| File --- | Note --- |
|---|---|
| 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 <V>= 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. |