long-period irregular variable
    LW11 : Long-period irregular variable
    LW12 : Long-period irregular variable
    LW13 : Long-period irregular variable
    LW14 : Long-period irregular variable
    LW15 : Long-period irregular variable
    LW16 : Long-period irregular variable
    LW17 : Long-period irregular variable
    LW18 : Long-period irregular variable
    LW19 : Long-period irregular variable
    LW20 : Long-period irregular variable
    LW21 : Long-period irregular variable
    LW22 : Long-period irregular variable
    LW23 : Long-period irregular variable
    LW24 : Long-period irregular variable
    LW25 : Long-period irregular variable
    LW26 : Long-period irregular variable
    
    All of these variables are outside the field-of-view of our previous study.

  
  
  


• NGC5286: Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V63 : SX Phe
    V64 : RR1
    V65 : RR0
    V66 : Semi-regular variable
    V67 : Semi-regular variable
    V68 : Semi-regular variable
    V69 : Long-period irregular variable
    V70 : Long-period irregular variable
    V71 : Long-period irregular variable
    V72 : Long-period irregular variable
    V73 : Long-period irregular variable
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC5466: Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2008):
  
  

  • We used the version of DanDIA described in Bramich et al. (2005) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V37 : Semi-regular variable
    V38 : Semi-regular variable
  
  
  • We announced the variable star candidates CV1, CV2 and CV3.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC5904 (M5): Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2015):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V170 : SX Phe
    V171 : Semi-regular variable
    V172 : Semi-regular variable
    V173 : Semi-regular variable
    V174 : Semi-regular variable
    V175 : Semi-regular variable
    V176 : Semi-regular variable
    V177 : Semi-regular variable
    V178 : Semi-regular variable
    V179 : Semi-regular variable
    V180 : Semi-regular variable
    V181 : Semi-regular variable
  
  
  • We reported that V23, V46, V48, V49, V51, V124, V136, V138, V140, V143, V144, V145, V146, V147, V148, V149, V150, V151, V152, V153 and V154, previously thought to be variable, are in fact non-variable.
  
  
  • We reclassified V155 as a W UMa eclipsing binary.
  
  
  • Our data are on CDS.

  
  Our variable star discoveries from Arellano Ferro et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We reclassified V104 and V127 as RR0 stars.
  
  
  • We classified V158 as an RR1 star.
  
  
  • Our data are on CDS.

  
  Since our above publications, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6093 (M80): Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V35 : Long-period irregular variable
    V36 : Long-period irregular variable
    V37 : Long-period irregular variable
    V38 : Long-period irregular variable
    V39 : Long-period irregular variable
    V40 : Long-period irregular variable
  
  
  • The star T Scorpii underwent an outburst on May 21st 1860 and consequently it became the first variable star discovered in the field of a globular cluster. We observed the first outburst of this Nova since the 1860 outburst, and therefore we have named this variable as V34. The Nova seems to be a cluster member from its position in the CMD.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6121 (M4): Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We did not discover any new variable stars, although we can be sure that there are no more RR Lyrae stars that are cluster members in the field of view of our study.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6229: Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2015):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V49 : RR0
    V50 : RR0
    V51 : RR0
    V52 : RR0
    V53 : RR0
    V54 : RR0
    V55 : RR0
    V56 : RR0
    V57 : RR0
    V58 : RR0
    V59 : RR1
    V60 : RR1
    V61 : RR1
    V62 : RR1
    V63 : RR1
    V64 : Semi-regular variable
    V65 : Semi-regular variable
    V66 : Semi-regular variable
    V67 : Population II Cepheid (BL Herculis)
    V68 : SX Phe
    V69 : Unclassified
    V70 : Semi-regular variable
    V71 : Semi-regular variable
    V72 : Semi-regular variable
    V73 : Tentatively classified as a Population II Cepheid
  
  
  • We reported that V25, V26 and V28, previously thought to be variable, are in fact non-variable.
  
  
  • We confirmed the variability of V29 and V30, both of which we classified as RR0 variables.
  
  
  • We reclassified V31 and V32 as RR0 variables.
  
  
  • We reclassified V39 and V48 as RR1 variables.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6333 (M9): Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2013):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V22 : RR1
    V23 : RR1
    V24 : W UMa eclipsing binary
    V25 : Algol-type eclipsing binary
    V26 : Long-period irregular variable
    V27 : Long-period irregular variable
    V28 : Long-period irregular variable
    V29 : Long-period irregular variable
    V30 : Long-period irregular variable
    V31 : Long-period irregular variable
    V32 : W UMa eclipsing binary
    V33 : RR0
    V34 : Long-period irregular variable
  
  
  • We reclassified V12 as an anomalous Cepheid pulsating in the fundamental mode and we conjectured that it is a cluster member.
  
  
  • We reclassified V19 as a RR01 (double mode) variable.
  
  
  • We confirmed the W UMa eclipsing binary classification for V21.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6366: Click for details...
  
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  Our variable star discoveries from Arellano Ferro et al. (2008):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V3 : Tentatively classified as an Anomalous Cepheid or a Population II Cepheid (W Virginis)
    V4 : Long-period irregular variable
    V5 : Long-period irregular variable
    V6 : SX Phe
    V7 : Long-period irregular variable
    V8 : Eclipsing binary
  
  
  • We announced the variable star candidates C1, C2, C3, C4, C5, C6, C7, C8, C9, C10 and C11.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6388: Click for details...
  
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  Our variable star discoveries from Skottfelt et al. (2015):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V74 : Tentatively classified as RR1
    V75 : RR1
    V76 : RR0
    V77 : Anomalous Cepheid
    V78 : Semi-regular variable
    V79 : Semi-regular variable
    V80 : RV Tauri
    V81 : Semi-regular variable
    V82 : RV Tauri
    V83 : Semi-regular variable
    V84 : Semi-regular variable
    V85 : Semi-regular variable
    V86 : Semi-regular variable
    V87 : Semi-regular variable
    V88 : Semi-regular variable
    V89 : Semi-regular variable
    V90 : Semi-regular variable
    V91 : Semi-regular variable
    V92 : Semi-regular variable
    V93 : Semi-regular variable
    V94 : Semi-regular variable
    V95 : Semi-regular variable
    V96 : Long-period irregular variable
    V97 : Long-period irregular variable
    V98 : Long-period irregular variable
    V99 : Long-period irregular variable
    V100 : Long-period irregular variable
    V101 : Long-period irregular variable
    V102 : Long-period irregular variable
    V103 : Long-period irregular variable
    V104 : Long-period irregular variable
    V105 : Long-period irregular variable
    V106 : Long-period irregular variable
    V107 : Long-period irregular variable
    V108 : Long-period irregular variable
    V109 : Long-period irregular variable
    V110 : Long-period irregular variable
    V111 : Long-period irregular variable
    V112 : Long-period irregular variable
    V113 : Long-period irregular variable
    V114 : Long-period irregular variable
    V115 : Long-period irregular variable
    V116 : Long-period irregular variable
    V117 : Long-period irregular variable
    V118 : Long-period irregular variable
    V119 : Tentatively classified as a long-period irregular variable
    V120 : Unclassified
    V121 : Unclassified
  
  
  • We classified V29, V63 and V69 as Population II Cepheids (BL Herculis).
  
  
  • We classified V70, V72 and V73 as Population II Cepheids (W Virginis).
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6401: Click for details...
  
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  Our variable star discoveries from Tsapras et al. (2017):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V38 : Long-period variable
    V39 : Long-period variable
    V40 : Long-period variable
    E1 : Eclipsing binary
    LPV2 : Long-period variable
    LPV4 : Long-period variable
    LPV5 : Long-period variable
    LPV6 : Long-period variable
    LPV7 : Long-period variable
    LPV8 : Long-period variable
    LPV9 : Long-period variable
    LPV10 : Long-period variable
    LPV11 : Long-period variable
  
  
  • We reported that V1, V20 and OGLE-BLG-RRLYR-23724, previously thought to be variable, are in fact non-variable.
  
  
  • We classified V3 as a Population II Cepheid (W Virginis).
  
  
  • We classified V8 as RR1.
  
  
  • We classified V10 and V14 as RR0.
  
  
  • We detected double mode pulsations in the RR Lyrae star V12 and identified that at least one of the modes is non-radial.
  
  
  • Our data are on CDS.

  
  Since our above publication:
  
  

  • Soszynski et al. (2016) discovered the new variables:
    
    V41 : Eclipsing binary
    V42 : Ellipsoidal variable
    V43 : Eclipsing binary
    V44 : Ellipsoidal variable
    V45 : Ellipsoidal variable
    V46 : Ellipsoidal variable
    V47 : Ellipsoidal variable
    V48 : Ellipsoidal variable
    V49 : Eclipsing binary
    V50 : Eclipsing binary
    V51 : Ellipsoidal variable
    V52 : Ellipsoidal variable
    V53 : Eclipsing binary
    V54 : Eclipsing binary
    
    These variables are all too faint to have been detected in our data.

  
  
  


• NGC6441: Click for details...
  
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  Our variable star discoveries from Skottfelt et al. (2015):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V151 : RR0
    V152 : Tentatively classified as RR0
    V153 : Population II Cepheid (W Virginis)
    V154 : Population II Cepheid (W Virginis)
    V155 : Unclassified
    V156 : Semi-regular variable
    V157 : Semi-regular variable
    V158 : Semi-regular variable
    V159 : Semi-regular variable
    V160 : Semi-regular variable
    V161 : Semi-regular variable
    V162 : Semi-regular variable
    V163 : Tentatively classified as a semi-regular variable
    V164 : Unclassified
    V165 : Semi-regular variable
    V166 : Semi-regular variable
    V167 : Semi-regular variable
    V168 : Semi-regular variable
    V169 : Long-period irregular variable
    V170 : Long-period irregular variable
    V171 : Long-period irregular variable
    V172 : Long-period irregular variable
    V173 : Long-period irregular variable
    V174 : Long-period irregular variable
    V175 : Long-period irregular variable
    V176 : Long-period irregular variable
    V177 : Long-period irregular variable
    V178 : Long-period irregular variable
    V179 : Long-period irregular variable
    V180 : Long-period irregular variable
    V181 : Long-period irregular variable
    V182 : Long-period irregular variable
    V183 : Long-period irregular variable
    V184 : Long-period irregular variable
    V185 : Long-period irregular variable
    V186 : Long-period irregular variable
    V187 : Long-period irregular variable
    V188 : Long-period irregular variable
    V189 : Long-period irregular variable
    V190 : Long-period irregular variable
    V191 : Long-period irregular variable
    V192 : Long-period irregular variable
    V193 : Long-period irregular variable
    V194 : Long-period irregular variable
    V195 : Long-period irregular variable
    V196 : Long-period irregular variable
    V197 : Long-period irregular variable
    V198 : Long-period irregular variable
    V199 : Long-period irregular variable
  
  
  • We classified V118 as RR0.
  
  
  • We classified V132 as a Population II Cepheid (BL Herculis).
  
  
  • We classified V126, V127, V128 and V129 as Population II Cepheids (W Virginis).
  
  
  • We reclassified V139 as a semi-regular variable.
  
  
  • We reclassified V145 as a RR01 (double mode) variable.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6528: Click for details...
  
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  Our variable star discoveries from Skottfelt et al. (2015):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V1 : RR1
    V2 : Tentatively classified as RR0
    V3 : Long-period irregular variable
    V4 : Long-period irregular variable
    V5 : Long-period irregular variable
    V6 : Long-period irregular variable
    V7 : Tentatively classified as an eclipsing binary
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6541: Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V21 : RR0
    V22 : Long-period irregular variable
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6638: Click for details...
  
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  Our variable star discoveries from Skottfelt et al. (2015):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V64 : RR1
    V65 : RR1
    V66 : RR0
    V67 : RR0
    V68 : RR0
    V69 : Semi-regular variable
    V70 : Semi-regular variable
    V71 : Long-period irregular variable
  
  
  • We classified V25, V26, V27, V30, V31 and V32 as RR0.
  
  
  • We classified V29 and V33 as RR1.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6652: Click for details...
  
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  Our variable star discoveries from Skottfelt et al. (2015):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V13 : Unclassified
    V14 : Eclipsing binary (blue straggler) or field RR1
  
  
  • We detected ~1.1 magniutude variations in the optical light curve of V11.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6656 (M22): Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We did not discover any new variable stars, although we can be sure that there are no more RR Lyrae stars that are cluster members in the field of view of our study.
  
  
  • We observed an outburst of the dwarf nova CV1.
  
  
  • Our data are on CDS.

  
  Since our above publication:
  
  

  • Rozyczka et al. (2017) discovered the new variables:
    
    V102 : SX Phe
    V103 : SX Phe
    V104 : SX Phe
    V105 : SX Phe
    V106 : SX Phe
    V107 : SX Phe
    V108 : SX Phe
    V109 : SX Phe
    V110 : SX Phe
    V111 : SX Phe
    V112 : SX Phe
    V113 : Sinusoidal variable
    V114 : Sinusoidal variable
    V115 : Sinusoidal variable
    V116 : Unclassified
    V117 : Tentatively classified as a W UMa eclipsing binary
    V118 : W UMa eclipsing binary
    V119 : W UMa eclipsing binary
    V120 : W UMa eclipsing binary
    V121 : W UMa eclipsing binary
    V122 : W UMa eclipsing binary
    V123 : Sinusoidal variable
    V124 : Sinusoidal variable
    V125 : Unclassified
    V126 : Sinusoidal variable
    V127 : W UMa eclipsing binary
    V128 : Sinusoidal variable
    V129 : W UMa eclipsing binary
    V130 : Eclipsing binary
    V131 : Algol-type eclipsing binary
    V132 : Unclassified
    V133 : Algol-type eclipsing binary
    V134 : Sinusoidal variable
    V135 : Algol-type eclipsing binary
    V136 : Semi-regular variable
    V137 : Semi-regular variable
    V138 : Semi-regular variable
    V139 : Semi-regular variable
    V140 : Long-period irregular variable

  
  
  


• NGC6681 (M70): Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variable:
    
    V6 : RR1
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6715 (M54): Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V212 : Eclipsing binary
    V213 : RR1
    V214 : RR1
    V215 : RR1
    V216 : RR1
    V217 : RR1
    V218 : RR1
    V219 : RR1
    V220 : RR1
    V221 : RR01 (double mode)
    V222 : Tentatively classified as RR0
    V223 : RR0
    V224 : Tentatively classified as RR0
    V225 : Tentatively classified as RR1
    V226 : Tentatively classified as RR0
    V230 : RR0
    V231 : RR0
    V232 : RR0
    V234 : RR0
    V235 : RR0
    V238 : RR0
    V239 : RR0
    V241 : RR0
    V242 : RR0
    V243 : RR0
    V245 : RR0
    V247 : RR0
    V248 : RR0
    V249 : RR0
    V254 : RR0
    V255 : RR0
    V256 : Population II Cepheid (W Virginis)
    V257 : Semi-regular variable
    V258 : Semi-regular variable
    V259 : Semi-regular variable
    V260 : Long-period irregular variable
    V261 : Long-period irregular variable
    V262 : Long-period irregular variable
    V263 : Long-period irregular variable
    V264 : Long-period irregular variable
    V265 : Long-period irregular variable
    V266 : Long-period irregular variable
    V267 : Long-period irregular variable
    V268 : Long-period irregular variable
    V269 : Long-period irregular variable
    V270 : Long-period irregular variable
    V271 : Long-period irregular variable
    V272 : Long-period irregular variable
    V273 : Long-period irregular variable
    V274 : Long-period irregular variable
    V275 : Long-period irregular variable
    V276 : Long-period irregular variable
    V277 : Long-period irregular variable
    V278 : Long-period irregular variable
    V279 : Long-period irregular variable
    V280 : Long-period irregular variable
    V281 : Unclassified
    V282 : Unclassified
    V283 : Unclassified
    V284 : Unclassified
    V285 : Unclassified
    V286 : Unclassified
    V287 : Unclassified
    V288 : Unclassified
    V289 : Unclassified
    V290 : Unclassified
    V291 : Unclassified
  
  
  • We reclassified V112 as a semi-regular variable.
  
  
  • Montiel & Mighell (2010) presented 33 RR Lyrae star candidates that lie within the field-of-view of our study. We found that 3 of these stars are previously known RR Lyraes, and we confirmed the variable nature of a further 22 candidates. However, we did not detect variability in the remaining 8 candidates.
  
  
  • McDonald et al. (2014) presented 18 variable star candidates that lie within the field-of-view of our study. We confirmed the variable nature of 2 of these candidates, but we did not detect variability in the others.
  
  
  • Our data are on CDS.

  
  Since our above publication:
  
  

  • Hamanowicz et al. (2016) independently discovered the variables V213, V214, V215, V217, V219, V220, V223, V230, V231, V234, V239, V241, V242, V247, V254, V255, V256, V262, V263, V270, V271, V273, V274, V275, V279, V280, V284, V285, V286, V287, V289, V290 and V291.
  
  
  • Hamanowicz et al. (2016) classified some of their independently discovered variables differently to our classifications for the same stars. Specifically, they classified V214, V220, V263, V284, V285 and V289 as RR0 stars. They classified V291 as an RR1 star. They classified V230 as a Population II Cepheid (BL Herculis). Finally, they classified V271, V273, V274, V275, V279, V280, V286 and V287 as semi-regular variables.
  
  
  • Hamanowicz et al. (2016) discovered the new variables V292-V347. Most of these variables are outside the field-of-view of our previous study.
  
  
  • Soszynski et al. (2014; 2016) discovered the new variables V348-V352. All of these variables are outside the field-of-view of our previous study.

  
  
  


• NGC6723: Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We did not discover any new variable stars, although we can be sure that there are no more RR Lyrae stars that are cluster members in the field of view of our study.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6752: Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2016):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We did not discover any new variable stars, although we can be sure that there are no more RR Lyrae stars that are cluster members in the field of view of our study.
  
  
  • We observed an outburst of the dwarf nova V26.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC6981 (M72): Click for details...
  
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  Our variable star discoveries from Bramich et al. (2011):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V43 : RR1
    V44 : Tentatively classified as RR0
    V45 : Tentatively classified as RR0
    V46 : RR1
    V47 : RR0
    V48 : RR0
    V49 : RR0
    V50 : RR0
    V51 : Tentatively classified as RR0
    V52 : RR0 or RR1
    V53 : RR0 or RR1
    V54 : SX Phe
    V55 : SX Phe
    V56 : SX Phe
  
  
  • We reported that V6, V19, V22, V26, V30, V33, V34, V37, V39, V40, V41, S1, S2, S4, S6, R1, R2, R5, R6 and R7, previously thought to be variable, are in fact non-variable.
  
  
  • Our data are on CDS.

  
  Our variable star discoveries from our follow-up paper Skottfelt et al. (2013):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the EMCCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V57 : RR1
    V58 : Unclassified
  
  
  • Our data are on CDS.

  
  Since our above publications:
  
  

  • Amigo et al. (2013) discovered the new variables:
    
    V59 : RR0
    V60 : RR0
    
    These variables are all outside the field-of-view of our previous studies.
  
  
  • Amigo et al. (2013) found that V38 is a non-variable star. We had not been able to study this star because it was close to a brighter saturated star in our data.
  
  
  • Amigo et al. (2013) found that V39 is a field RR0 variable star behind the cluster. We had not detected variability in this star.
  
  
  • Amigo et al. (2013) found that V42 is a variable star but they were unable to classify it. This star was saturated in our data.
  
  
  • Amigo et al. (2013) confirmed our classification of V44 and V51 as RR0 stars.
  
  
  • Amigo et al. (2013) reclassified V45 as an RR1 star. We had tentatively classified this variable as an RR0 star.
  
  
  • Amigo et al. (2013) confirmed our classification of V52 and V53 as RR Lyrae stars and further classified them as RR0 stars.

  
  
  


• NGC7089 (M2): Click for details...
  
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  Our variable star discoveries from Lazaro et al. (2006):
  
  

  • We used the version of DanDIA described in Bramich et al. (2005) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V35 : RR1
    V36 : RR1
    V37 : RR0
    V38 : RR0
    V39 : RR0
    V40 : RR0
    V41 : RR0
    V42 : RR1
  
  
  • Our data are on CDS.

  
  Since our above publication:
  
  

  • Salinas et al. (2016) discovered the new variables:
    
    V43 : RR Lyrae
    V44 : RR Lyrae
    V45 : RR Lyrae
    V46 : RR Lyrae
    V47 : RR Lyrae
    V48 : RR Lyrae
    V49 : Tentatively classified as RR Lyrae
    V50 : RR Lyrae
    V51 : RR Lyrae
    V52 : RR Lyrae
    V53 : RR Lyrae
    V54 : RR Lyrae
    V55 : RR Lyrae
    V56 : SX Phe
    V57 : SX Phe

  
  
  


• NGC7099 (M30): Click for details...
  
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  Our variable star discoveries from Kains et al. (2013):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V14 : RR1
    V16 : RR1
    V17 : Tentatively classified as SX Phe
    V18 : Eclipsing binary (blue straggler)
    V20 : SX Phe
    V21 : Unclassified
  
  
  • We reported that V5, V6, V7, V8, V9, V10, V11, V12 and V13, previously thought to be variable, are in fact non-variable.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.
  
  


• NGC7492: Click for details...
  
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  Our variable star discoveries from Figuera Jaimes et al. (2013):
  
  

  • We used the version of DanDIA described in Bramich (2008) to perform difference image analysis on the CCD images in order to extract the light curves.
  
  
  • We discovered the new variables:
    
    V5 : Long-period irregular variable
    V6 : SX Phe
    V7 : SX Phe
  
  
  • We announced the variable star candidate CSX1 which we tentatively classify as an SX Phe star.
  
  
  • We can be sure that there are no more RR Lyrae stars that are cluster members in the field of view of our study.
  
  
  • Our data are on CDS.

  
  Since our above publication, there has been no new work published in the literature on the variable stars in this cluster.