C0021m723 |V1-28: The RA and dec are from Samus et al. (2009). C0021m723 | For the stars classified as M, SR or L, the periods, mean C0021m723 | magnitudes and classifications are from Lebzelter et al. (2005) C0021m723 | or from Lebzelter & Wood (2005) and the V amplitudes were derived C0021m723 | from their published light curves, unless indicated otherwise in C0021m723 | the notes on individual stars. "Fox" in the remarks column C0021m723 | indicates the the period is from Fox (1982). "+long" in the C0021m723 | remarks column indicates that a longer period is superimposed C0021m723 | on the published period. C0021m723 | The source for the remaining stars (classified as RR, CST or ?) C0021m723 | are indicated in the Notes on individual stars. C0021m723 |V29-41 (= Edmonds et al. V1-13): C0021m723 | The RA and dec are from Samus et al. (2009) C0021m723 | The periods and magnitudes are from Edmonds et al. (1996) unless C0021m723 | indicated otherwise in the notes on individual stars. C0021m723 | A few of these stars (V32=PC1-V04, V35=PC1-V07, V36=PC1-V08, C0021m723 | V38=PC1-V10, V39=PC1-V11, and V40=PC1-V12) were later C0021m723 | investigated by Albrow et al. (2001). C0021m723 | For these stars, the period, mean magnitude and amplitude are C0021m723 | from Albrow et al. (2001) or from the sources indicated in Notes C0021m723 | on individual stars. C0021m723 | The RA values derived by Albrow et al. (2001) for these stars C0021m723 | have a systematic shift relative to the values of Samus et al. C0021m723 | (2009) which were based on Geffert et al. (1997). C0021m723 | The Samus/Geffert values are larger on average by 0.29 sec than C0021m723 | those derived by Albrow et al. This is equivalent to about C0021m723 | 1.3 arcseconds. C0021m723 |V42-53: C0021m723 | The RA and dec are from Samus et al. (2009). C0021m723 | The periods and magnitudes are from Kaluzny et al. (1998) unless C0021m723 | indicated otherwise in the notes on individual stars. C0021m723 |V54-56: C0021m723 | The RA and dec are from Samus et al. (2009). C0021m723 | The remaining data are from the discovery paper by C0021m723 | Gilliland et al. (1998) C0021m723 |------------ C0021m723 |The variables following V56 have been assigned numbers that have been C0021m723 |designated according to their discovery papers. C0021m723 |"Par" and "Sha" C0021m723 | refer to variables announced by Paresce et al. (1992, 1994) and C0021m723 | by Shara et al. (1996). These stars are discussed further in the C0021m723 | notes on individual stars. C0021m723 |"PC1, WF2, WF3, WF4" C0021m723 | designate the variables discovered by Albrow et al. (2001) when C0021m723 | they used the HST to search for Jupiter-sized planetary transits. C0021m723 | The "W" numbers in the remarks column refer to the Chandra X-ray C0021m723 | sources for which the variable star is the optical counterpart C0021m723 | according to Edmonds et al. (2003a) or Heinke et al. (2005). C0021m723 | The W numbers were assigned to Chandra X-ray sources in 47 Tuc C0021m723 | by Grindlay et al. (2001) and authors of subsequent studies C0021m723 | followed their numbering system. C0021m723 | The data for these variables are from the discovery paper of C0021m723 | Albrow et al. (2001) unless indicated otherwise in the Notes/Remarks C0021m723 | column. E2003 in the Remarks column indicates that the data are C0021m723 | from Edmonds et al. (2003a,b). C0021m723 |"W#_opt" C0021m723 | refers to variables discovered by Edmonds et al. (2001, 2002, C0021m723 | 2003a,b) when they used the HST images of Albrow et al. (2001) C0021m723 | to search for optical counterparts to Chandra X-ray sources. C0021m723 | The data for these stars are from the discovery papers by Edmonds C0021m723 | and collaborators. C0021m723 |"LW" refers to long period variables discovered by Lebzelter & Wood C0021m723 | (2005). The data for A19 and the LW stars are from Lebzelter & C0021m723 | Wood (2005) or from Lebzelter et al. (2005). C0021m723 |"Wel" refers to variables discovered by Weldrake et al. (2004) in C0021m723 | their search for planetary transits. All the data are from their C0021m723 | discovery paper unless indicated otherwise in the notes on C0021m723 | individual stars. C0021m723 |"KalW" and "KalE" C0021m723 | refer to the west and east fields observed by Kaluzny et al. (2013) C0021m723 | in their search for eclipsing binaries. All the data are from C0021m723 | their discovery paper unless indicated otherwise in the Notes on C0021m723 | individual stars. C0021m723 |"EM" refers to the variables discovered by Figuera Jaimes et al. (2016) C0021m723 | based on their observations made with an electron-multiplying (EM) C0021m723 | CCD. All the data are from their discovery paper unless indicated C0021m723 | otherwise in the Notes on individual stars. C0021m723 |---------------------------------- C0021m723 |Cataclysmic variables C0021m723 | A number of variables have been classified as candidate CVs in C0021m723 | investigations of 47 Tuc. This was based on their location in the C0021m723 | CM diagram, their spectroscopic properties and the fact that they C0021m723 | are optical counterparts of X-ray sources. C0021m723 | Two of these stars (V39 and Par-V2) are confirmed CVs because they C0021m723 | have exhibited eruptions on more than one occasion (see the Notes C0021m723 | below). C0021m723 | In the above table, the remaining CV candidates are designated C0021m723 | "CV?" or "E/CV?" if a binary period has been derived. C0021m723 | Michael Shara and his collaborators (2017, private communiction) C0021m723 | have continued to monitor 47 Tuc with HST observations (~50 times C0021m723 | since 1996) and plan to report their latest results in 2017. C0021m723 |-------------------------------------------- C0021m723 |According to the 2010 update to the Harris (1996) catalogue, 47 Tucanae C0021m723 |has a tidal radius of approximately 42 arcminutes. However, 47 Tuc is C0021m723 |located close to the SMC in the sky and as a result, at distances C0021m723 |greater than 20 arcminutes from the cluster centre, there is significant C0021m723 |contamination from the SMC and the Milky Way. This is illustrated in a C0021m723 |paper by Cioni et al. (2016 -see Fig.3). Variables that are clearly C0021m723 |known to be field stars are designated "f" in the above table. C0021m723 |However, for some stars, the membership status may be ambiguous. C0050m268 |The RA and dec for V1 are from Samus et al. (2009) and the remaining C0050m268 |data are from Oosterhoff (1943). C0050m268 |All of the data for V2-V10 are from Kaluzny et al. (1997). Arellano C0050m268 |Ferro et al. (2013) made VI observations of all of these variables and C0050m268 |derived periods and magnitudes comparale to the values of Kaluzny et al. C0050m268 |(1997). C0100m711 |NGC 362 is located near the Small Magellanic Cloud in the sky and as a C0100m711 |result, many SMC stars are included in the field surrounding NGC 362. C0100m711 |It was one of the clusters investigated by Bailey (1902) in his classic C0100m711 |paper on globular cluster variables. C0100m711 |CCD studies of the variables in the field around NGC 362 have been made C0100m711 |by Szekely et al. (2007 = S07), Lebzelter & Wood (2011) and Rozyczka et C0100m711 |al. (2016 = R16). C0100m711 |S07 tabulated data for 84 variables in and around the cluster. Among C0100m711 |these were 15 of the 16 previously known variables. In the above table, C0100m711 |we use the original numbering system of Bailey (1902) and Sawyer Hogg C0100m711 |(1973) for these variables and indicate the Szekely (Sz) numbers in C0100m711 |the remarks column. The new Sz variables that were considered to be C0100m711 |cluster members are listed by their Sz numbers in the table and the C0100m711 |published data for these variables are from S07 unless indicated C0100m711 |otherwise in the Notes/Remarks column. C0100m711 |A discussion of the status of the remaining variables announced by S07 C0100m711 |is given below, at the end of the section on discovery of the variables. C0100m711 |Lebzelter & Wood (2011) studied the long period variables, two C0100m711 |previously known and 10 new discoveries. Their new varables are C0100m711 |designated as LW1-10. C0100m711 |R16 obtained light curves for 151 variables, including 100 new and C0100m711 |4 suspected new variables. Among the "new" variables, 12 (V17-V28) C0100m711 |are proper motion members of the cluster and 4 (VN01-VN04) are likely C0100m711 |members. These 16 stars are all listed in the above table. C0100m711 |The rest were considered to be field variables and are not included. C0100m711 |R16 also published significant new information for some of the C0100m711 |previously known variables. Their new results are included in the C0100m711 |above table. C0100m711 | C0100m711 |In the table, all the data for V17-V28 and VN01-VN04 are from C0100m711 |the discovery paper by Rozyczka et al. (R16). C0100m711 |The data for the LW variables are from the discovery paper by C0100m711 |Lebzelter & Wood (2011) and for the remaining variables, the data C0100m711 |are from Szekely et al. (S07) unless indicated otherwise in the Notes C0100m711 |on individual stars or in the Notes/Remarks column, where R16 C0100m711 |indicates that the data are from Rozyczka et al. (R16). C0310m554 |The RA and dec for V1-21 are from Samus et al. (2009). C0310m554 |The periods, magnitudes, amplitudes and variable types for V2-15 C0310m554 |are from Wehlau & Demers (1977). They also published an ID chart for C0310m554 |these variables. Salinas et al. (2007) confirmed the CST status for V1. C0310m554 |The periods, magnitudes, amplitudes and variable types listed for C0310m554 |V16-21 are from Wehlau et al. (1977, IBVS 1361) - except for V18 and C0310m554 |V19 as indicated in the notes on individual stars. C0310m554 |All the data for V22-30 are from Salinas et al. (2007). C0310m554 |Kravtsov et al. (2010) published UBVI photometry for 5481 stars in a C0310m554 |14 by 14 arcmin field around the cluster. C0325p794 |Variable searches of Pal 1 were carried out by Kinman & Rosino (1962) C0325p794 |and by Ortolani & Rosino (1985). C0325p794 | C0325p794 |A VI color-magnitude diagram by Rosenberg et al. (1998a) does not C0325p794 |indicate any obvious HB stars. Based on this and on the metal C0325p794 |abundance they derived, [Fe/H]=-0.6, (1998, AJ 115, 658), Rosenberg C0325p794 |et al. (1998b) concluded that Palomar 1 is a very young globular cluster. C0325p794 |The young age (as much as 8 Gyr younger than 47 Tuc) was confirmed by C0325p794 |Sarajedini et al. (2007) who also said they could not rule out the C0325p794 |possibility that Palomar 1 has been misclassified as a globular cluster. C0325p794 |An analysis by Monaco et al. (2011) indicated that the chemical C0325p794 |abundance is similar to that of Galactic open clusters. They proposed C0325p794 |that Pal 1 might be a globular cluster that experienced a peculiar C0325p794 |chemical evolution or an open cluster ejected from the Galactic disk. C0325p794 |From a study of tidal tails, Niederste-Ostholt et al. (2010) suggested C0325p794 |that Pal 1 may have been accreted from a now disrupted dwarf galaxy C0325p794 |about 500 Myr ago. C0354m498 |Aaronson et al. (1984) published a BV color-magnitude diagram that C0354m498 |indicates this object is a globular cluster with a prominent red C0354m498 |horizontal branch. A VI color-magnitude diagram by Dotter et al. C0354m498 |(2008) confirms this. Thus it is a "second parameter" cluster" in the C0354m498 |sense that it has a red HB compared with inner halo clusters with the C0354m498 |same metallicity, [Fe/H] = -1.70. The metallicity was derived by C0354m498 |Suntzeff et al. (1985) based on the calcium H and K line strengths of two C0354m498 |giants. C0422m213 |Ortolani & Gratton (1986) published a BV color-magnitude diagram C0422m213 |that showed an extremely red HB. A VI color-magnitude diagram by C0422m213 |Stetson et al. (1999) confirmed this and also showed about a dozen C0422m213 |blue stragglers. C0443p313 |A variable search of Pal 2 was carried out by Rosino & Pinto (1973). C0443p313 |They concluded that the cluster does not contain any red variables, C0443p313 |but the possibility that any RR Lyrae may be present could not be C0443p313 |ruled out. C0443p313 |A CM diagram was published by Harris et al. (1997). They found a C0443p313 |well populated red horizontal branch with a sparser extension to the C0443p313 |blue. Based on this, they concluded that it is likely that Pal 2 C0443p313 |contains RR Lyrae variables, but their observational data were not C0443p313 |suitable for performing a search. C0443p313 |A VI color-magnitude diagram published by Sarajedini et al. (2007) C0443p313 |confirms that the HB is bimodal in color and that the cluster is C0443p313 |located in a direction of high foreground absorption and differential C0443p313 |reddening. C0512m400 |The periods, magnitudes, amplitudes and variability types C0512m400 |for the RR Lyrae variables numbered up to V33 are from C0512m400 |Walker (1998). All of them are considered to be cluster members. C0512m400 |The RA and dec for V1-33 are from Samus et al. (2009). C0512m400 |For variables V34-52, the data are from Sumerel+ (2004IBVS.5533....1S) C0512m400 |unless indicated otherwise in the notes on individual stars. C0512m400 |The data for V53-55 and PSR are from the discovery papers. C0522m245 |A major paper on the variables in NGC 1904 (M79) is by Kains et al. C0522m245 |(2012). They carried out a thorough analysis of the RR Lyrae variables. C0522m245 |In the above table, all the data for V3-7 and V9-14 are from the study C0522m245 |by Kains et al. C0522m245 |V2 and V8 were saturated in their reference images, so the RA and dec C0522m245 |for these two stars are from Samus et al. (2009) and the magnitude, C0522m245 |amplitude and classification for V2 are from Rosino (1952). It seems C0522m245 |probable that V8 might also be a semi-regular, like V2. C0647m359 |The RA and dec for V1-4 are from Samus et al. (2009) and their period, C0647m359 |magnitudes, amplidues and classification are from Clement et al. C0647m359 |(1995). C0647m359 |This cluster is currently undergoing disruption. De Marchi & Pulone C0647m359 |(2007) found a deficiency of low-mass stars and estimated that the C0647m359 |cluster has lost 85% of its original mass. Balbinot et al. (2011) C0647m359 |have detected several extra-tidal features, including a leading and C0647m359 |trailing tail around NGC 2298. C0734p390 |All of the data listed in the above table are from the V photometry C0734p390 |reported by Di Criscienzo et al. (2011a). Their study also included C0734p390 |BI data. C0734p390 |NGC 2419 is one of the brightest GCs in the Milky Way. Recent studies C0734p390 |by Bruns & Kroupa (2011), Cohen et al. (2010) and Di Criscienzio et C0734p390 |al. (2011b) all support the hypothesis that this cluster is the remnant C0734p390 |of a much more massive system. The cluster also has a large population C0734p390 |of blue straggler stars. Dalessandro et al. (2008) published RA, Dec, C0734p390 |and BVI photometry for 232 BSS candidates and noted that their radial C0734p390 |distribution was essentially the same as that of the other stars in the C0734p390 |cluster. C0906m370 |Pyxis is a distant globular cluster, located approximately 40 kpc from C0906m370 |the Galactic centre. A CM diagram published by Dotter et al. (2011), C0906m370 |based on HST photometry, shows a prominent red HB. Harris (1996) C0906m370 |lists [Fe/H] = -1.20 in the 2010 update to his catalogue. C0911m646 |V1-12: The RA and Dec are from Samus et al. (2009) and are updated C0911m646 |from an earlier paper by Evstigneeva et al. (1997). C0911m646 |Most of the remaining information for these stars (except V1, V6 and C0911m646 |V11) is from Clement & Hazen (1989). Lebzelter & Wood (2011) derived C0911m646 |periods and magnitudes for V1 and V11 as part of their study of long C0911m646 |period variables and Kunder et al. (2011) derived a period, magnitude C0911m646 |and amplitude for V6 in their investigation of RR Lyrae variables. C0911m646 |V13-30: The periods and classifications for most of these variables C0911m646 |are from a paper by Corwin et al. (2004). [For the stars indicated by K11 C0911m646 |in the comments column, the data were derived by Kunder et al. (2011).] C0911m646 |Corwin et al. (2004) did not derive magnitudes or amplitudes because they C0911m646 |used the image subtraction method. C0911m646 |The RA and dec listed for V13-V30 in the above table were provided C0911m646 |independently by Corwin (2010, private communication) because there C0911m646 |were errors in the coordinates they published in Table 1 on page C0911m646 |669 of their 2004 paper. C0911m646 |V31-50: The RA, dec, periods and mean magnitudes are from Lebzelter & C0911m646 |Wood (2011) who designated them as LW1-20. The amplitudes listed for C0911m646 |these stars have been estimated to the nearest 0.1 mag from their C0911m646 |published light curves. C0921m770 |The data for V1-2 are from the discovery paper by Mochejska et al. C0921m770 |(2000) C0921m770 |Sarajedini et al. (2007) published a CM diagram which showed no C0921m770 |HB population. They concluded that this indicates there has been C0921m770 |significant mass segregation and/or mass loss. C1003p003 |The RA and dec for V1-12 are from Samus et al. (2009). C1003p003 |The remaining data for V1-3 are from Gratton & Ortolani (1984). The C1003p003 |data for V5-12 are from Borissova et al. (1998) where the adopted mean V C1003p003 |magnitudes are the means of the magnitudes that they listed for each C1003p003 |star. In their paper, V5-12 were listed as BS58, V1-5 and V9-10 C1003p003 |respectively. C1003p003 |All of the data for V13-14 are from Stetson et al. (1999) where C1003p003 |the mean V magnitudes were estimated from their light curves. C1015m461 |The RA and dec for V1-101 are from Samus et al. (1999). C1015m461 |They published ID charts in an earlier paper (Samus et al. 1996). C1015m461 |Fourcade et al. (1966) also published charts, but Samus et al. (1996) C1015m461 |pointed out that some of Fourcade's identifications were erroneous. C1015m461 |Most of the elements for variables V1-100 are taken from Layden & C1015m461 |Sarajedini (2003) because their study was the most comprehensive. C1015m461 |(They also confirmed the "CST" classification that was previously C1015m461 |reported by Wright (1941) and Kukarkin (1971) for V33, V70, V74, C1015m461 |V75 and V82.) C1015m461 |However, some variables were outside the Layden & Sarajedini field C1015m461 |which was approximately 9.5 by 10 arcmin. In these cases, data from C1015m461 |other sources are listed and this is indicated in the remarks column: C1015m461 | P02 refers to a CCD investigation by Piersimoni et al. (2003). C1015m461 | C84 refers to the photographic investigation by Cacciari (1984) C1015m461 | W41 refers to stars for which Wright (1941) listed the only available C1015m461 | data. These stars were all outside the field of the other C1015m461 | studies. Based on their mean magnitudes and the fact that they C1015m461 | all lie within the 25.3 arcmin tidal radius derived from the C1015m461 | 2010 update to the Harris catalogue, they appear to be cluster C1015m461 | members. C1015m461 | K71 refers to Kukarkin (1967,1971a,b). In 1967 and 1971a, he listed C1015m461 | periods and in 1971b, he published the individual magnitudes. C1015m461 | If no data were available from P02, the C84 data are listed and if C84 C1015m461 | did not study the star, the W41 data are listed and failing that, K71. C1015m461 | Kukarkin derived periods for variables announced by Wilkens (1965) that C1015m461 | were outside the field of view in the other studies. He also C1015m461 | investigated a few of the "outer" variables for which Wright (1941) C1015m461 | was unable to derive periods. C1015m461 | C1015m461 | "A" in the remarks column indicates that the period is from the study C1015m461 | by Arellano Ferro et al. (2014). They derived their periods by C1015m461 | combining their observations (made on 4 consecutive nights in March C1015m461 | 2013) with those of Layden & Sarajedini (LS). Arellano Ferro's field C1015m461 | of view was 5.1 by 5.1 arcminutes and included 34 of the 58 RRL stars C1015m461 | observed by LS. C1015m461 | Their paper also includes an excellent finding chart that labels all C1015m461 | of the variable stars in their field of view. C1015m461 |The data for V101 (=V6 of von Braun & Mateo 2002), V102-112 (V1-11 of C1015m461 |Mazur et al. 2003), V113-121 (Layden & Sarajedini 2003), V122-124 C1015m461 |(Arellano Ferro et al. 2014) and V125-160 (Kaluzny et al 2016) are C1015m461 |from the discovery papers unless indicated otherwise in the notes on C1015m461 |individual stars. C1015m461 |The effects of differential reddening across the face of NGC 3201 are C1015m461 |substantial. This is illustrated in an extinction map published by C1015m461 |von Braun & Mateo (2001) and was taken into account by Arellano Ferro et C1015m461 |al. (2014) when they estimated the membership status of the SX Phe C1015m461 |variables. C1015m461 |Carretta et al. (2010) and Kravtsov et al. (2010) reported evidence for C1015m461 |inhomogeneity in this cluster's stellar populations associated with C1015m461 |radial distribution. C1126p292 |Periods, magnitudes, amplitudes and variablity types For V1-2 are from C1126p292 |Rosino & Pinto (1973). The RA and dec are from Samus et al. (2009) C1126p292 |According to Burbidge & Sandage (1958), there are no RR Lyrae in Pal 4, C1126p292 |a result confirmed by Stetson et al. (1999). The CM diagram has a red HB C1126p292 |that does not extend blueward to the instability strip. C1207p188 |RA, dec, magnitudes, amplitudes and variability types from Stetson et C1207p188 |al. (2005). C1207p188 |NGC 4147 might be connected with the Sgr dwarf galaxy, but according to C1207p188 |Jordi & Grebel (2010), there is still some debate about this. C1223m724 |The BV CM diagram published by Kaluzny & Krzeminski (1993) shows an C1223m724 |extended blue HB and a blue straggler sequence. NGC 4372 is a metal C1223m724 |poor cluster with [Fe/H] = -2.17 according to the 2010 version of the C1223m724 |Harris (1996) catalogue. C1223m724 |The RA and dec for V1 and V2 are from Samus et al. (2009) C1223m724 |The positions, periods and magnitudes for V3-22 are from Kaluzny & C1223m724 |Krzeminski (1993). C1223m724 |The membership status for the W Ursa Majoris (EW) variables: V4, 5, 10, C1223m724 |12, 15, 19, 20, 22 are from Rucinski (2000). C1235m509 |A CM diagram of Ruprecht 106 by Dotter et al. (2011) shows a red HB C1235m509 |and a well populated blue straggler sequence. There is some uncertainty C1235m509 |about the metal abundance of this cluster with values ranging from C1235m509 |[Fe/H] = -1.9 to greater than -1.6. Values based on photometric C1235m509 |indicators are more metal poor than those based on spectroscopy. C1235m509 |Dotter et al. (2011) suggested that this discrepancy might be due to C1235m509 |its unusually low [alpha/Fe] ratio compared with other metal poor C1235m509 |clusters. C1235m509 |In the above table, the RA and dec are from Samus et al. (2009). C1235m509 |The periods, magnitudes, amplitudes and classifications are from the C1235m509 |discovery paper by Kaluzny et al. (1995). C1235m509 |The field status of V7 and V17 are from Rucinski (2000). C1236m264 |The RA and dec for V1-48 are from Samus et al. (2009) and for V49-53, C1236m264 |they are from Kains et al. (2015). C1236m264 |All of the remaining data in the above table are from Kains et al. C1236m264 |(2015) unless indicated otherwise in the Notes on individual stars. C1256m706 |The coordinates for V1-23 are from Samus et al. (2009) and the ones for C1256m706 |V24-34 are from Darragh & Murphy (2012). C1256m706 |The periods, magnitudes, amplitudes and classifications for the RR Lyrae, C1256m706 |SX Phe and eclipsing variables are from the study by Darragh & Murphy C1256m706 |(2012) unless indicated otherwise in the notes. C1256m706 |The Mira variables (V2, V11) and the semi-regular variables (V9, V10, V16) C1256m706 |were not investigated by Darragh & Murphy because they were too bright or C1256m706 |outside their field of view. These five stars are discussed in the notes C1256m706 |below. C1310p184 |V1-105: The data for all except 20 of these stars are from Arellano C1310p184 | Ferro et al. (2011). These authors also published ID charts for all C1310p184 | of the variables they studied. Some of the mean magnitudes and C1310p184 | amplitudes were published in their 2011 MNRAS paper and the rest were C1310p184 | supplied by Arellano Ferro (2011, private communication). The C1310p184 | amplitudes listed for the SX Phe variables in the above table are C1310p184 | double the values that were published by Arellano Ferro et al. (2011). C1310p184 | In a separate paper (Arellano Ferro et al. 2012), they discussed the C1310p184 | properties of the M53 Blazkko variables. C1310p184 | The 20 variables not included in the study of Arellano Ferro et al. C1310p184 | (2011) are V12, 13, 14, 20, 21, 22, 26, 28, 30, 48, 77, 88, 90 which C1310p184 | were not in their field of view and V49, 50, 65, 66, 68, 69, 70 which C1310p184 | were saturated in their images. The RA and dec listed above for these C1310p184 | 20 stars are from Samus et al. (2009). C1310p184 | The sources for their periods, magnitudes, amplitudes and variability C1310p184 | types are indicated in the remarks column where C1310p184 | Gor refers to Goranskij (1976), C1310p184 | Cuf refers to Cuffey (1965, 1966), C1310p184 | Kop refers to Kopacki (2000), C1310p184 | DK refers to Dekany & Kovacs (2009) and C1310p184 | Jeon refers to Jeon (2003). C1310p184 | The Goranskij study was based on photographic observations and the mean C1310p184 | B magnitude is the mean of their B_max and B_min. C1310p184 | Kopacki (2000) reduced his data using the image subtraction method and C1310p184 | therefore did not derive magnitudes for many of the variables in his C1310p184 | investigation, including the SR variables he discovered. C1310p184 |Kopacki's paper gave a good summary of previous investigations C1310p184 |of the variables in M53. He also published an ID chart covering an area C1310p184 |of about 6 by 4 arcmin and labelled all of the variables (up to V70) C1310p184 |in the field of view. C1310p184 |V106-109: All the data are from Bramich et al. (2012). C1313p179 |The RA and dec for V1-15 are from Samus et al. (2009). C1313p179 |The periods, magnitudes, amplitudes and classifications for V1 to V10 C1313p179 |are from Nemec (2004) and for V11-15 are from Nemec et al. (1995). C1313p179 |According to Law & Majewski (2010), NGC 5053 might be associated with C1313p179 |the Sgr dwarf galaxy, but this can not be conclusively determined until C1313p179 |its proper motion is measured. C1323m472 |The RA, dec and most of the elements listed for V1-410 in the above table C1323m472 |are from the catalogue published by Kaluzny et al. (2004). In cases where C1323m472 |they adopted the periods, magnitudes, amplitudes and classification C1323m472 |from other sources because the stars' images were saturated on their C1323m472 |frames or if they were outside their field of view, this is indicated in C1323m472 |the remarks column where the source is indicated as follows: C1323m472 | Bai refers to Bailey (1902) C1323m472 | Mar refers to Martin (1938) C1323m472 | vG refers to van Gent (1948) C1323m472 | Fea refers to Feast (1965) C1323m472 | Wil refers to Wilkens (1965) C1323m472 | DC refers to Dickens & Carey (1967) C1323m472 | DFL refers to Dickens et al. (1972) C1323m472 | Eg refers to Eggen (1970) C1323m472 | GSz refers to Geyer & Szeidl (1970) C1323m472 | HSH3 refers to Sawyer Hogg's 3rd (1973) catalogue C1323m472 | K96 refers to Kaluzny et al. (1996) C1323m472 | K97a refers to Kaluzny et al. (1997a) C1323m472 | K97b refers to Kaluzny et al. (1997b) C1323m472 | vL refers to van Leeuwen et al. (2000) C1323m472 | Wel refers to Weldrake et al. (2007) C1323m472 |The data for V411 are from Navarrete et al. (2013,2015). C1323m472 |All the data for V412-V450 are from Weldrake et al. (2007). Mean C1323m472 |magnitudes have not been listed for these stars because the V magnitudes C1323m472 |that they published were not mean values. Also the amplitudes have not C1323m472 |been listed because the observations were not made on the standard V C1323m472 |system; they are a combination of V and R. C1323m472 |The data for V451-V454 and V460 are from Randall et al. (2011, 2016). C1323m472 |The sdOV classification is based on the system devised by Kilkenny et C1323m472 |al. (2013). C1323m472 |The data for V455 and V456 are from Navarrete et al. (2015). C1323m472 |The data for V457-459 are from Figuera Jaimes et al. (2016) C1323m472 |The field status for V240 (Ogle #48), V247 (Ogle #57) and V257 (Ogle C1323m472 |#67) was established by Rucinski (2000) who determined that the other C1323m472 |EW variables discovered by Kaluzny et al. (1996, 1997a), i.e., the EW C1323m472 |stars with numbers in the range V197-V260, are cluster members. C1323m472 |Samus et al. (2009) have pointed out that V1, V2, V56, V65, V78, V129, C1323m472 |V133, V168, V269, V283 are listed in the GCVS as NSV 06235 and V0825, C1323m472 |V0833, V0813, V0814, V0826, V0594, V0832, V0791, V1045 Cen, C1323m472 |respectively. C1323m472 |Braga et al. (2016) published homogenous pulsation parameters for 187 C1323m472 |candidate RR Lyrae variables. C1339p286 |For V1 to V274: C1339p286 | The RA and dec, as well as the variability types, listed in the C1339p286 | above table are from Bakos et al. (2000), unless otherwise indicated C1339p286 | in the notes on individual stars. C1339p286 | The periods are from Benko et al. (2006, MNRAS 372, 1657) unless C1339p286 | otherwise indicated in the notes on indvidual stars. C1339p286 | RR Lyrae magnitudes and amplitudes are mainly from Corwin & Carney C1339p286 | (2001) or from Benko et al. (2006), if designated "Benko" in the C1339p286 | remarks column. Exceptions are explained in the notes on indiviual C1339p286 | stars. Since Benko et al. (2006) did not list amplitudes in their C1339p286 | table, the amplitudes were estimated from their light curves. C1339p286 | Note that the V magnitude system of Benko could be 0.02 mag fainter C1339p286 | on average than Corwin's. C1339p286 | No magnitudes or amplitudes have been listed for stars that had C1339p286 | blended images in the data of both Corwin & Carney (2001) and Benko C1339p286 | et al. (2006). These stars are designated "blend" in the "Remarks" C1339p286 | column. C1339p286 |For V286 to V297: C1339p286 | All of the information listed in the above table is from the C1339p286 | discovery paper by Hartmann et al. (2005). C1339p286 |Identification charts for most of the variables numbered up to V259 C1339p286 |have been published by Kholopv (1977) or by Kadla & Gerashchenko (1982). C1339p286 |However, the numbering system for V226 and up was assigned after C1339p286 |these papers were published so these higher numbered stars were C1339p286 |labelled by their designations according to Kholopov or Kadla. C1339p286 |An important catalog of 1571 M3 stars was published by von Zeipel C1339p286 |(1908). It is available from the Harvard ADS. Many authors have cited C1339p286 |the von Zeipel numbers. Sawyer (1955) listed vZ numbers for variables C1339p286 |V1-204 in her second catalog and for V205-225 in her third catalog (1973). C1339p286 |==== C1339p286 |Notes on individual stars C1339p286 |V2: Shapley (1914) commented that V2 (star 9 in his Table II) is a C1339p286 | close double and that it is almost certain that both components C1339p286 | are variable. However, Bakos et al. (2000) found that neither C1339p286 | component varied on the CCD images they obtained. We have C1339p286 | therefore classified V2 as non-variable. C1339p286 |V13: The double-mode nature of V13, V200 and V251 was first C1339p286 | recognized by Clementini et al. (2004) C1339p286 |V29: V29 and V155 were interchanged by Evstigneeva et al. (1994) C1339p286 | and by Corwin & Carney (2001). The period we list for V29 is C1339p286 | from Benko et al. (2006) and the mean magnitude and amplitude C1339p286 | are the ones Corwin & Carney (2001) listed for V155. C1339p286 |V82: Benko et al. (2006) did not list a period for V82, V91, C1339p286 | V115 or V192. For these stars, we list the periods, as C1339p286 | well as the mean magnitudes and amplitudes, published C1339p286 | by Corwin & Carney (2001) C1339p286 |V91: See V82. C1339p286 |V95: The period, magnitude and amplitude listed for V95 and C1339p286 | V225 are from Russev (1971). Rosino (1978) classified V95, C1339p286 | V138 and V225 as semi-regular variables. C1339p286 |V96: For V96, V139, V168, V188 and V195, we list the magnitudes C1339p286 | from Benko et al. (2006) and amplitudes from Corwin & Carney C1339p286 | (2001). Corwin & Carney did not publish mean magnitudes for C1339p286 | these stars. C1339p286 |V112: Bailey (1913, HA 78, p. 67) commented that the range of C1339p286 | variation was small for V112 so no effort was made to C1339p286 | determine a period. C1339p286 | Sawyer (1939) classified it as non-variable all of her C1339p286 | catalogs. The star was not included in subsequent C1339p286 | investigations by other authors. C1339p286 |V113: The period, magnitude and amplitude listed for V113 and C1339p286 | V123 are from Szeidl (1965). According to Samus (2009, private C1339p286 | communication), V113 is XX CVn in the GCVS. C1339p286 |V115: Period, as well as the mean magnitude and amplitude, published C1339p286 | by Corwin & Carney (2001). See V82. C1339p286 |V123: Data from Szeidl. See V113. C1339p286 |V127: Bailey (1913) was unable to derive a period for V127 C1339p286 | because it had two close companions. Muller (1933, Berlin C1339p286 | Babelsberg Veroff 11, 1) subsequently showed that the northern C1339p286 | component, which he designated as V146, was the variable. C1339p286 | Sawyer Hogg (1939) therefore classified V127 as non-variable C1339p286 | in her first and subsequent catalogs. C1339p286 | Later, Kholopov (1963) found that the southwest component (his C1339p286 | X34 = vZ 1198) was also variable. C1339p286 | Sawyer Hogg (1973) designated X34 as V222 in her 3rd catalog. C1339p286 |V138: Period, magnitude and amplitude from Olah and Russev (1979). In C1339p286 | an earlier paper, Russev (1971) derived a longer period. Rosino C1339p286 | (1978) classified V95, V138 and V225 as semi-regular variables. C1339p286 |V139: Magnitudes from Benko et al. and amplitude from Corwin & Carney. C1339p286 | See V96. C1339p286 |V140: When this M3 file was posted in 2009, V140 was incorrectly C1339p286 | listed as an RR0 type. It should be RR1. Marcio Catelan C1339p286 | (2011- private communication) pointed out the error. C1339p286 |V141: V141=RV CVn in the GCVS. Period, magnitude, amplitude and C1339p286 | classification are from Szeidl (1973) who considered it to be a C1339p286 | field star. C1339p286 | However, a proper motion study by Tucholke et al. (1994) C1339p286 | indicates that it is a probable member. C1339p286 |V146: According to Benko et al. (2006), V146 and V222 were C1339p286 | interchanged by Corwin & Carney (2001) and by Clementini et al. C1339p286 | (2004). The magnitude and amplitude that we list for V146 in the C1339p286 | above table are the values listed by Corwin & Carney for V222. C1339p286 | Kholopov (1977) pointed out that the observations that Greenstein C1339p286 | (1935) published for V146 are really for V222. C1339p286 | See also the comment for V127. C1339p286 |V154: Period, magnitude, amplitude and variability type listed C1339p286 | in the above table are from Kholopov (1972) C1339p286 |V155: V29 and V155 were interchanged by Evstigneeva et al. (1994) C1339p286 | and by Corwin & Carney (2001) C1339p286 | The period we list for V155 is from Benko and the mean C1339p286 | magnitude and amplitude are the ones Corwin & Carney (2001) C1339p286 | listed for V29. C1339p286 |V157: Mean magnitude from Benko et al. (2006) because Corwin & C1339p286 | Carney (2001) did not publish a value. Amplitude difficult to C1339p286 | estimate because of Blazhko effect. C1339p286 |V158: Greenstein (1935) derived a period of 0.50809 which was listed C1339p286 | by Sawyer Hogg in her catalogs. However, in her 2nd and 3rd C1339p286 | catalogs, she indicated that the period was uncertain. C1339p286 | Bakos et al. (2000) did not detect any variation. C1339p286 |V162: Greenstein (1935) classified this star as non-variable. He noted C1339p286 | that it was part of a triple system. C1339p286 | Later Kholopov (1963, Per Zvez 14, 275) found that one of C1339p286 | the other stars in the triplet (vZ 950 = X28) was variable. C1339p286 | Sawyer Hogg (1973) designated vZ 950 as V218 in her 3rd catalog. C1339p286 |V163: Greenstein (1935) classified this star as non-variable. Bakos C1339p286 | et al (2000) noted that the x,y position listed in Sawyer Hogg's C1339p286 | catalogs was midway between V180 and a non-variable. According C1339p286 | to Bakos, Kholopov (1977) labelled the non-variable as V163. C1339p286 | Bakos therefore accepted the non-variable as V163 to avoid C1339p286 | confusion. C1339p286 | See also the comments for V180. C1339p286 |V164: Greenstein (1935) noted that this star was badly blended and C1339p286 | and that, if it was variable, its range was les than 0.35 mag. C1339p286 | Benko et al (2006) classified it as non variable. C1339p286 | Corwin & Carney derived a period, but according to Clementini C1339p286 | et al. (2004), the star that they studied was V234, not V164. C1339p286 |V165: Bakos et al. pointed out that there was an error in the sign C1339p286 | of the "y" coordinate listed for this star in Sawyer Hogg's C1339p286 | (1973) 3rd catalog, but it was correct in the 1939 and 1955 C1339p286 | editions. The mean magnitude and amplitude we list for V165 C1339p286 | were derived by Benko et al. because Corwin & Carney did not C1339p286 | publish an amplitude or mean magnitude for it. C1339p286 |V168: Magnitudes from Benko et al. and amplitude from Corwin & Carney. C1339p286 | See V96. C1339p286 |V179: Greenstein (1935) commented that the star was difficult to C1339p286 | measure and that if it was variable, it had a small range. C1339p286 | Sawyer (1939) classified it as non-variable in all 3 of her C1339p286 | catalogs. Bakos et al. (2000) were unable to locate the star C1339p286 | unambiguously on POSS images. The RA and dec listed in the C1339p286 | above table were calculated by Samus (2009, private C1339p286 | communication). He derived a relation between x,y and RA, dec C1339p286 | based on 39 M3 stars and used it to calculate the RA and dec C1339p286 | for V179 from the published x,y coordinates. C1339p286 | There is a 2MASS star in the same location. The RA and dec C1339p286 | listed in the 2001 on-line update to the catalog were C1339p286 | incorrect. C1339p286 |V180: V180 = vZ 676: Shapley (1914) stated that vZ676 was composed C1339p286 | of five distinct stars, of which the variable is the brightest C1339p286 | and most centrally located. Greenstein (1935) could not measure C1339p286 | it because of the crowding. Sawyer (1939) classified it as C1339p286 | non-variable in all three of her catalogs. However, Kholopov C1339p286 | (1977) and Bakos et al. (2000) found that there are two RR Lyrae C1339p286 | variable stars close to (and equidistant from) the position C1339p286 | listed for V180 in Sawyer Hogg's catalogs. The eastern component C1339p286 | was chosen by them to be V180 and the western component, C1339p286 | Kholopov's X13 was designated V239 by Bakos et al. C1339p286 | The period, magnitude, amplitude and classification we list in C1339p286 | the above table are from Bakos et al. (2005). We estimated the C1339p286 | amplitude from their published light curve. C1339p286 |V182: Greenstein could not confirm the variability of this star. C1339p286 | Sawyer (1939) classified it as non variable in all three C1339p286 | of her catalogs and Bakos et al. (2000) and Benko et al. C1339p286 | (2006) confirmed its non-varable status. C1339p286 |V183: Greenstein commented that V183 was blended with V145. C1339p286 | Sawyer (1939) classified it as non-variable in all three C1339p286 | of her catalogs. Bakos et al. (2000) confirmed its non-variable C1339p286 | status. C1339p286 |V185: Greenstein commented that this was a bright star with a small C1339p286 | range. Bakos et al. (2000) did not detect any variation. Corwin & C1339p286 | Carney (2001) and Benko et al (2006) did not study it. C1339p286 |V188: Magnitudes from Benko et al. and amplitude from Corwin & Carney. C1339p286 | See V96. C1339p286 |V192: Period from Corwin & Carney. See V82. C1339p286 |V195: Magnitudes from Benko et al. and amplitude from Corwin & Carney. C1339p286 | See V96. C1339p286 |V196: The variation of V196 was announced by Greenstein. He could C1339p286 | not derive a period because it was a double and difficult C1339p286 | to measure. Bakos et al. (2000) found that both components C1339p286 | are constant. C1339p286 |V198: Bakos et al. did not confirm variation in this star based on C1339p286 | one night of observations. However, Corwin & Carney derived C1339p286 | a period from their observations and commented that the star C1339p286 | appears to be slightly above the HB of the CMD. C1339p286 |V199: The magnitude and amplitude listed above are from C1339p286 | Greenstein's (1935) paper. He derived a period of 0.488, but C1339p286 | noted that it was doubtful. Corwin & Carney derived 0.40891, C1339p286 | but indicated that it was uncertain. They did not publish a C1339p286 | light curve or list a mean magnitude. C1339p286 |V200: The period, magnitude and variability type are from Benko et al. C1339p286 | (2006). The double-mode nature of V200 was first recognized by C1339p286 | Clementini et al. (2004). C1339p286 |V204: This star was incorrectly listed as von Zeipel 390 (instead of C1339p286 | 1390) in Sawyer's (1955) 2nd catalog. As a result, its x,y was C1339p286 | incorrect in her 2nd and 3rd catalogs. According to Corwin & C1339p286 | Carney (2001) and Benko et al. (2006), this star is non-variable. C1339p286 | However, Yao (2007) claims that it is a red HB star with a period C1339p286 | of 0.74785 and V amplitude 0.04. C1339p286 | C1339p286 |V205, 206: C1339p286 | Evstigneeva et al. (1994) pointed out that V205 and 206 are WY C1339p286 | CVn and VZ CVn in the GCVS. C1339p286 | The periods and magnitudes we list for these two stars are from C1339p286 | Kukarkin (1960, Ast Tsirk 216, 29). C1339p286 |V217: Guhathakurta et al. (1994) classified this star (Gu9023) C1339p286 | as an RR Lyrae. C1339p286 |V222: According to Benko et al. (2006), V146 and V222 were C1339p286 | interchanged by Corwin & Carney (2001) and by Clementini et C1339p286 | al. (2004). The magnitude and amplitude that we list for V222 C1339p286 | in the above table are the values listed by Corwin & Carney for C1339p286 | V146. See the comment for V146. C1339p286 |V224: Bakos et al. (2000) confirmed that this star was variable, but C1339p286 | also commented that its image merges with that of a nearby star. C1339p286 | It was not investigated further in their subsequent paper (Benko C1339p286 | et al. 2006). C1339p286 |V225: The period, magnitude and amplitude listed for V95 and C1339p286 | V225 are from Russev (1971). Rosino (1978) classified V95, C1339p286 | V138 and V225 as semi-regular variables. C1339p286 |V230: This was Kholopov's (1977) X41. It was not labelled on his ID C1339p286 | chart because it was too far from the cluster centre. It was not C1339p286 | studied by Corwin & Carney (2001) or by Benko et al. (2006). C1339p286 |V234: According to Corwin & Carney (2001), this star is an RR Lyrae C1339p286 | that might be more distant than the cluster so we have classified C1339p286 | it as a field star. In their investigation, they called the C1339p286 | star V164, but Clementini et al. (2004) later pointed out that it C1339p286 | was V234. C1339p286 |V236 (vZ 1397): C1339p286 | Period, magnitude and amplitude in the above table are from C1339p286 | Olah (1979) based on 195 Budapest observations obtained between C1339p286 | 1938 and 1962. A period of 215.8 days also fit the data. The C1339p286 | star was also discussed by Welty (1985) who derived periods of C1339p286 | 32.2 and 60.2 from Yerkes observations obtained between 1978 and C1339p286 | 1983. He preferred the 60 day period. We classify the star as SR. C1339p286 |V237, V238, V239: C1339p286 | Benko et al. (2006) pointed out that the dec for V238 and V239 C1339p286 | were incorrectly listed in the 2001 on-line version of the C1339p286 | catalog. Meanwhile, Hartman et al. (2005) pointed out C1339p286 | that the coordinates of V237 and V238 were switched in the C1339p286 | discovery paper (Kaluzny) and that this error had propagated C1339p286 | through to the catalog of Bakos et al. (2000). The coordinates C1339p286 | listed for V237, V238, V239 have all been revised accordingly C1339p286 | in the above table. C1339p286 | V237: Period, magnitude, amplitude and classification from C1339p286 | Hartman et al. (2005). C1339p286 | V238: Period, magnitude, amplitude and classification C1339p286 | from the discovery paper by Kaluzny et al. (1998) C1339p286 | The non-membership status for V238 is from Rucinski (2000). C1339p286 |V240: Mean magnitude from Corwin & Carney (2001) and amplitude C1339p286 | estimated from the light curve published by Benko et al. (2006) C1339p286 |V250n, V250s: C1339p286 | Benko et al. (2006) discovered that the image of V250 consisted C1339p286 | of two close companions, both RR0 variables. They derived a C1339p286 | period for each star, but it was not possible to derive individual C1339p286 | magnitudes or amplitudes. C1339p286 |V251: The double-mode nature of V251 was first recognized by C1339p286 | Clementini et al. (2004). C1339p286 |V260: This star (vZ 297) is among the brightest stars on the giant C1339p286 | branch and Walker (1955) suggested that it might be variable. C1339p286 | However, the variation was not confirmed by Olah (1979) nor by C1339p286 | Welty (1985). The mean magnitude we list in the above table is C1339p286 | from Olah's paper. C1339p286 | We classify it as SR? because its colour and magnitude are C1339p286 | comparable to the SR variables in M3: V95, V138, V225 and V236. C1339p286 |V262: Guhathakurta et al. (1994) classified this star (Gu 552) as an C1339p286 | RR Lyrae variable, but Bakos et al. (2000) found no trace of C1339p286 | variation, hence the "CST?" designation. C1339p286 | C1339p286 |V265, V267, V268: C1339p286 | V265=Gu 1489, V267=Gu 9016, V268=Gu 9025: These stars all have C1339p286 | close companions. The variability types were assigned by C1339p286 | Guhathakurta et al. (1994, AJ 108, 1786) but they did not derive C1339p286 | precise periods for any of them. C1339p286 |V270n, V270s: C1339p286 | Benko et al. (2006) discovered that the image of V270 consisted C1339p286 | of two close companions, both RR0 variables. They derived a C1339p286 | period for each star, but it was not possible to derive individual C1339p286 | magnitudes or amplitudes. C1339p286 |V272, V273, V274: C1339p286 | Light curves based on the image subtraction method were C1339p286 | published by Bakos et al. (2000). Benko et al. (2006) C1339p286 | published a period for V273. We have classified them all C1339p286 | as SR because Benko et al. indicated that they varied on C1339p286 | "long" time scales. C1339p286 |S1-S11: C1339p286 | Strader et al. (2002) announced the discovery of 11 new C1339p286 | suspected variables (S1-11). They derived periods ranging from C1339p286 | 7 to 32 hours for 9 of the stars, but the observations of Benko C1339p286 | et al. (2006) did not confirm any of these discoveries. C1339p286 | When Hartmann et al. (2005) set up their numbering system for C1339p286 | V286 to V297, they left a gap from V275 to V285 to accommodate C1339p286 | these 11 variables. C1339p286 | However, we have not assigned numbers to them because of C1339p286 | Benko's result. C1339p286 |V298: This star is N2 in the paper by Benko et al. (2006) and C1339p286 | all of the information listed for it is from their paper. C1339p286 | C1343m511 |A major study of the variables in NGC 5286 was carried out by Zorotovic C1343m511 |et al. (2010). C1343m511 |The data for V1-62 in the above table are from their study unless indicated C1343m511 |otherwise in the notes on individual stars. C1343m511 |NOTE that the mean V values that Zorotovic et al. (2010) published, and C1343m511 |listed in the above table, were corrected for reddening according to a C1343m511 |method described in an earlier paper (Zorotovic et al. 2009). C1343m511 |The data for V63-73 are from the discovery paper of Figuera Jaimes et C1343m511 |al. (2016). C1353m269 | Inman & Carney (1987, AJ 93, 1166) published a C1353m269 | BV color-magnitude diagram which had no giant C1353m269 | or HB stars. Its brightest stars are post-main C1353m269 | sequence subgiants. They concluded that AM4 is an C1353m269 | unusually faint, low-mass object. It could be C1353m269 | a globular cluster similar to M3 in age and C1353m269 | metal abundance. C1353m269 | Carraro (2009, AJ 137, 3809) obtained BVI photometry C1353m269 | that confirmed this. The cluster is tidally distorted C1353m269 | and could be "an almost dissolved cluster" of extragalactic C1353m269 | origin. C1403p287 |The RA and dec for V1-36 were taken from Samus et al. (1999) and for C1403p287 |V39-41 from Jeon et al. (2004). Jeon et al. also derived RA and dec C1403p287 |for V31-36 and these are in good agreement with the values of Samus et al. C1403p287 |The periods, magnitudes and classifications for all of the variables C1403p287 |numbered from V1-27 (with the exception of V1 and V20) are from C1403p287 |Corwin et al. (1999). V1 and V20 are discussed in the notes on individual C1403p287 |variables. C1403p287 |Periods, magnitudes, amplitudes and classification for V28-30 are C1403p287 |from Mateo et al. (1990) who concluded that all three were probably cluster C1403p287 |members. The membership status for V28 and V29 was confirmed by C1403p287 |Rucinski (2000). V30 was not included in his study. C1403p287 |Periods, magnitudes, amplitudes and classifications for V31-V36 are from C1403p287 |Jeon et al. (2004) who listed the stars according to the numbering system C1403p287 |of the Nemec & Mateo (1990): NH 29, 49, 35, 27, 39, 38. C1403p287 |All the data for V37 and V38 are from the paper by Arellano Ferro et al. C1403p287 |(2008). The periods they derived are in the RR Lyrae range, but with C1403p287 |unusally low amplitudes. They are brighter than the RR Lyrae variables in C1403p287 |the cluster and might be field stars. C1403p287 |All of the data listed for V39-41 are from the paper by Jeon et al. C1403p287 |(2004). Their paper presented several frequencies and amplitudes. The C1403p287 |periods that we list in the above table are the ones associated with C1403p287 |their dominant frequency. C1427m057 |For V1-7, the RA and dec are from Samus et al. (2009) and the periods, C1427m057 |magnitudes and classification are from Liller & Sawyer Hogg (1976) C1427m057 |unless indicated otherwise in the notes on individual stars. C1427m057 |The periods and classifications for V8-21 are from the discovery paper C1427m057 |by Salinas et al. (2005). The RA and dec were derived from the study C1427m057 |by Salinas et al. (2012) and were provided by Salinas (2013, private C1427m057 |communication), unless indicated otherwise in the note on individual C1427m057 |stars. C1427m057 |Salinas et al. (2012) studied the spatial distribution of the blue C1427m057 |stragglers in NGC 5634, as well as in three other Sagitarrius dwarf C1427m057 |galaxy GCs: Arp 2, Pal 12 and Terzan 8. C1436m263 |All of the data in the above table are from the discovery paper by C1436m263 |Rodrigues de Andrade et al. (2012). No variables were detected in the C1436m263 |earlier photographic searches by Baade (1934) or Hazen (1996). C1452m820 |IC 4499 is a unique cluster because it has a high frequency of RR Lyrae C1452m820 |variables. Also IC 4499 and M3 are the only Galactic Oosterhoff type I C1452m820 |clusters that have double-mode RR Lyrae (RR01) variables. C1452m820 |The RA and dec n the above table are from Samus et al. (2009). C1452m820 |All of the periods, magnitudes and amplitudes in the above table C1452m820 |were taken from the paper by Walker & Nemec (1996). In addition, C1452m820 |the variability types we have listed for all of the stars classified C1452m820 |as RR0, RR01, RR1, RR2 and SXPHE are the types adopted by Walker & Nemec. C1500m328 |The periods, magnitudes, amplitudes and classifications for V1-27 are C1500m328 |from the study by Rosino (1961). However, Rosino noted that there is a C1500m328 |constant zero-point error in the magnitudes that he derived. C1500m328 |The RA and dec are from the paper by Samus et al. (2009). C1500m328 |A BV colour magitude diagram by Brocato et al. (1996) shows a well C1500m328 |defined blue HB. Saviane et al. (2010) showed evidence for an intrinsic C1500m328 |internal abundance spread among giant branch stars in NGC 5824. C1513p000 |Pal 5 is a sparsely populated cluster. According to Odenkirchen et al. C1513p000 |(2003), tidal tails associated with Pal 5 can be traced over an arc of C1513p000 |10 degrees on the sky. C1513p000 |The RA and dec in the above table are from Samus et al. (2009). C1513p000 |The periods, magnitudes, amplitudes and variablity types in the above C1513p000 |table are from Kinman & Rosino (1962 - Table 1). Vivas et al. (2004) C1513p000 |derived periods that were significantly for V1, V3 and V4, but concluded C1513p000 |that the periods of Kinman & Rosino (1962) were more reliable because C1513p000 |their observartions were more extensive.. C1514m208 |The RA and dec are from Samus et al. (2009). The remaining data are C1514m208 |from Clement & Rowe (2001) unless indicated otherwise in the notes on C1514m208 |individual variables. C1514m208 |The RR2 classifications for V7, V8, V12, and V13 were made by Clement & C1514m208 |Rowe (2001). However, these are now called into question. These C1514m208 |four stars are probably first overtone pulsators. They all have periods C1514m208 |and amplitudes comparable to Omega Cen variables that were previously C1514m208 |considered to be RR2 variables. However, after Kaluzny et al. (2004) C1514m208 |derived (B-V) colours for the Omega Cen variables, it was clear that C1514m208 |these Omega Cen stars were RR1 variables. C1516p022 |The RA and dec for V1-169 are from Samus et al. (2009) C1516p022 |All the data for V170-181 are from Arellano Ferro et al. (2015). C1516p022 |Most of the periods, amplitudes, magnitudes and classifications for C1516p022 |V1-169 are from the study by Kaluzny et al. (2000). Otherwise, the source C1516p022 |is indicated in the remarks column: C1516p022 | Oost refers to Oosterhoff (1941) whose study was based on C1516p022 | photographic observations. These stars are generally C1516p022 | outside of the field of view of the CCD investigations of M5. C1516p022 | Storm refers to Storm et al. (1991) C1516p022 | Reid refers to Reid (1996) C1516p022 | RSPO refers to Rabidoux et al. (2010) C1516p022 | Kal99 refers to Kaluzny et al. (1999) C1516p022 | Krav92 refers to Kravtsov (1992) C1516p022 | Olech refers to Olech et al. (1999) C1516p022 | Cap refers to Caputo et al. (1999) C1516p022 | OlCap indicates the periods are from Olech et al. (1999) and the C1516p022 | remaining data are from Caputo et al. C1516p022 | Samus refers to Samus et al. (1999) C1516p022 | Ar refers to Arellano Ferro et al. (2015). C1516p022 | ArRd indicates that the position is from Arellano Ferro et al. (2015) C1516p022 | and the remaining data are from Reid (1996). C1516p022 | ArSz indicates that the position is from Arellano Ferro et al. (2015) C1516p022 | and the period is from Szeidl et al. (2011). C1516p022 | DS refers to Drissen & Shara (1998) C1516p022 |Coppola et al. (2011, 2012) made J, K-band time series observations of C1516p022 |the RR Lyrae variables and derived PLK and PLJ relations. C1524m505 |The RA and dec are from Samus et al. (2009). All of the remaining data C1524m505 |are from Lloyd Evans & Menzies (1977). Lloyd Evans & Menzies also C1524m505 |listed magnitudes and colours for two additional red variables that were C1524m505 |probable non-members. C1531m504 |The RA and dec for the variables are from Samus et al. (2009). The C1531m504 |remaining data are from Liller (1983) who also presented data for 12 C1531m504 |field variables in the cluster vicinity. C1531m504 |NGC 5946 has not been well studied. It is a difficult cluster to observe C1531m504 |because it lies near the galactic plane and is heavily reddened. In the C1531m504 |2010 update to his catalogue of GC parameters, Harris (1996) lists C1531m504 |[Fe/H] =-1.29 based on observations by Armandroff & Zinn (1988) and a C1531m504 |CMD published by Alcaino et al. (1991) shows a predominantly blue HB. On C1531m504 |the basis of the giant branch slope, both Alcaino et al. (1991) and C1531m504 |Davidge (1985) have concluded that the metallicity of this cluster is C1531m504 |lower than generally assumed. C1542m376 |The CM diagram of NGC 5986 has a predominantly blue HB (Alves et al. C1542m376 |2001). C1542m376 |In the above table, the RA and dec for V1-12 are from Samus et al. (2009). C1542m376 |The remaining data for stars with V mags listed are from Alves C1542m376 |et al. (2001). For stars outside their field of view, the B data from C1542m376 |Liller & Lichten (1978) are listed. C1542m376 |All the data for V13 are from the discovery paper by Matsunaga et al. C1542m376 |(2006). C1607m551 |This was thought to be an open cluster until Ortolani et al. (1993) C1607m551 |showed it to be a thick disk globular cluster. C1607m551 |A VI CM diagram by Sarajedini et al. (2007) shows a prominent HB red C1607m551 |clump. C1607m551 |The data listed for V1 are from Sloan et al. (2010) who conclude that it C1607m551 |is a carbon star, but probably a cluster member. C1608p150 |A CM diagram by Da Costa et al. (1982, ApJ 257, 633) C1608p150 |indicates that the HB stars are red. C1608p150 |This is confirmed in a more recent paper by Dotter et al. C1608p150 |(2008, AJ 136, 1407) C1608p150 |Rosino & Ortolani C1608p150 |(1985, Mem Soc Ast It, 56, 113) stated that further C1608p150 |observations would be required to determine if the cluster C1608p150 |has any variables. C1614m228 |The data for V1-33 are from Kopacki (2013) unless indicated otherwise in C1614m228 |the notes on individual stars (e.g. V6, V7, V11, V12) C1614m228 |Four of the RR Lyrae variables, (V10, V17, V19, V20), were observed by C1614m228 |Figuera Jaimes et al (2016) who made small revisions to the periods. C1614m228 |FJ in the remarks column indicates that the period was derived by them. C1614m228 |The data for V34-40 are from Figuera Jaimes et al. (2016). C1614m228 |For the Nova, the RA and dec are from Dieball et al. (2010). It is their C1614m228 |X-ray source CX01. The maximum visual apparent magnitude was derived by C1614m228 |Sawyer (1938 - see page 75), based on the estimates of 7.0 and 6.5 by C1614m228 |Auwers and Luther respectively, on May 21, 1860. C1620m264 |V1-92, V111-112 C1620m264 |Stetson et al. (2014) investigated all of the variables numbered V1-92 C1620m264 |and V111-112; the RA and dec for most of these stars are from their C1620m264 |study. For stars with "Sam" indicated in the "remarks" column, the C1620m264 |RA and dec are from Samus et al. (2009). C1620m264 |The remaining data for these stars are also from Stetson et al. (2014) C1620m264 |unless indicated otherwise in the "Notes on individual stars". C1620m264 |If K13a/K13b is listed in the "Remarks column, the periods, magnitudes, C1620m264 |amplitudes and classifications are from Kaluzny et al. (2013a/b). C1620m264 |V93-109 (= N1, N2, etc.) C1620m264 |All of the data for these variables are from the discovery paper by C1620m264 |Nascimbeni et al. (2014). They noted that the V magnitudes they C1620m264 |listed were obtained by cross-matching their catalogue with that of C1620m264 |Sarajedini et al. (2007) and do not represent the intensity-weighted C1620m264 |averages derived from light curves. The V amplitudes listed for these C1620m264 |variables in the above table were read from the light curves plotted in C1620m264 |Figures 4 and 5 of the Nascimbeni et al. paper. They established C1620m264 |membership status for their new variables by estimating proper motions C1620m264 |from HST observations made at two epochs separated by ~6 years. C1620m264 |Other proper motion/membership studies of stars in M4 have been carried C1620m264 |out by Cudworth & Rees (1990) and by Zloczewski et al. (2012). C1620m720 |The most comprehensive studies of the RR Lyrae in NGC 6101 were by Cohen C1620m720 |et al. (2011) and Fitzgerald et al. (2012). The Cohen observations were C1620m720 |obtained on 6 consecutive nights in July 2008 and the Fitzgerald C1620m720 |observations were made on 31 nights between June 2010 and April 2011. C1620m720 |The variables V1-10, V20, V22 were studied by both groups and for these C1620m720 |stars, we adopt the periods derived by Fitzgerald et al. and the RA, dec, C1620m720 |magnitudes and amplitudes from Cohen et al. C1620m720 |All the data for V16-19 and V21 are from Cohen et al. (2011) and the C1620m720 |data for V23 are from Fitzgerald et al. (2012). C1620m720 |The RA and dec for V11-15 are from Samus et al. (2009) and the remaining C1620m720 |data for these stars are from the discovery paper by Liller (1981) C1620m720 |Sarajedini & Da Costa (1999) showed that NGC 6101 has a significant blue C1620m720 |straggler population, but no variable star searches have yet been C1620m720 |undertaken among the BSS population. C1624m259 |Neely et al. (2000) pointed out that the cluster is located in the C1624m259 |region of the Rho Ophiuchus dust cloud and it seems that both of the C1624m259 |variables are irregular, eruptive variables associated with the nebula. C1624m259 |The RA and dec in the above table are from Samus et al. (2009). C1624m259 |The remaining data are from the GCVS, based on the study of C1624m259 |Satyvoldiev (1982). V1 shows short term variations. C1624m387 |The RA and dec are from Samus et al. (2009). The remaining data are C1624m387 |from Hazen (1991). The long period variabes V1-3 are brighter than the C1624m387 |RR Lyrae variables and are considered to be cluster members. The C1624m387 |candidate cataclysmic variable had one outburst and was below the plate C1624m387 |limit (Bmag > 19.6) the rest of the time. C1625m352 |Terzan 3 is a low concentration cluster projected on the outskirts of C1625m352 |the Galactic bulge. A near infra-red CM diagram (K, J-K) by Valenti et C1625m352 |al. (2007) shows a red clumpy HB indicative of a moderately high C1625m352 |metallicity. They used their data to derive a photometric [Fe/H] = C1625m352 |-0.82. This is in good agreement with the value [Fe/H]= -0.75 that Cote C1625m352 |(1999) derived by measuring the equivalent width of an FeI spectral line C1625m352 |in a few red giants. C1629m129 |Periods, magnitudes and variability types are from Clement & C1629m129 |Shelton (1997) unless designated "Dkns" in the remarks column C1629m129 |(see V2, V3, V5, V11, V13, V16). For these stars, this C1629m129 |information is from Dickens (1970). C1629m129 |The RA and dec are from Samus et al. (2009) unless indicated otherwise C1629m129 |in the Notes on individual stars. C1629m129 |Cudworth et al. (1992) derived membership probabilities for some of the C1629m129 |RR Lyrae variables in NGC 6171 from a proper motion study. C1636m283 | Bica et al. (1999, A&A Supp 136, 363) published C1636m283 | a VI color-magnitude diagram and confirmed C1636m283 | that this object is a poorly populated globular C1636m283 | cluster wth evidence of depletion at the lower C1636m283 | main sequence. The morphology of the HB is C1636m283 | "not purely red". C1636m283 | More recently, Cornish et al. (2006, AJ 131, 2543) C1636m283 | published a VI CMD and found the features were C1636m283 | consistent with the Bica et al. diagram. C1639p365 | A major paper on the variables in M13 was written by C1639p365 | Kopacki et al. (2003, A&A 398, 541). They investigated C1639p365 | all of the variables numbered up to V45, with the exception of C1639p365 | V14, 16, 20, 32 and 33 which were not in their field of view. C1639p365 | These authors also published RA and dec (J2000) and C1639p365 | an ID chart for the variable stars in their investigation. C1639p365 | The positions, periods, magnitudes, amplitudes and classifications C1639p365 | for V1-45 in the above table are from the Kopacki et al. paper C1639p365 | unless indicated otherwise in the Notes. C1639p365 | A designation "Os" in the Notes/Remarks column indicates that the C1639p365 | periods, magnitudes, amplitudes and classifications are from a paper C1639p365 | by Osborn et al. (2017). Their paper deals with the long period C1639p365 | variables in M13, i.e. the variables classified as type SR and L. C1639p365 | The data for the remaining variables are from the discovery papers C1639p365 | unless indicated otherwise in the Notes. C1639p365 | Cudworth & Monet (1979) and Cudworth (1979) derived membership C1639p365 | probabilities for stars in M13. C1644m018 |V1: Period, magnitude, amplitude and classification for V1 C1644m018 | from Clement et al. (1988) The RA and dec are from Samus C1644m018 | et al. (2009). C1644m018 |V2: All the data for vB1 are from the paper by von Braun et al. C1644m018 | (2002) C1645p476 |The data in the above table are all from Arellano Ferro et al. (2015) - C1645p476 |except for the stars classified as "CST". For these stars, "Sam" in C1645p476 |the remarks column indicates that the RA and dec are from Samus et al. C1645p476 |(2009). C1650m220 |The periods, amplitudes and classifications for V1-5 are from Liller's C1650m220 |(1977) photographic investigation and the B magnitudes are derived from C1650m220 |Liller's (1980) revised calibration of the magnitudes. C1650m220 |The RA and dec are from Samus et al. (2009). C1650m220 |Howland et al. (2003) published a CCD CM diagram which showed a C1650m220 |predominantly blue HB. They pointed out that the cluster is in the C1650m220 |Ophiuchus-Scorpius region and therefore subject to differential reddening. C1654m040 | C1654m040 | The RA and dec for V1-4 are from Samus et al. (2009) C1656m370 |NGC 6256 is a heavily reddened core-collapsed cluster in the Galactic C1656m370 |bulge. A VI CM diagram by Ortolani et al. (1999) shows an extended blue C1656m370 |HB with no evidence for a red HB. Their diagram does not extend faint C1656m370 |enough to define a blue straggler region. C1656m370 |Stephens & Frogel (2004) estimated [Fe/H] = -1.35 +/- 0.09 from a C1656m370 |spectroscopic study of 5 giant stars. C1656m370 |The data for V1 are from the discovery paper by Matsunaga et al. (2006). C1657m004 |A variable star search of Pal 15 was carried out by Kinman & Rosino (1962). C1657m004 |In their paper, the cluster was referred to as "Anon". C1657m004 |They searched 9 photographic plates which had a limiting magnitude of C1657m004 |m_pg=22 mag. No variables were found. C1657m004 |A CM diagram by Harris (1991) based on CFHT data shows a blue HB and a C1657m004 |significant number of blue stragglers. This result was later confirmed C1657m004 |by Dotter et al. (2011) who used HST data. C1658m300 |Contreras (October 2013 - private communication) has pointed out that C1658m300 |there are some problems with the coordinates published in their paper C1658m300 |(Contreras et al. 2010). They intend to publish an erratum soon. C1658m300 |The data listed for V1-262 in the above table are from Contreras et al. C1658m300 |(2010) unless the stars are indicated by "vA" in the Notes/Remarks C1658m300 |column. C1658m300 |The "vA" stars were outside the fields that Contreras et al. analysed. C1658m300 |Their periods and classification types are from van Agt & Oosterhoff C1658m300 |(1959), and their magnitudes and amplitudes are from Sawyer Hogg's C1658m300 |3rd (1973) catalogue. She received the data from van Agt (1971, C1658m300 |Private Communication). C1658m300 |The RA and Dec listed for the "vA" variables are the values published C1658m300 |by Samus et al. (2009). Some of the variables investigated by van Agt & C1658m300 |Oosterhoff are beyond the tidal radius (8.97 arcmin, listed by Harris in C1658m300 |the 2003 edition of his on-line catalog) and these are indicated as C1658m300 |possible field stars (f?). C1658m300 |A serious problem in investigations of M62 is the differential reddening C1658m300 |across the field. However, Contreras et al. (2010) have addressed this C1658m300 |problem by deriving the colour excess E(B-V) for the RR Lyrae variables C1658m300 |by measuring their (B-V) colour at minimum light. C1659m262 |All of the RA and dec in the above table are from Samus et al. (2009). C1659m262 |The remaining data are from Clement and Sawyer Hogg (1978). C1701m246 |The RA and dec listed in the above table are from Samus et al. (2009). C1701m246 |Samus et al. also noted that V10 and V11 are V2121 and V2123 Oph. C1701m246 |The remaining data were taken from Clement et al. (1980) C1701m246 |A BV color-magnitude diagram by Piotto et al. (2002) indicates a C1701m246 |pronounced blue HB which is a characteristic of globular clusters that C1701m246 |have type II Cepheids (CW stars). Clusters with Mira variables C1701m246 |generally have red HBs. Also, based on the frequency distribution of C1701m246 |Miras in the surrounding field, it is unlikely that either of the Mira C1701m246 |variables, V10 or V12, are cluster members. C1702m226 |The RA and dec in the above table are from Samus et al. (2009). C1702m226 |All of the other data are taken from Stetson & West (1994). C1702m226 |This cluster lies in the Galactic plane and is subject to considerable C1702m226 |differential reddening. C1702m226 |HST CM diagrams by Fulton et al. (1999) and by Lee et al. (2001) C1702m226 |show a predominantly blue HB and a blue straggler sequence. C1707m265 |The RA and dec for all the variables are from Samus et al. (2009). The last C1707m265 |four variables in the above table were assigned the numbers V9-12 in the C1707m265 |Samus et al. catalogue. C1707m265 |The remaining data in the above table were taken from Clement et al. (1982). C1707m265 |Clement et al. concluded that the Mira variables were not cluster members C1707m265 |on the basis of the cluster's low metallicity and the frequency distribution C1707m265 |of Mira variables in the surrounding field. C1707m265 |A BV color-magnitude diagram by Piotto et al. (2002) indicates a C1707m265 |pronounced blue HB. Clusters with Mira variables generally have red HBs. C1707m265 |Thus it is unlikely that the Mira variables are cluster members. C1707m265 |Discovery of the variable stars in NGC 6293: C1711m294 |The cluster NGC 6304 is a metal rich cluster located in a rich field C1711m294 |in the galactic bulge. C1711m294 |The first investigations of variable stars were by Rosino (1962) and C1711m294 |Terzan (1966, 1968), but no periods were derived by either of these C1711m294 |authors. C1711m294 |A later study of the variables in NGC 6304 and the surrounding C1711m294 |field was by Hartwick et al. (1981). They derived periods for the 40 C1711m294 |RR Lyrae stars in their field and identified a number of other suspected C1711m294 |variables, many of which they classified as long period variables. C1711m294 |It is generally assumed that most of the variables belong to the field C1711m294 |around NGC 6304 and not to the cluster itself. C1711m294 |De Lee et al. (2006) carried out a new study of the RR Lyrae variables C1711m294 |to investigate the possibility that some of them might be cluster C1711m294 |members in light of the discovery of long period RR Lyrae variables C1711m294 |in the metal rich clusters NGC 6388 and NGC 6441. They estimated the C1711m294 |membership status based on distance from the cluster, mean C1711m294 |magnitude and reddening. C1711m294 |The membership status listed for the RR Lyrae variables is based on C1711m294 |their study. C1711m294 |For RR Lyrae stars with V magnitudes listed in the above table, the C1711m294 |periods, magnitudes and amplitudes are from the OGLE III catalogue C1711m294 |(Sosyzynski et al. 2011). C1711m294 |The periods, classifications and membership status for V5-6, V8-9 and C1711m294 |V11-21 are from Hartwick et al. (1981). C1711m294 |The RA and dec in the above table for V1-21 are from Samus et al. (2009) C1711m294 |and for V22-24 from (Sosyzynski et al. 2011). C1713m280 |The periods, magnitudes, amplitudes, classifications, and membership C1713m280 |status are from the discovery paper by Layden et al. (2003). C1713m280 |The RA and dec for the four variables V14, V15, V18, V19 are from the GCVS C1713m280 |where they are listed as V2719 Oph, V2721 Oph, V2718 Oph and V2720 Oph C1713m280 |respectively. C1713m280 |For the remaining variables, the RA and dec are from matches C1713m280 |with 2MASS sources. Initially, provisional values were calculated from C1713m280 |relationships derived by Layden et al. (2003): C1713m280 |Delta RA = -0.396*(X_pix - 1059); Delta dec = -0.396*(Y_pix - 993). C1713m280 |For these calculations, the cluster centre was assumed to be 17:16:37.3, C1713m280 |-28:08:24.4, the value published in the 2010 version of the Harris (1996) C1713m280 |catalogue. The provisional coordinates and the 2MASS coordinates C1713m280 |agreed to within 1 arcsec for all the variables except V11 for which the C1713m280 |difference was 3 arcsec. C1714m237 |This cluster is embedded in a crowded field in the Galactic bulge. C1714m237 |According to the 2010 version of the Harris (1996) catalogue, it is a C1714m237 |core collapsed cluster with [Fe/H] = -1.25. C1714m237 |BVI photometry by Ortolani et al. (2003) shows a prominent blue HB C1714m237 |with evidence for a blue tail. C1714m237 |The data for V1 and 2 are from the discovery paper by Matsunaga et al. C1714m237 |(2006). C1715p432 |A good summary of investigations of the variable stars in M92 was given C1715p432 |by Kopacki (2001). C1715p432 |V1-32 C1715p432 |The RA and dec are from Samus et al. (2009). C1715p432 |The periods, magnitudes, amplitudes and classifications are from Kopacki C1715p432 |(2001) unless indicated otherwise in the notes on individual stars. C1715p432 |V14 and V16 were outside his field of view. C1715p432 |V33-39 C1715p432 |All the data are from Kopacki (2007). C1716m184 |The most comprehensive study of the variables in M9 is a paper by C1716m184 |Arellano Ferro et al. (2013). All of the material in the above table is C1716m184 |from their study unless indicated otherwise in the notes. C1716m184 |A serious problem in deriving the magnitudes and colours of the stars C1716m184 |in M9 is that the cluster is subject to differential reddening. There is C1716m184 |a heavy obscuring cloud to the southwest of the cluster. This can be C1716m184 |detected on the photograph published by Clement et al. (1984) and is C1716m184 |even more marked on the E and O plates of the Palomar Sky Survey. C1716m184 |Arellano et al. (2013) used a reddening map by Alonso-Garcia et al. C1716m184 |(2012) to correct for this effect. C1716m184 |V3, V7, V12 and V13 appear in the Moscow GCVS as V1864, V1845, V1840 and C1716m184 |V2208 Oph respectively. C1718m195 |A CM diagram based on VI photometry by Heitsch & Richtler (1999) shows C1718m195 |a pronounced red HB. C1718m195 |According to the 2010 version of the Harris (1996) catalogue, NGC 6342 C1718m195 |is a core collapsed cluster with [Fe/H] = -0.55. C1718m195 |A binary radio pulsar PSR B1718-19 was discovered in the field of C1718m195 |NGC 6342 by Lyne et al. (1993). It has an unusally long period (1 sec) C1718m195 |for a binary pulsar associated with a globular cluster. (Pulsars in C1718m195 |binary systems in globular clusters are usually millisecond pulsars.) C1718m195 |van Kerkwijk et al. (2000) and Janssen & van Kerkwijk (2005) discussed C1718m195 |scenarios for the formation of such a system. Their preferred C1718m195 |explanation is that the system formed when a dormant pulsar in the C1718m195 |cluster core had an interaction with a binary. C1720m177 |The RA and dec for the variables are from Samus et al. (2009). C1720m177 |V1-6: Periods, magnitudes, amplitudes, variability types for V1-6 C1720m177 | are from Clement & Sawyer Hogg (1977) C1720m177 | C1720m177 | Membership status for V3 is based on a radial velocity study by C1720m177 | Feast (1972). Possible field status for V4 is from Lloyd Evans C1720m177 | & Menzies (1973) and for V6 from Clement & Sawyer Hogg (1977). C1720m177 | With a distance of 9.8 arcmin from the cluster centre, V6 is C1720m177 | outside the tidal radius of 9.3 arcmin (Harris 1996 - 2010 C1720m177 | update). C1720m177 |V7-10: Magnitudes and amplitudes for V7-10 are from Lloyd Evans C1720m177 | & Menzies (1977). They classified these stars as red variables. C1720m177 | Since the GCVS does not use this term, we have classified them C1720m177 | as Lb. C1720m263 |NGC 6355 is embedded in a crowded field in the Galactic bulge. C1720m263 |Chen & Chen (2007) used the 2MASS Point Source Catalogue to study shapes C1720m263 |of clusters and concluded that NGC 6355 is suffering from strong tidal C1720m263 |distortion. C1720m263 |According to the 2010 version of the Harris (1996) catalogue, NGC 6355 C1720m263 |is a core collapsed cluster with [Fe/H] = -1.37. C1720m263 |Soszynski et al. (2014) listed a radius of 2.1 arcminutes for NGC 6355 C1720m263 |and the variable stars are all well within that boundary. C1720m263 |BVI photometry was published by Ortolani et al. (2003). Their CM diagram C1720m263 |shows a prominent blue HB. C1721m484 |The RA and dec listed above are from Samus et al (2009). C1721m484 |CM diagrams by Hartwick & Hesser (1972) and by Fullton et al. (1995) C1721m484 |show a red HB and a blue straggler sequence. C1724m070 |We assigned the "IAU nomenclature" name for this cluster on the basis C1724m070 |of its 1950 position. C1724m070 |IC 1257 has only been recognized as a Galactic globular cluster C1724m070 |since Harris et al. (1997) published a CM diagram which reveals that it C1724m070 |is a highly reddened luster well beyond the Galactic centre. C1724m070 |The diagram shows a well defined blue HB, but the observations do not C1724m070 |extend faint enough to show the subgiant region or main sequence turnoff. C1725m050 |The RA and dec for V1 and V2 are from Lloyd et al. (2008). C1725m050 |The RA and dec for V3-8 were derived by Arellano Ferro (2014 - C1725m050 |private communication) by locating their images in the ALADIN sky C1725m050 |atlas. The remaining data for V3-8 are from Arellano Ferro et al. C1725m050 |(2008). C1726m670 |The periods, magnitudes, amplitudes and classifications for V1-37 C1726m670 |are from Olech et al. (2001) and for V38-52 are from Mazur et al. C1726m670 |(1999). The non-membership status of the EC variables V43, 45 and 52 C1726m670 |was confirmed by Rucinski (2000). C1726m670 |The RA and dec for most of V1-52 are from Samus et al. (2009); the C1726m670 |exceptions are V11, 23, 24, 26, 28, 29, 32 and 38-41 which are from C1726m670 |Mazur et al. (1999). C1727m299 |A VI colour-magnitude diagram by Ortolani et al. (1997) shows an C1727m299 |extended blue HB. Barbuy et al. (2016) derived [Fe/H] = -1.06. C1727m299 |The RA and dec for V1 to 15 were derived by Samus et al. (2009) who C1727m299 |considered them all to be field stars. C1727m299 |They are all listed in the Moscow NSV catalogue and their NSV numbers C1727m299 |are indicated in the remarks column of the above table. C1727m299 |The data for V16 and 17 are from the discovery paper by Matsunaga et al. C1727m299 |(2006). C1727m315 |Terzan 4 is a heavily reddened cluster in a rich field in the Galactic C1727m315 |bulge. Valenti et al. (2010) published a near infra-red CM diagram C1727m315 |(K, J-K) which is heavily contaminated by stars in the surrounding metal C1727m315 |rich field population. When looking at stars within 40 arcsec of the C1727m315 |cluster centre, they detected a blue HB. C1727m315 |They used their data to derive a photometric [Fe/H] = -1.58, in good C1727m315 |agreement with the [Fe/H]=-1.6 published by Stephans & Frogel (2004) and C1727m315 |by Origlia & Rich (2004) from studies based on high-resolution IR C1727m315 |spectroscopy. C1730m333 |This cluster, located in the error box of the X-ray burster MXB 1730-33, C1730m333 |was discovered by Liller (1977) on deep plates taken in the near IR with C1730m333 |the CTIO 4 metre telescope. C1730m333 |It was subsequently found by Tam et al. (2011) to be a Gamma-ray C1730m333 |emitting cluster C1730m333 |An infrared colour magnitude diagram by Ortolani et al. (2001) showed C1730m333 |a red HB morphology, characteristic of a metal rich population and C1730m333 |Origlia et al (2002) derived [Fe/H] = -0.3, based on H-band echelle C1730m333 |spectra of two of the brightest giant stars in the cluster. C1730m333 |Thus it is unlikely that there will be any RR Lyrae or Cepheid C1730m333 |variables. The cluster lies in a heavily reddened field near the C1730m333 |Galactic centre with V(HB) = 24.84 according to the 2010 version of C1730m333 |the Harris (1996) catalogue. Blue stragglers would be too faint to C1730m333 |be detected. C1731m390 |NGC 6380 is a metal rich bulge cluster. According to the 2010 version C1731m390 |of the Harris (1996) catalogue, it has [Fe/H] = -0.75 and is probably a C1731m390 |core collapsed cluster. C1731m390 | C1731m390 |VI photometry by Ortolani et al. (1998) showed a red HB morphology. C1731m390 |Thus it is unlikely that there will be any RR Lyrae or Cepheid C1731m390 |variables. The existing photometry does not extend to a faint enough C1731m390 |level to delineate a blue straggler region. C1731m390 |Discovery of the variable star in NGC 6380: C1731m390 | V1 C1731m390 | Fourcade et al. (1966) with x,y coordinates and an ID chart C1731m390 | The RA and dec for V1 were drived by Samus et al. (2009). C1731m390 | No further data are available for this star. C1732m304 |Terzan 1 is a highly obscured cluster in the Galactic bulge. C1732m304 |CM diagrams published by Ortolani et al. (1999) and by Valenti et al. C1732m304 |(2010) show a red HB. Valenti et al (2015) derived a metal abundance, C1732m304 |[Fe/H]=-1.26. C1732m304 |*The RA and dec listed for the cluster centre are from the 2003 version C1732m304 |of the Harris (1996) catalogue. The dec Harris listed in 2010 (-30:28:11) C1732m304 |is too far north. C1732m304 |The data for the RR Lyrae variables in the above table are from the C1732m304 |OGLE IV investigation by Soszynski et al. (2014). In the above table, C1732m304 |the only OGLE variables listed are the ones that are located less C1732m304 |than 1.4 arcminutes from the cluster centre. Soszynski et al. (2014) C1732m304 |listed a radius of 1.2 arcminutes for the cluster. The Note below for C1732m304 |V14 explains why the threshold has been set at 1.4 arcminutes. C1732m304 |V1, V2 and V3 are also located within 1.4 arcminutes of the cluster C1732m304 |centre, but V4 is more distant (1.83 arcmin). The RA and dec for V1-4 C1732m304 |are from Samus et al. (2009). C1732m447 |NGC 6388 is a massive Galactic bulge cluster with [Fe/H]= -0.55 C1732m447 |according to the 2010 version of the Harris (1996) catalogue. Pritzl et C1732m447 |al. (2002) discovered that it had a significant number of RR Lyrae C1732m447 |variables with relatively long periods, an unexpected result for such a C1732m447 |metal rich cluster. NGC 6388 shares these properties with NGC 6441. C1732m447 |Bellini et al. (2013) have examined the CM diagrams for both clusters C1732m447 |and provided evidence that both clusters host at least two stellar C1732m447 |populations. C1732m447 |The RA and dec in the above table are from the following sources C1732m447 |V1-26 and V28 from Samus et al. (2009). C1732m447 |V70-121 and the variables indicated by "Sk" in the remarks column C1732m447 |from Skottfelt et al. (2015). C1732m447 |For the remaining variables, the RA and dec were derived from the Delta RA C1732m447 |and Delta dec coordinates published by Pritzl et al. (2002) or by Corwin C1732m447 |et al. (2006). For these calculations, it was assumed that the position C1732m447 |of the cluster centre was RA=17:36:17.15 and dec=-44:44:06.9. These C1732m447 |coordinates for the cluster centre yielded RA and dec in agreement with C1732m447 |the values that Samus et al. derived for V1-26 and matched with the C1732m447 |2MASS catalogue. C1732m447 |The remaining data for V1-73 in the above table are from Pritzl et al. C1732m447 |(2002) unless designated LM, Sl, HH, Corw or Sk in the remarks column, C1732m447 |in which case they are from Lloyd Evans & Menzies (1977), Sloan et al. C1732m447 |(2010), Hazen & Hesser (1986), Corwin et al. (2006) or Skottfelt et al. C1732m447 |(2015). C1732m447 |Most of the "HH" variables are considered to be field variables because C1732m447 |they are outside the tidal radius which is 6.75 arcmin according to the C1732m447 |2010 version of the Harris (1996) catalogue. C1732m447 |All the data for V74-V121 are from the discovery paper by Skottfelt et C1732m447 |al. (2015). C1733m390 |VI photometry by Bica et al. (1996) shows the colour-magnitude diagram C1733m390 |has a red HB and indicates that the cluster is metal rich, [Fe/H] = ~-0.6. C1733m390 |Their photometry extended to the main sequece turn-off region and showed C1733m390 |a blue straggler population. However, they did not carry out a variable C1733m390 |star search and did not discuss the known variable stars. C1735m032 |There are two major papers summarizing the properties of the variables C1735m032 |in M14: Wehlau & Froelich (1994) and Conroy et al. (2012). C1735m032 |Another major study is currently being undertaken by Contreras Pena and C1735m032 |collaborators who published a BV color-magnitude diagram (Contreras Pena C1735m032 |et al. 2013). C1735m032 |Wehlau & Froelich provided a good summary of variables V1-93. They C1735m032 |published ID charts for all except V28 which was outside the field of C1735m032 |their chart. In addition, they listed mean B magnitudes, (B-V) colours C1735m032 |and B amplitudes for all of the stars they classified as pulsating. C1735m032 |Their paper also included an appendix with notes on many of the C1735m032 |individual stars, including all of the catalogued variables that they C1735m032 |were unable to classify. C1735m032 |Conroy et al. applied the image subtraction technique to a set of images C1735m032 |obtained on 11 nights in June and July, 2010. They confirmed the C1735m032 |variability of 61 of the variables discussed by Wehlau & Froelich (1994) C1735m032 |and identified 71 new ones which they numbered V94-164. C1735m032 |In addition, they listed RA and dec, derived periods and plotted light C1735m032 |curves for all of the stars they found to be variable. C1735m032 |All the data for V94-V164 are from their study. C1735m032 |V1-V93: C1735m032 |In the above table, the periods and variability types for stars with C1735m032 |periods greater than a day are from Wehlau & Froelich (1994) and for C1735m032 |stars with periods less than a day they are are from Conroy et al. C1735m032 |(2012), unless indicated otherwise in the notes on individual stars. C1735m032 |The B magnitudes and amplitudes are from Wehlau & Froelich's paper C1735m032 |because Conroy et al. did not derive any magnitudes. C1735m032 |The non-variable ("CST") classifications are based on the fact that C1735m032 |Conroy et al. did not detect any variability. In most of these cases, C1735m032 |Wehlau & Froelich (1994) had already indicated that the stars might not C1735m032 |be variable. C1735m032 |The numbers designated by "C" in the remarks column refer to the C1735m032 |numbering system of Conroy et al. C1735m032 |The RA and dec for the stars investigated by Conroy are their values. C1735m032 |For the remaining stars, i.e., V27 and V28, which were outside their C1735m032 |field of view, and the stars for which Conroy et al. did not detect C1735m032 |variability, the RA and dec are from Samus et al. (2009). C1735m032 |There is a systematic offset between the RA values of Samus and Conroy in C1735m032 |the sense that Samus' values are on average 0.2 seconds larger. Their C1735m032 |dec values agree to within 1 arcsec. C1735m238 |NGC 6401 is located in a rich, heavily reddened field in the Galactic bulge. C1735m238 |This is illustrated in a VI CM diagram published by Barbuy et al. (1999). C1735m238 |It is very "noisy" due to differential reddening and contamination from C1735m238 |field stars. Nevertheless, Barbuy et al. concluded that the cluster has C1735m238 |a red HB. C1735m238 |The most comprehensive investigation of the variable stars in NGC 6401 C1735m238 |was by Tsapras et al. (2017) who searched for variables in a 15.8 C1735m238 |by 15.8 arcminute field centred on the cluster - down to a limiting C1735m238 |magnitude of V~19.5 mag. C1735m238 |The field around the cluster was also included in the OGLE IV Galactic C1735m238 |Bulge survey. Results have been published for RR Lyrae variables C1735m238 |(Soszynski et al. 2014) and for eclipsing binaries (Soszynski et al. 2016). C1735m238 |The core radius and tidal radius listed by Harris (2010) are 0.25 and C1735m238 |12.24 arcminutes respectively. C1735m238 |However, it is unlikely that all the stars within the tidal radius are C1735m238 |cluster members. C1735m238 |In the above table, only stars within 2.4 arcminutes of the cluster C1735m238 |centre are included. This was the NGC 6401 radius listed by Soszynski C1735m238 |et al. (2014) and the radius adopted by Tsapras et al. (2017) for C1735m238 |their investigation as well. C1735m238 |V1-40: C1735m238 | The data in the above table are from Tsapras et al. (2017), unless C1735m238 | indicated otherwise in the notes on individual stars. C1735m238 | Most of these stars were also included in the OGLE IV survey. C1735m238 | Tsapras et al. (2017) listed the OGLE numbers in their tables. C1735m238 |V41-54: C1735m238 | All of these stars are eclipsing binaries and the data are from C1735m238 | the OGLE IV survey (Soszynski et al. 2016). In stars for which two C1735m238 | eclipses were observed, the amplitudes refer to the primary eclipses. C1736m536 |NGC 6397 is a core-collapsed globular cluster with at least 79 Chandra C1736m536 |X-ray sources within its half-mass radius. These sources are the C1736m536 |subject of numerous investigations. C1736m536 |Variability in the optical counterparts of some of these sources has C1736m536 |been detected (e.g. V12, V13, V16, V33, V34 in the above table), but C1736m536 |investigations continue and more variables may be identified in future. C1736m536 |In the above table, the RA and dec are from the following sources: C1736m536 |V1 (V639 Ara) and V2 (V825 Ara) from (Samus et al. (2009) C1736m536 |V3-V11 (Kaluzny 1997) C1736m536 |V12-V24 (Kaluzny & Thompson 2003) C1736m536 |V25-V36 (Kaluzny et al. 2006). C1736m536 |The remaining data for V3-36 are from Kaluzny et al. (2006) unless C1736m536 |indicated otherwise in the Notes/Remarks column where C1736m536 |K97 refers to Kaluzny (1997) and C1736m536 |KT refers to Kaluzny & Thompson (2003). C1740m262 |VI photometry by Ortolani et al. (1995) and JHK photometry by C1740m262 |Lee & Carney (2002) show the clear presence of a red horizontal branch. C1740m262 |The photometry does not extend deep enough to establish the existence of C1740m262 |a blue straggler sequence. C1740m262 |The metal abundance of Pal 6 is uncertain because the cluster lies in C1740m262 |a crowded metal rich star field near the Galactic Centre and field C1740m262 |contamination is a problem. The best estimates are based on infrared C1740m262 |spectroscopy of its brightest stars. C1740m262 |Stephens & Frogel (2004) derived [Fe/H]=-0.52 +/- 0.11 from medium C1740m262 |resolution K-band spectroscopy of 5 stars. C1740m262 |Lee et al. (2004) derived [Fe/H]=-1.0 +/- 0.1 from 3 stars based on C1740m262 |high resolution infrared echelle spectroscopy. They derived radial C1740m262 |velocities to ensure that the stars in their sample were cluster C1740m262 |members. C1740m262 |Terzan (1966) discovered 28 variables in the field around the cluster. C1740m262 |He informed Sawyer Hogg (1973) that none is a probable cluster member. C1740m262 |Sloan et al. (2010) announced a Mira variable with P=566 days at C1740m262 |RA =17:43:49.48, dec = -26:15:27.9 (2000), a distance of 2.67 arcmin from C1740m262 |the cluster centre, well within the tidal radius, which is 8.3 arcmin C1740m262 |according to the 2010 update to the Harris (1996) catalogue. However, C1740m262 |based on its observed K magnitude and circumstellar extinction, they C1740m262 |concluded that the Mira variable must be a foreground object and not C1740m262 |a cluster member. C1740m262 |Lynch & Ransom (2011) conducted a search for pulsars, but did not find C1740m262 |any in Palomar 6. C1742p031 |The RA and dec in the above table are from Samus et al. (2009) C1742p031 |The remaining data are from Papadakis et al. (2000) unless indicated C1742p031 |otherwise in the Notes/Remarks column where "Gru" refers to Grubissich C1742p031 |(1958). C1744m330 |This cluster lies in a crowded field near the Galactic centre. C1744m330 |A near IR (K, J-K) CM diagram was published by Valenti et al. (2010) C1744m330 |who estimated [Fe/H] = -1.51, based on the slope of the RGB. C1744m330 |The CM diagram indicated an HB red clump in the general field around C1744m330 |the cluster, but when only stars less than 20 arcsec from the cluster C1744m330 |centre were included, it disappeared. Thus the red clump is probably C1744m330 |due to field contamination. C1745m247 |The RA and dec for V1 and V2 are from Samus et al. (2009). C1745m247 |The remaining data for V1 are from Spinrad et al. (1974) and C1745m247 |for V2, they are from Sloan et al. (2010). C1745m247 |For V3-4 and V5-9, all the data are from the discovery papers: C1745m247 |Edmonds et al. (2001) and Sloan et al. (2010) respectively. C1745m247 |Origlia et al. (2011) showed that Terzan 5 has two stellar C1745m247 |populations with distinct iron abundances. Because the chemical C1745m247 |abundance patterns are unique, they propose that Terzan 5 is not a C1745m247 |true globular cluster, but a stellar system with a much more complex C1745m247 |history of star formation and chemical enrichment. The nature of the C1745m247 |Terzan 5 stellar system is a subject that continues to be discussed C1745m247 |in the literature. C1745m247 |Terzan 5 has more millisecond pulsars than any other globular cluster. C1746m203 |NGC 6440 is a heavily reddened metal rich cluster near the Galactic C1746m203 |centre. According to the 2010 update to the Harris (1996) catalogue, C1746m203 |it has [Fe/H] = -0.36 and a CM diagram by Piotto et al. (2002) based on C1746m203 |BV HST observations shows a prominent red HB. The CMD does not extend C1746m203 |as faint as the main sequence turnoff and has too much scatter to make C1746m203 |it possible to discern a blue straggler sequence. C1746m203 |Using Chandra observations, Pooley et al. (2002) found 24 X-ray sources C1746m203 |within the cluster half-mass radius and these have been discussed in C1746m203 |subsequent papers. Some of them may be LMXBs and others are probably C1746m203 |cataclysmic variables. C1746m203 |According to Paulo Freire's website, there are 6 millisecond pulsars in C1746m203 |NGC 6440. (www.naic.edu/~pfreire/GCpsr.html) C1746m370 |NGC 6441 is a massive metal rich cluster that is located in a rich C1746m370 |field in the Galactic bulge. Its [Fe/H]= -0.46 according to the 2010 C1746m370 |version of the Harris (1996) catalogue. C1746m370 |Layden et al. (1999) and Pritzl et al. (2001) discovered that it had a C1746m370 |significant number of RR Lyrae variables with relatively long periods, C1746m370 |an unexpected result for such a metal rich cluster. NGC 6441 shares C1746m370 |these properties with NGC 6388. C1746m370 |Bellini et al. (2013) have examined the CM diagrams for both clusters C1746m370 |and provided evidence that both clusters host at least two stellar C1746m370 |populations. C1746m370 |The RA and dec in the above table are from the following sources: C1746m370 |V1-V104 from Samus et al. (2009), C1746m370 |V105 to V145 from Pritzl et al. (2003), C1746m370 |V146-V150 from Corwin et al. (2006) and C1746m370 |V151-V199 from Skottfelt et al. (2015). C1746m370 |The remaining data are from the following sources: C1746m370 |V1-V36 from Layden et al. (1999), C1746m370 |V37-V104 from Pritzl et al. (2001) C1746m370 |V105-V148 from Pritzl et al. (2003) C1746m370 |V151-V199 from Skottfelt et al. (2015) C1746m370 |unless indicated otherwise in the Notes/Remarks column. C1746m370 |"Ogle" in the Remarks column indicates that the period, magnitude, C1746m370 |amplitude and classification are from the Ogle III Catalog of Long C1746m370 |Period variables in the Galactic Bulge by Soszynski et al. (2013). C1746m370 |The Ogle observations provided better coverage for long period C1746m370 |variables than the other studies so they are included when available. C1746m370 |Soszynski et al. (2011) also published a catalog of RR Lyrae C1746m370 |variables in the Galactic Bulge which includes some of the RR Lyrae C1746m370 |variables in NGC 6441, but their data have not been included here. C1746m370 |V47, V48, V49, V50, V68 are listed in the Moscow GCVS as V1168, V1170, C1746m370 |V1169, V1167 and V1166 Sco respectively. C1747m312 |Terzan 6 is a heavily reddened cluster in the inner bulge region. C1747m312 |According to the 2010 update to the Harris (1996) catalogue, Terzan 6 is C1747m312 |a core-collapsed cluster. A near infrared [K,J-K] CM diagram by Valenti C1747m312 |et al. (2007) shows a red HB. From their data, they derived a C1747m312 |photometric [Fe/H] = -0.62. C1747m312 |According to Bahramian et al. (2016), GRS 1747-312 is a low mass X-ray C1747m312 |binary in Terzan 6. C1748m346 |This cluster is located in a rich field in the Galactic bulge. C1748m346 |A VI CM diagram by Ortolani et al. (1999) shows a blue HB. C1748m346 |A JK CM diagram by Valenti et al. (2010) shows a blue steep RGB C1748m346 |with no evidence of a red HB, indicating a low-intermediate metallicity. C1748m346 |Harris (1996) listed [Fe/H] = -1.50 in the 2010 update of his catalogue. C1748m346 |The data for all the RR Lyrae variables listed in the above table are C1748m346 |from the OGLE IV database (Soszynski et al. 2014). These are the only C1748m346 |RR Lyrae variables located within 3.8 arcminutes of the cluster centre, C1748m346 |the radius they listed for the cluster. They estimated that 2 of them C1748m346 |might be field stars, and based on the mean magnitudes, it appears that C1748m346 |V3 and V10 are field stars. C1748m346 |The data for the RV Tauri variables are from the OGLE III catalogue C1748m346 |(Soszynski et al. 2011b). C1748m346 |Fourcade et al. (1966) observed NGC 6453 to search for variables, but C1748m346 |did not find any. C1751m241 |UKS 1 is a faint globular cluster in the bulge. C1751m241 |Origlia et al. (2005) derived [Fe/H] = -0.78 from near-infrared C1751m241 |photometry and high resolution spectroscopy. C1751m241 |Using HST/NICMOS and NTT/SOFI infrared photometry, Ortolani et al. (2007) C1751m241 |derived a distance that indicated that UKS1 is beyond the Galactic C1751m241 |centre. C1751m241 |UKS2 = BH 66 = ESO 166-SC11 (RA = 09:25.3, Dec = -54:53, J2000) was C1751m241 |long thought to be a globular cluster. However, Bica et al. (2000) C1751m241 |showed that UKS 2 is an open cluster with age comparable to that of C1751m241 |the Hyades. C1755m442 |The data in the above table are from the discovery paper by Abbas et al. C1755m442 |(2015). C1755m442 |CM diagrams published by Fraga et al. (2013) and Abbas et al. (2015) C1755m442 |show a prominent red clump on the horizontal branch, characteristic of a C1755m442 |metal rich cluster. No RR Lyrae variables have been discovered. C1758m268 |Terzan 9 is a heavily reddened cluster in a rich field in the inner C1758m268 |bulge. C1758m268 |A near infrared [K,J-K] CM diagram by Valenti et al. (2007) shows that C1758m268 |the innermost cluster region (r less than 30 arcsec) is characterized C1758m268 |by a narrow RGB and a blue HB. From their data, they derived a C1758m268 |photometric [Fe/H] = -1.21. C1758m268 |Lynch & Ransom (2011) conducted a search for pulsars, but did not find C1758m268 |any in Terzan 9. C1758m278 |The "IAU nomenclature" name for this cluster was assigned by Clement C1758m278 |et al. (2001) based on its 1950 position. C1758m278 |This cluster lies in a crowded field near the Galactic centre. C1758m278 |Valenti et al. (2010) published a near IR (K, J-K) CM diagram and C1758m278 |estimated [Fe/H] = -0.65, based on the slope of the RGB. Harris (1996) C1758m278 |listed V(HB)=17.60 in the 2010 update to his catalogue. He estimated C1758m278 |this value from the paper by Valenti et al. C1758m278 |The data for all the variables listed in the above table are from C1758m278 |Soszynski et al. (2014). These stars are all located within 2 C1758m278 |arcminutes of the cluster centre, well within the tidal radius, C1758m278 |10.5 arcminutes, according to the 2010 update to the Harris (1996) C1758m278 |catalogue. Harris listed half-light radius = 0.83 arcminutes. C1758m278 |These 7 variables have mean = 17.954 according to Soszynski et al. C1758m278 |(2014). In view of the uncertainties involved in Harris's estimate C1758m278 |of V(HB), it is reasonable to assume that they belong to the cluster. C1759m089 |A VI CM diagram by Kavelaars et al. (1995) shows a blue HB and a number C1759m089 |of stars that could be blue stragglers. The cluster is [Fe/H]=-1.49 C1759m089 |according to the 2010 update to the Harris (1996) catalogue. C1759m089 |Paulo Freire's website, (www.naic.edu/~pfreire/GCpsr.html) lists four C1759m089 |millisecond pulsars in NGC 6517. According to Lynch et al. (2011), C1759m089 |three of them are isolated and PSR J1801-0857B is in a binary system C1759m089 |with P=59.8 days. C1800m260 |Terzan 10 is a heavily reddened cluster in the Galactic bulge. C1800m260 |* The RA and dec listed for the cluster centre are from the 2003 C1800m260 |version of the Harris (1996) catalogue. According to Alonso-Garcia C1800m260 |et al. (2015), they are more accurate than the values Harris listed C1800m260 |in 2010. C1800m260 |Alonso-Garcia et al. (2015) published a K,J-K CM diagram but found that C1800m260 |it was difficult to disentangle cluster stars from stars in the Galactic C1800m260 |disk and bulge. Contamination by these field stars is significant, even C1800m260 |at distances smaller than the half light radius (1.55 arcminutes). C1800m260 |The data for V1-48 are from the discovery paper by Alonso-Garcia et al. C1800m260 |(2015). These are the variables that lie within the tidal radius, 5.06 C1800m260 |arcminutes, but many of them are probably field stars. C1800m260 |In fact, Alonso-Garcia et al. concluded that the vast majority of the C1800m260 |unclassified variables are disk field variables, based on their C1800m260 |positions in the CM diagram. C1800m300 |The field around NGC 6522 was observed by Baade (1946, 1951) in his C1800m300 |investigations to characterize the nature of the nucleus of the Milky C1800m300 |Way galaxy and to determine its distance from the Sun. He used the C1800m300 |Mount Wilson 100-inch telescope to study the field within 16 arcminutes C1800m300 |of the cluster and discovered 285 variable stars. Their elements were C1800m300 |later published by Gaposchkin (1955). C1800m300 |This field is now known as "Baade's window" because it is an area with C1800m300 |relatively low absorption near the Galactic centre and has been the C1800m300 |subject of many studies. C1800m300 |NGC 6522 is a core collapsed cluster with 0.05 arcminute core radius, C1800m300 |1.0 arcminute half-light radius and [Fe/H] = -1.34 according to the C1800m300 |2010 update to the Harris (1996) catalogue. Soszynski et al. (2011a) C1800m300 |listed a cluster radius of 4.7 arcminutes. C1800m300 |Since the cluster is located in a very rich field, only variables that C1800m300 |lie less than 2 arcminutes of the cluster centre have been included C1800m300 |in the above table. Some of these (e.g. V6) are probably field stars, C1800m300 |while some stars beyond 2 arcminutes might be cluster members. C1800m300 |A proper motion study by Terndrup et al. (1998) showed that most stars C1800m300 |up to 2.2 arcminutes from the cluster centre are probable members. C1800m300 |However, some stars less than 1 arcminute from the centre may belong to C1800m300 |the field. C1800m300 |The data for the RR Lyrae variables are from the Ogle IV survey C1800m300 |(Soszynski et al. 2014) where C1800m300 | V1 = OGLE-BLG-RRLYR-12073 C1800m300 | V2 = OGLE-BLG-RRLYR-12117 C1800m300 | V3 = OGLE-BLG-RRLYR-12127 C1800m300 | V4 = OGLE-BLG-RRLYR-12132 C1800m300 | V5 = OGLE-BLG-RRLYR-12154 C1800m300 | V9 = OGLE-BLG-RRLYR-12099 = V1438 Sgr C1800m300 | V10 = OGLE-BLG-RRLYR-12115 C1800m300 | V11 = OGLE-BLG-RRLYR-12114 C1800m300 | V12 = OGLE-BLG-RRLYR-12072 = V4113 Sgr C1800m300 | V13 = OGLE-BLG-RRLYR-12108 C1800m300 | V14 = OGLE-BLG-RRLYR-33606 C1800m300 |The sources for variables, V6, V7, V8, and V15 are indicated in the C1800m300 |notes on individual stars. C1801m003 |A CM diagram by Sarajedini (1994) shows a predominanty blue HB and C1801m003 |significant population of blue straggler candidates. The 2010 update to C1801m003 |the Harris (1996) catalogue lists [Fe/H] = -1.79. C1801m003 |The RA and dec for V1 and V2 are from Samus et al. (2009) and the other C1801m003 |elements are from Liller & Clement (1977). The field status for both C1801m003 |variables is based on their location in the CM diagram of Liller (1980). C1801m003 | C1801m300 |NGC 6528 is a metal rich cluster that is located in a rich field in the C1801m300 |Galactic bulge. Harris (1996) lists [Fe/H] = -0.11 in the 2010 update C1801m300 |to his catalogue. C1801m300 |A CM diagram by Lagoia et al. (2014) shows a prominent red HB. C1801m300 |The data in the above table are from Skottfelt et al. (2015) unless C1801m300 |indicated "Ogle" in the Remarks column. For the Ogle stars, the C1801m300 |period, magnitude, amplitude and classification are from Soszynski C1801m300 |et al. (2013). C1802m075 |NGC 6539 is a metal rich globular cluster located in a rich, heavily C1802m075 |reddened field near the Galactic centre. According to the 2010 update C1802m075 |to the Harris (1996) catalogue, its [Fe/H]=-0.63 and a CM diagram by C1802m075 |Baker et al. (2007) shows a strong red HB clump, characteristic of a C1802m075 |metal rich cluster. C1802m075 |The data for V1-11 are from the discovery paper by Baker et al. (2007) C1802m075 |and the numbers in the remarks column are the ones that they used C1802m075 |in their paper. All of these stars are considered to be long period C1802m075 |variables. However, firm classifications could not be made because C1802m075 |the observations were limited to a span of three nights in May and C1802m075 |eight in June 1996 with a gap of 31 days between. Based on the C1802m075 |cluster's high metallicity, it is possible that some of them are Mira C1802m075 |stars. C1802m277 |NGC 6540 was thought to be an open cluster until Bica et al. (1994) C1802m277 |showed it to be a thick disk globular cluster. C1802m277 |A near IR (K, J-K) CM diagram published by Valenti et al. (2010) C1802m277 |is characterized by a steep poorly populated RGB and a blue HB C1802m277 |which was also present in the optical CMD of Bica et al. (1994). C1802m277 |They estimated [Fe/H]=-1.29, based on the slope of the RGB, a value C1802m277 |that is in agreement with [Fe/H] = -1.40 +/- 0.40 derived by Cote C1802m277 |(1999) for four stars from the equivalent of a few Fe I lines. C1802m277 |The data for the RR Lyrae variables are from the OGLE IV survey C1802m277 |(Soszynski et al. 2014). C1804m250 |A CM diagram by Cohen et al. (2014) shows a well populated blue HB with C1804m250 |an extended tail and a centrally concentrated blue straggler population. C1804m250 |The 2010 update to the Harris (1996) catalogue lists [Fe/H] = -1.40. C1804m250 |In the above table, the RA and dec are from Samus et al. (2009). The C1804m250 |data for V1 are from the discovery paper by Hazen (1993). C1804m437 |CM diagrams published by Alcaino et al. (1997) and by Lee & Carney C1804m437 |(2006) show a cluster deficient in RGB stars and an extended blue HB. C1804m437 |Fiorentino et al. (2014) subsequently discovered 70 blue straggler stars C1804m437 |and detected variabiity in 12 of them. C1804m437 |The RA and dec for V1-8 were derived by Samus et al. (2009). C1804m437 |The remaining data listed for V2-8 are from Hazen (1994). C1804m437 |Hazen noted that the positions of the V3-8 so far from the cluster C1804m437 |centre made cluster membership seem unlikely. However, she also showed C1804m437 |that they all were located within the tidal radius, which at the time, C1804m437 |was considered to be approximately 32 arcminutes, so that firm C1804m437 |conclusions about their membership could not be made. Now however, C1804m437 |according to the 2010 update of the Harris (1996) catalogue, the C1804m437 |estimated tidal radius of NGC 6541 is approximately 13 arcminutes. C1804m437 |Thus it is probable that most of these variables belong to the C1804m437 |surrounding field. They are listed as field stars. C1804m437 |The data for V9-20 are from the discovery paper by Fiorentino et al. C1804m437 |(2014). The numbers that they assigned: WU1-3 and SX1-9 are indicated C1804m437 |in the remarks column. C1804m437 |The data for V21-22 are from the discovery paper by Figuera Jaimes et C1804m437 |al. (2016). C1806m259 |NGC 6553 is a metal rich cluster located in a heavily reddened C1806m259 |field near the galactic centre. According to the 2010 version of C1806m259 |the Harris (1996) catalogue, [Fe/H] = -0.18. A CM dagram by Zoccali C1806m259 |et al. (2001) shows a stubby red HB and a blue straggler star sequence. C1806m259 |In the above table, the RA and dec are from Samus et al. (2009). C1806m259 |For V1-3, the periods and magnitudes and classifications are from C1806m259 |Soszynski et al. (2011). C1806m259 |The period, magnitude, amplitude and classification for V4 is from C1806m259 |Sloan et al. (2010). C1806m259 |The classifications for V5-14 are from Lloyd Evans & Menzies who C1806m259 |plotted their positions on a CM diagram. All of these variables C1806m259 |(with the exception of V11 and V12) have been detected in the VVV C1806m259 |survey (Minniti et al. 2010) but no periods have been published. C1807m317 |NGC 6558 is a relatively metal poor, core collapsed cluster in the C1807m317 |Galactic bulge. According to the 2010 version 0f the Harris (1996) C1807m317 |catalogue, it has [Fe/H] = -1.32, a tidal radius of 9.5 arcminutes, C1807m317 |and a half-light radius of 2.15 arcminutes. C1807m317 |Soszynski et al. (2014) listed the cluster radius as 2.1 arcminutes. C1807m317 |A VI CM diagram by Rich et al. (1998) shows an extended blue HB and C1807m317 |a sparsely populated RGB. C1807m317 |All of the data for the RR Lyrae variables are from the OGLE IV survey C1807m317 |(Soszynski et al. 2014) where C1807m317 | V1 = OGLE-BLG-RRLYR-14886 = BB#25 r=0.43' C1807m317 | V3 = OGLE-BLG-RRLYR-14929 = BB#30 r=1.04' C1807m317 | V4 = OGLE-BLG-RRLYR-14866 = BB#24 r=1.02' C1807m317 | V5 = OGLE-BLG-RRLYR-14867 = BB#A = V4301 Sgr r=2.26' C1807m317 | V6 = OGLE-BLG-RRLYR-14888 = BB#E2 r=0.93' C1807m317 | V8 = OGLE-BLG-RRLYR-14897 = BB#26 = V4601 Sgr r=3.09' C1807m317 | V9 = OGLE-BLG-RRLYR-14732 = BB#16 = V4595 Sgr r=5.82' C1807m317 | V13 = OGLE-BLG-RRLYR-14809 r=6.07' C1807m317 | V14 = OGLE-BLG-RRLYR-15057 r=6.01' C1807m317 | V16 = OGLE-BLG-RRLYR-14912 = BB#29 r=0.51' C1807m317 | V17 = OGLE-BLG-RRLYR-14892 r=0.32' C1807m317 |The BB numbers refer to a paper by Blanco & Blanco (1997) and C1807m317 |r refers to the distance from the cluster centre. C1807m317 |The RA and dec for the "CST?" stars V2, V7 and the "L?" variables C1807m317 |V10-12 and V15 are from Samus et al. (2009). C1807m317 |The magnitudes and amplitudes for the "L?" variables (V10-12 and V15) C1807m317 |are from Dominici et al. (1999). Neither Hazen (1996) nor Dominici C1807m317 |et al. (1999) had sufficient data to make definitive classifications C1807m317 |for these variables. None of them were listed in the OGLE III C1807m317 |(Soszynski et al. 2013) catalogue of Long Period Variables. With C1807m317 |distances of 4.0, 5.0, 5.6 and 5.5 arcminutes from the cluster centre, C1807m317 |they are all located beyond Soszynski's cluster radius, 2.1 arcminutes. C1808m072 |The RA and dec are from Samus et al. (2009). C1808m072 |The periods and classifications for V1 and V3, the two Mira variables, C1808m072 |are from Sloan et al. (2010) who published K band light curves. The B C1808m072 |magnitudes and amplitudes for these stars are from Kinman & Rosino (1962). C1808m072 |The periods, magnitudes, amplitudes and variability types for V2, V4 and C1808m072 |V5 are from Kinman & Rosino (1962). C1808m072 |All of the variables are considered to be cluster members. Their C1808m072 |magnitudes are appropriate for cluster membership and they are all C1808m072 |well inside the tidal radius which is 21.6 arcmin according to the C1808m072 |2010 update to the Harris (1996) catalogue. C1808m072 |Barbuy et al. (1998) published a BV colour-magnitude diagram that C1808m072 |showed a prominent red HB, characteristic of a metal rich population. C1808m072 |Cote (1999) later derived [Fe/H] = -0.75 from the equivalent widths of C1808m072 |iron lines in 5 RG stars considered to be cluster members on the basis C1808m072 |of their radial velocities. C1809m227 |Ortolani et al. (1998) published a VI CMD which had a red HB, a C1809m227 |characteristic of a metal-rich cluster and estimated a tentative value C1809m227 |[Fe/H] = -0.5 based on the slope of the RG branch. C1809m227 |The data for V1 are from Sloan et al. (2010) who conclude that the star C1809m227 |is a cluster member. C1810m318 |The RA and dec in the above table are from Samus et al. (2009). C1810m318 |The remaining data are from Hazen-Liller (1985). C1810m318 |NGC 6569 is a massive metal-rich cluster located in the Galactic bulge. C1810m318 |A CM diagram based on BVI data by Ortolani et al. (2001) showed that the C1810m318 |HB is predominantly red, but some bluer stars may be present. They C1810m318 |plotted the positions of the variable stars on the CM diagram and found C1810m318 |that the magnitudes and colours of most of them were consistent with C1810m318 |cluster membership. C1810m318 |A subsequent study by Mauro et al. (2012), based on JK photometry C1810m318 |showed that that the cluster's HB is split into two distinct clumps C1810m318 |separated by ~0.1 mag in the K_s band. C1810m318 |A study of the RR Lyrae variables in NGC 6569 has been undertaken by C1810m318 |Kunder et al. (2015) who published a preliminary report. They C1810m318 |identified 27 RR Lyrae variables, of which 15 were new discoveries. C1814m522 |The two main studies of the variables in NGC 6584 are by Millis & Liller C1814m522 |(1980) and by Toddy et al. (2012). C1814m522 |Millis & Liller discovered variables V2-48 and carried out a photographic C1814m522 |study of V1-48. C1814m522 |Toddy et al. applied the image substraction technique to a set of images C1814m522 |obtained on 8 nights in May, June, July 2011. They discovered 26 new C1814m522 |variables (NV1-26) which have been assigned the numbers V49-74 in this C1814m522 |catalogue. C1814m522 |All of the data listed for V49-74 are from Toddy et al. C1814m522 |For V1-48, the RA, dec, periods and classifications are also from Toddy C1814m522 |et al., unless indicated otherwise in the remarks column. The 5 stars C1814m522 |indicated "M&L" were outside Toddy's field of view. For these 5 stars, C1814m522 |the RA and dec are from Samus et al. (2009) and the reaming data are C1814m522 |from Millis & Liller (1980). C1814m522 |The magnitudes and amplitudes for V1-48 are from Millis & Liller. C1814m522 |V15, V24, V27, V39 are listed in the Moscow GCVS as PXTel, PU Tel, PT C1814m522 |Tel, PS Tel respectively. C1820m303 |NGC 6624 is a metal rich bulge cluster with [Fe/H] = -0.44 according to C1820m303 |the 2010 revision of the Harris (1996) catalgue. A VI CM diagram C1820m303 |published by Heasley et al. (2000) shows a prominent red HB. C1820m303 |In the above table, the RA and dec for V1-5 are from Samus et al. (2009) C1820m303 |The magnitudes, ammplitudes and classifications are from Liller & Liller C1820m303 |(1976). C1820m303 |According to the VizieR Service, V1-5 are all listed in the catalogue C1820m303 |of VISTA Variables in the Via Lactea Survey DR1 (Minniti et al. 2014). C1820m303 |but no periods have been published by the VISTA group. C1821m249 |For V1-24, the RA and dec are from Samus et al. (2009). The period, C1821m249 |magnitude, amplitude, variability type and membership status are from C1821m249 |Wehlau & Butterworth (1990) unless designated W&SH or P12 in the C1821m249 |remarks column: C1821m249 | W&SH indicates that they are from Wehlau & Sawyer Hogg (1984) C1821m249 | P12 indicates that the period and classification are from Prieto C1821m249 | et al. (2012). C1821m249 |Samus et al. (2009) noted that V7=V4137 Sgr, V15=V4128 Sgr, V16=V4130 Sgr, C1821m249 |V17=V2342 Sgr and V24=V4129 Sgr. C1821m249 |All the data for V25-V33 are from the discovery paper by Prieto et al. C1821m249 |(2012). The numbers that these authors assigned to these stars, NV1-9 C1821m249 |are indicated in the remarks column. C1821m249 |A VI CM diagram by Testa et al. (2001) shows an extended blue HB and a C1821m249 |few BS stars. C1827m255 |A BV CM diagram by Piotto et al. (2002) based on HST data shows a blue C1827m255 |straggler sequence and a horizontal branch that is populated on both C1827m255 |sides of the instability strip. C1827m255 |The RA and dec for V1-63 in the above table are from Samus et al. C1827m255 |(2009) unless indicated "Sk" in the remarks column in which case they C1827m255 |are from Skottfelt et al. (2015). C1827m255 |Samus et al. pointed out that there were serious errors in the RA C1827m255 |and dec values published earlier by Rutily & Terzan (1977). C1827m255 |The periods, magnitudes and classifications for V1-63 are based mainly C1827m255 |on the data of Rutily & Terzan (1977). They treated the variable stars C1827m255 |in two groups: red variables (V1-V19 and V46-V63) C1827m255 | and blue variables (V20-V45). C1827m255 |Most of the red variables are located outside the tidal radius C1827m255 |(~4.7 arcminutes according to the 2010 update of the 1996 Harris C1827m255 |catalogue) and probably belong to the field around the cluster. C1827m255 |Consequently they are all listed in the Moscow GCVS or NSV catalogues. C1827m255 |Samus et al. (2009) listed the GCVS and/or NSV designations for these C1827m255 |variables in Table 1 of their paper. C1827m255 |Skottfelt et al. (2015) published RA, dec, periods, magnitudes and C1827m255 |amplitudes for some of the blue variables. These stars are indicated C1827m255 |"Sk" in the remarks column. C1827m255 |Smith & Stryker (1986) derived radial velocities and Delta S values for C1827m255 |a few of the RR Lyrae variables. They found that V37, V38, V42, V45 C1827m255 |were probable members and that the membership membership status of C1827m255 |V40 and V43 was questionable. C1828m235 |A CM diagram based on HST observations by Balbinot et al. (2009) shows C1828m235 |a well populated blue straggler sequence and a well developed HB. C1828m235 |The RA and dec for V1-18 in the above table are from Samus et al. (2009). C1828m235 |The V magnitude for V1 is from Barbuy et al. (2006) and the period and C1828m235 |classification are from Hoffleit (1972). C1828m235 |The remaining data for V2-18 are from Hazen (1993). C1828m235 |Barbuy et al. (2006) published V magnitudes for 9 of the RR Lyrae C1828m235 |variables: V3-5, V7, V9, V11-13, and V15 and derived a mean V of C1828m235 |16.43 +/- 0.06 mag. They also showed that V1 lies near the RG tip in C1828m235 |the CM diagram. C1828m323 |NGC 6637 is a metal rich bulge cluster with [Fe/H]= -0.8 (Minniti 1995). C1828m323 |A VI CM diagram published by Heasley et al. (2000) shows a pronounced red HB. C1828m323 |The RA and dec for V1-8 are from Samus et al. (2009). The remaining data are C1828m323 |from the following sources. C1828m323 | V1-3: C1828m323 | The magnitudes listed for V1-V3 are from Rosino (1962). C1828m323 | V2: C1828m323 | The period for V2 (V3484 Sgr) is from the GCVS. C1828m323 | Hartwick & Sandage classified the RR Lyrae V2 as a field star C1828m323 | because it is more than 5 arcmin from the cluster centre and C1828m323 | at least a magnitude fainter than the HB. C1828m323 | V4-5: C1828m323 | The periods, magnitudes and amplitudes listed for V4-V5 are from C1828m323 | Sloan et al. (2010). C1828m323 | The Mira classification for these variables was by Lloyd Evans & C1828m323 | Menzies (1971). Catchpole et al. (1970) derived their radial C1828m323 | velocities and concluded that both stars were plausible cluster C1828m323 | members and probably Mira variables. C1828m323 | V5: C1828m323 | This star was numbered V10 by Rosino (1962) in his discovery paper. C1828m323 | The number V5 was assigned by Sawyer Hogg in her 3rd (1973) catalogue C1828m323 | because Rosino considered his V5-V9 to all be field stars. C1828m323 | The star referred to as V10 by Catchpole et al. (1970) and by C1828m323 | Lloyd Evans & Menzies (1971, 1973) is V5 because their work was C1828m323 | published before Sawyer Hogg assigned the new numbering system. C1828m323 | V6-8: C1828m323 | The magnitudes listed for V6-8 are from Hartwick & Sandage (1968). C1832m330 |A BV CM diagram by Ortolani et al. (1994) shows a red HB and a well C1832m330 |populated blue straggler sequence. C1832m330 |The RA and dec for V1-9 and V11 are from Samus et al. (2009). C1832m330 |The remaining data for V1-9 are from the discovery paper by Hazen C1832m330 |(1989). C1832m330 |The data for V10 and V12 are from Heinke et al. (2001). C1832m330 |The data for V13 and 14 are from Skottfelt et al. (2015). C1833m239 |The positions listed above for V1-43 are from Samus et al. (2009). C1833m239 |For the remaining variables, the positions and other data are taken C1833m239 |from the discovery papers unless indicated otherwise in the notes. C1833m239 |The periods, magnitudes, amplitudes, classifications and membership C1833m239 |status for all of the RR Lyrae variables are from Kunder et al. (2013). C1833m239 |The periods, magnitudes, amplitudes, variability type and membership C1833m239 |status listed for all the "non-RR Lyrae" variables numbered from V1 to C1833m239 |V35 are from Wehlau & Sawyer Hogg (1977, 1978) unless otherwise noted C1833m239 |in the remarks column. They also published ID charts for V1-35; the C1833m239 |'outer' variables are shown in their 1977 paper and the 'inner' variables C1833m239 |in 1978. C1833m239 |The magnitudes, amplitudes and membership status for V36-43 are from the C1833m239 |discovery paper by Kravtsov et al. (1994). C1833m239 |The membership of V5, V8, V9, V11 and the non-membership of V14 are from C1833m239 |a radial velocity study by Joy (1949). Radial velocities confirming the C1833m239 |membership of V5, V8, V9 and V30 were subsequently obtained by Peterson C1833m239 |& Cudworth (1994). C1833m239 |Samus et al. (2009) listed GCVS numbers for V14, V17, V22, V26, V28, V31, C1833m239 |V32 and V33. They are Sgr variables V1311, V4068, V3853, V2007, V2367, C1833m239 |V3855, V4067, and V4069 respectively. V29 and V30 are NSV 11080 and C1833m239 |11084. In addition, Samus (private communication, 2012) pointed out that C1833m239 |Sebastian Otero noted that V27 is V2592 Sgr. C1838m198 |Armandroff (1988) obtained CCD images in the V,R,I bands to compare the C1838m198 |CM diagram of Pal 8 with that of 47 Tuc. He found that the HB of Pal 8 C1838m198 |lies entirely redward of red edge of the instability strip, characteristic C1838m198 |of a metal rich cluster. It does not extend as far to the blue as the red C1838m198 |HB of 47 Tuc. C1840m323 |NGC 6681 is located in the same region of the sky as the main body of the C1840m323 |Sagittarius dwarf galaxy. CM diagrams by Brocato et al. (1996) and C1840m323 |Massari et al. (2013) show an extended blue HB. C1840m323 |The RA and dec for V1-5 are from Samus et al. (2009). C1840m323 |The remaining data are from Liller (1983). C1840m323 |The data for V6 are from the discovery paper by Figuera Jaimes et al. C1840m323 |(2016). C1850m087 |NGC 6712 is a moderately metal rich ([Fe/H]=-1.02) cluster located in C1850m087 |a rich star field in the Scutum cloud. C1850m087 |A CM diagram by Paltrinieri et al. (2001) shows a well populated blue C1850m087 |straggler sequence and an HB that is predominantly red. C1850m087 |According to the 2010 update to the Harris (1996) catalogue, its tidal C1850m087 |radius is 8.5 arcminutes, but the CM diagram shows that field stars C1850m087 |dominate at distances greater than 2.5 arcminutes from the cluster C1850m087 |centre. C1850m087 |Some of the variables are listed in the Moscow GCVS. For these stars, C1850m087 |the GCVS designation is listed in the remarks column. C1850m087 |In the above table, the RA and dec for V1-22 are from Samus et al. C1850m087 |(2009). C1850m087 |The remaining elements for these stars are from Sandage et al. (1966) C1850m087 |unless indicated otherwise in the remarks column where C1850m087 | Ros refers to Rosino (1966) C1850m087 | PK refers to Pietrukowicz & Kaluzny (2004) C1850m087 | Sl refers to Sloan (2010) C1850m087 | LEM refers to Lloyd Evans & Menzies (1977) and C1850m087 | KC refers to Cudworth (1988). C1850m087 |For V23-29, all of the elements are from the discovery papers. C1851m305 |NGC 6715 (M54) is located in a Milky Way Galactic Bulge field. However, C1851m305 |the cluster resides in the centre of the Sagittarius dwarf galaxy which C1851m305 |is about three times more distant than the Galactic Bulge. C1851m305 |The cluster and its surrounding field were observed in the OGLE IV C1851m305 |Galactic Bulge survey. Results from this survey have been reported by C1851m305 |Soszynski et al. (2014 - hereafter Sos14) for RR Lyrae variables and C1851m305 |by Soszynski et al. (2016 - hereafter Sos16) for eclipsing binaries. C1851m305 |The most comprehensive investigation of the variable stars in NGC 6715 C1851m305 |was by Hamanowicz et al. (2016 - hereafter H16), based on the OGLE IV C1851m305 |data. They announced 52 new variables, V296-V347 and also published C1851m305 |data for most of the previously known variables. C1851m305 |Among their new variables, H16 listed only variable stars located less C1851m305 |than 7.5 arcmin from the cluster centre, the tidal radius that was C1851m305 |published in the 1999 and 2003 updates to the Harris (1996) catalogue. C1851m305 |A few additional OGLE IV variables have been included in this catalogue, C1851m305 |variables with r<9.5 arcminutes, which is the tidal radius derived from C1851m305 |the data published by Harris (2010.) C1851m305 |The data in the above table are from H16 unless indicated otherwise C1851m305 |in the Notes/Remarks column where C1851m305 | S10 refers to Sollima et al. (2010). These stars were located C1851m305 | in the gaps between CCDs in OGLE IV investigation. C1851m305 | FJ16 refers to Figuera Jaimes et al. (2016), a study of the C1851m305 | central region of the cluster. FJ16 discovered 80 new C1851m305 | variables in the central region and the RA and dec listed C1851m305 | for these variables are from their study. C1851m305 | 45 of the FJ16 variables were also recovered by H16 and in C1851m305 | these cases, the Notes on individual stars indicate the C1851m305 | source for the entries in the table C1851m305 | Sos14 refers to Soszynski et al. (2014), OGLE IV RR Lyrae data C1851m305 | Sos16 refers to Soszynski et al. (2016), OGLE IV eclipsing data C1851m305 |For variable stars in clusters located in Galactic bulge fields, it is C1851m305 |challenging to establish cluster membership because field stars can often C1851m305 |be found within the tidal radius. Without radial velocities or proper C1851m305 |motions, the best approach is to consider the location in the CM diagram C1851m305 |as well as distance from the cluster centre. C1852m227 |BV colour magnitude diagrams by Brocato et al. (1996) and Ortolani et al. C1852m227 |(1999) show an extended blue HB which is unusual for a cluster with such C1852m227 |a relatively high metal abundance. According to the 2010 version of the C1852m227 |Harris catalogue, [Fe/H] = -1.26. C1852m227 |The period, mean magnitude, amplitude and variability type C1852m227 |listed for V1 are from Goranskij (1978) and the RA and dec are from C1852m227 |Samus et al. (2009). Based on its location in the CM diagram, it is C1852m227 |considered to be a cluster member. C1856m367 |The data in the above table are from Lee et al. (2014) unless indicated C1856m367 |otherwise in the notes on individual stars. The NV numbers listed for C1856m367 |V33-V47 are from their paper; the numbers V33-47 have been assigned C1856m367 |in this catalogue. C1902p017 |VI color-magnitude diagrams published by Kaisler et al. (1997) and by C1902p017 |Rosino et al. (1997) show a blue HB. Rosino et al. concluded that C1902p017 |this is a halo cluster located close to the Galactic plane. The C1902p017 |surrounding field is rich in Mira variables (75 within 1 degree of the C1902p017 |cluster centre), but they do not appear to be members. They are probably C1902p017 |associated with the metal rich disc/bulge population. Skiff (2001) C1902p017 |listed RA, dec and magnitudes for the variables, but agreed with Rosino C1902p017 |that probably none of theMira variables are related to the cluster. C1902p017 |The data for the type II Cepheid V1 are from Matsunaga et al. (2006). C1906m600 |NGC 6752 is the subject of many recent studies because of its milli-second C1906m600 |pulsars and its X-ray sources. In addition, its multiple stellar C1906m600 |populations have been investigated by numerous authors, see e.g., Kravtsov C1906m600 |et al. (2014). The cluster is relatively metal poor, with [Fe/H] = -1.54, C1906m600 |according to the 2010 update to the Harris (1996) catalogue. Its CM diagram C1906m600 |has an extended blue HB. No RR Lyrae variables have been discovered. C1906m600 |V1-3: The RA and dec are from Samus et al. (2009). They also pointed C1906m600 |out that the y coordinate published for V1 in the previous on-line catalogue C1906m600 |(Clement et al. 2001) was incorrect. It should have been +143.0 (not C1906m600 |+14.30). The remaining data for V1 are from Lee (1974) and for V3 from C1906m600 |the discovery paper by Cannon & Stobie (1973). C1906m600 |V4-14: Most of the data are from the discovery paper by Thompson et al. C1906m600 |(1999) unless indicated otherwise in the Notes on individual stars. C1906m600 |The "f" classification for V5, V6, V9, V11 was by Rucinski (2000) C1906m600 |based on photometric criteria. C1906m600 |Samus et al. (2009) pointed out that V4, V5, V6, V8 and V11 are V0394, C1906m600 |0395, 0396, 0397 and 0398 Pav respectively. C1906m600 |V15-24: All the data are from the discovery paper by Kaluzny & Thompson C1906m600 |(2009). C1906m600 |V25-27: All the data are from Thomson et al. (2012). C1906m600 |The data for the PSR objects are from D'Amico et al. (2002). C1908p009 |NGC 6760 is a metal rich cluster in the Galactic bulge. The 2010 C1908p009 |update to the Harris (1996) catalogue lists [Fe/H] = -0.4. A VI C1908p009 |CM diagram by Heitsch & Richtler (1999) shows a prominent red HB and C1908p009 |also demonstrates that the cluster is located in a rich field near the C1908p009 |plane of the Galaxy. C1908p009 |For V1 and V2, the magnitudes are from the discovery paper by Sawyer C1908p009 |(1953) and the RA and dec are from Samus et al. (2009). C1908p009 |All the data for V3 and V4 are from Sloan et al. (2010). C1914m347 |Terzan 7 is probably a member of the Sagittarius dwarf galaxy. C1914m347 |A BV CM diagram by Buonanno et al. (1995) shows a steep red giant branch C1914m347 |and a compact red HB, characteristics of a metal-rich cluster. C1914m347 |A VI CM diagram by Held et al. (2002) shows a well populated blue C1914m347 |straggler sequence. C1914m347 |Sbordone et al. (2005) derived [Fe/H] = -0.6 from high resolution C1914m347 |UVES-VLT spectra of 5 giant stars. C1914m347 |In the 2010 update to his catalogue, Harris (1996) adopted [Fe/H]= -0.32. C1914p300 |V1-12: The periods, magnitudes and membership status are from Wehlau C1914p300 | & Sawyer Hogg, (1985). Their membership status for V1, V3, V5, C1914p300 | V7, V8, V9 and V11 was based on a proper motion study by Rishel C1914p300 | et al. (1981); V6 based on a radial velocity study by Joy (1949) C1914p300 | and V10 based on its faint mean magnitude. The RA and dec are C1914p300 | from Samus et al. (2009). C1914p300 | V7-11 are V0487, V0485, V0486, V0483 and V0484 resepctively C1914p300 | in the Moscow GCVS (Samus et al.) C1914p300 |V13-14: The data are from the discovery paper by Pietrukowicz et C1914p300 | al. (2008). They classified V13 as a pulsating variable, C1914p300 | possibly on the AGB - no color information was available. C1916p184 |The RA and dec for V2 and V3 are from Samus et al. (2009) who have C1916p184 |pointed out that these stars are MV Sge and MZ Sge respectively. C1916p184 |The periods, magnitudes, amplitudes and variability types for C1916p184 |V2 and V3 are from Rosino & Guzzi (1978) and their membership status C1916p184 |is from Canterna & Rosino (1981). However, Rosino & Ortolani (1985) C1916p184 |commented that, since they lie in a field rich of Mira variables, it is C1916p184 |possible that they both belong to the field. C1916p184 |A VI CM diagram by Kaisler et al. (1997) shows a purely red HB, C1916p184 |characteristic of a metal rich cluster. The cluster is heavily reddened C1916p184 |and also differentially reddened. C1925m304 |The periods and variability types in the above table are from Salinas C1925m304 |et al (2005). No magnitudes or amplitudes were derived because they used C1925m304 |the image subtraction technique for their study. The RA and dec were C1925m304 |provided by Salinas (2013, private communication) and were derived from C1925m304 |the study by Salinas et al. (2012). C1936m310 |All the data listed for V1-V15 are from Olech et al. (1999). C1936m310 |The data for V16-V42 are from the discovery paper by Pych et al. (2001). C1936m310 |They classified V16-V30 as single-mode SXPhe variables and V31-V42 as C1936m310 |double-mode SXPhe variables. For all of the double-mode stars (except C1936m310 |V41), one of the modes is considered to be non-radial in origin. The C1936m310 |periods listed for V31-V42 in the above table are the longer of the C1936m310 |stars' two periods and the amplitudes are the amplitudes associated with C1936m310 |these longer periods (except in the case of V38). C1936m310 |The data for V43 are from the discovery paper by Kaluzny et al. (2005) C1936m310 |The data for V44-V71 are from the discovery paper by Kaluzny et al. C1936m310 |(2010). However, it should be noted that the amplitudes listed for the C1936m310 |SX Phe variables seem to be unusually low. It appears that they C1936m310 |represent half of the total light range. More than 20 of the SXPhe C1936m310 |variables in M55 were studied by Pych et al. (2001) and when the amplitudes C1936m310 |they derived are compared with the values of Kaluzny et al. (2010), C1936m310 |Pych's amplitudes are more than a factor of 2 larger. C1936m310 |The Sagittarius (Sgr) dwarf galaxy is visible in the background field of C1936m310 |M55. As a result, some of the variables in the M55 field are associated C1936m310 |with the Sgr galaxy and not the cluster. This is noted in the remarks C1936m310 |column. C1936m310 |A proper motion study by Zloczewski et al. (2011) showed that variables C1936m310 |V2, V4, V5, V6, V7, V8, V10, V11, V12, V16-V27, V31-V38, V41, V42, V44, C1936m310 |V45, V47, V48, V53-V55, V57, V60-V65, V67 and V69 are all probably C1936m310 |cluster members and that V15 and V49-V51 are field stars. C1936m310 | C1936m310 |Some of the variables (V5, V24, V35, V38, V40) were included in the C1936m310 |proper motion study by Sariya et al. (2012) and all were found to be C1936m310 |cluster members. C1938m341 |The periods and classifications are from Salinas et al. (2005). C1938m341 |The RA and dec were derived from the study by Salinas et al. (2012) C1938m341 |and were provided by Salinas (2013, private communication). C1942m081 |A variable star search of Pal 11 was carried out by Kinman & Rosino C1942m081 |(1962) but no variables were detected. C1942m081 |A VI color-magnitude diagram published by Lewis et al. (2006) shows C1942m081 |noticeable, but depleted red giant and subgiant branches. It has a red C1942m081 |horizontal branch, characteristic of a metal rich cluster cluster. C1942m081 |In fact, they found that the CMD was virtually identical to that of the C1942m081 |metal rich cluster NGC 5927. C1942m081 |There are also a few blue stragglers but the data were not extensive C1942m081 |enough to carry out a search for variables. C1942m081 | C1951p186 |The RA and dec for V1-6 are from Samus et al. (2009) and for P1-23, they C1951p186 |are from Park & Nemec (2000). In the above table, P1-23 are v1-23 on the C1951p186 |numbering system of Park & Nemec and V7-29 in the paper by Samus et al. C1951p186 |The periods, mean magnitudes and amplitudes for V2, V5 and V6 are C1951p186 |from Welty (1985) who considered V2 and V5 to be cluster members, but C1951p186 |concluded that the membership of V6 (V0345 Sge) is unlikely based on a C1951p186 |proper motion study by Cudworth (1985). C1951p186 |The remaining data for V1, 3 and 4 are discussed in the notes on C1951p186 |individual stars. C1951p186 |The periods, magnitudes, amplitudes and classifications for V7-29 are C1951p186 |from the study by Park & Nemec (2000). The membership status of V7, 8, 9 C1951p186 |and 11 is from Rucinski (2000). He did not analyse any of the other C1951p186 |variables. C2003m220 |Note that V18-47 are NV1-30 of Corwin et al. (2003) and V48-51 are NV1-4 C2003m220 |of Scott et al. (2006). C2003m220 |The RA and dec for V1-17 are from Samus et al. (2009). C2003m220 |The RA and dec for most of the other stars were supplied by Rodrigo C2003m220 |Contreras (2012, private communication) from the investigation by C2003m220 |Contreras et al. (2012). C2003m220 |The exceptions were V21, V24, V27, V28, V34 and V47-51. For these stars, C2003m220 |the RA and dec were calculated from the x,y positions published C2003m220 |by Corwin et al. (2003) and Scott et al. (2006). For these calculations, C2003m220 |it was assumed that the origin of their x,y system was RA=20:06:04.90 and C2003m220 |dec=-21:55:17.8. Making this assumption gave good agreement with the C2003m220 |coordinates Contreras et al. derived for the other stars. C2003m220 |All of the remaining data for V1-47 are from Corwin et al. (2003) unless C2003m220 |indicated by PRC in the remarks column, in which case they are from Pinto C2003m220 |et al. (1982). Corwin et al. did not derive magnitudes and amplitudes C2003m220 |for all of the variables because they used the image subtraction technique C2003m220 |for their analysis. They observed in B and V, but only V magnitudes are C2003m220 |listed here. C2003m220 |All of the data for V48-51 are from Scott et al. (2006). C2003m220 |Contreras et al (2012) identified 62 blue straggler stars which are C2003m220 |highly segregated in the cluster core. They published their RA, dec and C2003m220 |magnitudes. Some of these are probably variable, but their data were C2003m220 |not suitable for carrying out a variable star search. However, the C2003m220 |position of their star BSS#5, RA=301.5202849 and dec -21.9213937, seems C2003m220 |to be close to the suspected binary V50 (NV4 of Scott et al. 2006). C2031p072 |NGC 6934 is an intermediate-metallicity cluster with [Fe/H]=-1.47 C2031p072 |according to the 2010 update of the Harris (1996) catalogue. A C2031p072 |BV CM diagram by Piotto et al. (1999), based on HST observations, C2031p072 |shows a well populated HB with an extended blue HB and a well defined C2031p072 |sequence of blue stragglers. C2031p072 |The most extensive investigation of the variable stars was by C2031p072 |Kaluzny et al. (2001). All of the data in the above table are from C2031p072 |their study unless indicated otherwise in the Notes on individual stars. C2050m127 |The RA and dec are from the following sources: V1-42 (Samus et al. 2009), C2050m127 |V43-56 (Bramich et al. 2011), V57-58 (Skottfelt et al. 2013b) and V59-60 C2050m127 |(Amigo et al 2013). C2050m127 |Most of the remaining data are from the study by Amigo et al. (2013) C2050m127 |unless indicated otherwise in the Notes on individual stars. C2050m127 |The "CST" classifications are from Bramich et al. (2011). Since Amigo et al. C2050m127 |(2013) did not present any results for these stars, it is assumed they C2050m127 |also did not detect any variability. C2059p160 |The remote globular cluster NGC 7006 was one of the first clusters known C2059p160 |to exhibit the "second parameter" effect. Although it is relatively C2059p160 |metal poor, with [Fe/H] = -1.52 according to the 2010 update of the C2059p160 |Harris (1996) catalogue, the predominance of red stars on its horizontal C2059p160 |branch is characteristic of a more metal rich cluster. C2059p160 |The most recent and comprehensive investigation of the variable stars in C2059p160 |NGC 7006 was by Wehlau et al. (1999). C2059p160 |In the above table, the RA and dec are from Samus et al. (2009). C2059p160 |The remaining data are from Wehlau et al. (1999) unless indicated C2059p160 |otherwise in the remarks column where C2059p160 | SW refers to Sandage & Wildey (1967) C2059p160 | RC refers to Rosino & Ciatti (1967) C2059p160 | PR refers to Pinto & Rosino (1973) C2059p160 | W92 refers to Wehlau et al. (1992) C2127p119 | A major study of the RR Lyrae variables in M15 was C2127p119 | published by Corwin et al. (2008). Consequently, most of the C2127p119 | data listed for the RR Lyrae and Cepheids in the above table C2127p119 | are from the Corwin paper. C2127p119 | If an RR Lyrae or Cepheid was not studied by Corwin et al., the C2127p119 | data are from the discovery paper or from the source indicated C2127p119 | in the "Notes on individual stars" or in the "Remarks" column C2127p119 | where: C2127p119 | "S&S" refers to Silbermann & Smith (1995), C2127p119 | "Bing" refers to Bingham et al. (1984), C2127p119 | "Rosino" refers to Rosino (1969), C2127p119 | "Kadla" refers to Kadla et al. (1984) C2127p119 | Samus et al. (2009) published the RA and dec for the C2127p119 | stars investigated in the 4 papers listed above. C2127p119 | "Tuair" refers to Tuairisg et al. (2003) who derived C2127p119 | the RA & dec in addition to the other elements. C2127p119 | and C2127p119 | "TuCo"indicates that the positions, periods and C2127p119 | variability types are from Corwin et al. (2008) and C2127p119 | the mean magnitudes and amplitudes are from the paper C2127p119 | by Tuairisg et al. (2003). C2127p119 | Corwin et al. (2008) also pointed out that there is some C2127p119 | overlap among the variables listed by different authors. C2127p119 | This confusion occurred because Tuairisg et al. (2003) and C2127p119 | Zheleznyak & Kravtsov (2003) were writing their papers at the same C2127p119 | time. These identities are indicated in the Notes/Remarks column. C2127p119 | The data for V122, V123, V124, V125 (=X-1, AC211), V126, V127, C2127p119 | V156, V157, V158, ZK47, ZK62, ZK68, K757, K825, X-2, CV1, CV2 C2127p119 | are from their discovery papers unless indicated otherwise in the C2127p119 | notes. C2127p119 | An identification chart and catalogue of x,y positions for C2127p119 | most variables numbered up to 123 was publishd by Kadla et al. C2127p119 | (1988). C2127p119 | Please note, however, that Kadla's V113, 114, 122 and 123 C2127p119 | are not the same stars as the ones listed in the above table. C2127p119 | Their V113 is our V122 and their V114 is NV3. Kadla's V122 and C2127p119 | V123 refer to Kustner #880 and #263 and are not listed in the C2127p119 | table because their variability has not been confirmed in other C2127p119 | investigations. Both stars were located in the field of view of C2127p119 | the investigation of Corwin et al. (2008), but were not detected C2127p119 | as variables. C2127p119 | Kustner (1921) listed x,y positions for 1137 stars in M15. His C2127p119 | catalog numbers have been cited by many authors. C2130m010 |For V1-34: C2130m010 | The RA and dec are from Samus et al. (2009) C2130m010 | Periods, magnitudes, amplitudes and variability types are C2130m010 | from Lee & Carney (1999) unless indicated otherwise in the C2130m010 | notes on individual stars. C2130m010 |For V35-V42: C2130m010 | All the data are from Lazaro et al. (2006). No magnitudes were C2130m010 | derived because they used the image subtraction technique. C2137m234 |The RA and dec listed for V1-13 are from Samus et al. (2009) and those C2137m234 |for V14-21 are from Kains et al. (2013). The remaining data are from C2137m234 |the study by Kains et al. (2013) unless indicated otherwise in the notes. C2137m234 |All of the data for V22-26 are from the discovery paper by Pietrukowicz & C2137m234 |Kaluzny (2004). They are their M30_04 to M30_08, respectively. C2143m214 |The RA and dec for V1-3 are from Samus et al. (2009). C2143m214 |V1-V2: The magnitudes, amplitudes and variability types for V1&2 C2143m214 | are from Kinman & Rosino (1962). The membership status is from C2143m214 | Rosino & Ortolani (1985) based on the CM diagram published by C2143m214 | Harris & Canterna (1980) C2143m214 |V3: The magnitude for V3 is from Kinman & Rosino (1962) and the C2143m214 | possibility that this object was a supernova in a faint C2143m214 | galaxy was suggested by Rosino & Ortolani (1985). C2143m214 |None of these variables were detected in a search for RR Lyrae variables C2143m214 |by Salinas et al. (2005). Thus their variability is questioned. C2304p124 |The periods, magnitudes, amplitudes and variability types for C2304p124 |V1-4 are from Ciatti et al. (1965). C2305m159 |All the data for V1-2 and V4-7 are from Figuera Jaimes et al. (2013). C2305m159 |V3 was outside their field. For V3, the RA and dec are from Samus et C2305m159 |al. (2009) and the remaining data are from the discovery paper by Barnes C2305m159 |(1968). C2305m159 |The CM diagram (VR) by Figuera Jaimes et al. (2013) shows a well C2305m159 |populated blue HB. CJ1808m198|This "candidate" globular cluster was discovered by by Hurt et al. CJ1808m198|(2000) in the Two Micron All-Sky Survey (2MASS) data set and CJ1808m198|confirmed by Ivanov et al. (2000) from an near IR (K,J-K) CM diagram. CJ1809m207|All of the data listed for V1-5 are from Borissova et al. (2007) who CJ1809m207|noted that the near IR (K,J-K) CM diagram has a predominantly red HB. CJ1809m207|This "candidate" globular cluster was discovered by by Hurt et al. (2000) CJ1809m207|in the Two Micron All-Sky Survey (2MASS) data set and confirmed by CJ1809m207|Ivanov et al. (2000) from an near IR (K,J-K) CM diagram. CJ1809m464|This object was considered to be a heavily obscured open cluster CJ1809m464|until Ortolani et al. (2000) plotted a VI CM diagram. The morphology CJ1809m464|of their CMD indicated a metal poor cluster with a blue HB.