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'I:Os|FiT3vA.u!wLfol1L d$IqfQ(*[2F 6VMnxR)kdcQ̲pqFW+2VpG!M +J"G/Ə^Ԉ.)YRu:<9IzY4?6#$0ɾGn͝$&B)%Gj䆓~|4--VXͦ>#FSˎWQ J;tuQH?Mg>-dFAw.ysOuY7)JR?j4=u^\dV8>MvtYOXIz(4(NOӇeqt,RFRyYR6VIC $5YnP=-ɷuw =.3H 4(Ov9yϡ]R'3%R>L>Cjϧn5'^%`YԬES,|z?ߚ; T&U3Lǡ OVwdM0iʱpl`o]eYslx-"nSѢf]i5-<^3v='h2N;<g1rEqct3I/ڡI v)KNTJHM*ҍiY9qV%+),LJ[bPeiSIؔ5 /| 4x0Ej>.%}n4?8 qL/bw܅z`}"ñרEL ާ 9`@@QKP7`]"tz,@Nf1zAH$s g}GPe9۾Y$䗄]Qb_|W7ͽ~< 4\"J.~ݕja  j ?) &chHVH"4FtSf#I^]5~xN0 sCTʫ39Sa޶fA n{^zy*fڨ}ʰd(3/ysN,E'Wz;7pq ;ct G|plZa xQ$=.@8.p}.C_&o!vj[ e ә/OZ84:Jl T((9$BI'OXf>^ f (dpc7X+,LvӸ=?$`Dyfd2q@ppe0*=$E7>e{"|9y 8a.ҫfs8b"# Ţ^βl7_bf"^ )F8H)e%tPZbu*gx2LRcq:MsJph ;VZ nKoo7`o2:lWd>BSR#Table: V/150/notedisc.dat (http://cdsarc.cds.unistra.fr) # ------------------------------------------------------------------------------------------------ File |Note ----------|------------------------------------------------------------------------------------- C0021m723 |V1-8 C0021m723 | Bailey (1902) with x,y positions (see Table XXIV, p 237) and an C0021m723 | ID chart (Plate 252.19) C0021m723 |V9-12 = HV 810, HV 811, HV 813, HV 814 C0021m723 | McKibben-Nail (1951) with x,y positions C0021m723 | The numbers V9-12 were assigned by Sawyer (1955) in her 2nd C0021m723 | catalogue. C0021m723 | These variables had been discovered earlier by Levitt (1908) in a C0021m723 | study of the SMC. There was also a suspected variable HV 812, but C0021m723 | McKibben-Nail (1951) considered its variability to be doubtful. C0021m723 | Consequently, Sawyer (1955) did not list it in her catalogue. C0021m723 | No ID charts were published at the time of discovery. C0021m723 | In subsequent studies of 47 Tuc, plates showing these variables C0021m723 | were published. C0021m723 | V9: An ID chart was published by Feast & Thackeray (1960). C0021m723 | V10 = HV 811: This star was labelled in the SMC Atlas (Hodge & Wright C0021m723 | 1977 - see chart 20B) C0021m723 | V11 = HV 813: This star was labelled as W12 by Lloyd Evans & Menzies C0021m723 | (1973) because, in their Table II, they noted that V11 (HV 813) C0021m723 | is star #12 labelled by Wildey (1961) C0021m723 | V12 = HV 814: C0021m723 | HV 814 was labelled in the SMC Atlas (Hodge & Wright 1977 - C0021m723 | see chart 20B). It was also labelled as star #7317 by C0021m723 | Lee (1977 - see section 4.2 and the southeast segment of C0021m723 | Figure 1 in his paper. C0021m723 | V9, V10 and V11 were also labelled on an ID chart by Fourcade et al. C0021m723 | (1966). C0021m723 |V13-14 C0021m723 | Fourcade et al. (1966) with x,y coordinates and an ID charts C0021m723 | They noted that Wilkens had discovered V13. C0021m723 |V15 = Star #300 labelled on an ID chart by Wildey (1961) C0021m723 | Arp et al. (1963) demonstrated that Wildey's star #300 C0021m723 | was probably variable and Eggen (1972) confirmed it. C0021m723 | The number V15 was assigned by Sawyer Hogg (1973). C0021m723 |V16 = Star #18 labelled on Plate I of Feast & Thackeray (1960) C0021m723 | According to Sawyer Hogg (1973), the variablility of this star was C0021m723 | announced by Brooke in a 1969 Doctoral Thesis at the Australian C0021m723 | Nat'l Univ (1969). Lloyd Evans & Menzies (1973) pointed out that C0021m723 | Brooke's variable is #18 of Feast & Thackeray (1960). C0021m723 | Lloyd Evans (1974) labelled it as R18 on Plate II in his paper. C0021m723 | The number V16 was assigned by Sawyer Hogg (1973). C0021m723 |V17 = Star #81 labelled on an ID chart by Wildey (1961) C0021m723 | Eggen (1972) showed that this star was variable. C0021m723 | The number V17 was assigned by Sawyer Hogg (1973). C0021m723 |V18-28 are red variables announced by Lloyd Evans & Menzies (1973) C0021m723 | who labelled most of them on a plate they published. C0021m723 | In addition, all but one of these variables were later labelled on C0021m723 | a plate by Lloyd Evans (1974) C0021m723 | V18 = L168 labelled as V11 in 1973 and L168 in 1974 (Plate II) C0021m723 | V19 = R10 identified in 1973 and 1974 (Plate I) C0021m723 | V20 = A1 identified in 1973 and 1974 (Plate I) C0021m723 | V21 = A2 identified in 1973 and 1974 (Plate I) C0021m723 | V22 = A4 identified in 1973 and 1974 (Plate I) C0021m723 | V23 = A6 identified in 1974 (Plate II), but not in 1973 C0021m723 | V24 = A8 identified in 1973, but not in 1974 C0021m723 | V25 = A9 identified in 1973 and 1974 (Plate II) C0021m723 | V26 = A13 identified in 1973 and 1974 (Plate I) C0021m723 | V27 = A18 identified in 1973 and 1974 (Plate I) C0021m723 | V28 = LR5 identified in 1974 (Plate II), but not in 1973 C0021m723 |V29-41 = V1-13 C0021m723 | Edmonds et al. (1996) who published x,y (arcsec) positions C0021m723 | and an ID chart C0021m723 | The numbers V29-41 were assigned in this electronic catalogue. C0021m723 | Samus et al. (2009) later derived RA and dec (Epoch 2000) C0021m723 | Albrow et al. (2001) referred to these stars as PC1-V01 to V13 C0021m723 | and published new data for six of them. For these 6 stars, the RA C0021m723 | values derived by Albrow et al. have a systematic shift relative to C0021m723 | the values of Samus et al. (2009) which were based on Geffert et al. C0021m723 | (1997). The Samus values are larger on average by 0.29 sec than those C0021m723 | derived by Albrow et al. This is equivalent to about 1.3 arcseconds. C0021m723 |V42-53 = OGLEC 214 (Wel61), 221 (Wel 32), 225 (Wel100), 227 (Wel6), C0021m723 | OGLEC 228 (Wel7), 238 (Wel30), 240 (Wel85), 244 (Wel56), C0021m723 | OGLEC 245 (Wel95), 249 (Wel51), 250 (Wel14), 253 (Wel12) C0021m723 | C0021m723 | Kaluzny et al. (1998) with 1950 RA and dec and X,Y coordinates C0021m723 | in pixels. In their study, they detected 42 new variables, but these C0021m723 | 13 were the ones they considered to be cluster members. C0021m723 | V42 (OGLEC 214) was announced in an earlier study by Kaluzny et C0021m723 | al. (1997) where it was listed as V6. A finder chart was published C0021m723 | in the 1997 paper. C0021m723 | The numbers V42-53 were assigned in this electronic catalogue and C0021m723 | the 2000 RA and dec were later derived by Samus et al. (2009) C0021m723 | These 12 variables were all detected later by Weldrake et al. C0021m723 | (2004) and the "Wel" numbers listed above refer to their numbering C0021m723 | system. C0021m723 | Kaluzny et al. (1998) also listed properties for 6 variable K giant C0021m723 | stars that might be cluster members: OGLEC 219, OGLEC 220, 222, C0021m723 | 229, 231, 237. C0021m723 | Variability was detected in four of these stars by Weldrake et al. C0021m723 | (2004) and they are now listed as variables Wel9 (222), Wel15 (219), C0021m723 | Wel28 (229) and Wel31 (220) in the above table. C0021m723 |V54-56 = V14-16 of Gilliland et al. (1998) C0021m723 | who published delta RA and delta dec in arcseconds. C0021m723 | The numbers V54-56 were assigned in this electronic catalogue. C0021m723 | Samus et al. (2009) later derived RA and dec (Epoch 2000) C0021m723 | Albrow et al. (2001) referred to thse stars as PC1-V14 to V16 C0021m723 |Par-V1 (= PC1-V47) C0021m723 | Par-V1 is a variable star that Paresce et al. (1992) discovered close C0021m723 | to Einstein X-ray source X0021.8-7221. In a later paper (Paresce et C0021m723 | al. 1994), they referred to it as V1. Its RA and dec were published C0021m723 | by Geffert et al. (1997). C0021m723 | In a subsequent study, Albrow et al. (2001) announced the variable as C0021m723 | PC1-V47 and derived an RA that was 0.31 seconds lower than Geffert's C0021m723 | value. Edmonds et al. (2003a) subsequently published an ID chart. C0021m723 |Par-V2 (= PC1-V53) C0021m723 | Par-V2 is V2 of Paresce & De Marchi (1994) and they identified the C0021m723 | variable on a series of three HST images. Its RA and dec were C0021m723 | published by Geffert et al. (1997) C0021m723 | In a later study, Albrow et al. (2001) announced the variable as C0021m723 | PC1-V53 and derived an RA that was 0.30 seconds lower than Geffert's C0021m723 | value. Edmonds et al. (2003a) subsequently published an ID chart. C0021m723 | NOTE: There are discrepancies in the values of the RA derived for C0021m723 | the "Paresce" variables by different authors. C0021m723 | For Paresce-V1 (W42, PC1-47) and V2 (W30, PC1-V53)) the RA values C0021m723 | of Geffert et al. (1997), Grindlay et al. (2001), and Heinke et al. C0021m723 | (2005) are approximately 0.3 seconds larger than those published by C0021m723 | Albrow et al. (2001) and Edmonds et al. (2003a). This corresponds C0021m723 | to approximately 1.4 arcseconds. C0021m723 | C0021m723 |Sha-V3 C0021m723 | Shara et al. (1996) with an HST "difference image" showing its C0021m723 | position relative to Par-V2 (Fig 3c). Grindlay et al. (2001) C0021m723 | identified the star as the optical counterpart to Chandra X-ray C0021m723 | source W27 and Edmonds et al. (2003b) published a finding chart (see C0021m723 | Figure 9 of their paper). C0021m723 |PC and WF variables C0021m723 | Albrow et al. (2001) with RA and dec C0021m723 | PC1, WF2, WF3, and WF4 in the numbering system refer to the C0021m723 | 4 different HST CCD fields. C0021m723 | Many of these variables are optical counterparts to Chandra C0021m723 | X-ray sources. Cross-reference lists were published by Edmonds C0021m723 | et al. (2003a) and by Heinke et al. (2005). C0021m723 |W11_opt = U_opt of Edmonds et al. (2001) who published a finding chart, C0021m723 | derived RA, dec and demonstrated that this is the white dwarf C0021m723 | companion to the MSP 47 Tuc U. The number W11_opt was assigned in C0021m723 | this catalogue. C0021m723 |W29_opt C0021m723 | Edmonds et al. (2002a) with a finding chart, RA and dec C0021m723 | They demonstrated that this is the optical companion to the C0021m723 | MSP 47 Tuc W. C0021m723 |W34_opt C0021m723 | Edmonds et al. (2002a) with RA, dec C0021m723 | They concluded that this object might be associated with an unknown C0021m723 | MSP. C0021m723 |Other W#_opt variables C0021m723 | Edmonds et al. (2003a) with RA, dec (see Tables 3 and 4) C0021m723 | Some of the stars were listed in Table 3, some in Table 4 and some in C0021m723 | both Tables. The Table 3 values are listed if available. In cases, C0021m723 | where stars were listed in both tables, there are systematic shifts C0021m723 | in RA and dec in the sense that the Table 4 RA values are ~0.3 seconds C0021m723 | further east (which corresponds to ~1 arcsecond) and 0.33 arcseconds C0021m723 | further south. C0021m723 | ID charts were published for some of the variables: C0021m723 | W15_opt, W21_opt, W25_opt, W26_opt, W34_opt, W44_opt, W45_opt by C0021m723 | Edmonds et al. (2003a) and C0021m723 | W44_opt, W51_opt, W53_opt, W56_opt, W120_opt, W122_opt by C0021m723 | Edmonds et al. (2003b). C0021m723 | These variables were detected in the HST data of Albrow et al. C0021m723 | (2001), but were not reported in Albrow's 2001 paper. C0021m723 |A19 C0021m723 | Lloyd Evans (1974) who identified it on plate II of his paper C0021m723 | The RA and dec were later published by Lebzelter & Wood (2005) C0021m723 |LW1-22 C0021m723 | Lebzelter & Wood (2005) who published RA and dec. C0021m723 |Wel9, Wel15, Wel16, Wel21, Wel25, Wel28, Wel31, Wel61, Wel69, Wel78, C0021m723 |Wel93, Wel96: C0021m723 | Weldrake et al. (2004) with RA, dec and individual finder charts. C0021m723 | These authors carrried out a comprehensive search for stellar C0021m723 | variability in 47 Tucanae as part of a search for transiting "hot C0021m723 | Jupiters" in 47 Tucanae. C0021m723 | They detected 100 variables, 69 of which were new discoveries. C0021m723 | Based on positions on a V-(V-I) plot, they concluded that most C0021m723 | of the variables belong to the SMC. The variables listed here are C0021m723 | are the ones that are probably associated with 47 Tuc. In addition, C0021m723 | Weldrake et al. recovered the 12 binary systems, V42-V53, that were C0021m723 | announced earlier by Kaluzny et al. (1998). (See announcement of C0021m723 | V42-53 above.) C0021m723 | The membership status of three additional variables, Wel26, Wel17 C0021m723 | and Wel34, was not clear, but in a subsequent investigation by C0021m723 | Kaluzny et al. (2013), it appears that they may belong to the C0021m723 | cluster. They are listed in the above table as KalE1, KalE35 and C0021m723 | KalE23 respectively. C0021m723 |KalW1, 2, 4, 5, 7, 8, 12, 14 and C0021m723 |KalE1, 8, 19, 23, 25, 31, 32, 33, 34, 35, 36, 39: C0021m723 | Kaluzny et al. (2013) with RA and dec for all of the variables C0021m723 | and individual finder charts for all except KalE1, E8, E23 and E35 C0021m723 | which had been identified previously by Kaluzny et al. (1998) or by C0021m723 | Weldrake et al. (2004). C0021m723 | Table 1 of Kaluzny et al. (2013) lists the IDs for the variables C0021m723 | from previous investigations. C0021m723 |EM1-7 C0021m723 | Figuera Jaimes et al. (2016) with RA, dec and an ID chart C0021m723 |-------------------------------------------------------------------- C0021m723 |PSR: According to Paulo Freire's website, there are 26 millisecond C0021m723 | pulsars in 47 Tuc. (www.naic.edu/~pfreire/GCpsr.html) C0021m723 |----------------------------------------------------------------------- C0021m723 |Edmonds, P. D. & Gilliland, R. L. 1996, ApJ, 464, L157 reported C0021m723 |the discovery of variability among K giants in 47 Tuc, mostly with C0021m723 |periods in the 2-4 day range and V amplitudes in the range 5-15 nmag. # C0050m268 | V1 C0050m268 | Oosterhoff (1943) with its 1900 RA & dec, x, y coordinates and an ID C0050m268 | chart C0050m268 | V2 C0050m268 | Hollingsworth & Liller (1977) with x,y coordinates and an ID chart C0050m268 | which showed the positions of both V1 and V2 C0050m268 | V3-7 C0050m268 | Kaluzny (1996) with X,Y in pixels for V1-V7 C0050m268 | V8-10 C0050m268 | Kaluzny et al. (1997) with RA & dec (2000) and finding charts C0050m268 | for V2-10. C0050m268 |--------------------------------------------------------------- C0050m268 |Arellano Ferro et al. (2013) conducted a search for additional C0050m268 |variables, but did not find any. C0050m268 |---------------------------------------------------------------- C0050m268 |Pietrukowicz et al. (2008) searched for dwarf novae in NGC 288, but did C0050m268 |not find any. However, they pointed out that their observations covered C0050m268 |only two nights in 2004 and seven nights in 2005. They also carried out C0050m268 |an independent visual inspection of optical counterparts to seven X-ray C0050m268 |sources listed by Kong et al. (2006), three of which (CX13, CX20 and C0050m268 |CX24) were CV candidates. They did not detect brightness variations at C0050m268 |the positions of any of these objects. C0050m268 |------------------------------------------------------------------- C0050m268 |Lynch & Ransom (2011) conducted a search for pulsars, but did not find C0050m268 |any in NGC 288. # C0100m711 |V1-14 C0100m711 | Bailey (1902) with x,y coordinates on pages 237-238 and an ID chart C0100m711 | (see Plate IX, Fig 1, page 252.15) C0100m711 |V15 C0100m711 | Fourcade et al. (1966) with x,y coordinates and an ID chart C0100m711 | According to Samus et al. (2009), these x,y coordinates are not C0100m711 | accurate. They do not agree with the position labelled on the ID C0100m711 | chart that Fourcade et al. published. The RA and dec listed in the C0100m711 | above table are from Szekely et al. (2007) who identified a variable C0100m711 | star near V15's position on Fourcade's chart. C0100m711 |V16 C0100m711 | Lloyd Evans (1983) with an ID chart C0100m711 |V17-28 C0100m711 | Rozyczka et al. (2016) with RA, dec and individual finding charts C0100m711 | and found them all to be cluster members based on proper motion. C0100m711 |VN01-04 C0100m711 | Rozyczka et al. (2016) identified these variables as possible cluster C0100m711 | members and listed their RA and dec. C0100m711 | In addition they discovered and derived periods for 42 field variables C0100m711 | which they numbered VN05 to VN46. A few of these had been previously C0100m711 | announced by Soszynski et al. (2016) in the OGLE survey. C0100m711 |Sz variables C0100m711 | Szekely et al. (2007) with RA and dec C0100m711 | The Sz variables that are probably cluster members are listed in the C0100m711 | above table. The others are discussed in the note at the end of this C0100m711 | section. C0100m711 |LW1-10 C0100m711 | Lebzelter & Wood (2011) with RA and dec C0100m711 | These authors also noticed three other red stars LW11-13 that showed C0100m711 | light variability but did not follow any (semi-)periodicity. C0100m711 | R16 observed LW12 and LW13(Sz61), but did not detect any variability. C0100m711 | LW13 is the same star as Sz61 and is listed as a possible long period C0100m711 | variable in the above table. C0100m711 |------------------------------------------------------------------------ C0100m711 |Dalessandro et al. (2013) announced the discovery of 7 new variables in C0100m711 |the cluster: C0100m711 |4 W UMa stars (C_WUMa 1 to 4) and 3 SX Phe stars (C_SX 1 to 3) C0100m711 |See section 5.2 of their paper. They plotted light curves (Figs 10 and C0100m711 |11), but did not publish positions, magnitudes or periods. C0100m711 |Therefore it is not known whether or not these variables were among the C0100m711 |WUMa and SXPhe variables subsequently announced by R16 C0100m711 |----------------------------------------------------------------------- C0100m711 |Pietrukowicz et al. (2008) searched for dwarf novae in the area outside C0100m711 |the core of NGC 362. Their data consisted of 1424 V frames obtained on C0100m711 |90 nights over the years 1997 to 2005. No outbursts were detected. C0100m711 |------------------------------------------------------------------------ C0100m711 |Margon et al. (2010) identified approximately 100 X-ray sources in NGC 362 C0100m711 |on Chandra images. The majority are assumed to be cluster members. C0100m711 |Multi-colour HST photometry of objects within 1 arcsec of these sources C0100m711 |indicates that many are probably associated with CVs. In addition, one C0100m711 |is probably a classical quiescent low-mass X-ray binary (qLMXB) based on C0100m711 |its position in an X-ray "luminosity-colour" diagram. Their C0100m711 |investigation is ongoing. C0100m711 |------------------------------------------------------------------------ C0100m711 |Notes about the Sz variables C0100m711 | Szekely et al. (2007) listed RA and dec for 84 variables in NGC 362 and C0100m711 | the surrounding field. Of these, 69 were new discoveries and 15 were C0100m711 | previously known. It should be noted that Szekely (2006) announced C0100m711 | some of these variables earlier, but in the earlier paper, he used a C0100m711 | different numbering system. The numbering system adopted in this C0100m711 | catalogue is from Szekely et al. (2007). C0100m711 | In the above table, the original numbering system is maintained for the C0100m711 | previously known variables. C0100m711 | Thus Sz7=V9, Sz15=V1, Sz23=V11, Sz27=V5, Sz31=V4, Sz35=V12, Sz40=V14, C0100m711 | Sz51=V16, Sz55=V13, Sz60=V8, Sz67=V6, Sz68=V3, Sz71=V7, Sz72=V15, C0100m711 | Sz75=V10. Szekely's numbers are noted in the remarks column. (The C0100m711 | semiregular variable V2 was not recovered by Szekely et al.) C0100m711 | A montage of CMDs plotted by Szekely et al. for different radial C0100m711 | distances shows significant contamination by field stars in the outer C0100m711 | regions. In fact, many of these field stars are located inside the C0100m711 | tidal radius which Harris (1996) estimated to be 10.4 arcmin in the 2010 C0100m711 | revision of his catalogue. The Sz variables which are considered to be C0100m711 | possible cluster members are listed in the above table. An explanation C0100m711 | for why the remaining variables are excluded is given in the discussion C0100m711 | below. C0100m711 | RR Lyrae C0100m711 | The RR Lyrae variables Sz1, Sz6, Sz8, Sz12, Sz16, Sz73, Sz80, Sz81 C0100m711 | are too faint to be cluster members. C0100m711 | R16 determined that Sz12 is not a cluster member, based on proper C0100m711 | motion and concluded the star is an SMC RR Lyrae variable. C0100m711 | Sz10: The classification of this star is uncertain because R16 did C0100m711 | not detect any regular variability. Furthermore S07 did not list C0100m711 | a mean magnitude, colour or period for this star, even though it was C0100m711 | located well outside the crowded central region. C0100m711 | Sz78: S07 did not list a mean magnitude or colour even though the star C0100m711 | is located well outside the crowded central region. Furthermore, the C0100m711 | period-amplitude data they listed for it are not appropriate for an C0100m711 | NGC 362 RR Lyrae variable. C0100m711 | Sz78 was not discussed by R16. It is assumed that Sz78 is not an C0100m711 | NGC 362 RR Lyrae variable. C0100m711 | Cepheids C0100m711 | The Cepheids Sz5, Sz11, Sz14, Sz21, Sz22, Sz30, SZ60 (=V8), Sz72 (=V15) C0100m711 | and Sz75 (=V10) are all too faint to be cluster members. C0100m711 | Also, the candidate Cepheids Sz25 and Sz76 are probably not cluster C0100m711 | members. Sz25 is too faint and Sz76 is too red. C0100m711 | R16 had difficulty producing a light curve for Sz25, but they were C0100m711 | certain that it is not a Cepheid. C0100m711 | R16 did not detect any variability in Sz76. C0100m711 | SXPhe C0100m711 | The Delta Scuti/SX Phe variable Sz79 is too faint for cluster membership. C0100m711 | Sz52 and Sz63 seem too bright, but both stars are close to the cluster C0100m711 | centre and their excessive brightness is attributed to the effects of C0100m711 | crowding. They are probably members and are included in the table. C0100m711 | Sz3, with r=11.1 arcmin, lies beyond the tidal radius, 10.6 arcmin, but C0100m711 | its position in the CMD is appropriate for membership in NGC 362. It C0100m711 | is a possible member and is therefore included in the table. C0100m711 | Eclipsing C0100m711 | The eclipsing variables Sz9, Sz13 and Sz28 all have CMD locations that C0100m711 | make them unlikely cluster members. Furthermore, Sz9 and Sz13 are C0100m711 | located ~10.4 and ~15 arcmin respectively from the cluster centre - C0100m711 | close to or beyond the tidal radius. C0100m711 | R16 observed Sz9 and Sz28 confirmed that they are not cluster members C0100m711 | based on proper motion. C0100m711 | Sz2, an Algol type eclipsing system, is located in the blue straggler C0100m711 | region of the CMD, but it lies 17 arcmin from the cluster centre, C0100m711 | well beyond the tidal radius. Sz82 and Sz83 are also beyond the tidal C0100m711 | radius. None of these stars are considered to be cluster members. C0100m711 | Sz18 is located at ~3 arcmin from the cluster centre. Its position on C0100m711 | the CMD is not known, but given its location in the central region of C0100m711 | the cluster, it is assumed to be a cluster member. R16 (2016) were C0100m711 | unable to derive reliable magnitudes for this star because its image C0100m711 | was partly blended with an overexposed star. C0100m711 | Long period C0100m711 | The long period variables Sz19 and Sz84 are not considered to be C0100m711 | cluster members. Sz19 is too faint and Sz84 is well beyond the tidal C0100m711 | radius. R16 confirmed the variability of Sz19 and concluded that the C0100m711 | star belongs to the SMC based on its proper motion and CM diagram C0100m711 | location. C0100m711 | Sz17, Sz36 (=LW1), Sz51 (=V16) and Sz61 are all considered C0100m711 | plausible cluster members and are listed in the above table. C0100m711 | However, R16 did not detect any variability in Sz61. C0100m711 | Unclassified C0100m711 | Sz4, Sz24, Sz59, Sz66, Sz70, Sz77 were not classified by S07. These C0100m711 | stars were all observed by R16 and consequently none of them are C0100m711 | listed in the above table for the following reasons. C0100m711 | Sz4 was not observed by R16 and not enough information is currently C0100m711 | available to list it in the table of variables. C0100m711 | Sz24, Sz59, Sz66, Sz77: R16 did not detect any variability in any C0100m711 | of these stars. Thus it is unlikely that any of them are variable. C0100m711 | Sz70: R16 concluded that this star is an SMC RR Lyrae variable. # C0310m554 | V1-11 C0310m554 | Fourcade et al. (1966) with x,y coordinates and an ID chart C0310m554 | In a separate paper, Laborde & Fourcade (1966) had announced C0310m554 | V1-6 with x,y coordinates and an ID chart. It turned out that they C0310m554 | had a different identification for V4 on their two ID charts C0310m554 | and neither was correct. This was pointed out by Wehlau et al. C0310m554 | (1977) who derived the correct coordinates. The ID chart for V1-15 C0310m554 | published by Wehlau & Demers (1977) shows the correct position for V4. C0310m554 | V12-15 C0310m554 | Bartolini et al. (1972) with x,y coordinates. Bartolini announced C0310m554 | these new variables in an earlier paper (Bartolini et al. 1971), C0310m554 | but with a different numbering system. When they wrote their 1971 C0310m554 | paper, they were aware of the discovery of V1-6, but not V7-11. The C0310m554 | numbering system assigned in their 1972 paper supersedes the older one. C0310m554 | The sign of the y coordinate they listed for V12 was incorrect. It C0310m554 | should have been +10.5 instead of -10.5. This incorrect value C0310m554 | also appeared in Sawyer Hogg's 3rd catalogue. The error was later C0310m554 | pointed out by Wehlau et al. (1977). C0310m554 | V16-21 C0310m554 | Wehlau et al. (1977) with x,y coordinates. C0310m554 | V22-30 C0310m554 | Salinas et al. (2007) with x,y coordinates and an ID chart. C0310m554 | No magnitudes or amplitudes were derived because they used the C0310m554 | image subtraction technique. C0310m554 | They also re-discovered all of the previously announced variables C0310m554 | except V1 and V18, which they considered to be non-variable. # C0512m400 |V1-2 = HV 3732-3733, = Z and Y Col C0512m400 | Bailey (1924) with x,y coordinates and 1900 RA and dec. The numbers C0512m400 | V1 and 2 were assigned by Sawyer (1939) in the first edition of her C0512m400 | variable star catalogue. C0512m400 |V3-10 C0512m400 | Fourcade et al. (1966) with x,y coordinates and an ID chart. V1 C0512m400 | and 2 were also labelled on their chart. C0512m400 |V11-14 C0512m400 | Liller (1975) with ID chart for V1-14 C0512m400 |V15-21 C0512m400 | Wehlau et al. (1978) with an ID chart for V1-21, x,y coordinates C0512m400 | for V11-21 and revised x,y coordinates for V3 and V7 because their C0512m400 | positions were incorrectly given by their discoverers, Fourcade et C0512m400 | al. (1966). C0512m400 |V22-25 = Stetson's stars 55, 159, 168, 244 C0512m400 | Stetson (1981) noted that these stars were all variable, but did C0512m400 | not have enough data to follow up. He published an ID chart for the C0512m400 | stars in his study. C0512m400 | Wehlau et al. (1982) confirmed their variability, assigned the numbers C0512m400 | V22-V25, and derived x,y coordinates. Wehlau et al. also published C0512m400 | revised x,y coordinates for V18 because an incorrect position was given C0512m400 | in their earlier paper (Wehlau et al. 1978). C0512m400 |V26 = Stetson's star 340 C0512m400 | Wehlau et al. (1982) with x,y coordinates. C0512m400 | Stetson (1981) had noted that this star was located in the RR Lyrae C0512m400 | instability strip of the CM diagram, but his data were not sufficient C0512m400 | to detect any variation. Stetson's star #368 was also in the C0512m400 | instability strip, but Wehlau et al. did not detect any variation. C0512m400 | They concluded that the apparent location of #368 in the instability C0512m400 | strip was due to its proximity to a blue star. C0512m400 |V27-33 C0512m400 | Walker (1998) with an ID chart for these 7 new variables. His ID C0512m400 | chart also included the 22 RR Lyrae stars among V1-26. C0512m400 |V34-52 C0512m400 | Sumerel et al. (2004) with x,y coordinates C0512m400 |V53 = RR7 C0512m400 | Downes et al. (2004) with RA, dec and ID charts and confirmed by C0512m400 | Corwin (2009, private communication). The number V53 has been assigned C0512m400 | in this catalogue. C0512m400 | Downes et al. listed 10 other RR Lyrae candidates, but some of C0512m400 | these were already announced by Sumerel et al. (2004). C0512m400 | Further discussion of Downes' candidate variables is given below, C0512m400 | at the end of this section. C0512m400 |V54-55 C0512m400 | Layden et al. (2010) with RA and dec C0512m400 | These authors also identified seven stars as new suspected variables. C0512m400 |X-1 = MX 0513-40 = 4U 0513-40 C0512m400 | This variable X-ray source was announced by Clark et al. (1975). C0512m400 | The variability of the optical component was detected by Zurek et al. C0512m400 | (2009) who derived a 17 minute periodicity based on FUV C0512m400 | observations. C0512m400 |PSR = PSR J0514-4002A, a binary millisecond pulsar: NGC 1851A C0512m400 | Freire et al. (2004) with RA and dec. (rotation period = 4.99 ms) C0512m400 |----- C0512m400 |Suspected RR Lyrae variables identified in other studies C0512m400 | Saviane et al. (1998) listed 7 RR Lyrae candidates with x,y C0512m400 | positions. They selected their candidates by comparing their observed C0512m400 | V magnitudes with the V magnitudes published by Walker (1992) for a CM C0512m400 | diagram study. They also used their data to derive a mean V magnitude C0512m400 | of the previously known RR Lyrae in the cluster and calculated the C0512m400 | differences between the observed V magnitudes of their candidates and C0512m400 | this mean. Their best four candidates, n1-4, appear to be V50, V29, C0512m400 | V27 and V32 in the above table. C0512m400 | Downes et al. (2004) listed 11 RR Lyrae candidates with RA and dec C0512m400 | (2000) and ID charts. They based their selection on HST far ultraviolet C0512m400 | photometry obtained over an interval of 320 minutes, in a 25 by 25 C0512m400 | arcsec field around the cluster core. C0512m400 | Corwin (2009, private communication) who was a co-author of the C0512m400 | Sumerel et al. paper investigated these candidates and reached C0512m400 | the following conclusions. Downes RR2, RR4, RR6, RR8 and RR11 are C0512m400 | V39, V44, V36, V41 and V43 respectively. RR9 and RR10 were not C0512m400 | resolved as separate stars in the Sumerel et al. data, but one of C0512m400 | them is probably V40. Among Downes' other candidates, Corwin C0512m400 | commented that RR1, RR3 and RR5 are possible variables and that C0512m400 | RR7 is variable. We have therefore listed RR7 as V53 in the above C0512m400 | table. C0512m400 | Amigo et al. (2011) announced four variables, NV1 to NV4, as part of C0512m400 | some preliminary work on variable stars in CMa globular clusters. C0512m400 | Their NV4 appears to be V21 and their NV3 could be the same star as V47. # C0522m245 |V1-5 C0522m245 | Bailey (1902) with x,y coordinates (page 238) and an ID chart C0522m245 | (plate X, Fig 2, page 252.19) C0522m245 |V6 C0522m245 | Rosino (1952) with x,y coordinates and an ID chart for V1-6 C0522m245 | (The ID chart appeared in the Bologna Pub version of his paper, but C0522m245 | not in the electronic edition of Memoirs of the Italian Astronomical C0522m245 | Society.) Rosino made small corrections to the y coordinates published C0522m245 | by Bailey for V3 and V4 and commented that his V3 was too faint to be C0522m245 | detected on the print published by Bailey (1902). C0522m245 | C0522m245 |V7-8 C0522m245 | Tsoo Yu-hua (reported to Sawyer Hogg in a 1965 letter) C0522m245 | In her 3rd catalogue, Sawyer Hogg (1973) assigned the numbers V7-8 C0522m245 | and published their x,y coordinates. C0522m245 |V9-13 = NV1-5 C0522m245 | Amigo et al. (2011) with RA and dec C0522m245 |V14 C0522m245 | Kains et al. (2012) with RA, dec and ID charts C0522m245 | Variables V2-14 are all labelled on their ID chart. # C0647m359 |V1-2 C0647m359 | Fourcade et al. (1966) with x,y coordinates and an ID chart C0647m359 |V3 C0647m359 | Liller (1976) with ID chart for V1-3 C0647m359 |V4 C0647m359 | Clement et al. (1995) with x,y, coordinates and ID chart for V1-4 C0647m359 | The x,y coordinates were derived relative to the cluster centre C0647m359 | established by Janes & Heasley (1988) and the coordinates for V1 and C0647m359 | V2 were converted to this system. C0647m359 |---------------------------------------------------------------------- C0647m359 |In her first two catalogues, Sawyer (1939, 1955) indicated that there C0647m359 |were "6 unpublished variables, 5 suspected" according to a letter she C0647m359 |received from Shapley, but no further information was given. C0647m359 |-------------------------------------------------------------------- C0647m359 |Lynch & Ransom (2011) conducted a search for pulsars, but did not find C0647m359 |any in NGC 2298. # C0734p390 |V1-36 C0734p390 | Baade (1935, ApJ 82, 396) with x,y coordinates and an ID chart C0734p390 | He said his list should be complete for variables at distances greater C0734p390 | than 40 arcsec form the cluster centre, but no attempt was made to C0734p390 | discover variables in the central burnt out area. C0734p390 | Baade also listed max and min magnitudes for many of the variables C0734p390 | and Sawyer published these in her 1939 (first) catalogue. There was some C0734p390 | confusion about the magnitudes for V35 and in her 1955 (second) C0734p390 | catalogue, this was clarified after private correspondence with Baade. C0734p390 |V37-41 C0734p390 | Pinto & Rosino (1976, 1977) with x,y coordinates for V1-41 listed in C0734p390 | both papers and an ID chart in the 1977 paper C0734p390 |V42-101 C0734p390 | Ripepi et al (2007) anounced the discovery of these variables. C0734p390 | Di Criscienzo et al. (2011a) described them in more detail and C0734p390 | published J2000 RA and Dec coordinates for all 101 variables # C0911m646 |V1-7 C0911m646 | Fourcade et al. (1966) with x,y coordinates and an ID chart C0911m646 |V8-9 = stars 27 and 35 of C0911m646 | Alcaino (1971 - see page 366) with an ID chart on page 364. C0911m646 | The direction north (N) is incorrectly labelled on Alcaino's chart. C0911m646 | North is on the right side not at the top as he states. East is at C0911m646 | the top. C0911m646 | The numbers V8 and V9 were assigned by Sawyer Hogg (1973) C0911m646 | in her 3rd catalog. C0911m646 |V10-12 C0911m646 | Clement & Hazen (1989, AJ 97, 414) with x,y positions and an C0911m646 | ID chart which includes V1 and V6 as well. C0911m646 |V13-30 C0911m646 | Corwin et al. (2004) with RA, dec and an ID chart C0911m646 | V1, V6, V10, and V12 are also labelled on their chart. C0911m646 |V31-50 = LW1-20 C0911m646 | Lebzelter & Wood (2011) with RA and dec C0911m646 | The numbers V31-50 have been assigned in this catalogue. C0911m646 |----------------------------------------------- C0911m646 |Additional investigations of variables C0911m646 |Dieball et al. (2005) identified 6 variable stars from HST FUV C0911m646 |observations. They published RA, dec and an ID chart for all of C0911m646 |them: C0911m646 | #358 - an RR Lyrae on the ZAHB which they believed to be C0911m646 | Corwin's V22 C0911m646 | #76, #124, #162 - blue stragglers near the main sequence, C0911m646 | #124 a probable binary and the other C0911m646 | two probably pulsating variables C0911m646 | #222, #397 - possible CVs, between the WD and MS regions C0911m646 |Servillat et al. (2008) studied X-ray data from Chandra and XMM-Newton C0911m646 |and Hubble FUV data and found one neutron star quiescent low mass C0911m646 |X-ray binary and 8 CV candidates. C0911m646 |The qLMXB candidate (Chandra source #1 in their paper) has 2000 position C0911m646 |RA 9:12:01.91, dec -64:51:50.67. They also stated that one of their C0911m646 |CV candidates, Chandra source #7, is the same object as Dieball #222. C0911m646 |----------------------------------------------------------------- C0911m646 |Pietrukowicz et al. (2008) searched for dwarf novae in NGC 2808 based on C0911m646 |observations made during 33 nights in 1998 and 1999. No outbursts were C0911m646 |detected. # C0921m770 | V1-2: Mochejska et al. (2000) who also published an ID chart C0921m770 |--------------------------------------------------------- C0921m770 |Lan et al. (2010) identified three X-ray sources within the half mass C0921m770 |radius; they expected all of them to be background sources. However, C0921m770 |they also indicated the possibility that one source, E3-CX02, could be C0921m770 |a cataclysmic variable. # C1003p003 | V1-4 = star # 34, 155, 283, 102 respectively C1003p003 | Gratton & Ortolani (1984) with x,y pixel positions and an ID chart. C1003p003 | The numbers V1-4 were assigned in our electronic update to the Sawyer C1003p003 | Hogg catalogs (Clement et al. 2001). Their star #34 was outside the C1003p003 | field of view of subsequent invesigations. C1003p003 | V5 = star 188 of Gratton & Ortolani (1984), formerly V1 C1003p003 | This variable was first detected by Burbidge & Sandage (1958) C1003p003 | who published an ID chart (Figure 6 of their paper). C1003p003 | It was subsequently designated as V1 by Sawyer Hogg in her 3rd C1003p003 | catalog, but was removed from the electronic edition after C1003p003 | Gratton & Ortolani (1984) detected no variability. Since C1003p003 | then, two independent investigations (Borissova et al. 1998; C1003p003 | Stetson et al. 1999) have confirmed that it varies C1003p003 | so it is included again and numbered as V5. C1003p003 | V6-12 = Borissova's V1-5 and V9-10 C1003p003 | Borissova et al. (1998) with x,y arcsec positions. C1003p003 | These authors also derived x,y arcsec positions for V2, V4 and C1003p003 | V5 which they listed as No. 155, Pop II Cep. and BS58 respectively. C1003p003 | Three of their candidates, V8-10 in the above table, did not satisfy C1003p003 | all of the variability criteria and are therefore classified as C1003p003 | "CST?". Furthermore V8 and V10 should have been in the field studied C1003p003 | by Stetson et al. (1999), but were not recognized as variables. Thus it C1003p003 | appears to be unlikely that they are variable. C1003p003 | V13-14 = Stetson's 2-368 and 3-269 C1003p003 | Stetson et al. (1999). Their RA and Dec were provided by Stetson C1003p003 | (2011, private communication). C1003p003 | Stetson et al. (1999) announced five other RR Lyrae variables in C1003p003 | Pal 3. They noted that three of them (1-233, 2-614 and 2-198) are C1003p003 | the same as Gratton & Ortolani's (1984) #155, 283 and 188 which are C1003p003 | V2, V3 and V5 in the above table. The RA and dec for the others, C1003p003 | 1-299 and 1-404 (Stetson 2011, private communication) indicate that C1003p003 | they are V1 and V2 of Borissova et al. (1998) which are V6 and V7 C1003p003 | in the above table. # C1015m461 |V1-56 C1015m461 | Woods (1919) with x,y coordinates C1015m461 |V57-61 C1015m461 | Bailey (1922) with x,y coordinates C1015m461 |V62-86 = HV 10328-10352 C1015m461 | Dowse (1940) with x,y coordinates and the corresponding HV numbers C1015m461 |V87 C1015m461 | Wright (1941) with x, y coordinates and a corrected y value for V80 C1015m461 | ID charts for V1-87 were later published by Fourcade et al. (1966). C1015m461 | However, in her 3rd catalogue, Sawyer Hogg (1973) reported that Kukarkin C1015m461 | had informed her that the Fourcade et al. identifications for V6, V11, C1015m461 | V45, V52, V57, V68 and V81 were all erroneous. Later, Samus et al. C1015m461 | (1996) found that V39 and V50 were also erroneously labelled. C1015m461 | Arellano Ferro et al. (2014) published an ID chart for all of the C1015m461 | variables that were in their field. C1015m461 |V88-96 = Nr. 1-9 C1015m461 | Wilkens (1965) with x,y coordinates to a precision of 0.1 arcmin and C1015m461 | finder charts: Nrs. 3, 5 & 10 appear on one chart and the other charts C1015m461 | are individual. C1015m461 | The numbers V88 to 96 were assigned by Sawyer Hogg (1973) who noted C1015m461 | that Wilkens' Nr. 10=V39. Kukarkin (1971a) noted that V94 and 95 C1015m461 | (Wilkens #7 and 8) were not variable. C1015m461 |V97-100 = Lee 1103, 1405, 2403, 2710 C1015m461 | Lee (1977) with ID charts. The numbers V97-100 were assigned in the C1015m461 | electronic update to the Sawyer Hogg catalogs (Clement et al. 2001). C1015m461 | Lee's ID chart also includes many of the other RR Lyrae variables C1015m461 | which are labelled according to his Table 2 numbering system. C1015m461 |V101 = V6 of von Braun & Mateo (2002) with ID chart and RA and dec. C1015m461 | These authors discovered a total of 14 short period variables in C1015m461 | the field of NGC 3201, but their V6 was the only one they C1015m461 | considered to be a cluster member. C1015m461 | The number V101 was assigned in the electronic update to the Sawyer C1015m461 | Hogg catalogs (Clement et al. 2001). C1015m461 | According to Kaluzny et al. (2016), proper motion data confirm that C1015m461 | von Braun & Mateo's V2 and V4 are not couster members. C1015m461 |V102-112 = Mazur V1-11 C1015m461 | Mazur et al. (2003) with RA, dec and finder charts C1015m461 | Their paper lists multiple frequencies for some of the stars and C1015m461 | they pointed out that some of these may be non-radial modes. C1015m461 | For each star, the period listed in the above table is the inverse C1015m461 | of the first frequency listed by Mazur et al. (their Table 3). C1015m461 | Three of these variables (Mazur V7, 8, 9) were independently discovered C1015m461 | by Layden and Sarajedini (2003) and are listed as #651, #1019, #752 C1015m461 | in their Table 8. There are a number of transcription errors in the C1015m461 | L&S paper. Consequently, the stars listed as #651, #1019, #752 in C1015m461 | Table 8 are #652, #1020, #753 in their Table 2. A similar problem has C1015m461 | occurred with their numbering system for some of the RR Lyrae C1015m461 | variables. C1015m461 | Layden (2011 - private communication) has indicated that this problem C1015m461 | might have occurred because they (L&S) published an incorrect version C1015m461 | of Table 2 in their paper. C1015m461 |V113-118 = LS 2, 4, 5, 6, 7, 12 C1015m461 | Layden & Sarajedini (2003) with X,Y pixel numbers C1015m461 | The RA and dec for these stars were derived by Layden (2012- private C1015m461 | communication), based on 2MASS identifications. C1015m461 | Layden also established that the IDs listed for all of the RGB C1015m461 | variables in Table 7 corresponded to the numbers listed in Table 2. C1015m461 | The classifications for V113-V118 in the above table were assigned C1015m461 | after consulation with Samus (2012 - private communication). C1015m461 | Layden & Sarajedini (2003) detected low level brightness variations C1015m461 | in most of the brighter red giants and plotted light curves. (See C1015m461 | their Fig. 7 and Table 7). C1015m461 | For this catalogue, stars #2, 4, 5, 6, 7, 12 have been selected as the C1015m461 | best candidate variables, on the basis of their V amplitudes (A_V>0.02) C1015m461 | and their DAOPHOT variability criteria (Lambda>3). L&S star #3 C1015m461 | (=V79) is also considered to be variable. L&S star #32 is variable, but C1015m461 | L&S considered it to be a field star. With (V-I)= 3.235, it lies C1015m461 | about 2 magnitudes redward of the cluster CMD. They also noted the C1015m461 | possibility that #2 could be a field variable, presumably because of C1015m461 | its red color - but the color is not extreme. C1015m461 |V119-121 = LS 565*, 776, 941 C1015m461 | Layden & Sarajedini (2003) with X,Y pixel numbers C1015m461 | *The star listed as LS#565 in their Table 2 is LS#564 in Table 8. C1015m461 | The RA and dec for these stars were derived by Layden (2012 - private C1015m461 | communication). C1015m461 |V122-124 C1015m461 | Arellano Ferro et al. (2014) with RA, dec and an ID chart C1015m461 | All of the variables, V1-121, that are included in their field are C1015m461 | also labelled on their ID chart. C1015m461 |V125-160 C1015m461 | Kaluzny et al. (2016) with RA, dec and individual finder charts C1015m461 | All of these stars are considered to be cluster memvers based on C1015m461 | proper motion studies. C1015m461 | Kaluzny announced an additional 21 variables which they numbered C1015m461 | VN1-VN21. None of these were confirmed to be cluster members C1015m461 |------------------ C1015m461 |Pietrukowicz et al. (2008) searched for dwarf novae in NGC 3201 and C1015m461 |found none. Their search was based on 751 V exposures obtained on 22 C1015m461 |nights during the years 2001-2005. They also checked at the location of 4 C1015m461 |X-ray sources that were indicated as possible CVs by Webb et al. (2006) C1015m461 |and found no brightness variations. # C1126p292 | V1-2 C1126p292 | Rosino (1957) with x,y positions and ID chart C1126p292 | In 1957, Palomar 4 was called Abell No. 4 C1126p292 | Burbidge & Sandage (1958) also published an ID chart (Figure 3). C1126p292 | V1 is their #44 and V2 is their #25. # C1207p188 | V1-3 C1207p188 | Baade (1930) with x,y positions and ID chart C1207p188 | V4 C1207p188 | Davis (1917) with x,y position C1207p188 | V5-14 C1207p188 | Sandage & Walker (1955) and/or Newburn (1957) with ID charts C1207p188 | for V1-V14 published by Sandage & Walker C1207p188 | V15-17 and non-variable status for V9 C1207p188 | Newburn (1957): V15-17 were labelled as IV-37, I-34 and I-6 by C1207p188 | Sandage & Walker (1955) C1207p188 | V18 a possible foreground (field) RR0 C1207p188 | and non-variable status of V5, 9 and 15 C1207p188 | Arellano Ferro et al. (2004) with ID chart for V18 C1207p188 | V19 and non-variable status of V5, 9, 15 and 18 C1207p188 | Stetson et al. (2005) with RA, Dec and ID chart for V19 # C1223m724 |V1-2 C1223m724 | Fourcade et al. (1966) with x,y coordinates and an ID chart C1223m724 | Both stars are located approximately 12 arcminutes from the cluster C1223m724 | centre, well beyond the half-light radius (~4 arcminutes), but inside C1223m724 | the tidal radius of~35 arcminutes according to the 2010 update of the C1223m724 | Harris (1996) catalogue. C1223m724 |V3-22 C1223m724 | Kaluzny & Krzeminski (1993) with RA, dec and ID charts C1223m724 | These authors identified 36 candidate variable stars which they C1223m724 | numbered V1-36. However, only 20 of these proved to be clearly C1223m724 | variable and they did not publish any information about the other 16. C1223m724 | The 20 "clear" variables were assigned the numbers V3-22 by Clement C1223m724 | et al. (2001) in their electronic catalogue. This numbering system C1223m724 | was also adopted by Samus et al. (2009). C1223m724 | The KK (Kaluzny & Krzeminski 1993) numbers are indicated beside our C1223m724 | assigned numbers in the ID column in the above table. C1223m724 |-------------------------------------------------------------------------- C1223m724 |Kaluzny & Krzeminski (1993) also noted the presence of two faint, blue C1223m724 |stars (b1 and b2) that could be hot subdwarfs. Their RA and dec were C1223m724 |listed in Table 2 of their paper. C1223m724 |--------------------------------------------------------------------- C1223m724 |Geraschenko et al. (1997) listed 4 possible RR Lyrae variables, based C1223m724 |on their location near the instabiity strip in the CMD. They published C1223m724 |an ID chart and derived x,y positions using the coordinate system of C1223m724 |Kaluzny & Krzeminski (1993) as a reference frame. C1223m724 |-------------------------------------------------------------------- C1223m724 |Pietrukowicz et al. (2008) searched for dwarf novae in NGC 4372, but C1223m724 |none were detected. Their search was carried out on images obtained on C1223m724 |14 nights in 2004 and 5 in 2005. C1223m724 |------------------------------------------------------------------- C1223m724 |Servillat et al. (2008) detected X-ray 10 sources, for which they listed C1223m724 |RA and dec, from XMM-Newton observations, none inside the half-mass C1223m724 |radius. However, the limiting luminosity of their observations was not C1223m724 |constraining for a possible population of faint CVs. # C1235m509 | V1-18 C1235m509 | Kaluzny et al. (1995) with RA, dec and X,Y pixel coordinates # C1236m264 |V1-19 C1236m264 | Shapley (1919) with x,y coordinates C1236m264 |V20-28 C1236m264 | Shapley (1920) with x,y coordinates and an ID chart for V1-28 C1236m264 | He also listed their photographic magnitudes from 10 plates and these C1236m264 | were used by Sawyer (1939) to derive max and min magnitudes for her C1236m264 | first catalogue of variable stars in globular clusters. C1236m264 |V29-31 C1236m264 | Rosino & Pietra (1954a,b) with x,y coordinates C1236m264 |V32-38 C1236m264 | van Agt & Oosterhoff (1959) with x,y coordinates and ID charts for C1236m264 | V1-38 C1236m264 | V32 was previously announced as HV 11069 with RA and dec (1900) by C1236m264 | Buttery (1942). It has subsequently been desginated as EN Hya in the C1236m264 | GCVS. C1236m264 |V39-42 C1236m264 | Terzan et al. (1973) with x,y coordinates and an ID chart C1236m264 | They also announced five new variables in the field around the C1236m264 | cluster. C1236m264 |V43-48 C1236m264 | Walker (1994) with ID chart for all the variables in his C1236m264 | investigation. For the variables that were not RR Lyrae, he also C1236m264 | published X,Y coordinates in pixels. C1236m264 |V49-52 C1236m264 | Kains et al. (2015) with RA, dec and an ID chart for all of the C1236m264 | variables as well as individual finder charts. C1236m264 |V53 = Standard #28 of Walker (1994) who noted that the star was ~0.1 mag C1236m264 | fainter in May 1993 than it was in March and July. He published an C1236m264 | ID chart and concluded that it was a red foreground star. C1236m264 | The number V53 was assigned by Kains et al. (2015) who listed the C1236m264 | star's RA and dec. and published an ID chart. C1236m264 | C1236m264 |---------------------------------------------------------------- C1236m264 |Sariya et al. (2014) announced 9 possible new variables for which they C1236m264 |derived periods ranging from 0.26 to 0.54 days. However, in a C1236m264 |subsequent study, Kains et al. (2015) observed these stars and did C1236m264 |not detect variability in any of them. Therefore they have not been C1236m264 |included in the above table. # C1256m706 |V1-2 C1256m706 | discovered by Bailey with RA and dec (epoch 1900) and Harvard variable C1256m706 | numbers; announced by Shapley (1923). C1256m706 | Their x,y positions were later published by Wright (1941). C1256m706 | The numbers V1 and V2 were assigned by Sawyer (1955) in her 2nd C1256m706 | catalogue. She also noted that these stars were RY Mus and RZ Mus C1256m706 | respectively. C1256m706 |V3-11 C1256m706 | discovered by various investigators at Harvard and announced by C1256m706 | Wright (1941) with x,y coordinates and Harvard variable numbers. C1256m706 | The numbers V3-11 were assigned by Sawyer (1955) C1256m706 |V12-16 C1256m706 | Fourcade et al. (1966) with x,y coordinates and an ID chart C1256m706 |V17-24 = B57,B84,B105,B121,B193,C80,C308,D199 on charts published by C1256m706 | Menzies (1972) who classified them as possible variables. C1256m706 | The numbers V17-24 were assigned by Demers & Wehlau (1977) who C1256m706 | published an ID chart for all of V1-24 except V11 (FQ Mus) which C1256m706 | was outside of their field of view. C1256m706 |V25-34 = NV1-10 C1256m706 | Darragh & Murphy (2012) with RA and dec C1256m706 | The numbers V25-34 have been assigned in this catalogue. # C1310p184 |V1-23 C1310p184 | Shapley (1920) with x,y coordinates and an ID chart C1310p184 | C1310p184 |V24-40 C1310p184 | Baade (1931) with x,y coordinates C1310p184 |V41-42 C1310p184 | Grosse (1932) with an ID chart. C1310p184 | Variables 1-40 were also identified on the chart. C1310p184 | In a later paper, Grosse (1933) discovered 7 additional variables in C1310p184 | the field around M53 and published their 1900 RA and dec. C1310p184 |V43-46 C1310p184 | van den Hoven van Genderen (1947) with x,y coordinates and an ID chart. C1310p184 | She also published x,y coordinates for V41 and V42 C1310p184 | and included them on the ID chart. C1310p184 |V47 C1310p184 | Margoni (1964) with x,y coordinates and an ID chart C1310p184 |V48-50 = Cuffey's V47-V49 = stars 4-7-8, 4-4-16 and K C1310p184 | Cuffey (1965) wth an ID chart. C1310p184 | The numbers V48-V50 were assigned by Sawyer Hogg (1973) in C1310p184 | her 3rd catalog because data for a new V47 had been published C1310p184 | previously by Margoni (1964). C1310p184 | Sawyer Hogg derived x,y coordinates for Cuffey's new variables, but C1310p184 | Kopacki (2000) discovered that they were incorrect and that the RA and C1310p184 | dec computed by Evstigneeva et al. (1997) were based on these C1310p184 | incorrect values. C1310p184 | Samus et al. (2009) computed the correct RA and dec for these three C1310p184 | stars. They all correspond to 2MASS positions. C1310p184 | C1310p184 |V51-60 = Kravtsov's V1-5,7-11 C1310p184 | Kravtsov (1990) with x,y coordinates and an ID chart. C1310p184 | The numbers V51-60 were assigned by Kopacki (2000) C1310p184 | Kopacki did not assign a new number for Kravtsov's V6 because C1310p184 | it was the same star as V44. C1310p184 |V61-70 C1310p184 | Kopacki (2000) with x,y coordinates and an ID chart. C1310p184 |V71-72 C1310p184 | Dekany & Kovacs (2009) with RA & dec C1310p184 | Arellano Ferro et al. (2011) found small errors in the coordinates C1310p184 | for both of these stars and provided ID charts and revised C1310p184 | coordinates. C1310p184 |V73-76 = SXP1, SXP2, SXP6, SXP7 C1310p184 | Jeon et al. (2002, 2003) with RA, dec and an ID chart in the 2003 C1310p184 | paper. The numbers V73-76 were assigned by Dekany & Kovacs (2009). C1310p184 |V77-86 C1310p184 | Dekany & Kovacs (2009) with RA & dec C1310p184 | Arellano Ferro et al. (2011) found a small errors in the coordinates C1310p184 | of V80 and provided an ID chart and revised coordinates. Also, the C1310p184 | variability of V81, V82 and V83 was not confirmed in the Arellano C1310p184 | Ferro et al. study. C1310p184 |V87-90 = SXP3, SXP4, SXP5, SXP8 C1310p184 | Jeon et al. (2002, 2003) with RA, dec and an ID chart in the 2003 C1310p184 | paper. The numbers V87-90 were assigned in the September 2009 C1310p184 | update to the CVSGC electronic catalog. C1310p184 | These stars were not studied by Dekany & Kovacs (2009) because V87 C1310p184 | was not resolved on their frames and the amplitudes of V88-90 were C1310p184 | too low to be identified in their data. C1310p184 |V91-105 C1310p184 | Arellano Ferro et al. (2011) with RA, dec and ID charts C1310p184 | They also listed 5 suspected variables, S1-5, that were blue C1310p184 | stragglers. C1310p184 |V106-108 = SX4, SX16, SX21 C1310p184 | Safanova & Stalin (2011) with RA, dec and ID chart C1310p184 | The numbers V106-108 were assigned by Bramich et al. (2012) who C1310p184 | confirmed their variability. C1310p184 | Some of the other SXPHE candidates announced by Safanova & Stalin C1310p184 | were independently discovered by Arellano Ferro et al. (2011) or were C1310p184 | known from previous studies. C1310p184 |V109 C1310p184 | Bramich et al. (2012) with RA, dec and an ID chart C1310p184 | V109 was announced as VC10, a candidate variable, with variations on C1310p184 | a time scale of a few hours, by Safanova & Stalin (2011). Bramich et C1310p184 | al. (2012) did not confirm the short term variability of VC10, but in C1310p184 | the course of their analysis discovered that it was a semi-regular C1310p184 | variable near the red giant tip. C1310p184 |---------------------------------------------------------------------- C1310p184 |The 2011 paper by Safanova & Stalin (2011) was based on R band observations C1310p184 |of M53 made over an interval of 7.2 hours on March 24, 2010. They recovered C1310p184 |most of the known variables and announced many new candidates. However, C1310p184 |their data were not extensive enough to confirm the variability of most C1310p184 |of the new candidates. An independent analysis of these stars was C1310p184 |carried out by Bramich et al. (2012) who found most to be non-variable, C1310p184 |with the exception of V106-V109 listed above. Also, Bramich et al. C1310p184 |tentatively confirmed the variability of S&S candidates W11 and SX12, but C1310p184 |commented that follow-up observations of better precision would be required C1310p184 |to establish their variable nature. # C1313p179 |V1-9: C1313p179 | Baade (1928) with x,y coordinates and an ID chart C1313p179 |V10: C1313p179 | Sawyer (1946) with x,y coordinates. C1313p179 | An ID chart for V1-V10 was later published by Rosino (1949) and also C1313p179 | by Sandage et al. (1977) C1313p179 | C1313p179 |V11-14 (= Blue stragglers # 7, 11, 13, 14) C1313p179 | Nemec & Cohen (1989) - see footnote on page 796 - C1313p179 | with X,Y pixel positions (Table 6) and finding charts C1313p179 | (Figure 1a for #7, 11, 13 and 1c for #14). C1313p179 | In their study of these variables, Nemec et al (1995) referred to C1313p179 | them as NC7, NC11, NC13, NC14. C1313p179 | The numbers V11-14 were assigned in our electronic catalogue in 2001. C1313p179 |V15 (= NC15) C1313p179 | Nemec et al. (1995) C1313p179 | This star is blue straggler #15 of Nemec & Cohen (1989) who published C1313p179 | its X,Y pixel position (see Table 6) and ID chart (see Figure 1c) C1313p179 | The number V15 was assigned in our electronic catalogue in 2001. C1313p179 |------------------------- C1313p179 |Probable variable stars C1313p179 |Blue stragglers: BS4, BS5, BS19, BS25, BS28, BS29, BS30 C1313p179 | are all candidate SX Phe variables according to Arellano Ferro et C1313p179 | al. (2010) - see their discussion of blue stragglers in section 5.3, C1313p179 | search for new variables in section 6 and ID chart in Figure 15. C1313p179 |RGB star: NV1 C1313p179 | Arellano Ferro et al. (2010) with ID chart in Figure 15, light curve C1313p179 | in Figure 12 and discussion in section 6.3 C1313p179 | C1313p179 |----------------------- C1313p179 |Suspected variable stars C1313p179 |Blue stragglers: BS22, BS23, BS31 C1313p179 | Arellano Ferro et al. (2010) - see section 6.1.2 # C1323m472 |V1-132 C1323m472 | Bailey (1902) with an ID chart (Plate I, Frontispiece) and x,y C1323m472 | coordinates (Table VI, pages 133-135). C1323m472 | By the time he published his paper, he considered V28, 31, 37 and 93 C1323m472 | to be non-variable (see page 14) and this conclusion was later C1323m472 | confirmed by Martin (1938) and by Kaluzny et al. (2004). C1323m472 |V133-165 C1323m472 | discovered by van Gent and Hertzsprung and announced by C1323m472 | Martin (1938) with x,y coordinates (bottom of page 20, Table 5 on C1323m472 | pages 22-27 or Table 6 on page 35) and ID charts (Plates I and II). C1323m472 | V133 and V159 were outside the field of his ID charts and were later C1323m472 | identified on ID charts by van Gent (1948). C1323m472 | All of Bailey's variables (except V80) are labelled on Martin's charts. C1323m472 |V166-167 C1323m472 | Martin (1938) with ID charts (Plates I and II) and x,y coordinates C1323m472 | (bottom of page 20). Martin assigned these numbers to his comparison C1323m472 | stars 89b and p3, (see page 16 and 18 of his paper) C1323m472 |V168 C1323m472 | Kooreman (1942) with x,y coordinates C1323m472 |V169 C1323m472 | Belserene (1956) with x,y coordinates C1323m472 |V170 = star G of Belserene (1959) who published x,y coordinates C1323m472 | Eggen (1961a,b) detected its variability. The number V170 C1323m472 | was assigned by Sawyer Hogg (1973) who also identified it as C1323m472 | RGO #53 (Woolley 1966). Woolley established that it is a cluster C1323m472 | member. However, it was not included in the studies of red variables C1323m472 | in Omega Cen by Dickens et al. (1972). C1323m472 |V171-180 = V1-10 of Wilkens (1965) who published ID charts and C1323m472 | x,y, coordinates. C1323m472 | The numbers V171-180 were assigned by Sawyer Hogg (1973). C1323m472 | Wilkens (1965) listed 5 additional variables, V11-15, but according C1323m472 | to Sawyer Hogg (1973), he later indicated (Letter, 1972) that these C1323m472 | were suspected variables. C1323m472 |V181-183 C1323m472 | Wesselink (1969,1972 in private correspondence with Sawyer Hogg) C1323m472 | The numbers V181-183 were assigned by Sawyer Hogg (1973) who also C1323m472 | published Wsselink's x,y coordinates and periods. C1323m472 |V184-185 C1323m472 | Butler et al. (1978) with no ID C1323m472 | By matching periods and approximate distance from the cluster centre, C1323m472 | Clement & Rowe (2000) determined that V184=Ogle #191 and V185=Ogle #71 C1323m472 | from the investigation of Kaluzny et al. (1997b). Kaluzny et al. C1323m472 | published RA, dec and X,Y pixel positions. C1323m472 |V186 =V184 of Fourcade et al. (1978) with ID chart and x,y coordinates C1323m472 | The number V186 was assigned in our electronic catalogue (Clement et C1323m472 | al. 2001) because Butler et al. (1978) had assigned the number 184 C1323m472 | to a different star. Fourcade's variable is the same star as RG 320 C1323m472 | that was discussed by Dickens et al. (1972) and confirmed as a cluster C1323m472 | member by Feast (1973 - page 138). C1323m472 |V187-193 = eclipsing binary candidates NJL #221, 216, 58, 1, 218, 5, 212 C1323m472 | of Niss et al. (1978) who published x,y coordinates and an ID chart. C1323m472 | The numbers 187-193 were assigned in our electronic catalogue C1323m472 | (Clement et al. 2001). C1323m472 | Niss et al. stated that NJL#5 was almost certainly eclipsing and that C1323m472 | the other six were reasonably certain variables. A subsequent study C1323m472 | by Kaluzny et al. (1996) confirmed the variability of NJL #5 (=Ogle #18), C1323m472 | but did not list the other six as variables. In a later paper, C1323m472 | Kaluzny et al. (2004) announced that none of the other six were variable. C1323m472 | Margon & Cannon (1989) measured the radial velocity of NJL#5 and C1323m472 | established its cluster membership. C1323m472 |V194 = candidate variable NJL #220 of Niss et al. (1978) who published C1323m472 | x,y coordinates and an ID chart. Its variability was later confirmed C1323m472 | by Niss (1981). The number 194 was assigned in our electronic C1323m472 | catalogue (Clement et al. 2001). C1323m472 |V195 = star NJL #79 of Niss et al. (1978) who published x,y coordinates C1323m472 | and an ID chart. C1323m472 | Jorgensen (1982) detected its variability and the number V195 C1323m472 | was assigned in our electronic catalogue (Clement et al. 2001). C1323m472 |V196 = E39 of Jorgensen & Hansen (1984) with ID chart C1323m472 | The number V196 was assigned in our electronic catalogue (Clement et C1323m472 | al. 2001). C1323m472 |V197-233 = Ogle #1-4, 6-17, 19-22, 24-40 of Kaluzny et al. (1996) with C1323m472 | RA and dec and X,Y pixel positions C1323m472 | The numbers V197-233 were assigned in our electronic catalogue C1323m472 | (Clement 2001). C1323m472 |V234-260 = Ogle #41, 43-49, 51, 53-70 of Kaluzny et al. (1997a) with C1323m472 | RA and dec and X,Y pixel positions C1323m472 | The numbers V234-260 were assigned in our electronic catalogue C1323m472 | (Clement 2001). C1323m472 |V261-291 = Ogle #81, 95-96, 108, 111, 115, 121-123, 131-132, 134, 139, C1323m472 | 148-149, 152, 155-156, 161-162, 167, 171-173, 177, 186, 196, 202-203, C1323m472 | 208-209 of Kaluzny et al. (1997b) with RA and dec and X,Y pixel C1323m472 | positions C1323m472 | The numbers V261-291 were assigned in our electronic catalogue C1323m472 | (Clement 2001). C1323m472 |V292-293 = #50259 and #55071 C1323m472 | van Leeuwen et al. (2000) with RA and dec C1323m472 | The numbers V292-293 were assigned in the 2002 update to the Clement C1323m472 | (2001) on-line catalog and were adopted by Kaluzny et al. (2004) when C1323m472 | they published their catalog. C1323m472 | van Leeuwen et al. listed two other candidate red variables that were C1323m472 | cluster members: C1323m472 | #37110 (RA 13:26:34.12, dec -47:26:21.1) C1323m472 | #39105 (RA 13:26:25.00, dec -47:27:06.3) which is star #201 in C1323m472 | Woolley's (1966) study. C1323m472 | C1323m472 |V294-410 = NV294-410 with RA, dec and individual finder charts C1323m472 | Kaluzny et al. (2004) C1323m472 |V411 = V133 of Weldrake et al. (2007) who published RA and dec C1323m472 | They stated that this star was the same as V144 of Kaluzny et C1323m472 | al. (2004), but Navarrete et al. (2013) showed that Weldrake's #133 C1323m472 | was a different star, not previously known to be variable. They C1323m472 | assigned the number V411 and published an ID chart for both V144 C1323m472 | and V411. C1323m472 |V412-450 C1323m472 | Weldrake et al. (2007) with RA and dec C1323m472 | They introduced their own numbering system which was different from C1323m472 | the one that is generally used for Omega Cen, i.e. the system C1323m472 | started by Bailey (1902) and continued by Martin (1938) and C1323m472 | subsequent investigators. The Weldrake (W) numbers are indicated in C1323m472 | the ID column of the above table. C1323m472 | Weldrake et al. announced 81 new variables, but only 43 are C1323m472 | included here. Variables for which they derived an amplitude less C1323m472 | than 0.05 mag (W1, W4, W15, W58, W68, W69, W86, W93, W98, W125, C1323m472 | W126, W130, W132, W187) have been excluded. In addition, variables C1323m472 | which appear to be field stars based on their location in the CM C1323m472 | diagram (e.g. W5, W6, etc.) and variables with 0% probability of C1323m472 | membership (W31, W59), based on the proper motion study of Bellini C1323m472 | et al. (2009) are also excluded. Future investigations might show C1323m472 | that some of these stars are variables that belong to Omega Centauri. C1323m472 |V451-454 = Randall's V1-4 with RA and dec C1323m472 | Randall et al. (2011) published the coordinates and summarized C1323m472 | the properties of these rapidly pulsating extreme horizontal branch C1323m472 | (EHB) stars. Three of them had been announced in earlier papers by C1323m472 | Randall and collaborators. C1323m472 | Finding charts were later published by Randall et al. (2016). C1323m472 | A fifth candidate was announced by Randall et al. (2013), but no C1323m472 | position was published. C1323m472 |V455-456 = NV455 and NV 456 of Naverrete et al. (2015) who published C1323m472 | finder charts and RA and dec (epoch 2000). C1323m472 | They also announced two other new RR Lyrae variables, NV457 and C1323m472 | NV458, but their locations on the CM diagram indicate that they are C1323m472 | too faint to be cluster members. C1323m472 |V457-459 C1323m472 | Figuera Jaimes et al. (2016) with RA, dec and a finder chart C1323m472 |V460 = Randall's V5 (another EHB star) with finding chart and RA and dec C1323m472 | Randall et al. (2016) C1323m472 | Randall et al. (2016) also detected an EHB variable with an apparent C1323m472 | periodicity of approximately 0.03 days and speculated on possible C1323m472 | explanations for its observed luminosity variation. C1323m472 |--------------------------------------------------------------------- C1323m472 |In a search for tidal tails around Omega Centarui, Fernandez-Trincado C1323m472 |et al. (2015) have discussed the properties of 48 RR Lyrae variables in C1323m472 |an area 50 square degrees around the cluster. Of these, 37 are new C1323m472 |discoveries, but all of them are outside the tidal radius of the C1323m472 |cluster. C1323m472 |--------------------------------------------------------------------- C1323m472 |Cool et al. (2013) reported optical counterparts for approximately C1323m472 |40 Chandra X-ray sources that are probably associated with the cluster. C1323m472 |These include 27 candidates, 3 BY Drcaonis stars, 1 qLMXB and 7 possible C1323m472 |magnetically active binaries. # C1339p286 | V1-137 and star b C1339p286 | Bailey (1902) with ID chart (Fig 1) and x,y coordinates C1339p286 | (pages 238-239) C1339p286 | Bailey (1913) with ID chart (Fig 1) and von Zeipel numbers C1339p286 | (page 10) C1339p286 | V138 = Bailey's star b (see Bailey 1913, pages 8-9) C1339p286 | The number 138 was assigned by Larink (1922) C1339p286 | V139-141 C1339p286 | Larink (1922) with x,y positions; V141 is RV CVn. C1339p286 | The variability of V141 was previously announced by C1339p286 | Larink (1921), but it was identified only by RA and dec in the C1339p286 | earlier paper. C1339p286 | V142-183 C1339p286 | Muller (1933) with x,y coordinates C1339p286 | V184-199 C1339p286 | Greenstein (1935) with x,y coordinates C1339p286 | V200-201 = star numbers 12 and 14 from Table I of C1339p286 | Shapley (1914). The numbers V200 and 201 were assigned by Sawyer C1339p286 | (1939) in her 1st catalog. She also derived their x,y coordinates C1339p286 | on the system of Bailey. C1339p286 | V202 = von Zeipel #190 C1339p286 | Schwarzschild (1940) announced that this star was variable and C1339p286 | Sawyer (1955) designated it as V202 in her 2nd catalog C1339p286 | V203-204 = star C and star I-I-42 in the ID chart C1339p286 | of Sandage (1953) C1339p286 | Roberts & Sandage (1955) announced the variability of these C1339p286 | two stars and Sawyer (1955) designated them as V203 and 204 in her C1339p286 | 2nd catalog. She also listed their von Zeipel numbers and derived x,y C1339p286 | coordinates. She incorrectly listed V204 as vZ 390, instead C1339p286 | of 1390. As a result, the x,y coordinates she listed for C1339p286 | V204 were incorrect. Bakos et al. (2000) listed the correct C1339p286 | position for this star. C1339p286 | V205-206 = SVS (Soviet Variable Star) 1264 and 1276 C1339p286 | Kurochkin (1959, 1960) C1339p286 | These studies announced new variable stars in the vicinity of C1339p286 | M3; SVS 1264 and 1276 were the only ones inside the tidal radius. C1339p286 | Kukarkin (1960) later identified them as von Zeipel 89 and 1221 C1339p286 | respectively and Sawyer Hogg (1973) designated them as V205 and C1339p286 | 206 in her 3rd catalog. C1339p286 | V207-224 = X3, X4, X6 X8, X9, X11, X12, X15, X16, X19, X27, C1339p286 | X28, X29, X31, X32, X34, X37, X38 C1339p286 | Kholopov (1963) with x,y coordinates, ID chart and von Zeipel C1339p286 | numbers if available. The numbers V207-224 were assigned by C1339p286 | Sawyer Hogg (1973) in her 3rd catalog. C1339p286 | V225 = von Zeipel 837 C1339p286 | Russev (1971) with von Zeipel number. C1339p286 | He also indicated that vZ 238 was variable. C1339p286 | Sawyer Hogg (1973) designated vZ 837 as V225 in her 3rd C1339p286 | catalog, but she did not include vZ 238 which had a smaller C1339p286 | amplitude. C1339p286 | V226 = SVS 2041 C1339p286 | Kholopov (1974) with x,y coordinates and ID chart C1339p286 | In a later paper, Kholopov (1977) listed it as X39. C1339p286 | We designated this as V226 in our first on-line update to the C1339p286 | catalog. C1339p286 | V227-235 = X7, X10, X40, X41, X42, X43, X44, X47, X49 C1339p286 | Kholopov (1977) with ID chart (for all except X41), C1339p286 | x,y coordinates, von Zeipel and/or SVS number. C1339p286 | These were designated as V227-235 in the first on-line update to the C1339p286 | Sawyer Hogg catalog. C1339p286 | V236 = von Zeipel 1397 C1339p286 | This star (vZ 1397) is among the brightest stars on the giant C1339p286 | branch and Walker (1955) suggested that it might be variable. C1339p286 | Olah (1973) confirmed the variation. C1339p286 | vZ 1397 was designated as V236 in the first on-line update to the C1339p286 | Sawyer Hogg catalog. C1339p286 | V237-238 C1339p286 | Kaluzny et al. (1998) with x,y coordinates and ID charts. C1339p286 | According to Hartman et al. (2005), the coordinates C1339p286 | of V237 and V238 were switched in the discovery paper and this C1339p286 | error propagated through to the compilation by Bakos (2000). The C1339p286 | coordinates listed for these two stars in the above table have C1339p286 | been revised accordingly. C1339p286 | V239-248 = X13, X14, X17, X20, X22, X23, X25, X30, X35, X36 C1339p286 | Kholopov (1963) with x,y coordinates, ID chart and von Zeipel C1339p286 | numbers if available. C1339p286 | The numbers V239-248 were assigned by Bakos et al. (2000). C1339p286 | Sawyer Hogg (1973) was aware of Kholopov's paper because it C1339p286 | was the discovery paper for her V207-224, but apparently she C1339p286 | did not consider these other stars to be variables. C1339p286 | V249-259 = KG1, KG2, KG3, KG4, KG7, KG8, KG9, KG11, KG12, C1339p286 | KG14, KG15 C1339p286 | Kadla & Gerashchenko (1980) listed 17 suspected variable stars, C1339p286 | 1 to 17 with x,y coordinates (on a different system from Bailey), C1339p286 | Delta B and von Zeipel number if available. C1339p286 | In a later paper (Kadla & Gerashchenko 1982), they listed only C1339p286 | KG 1-15 as new variables and published ID charts for these stars as C1339p286 | well as for V1-225 and Kholopov's (1963, 1977) variables. Eleven of C1339p286 | these KG stars were designated as V249-259 by Bakos et al. (2000). C1339p286 | Bakos et al. did not consider KG5, KG6 or KG13 to be variable and C1339p286 | they concluded that KG10 was the same star as V194. C1339p286 | V260 = von Zeipel 297 C1339p286 | 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). C1339p286 | vZ 297 was later designated as V260 by Bakos et al. (2000). C1339p286 | V261-268 = Gu32, Gu552, Gu576, Gu586, Gu1489, Gu9012, C1339p286 | Gu9016, Gu9025 C1339p286 | Guhathakurta et al. (1994). These stars were C1339p286 | designated as V261-268 by Bakos et al. (2000) C1339p286 | V269-274 = B1-6 C1339p286 | Bakos et al. (2000) C1339p286 | S1-S11: C1339p286 | Strader et al. (2002) C1339p286 | However, Benko et al. (2006) were unable to confirm these discoveries. C1339p286 | V286-297 = New Variables 286-297 C1339p286 | Hartman et al. (2005) C1339p286 | The gap in the numbering system between V274 and V286 occurs C1339p286 | because of the 11 Strader et al. suspected variables which C1339p286 | were not considered by Benko et al. to be variable. C1339p286 | V298 = N2 C1339p286 | Benko et al. (2006) C1339p286 | These authors also made independent discoveries of C1339p286 | V291 (their N1) and V292 (their N3) # C1343m511 |V1-8 C1343m511 | Fourcade et al. (1966) with x,y coordinates and an ID chart C1343m511 | V1 was previously announced as HV 4794 by Hoffleit (1930) C1343m511 |V9-14 C1343m511 | announced by Fourcade et al. (1975, 1978) C1343m511 | The x,y coordinates and ID charts were published by Liller & Lichten C1343m511 | (1978) based on a preprint of the Fourcade et al. (1978) paper. C1343m511 |V15-16 C1343m511 | Liller & Lichten (1978) with x,y coordinates and ID charts C1343m511 |V17-24 = suspected RR Lyrae variables V1-8 C1343m511 | Gerashchenko et al. (1997) with x,y coordinates and an ID chart C1343m511 | The selection was based on the stars' location in the CM diagram. C1343m511 | The numbers V17-24 were assigned by Clement et al. (2001). C1343m511 | C1343m511 | There is some confusion about the numbering of these stars because C1343m511 | the coordinates Gerashchenko et al. listed in their Table 1 for C1343m511 | #4, #5 and #6 did not match the positions labelled on their Figure 2 C1343m511 | ID chart. In fact, #6 was not labelled on their chart, but two C1343m511 | stars were labelled as #5. A correction to the Gerashchenko et al. C1343m511 | paper was later reported by one of the authors, Malakhova and was C1343m511 | appended as a "Corrigenda" to the original paper on the NASA ADS C1343m511 | website. C1343m511 | In the above table, V20 is the star labelled as #4 on the chart of C1343m511 | Gerashchenko et al. and V21 is the more southern of the two stars C1343m511 | labelled as #5. The other #5 is listed as V22. C1343m511 | In a separate paper (Kadla et al. 1998), the same authors announced C1343m511 | x,y coordinates for 12 suspected RR Lyrae variables, 7 of which had C1343m511 | been listed in the 1997 study, but in the 1998 paper, they assigned C1343m511 | different numbers and did not cite their 1997 paper. C1343m511 | It is worth noting however, that Kadla (1998) #11 & #8 = V30 & V33 = C1343m511 | Zorotovic NV6 & NV9. C1343m511 |V25-62 = NV1-38 C1343m511 | Zorotovic et al. (2010) with RA, dec and ID charts C1343m511 | The numbers V25-62 have been assigned in this catalogue. C1343m511 |V63-73 C1343m511 | Figuera Jaimes et al. (2016) with RA, dec and an ID chart # C1403p287 |V1-14 C1403p287 | Baade (1926a) with x,y coordinates and an ID chart for V2-14. C1403p287 | Baade (1926b) also announced 5 variables in the field around the C1403p287 | cluster and listed RA and dec (epoch 1925) for them. C1403p287 |V15-18 C1403p287 | Sawyer (1945) with x,y coordinates, an ID chart and Hopmann (1927) C1403p287 | catalogue numbers for V2-18 C1403p287 |V19 = Star L C1403p287 | Cuffey (1961) with an ID chart. He proposed that it be designated C1403p287 | as V19 and Sawyer Hogg (1973) adopted this number in her 3rd catalog. C1403p287 | This star was independently announced as SVS 1295 by Kurochkin C1403p287 | (1961) who listed its 1900 RA and dec. It was subsequently included in C1403p287 | the Moscow GCVS as BL Boo. C1403p287 | It was also announced by Gryzunova (1969, 1972) who listed its x,y C1403p287 | coordinates and designated it by its Hopmann number: 216. C1403p287 | Zinn & Dahn (1976) gave a good discussion of the discovery of V19. They C1403p287 | also showed that it is an anomalous Cepheid and a cluster member. C1403p287 |V20-21 = Star 2-3-17 and 4-1-11 (both on the HB) C1403p287 | Cuffey (1961) with ID chart. Sawyer Hogg derived their x,y C1403p287 | coordinates for her 3rd (1973) catalog. C1403p287 | Cuffey also found his star 3-5-2 to be variable and recommended that C1403p287 | it be designated as V22. However, this star's position in the CM C1403p287 | diagram (faint and red) is not consistent with cluster membership and C1403p287 | it was therefore not included by Sawyer Hogg in her catalog. It was C1403p287 | not detected as a variable in the subsequent studies by Buonanno et C1403p287 | al. (1984) and Corwin et al. (1999). C1403p287 |V22 = Hopmann 35 C1403p287 | Gryzunova (1969, 1972) with Hopmann number and x,y coordinates. C1403p287 | These coordinates were derived from Hopmann's (1922) x,y coordinates C1403p287 | using corrections (Delta x = 21.8" and Delta y = 26.7") that he derived C1403p287 | in a later paper (Hopmann 1927). The number V22 was assigned by Sawyer C1403p287 | Hogg in her 3rd (1973) catalog. Corwin et al. (1999) could not locate C1403p287 | a variable at the x,y coordinates reported by Gryzunova and Sawyer Hogg C1403p287 | and V22 is now considered to be non-variable. See note above. C1403p287 |V23 = Hopmann 235 = Cuffey 3-5-1 C1403p287 | Gryzunova (1969, 1972) with Hopmann number and x,y coordinates. The C1403p287 | number V23 was assigned by Sawyer Hogg in her 3rd (1973) catalog. C1403p287 | Buonanno et al. (1984) detected variations in Cuffey's star 3-5-1 C1403p287 | and derived x,y coordinates which were in good agreement with the C1403p287 | ones derived by Gryzunova (1969) for Hopmann 235 (V23). C1403p287 | Corwin et al. (1999) pointed out that they were the same star. C1403p287 |V24-27 = Cuffey 2-3 17, 4-1-11, 4-1-22 and Buonanno PV C1403p287 | Buonanno et al. (1984) with x,y coordinates and an ID chart. We C1403p287 | assigned the numbers V24-V27 in our first on-line catalogue in 1998 C1403p287 | without realizing that the stars that Sawyer Hogg (1973) listed as V20 C1403p287 | and V21 in her 3rd catalog were Cuffey 2-3-17 and 4-1-11 respectively. C1403p287 | Thus V24=V20 and V25=V21. Corwin et al. (1999) subsequently found C1403p287 | that V26 and V27 were not variable. (See above in the "Notes on C1403p287 | individual stars" section.) C1403p287 | Buonanno et al. also noted that Cuffey's (1961) stars 3-4-20 and C1403p287 | 3-4-21 might be variable but Corwin et al. (1999) did not detect any C1403p287 | variability. C1403p287 |V28-30 = blue stragglers NH19, NH30, NH31 C1403p287 | Mateo et al. (1990) C1403p287 | The NH numbers were labelled on a print published by Nemec & Harris (1987) C1403p287 |V31-36 = blue stragglers NH29, NH49, NH35, NH27, NH39, NH38 identified C1403p287 | on a print published by Nemec & Harris (1987) C1403p287 | These stars were announced as variables by Nemec & Mateo (1990) and the C1403p287 | numbers V31-V36 were assigned in our electronic editions of the GC C1403p287 | variable star catalog, beginning in 1997. C1403p287 |V37-38 C1403p287 | Arellano Ferro et al. (2008) with an ID chart C1403p287 |V39-41 = SXP 1, 2 and 3 C1403p287 | Jeon et al. (2004) with RA & Dec and and an ID chart. C1403p287 | The numbers V39-41 have been assigned in this catalogue. C1403p287 | Jeon et al. also included V31-36 in their study, using the NH C1403p287 | numbering system assigned by Nemec & Harris (1987). C1403p287 |--------------------------- C1403p287 |The 5 variables that Baade (1926b) discovered in the field around the C1403p287 |cluster were subsequently studied by Kukarkin (1959) who published ID C1403p287 |charts and by Gryzunova (1972) who derived periods. C1403p287 |These 5 variables are listed in the Moscow GCVS as UW CVn, UV CVn, C1403p287 |BI Boo, BN Boo and UU CVn respectively. C1403p287 |Kukarkin (1959) commented that Baade F#3 (BI Boo) and Baade F#4 (BN Boo) C1403p287 |are both possible cluster members. Kholopov (1962) noted that Baade C1403p287 |F#5 (UU CVn) might also be a cluster member. F#3, F#4 and F#5 are all C1403p287 |RR0 variables with periods of 0.5762165, 0.5196619 and 0.5409589 C1403p287 |respectively. C1403p287 |Kurochkin (1961) announced two variables in the corona of NGC 5466: C1403p287 |SVS 1294 and 1295 which are listed in the GCVS as BK Boo and BL Boo C1403p287 |respectively. BL Boo is the anomalous Cepheid, V19 and considered to be C1403p287 |a cluster member. According to the GCVS, BK Boo might be a constant star. # C1427m057 |V1-7 C1427m057 | Baade (1945) with x,y coordinates and an ID chart C1427m057 |V8-21 C1427m057 | Salinas et al. (2005) with x,y coordinates and an ID chart # C1436m263 |V1-15 C1436m263 | Rodrigues de Andrade et al. (2012) with RA, dec and an ID chart # C1452m820 | V1-129 (confirmed) and V130-170 (suspected) by Fourcade C1452m820 | ID charts were published and x,y coordinates listed for V1-169 C1452m820 | by Fourcade & Laborde (1969), for V1-6 by Fourcade & Laborde (1965) C1452m820 | and for V1-34 by Fourcade et al. (1966). C1452m820 | Fourcade et al. (1974) also published an ID chart. Unfortunately, C1452m820 | in the University of Toronto copy, it is inaccessible because it C1452m820 | is folded into the binding. However, according to Samus (2009, C1452m820 | private communication) two different stars are listed as V65 and C1452m820 | V106 is incorrectly labelled as V108. C1452m820 | Most of Fourcade's suspected variables (130-170) were not detected C1452m820 | as variables in subsequent studies and are therefore not listed in C1452m820 | the above table. Clement et al. (1979 - Table 2) summarized C1452m820 | their findings with regard to these stars. V153 and V167 were C1452m820 | later recovered as RR Lyrae variables by Walker & Nemec (1996). C1452m820 | V171 is RR star #26 of Sarajedini (1993 - Fig. 1 and Table 3) C1452m820 | It was also identified as V1575 by Walker & Nemec (1996 - Fig 3 C1452m820 | and Table 8). C1452m820 | The number V171 was assigned in the electronic catalogue of C1452m820 | Clement et al. (2001). C1452m820 | Sarajedini's other two "new" RR Lyrae variables, #2 and #14 C1452m820 | were later shown by Walker & Nemec to be Fourcade's V17 and V88; C1452m820 | they had been misidentified on Fourcade's original finding chart. C1452m820 | V172 = blue straggler #4, a suspected BSS variable (Sarajedini 1993) C1452m820 | who listed its X,Y pixel numbers in Table 4 of his paper. C1452m820 | Its variability was later confirmed by Walker & Nemec (1996) who C1452m820 | labelled it on a chart (Fig. 3 in their paper). C1452m820 | The number V172 was assigned in the electronic catalogue of C1452m820 | Clement et al. (2001). C1452m820 | Sarajedini (1993) noted the possibiity of variation in two C1452m820 | other blue stragglers (his #2 and #16), but Walker & Nemec did C1452m820 | not detect any variability in these stars. C1452m820 | V173 = star #434 of Walker & Nemec (1996), a foreground RR Lyrae C1452m820 | they identified in Fig 2 of their paper. They also derived this C1452m820 | star's x,y position. C1452m820 | The number V173 was assigned in the electronic catalogue of C1452m820 | Clement et al. (2001). C1452m820 |--------------------------------------------------------------------- C1452m820 |Sahay et al. (2014) detected two long period variables in the field of C1452m820 |IC 4499. They designated them as SLW1 and SLW2 and listed their RA, C1452m820 |dec, V, I, J, H, K magnitudes and derived periods of 67 and 35 days C1452m820 |respectively, based on V magnitudes. They tentatively classified both C1452m820 |stars as non-members based on their location relative to the IC 4499 C1452m820 |giant branch defined by Hankey & Cole (2011) on a K-(J-K) plot. # C1500m328 | C1500m328 |V1-27 C1500m328 | Rosino (1961) with ID charts and x,y, coordinates # C1513p000 | V1-5 C1513p000 | Rosino (1951) with x,y positions and ID chart. C1513p000 | Rosino also identified 5 suspected variables s1-s5, but C1513p000 | Kinman & Rosino (1962) did not find any evidence for variability C1513p000 | in these stars. C1513p000 |-------------------------------------------------------------------- C1513p000 |Three additional RR Lyrae variables that might be associated with Pal 5 C1513p000 |have been discovered in surveys by Vivas et al. (2004): QUEST #403 and C1513p000 |#405 and by Wu et al. (2005): Wu #133. These variables all lie C1513p000 |outside the tidal radius which is 7.58 arcmin according to the 2010 C1513p000 |update of the Harris (1996) catalogue. However, they might be part of C1513p000 |the tidal tail identified by Odenkirchen et al. (2003). # C1514m208 |V1-4 C1514m208 | Sawyer (1953) with x,y coordinates and an ID chart C1514m208 |V5-7 C1514m208 | Sandage & Katem (1968) with ID chart; the x,y coordinates C1514m208 | were published by Sawyer Hogg (1973) in her 3rd catalogue. C1514m208 | Wehlau & Sawyer Hogg (1979) later pointed out that V7 was incorrectly C1514m208 | identified by Sandage & Katem (1969). V7 is actually SK#161 not SK#119. C1514m208 | Corrected x,y coordinates were published by Clement & Rowe (2001). C1514m208 |V8 = Star 63 of Sandage & Katem (1968) who suggested that it may vary. C1514m208 | Wehlau & Sawyer Hogg (1979) confirmed the variation and assigned the C1514m208 | number V8 and x,y coordinates were derived by Clement & Rowe (2001). C1514m208 | C1514m208 |V9 C1514m208 | Wehlau et al. (1996) with ID chart and x,y coordinates C1514m208 |V10-13 C1514m208 | Clement & Rowe (2001) with ID chart and x,y coordinates for all C1514m208 | of the variables except V5 and V9. C1514m208 |---------------------------------------------------------- C1514m208 |Lynch & Ransom (2011) conducted a search for pulsars, but did not find C1514m208 |any in NGC 5897 # C1516p022 |V1-92 C1516p022 | Bailey (1902) with x,y positions on page 239-240 and an ID chart C1516p022 | (Plate VIII, Fig 2, caption on page 248-249) C1516p022 | In a later paper devoted entirely to M5, Bailey (1917) gave a good C1516p022 | description of the early work on the variables in M5. He also noted C1516p022 | that the variability of V22, V23, V25, V46, V48, V49, V51, V53 was C1516p022 | doubtful. Oosterhoff (1941) later confirmed that V22, V23, V46, V48, C1516p022 | V49 were non-variable and that the variability of V51 was uncertain, C1516p022 | but classified V25 and V53 as variables. C1516p022 |V93-103 C1516p022 | Oosterhoff (1941) with x,y positions in Table 3 and ID chart (Plate C1516p022 | I) C1516p022 |V104-114 C1516p022 | Kadla et al. (1987) and summarized in English by Gerashchenko (1987) C1516p022 | with x,y positions C1516p022 |V115-131 = variables 1, 2, 8, 9, 11, 12, 15, 16, 19-27 C1516p022 | Kravtsov (1988) with ID chart and 1950 RA and dec. C1516p022 | The numbers V115-131 were later assigned by Kravtsov (1991). C1516p022 | A total of 27 variables were announced by Kravtsov (1988), but C1516p022 | #18, 17, 14, 13, 7, 6, 10, 3, 4 and 5 were the same as Kadla's C1516p022 | V105-114. C1516p022 |V132-133 C1516p022 | Kravtsov (1991) with ID chart, x,y coordinates and 1950 RA and dec C1516p022 |V134-141 C1516p022 | Sandquist et al. (1996) with x,y coordinates C1516p022 | It was later shown by Caputo et al. (1999) that V134 was the same C1516p022 | star as V129. Apparently Sandquist et al. did not realize this C1516p022 | because the y coordinate they listed for V129 was incorrect. Also, C1516p022 | according to Samus et al. (2009), V135 is the same star as V36. C1516p022 | Arellano Ferro et al. (2015) did not detect any variability in C1516p022 | V136, V138 or V140. They also pointed out that there was a typo C1516p022 | in the RA listed for V140 in an earlier version of this catalogue. C1516p022 |V142-143 = V123, V116 C1516p022 | Brocato et al. (1996) with ID chart. The numbers V142 and V143 were C1516p022 | assigned later by Caputo et al. (1999) because the numbers V116 and C1516p022 | V123 had been previously assigned to other variables by Kravtsov C1516p022 | (1988). C1516p022 | Brocato et al. announced more than 20 other "new" variables, but C1516p022 | the majority of these had already been discovered by other authors. C1516p022 | Caputo et al. (1999 - Table 1) published a table with C1516p022 | cross-identifcations for these stars. C1516p022 | Caputo et al. also published ID charts for all of V104-144, with C1516p022 | the exception of V133 and V141, which were outside their field of C1516p022 | view. C1516p022 |V144-148 = star #596, 629, 648, 651, 652 C1516p022 | Reid (1996) with pixel numbers and ID charts (#596 in quadrant #3 and C1516p022 | the others in quadrant #4). The numbers V144-148 were assigned by C1516p022 | Caputo et al. (1999) C1516p022 | Caputo et al. questioned the variability of V144 (#596) and Kaluzny C1516p022 | et al. (1999) stated that the other four variables were all spurious C1516p022 | detections. This result was subsequently confirmed by Arellano Ferro C1516p022 | et al. (2015) who did not detect variability in any of these stars. C1516p022 | Reid published an errata for his paper because some of the C1516p022 | previously known RR Lyrae variables were incorrectly identified. C1516p022 |V149-154 = V1-6 C1516p022 | Yan & Reid (1996) with an ID chart and x,y coordinates. The numbers C1516p022 | V149-154 were assigned by Caputo et al. (1999). C1516p022 | Kaluzny et al. (1999) stated that these variables were all spurious C1516p022 | detections. This result was subsequently confirmed by Arellano Ferro C1516p022 | et al. (2015) who did not detect variability in any of these stars. C1516p022 |V155-159 = HST-V6, V15, V16, V19, V28 C1516p022 | Drissen & Shara (1998) with RA & dec and an ID chart C1516p022 | The numbers 155-159 were assigned by Caputo et al. (1999). C1516p022 | Drissen & Shara recovered 24 additional variables in their study, all C1516p022 | of which were previously discovered. Table 1 of Caputo et al. (1999) C1516p022 | lists cross-references for the variables V104 to V159. C1516p022 |V160-163 C1516p022 | Olech et al. (1999) with x,y coordinates and ID charts C1516p022 |V164-168 = NV1-5 C1516p022 | Kaluzny et al. (1999) RA, dec and ID charts C1516p022 | The numbers V164-168 were assigned in our on-line catalogue C1516p022 | (Clement et al. 2001) C1516p022 |V169 = Zhukov 963 C1516p022 | Rees (1993) noted that Zhukov 963 was probably variable and C1516p022 | Kaluzny et al. (2000) confirmed this. The number V169 was assigned C1516p022 | in our on-line catalogue (Clement et al. 2001). C1516p022 |V170-181 C1516p022 | Arellano Ferro et al. (2015) with RA, dec and ID charts C1516p022 |PSR-M5A and PSR-M5B = PSR B1516+02A and PSR B1516+02B C1516p022 | The data above are from Freire et al. (2008). The discovery was C1516p022 | originally announced by Wolszczan et a. (1989). C1516p022 | M5B is in a binary system with orbital period = 6.86 days C1516p022 |PSR-M5C, PSR-M5D, PSR-M5E = PSR J1518+0204C, PSR J1518+0204D, PSR C1516p022 | J1518=0204E, millisecond pulsars in binary systems C1516p022 | Hessels et al. (2007) who derived orbital periods of 2.08, 29.3 and C1516p022 | 26.3 hr. respectively for M5C, M5D and M5E. C1516p022 |------------------------------------------------------------------------ C1516p022 |Pietrukowicz et al. (2008) searched for dwarf novae in M5 and easily C1516p022 |detected V101. Their observations covered 34 nights in the years C1516p022 |1997-1999 and 2002-2004. No new erupting objects were found in the C1516p022 |field of M5. C1516p022 |------------------------------------------------------------------------ C1516p022 |Raney et al. (2014) are undertaking an automated search for RR Lyrae C1516p022 |variables in M5 using data from the Catalina Real-Time Transient Survey. C1516p022 |-------------------------------------------------------------------------- C1516p022 |Kraemer et al. (2013) announced that they are making optical and C1516p022 |near-infrared observations in order to identify the long period variables C1516p022 |on the AGB. # C1524m505 |V1&2 = Fourcade #4 and #14 C1524m505 | Fourcade et al. (1966) announced 15 variables in the field of NGC 5927 C1524m505 | and published x,y coordinates and an ID chart. C1524m505 | Sawyer Hogg (1973) designated Fourcade's V4 and V14 as V1 and V2 in her C1524m505 | 3rd catalogue. C1524m505 |V3 C1524m505 | Osborn (1968) with x,y coordinates and an ID chart C1524m505 | The number V3 was assigned by Sawyer Hogg (1973) in her 3rd catalogue. C1524m505 |V4-11 = V3, V6, V7, V8, V9, V10, L43, L17 of Lloyd Evans & Menzies C1524m505 | (1973), but no identification was provided by these authors. C1524m505 | After consultation with Lloyd Evans and Menzies, Sawyer Hogg (1973) C1524m505 | assigned the numbers V4-11 in her 3rd catalogue and Menzies (1974) C1524m505 | labelled them, along with V1 and V2, on an ID chart (see Plate II of his C1524m505 | paper). C1524m505 |--------------------------------------------------------------------------- C1524m505 |Liller (1983) conducted a search for RR Lyrae variables in NGC 5927, but C1524m505 |did not discover any. She derived mean B magnitudes for the known C1524m505 |variables from her observations. The cluster CMD has a stubby red HB C1524m505 |that does not extend into the instability strip. # C1531m504 |V1-3 = Fourcade #1, 2 and 4 C1531m504 | Fourcade et al. (1966) announced 8 variables in the field of NGC 5946 C1531m504 | and published x,y coordinates and an ID chart. Sawyer Hogg (1973) C1531m504 | designated Fourcade's V1, 2 and 4 as V1, 2 and 3 in her 3rd catalogue C1531m504 | and considered the other 5 to be field variables. C1531m504 |V4-7 C1531m504 | Liller (1983) with x,y coordinates and an ID chart C1531m504 | Liller also announced an additional 7 field variables. # C1542m376 |V1-5 C1542m376 | Rosino (1962) with an ID chart and x,y coordinates C1542m376 |V6-12 C1542m376 | Liller & Lichten with an ID chart and x,y coordinates C1542m376 |V13 C1542m376 | Matsunaga et al. (2006) with RA and dec C1542m376 |PSR = PSR J1546-3747A = NGC 5986A C1542m376 | Lynch & Ransom (2011) who derived orbital P = 1.3 days C1542m376 |---------------------------- C1542m376 |Moni Bidin et al. (2009) detected a close binary candidate: C1542m376 |their star #4175, an EHB star. # C1607m551 | C1607m551 | V1 C1607m551 | Sloan et al. (2010) with RA and dec. C1607m551 |-------------------------------------------------------------------- C1607m551 |References C1607m551 |Ortolani, S., Bica, E., Barbuy, B. 1993, A&A, 273, 415 C1607m551 |Sarajedini, A. et al. 2007, AJ, 133, 1658 C1607m551 |Sloan, G. C., Matsunaga, N., Matsuura, M., Zijlstra, A. A., Kraemer, K. C1607m551 |E., Wood, P. R., Nieusma, J., Bernard-Salas, J., Devost, D., Houck, J. R. C1607m551 |2010, ApJ, 719, 1274 # C1614m228 |V1-2 C1614m228 | Bailey (1902) with x,y position and ID chart C1614m228 | (see Appendix page 237 for x,y tables and page 246 for C1614m228 | description of plates). C1614m228 |V3-6 C1614m228 | Sawyer (1942) with x,y positions and an ID chart. C1614m228 |V6-7 = S Sco, R Sco C1614m228 | These are both Mira variables in the field and were discovered in C1614m228 | 1853. The number V6 was assigned by Sawyer (1942) and V7 by Sawyer C1614m228 | (1955) in the 2nd edition of her catalogue. C1614m228 | C1614m228 |V8-10 C1614m228 | Wehlau et al. (1984) with x,y coordinates C1614m228 | ID charts for V1-10 were later published by Wehlau et al. (1990). C1614m228 |V11-V12 = DN1&DN2 C1614m228 | Shara et al. (2005 ) with RA, dec and ID chart C1614m228 | The numbers V11&V12 are assigned here. C1614m228 |V13-V32 C1614m228 | Kopacki (2013) with RA and dec C1614m228 | In a preliminary report, Kopacki (2009) announced his new variables, C1614m228 | but used a different numbering system. In the above table, we use C1614m228 | the numbers he assigned in his 2013 paper. C1614m228 |V33 = Dieball et al. (2010) #2238 = TDK #2 of Thomson et al. (2010) C1614m228 | The number V33 was assigned by Kopacki (2013) C1614m228 | Dieball et al. (2010) and Thomson et al. (2010) identified this C1614m228 | star as a blue straggler and derived a period of approximately C1614m228 | 55 minutes. They classified it as an SX Phe variable. C1614m228 |V34-40 C1614m228 | Figuera Jaimes et al. (2016) with RA, dec and ID chart C1614m228 | C1614m228 |Nova = T Sco C1614m228 | The nova was discovered in 1860. An account of its discovery C1614m228 | was given by Sawyer (1938) and also by Wehlau et al. (1990). C1614m228 | The RA and dec listed above are from Dieball et al. (2010) C1614m228 |---------------------------------------------------- C1614m228 |Additional candidate variables C1614m228 | Heinke et al. (2003) identified 19 Chandra X-ray sources: CX1-CX19 C1614m228 | in M80. C1614m228 | They classified CX2 and CX6 as quiescent LMXBs C1614m228 | and CX3, CX4, CX5 and CX15 as candidate cataclysmic variables. C1614m228 | They also suggested that CX1 might be the X-ray counterpart of C1614m228 | Nova 1860 and Dieball et al. (2010) concur. C1614m228 | Moni Bidin et al. (2009) identified a candidate C1614m228 | EHB close binary in M80 (their star #16389). # C1620m264 | V1-33 C1620m264 | Leavitt & Pickering (1904) with x,y positions C1620m264 | An ID chart was subsequently published by Sawyer (1931). C1620m264 | V34-43 C1620m264 | de Sitter (1947) with x,y positions for V34-43 and Greenstein's C1620m264 | (1939) numbers for V35-42. Greenstein's paper included an ID chart. C1620m264 | In an earlier report, de Sitter (1941) listed the x,y coordinates C1620m264 | for these new variables C1620m264 | V44 = Alcaino #246 C1620m264 | V45 = Alcaino #381 C1620m264 | V46 = Alcaino #382 C1620m264 | V47 = Alcaino #505 C1620m264 | These are HB stars that Alcaino (1975) indicated as variables C1620m264 | in Table 3 of his paper. He labelled them on his ID charts. C1620m264 | The numbers V44-47 were assigned by Clement (1997) in the first C1620m264 | electronic update of the Sawyer Hogg (1973) catalogue. C1620m264 | V48 = Lee #1717 = Greenstein 172 = Alcaino 522 C1620m264 | V49 = Lee #3602 = Greenstein 140 = Alcaino 488 = ZB 19 C1620m264 | V50 = Lee #3732 C1620m264 | V51 = Lee #1610 C1620m264 | V52 = Lee #2630 = Greenstein 37 = Alcaino 433 = ZB 18 C1620m264 | These are HB stars that Lee (1977) considered to be RR Lyrae C1620m264 | variables (V48-50) or suspected RR Lyrae variables (V51-52). C1620m264 | See Table 3 of his paper. They were all labelled on finding C1620m264 | charts in his paper. C1620m264 | The numbers V48-52 were assigned by Clement (1997) in the first C1620m264 | electronic update of the Sawyer Hogg (1973) catalogue. C1620m264 | V49 (ZB 19, G140) and V52 (ZB 18, G37) were independently discovered C1620m264 | by Yao (1980a,b) who listed their x,y coordinates and Greenstein C1620m264 | (1939) numbers. The Alcaino (1975) numbers for Lee #3602 (V49) and C1620m264 | Lee #2630 (V52) were published by Cudworth & Rees (1990) and the ID C1620m264 | charts of Alcaino and Greenstein can be readily compared. C1620m264 | V53 = ZB 44 = Greenstein 512 = Lee 1411 = Alcaino 219 C1620m264 | V54 = ZB 38 = Greenstein 30 = Lee 3621 = Alcaino 464 C1620m264 | V55 = ZB 39 = Greenstein 327 = Lee 3315 = Alcaino 64 C1620m264 | suspected variables announced by Yao et al. (1981a,b) C1620m264 | who identified them according to their Greenstein (1939) numbers. C1620m264 | ID charts were published by Greenstein (1939). C1620m264 | ZB is the abbreviation for Zhongguo Bianxing (Chinese Variable Star). C1620m264 | C1620m264 | The numbers V53-55 were assigned by Clement (1997) in the C1620m264 | first electronic update of the Sawyer Hogg (1973) catalogue. C1620m264 | In Table 1 of his paper, Alcaino (1975) indicated that Greenstein C1620m264 | #512 and #30 were Alcaino #219 and #464 respectively and C1620m264 | Cudworth & Rees (1990) listed their Lee numbers: #1411 and #3621. C1620m264 | ID charts were published by Alcaino (1975) and by Lee (1977). C1620m264 | In a subsequent paper, Yao (1991) listed the Alcaino and Lee numbers C1620m264 | for Greenstein #327 (V55). C1620m264 | V56 = ZB 37 = Greenstein 265 = Alcaino 375 = Lee 4508 C1620m264 | V57 = ZB 43 = Greenstein 266 = Alcaino 374 = Lee 4509 C1620m264 | suspected variables announced by Yao (1979a) who identified them C1620m264 | according to their Greenstein (1939) numbers. ID charts were C1620m264 | published by Greenstein (1939). C1620m264 | ZB is the abbreviation for Zhongguo Bianxing (Chinese Variable Star). C1620m264 | The numbers V56 and V57 were assigned by Clement (1997) in the C1620m264 | first electronic update of the Sawyer Hogg (1973) catalogue. C1620m264 | In Table 1 of his paper, Alcaino (1975) noted that the Greenstein C1620m264 | #265 and #266 were Alcaino #375 and #374 respectively and Cudworth C1620m264 | & Rees (1990) listed their Lee numbers: #4508 and #4509. ID charts C1620m264 | were published by Alcaino (1975) and by Lee (1977). C1620m264 | V58 = Greenstein 206 = Alcaino 491 = Lee 4632 C1620m264 | V59 = Greenstein 481 = Alcaino 371 = Lee 4512 C1620m264 | V60 = Greenstein 543 = Alcaino 376 = Lee 4507 C1620m264 | suspected variables announced by Yao (1987) who identified them C1620m264 | according to the numbers of Greenstein (1939), Alcaino (1975) and Lee C1620m264 | (1977). Id charts were published in all three of these papers. C1620m264 | The numbers V58-60 were assigned by Clement (1997) in the C1620m264 | first electronic update of the Sawyer Hogg (1973) catalogue. C1620m264 | V61 = Greenstein 46 = Alcaino 440 = Lee 2616 C1620m264 | Yao (1988) with ID chart, x,y position and Greenstein (1939) number. C1620m264 | The number V61 was assigned by Clement (1997) in the first C1620m264 | electronic update of the Sawyer Hogg (1973) catalogue. C1620m264 | A comparison of the ID charts of Greenstein and Alcaino shows that C1620m264 | Greenstein #46 = Alcaino #440 and Cudworth & Rees (1990) listed C1620m264 | Lee 2616 = Alcaino 440. C1620m264 | V62 = V55 C1620m264 | = Greenstein 327 = Alcaino 64 = Lee 3315 C1620m264 | Yao (1991) with the Greenstein, Alcaino and Lee numbers C1620m264 | The number V62 was assigned by Clement (1997) in the first C1620m264 | electronic update of the Sawyer Hogg (1973) catalogue, but C1620m264 | it is now known that this is the same star as V55 which was C1620m264 | announced by Yao (1981a,b) in an earlier paper. C1620m264 | V63-V74 are V44-V55 of C1620m264 | Kaluzny et al. (1997) who published ID charts and 1950 RA and dec. C1620m264 | The 2000 RA and dec listed in the above table are from Stetson et C1620m264 | al. (2014). C1620m264 | The numbers V63-V74 were assigned in the electronic update C1620m264 | to Sawyer Hogg's 1973 catalog (Clement et al. 2001). C1620m264 | V75 = ZB 36 = Greenstein 343 C1620m264 | Yao (1979b) with x,y position and ID chart. C1620m264 | Greenstein's 1939 paper also included an ID chart. C1620m264 | ZB is the abbreviation for Zhongguo Bianxing (Chinese Variable Star). C1620m264 | The number V75 was assigned in this electronic catalogue in 2009. C1620m264 | V76 = ZB14 C1620m264 | Yao (1977,1978) with x,y position and ID chart. C1620m264 | ZB is the abbreviation for Zhongguo Bianxing (Chinese Variable C1620m264 | Star). C1620m264 | C1620m264 | The number V76 was assigned in this electronic catalogue in 2009. C1620m264 | V77-78 = variables numbered 56 and 57 of Mochejska et al. (2002) C1620m264 | with RA, dec and ID charts C1620m264 | The numbers V77 and V78 were assigned in this electronic catalogue C1620m264 | in 2009. C1620m264 | Stetson did not detect variabiity in V78. C1620m264 | V79 = Greenstein 302 = Lee 3107 C1620m264 | Yao et al. (2004a,b) with Greenstein (1939) and Lee (1977) numbers C1620m264 | and an ID chart C1620m264 | The number V79 was assigned in this electronic catalogue in 2009. C1620m264 | V80 = Alcaino 66 C1620m264 | Yao et al. (2006) with RA and dec. C1620m264 | Alcaino (1975) published an ID chart. C1620m264 | The number V80 was assigned in this electronic catalogue in 2009. C1620m264 | V81-90 = K58-K66, K68 C1620m264 | Kaluzny et al. (2013b) with RA and dec C1620m264 | Finder charts for K65 and K66 were published by Kaluzny et al. C1620m264 | (2013a) and finder charts for the others were published by C1620m264 | Kaluzny et al. (2013b). C1620m264 | V91 = K69 C1620m264 | Kaluzny et al. (2013a) with RA, dec and a finding chart C1620m264 | V92 = N31 of Nascimbeni et al. (2014) who published RA and dec C1620m264 | = C1 of Stetson et al. (2014) who published RA and dec C1620m264 | The authors of both of these investigations recognized that this C1620m264 | RR Lyrae variable was a close companion to the RR Lyrae variable C1620m264 | V40 that had not been adequately resolved in earlier photographic C1620m264 | studies. C1620m264 | V93-109 = N1, N2, N3, N8, N9, N11, N12, N13, N16, N17, N18, N21, C1620m264 | N29, N32, N33, N36, N38 C1620m264 | New variables announced by Nascimbeni et al. (2014) and C1620m264 | identified by their RA and dec C1620m264 | Not included in this list is their N19, an eclipsing binary C1620m264 | that is not a cluster member, based on its proper motion. C1620m264 | V110-111 = C6, C7 C1620m264 | New variables announced by Stetson et al. (2014) and identified by C1620m264 | their RA and dec C1620m264 | Stetson et al. announced five other new variables - C1 which is now C1620m264 | known as V92 and C2-5 which are not cluster members, based on their C1620m264 | location in the CM diagram. C1620m264 | PSR = PSR B1620-26 C1620m264 | Lyne et al. (1988) reported the discovery of an 11-ms pulsar in M4 C1620m264 |---------------------------------------------------------------- C1620m264 | Pietrukowicz et al. (2008) searched for dwarf novae in M4 and found C1620m264 | none. C1620m264 | Frandsen et al. (2007) observed 24 K giants in M4 in an attempt to C1620m264 | detect photometric variability due to p-mode oscillations. They were C1620m264 | unable to claim an unambiguous detection. C1620m264 | Figuera Jaimes et al (2016) searched for variables in 41 by 41 arcsec C1620m264 | field around the cluster centre and recovered V21, V81 and V101, but did C1620m264 | not detect any new ones. # C1620m720 | V1-15 C1620m720 | Liller (1981) with x,y coordinates and an ID chart C1620m720 | Fourcade et al. (1966) had previously observed the cluster but did C1620m720 | not discover any variables. C1620m720 | V16-22 C1620m720 | Cohen et al. (2011) with RA, dec and and an ID chart C1620m720 | V23 C1620m720 | Fitzgerald et al. (2012) with RA, dec and an ID chart # C1624m259 | V1 = BP Sco C1624m259 | Sawyer (1953) with x,y coordinate C1624m259 | V2 = BO Sco C1624m259 | Liller (1983) with x,y coordinates and an ID chart for V1 and V2 C1624m259 | Liller recovered Sawyer's V1 and found that Sawyer's previously C1624m259 | published y coordinate was incorrect. C1624m259 |-------------------------------------------------------- C1624m259 |Sarajedini et al. (2007) published a V-I color magnitude diagram which C1624m259 |shows a blue HB and a well defined blue straggler sequence. C1624m259 |Some of the blue stragglers are probably variable but a variability C1624m259 |search has not been carried out. Because the HB is populated only on C1624m259 |the blue side of the instability strip, it is not surprising that no RR C1624m259 |Lyrae variables have been detected. # C1624m387 | V1-10 C1624m387 | Hazen (1991) with x,y coordinates and ID charts C1624m387 | Hazen also provided data for 6 field variables, F1-6, which she C1624m387 | discovered outside the cluster's tidal radius. C1624m387 | Fourcade et al. (1966) had previousy observed the cluster but did C1624m387 | not discover any variables. # C1629m129 | V1-24 C1629m129 | Oosterhoff (1938) with x,y positions and ID chart C1629m129 | V25 C1629m129 | Lloyd Evans & Menzies (1973) C1629m129 | V25 is star 217 in the insert to Fig 1 of Sandage & Katem C1629m129 | (1964) C1629m129 | V26: C1629m129 | McCombs et al. (2012) with RA dec and an ID chart # C1639p365 | A good discussion of the history of the investigations of C1639p365 | variable stars in M13 was given by Kopacki et al. (2003, A&A 398, 541). C1639p365 | Ludendorff (1905, Potsdam Publ 15, Nr. 50) listed C1639p365 | 'delta RA' and 'delta Dec' for 1118 stars in M13. C1639p365 | His catalog numbers have been cited by many of C1639p365 | the authors whose discoveries are listed below. C1639p365 | Ludendorff's xy positions have been converted to C1639p365 | J2000 coordinates which are available through the Simbad database. C1639p365 | V1-2 C1639p365 | Bailey (1902, Harvard Annals 38) with ID chart (Plate X, p252.19) and x,y C1639p365 | coordinates (p241) C1639p365 | V3-6 = Ludendorff 135, 322, 806 (north componentof a double) and 872 C1639p365 | Shapley (1915, PASP 27, 134) who listed the Ludendorff (1905) catalogue numbers. C1639p365 | The numbers V3 to V6 were assigned by Sawyer (1940) C1639p365 | V7 = Ludendorff 344 C1639p365 | Shapley (1915, PASP 27, 238) who identified it by its Ludendorff number C1639p365 | Shapley also noted that Barnard (1914) had called attention to C1639p365 | this variable and published its 1902 RA and dec. C1639p365 | The number V7 was assigned by Sawyer (1940) C1639p365 | V8-11 C1639p365 | Sawyer (1940, DDO Publ. 1, No. 5) who listed Ludendorff numbers, x,y positions C1639p365 | and published an ID chart for V1-11 C1639p365 | V1 = L816, V2 = L306, V3 = L135, V4 = L322, V5 = L806_beta, C1639p365 | V6 = L872, V7 = L344, V8 = L206, V9 = L806_alpha, V10 = L487, C1639p365 | V11 = L324 C1639p365 | V12-14 = Ludendorff #187, 327, 527 C1639p365 | Kollnig-Schattschneider (1942, AN 273, 145). The numbers C1639p365 | V12-14 were assigned by Sawyer (1955) in her 2nd catalogue. C1639p365 | Sawyer (1955) also pointed out that the variable identified as C1639p365 | L200 by Kollnig-Schattschneider should have been L206 (now known as V8) C1639p365 | The RA and dec we list for V14 is from Osborn (2000) C1639p365 | V15 = Ludendorff #835 C1639p365 | Arp (1955a,b): C1639p365 | V15 was labelled in Fig. 3 by Arp (1955a) and in Arp (1955b), C1639p365 | V15 is labelled as star IV-48 in Fig 2 and Table 1 where C1639p365 | it is described as an irregular variable. C1639p365 | Sawyer (1955) listed V15 and its Ludendorff number (835) in her C1639p365 | 2nd catalogue based on correspondence with Arp. C1639p365 | V16 = #A18 of Savedoff (1956, AJ 61, 254) = Ludendorff #1079 C1639p365 | This variable was announced by Sawyer Hogg (1973) who noted that C1639p365 | it was discovered by Tsoo Yu-hua who had sent her a finding C1639p365 | chart. Sawyer Hogg identified V16 as Savedoff A18 which was C1639p365 | probably Ludendorff #1113, but Cudworth & Monet (1979) found that C1639p365 | Savedoff A18=Ludendorff #1079. Osborn (2008, private C1639p365 | communication to C Clement) examined a photocopy of Tsoo's C1639p365 | finding chart provided by Sawyer Hogg and confirmed that C1639p365 | V16 = A18 = L1079. He also provided the RA and dec which are C1639p365 | listed above, based on the 2MASS catalog. C1639p365 | In addition, Sawyer Hogg (1973) noted that Tsoo discovered a C1639p365 | variable in the surrounding field. These 2 suspected variables C1639p365 | were also mentioned in Sawyer Hogg's (1967) IAU report. C1639p365 | V17 = Ludendorff #973 = Arp (1955b) I-48 C1639p365 | Rusev (1974) indicated that L973 might be variable and this was C1639p365 | confirmed by Fuenmayor & Osborn (1974). C1639p365 | The number V17 was assigned by Clement (1997) in the first electronic C1639p365 | update of the Sawyer Hogg (1973) catalogue. C1639p365 | V18-20 = Ludendorff #72, 194, 70 C1639p365 | announced by Russeva & Russev (1980, IBVS 1769) who listed their C1639p365 | (1905) numbers. C1639p365 | The numbers V18, V19, V20, were assigned by Clement (1997) in the C1639p365 | first electronic update of the Sawyer Hogg (1973) catalogue. C1639p365 | V19 (L194) had been previously announced as a supected variable C1639p365 | by Kadla et al. (1976). C1639p365 | V20 (L70) was previously suspected to be variable by Pike & Meston C1639p365 | (1977) who identified it as Arp (1955b) II-67. The RA and dec C1639p365 | listed for V20 are from Osborn (2000). C1639p365 | Russeva & Russev also indicated that L240 and L261 met their C1639p365 | suspected variability criterion, but gave no further discussion of C1639p365 | these two stars. L240 and L261 are not listed as variables in the C1639p365 | above table because Osborn (2000) observed them both and did not C1639p365 | detect any variabiity. L261 was also observed by Kopacki et al. C1639p365 | (2003) who did not detect any variability. C1639p365 | V21-31 = Stars X1-11 listed with x,y positions by Kadla et al. (1980) C1639p365 | who also included Ludendorff numbers when available: C1639p365 | X1=L216, X4=L598, X7=L254, X8=L569, X9=L717, X10=L743, X11=L807 C1639p365 | In an earlier paper, Kadla et al. (1976) announced that X4 C1639p365 | (=L598=B140) was probably variable. They also indicated that C1639p365 | L222 (=Barnard 29), a known binary star, might be variable, but C1639p365 | did not mention it in their 1980 paper. Kopacki et al (2003) C1639p365 | observed L222 and did not detect any variability. C1639p365 | The numbers V21-31 were assigned by Clement (1997) in the first C1639p365 | electronic update of the Sawyer Hogg (1973) catalogue. C1639p365 | V32 = Ludendorff #66 C1639p365 | Russeva et al (1982) who listed the Ludendorff number. C1639p365 | The RA and dec have been provided by Osborn (2008, private C1639p365 | communication) based on the 2MASS catalog. C1639p365 | The number V32 was assigned by Clement (1997) in the first C1639p365 | electronic update of the Sawyer Hogg (1973) catalogue. C1639p365 | Russeva et al (1982) also confirmed the variability of V24 C1639p365 | (=X4=L598) previously announced by Kadla et al. (1980) C1639p365 | V33 = Ludendorff #954 C1639p365 | announced by Welty (1985) with Ludendorff number C1639p365 | The RA and dec listed above are from Osborn (2000) C1639p365 | The number V33 was assigned by Clement (1997) in the first C1639p365 | electronic update of the Sawyer Hogg (1973) catalogue. C1639p365 | V34-37 C1639p365 | Kopacki et al (2003, A&A 398, 541) with ID chart, RA and dec C1639p365 | V38 = Ludendorff #414 C1639p365 | Russev (1973) and Rusev (1974) indicated that L414, might be C1639p365 | variable but Fuenmayor & Osborn (1974) could not confirm this in C1639p365 | their observations. C1639p365 | However, Kopacki et al. (2003) detected variability and assigned C1639p365 | the number V38. C1639p365 | V39-40 = Ludendorff #629, 940 C1639p365 | Osborn (2000) with RA, dec (J2000) and Ludendorff numbers C1639p365 | Osborn concluded that the variablility was certain for L629 and C1639p365 | possible for L940. C1639p365 | Kopacki et al. (2003) found both stars to be variable and assigned C1639p365 | the numbers V39 and V40. C1639p365 | V41-45 C1639p365 | Kopacki et al. (2003) with ID chart, RA and dec C1639p365 | V46-49 = M13_01 to M13_04 announced by C1639p365 | Pietrukowicz & Kaluzny (2004, AcA 54, 19) with RA and dec. C1639p365 | The numbers V46-49 were assigned by Kopacki (2005, AcA 55, 85) C1639p365 | V50 C1639p365 | Kopacki (2005) with ID chart, RA and dec (J2000) C1639p365 | The positions of V37, V46, and V47 were also labelled on the C1639p365 | ID chart C1639p365 | V51 = suspected variable star c of Meinunger (1978) who published C1639p365 | an ID chart. C1639p365 | Servillat et al. (2011) confirmed variability from U data and C1639p365 | derived its RA and dec and published an ID chart. It was C1639p365 | variable #7 in their study. C1639p365 | The number V51 has been assigned in this catalogue. C1639p365 | V51 is also L993 (Lundendorff 1905), IV-52 (Arp 1955b) and star #3 C1639p365 | on the list of UV bright stars in M13 (Zinn et al. 1972). C1639p365 | V52 = variable #4 of Servillat et al. (2011) who derived RA and dec C1639p365 | (J2000) and published an ID chart. They concluded that this C1639p365 | star is the optical counterpart of Chandra source X6. C1639p365 | The number V52 has been assigned in this catalogue. C1639p365 | V53 = variable #2 of Servillat et al. (2011) who derived RA and dec C1639p365 | (J2000) and published an ID chart. C1639p365 | The number V53 has been assigned in this catalogue. C1639p365 | PSR: According to Paulo Freire's website, there are 5 millisecond C1639p365 | pulsars in M13. (www.naic.edu/~pfreire/GCpsr.html) C1639p365 |------------------------------------------------------------------ C1639p365 | Meinunger (1978) announced 3 suspected variables, which she labelled C1639p365 | as a,b,c on ID charts that also included V6 and V15. C1639p365 | Kopacki et al. (2003) discussed these three stars. C1639p365 | Star a (Ludendorff #765) was outside their field of view. C1639p365 | Variability of star a has not been detected in any subsequent studies. C1639p365 | Star b was a blend of two stars on their CCD frames and therefore C1639p365 | unlikely to be variable. C1639p365 | Star c is now known as V51. (see above) # C1644m018 | V1 C1644m018 | Sawyer (1938) with ID chart and x,y coordinates C1644m018 | V2 = von Braun's M12-V1 C1644m018 | von Braun et al. (2002) with ID chart, RA and dec C1644m018 | von Braun et al. also discovered a field variable which they C1644m018 | called M12-V2. It is a foreground WUMa. C1644m018 | C1644m018 |----------------------------------------------------------------- C1644m018 | Two suspected RR Lyrae (based on their positions in the CM diagram) C1644m018 | were announced by Malakhova et al. (1997) with X,Y positions in C1644m018 | pixels and an ID chart. C1644m018 | Pietrukowicz et al. (2008) searched for dwarf novae in M12 and found C1644m018 | none. C1644m018 | Lu et al. (2009) identified 6 X-ray sources in M12 and suggested that C1644m018 | there may be 2-5 active binaries or cataclysmic variables in the C1644m018 | cluster. C1644m018 | Zloczewski et al. (2012) have identified nine variable blue straggler C1644m018 | stars in M12. They plotted their locations on a V-(B-V) plot C1644m018 | on which they also indicated the locations of six fainter variables C1644m018 | (see Figure 14 of their paper). C1644m018 | Dynamical properties of M12 blue straggler stars have been C1644m018 | investigated by Simunovic & Puzia (2014). # C1645p476 | V1-21 C1645p476 | Baade (1945) with x,y coordinates and an ID chart C1645p476 | V8 had been previously announced by Davis (1917) with delta RA and C1645p476 | delta dec values listed C1645p476 | V22 C1645p476 | Sawyer (1953) with x,y coordinates C1645p476 | V23-24 = suspected RR Lyrae variables: star #88 and #155 of Carney et C1645p476 | al. (1991) who listed x,y pixel coordinates for locating the stars C1645p476 | on their published chart C1645p476 | The numbers V23, 24 were assigned by Borissova et al. (2001) who C1645p476 | published x,y coordinates and identified them on an ID chart. C1645p476 | Carney et al. (1991) listed two other possible RR Lyrae candidates C1645p476 | (their #104 and #134), but Borissova et al. (2001) did not detect any C1645p476 | variability in these stars. C1645p476 | V25-36 = stars #1-12 C1645p476 | Spassova & Borissova (1996) with x,y coordinates and an ID chart C1645p476 | The x,y coordinates they listed for three of the stars: #3, 4 and 5 C1645p476 | are incorrect. They do not correspond to the positions on their chart C1645p476 | which are the positions adopted by Borissova et al. (2001) in their C1645p476 | subsequent, definitive study of the variables in NGC 6229. Samus et C1645p476 | al. (2009) based their RA and dec on the chart published by C1645p476 | Borissova et al. (2001). C1645p476 | Borissova et al. (1997) also listed the Spassova & Borissova C1645p476 | (1996) x,y coordinates for these candidate variables, but the C1645p476 | x,y coordinates were interchanged in the 1996 paper, so they are C1645p476 | incorrect. C1645p476 | V37-48 C1645p476 | Borissova et al. (2001) with x,y coordinates and an ID chart. C1645p476 | These authors labelled all the variables V1-48 (except V3 which was C1645p476 | outside their field of view) on their finding chart. C1645p476 | V49-73 C1645p476 | Arellano Ferro et al. (2015) with RA, dec and finding charts C1645p476 |---------------------------------------------------------------------------- C1645p476 |A possible long period variable C1645p476 | Carney et al. (1991) noted that two stars near the RG tip in the CMD: C1645p476 | their #4 and star IV-12 of Searle and Zinn (1978) might be long C1645p476 | period variables (see section 2.4 on page 1701 and section 3.2 on C1645p476 | page 1713 of Carney's paper.) C1645p476 | Arellano Ferro et al. (2015) observed star #4, and did not detect C1645p476 | any variability. Star IV-12 is their V72. # C1650m220 | V1-2 C1650m220 | Sawyer (1953) with x,y coordinates and an ID chart C1650m220 | V3-5 C1650m220 | Liller (1977) with x,y coordinates and an ID chart # C1654m040 | V1-2 C1654m040 | Sawyer (1938) with ID chart and x,y coordinates C1654m040 | V3 C1654m040 | Arp (1955a) with ID chart for V2&3. C1654m040 | Sawyer (1955) listed the x,y coords in her 2nd catalogue C1654m040 | V4 = Arp IV-37 (see Arp 1955b) C1654m040 | by Voroshilov (1971) who found that this was an HB star in C1654m040 | the instability strip. The number V4 was assigned by Sawyer C1654m040 | Hogg (1973) in her 3rd catalogue. C1654m040 |----------------------------------------------------------------- C1654m040 | Field variables not listed above C1654m040 | M10:V1-3 by von Braun et al. (2002) C1654m040 | vB#1 is a foreground WUMa, #2 is a background RR0 C1654m040 | and #3 is a background SXPhe (or delta Scuti) C1654m040 |------------------------------------------------------------------- C1654m040 | Pietrukowicz et al. (2008, MNRAS 388, 1111) searched for C1654m040 | dwarf novae in M10 and found none. C1654m040 |--------------------------------------------------------------------- C1654m040 |Dalessandro et al. (2013) counted 120 blue straggler stars within the C1654m040 |tidal radius of M10, but no variability search has been carried out. # C1656m370 |V1 C1656m370 | Matsunaga et al. (2006) with RA and dec # C1658m300 |V1-26 C1658m300 | Bailey (1902) with x,y positions on page 241 and an ID chart C1658m300 | (page 252.21, Plate XI, Fig.1, caption on page 250) in which all of C1658m300 | the variables were labelled, with the exception of V10 and V11, which C1658m300 | were outside the field. C1658m300 | In earlier papers, Pickering & Bailey (1897, 1898) gave progress C1658m300 | reports on Bailey's searches for variable stars in globular clusters. C1658m300 |V27-83 C1658m300 | van Agt & Oosterhoff (1959) with x,y coordinates (pp. 289-290) and ID C1658m300 | charts (pp 263-264) on which all of the variables except V1 and V13 C1658m300 | were identified. C1658m300 |V84-262 = NV84-NV262 C1658m300 | Contreras et al. (2010) with RA and dec and finding charts. C1658m300 | Sawyer Hogg (1973) designated six stars as V84-89 in her 3rd C1658m300 | catalogue, but they are not the ones listed here. C1658m300 | The "old" (1973) V84-89 were six new variables announced by Gascoigne C1658m300 | & Ford (1967) and the numbers V84-89 were assigned by Sawyer Hogg C1658m300 | (1973). Unfortunately, Gascoigne & Ford never published periods, C1658m300 | positions or identifications for any of these stars. Undoubtedly, C1658m300 | they are among the 179 new variables discovered by Contreras et al. C1658m300 | (2010). C1658m300 |PSR J1701-3006A C1658m300 | D'Amico et al. (2001a) C1658m300 |PSR J1701-3006B,C C1658m300 | D'Amico et al. (2001b); RA and dec reported for A, B and C C1658m300 | by Possenti et al. (2003) C1658m300 | C1658m300 |PSR J1701-3006D,E,F C1658m300 | Sandler (2003) C1658m300 |---------------------------------------------------------- C1658m300 |Malakhova et al. (1997) listed x,y coordinates and published an ID chart C1658m300 |for 43 "suspected RR Lyrae variables" based on position in the C1658m300 |colour-magnitude diagram. Contreras et al. (2010) confirmed the C1658m300 |variability for 27 of these candidates and found the remaining 16 to be C1658m300 |non-variable in their data. # C1659m262 | V1-V4, F1=V6 (=NSV 20887 in the Moscow GCVS) C1659m262 | Sawyer (1943) with x,y positions and ID chart C1659m262 | The number V6 was assigned by Clement & Sawyer Hogg (1978) C1659m262 | C1659m262 | V5 C1659m262 | announced by Coutts et al. (1975) with x,y position C1659m262 | and ID chart published by Clement & Sawyer Hogg (1978) C1659m262 | V7= SVS 2155 C1659m262 | Samus (1976) with ID chart and 1950 RA and dec C1659m262 | The number V7 was assigned by Clement & Sawyer Hogg (1978) C1659m262 | V7 is also V2135 Oph in the Moscow GCVS # C1701m246 | V1-6 and 4 field variables, F1-F4 C1701m246 | Sawyer (1943) with x,y positions and ID chart C1701m246 | V7-12 C1701m246 | Clement et al. (1980) with x,y positions and ID chart for V1-12 C1701m246 | and F1-2. # C1702m226 | V1-3 C1702m226 | Sawyer (1943) with x,y positions and ID chart C1702m226 | V4-9 C1702m226 | These are "candidate" variables announced by Stetson & West C1702m226 | (1994 - Table 4) with x,y positions. C1702m226 | The numbers V4-9 were assigned by Clement et al. (2001) C1702m226 | The SW numbers are listed in the remarks column. # # C1707m265 | V1-3 C1707m265 | Shapley (1920) with x,y positions C1707m265 | V4-5 and 3 field variables, F1-3 C1707m265 | Sawyer (1943) with x,y positions for all of the known variables C1707m265 | and an ID chart for V1-5. Clement et al. (1982) later published C1707m265 | an ID chart for all of these variables except F3 which was outside C1707m265 | their field of view. C1707m265 | V6-8 C1707m265 | Clement et al. (1982) with x,y positions and ID chart C1707m265 | HV 3943 C1707m265 | Woods (1926) with RA, Dec (1900) C1707m265 | An ID chart was published by Swope (1932) and later by Clement et C1707m265 | al. (1982). C1707m265 | HV 4409 = IW Oph C1707m265 | Swope (1928) with RA, Dec (1900) C1707m265 | An ID chart was published by Swope (1932) and later by Clement et C1707m265 | al. (1982). C1707m265 |----------------------------------------------------------------- C1707m265 |Lee & Carney (2006) found 22 blue stragglers, most of which were C1707m265 |centrally concentrated, from a photometric study based on HST VI C1707m265 |data. The time distribution of their observations was not suitable for C1707m265 |detecting variability. # C1711m294 | V1-11 C1711m294 | Rosino (1962) with x,y coordinates and an ID chart C1711m294 | Some of these variables are also in the OGLE III catalogue C1711m294 | (Sosyzynski et al. 2011). C1711m294 | V1, 2, 3, 4, 7, 10 are OGLE-BLG-RRLYR 00247, 00232, 00253, 00225, C1711m294 | 00242, 00201 respectively. C1711m294 | V12-18 = #28, 29, 30, 32, 33, 40, 43 C1711m294 | Terzan (1966) with an ID chart C1711m294 | The numbers V12-18 were assigned by Sawyer Hogg (1973) in her 3rd C1711m294 | catalogue. Terzan announced 58 (V1-58) variables in his paper, but C1711m294 | Sawyer Hogg assigned numbers only to the ones that were located C1711m294 | within approximately 15 arcminutes of the cluster centre. The 2010 C1711m294 | revision of the Harris (1996) catalogue inicates a tidal radius of C1711m294 | 13.25 arcminutes for NGC 6304. C1711m294 | V19-21 = #68, 69, 72 C1711m294 | Terzan (1968) with an ID chart C1711m294 | The numbers V19-21 were assigned by Sawyer Hogg (1973) in her 3rd C1711m294 | catalogue. Terzan announced 25 new variables (V59-83) in his paper, C1711m294 | but Sawyer Hogg assigned numbers only to the ones within 15 C1711m294 | arcminutes of the cluster centre. C1711m294 | V22-23 = #1247 & #4209, suspected variables C1711m294 | Hesser & Hartwick (1976) with ID chart C1711m294 | Their variability was later confirmed by De Lee et al. (2006). C1711m294 | Both stars are included in the OGLE III catalogue of RR Lyrae C1711m294 | variables as OGLE-BLG-RRLYR 00246 and 00237 respectively C1711m294 | The numbers V22 and V23 have been assigned in this on-line C1711m294 | (Sosyzynski et al. 2011). C1711m294 | catalogue. C1711m294 | V24 = NV1 C1711m294 | De Lee et al. (2006) with no ID or coordinates C1711m294 | However, based on the period they derived, this star appears to C1711m294 | be OGLE-BLG-RRLYR-00255 (Sosyzynski et al. 2011). C1711m294 | The number V24 has been assigned in this on-line catalogue. C1711m294 | De Lee et al. included a few other 'new' RR Lyrae variables in C1711m294 | their investigation, but they did not consider any of them C1711m294 | to be possible cluster members. Therefore they are not listed C1711m294 | in the above table. These stars were listed as HBH67, Va46, NV2 C1711m294 | which are the same stars as OGLE-BLG-RRLYR-00256,-00251 and -00238 C1711m294 | respectively (Sosyzynski et al. 2011). # C1713m280 | V1-19 C1713m280 | Layden et al. (2003) with pixel numbers # C1714m237 |V1-2 C1714m237 | Matsunaga et al. (2006) with RA and dec # C1715p432 |V1-14 C1715p432 | Hachenberg (1939) with x,y positions and numbers from the Hopman C1715p432 | (1930) catalogue. C1715p432 | Hachenberg noted that these variables had been previously discovered C1715p432 | by Woods (1922) and Guthnick & Prager (1925). C1715p432 | Woods announced the discovery and published x,y coordinates for the C1715p432 | variable now known as V11. Guthnick & Prager (1925) announced that C1715p432 | they had discovered 13 variables in M92, but did not publish any C1715p432 | positions. The numbers V1-14 were assigned by Hachenberg. C1715p432 | Most of these variables were independently discovered by Nassau (1938) C1715p432 | who published an ID chart. However, the Nassau and Hachenberg numbering C1715p432 | systems were different. Sawyer (1939, 1955) adopted Hachenberg's C1715p432 | (1939) system in her catalogues. A table with cross correlations between C1715p432 | the different numbering systems was published by Kadla et al. (1983). C1715p432 |V15 = V12 of Nassau (1938) who labelled it on a chart C1715p432 | The number V15 was assigned by Sawyer Hogg (1973) in her 3rd C1715p432 | catalogue. In her first two catalogues (Sawyer 1939, 1955), she C1715p432 | designated this star as V16 and Nassau's V10 was designated as V15. C1715p432 | Bartolini et al. (1968) later discovered that Nassau's V10 C1715p432 | was the same star as Hachenberg's V12. Sawyer (1939, 1955) had not C1715p432 | realized this because the x coordinate Hachenberg (1939) published C1715p432 | for his V12 was incorrect. C1715p432 |V16-17 = Nassau's (1938) suspected variables V15-16 which he labelled C1715p432 | on an ID chart. Their x,y coordinates were derived by Kadla et al. C1715p432 | (1983) and the numbers V16-17 were later assigned by Clement et al. C1715p432 | (2001) in accordance with the system established by Kadla et al. C1715p432 | (1983). C1715p432 | C1715p432 |V18-28 C1715p432 | Kadla et al. (1983) with x,y coordinates and an ID chart C1715p432 | They also published a table with cross correlations between the C1715p432 | numbering systems of Sawyer (1939,1955), Sawyer Hogg (1973) and C1715p432 | Nassau (1938) for V1-17. C1715p432 |V29-34 C1715p432 | Kopacki (2001) with x,y coordinates and an ID chart C1715p432 |V35-39 C1715p432 | Kopacki (2007) with RA, dec and ID chart C1715p432 | Kopacki also provided ID for 3 blue stragglers suspected of C1715p432 | variability. C1715p432 |---------------------------------------------------------------- C1715p432 |Walker (1955) suspected that three stars near the RG tip might be C1715p432 |variable, but Welty (1985) did not detect any variablility with B C1715p432 |amplitude greater than 0.2 mag for any of them. C1715p432 |---------------------------------------------------------------------- C1715p432 |Shara et al. (1994) surveyed the cluster for erupting dwarf novae but C1715p432 |did not detect any; they established an upper limit based on their C1715p432 |results. Tuairisg et al. (2003) later announced a possible dwarf nova C1715p432 |candidate. C1715p432 |----------------------------------------------------------------------- C1715p432 |Lynch & Ransom (2011) conducted a search for pulsars, but did not find C1715p432 |any in M92. # C1716m184 | V1 C1716m184 | Shapley (1916) with delta RA and delta dec C1716m184 | The number V1 was assigned by Sawyer (1951) who included it in her C1716m184 | ID chart and derived its x,y coordinates. C1716m184 | V2-13 C1716m184 | Sawyer (1951) with x,y coordinates and an ID chart C1716m184 | V14-21 C1716m184 | Clement & Shelton (1996) with x,y coordinates and an ID chart C1716m184 | V22-34 C1716m184 | Arellano Ferro et al. (2013) with RA, dec and ID charts C1716m184 | These authors published RA, dec and ID charts for all of the C1716m184 | variables. # C1720m177 | V1-5, F1=V6 C1720m177 | Sawyer, JRASC 47, 229 (1953) with x,y positions and ID chart C1720m177 | for V1-5 C1720m177 | Sawyer Hogg (1973) assigned the number V6 to F1 in her 3rd C1720m177 | catalogue and an ID chart for V6 was published by Clement & C1720m177 | Sawyer Hogg (1977). C1720m177 | In the Moscow GCVS, V5 and V6 are listed as V2009 and V1995 Oph C1720m177 | respectively.. C1720m177 | V7-10 C1720m177 | Lloyd Evans & Menzies (1973) who identify them as stars 34, 72, C1720m177 | 30 and 46 of Sandage & Wallerstein (1960 - see Fig 2) C1720m177 | Sandage & Wallerstein (1960) also labelled V1 and V3 in Fig.2 and C1720m177 | V2, V4 and V5 in Fig. 1 of their paper. # C1720m263 | V1-5 = OGLE-BLG-RRLYR-17494, OGLE-BLG-RRLYR-17497, C1720m263 | OGLE-BLG-RRLYR-17501, OGLE-BLG-RRLYR-17508, C1720m263 | OGLE-BLG-RRLYR-17516 C1720m263 | from the OGLE IV survey (Soszynski et al. 2014) with RA and dec C1720m263 | These variables have magnitudes and colours appropriate for C1720m263 | cluster membership according to the CM diagram published by C1720m263 | Ortolani et al. (2003). # C1721m484 | V1-3 = FL 1, 4, 8 C1721m484 | Fourcade & Laborde (1966) with x,y positions and ID chart C1721m484 | Sawyer Hogg in her 3rd catalog assigned the numbers V1-3 and C1721m484 | stated that FL 2, 3, 5, 6, 7, 9-12 are considered field stars. C1721m484 | V4-5 C1721m484 | Lloyd Evans & Menzies (1973) C1721m484 | V4=HH113 of Hartwick & Hesser (1972) C1721m484 | V5=L36 identified in chart by Lloyd Evans & Menzies (1977) C1721m484 | The number V4 was assigned by Sawyer Hogg (1973). At that time, C1721m484 | L36 was considered to be a field star, but after Lloyd Evans & C1721m484 | Menzies (1977) classified it as a probable member, it was assigned C1721m484 | the number V5 in our electronic catalogue (Clement et al. 2001). C1721m484 | V6 = star E of Hartwick & Hesser, ApJ 175, 77 (1972) C1721m484 | with variability announced by Hesser (1980, IBVS 1758) C1721m484 | The number V6 was assigned in our electronic catalogue (Clement et C1721m484 | al. 2001). # C1725m050 | V1-2 C1725m050 | Sawyer (1940) with x,y positions and ID chart C1725m050 | V3-8 C1725m050 | Arellano Ferro et al. (2008) with positions labelled on an C1725m050 | ID chart. The RA and dec were later derived by Arellano Ferro C1725m050 | (2014- private communication). C1725m050 | These authors also identified a number of candidate variables: C1725m050 | C1-C7 - possible long period variables or Cepheids - the C1725m050 | timing of their observations was not suitable for confirming C1725m050 | this. C1725m050 | C8-11 - short period variables that could be eclipsing binaries C1725m050 | of the W UMa type. # C1726m670 | V1-15 C1726m670 | Woods (1919) with x,y coordinates C1726m670 | According to Shapley (1930), Woods discovered 17 variables in C1726m670 | NGC 6362, but it appears that 2 were unpublished and there is no C1726m670 | further information about them. In the 3rd catlogue, Sawyer Hogg C1726m670 | (1973) mentioned a field variable announced by Shapley (1922) C1726m670 | V16-31 C1726m670 | van Agt (1961) with x,y coordinates and an ID chart for all C1726m670 | of V1-31 (except V4 and V9). van Agt also made small revisions to C1726m670 | some of the x,y coordinates derived by Woods (1919) C1726m670 | V32 C1726m670 | Fourcade et al. (1966) with x,y coordinates and ID chart for V1-32 C1726m670 | V33 = VH 11 C1726m670 | van Hoof (1961) with x,y coordinates and an ID chart C1726m670 | The number V33 was assigned by Sawyer Hogg (1973) in her 3rd C1726m670 | catalogue. van Hoof announced the discovery of seven other C1726m670 | variables, but these were all independently discovered by van Agt C1726m670 | (1961) so Sawyer Hogg adopted van Agt's numbering system for her C1726m670 | catalogue. However, all of the epochs, periods and magnitudes listed C1726m670 | for the NGC 6362 variables in her 3rd catalogue were from van Hoof's C1726m670 | paper. C1726m670 | V34-52 C1726m670 | Mazur et al. (1999) with RA, dec and individual finder charts C1726m670 | They also discovered a hot subdwarf with V=19.1, V-I=-0.24, C1726m670 | B-V=-0.28 at RA=17:31:46.3, dec=-67:05:03 (2000) which Zloczewski et C1726m670 | al. (2012) found to be a probable cluster member based on its proper C1726m670 | motion. C1726m670 |------------------- C1726m670 |Pietrukowicz et al. (2008) searched for dwarf novae in NGC 6362 and C1726m670 |found none. Their search was based on observations made on 104 nights, C1726m670 |spanning 7 years, from 1999 to 2005. # C1727m299 |With L=357.44 and B=2.12, HP1 is located in a rich field near the C1727m299 |Galactic centre. In the 1960s, Terzan undertook a search for variable C1727m299 |stars and discovered more than 250 new ones in the vicinity of HP1 C1727m299 |and the star 45 Ophiuchi. Sawyer Hogg (1973) included the variable stars C1727m299 |that were closest to HP1 in her 3rd catalogue. They are now considered C1727m299 |to be field stars (Samus et al. 2009). C1727m299 | V1-2 = T248-T249 C1727m299 | announced by Terzan (1964) and identified as 248 and 249 on an ID C1727m299 | chart. They were later labelled, along with some of the C1727m299 | other variables, in Figure 6 of Terzan (1966a and 1996b). C1727m299 | The numbers V1 and 2 were assigned by Sawyer Hogg (1973) in her C1727m299 | 3rd catalogue. C1727m299 | V3-6 = T361-T364 C1727m299 | announced by Terzan (1965) and identified as 361, 362, 363, C1727m299 | 364 in Figure 1 of his paper. C1727m299 | The numbers V3 to 6 were assigned by Sawyer Hogg (1973) in her C1727m299 | 3rd catalogue. C1727m299 | V7-10 = T126, T130, T247, T251 C1727m299 | announced by Terzan (1966a and 1966b) and identified as C1727m299 | 126, 130, 247, 250 in Figure 6 of these two papers. C1727m299 | The numbers V7 to 10 were assigned by Sawyer Hogg (1973) in her C1727m299 | 3rd catalogue. C1727m299 | V11-15 = T136, T137, T139, T142, T143 C1727m299 | announced by Terzan (1966a and 1966b) and identified as C1727m299 | 136, 137, 139, 142, 143 in Figure 8 of these two papers. C1727m299 | The numbers V11 to 15 were assigned by Sawyer Hogg (1973) in her C1727m299 | 3rd catalogue. C1727m299 | V16-17 C1727m299 | Matsunaga et al. (2006) with RA and dec C1727m299 |----------------------------------------------------------------------- C1727m299 |Cailliatte (1962a and b) published 1950 RA and dec for 9 red variables C1727m299 |discovered in the vicinity of HP1 and published mean I magnitudes, C1727m299 |amplitudes, periods and spectral types for them (Cailliatte 1964). C1727m299 |They were all classified as Mira variables and probably belong to the C1727m299 |galactic field. C1727m299 | # 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 |V1-4 C1732m304 | Terzan & Rutily (1975) with x,y coordinates and an ID chart C1732m304 | According to the VizieR Service, V3 and 4 are listed in the catalogue C1732m304 | of VISTA Variables in the Via Lactea Survey DR1 (Minniti et al. 2014), C1732m304 | as VVVJ1173553.42-302921.63 and VVVJ173555.19-302948.42 respectively. C1732m304 | No periods have yet been published by the VISTA group. C1732m304 |V5 C1732m304 | Matsunaga et al. (2006) with RA and dec C1732m304 |V6-17 = OGLE-BLG-RRLYR-22087, OGLE-BLG-RRLYR-22095, C1732m304 | OGLE-BLG-RRLYR-22102, OGLE-BLG-RRLYR-22104, C1732m304 | OGLE-BLG-RRLYR-22107, OGLE-BLG-RRLYR-22108, C1732m304 | OGLE-BLG-RRLYR-22112, OGLE-BLG-RRLYR-22118, C1732m304 | OGLE-BLG-RRLYR-22135, OGLE-BLG-RRLYR-22139, C1732m304 | OGLE-BLG-RRLYR-22170, OGLE-BLG-RRLYR-22196 C1732m304 | These are RR Lyrae variables in the Galactic Bulge detected C1732m304 | in the OGLE investigations and discussed by Soszynski et al. C1732m304 | (2014). C1732m304 | The catalog is available from the following website- C1732m304 | ftp://ftp.astrouw.edu.pl/ogle/ogle4/OCVS/blg/rrlyr/ C1732m304 | These variables are located with 1.4 arcminutes of the cluster C1732m304 | centre based on Harris's 2003 position. There are an additional C1732m304 | 11 RR Lyrae variables located between 1.4 and the half light C1732m304 | radius, 3.82 arcminutes: C1732m304 | 21979, 22033, 22042, 22051, 22063, 22199, 22205, 22228, 22234, C1732m304 | 22246, 22258. # C1732m447 | V1-9 = C1732m447 | V1-4, V6-8, V10-11 of Lloyd Evans & Menzies (1973) C1732m447 | who labelled them on an ID chart. The numbering system C1732m447 | V1-9 was assigned by Sawyer Hogg (1973) in her 3rd catalogue. C1732m447 | C1732m447 | V10-12 C1732m447 | Lloyd Evans & Menzies (1977) with an ID chart for V1-12 C1732m447 | V13-26 C1732m447 | Hazen & Hesser (1986) with x,y coordinates and an ID chart for C1732m447 | V3-V26. (V1 and V2 were too close to the centre on their C1732m447 | photographs.) Hazen & Hesser also discovered 4 field variables C1732m447 | that they numbered F1-4. C1732m447 | V27-29 C1732m447 | Silbermann et al. (1994) with x,y coordinates and ID charts C1732m447 | They also announced 4 suspected variables, three of which, S1-3, C1732m447 | were later confirmed by Pritzl et al. (2002) and numbered V32, V49 C1732m447 | and V53. Pritzl et al. were unable to find any variation in S4, C1732m447 | but noted that crowding might have been an issue. However, no C1732m447 | variation was detected by Corwin et al. when they applied the image C1732m447 | subtraction technique to the observations. C1732m447 | V30-57 C1732m447 | Pritzl et al. (2002) with x,y in pixels and arcsec, and ID charts C1732m447 | V58-69 C1732m447 | Corwin et al. (2006) with x,y coordinates in arcsec C1732m447 | These authors also published data for six "suspected" variables C1732m447 | which they numbered SV1-SV6. C1732m447 | V70-73 = SV1, SV2, SV4, SV5 of Corwin et al. (2006) C1732m447 | The numbers V70-73 were assigned by Skottfelt et al. (2015) C1732m447 | confirmed their variability, derived RA and dec and published C1732m447 | a finding chart. C1732m447 | C1732m447 | V74-121 C1732m447 | Skottfelt et al. (2015) with RA, dec and a finding chart. C1732m447 |------------------------------------------------------------------------- C1732m447 |Dalessandro et al. (2008) identified a substantial population of BS C1732m447 |stars from HST observations, but they did not search for variability in C1732m447 |their data. # C1733m390 | V1-2 C1733m390 | Fourcade et al. (1966) with x,y positions and ID chart C1733m390 | The RA and dec were derived by Samus et al. (2009) who commented C1733m390 | that V2 is very red. # C1735m032 | V1-72 C1735m032 | Sawyer (1938) with x,y positions and an ID chart (but V27&28 were C1735m032 | outside the field of the chart). C1735m032 | V73-76 C1735m032 | Sawyer Hogg & Wehlau (1966) with x,y positions and an ID chart C1735m032 | V77-88 C1735m032 | Wehlau & Potts (1972) with x,y positions C1735m032 | V89-93 C1735m032 | Wehlau et al. (1974) with x,y positions C1735m032 | Nova C1735m032 | Sawyer Hogg & Wehlau (1964) with x,y position and ID chart # C1735m238 | V1 = star #41 of Terzan & Rutily (1972) who published 1950 RA & dec C1735m238 | and an ID chart. It is also NSV 09335 in the GCVS. C1735m238 | The number V1 was assigned by Sawyer Hogg (1973). C1735m238 | In their discovery paper, Terzan & Rutily announced the discovery C1735m238 | of 102 variables, but most were considered to belong to the rich C1735m238 | field surrounding the cluster. C1735m238 | V2-3 = stars #157 and #164 of Terzan & Rutily (1973) C1735m238 | who published 1950 RA & dec and an ID chart C1735m238 | The numbers V2-3 were assigned by Sawyer Hogg (1973). C1735m238 | In their paper, Terzan & Rutily announced the discovery of C1735m238 | 115 variables which they numbered #103 to #217. Most were C1735m238 | considered to belong to the rich field surrounding the cluster. C1735m238 | V4-25 C1735m238 | Terzan & Rutily (1975) with x,y coordinates and an ID chart C1735m238 | On the chart, these stars were labelled #218 to #239 respectively. C1735m238 | and the other variables (V1, 2, 3 = stars #41, 157 and 164) C1735m238 | were also labelled. No magnitudes or periods were published. C1735m238 | V26-37 C1735m238 | Tsapras et al. (2017) with RA, dec, ID chart and individual finder C1735m238 | charts C1735m238 | These are all RR Lyrae variables that are located within 2.4 C1735m238 | arcminutes of the cluster centre (the radius designated by C1735m238 | Soszynski et al. 2014). Tsapras et al. also published data for C1735m238 | 17 additional RR Lyrae that were located beyond 2.4 arcminutes. C1735m238 | On the OGLE IV website (Soszynski et al. 2014), data are listed C1735m238 | for 33 RR Lyrae variables located at distances between 2.4 C1735m238 | arcminutes and the tidal radius (12.24 arcminutes). C1735m238 | V38-40 (=LPV1, LPV3, LPV12) C1735m238 | Tsapras et al. (2017) with RA, dec, ID chart and individual finder C1735m238 | charts C1735m238 | The numbers V38-40 have been assigned in this catalogue. C1735m238 | Tsapras et al. discovered 12 long period variables (LPV1-12), but C1735m238 | only these three are located within 2.4 arcminutes of the cluster C1735m238 | centre, their designated cluster radius. C1735m238 | C1735m238 | V41-54 C1735m238 | V41 = OGLE-BLG-ECL-051686, V42 = OGLE-BLG-ECL-051718 C1735m238 | V43 = OGLE-BLG-ECL-051888, V44 = OGLE-BLG-ECL-052111 C1735m238 | V45 = OGLE-BLG-ECL-052212, V46 = OGLE-BLG-ECL-052246 C1735m238 | V47 = OGLE-BLG-ECL-052291, V48 = OGLE-BLG-ECL-052324 C1735m238 | V49 = OGLE-BLG-ECL-052388, V50 = OGLE-BLG-ECL-052772 C1735m238 | V51 = OGLE-BLG-ECL-052829, V52 = OGLE-BLG-ECL-052850 C1735m238 | V53 = OGLE-BLG-ECL-052984, V54 = OGLE-BLG-ECL-053107 C1735m238 | Soszynski et al. (2016) with RA and dec (OGLE IV Galactic Bulge C1735m238 | survey) C1735m238 | The numbers V41-54 have been assigned in this catalogue. C1735m238 | These 14 binary systems are located within 2.4 arcminutes of C1735m238 | the cluster centre, the radius that Soszynski et al. (2014) C1735m238 | listed for NGC 6401. (They were all to faint to be detected C1735m238 | by Tsapras et al.) C1735m238 | In addition to these 14 stars, the OGLE IV website lists data for C1735m238 | 333 other eclipsing binaries that are located within the tidal C1735m238 | radius of NGC 6401 (12.24 arcminutes). # C1736m536 | V1&2 (=V639 and V825 Ara) C1736m536 | Bailey (1902) with x,y coordinates (page 241) and an ID chart C1736m536 | (Plate XI, Fig. 2, caption on page 250) C1736m536 | Bailey (1923) published data for 4 additional variables in the C1736m536 | surrounding field. C1736m536 | V3 C1736m536 | Swope (unpublished correspondence with Sawyer) C1736m536 | The number V3 was assigned by Sawyer (1955) in her 2nd C1736m536 | catalogue where she published the x,y coordinates C1736m536 | V3 is considered to be a field star and is designated as V826 Ara C1736m536 | in the Moscow GCVS. C1736m536 | V4-11 C1736m536 | Kaluzny (1997) with RA and dec, as well as X,Y pixel numbers C1736m536 | that refer to a template image that they submitted to the data C1736m536 | centre at Strasburg. V10 is BS#11 that was identified by C1736m536 | Lauzeral et al. (1992). C1736m536 | El-Worfaly & Budding (1983) discussed and identified a variable C1736m536 | which they called V4. It is a different star and is considered to C1736m536 | be a field star based on its distance from the cluster. It is C1736m536 | listed as V826 Ara in the Moscow GCVS. C1736m536 | V12-13 C1736m536 | Kaluzny & Thompson (2003) with RA, dec and X,Y pixel numbers C1736m536 | that refer to an HST archival image C1736m536 | These two variables are the optical counterparts to CV1 and CV6, C1736m536 | candidate cataclysmic variables detected by Grindlay et al. C1736m536 | (2001) with the Chandra telescope. C1736m536 | V14-24 C1736m536 | Kaluzny & Thompson (2003) with RA, dec and X,Y pixel numbers C1736m536 | that refer to an HST archival image for V14-21. V22 and V23 C1736m536 | are BS#8 and BS#16 that were identified by Lauzeral et al. (1992). C1736m536 | V25-36 C1736m536 | Kaluzny et al. (2006) with RA, dec C1736m536 | They published finding charts for most of these variables C1736m536 | and for the others (V31, V33 and V34) they cited sources C1736m536 | where the charts can be located (see page 549). C1736m536 | C1736m536 |------------------------------------------------------ C1736m536 |In an investigation to detect planetary transits among low main C1736m536 |sequence stars in NGC 6397, Nascimbeni et al. (2012) identified C1736m536 |12 new variable stars. All of them were considered to be C1736m536 |field stars, based on the proper motions and position in the CM C1736m536 |diagram. # C1742p031 | V1-10 + a field variable C1742p031 | Baade in an unpublished letter to Sawyer (1939) C1742p031 | The numbers V1-11 were assigned and x,y coordinates were derived C1742p031 | by Sawyer (1955). C1742p031 | The field variable V11 is V979 Oph in the Moscow GCVS. C1742p031 | V12-13 + 3 field variables C1742p031 | Grubissich (1958) with x,y coordinates and an ID chart for V1-13 C1742p031 | V14-16 C1742p031 | Papadakis et al. (2000) with X,Y in pixels and an ID chart for V1-16 # C1745m247 | V1-2 = V and V_S C1745m247 | Spinrad et al. (1974) who labelled the stars on an ID chart C1745m247 | The numbers V1 and V2 were assigned by Clement (1997) in the C1745m247 | first electronic update of the Sawyer Hogg (1973) catalogue. C1745m247 | V3-4 = V1 and V2 of Edmonds et al. (2001) C1745m247 | who published RA, dec and finder charts C1745m247 | The numbers V3 and V4 were assigned by Clement et al. (2001). C1745m247 | V5-9 C1745m247 | Sloan et al. (2010) who published RA and dec C1745m247 |---------------------------------------------------------------------- C1745m247 | PSR: According to Paulo Freire's website (July 2016), there C1745m247 | are 34 millisecond pulsars in Terzan 5. C1745m247 | (www.naic.edu/~pfreire/GCpsr.html) # C1746m370 | V1-10 C1746m370 | Fourcade et al. (1966) with x,y coordinates and an ID chart C1746m370 | V7 and V8 have not been studied in subsequent investigations of C1746m370 | NGC 6441 because they were outside the field of view. Both are C1746m370 | considered to be field stars because they are outside the tidal C1746m370 | radius. C1746m370 | V11-12 = star #4427 and 4323 (suspected RR Lyrae variables) C1746m370 | Hesser & Hartwick (1976) with ID chart C1746m370 | The numbers V11 and V12 were assigned by Clement (1997) in C1746m370 | the first electronic update of the Sawyer Hogg (1973) catalogue. C1746m370 | Layden et al. (1999) did not confirm their variability. C1746m370 | V13-50 C1746m370 | Layden et al. (1999) with X,Y pixel numbers and individual finder C1746m370 | charts C1746m370 | Their observations were made on 3 nights in May and 8 nights in C1746m370 | June 1996. As a result, they were able to identify many long C1746m370 | period variables in their field, but they could not derive their C1746m370 | periods. Some of these long period variables were included in the C1746m370 | Ogle III catalog of long period variables in the Galactic Bulge C1746m370 | (Soszynski et al. 2013) and for those stars, the Ogle data are C1746m370 | listed in the above table. C1746m370 | C1746m370 | Layden et al. also published finder charts for 9 suspected variables C1746m370 | SV1-9. Pritzl et al. (2001) found that SV1-5 and SV8 were variable C1746m370 | and numbered them V68, V69, V80, V70, V71 and V51 respectively. C1746m370 | SV9 was outside their field of view and they did not detect any C1746m370 | variation in SV6 or SV7. However, in a later paper (Pritzl et al. C1746m370 | 2003), they discovered that SV7 was a long period variable and C1746m370 | assigned the number V105. C1746m370 | V51-104 C1746m370 | Pritzl et al. (2001) with x,y coordinates and ID charts C1746m370 | They concluded that most of the binaries they discovered were not C1746m370 | likely to be members of the cluster. C1746m370 | Pritzl et al. also derived properties of 6 suspected variables which C1746m370 | they numbered SV10-15 and labelled on finding charts. C1746m370 | In a later study, Pritzl et al. (2003) confirmed the variability of C1746m370 | SV14 and SV15 and assigned the numbers V106 and V140 respectively. C1746m370 | V105-145 C1746m370 | Pritzl et al. (2003) with RA, dec and individual finder charts C1746m370 | V146-150 C1746m370 | Corwin et al. (2006) with RA, dec C1746m370 | V151-199 C1746m370 | Skottfelt et al. (2015) with RA, dec and a finding chart C1746m370 |------------------------------------------------------------------- C1746m370 | PSR: According to Paulo Freire's website, there are 4 pulsars C1746m370 | in NGC 6441. (www.naic.edu/~pfreire/GCpsr.html) C1746m370 |-------------------------------------------------------------------- C1746m370 | U1 - the probable optical counterpart to the X-ray burster X1746-370 C1746m370 | (4U 1746-37) according to Homer et al. (2002) who published its RA C1746m370 | and dec. They concluded that it is probably an LMXB with a period C1746m370 | of 5.73 hours. C1746m370 |-------------------------------------------------------------------- C1746m370 |Alonso-Garcia et al. (2013) announced that the VVV is surveying C1746m370 |the central regions of the Milky Way at near-infrared wavelengths to C1746m370 |look for variable stars, especially RR Lyrae, in globular clusters. C1746m370 |NGC 6441 is one of the clusters in their study. # C1748m346 |V1-2 C1748m346 | Matsunaga et al. (2006) with RA and dec C1748m346 | V1 is also OGLE-BLG-T2CEP-342 and C1748m346 | V2 is OGLE-BLG-T2CEP-102 = V0708 Sco C1748m346 | of Soszynski et al. (2011b) in the OGLE III Catalogue of Type II C1748m346 | Cepheids in the Galactic Bulge C1748m346 | Soszynski et al. (2011b) identified another RV Tauri star and a C1748m346 | Type II Cepheid, located at distances of 11.7 and 15.0 arcminutes C1748m346 | respectively, from the cluster centre, within the tidal radius, C1748m346 | 15.8 arcminutes. C1748m346 |V3-4 = OGLE-BLG-RRLYR-04365 (NGC6453 V1) and C1748m346 | OGLE-BLG-RRLYR-04337 (NGC6453 V2) of C1748m346 | Soszynski et al. (2011a) in the OGLE III Catalogue of RR Lyrae C1748m346 | variables in the Galactic Bulge C1748m346 | The numbers V3-4 have been assigned in this catalogue. C1748m346 |V5-12 = OGLE-BLG-RRLYR-04284, OGLE-BLG-RRLYR-04326, C1748m346 | OGLE-BLG-RRLYR-04341, OGLE-BLG-RRLYR-04458, C1748m346 | OGLE-BLG-RRLYR-30442, OGLE-BLG-RRLYR-30454, C1748m346 | OGLE-BLG-RRLYR-30460, OGLE-BLG-RRLYR-30506 C1748m346 | of Soszynski et al. (2014) from the their study of RR Lyrae variables C1748m346 | in the Galactic bulge. C1748m346 | The numbers V5-12 have been assigned in this catalogue. C1748m346 | Soszynski et al. (2014) identified 39 additional RR Lyrae variables C1748m346 | that are located beyond 3.8 arcminutes from the cluster centre C1748m346 | and inside the tidal radius, 15.8 arcminutes. C1748m346 |-------------------------------------------------------------------- C1748m346 |The OGLE III catalogue (Soszynski et al. 2013) also includes C1748m346 |approximately 50 Long Period variables in the vicinity of the cluster. C1748m346 |Many of them seem too faint, but some might be associated with the cluster. C1748m346 |-------------------------------------------------------------------- C1748m346 |According to the VizieR Service, many of the variables are also C1748m346 |listed in the catalogue of VISTA Variables in the Via Lactea Survey C1748m346 |DR1 (Minniti et al. 2014), but no periods have been published by C1748m346 |the VISTA group. # C1755m442 |V1-13: Abbas et al. (2015) with RA, dec and ID charts C1755m442 | Abbas et al. also investigated star ASAS 175901-4411.5 C1755m442 | (Pojmanski & Maciejewski 2004) which was in their field of C1755m442 | view, at a projected angular distance of 4.4 arcmin from the C1755m442 | cluster centre. They concluded that it was too bright to be C1755m442 | a cluster member. # C1758m278 |V1-7 = OGLE-BLG-RRLYR-11141, OGLE-BLG-RRLYR-11190, C1758m278 | OGLE-BLG-RRLYR-11215, OGLE-BLG-RRLYR-11218, C1758m278 | OGLE-BLG-RRLYR-11223, OGLE-BLG-RRLYR-11125, C1758m278 | OGLE-BLG-RRLYR-11257 C1758m278 | Soszynski et al. (2011) in the OGLE III Catalogue of RR Lyrae C1758m278 | variables in the Galactic Bulge C1758m278 | Their RA and dec are listed by the Vizier Service. C1758m278 | These variables have mean =16.363 and mean =17.954 mag. C1758m278 |Soszynski et al. (2014) identified 10 additional RR Lyrae variables that C1758m278 |are located within 5 arcminutes of the cluster centre: BLG-RRLYR-11044, C1758m278 |11049, 11060, 11075, 11137, 11142, 11249, 11252, 11372, 11376. C1758m278 |Most of these additional variables have mean magnitudes that indicate C1758m278 |they are probably in the cluster foreground or beyond the cluster. # C1800m260 | V1-48 = NV1-NV48 C1800m260 | Alonso-Garcia et al. (2015) with RA, dec and an ID chart C1800m260 | These variables all lie inside the tidal radius which is 5.06 C1800m260 | arcminutes according to the 2010 update to the Harris (1996) C1800m260 | catalogue. C1800m260 | In their investigation, Alonso-Garcia et al. discovered an additional C1800m260 | 112 variables outside the tidal radius. They numbered them NV49 to C1800m260 | NV160 and considered them all to be field variables. C1800m260 | V49-52 = OGLE_BLG_RRLYR-33518, OGLE_BLG_RRLYR-33521, C1800m260 | OGLE_BLG_RRLYR-33525, OGLE_BLG_RRLYR-33542 C1800m260 | These 4 variables and their RA and dec were announced in the C1800m260 | OGLE-IV survey (Soszynski et al. 2014). They all lie within C1800m260 | 5 arcminutes of the centre of Terzan 10. C1800m260 | An additional RR1 variable, OGLE_BLG_RRLYR-33551 is located 3.24 C1800m260 | arcminutes from the cluster centre, but appears too bright C1800m260 | (I=17.499) to be a cluster member. C1800m260 | In their survey, Soszynski et al. 2014 also recovered all (except C1800m260 | V5) of the RR Lyrae variables announced by Alonso-Garcia et al. C1800m260 | (2015). # C1800m300 | V1-9 = Gaposchkin # 222, 133, 44, [170?*], 37, 247, 172, 27, 232 C1800m300 | labelled on a photograph published by Gaposhkin (1955) who C1800m300 | also listed their 1900 RA and dec. C1800m300 | Sawyer (1955) assigned the numbers V1-9 and published x,y C1800m300 | coordinates in consultation with Baade (private correspondence). C1800m300 | In his correspondence with Sawyer (1955), Baade also indicated that C1800m300 | V7, V8 and V9 were field stars. Therefore they are listed in the C1800m300 | GCVS as V3900, V1437, V1438 Sgr respectively. However, these three C1800m300 | stars are now considered to be probable cluster members. C1800m300 | *Gaposchkin #170 (V4): Sawyer (1955, 1973) published the correct C1800m300 | x,y coordinates for this star. However, it was incorrectly C1800m300 | labelled on Gaposchkin's (1955) plate and this caused confusion C1800m300 | in subsequent studies. Authors assumed that the star labelled as C1800m300 | #170 by Gaposchkin (1955) was V4. He labelled the star correctly C1800m300 | in a later paper (Gaposchkin 1956), on a hand drawn finder chart, C1800m300 | but the chart was difficult to decipher. C1800m300 | V10-11 = OGLE-BLG-RRLYR-12115, OGLE-BLG-RRLYR-12114 C1800m300 | identified by RA and dec in the Ogle III survey C1800m300 | (Soszynski et al. 2011a) who assigned the numbers V10-11. C1800m300 | V12 = Blanco (1984) #54 = V4113 Sgr = OGLE-BLG-RRLYR-12072 C1800m300 | Blanco published RA and dec (Epoch 1950) and an ID plate. C1800m300 | The number V12 has been assigned in this catalogue. C1800m300 | V13 = OGLE-BLG-RRLYR-12108 C1800m300 | identified by RA and dec in the Ogle III survey C1800m300 | (Soszynski et al. 2011a). The number V13 has been assigned in C1800m300 | this catalogue. C1800m300 | V14 = OGLE-BLG-RRLYR-33606 C1800m300 | identified by RA and dec in the Ogle IV survey C1800m300 | (Soszynski et al. 2014). The number V14 has been assigned in C1800m300 | this catalogue. C1800m300 | ---------------------------------- C1800m300 | There are 5 additional RR Lyrae that have V and I magnitudes C1800m300 | appropriate for cluster membership and are located beyond 2 C1800m300 | arcminutes and within 4 arcminutes of the cluster centre: C1800m300 | OGLE-BLG-RRLYR-11972 = V1416 Sgr = Gaposchkin #46 (r=3.9') C1800m300 | OGLE-BLG-RRLYR-11993 = V1418 Sgr = Gaposchkin #50 (r=3.4') C1800m300 | OGLE-BLG-RRLYR-12032 = V1426 Sgr = Gaposchkin #45 (r=2.4') C1800m300 | OGLE-BLG-RRLYR-12044 = V1427 Sgr = Gaposchkin #51 (r=3.8') C1800m300 | OGLE-BLG-RRLYR-12185 (r=2.9') C1800m300 | OGLE-BLG-RRLYR-33568 (r=3.8') C1800m300 | --------------------------------------- C1800m300 | V15 = OGLE-BLG-T2CEP-284 C1800m300 | identified by RA and dec in the OGLE III Catalogue of C1800m300 | Type II Cepheids in the Galactic Bulge (Soszynski et al. 2011b) C1800m300 | The number V15 has been assigned in this catalogue. C1800m300 |---------------------------------------------------------------------- C1800m300 | In the OGLE III survey of Long period Variables in the Galactic C1800m300 | Bulge, Soszynski et al. (2013) identified eight long period C1800m300 | variables within 2 arcminutes of the cluster centre and with C1800m300 | less than 14.5 mag. Some of these might be cluster members: C1800m300 | OGLE-BLG-LPV-193749 (r=1.31') SRV =V5466 Sgr C1800m300 | OGLE-BLG-LPV-194243 (r=0.13') OSARG C1800m300 | OGLE-BLG-LPV-194274 (r=0.23') OSARG C1800m300 | OGLE-BLG-LPV-194290 (r=0.23') OSARG C1800m300 | OGLE-BLG-LPV-194311 (r=0.29') OSARG C1800m300 | OGLE-BLG-LPV-194316 (r=1.02') OSARG C1800m300 | OGLE-BLG-LPV-194544 (r=0.84') OSARG C1800m300 | OGLE-BLG-LPV-194566 (r=1.49') OSARG C1800m300 |-------------------------------------------------------------------- C1800m300 | PSR: According to Paulo Freire's website, there are 3 millisecond C1800m300 | pulsars in NGC 6522. (www.naic.edu/~pfreire/GCpsr.html) # C1801m003 | V1 = MO Ser C1801m003 | Sawyer (1953) with x,y coordinates and an ID chart C1801m003 | V2 = MP Ser C1801m003 | Liller & Clement (1977) with x,y coordinates and an ID chart C1801m003 | on which both V1 and V2 were labelled. C1801m003 |---------------------------------------------------------------------- C1801m003 |Liller (1980) noted that star #41 (identified on an ID chart) might be C1801m003 |variable. It lies near the RG tip in the CM diagram. # C1801m300 | V1-7 C1801m300 | Skottfelt et al. (2015) with RA, dec and a finding chart C1801m300 | V3 and V4 (Ogle #13921 and #13923 respectively) were C1801m300 | independently discovered by Soszynski et al. (2013) in the C1801m300 | Ogle III investigation of long period variables in the Galactic C1801m300 | Bulge. # C1802m075 | V1-11 = variables announced by C1802m075 | Baker et al. (2007) with RA & dec from 2MASS identifications C1802m075 | The numbers V1-11 have been assigned in this catalogue. Baker's C1802m075 | numbers are listed in the remarks column. C1802m075 | Baker et al. also announced two additional variables: #14, a long C1802m075 | period variable, and #607, an RR Lyrae. They concluded that C1802m075 | neither is a cluster member so they are not listed in the above C1802m075 | table. Furthermore, Layden (private communication, 2015) noted C1802m075 | that he was uncertain about the variability of #14. It was so C1802m075 | bright that there may have been saturation or liniarity issues C1802m075 | with the CCD. C1802m075 | PSR: According to Paulo Freire's website, there is a millisecond C1802m075 | pulsar in NGC 6539. (www.naic.edu/~pfreire/GCpsr.html) C1802m075 |------------------------------------------------------------------ C1802m075 |In her early catalogues, Sawyer (1939, 1955) noted that Baade had C1802m075 |discovered one variable on Mount Wilson plates, but no further C1802m075 |information was provided about the star. # C1802m277 | V1-3 = OGLE-BLG-RRLYR-13297, OGLE-BLG-RRLYR-13300, C1802m277 | OGLE-BLG-RRLYR-13306 C1802m277 | identified by RA and dec in the OGLE III survey (Soszynski et al. C1802m277 | 2011a). The numbers V1-3 have been assigned in this catalogue. C1802m277 |---------------------------------------------------------------------- C1802m277 |The OGLE III investigation of the Galactic Bulge also included C1802m277 |catalogues of Type II Cepheids (Soszynski et al 2011b) and Long Period C1802m277 |variables (Soszynski et al. 2013). In these surveys, no variables were C1802m277 |announced within 0.8 arcminutes of NGC 6540, the radius listed by C1802m277 |Soszynski et al. (2011a). # C1804m250 | V1-2 C1804m250 | Hazen (1993) with x,y coordinates, 1950 RA & dec, and an ID chart C1804m250 | She also identified two field variables: F1 and F2. C1804m250 |--------------------------------------------------------------------- C1804m250 | PSR: According to Paulo Freire's website, there are 2 millisecond C1804m250 | pulsars in NGC 6544. (www.naic.edu/~pfreire/GCpsr.html) # C1804m437 |V1 C1804m437 | Woods, reported by Shapley (1922) with 1900 RA and dec. The C1804m437 | observed range of mpg was from 12.5 to fainter than 16. C1804m437 |V2-8 C1804m437 | Hazen (1994) with ID charts, 1950 RA and Dec and x,y coordinates C1804m437 | V1 was also included in the ID chart. C1804m437 |V9-20 = WUMa1-3, SXP1-9 C1804m437 | Fiorentino et al. (2014) with RA and dec C1804m437 |V21-22 C1804m437 | Figuera Jaimes et al. (2016) # C1806m259 | V1-5 C1806m259 | Thackeray who provided his unpublished x,y coordinates to Sawyer C1806m259 | (1955) C1806m259 | V6-14 = A1, A2, 3, 6, 7, 13, 14, 24, 33 of Lloyd Evans & Menzies (1973) C1806m259 | who labelled them on an ID chart C1806m259 | The numbers V6-14 were assigned by Sawyer Hogg (1973). C1806m259 | C1806m259 | Nova = Nova Sgr 1943 = V1148 Sgr C1806m259 | Mayall (1949) with 1950 RA and dec C1806m259 | Sawyer (1955) listed the x,y coordinates based on information C1806m259 | provided in a letter from A. D. Thackeray and Samus et al. (2009) C1806m259 | later derived the RA and dec (J2000). C1806m259 |--------------------------------------------------------------------- C1806m259 |A search for long period variable stars in NGC 6553 was undertaken C1806m259 |with the PROMPT4 telescope at Cerro Tololo with preliminary results C1806m259 |reported by Kager (2010). Layden and his collaborators have obtained C1806m259 |additional observations and are currently analysing their data. # C1807m317 | V1-9 C1807m317 | Rosino (1962) with x,y coordinates and ID charts C1807m317 | He also provided identifications for 14 variables in the C1807m317 | surrounding field. They were listed as V10-22 and V738 Sgr C1807m317 | V10-15 C1807m317 | Hazen (1996) with x,y coordinates and an ID chart C1807m317 | Hazen also identified V1-9. C1807m317 | Hazen's V10-15 were NOT the stars that were listed as V10-15 by C1807m317 | Rosino (1962) because his were considered to be field stars. C1807m317 | V1-15 all lie within 6.3 arcminutes of the cluster centre, which C1807m317 | was assumed to be the tidal radius when Hazen published her paper. C1807m317 | Hazen also announced discovery of 36 new variables in the field C1807m317 | around the cluster with x,y coordinates and ID chart. In addition, C1807m317 | 11 of Rosino's 14 field variables were in the field of Hazen's C1807m317 | investigation. C1807m317 | V16-17 OGLE-BLG-RRLYR-14912, OGLE-BLG-RRLYR-14892 C1807m317 | identified by RA and dec in the Ogle III survey C1807m317 | (Soszynski et al. 2011a) who assigned the numbers V16-17. C1807m317 | V16 was previously announced as star #29 by Blanco & Blanco (1997) C1807m317 | who published Epoch 1950 RA and dec and an ID chart. C1807m317 |----------------------------------------------------------------------- C1807m317 |The OGLE III survey of the Galactic Bulge also included catalogues of C1807m317 |Type II Cepheids (Soszynski et al 2011b) and Long Period Variables C1807m317 |(Soszynski et al. 2013). C1807m317 |In these surveys, no type II Cepheids were announced within 2.1 arcminutes C1807m317 |of the centre of NGC 6558, the radius listed by Soszynski et al. (2014). C1807m317 |The LPV catalogue includes an OSARG variable: OGLE-BLG-LPV-222123 C1807m317 |(r=0.79). Its V magnitude (16.38) seems faint for a cluster member and the C1807m317 |star probably belongs to the rich field surrounding the cluster. # C1808m072 | V1 C1808m072 | Sawyer Hogg (1959) with ID chart C1808m072 | The cluster was referred to as IC 1276 in her paper. C1808m072 | V2-5 C1808m072 | Kinman & Rosino (1962) with x,y positions and ID chart for V1-5 C1808m072 | The cluster was referred to as Abell 7 = IC 1276 in their paper. # C1809m227 |V1 C1809m227 | Sloan et al. (2010) with RA and dec # C1810m318 |V1-5: Rosino (1962) with x,y coordinates and ID charts C1810m318 | Rosino discovered 3 additional variables V6-8 which were considered C1810m318 | to be field stars. C1810m318 |V6 = Rosino's V7 C1810m318 | The number V6 was assigned by Hazen-Liller (1985) who noted that C1810m318 | this star was within the tidal radius. C1810m318 |V7-23: Hazen-Liller (1985) with x,y coordinates and an ID chart. C1810m318 | Hazen-Liller also discovered 20 new field variables (F3-F22) and C1810m318 | published their 1950 RA and dec, along with an ID chart. She C1810m318 | listed Rosino's V6 and V8 as F1 and F2. # C1814m522 |V1 C1814m522 | Fourcade et al. (1966) with x,y coordinates and an ID chart C1814m522 |V2-48 C1814m522 | Millis & Liller (1980) with x,y coordinates and ID charts for V1-48 C1814m522 | They made a small revision to the x,y position of V1. C1814m522 |V49-74 = NV1-26 C1814m522 | Toddy et al. (2012) with RA and dec C1814m522 | They also published RA and dec for most of the variables V1-48. # C1820m303 |V1-4 = V1, V2, V11 and V14 of Fourcade et al. (1966) C1820m303 | with x,y coordinates and an ID chart C1820m303 | Fourcade et al. announced 33 variables, but only 4 of them were C1820m303 | considered to be cluster members. Sawyer Hogg (1973) assigned the C1820m303 | numbers V3 and V4 to FL #11 and #14. C1820m303 |V5: Liller & Liller (1976) with an ID chart for V1-5 C1820m303 |----------------------------------------------------------------------- C1820m303 |A possible quiescent cataclysmic variable (or LMXB) was announced by C1820m303 |Deutsch et al. (1999). Dalessandro et al. (2014) followed up on this C1820m303 |system with HST observations and identified a star that appeared to be C1820m303 |the optical counterpart of the X-ray source Star 1. They called it C1820m303 |COM_Star1. It exhibited sinusoidal variations with an amplitude of ~0.7 C1820m303 |mag in F435W and an orbital period of ~98 minutes. However, they could C1820m303 |not make a definitive conclusion on the nature of the system: whether it C1820m303 |was a CV or LMXB. C1820m303 |------------------------------------------------------------------- C1820m303 |PSR: According to Paulo Freire's website, there are 6 millisecond C1820m303 | pulsars in NGC 6624. (www.naic.edu/~pfreire/GCpsr.html) # C1821m249 | V1-9 C1821m249 | Bailey (1902) with x,y positions (page 242) and ID chart (Plate XI, C1821m249 | Fig. 3) C1821m249 | V10-16 C1821m249 | Sawyer (1949) with x,y positions C1821m249 | V17 = Star #5 of Hoffleit (1965) and star 63a of Hoffleit (1972) C1821m249 | with 1900 RA and dec in both papers and an ID chart in 1972 C1821m249 | The number V17 was assigned by Sawyer Hogg (1973) in her 3rd C1821m249 | catalog and x,y coordinates were later derived by Wehlau & C1821m249 | Sawyer Hogg (1982). C1821m249 | V18, V20, V21, V24 C1821m249 | Wehlau & Sawyer Hogg (1982) with x,y positions C1821m249 | These authors pointed out that the star listed as V18 in C1821m249 | Sawyer Hogg's (1973) 3rd catalogue is V12. C1821m249 | They also listed coordinates for three other variables that they C1821m249 | designated V19, V22 and V23. However, in a subsequent study C1821m249 | (Wehlau & Sawyer Hogg 1984), they found that these three stars were C1821m249 | not variable and so they assigned these numbers to three other C1821m249 | variables. C1821m249 | V19, V22, V23 C1821m249 | Wehlau & Sawyer Hogg (1984) with x,y positions for these variables C1821m249 | and ID charts for V1-24 C1821m249 | PSR C1821m249 | A millisecond pulsar, PSR 1821-24, was discovered in the core of C1821m249 | M28 by Lyne et al. (1987). They published 1950 RA, dec and an ID C1821m249 | chart. Additional pulsars have been discovered since then. The RA C1821m249 | and dec for most of them have been published by Becker & Hui (2013). C1821m249 | According to Freire (2014), there are now 12 known pulsars in M28. C1821m249 | Optical counterparts that are variable stars have been identified by C1821m249 | Pallanca et al. (2010) for PSR J1824-2452H and by Pallanca et al. C1821m249 | (2013) for PSR J1824-2452I. C1821m249 |------------------------------ C1821m249 | Rees & Cudworth (1991) found strong evidence for variation of 3 additional C1821m249 | stars: their 2-56 and RC11 which are near the RG tip and RC133 which might C1821m249 | be an RR Lyrae. However, Prieto et al. (2012) could not confirm the C1821m249 | variability of star 2-56 or RC11, but they concluded that RC133 might be C1821m249 | the same star as their NV5. # C1827m255 |V1-19 C1827m255 | Terzan (1968) with an ID chart C1827m255 | Three of these variables #9, #10 and #11 were listed as V1-3 C1827m255 | by Sawyer Hogg (1973) in her 3rd catalogue. The remaining 16 C1827m255 | were not included because she considered them to be field stars. C1827m255 | No elements were listed by Sawyer Hogg (1973) for any of the C1827m255 | variables. C1827m255 | Terzan's original numbering system (V1-19) has been used in the C1827m255 | above table because it was adopted in a later paper by Rutily & Terzan C1827m255 | (1977) for the variable stars in and around NGC 6638. The 1977 paper C1827m255 | includes ID charts for all of the variables. C1827m255 |V20-45 = V4-29 of Sawyer Hogg et al. (1974) and Terzan & Rutily (1975) C1827m255 | The x,y coordinates were listed in both of the above papers. C1827m255 | The numbers V20-45 were assigned in a later paper by Rutily & C1827m255 | Terzan (1977). In their 1977 paper, Rutily & Terzan published C1827m255 | an ID chart for V20-45. C1827m255 |V46-63 C1827m255 | Rutily & Terzan (1977) with 1950 RA and Dec and an ID C1827m255 | chart for V1-19 and V44-63. C1827m255 |V64-71 C1827m255 | Skottfelt et al. (2015) with RA, dec and a finding chart # C1828m235 |V1 (V2578 Sgr) & V2 = 145a & 145b of Hoffleit (1972) C1828m235 | who listed the RA and dec for epoch 1900 and published a C1828m235 | finder chart. C1828m235 | The numbers V1 and V2 were assigned by Sawyer Hogg (1973). C1828m235 |V3-18 C1828m235 | Hazen (1993) with x,y coordinates and an ID chart C1828m235 | Hazen also discovered 11 field variables and published their C1828m235 | 1950 RA and dec and an ID chart. # C1828m323 |V1-3 C1828m323 | Rosino (1962) with x,y coordinates and ID chart C1828m323 | V2=V3484 Sgr and is listed in the GCVS. C1828m323 |V4 = V1894 Sgr = Ponsen Star 69 C1828m323 | Ponsen (1957) with 1900 RA and Dec C1828m323 | Rosino (1962) assigned the number V4 and published x,y coordinates C1828m323 | and an ID chart. C1828m323 |V5 = Rosino V10 C1828m323 | Rosino (1962) with x, y coordinates and an ID chart C1828m323 | The number V5 was later assigned by Sawyer Hogg in her 3rd catalogue. C1828m323 | Rosino (1962) published data for 10 variables, which he numbered C1828m323 | V1 t0 V10, but five of them were considered to be field stars, C1828m323 | based on their brightness and their distance from the cluster centre. C1828m323 | According to Catchpole et al. (1970), the star that Hartwick & C1828m323 | Sandage (1968) identified as V10 is not variable. C1828m323 |V6-8 = II-37, III-43 (annulus 1' -2') and IV-11 (inner 1') of C1828m323 | Hartwick & Sandage (1968). See Fig. 2 of their paper. C1828m323 | The variability of these three stars was announced by Lloyd Evans & C1828m323 | Menzies (1971) and confirmed by Lloyd Evans & Menzies (1973). C1828m323 | The numbers V6-8 were assigned by Sawyer Hogg in her 3rd (1973) C1828m323 | catalogue. C1828m323 |-------------------------------------------------------------------- C1828m323 |Escobar et al. (2010) conducted a search for stellar variability in this C1828m323 |cluster and discovered 54 new variable stars. Among the new variables are C1828m323 |9 RR Lyrae, 7 SX Phe and 18 LPV candidates. Since the cluster lies in a C1828m323 |rich field near the Galactic centre, the authors conclude that many of these C1828m323 |variables are not cluster members. Their results were presented in a poster C1828m323 |paper. Detailed information about the individual variables has not yet been C1828m323 |published. # C1832m330 | V1-9 C1832m330 | Hazen (1989) with x,y coordinates and ID chart C1832m330 | Hazen also provided data for an additional 15 variables outside the C1832m330 | cluster tidal radius which was considered at the time to be 466 C1832m330 | arcsec. C1832m330 | V10 = Optical counterpart of X-ray source A C1832m330 | Heinke et al. (2001) with RA, dec for source A and Chandra C1832m330 | X-ray image for sources A-C with optical counterparts C1832m330 | superimposed. C1832m330 | Engel et al. (2012) derived a 2.15 hour orbital period for the C1832m330 | binary. C1832m330 | V11 = optical counterpart of X-ray source B C1832m330 | = star 49 of Deutsch et al. (1998) who published an ID chart C1832m330 | The optical variability was first detected by Deutsch et al. (2000) C1832m330 | who concluded it was the optical counterpart of the strong X-ray C1832m330 | source (now referred to as source A) in NGC 6652. C1832m330 | However, Heinke et al. (2001) subsequently showed that Deutsch's C1832m330 | star 49 was associated with X-ray source B, not source A. C1832m330 | In the electronic catalogue by Clement et al. (2001), star 49 was C1832m330 | initially assigned the number V10 and Samus et al. (2009) derived its C1832m330 | RA and dec. V10 is now considered to be the variable star C1832m330 | associated with X-ray source A. C1832m330 | V12 = Optical counterpart of X-ray source C C1832m330 | Heinke et al. (2001) with RA, dec for source C and Chandra C1832m330 | X-ray image for sources A-C with optical counterparts C1832m330 | superimposed. C1832m330 | C1832m330 | V13-14 C1832m330 | Skottfelt et al. (2015) with RA, dec and a finding chart C1832m330 | V13 exhibited an outburst in the course of their observations and C1832m330 | is probably the optical counterpart of X-ray source H. C1832m330 | PSR: C1832m330 | According to Paulo Freire's website: www.naic.edu/~pfreire/GCpsr.html C1832m330 | a millisecond pulsar in NGC 6652 was discovered by DeCesar et al. C1832m330 | (2011). C1832m330 |------------------------------------------------------------------------ C1832m330 |In an analysis of Chandra X-ray sources in NGC 6652, Stacey et al. C1832m330 |(2012) discussed the properties of 12 X-ray sources (A-L). C1832m330 |Four of these sources (A, B, C, and H) are listed as V10-13 in the C1832m330 |above table because they have all been detected as optical variable stars. # C1833m239 | V1-16 C1833m239 | Bailey (1902) with ID chart C1833m239 | V17 C1833m239 | by Swope and announced by Shapley (1927) with x,y positions for V1-17 C1833m239 | V18-25 C1833m239 | Sawyer (1944) with x,y positions for V1-25 and ID chart for V1-21 C1833m239 | and V23-25. (V22 was outside the field.) C1833m239 | V26-31 = #181a,181b,173a,187b,191,185 C1833m239 | by Hoffleit (1972) with 1900 RA & dec and GCVS numbers for C1833m239 | some of them. These variables were later identified on an ID C1833m239 | chart by Wehlau & Sawyer Hogg (1977). The numbers V26-31 were C1833m239 | assigned by Sawyer Hogg (1973) in her 3rd catalogue. C1833m239 | V32-33 C1833m239 | V. Sherwood, an assistant to Sawyer Hogg (unpublished) and C1833m239 | identified on the chart by Wehlau & Sawyer Hogg (1977). C1833m239 | V34-35 C1833m239 | Lloyd Evans (1978) reported (see page 300) that Kukarkin had C1833m239 | discovered two red variables not previously known. C1833m239 | These were star IV-17 labelled on a plate by Arp & Melbourne (1959) C1833m239 | and star V-9 labelled by Lloyd Evans (1975). Wehlau & Sawyer Hogg C1833m239 | (1978) numbered these two variables as V34 and V35 respectively and C1833m239 | identified them on their ID chart. Both stars are near the red giant C1833m239 | tip. C1833m239 | C1833m239 | V36-43 C1833m239 | Kravtsov et al. (1994) with ID chart and the RA & dec (Epoch 1950). C1833m239 | They noted that these are faint for RR Lyrae cluster members, but they C1833m239 | could be members if they are subgiants. C1833m239 | KT-01 to KT-55 (CASE M22 variables) C1833m239 | Kaluzny & Thompson (2001) with RA & dec C1833m239 | The designation KT-01 to KT-55 has been assigned in this catalogue. C1833m239 | These authors initially selected 55 candidate variables, but only C1833m239 | 36 of them turned out to be new variables: 6 were spurious and 13 C1833m239 | were RR Lyrae variables that were already known. C1833m239 | Proper motions for some of these variables were later obtained by C1833m239 | Zloczewski et al. (2012). Their study indicated that KT-01, 04, C1833m239 | 16, 20, 23, 28, 34, 37, and 38 are probable members and that KT-03, C1833m239 | 05, 15, 18, 39, 42, and 54 are probably non-members. C1833m239 | PK-04 to PK-11 C1833m239 | Pietrukowicz & Kaluzny (2003) with RA & dec C1833m239 | P&K referred to these stars as M22_04 to M22_11. The designation C1833m239 | PK-04 to PK-11 has been assigned in this catalogue. C1833m239 | P&K also listed data for three stars numbered 1 to 3 which are C1833m239 | the same stars as KT-27, 13 and 43 respectively. C1833m239 | CV1 C1833m239 | Anderson et al. (2003) with RA, dec and ID chart C1833m239 | This object had been previously announced as a microlensing event C1833m239 | in the Galactic bulge by Sahu et al. (2001), but Anderson et al. C1833m239 | concluded that it was more likely the outburst of a cataclysmic C1833m239 | variable because its proper motion indicated it was a cluster C1833m239 | member. Also it exhibited H_alpha emission and variability in C1833m239 | quiescence and was associated with an X-ray source. C1833m239 | Cataclysmic outbursts of the star were subsequently detected in C1833m239 | other studies including that of Pietrukowicz et al. (2005) and most C1833m239 | recently by Alonso-Garcia et al. (2015) who reported an increment C1833m239 | in brightness of more than 1 mag in K mag, the first dwarf nova C1833m239 | eruption observed at near infra-red wavelengths in a globular C1833m239 | cluster. C1833m239 | CV2 C1833m239 | Pietrukowicz et al. (2005) with RA, dec and ID chart. C1833m239 | Webb et al.(2004) announced that there are 5 (+/-3) X-ray sources C1833m239 | associated with M22 and Pietrukowicz concluded that CV2 is C1833m239 | associated with one of them. C1833m239 | P1 is a probable microlensing event detected by C1833m239 | Pietrukowicz et al. (2005) who listed the RA & dec and published C1833m239 | an ID chart. C1833m239 | Ku-1 to Ku-4 = NV1-4 C1833m239 | Kunder et al. (2013) with RA and dec C1833m239 | SLW-4, SLW-5, SLW-7, SLW-8, SW-11 C1833m239 | Sahay et al. (2014) with RA and dec. C1833m239 | These stars are located near the RG tip in the K,(J-K) CM diagram C1833m239 | and are considered to be cluster members. Sahay et al. announced 6 C1833m239 | other new long period variables but, based on their location in the C1833m239 | CM diagram, SLW 1-3, SLW 6 and SLW 9-10 are considered to be field C1833m239 | stars. V14 which was also part of their study and is displaced to C1833m239 | the red in the CM diagram is known to be a Mira variable in the field. C1833m239 | In their study, Sahay et al. also discovered 11 candidate long period C1833m239 | variables. C1833m239 | PSRA, B = J1836-2354, J1836-2354B C1833m239 | Lynch et al. (2011) with RA and dec C1833m239 | C1833m239 |-------------------------------------------------------------- C1833m239 |Figuera Jaimes et al. (2016) searched for new variables in a 41 by 41 C1833m239 |arcsec field around the cluster centre and found none. # C1840m323 | V1-2 = V1 and V3 of Rosino (1962) who published x,y coordinates C1840m323 | and an ID chart for five variables, V1-5 C1840m323 | Sawyer Hogg (1973) assigned the number V2 to Rosino's V3 because C1840m323 | Rosino's V2 was considered to be a field star. C1840m323 | V3-5 C1840m323 | Liller (1983) with x,y coordinates and an ID chart C1840m323 | Kadla et al. (1996) pointed out that the x coordinates Liller C1840m323 | published for V3 and V4 had an error in sign. The corrected C1840m323 | coordinates are x=-8 (V3) and x=+142 (V4). C1840m323 | Liller also published identifications for 13 field variables C1840m323 | including Rosino's V2, V4 and V5. C1840m323 | V6 C1840m323 | Figuera Jaimes et al. (2016) with RA, dec and a finding chart. C1840m323 |----------------------------------------------------------------------- C1840m323 |Kadla et al. (1996) announced an additional 7 RR Lyrae variables, based C1840m323 |on B and V photometry they obtained for stars in the instability strip C1840m323 |of the CM diagram. They published x,y ccoordinates, but did not carry C1840m323 |out any further analysis. C1840m323 |Of Kadla's seven new variables, six should have been in the 41 by 41 C1840m323 |arcsecond field observed by Figuera Jaimes et al. (2016). However, C1840m323 |Figuera Jaimes et al. did not detect variability in any of them, with C1840m323 |the possible exception of one star. The Kadla et al. chart is difficult C1840m323 |to decipher, but it appears that their N7 might be V6. # C1850m087 | V1 C1850m087 | Davis (1917) with x,y coordinates C1850m087 | V2 = AP Sct C1850m087 | Oosterhoff (1943) with 1900 RA & dec and a finder chart C1850m087 | The number V2 was assigned by Sawyer (1953). C1850m087 | V3-12 C1850m087 | Sawyer (1953) with x,y coordinates and an ID chart for V1-12 C1850m087 | V13 = #144 of Harwood (1962) who derived RA & dec (1900) C1850m087 | The number V13 was assigned by Sandage et al. (1966) who published C1850m087 | x,y coordinates and an ID chart C1850m087 | V14-15 = #131, #160 of Harwood (1962) who derived RA & dec (1900) C1850m087 | The numbers V14 and V15 were assigned by Sandage et al. (1966) who C1850m087 | published x,y coordinates. These stars were labelled on the finding C1850m087 | chart of Sandage & Smith (1966). C1850m087 | V16&17 = #141 & #151 of Harwood (1962) who derived RA & dec (1900) C1850m087 | The numbers V16 and V17 were assigned by Sandage et al. (1966) C1850m087 | who published x,y coordinates and an ID chart. C1850m087 | However, neither Sandage et al. (1966) nor Rosino (1966) detected C1850m087 | variability in V17. C1850m087 | V18-20 C1850m087 | Sandage et al. (1966) with x,y coordinates and an ID chart C1850m087 | V21 = L18 of Lloyd Evans & Menzies (1973) C1850m087 | The number V21 was assigned by Sawyer Hogg (1973) in her 3rd C1850m087 | catalogue. Lloyd Evans & Menzies (1977) published an ID chart and C1850m087 | Samus et al. (2009) derived the RA and dec based on the ID chart. C1850m087 | V22 = KC460 of Cudworth (1988) who published x,y coordinates and stated C1850m087 | that the star exhibited low amplitude variability (see page 113). C1850m087 | The number V22 has been assigned in this catalogue. C1850m087 | V23-24 = P1 & P2 of Tuairisg et al. (2003) who published RA, dec and C1850m087 | an ID chart. C1850m087 | The numbers V23 and V24 have been assigned in this catalogue. C1850m087 | V25 = NGC6712_01 of Pietrukowicz & Kaluzny (2004) who published RA C1850m087 | and dec. C1850m087 | This star is the optical counterpart of the X-ray source C1850m087 | X1850-087 and its optical variability was originally detected by C1850m087 | Homer et al. (1996) from HST U filter observations. C1850m087 | V26-29 = NGC6712_06, _07, _08, _09) of Pietrukowicz & Kaluzny C1850m087 | (2004) who published RA and dec. # C1851m305 |V1-28 C1851m305 | Rosino (1952) with x,y (arcsec) coordinates and ID charts C1851m305 |V29-82 C1851m305 | Rosino & Nobili (1958) with x,y (arcsec) C1851m305 | coordinates and ID charts. Also all the variables from V1-28 C1851m305 | (with the exception of V11, 16 and 19) were labelled on the charts. C1851m305 |V83-117 C1851m305 | Layden & Sarajedini (2000) with X,Y (pixel) coordinates. C1851m305 | They also published small finder charts (field 20 by 20 arcsec) for C1851m305 | each of the variables they studied. These authors also announced C1851m305 | three candidate variables which they numbered SV1-3. C1851m305 | Their study was based on VI photometry. C1851m305 |V118-211 C1851m305 | Sollima et al. (2010) with RA and dec. C1851m305 | They published magnitudes, amplitudes and colours based on BVI C1851m305 | photometry for the variables in their investigation. C1851m305 |V212-291 C1851m305 | Figuera Jaimes et al. (2016) with RA, dec and an ID chart C1851m305 |V292-295 = VC16, VC22, VC24, VC38 of C1851m305 | Montiel & Mighell (2010) with RA and dec C1851m305 | The numbers V292-295 were assigned by H16. C1851m305 |V296-347 C1851m305 | H16 with RA, dec and finder charts C1851m305 | Their investigation was based on data from the OGLE IV survey C1851m305 | and their tables and charts are available from the OGLE FTP Site: C1851m305 | ftp://ftp.astrouw.edu.pl/ogle/ogle4/OCVS/M54/ C1851m305 | Among their new variables, H16 list only variables that are located C1851m305 | less than 7.5 arcmin from the cluster centre, the tidal radius that C1851m305 | was published in the 1999 and 2003 updates to the Harris (1996) C1851m305 | catalogue. C1851m305 |V348 = OGLE-BLG-RRLYR-37496 C1851m305 | from the Ogle IV investigation of RR Lyrae variables in the Galactic C1851m305 | Bulge by Sos14. C1851m305 | The number V348 has been assigned in this catalogue. C1851m305 | Data and chart for V348 are available from the OGLE FTP Site: C1851m305 | ftp://ftp.astrouw.edu.pl/ogle/ogle4/OCVS/blg/rrlyr C1851m305 | With r=8.2 arcmin, V348 is inside the tidal radius, 9.7 arcmin, C1851m305 | derived from the core concentration and radius publihed by Harris C1851m305 | (2010). #37496 was independently announced by Cseresnjes et al. C1851m305 | (2000) as vs11f53. C1851m305 | C1851m305 | Another RR Lyrae variable, OGLE-BLG-RRLYR-37506, with r=9.0 C1851m305 | arcmin is located within the tidal radius, but its magnitudes are C1851m305 | too bright for cluster membership. C1851m305 |V349 = OGLE-BLG-ECL-424672 (r=7.5') C1851m305 |V350 = OGLE-BLG-ECL-424680 (r=4.1') C1851m305 |V351 = OGLE-BLG-ECL-424692 (r=3.1') C1851m305 |V352 = OGLE-BLG-ECL-424696 (r=0.7') C1851m305 | from the Ogle IV investigation of eclipsing binary stars in C1851m305 | the Galactic Bulge by Sos16. C1851m305 | Data and charts are available from the OGLE FTP Site: C1851m305 | ftp://ftp.astrouw.edu.pl/ogle/ogle4/OCVS/blg/ecl C1851m305 | The numbers V349-352 have been assigned in this catalogue. C1851m305 |Two other eclipsing stars within the tidal radius, C1851m305 | OGLE-BLG-ECL-000216 (r=9.5') and OGLE-BLG-ECL-424733 (r=7.9') C1851m305 | appear to be field stars based on their positions in the CMD C1851m305 |---------------------------- C1851m305 |Montiel & Mighell (2010) announced 50 RR Lyrae candidates based on an C1851m305 |analysis of archival HST WFPC2 data. They assigned numbers VC1 to VC50 C1851m305 |to their candidates. The HST observations were obtained over an interval C1851m305 |of a few hours on one day and were not sufficient for period determination. C1851m305 |However, a comparison with the known RR Lyrae variables indicates that 40 C1851m305 |of their candidates have been confirmed as RR Lyrae variables in other C1851m305 |investigations: C1851m305 |VC1=V241, VC2=V127, VC4=V220, VC5=V255, VC7=V234, VC8=V221, VC9=V216, C1851m305 |VC10= V223, VC11=V162, VC12=V163, VC13=V95, VC14=V164, VC15=V142, C1851m305 |VC16=V292, VC17=V129, VC18=V179, VC20=V224, VC22=V293, VC23=V250, C1851m305 |VC24=V294, VC25=V215, VC26=V245, VC27=V291, VC28=V181, VC30=V233, C1851m305 |VC31=V237, VC32=V284, VC33=V285, VC34=V160, VC35=V212, VC36=V236, C1851m305 |VC37=V225, VC38=V295, VC39=V214, VC40=V213, VC41=V232, VC44=V46, C1851m305 |VC45=V148, VC46=V192, VC47=V76. The declinations listed in the above C1851m305 |table are on average 1 arcsec south of the decs listed by Montiel & C1851m305 |Mighell and the RAs are approximately 0.02 seconds (of time) east. # C1852m227 | V1 = SPZ 2200 C1852m227 | Goranskij (1978) with x,y position and ID chart C1852m227 | An ID chart for SPZ 2200 was also published by Goranskij (1979) C1852m227 | The number V1 was assigned by Clement et al. (2001). C1852m227 | C1852m227 | Another (suspected) RR Lyrae (based on its position in the CM C1852m227 | diagram) was announced by Gerashchenko et al. (1997) C1852m227 | On their ID chart, the star is located at pixel position: C1852m227 | X~72, Y~453. # C1856m367 |V1-16 C1856m367 | Bailey (1902) with x,y coordinates (see page 242) and an ID chart C1856m367 | (see Plate XI, Fig. 4 which is Plate 252.21 in the scanned version C1856m367 | of the paper on SAO/NASA ADS) C1856m367 | In subsequent papers, (Bailey 1924a,b), he derived elements for the C1856m367 | variables and discovered 6 additional variables in the field near the C1856m367 | cluster. C1856m367 |V17 = V12 of van Gent (1932) who published x,y coordinates C1856m367 | on Bailey's system and RA and dec (epoch 1875) C1856m367 | The number V17 was assigned by Sawyer (1939) in her first catalogue. C1856m367 |V18-V19 = V123 and V154 of van Gent (1933) who published RA and dec C1856m367 | (epoch 1875). C1856m367 | The numbers V18 and V19 were assigned by Sawyer (1939) in her C1856m367 | first catalogue. She also publsihed x,y coordinates for the two C1856m367 | stars. C1856m367 |V20 C1856m367 | Fourcade et al. (1966) with x,y coordinates and an ID chart C1856m367 | They also published ID charts for all of the previously known C1856m367 | variables. C1856m367 |V21-29 C1856m367 | Most of these variables were discovered by Menzies and investigated as C1856m367 | part of his 1967 PhD thesis at the Australian National University. C1856m367 | They were subsequently discussed by Lloyd Evans & Menzies (1973) and C1856m367 | by Menzies (1973), but their positions were not published in these C1856m367 | papers. C1856m367 | Sawyer Hogg (1973) listed their x,y coordinates in her 3rd catalogue, C1856m367 | based on private correspondence with these authors. C1856m367 | In a later paper, Menzies (1974) published x,y coordinates for all of C1856m367 | the known variables and an ID chart for all except V8 and V20 which C1856m367 | were too close to the cluster centre. C1856m367 |V30-32 C1856m367 | Menzies (1974) with x,y coordinates and an ID chart C1856m367 |V33-47 = NV1-14 and NV19 of Lee et al. (2014) who published finding C1856m367 | charts and RA & dec. C1856m367 | They announced 7 other new variables: 2 delta Scuti variables and C1856m367 | 5 W UMa-type eclipsing binaries, but they considered all of these C1856m367 | to be field stars based on the absolute magnitudes and distances C1856m367 | they derived. C1856m367 | For the delta Scuti variables, NV16 and NV18, they calculated C1856m367 | the absolute magnitudes from relationships derived by McNamara (2011) C1856m367 | and by Cohen & Sarajedini (2012). For the W UMa binaries, NV15, C1856m367 | NV17, NV20, NV21, and NV22, they calculated the absolute magnitudes C1856m367 | from an empirical relation derived by Rucinski (2000). C1856m367 |-------------------------------------------------------------------- C1856m367 |Figuera Jaimes et al. (2016) conducted a search for variables in a C1856m367 |41 by 41 arcsecond field around the cluster centre. They recovered C1856m367 |V8, V34, V35 and V44, but did not discover any new variables. # C1902p017 |V1 C1902p017 | Matsunaga et al. (2006) with RA and dec C1902p017 |PSR: According to Paulo Freire's website, there are 2 millisecond C1902p017 | pulsars in NGC 6749. (www.naic.edu/~pfreire/GCpsr.html) # C1906m600 | V1-2 C1906m600 | Fourcade et al. (1966) with x,y coordinates and an ID chart C1906m600 | According to Fourcade et al., V1 is considered to be the variable C1906m600 | that Sawyer mentioned in her first two catalogues and she C1906m600 | acknowledged this in her 3rd edition. The variable was originally C1906m600 | announced by Bailey (1902 - in Table 1 on page 2), but no position C1906m600 | was published. C1906m600 | V3 = star #126 C1906m600 | Cannon & Stobie (1973) with ID chart C1906m600 | V4-14 C1906m600 | Thompson et al. (1999) with ID charts and RA and dec C1906m600 | According to Samus et al. (2009), their charts for C1906m600 | V4, V6, V11 and V14 are incorrect, but their RA and dec are C1906m600 | correct. C1906m600 | Proper motions for some of these variables were later obtained by C1906m600 | Zloczewski et al. (2012). Their study indicated that V7, V8 and C1906m600 | V12 are probable members and that V9 is probably not a member. C1906m600 | V15-24 C1906m600 | Kaluzny & Thompson (2009) with ID charts and RA and dec C1906m600 | Preliminary results for some of these variables were reported in C1906m600 | the proceedings of a conference (Kaluzny & Thompson 2008). C1906m600 | Proper motions for some of these variables were later obtained by C1906m600 | Zloczewski et al. (2012). Their study indicated that V15, V16, V17, C1906m600 | V23 and V24 are probable members and that V19, V20 and V22 are C1906m600 | probably non-members. C1906m600 | V25 = Bailyn CV candidate #1 = CX4 of Pooley et al. (2002) C1906m600 | Bailyn et al. (1996) with ID chart and RA and dec C1906m600 | Kaluzny & Thompson (2009) confirmed the CV status of this star C1906m600 | and assigned the number V25. C1906m600 | V26 = Bailyn CV candidate #2 = CX7 of Pooley et al. (2002) C1906m600 | Bailyn et al. (1996) with ID chart and RA and dec C1906m600 | Thomson et al. (2012) confirmed the CV status of this star and the C1906m600 | number V26 has been assigned in this electronic catalogue. C1906m600 | V27 = optical counterpart of CX1 of Pooley et al. (2002) C1906m600 | Thomson et al. (2012) with ID charts and RA and dec C1906m600 | Pooley et al. (2002) listed this source as a possible CV and Thomson C1906m600 | et al. confirmed its CV status. C1906m600 | Thomson et al. also discovered an SX Phe variable (their star #7581), C1906m600 | but it appears too faint to be a cluster member. C1906m600 | PSRA=J1911-5958A C1906m600 | D'Amico et al. (2001) who designated it as PSR J1910-59 C1906m600 | Further information is available from the GC pulsar website: C1906m600 | http://www.naic.edu/~pfreire/GCpsr.html C1906m600 | PSRB, C, D, E = J1910-5959B, J1911-6000C, J1910-5959D, J1910-5959E C1906m600 | D'Amico et al. (2002) C1906m600 |--------------- C1906m600 |Dupree & Hartmann (1990) and Dupree et al. (1990) demonstrated C1906m600 |spectroscopically that two stars near the red giant tip, #31 and #59 of C1906m600 |Alcaino (1972), might be pulsating. Neither of these stars was measured C1906m600 |in the Cannon & Stobie (1973) study in which V3 was discovered. C1906m600 |--------------- C1906m600 |Pooley et al. (2002) detected 19 Chandra X-ray sources in NGC 6752 and C1906m600 |made 12 optical identifications. They concluded that 10 of them might C1906m600 |be cataclysmic variables. Subsequent studies by Kaluzny & Thompson C1906m600 |(2009) and by Thomson et al. (2012) have confirmed that three of their C1906m600 |sources CX4, CX7 and CX1 are CVs. They have been assigned the numbers C1906m600 |V25, V26 and V27. C1906m600 |Kaluzny & Thompson also detected periodic variability at the position C1906m600 |of CX19 and proposed that it is an excellent candidate for a close C1906m600 |degenerate binary caught in quiescence. C1906m600 |---------------- C1906m600 |Catelan et al. (2008) announced a candidate variable on the blue C1906m600 |extension of the HB. No coordinates were listed for the star. C1906m600 |---------------- C1906m600 |Moni Bidin et al. (2008) detected a hot (25000K) close binary candidate C1906m600 |in a radial velocity study of 145 HB stars. No coordinates were C1906m600 |listed for the star. C1906m600 |---------------- C1906m600 |Lee et al. (2015) reported that they were carrying out a search for C1906m600 |variable stars in NGC 6752 and five other clusters (NGC 288, NGC 1851, C1906m600 |NGC 3201, NGC 4372 and NGC 6809). C1906m600 |----------------- C1906m600 |Figuera Jaimes et al. (2016) conducted a search for variables in a 41 by C1906m600 |41 arcsec field around the cluster centre and detected an outburst in C1906m600 |V26, but did not discover any new variables. # C1908p009 | V1-4 C1908p009 | Sawyer (1953) with x,y coordinates and an ID chart C1908p009 | Prosser (1988) later published a more legible ID chart C1908p009 |-------------------------------------------------------------------- C1908p009 | PSR: According to Paulo Freire's website, there are 2 millisecond C1908p009 | pulsars in NGC 6760. (www.naic.edu/~pfreire/GCpsr.html) # C1914p300 |V1-3 C1914p300 | Shapley (1920) with x,y coordinates and ID chart. C1914p300 | V2 was a suspected variable. V3 was independently discovered by Davis C1914p300 | (1917) who listed Delta RA & dec, but the x,y coordinates assigned C1914p300 | by Shapley were different. C1914p300 |V4-9 C1914p300 | Sawyer (1940) with x,y coordinates and an ID chart for V1-9 as well C1914p300 | as the numbers assigned in Kustner's (1920) catalogue. Later Sawyer C1914p300 | (1949) classified V6 as an RV Tauri type. C1914p300 |V10-11 C1914p300 | Rosino (1944) with x, y coordinates and finding chart for V1-11 C1914p300 | (V2 not included) C1914p300 |V12 = Kustner #68 C1914p300 | Sawyer (1953) with x,y coordinates C1914p300 |V13-14 C1914p300 | Pietrukowicz et al. (2008) with RA and dec C1914p300 |------------------ C1914p300 |Additional variables C1914p300 | In a series of papers, Kurochkin (1968, 1970, 1971, 1972) identified C1914p300 | a total of 82 new variables in a field within 10 by 10 degrees of the C1914p300 | cluster centre. Wehlau & Sawyer Hogg (1985) concluded that none were C1914p300 | cluster members. C1914p300 | Russeva (1999) announced the variability of four red giants: Kustner C1914p300 | numbers 204, 235, 251 and K343 and derived periods in the range of 22 C1914p300 | to 33 days for all of them. They noted that the radial velocity C1914p300 | derived by Harris et al. (1983) for K204 indicated cluster membership. C1914p300 | Pietrukowicz et al. (2008) stated that their analysis did not indicate C1914p300 | any variability for K204, but they did not mention the other three. # C1916p184 | V1 C1916p184 | announced by Sawyer Hogg in her 3rd catalog because of a C1916p184 | 1972 letter from Rosino. He discovered the variable on red C1916p184 | plates. It had a large amplitude and was near the centre of C1916p184 | the cluster. No further information was given. C1916p184 | It is probable that this is one of the variables subsequently C1916p184 | announced by Rosino & Guzzi (1978), probably V2 (MV Sge) according to C1916p184 | Samus et al. (2009). C1916p184 | V2-3 = R&G 66 and R&G 70 = MV Sge and MZ Sge C1916p184 | Rosino & Guzzi (1978) with 1950 RA and Dec and ID chart. Rosino & C1916p184 | Ortolani (1985) also published an ID chart. C1916p184 | The numbers V2 and V3 were assigned in the electronic update to the C1916p184 | catalogue (Clement et al. 2001). # C1925m304 | V1-12 C1925m304 | Salinas et al. (2005) with an ID chart and x, y coordinates with C1925m304 | respect to the cluster centre. C1925m304 | They pointed out that V1-4 were V4, V5, V25 and V28, respectively C1925m304 | in the 2001 Univ. of Bologna thesis of Valenti, but they did not C1925m304 | confirm the variation of the other variables reported by Valenti. # C1936m310 |V1-2 C1936m310 | Bailey (1902) with x,y coordinates C1936m310 | (page 243) and an ID chart (plate XII: Fig 1, page 252.23, C1936m310 | description on page 251) C1936m310 |V3-6 C1936m310 | King (1951) with x,y coordinates. C1936m310 | No finding chart was provided, but in a later paper (King & Bruzual C1936m310 | 1976), he pointed out that Figures 2 and 3 in a paper by Alcaino C1936m310 | (1975) serve as convenient finding charts. V1-V6 are equivalent to C1936m310 | Alcaino #59, 366, 96, 433, 592, and 456, respectively. C1936m310 |V7-15 C1936m310 | Olech et al. (1999) with RA, dec and findng charts. C1936m310 | C1936m310 |V16-42 C1936m310 | Pych et al. (2001) with RA, dec and finding charts C1936m310 |V43 = CV1 (a dwarf nova) C1936m310 | Kaluzny et al. (2005) with RA, dec and finding chart. C1936m310 | The number V43 was assigned in this electronic catalogue. C1936m310 | These authors also detected a blue variable (M55-B1) that they C1936m310 | concluded might be a candidate quasar. The extragalactic nature of C1936m310 | this source was confirmed by Webb et al. (2006). It was their C1936m310 | X-ray source #39. C1936m310 |V44-71 C1936m310 | Kaluzny et al. (2010) with RA, dec and finding charts # C1938m341 |V1-2 = Montegriffo's #1350 and #117 C1938m341 | Montegriffo et al. (1998) announced 5 candidate variables: 117, 688, C1938m341 | 1350, 1582 and 2784. They labelled them on an ID chart and published C1938m341 | pixel positions (X,Y). C1938m341 | Salinas et al. (2005) confirmed the variablility of #1350 and #117 C1938m341 | and assigned the numbers V1 and 2. They also published x,y C1938m341 | coordinates and a finding chart. However, the x,y coordinates they C1938m341 | listed for V1 and V2 do not match the postions labelled on their C1938m341 | chart. They are reversed. The numbering system used in ths catalogue C1938m341 | corresponds to the positions on their chart. C1938m341 | Montegriffo's candidate variable #2784 appears to be just outside C1938m341 | the field of the finding chart of Salinas et al. Therefore it should C1938m341 | still be considered a candidate variable. The other two candidates C1938m341 | (#688 and #1582) are considered to be non-variable because Salinas C1938m341 | et al. (2005) did not detect any variability. C1938m341 |V3-4 C1938m341 | Salinas et al. (2005) with x,y, coordinates and an ID chart # C1951p186 | V1-2 = Z Sge and 48.1928 Sge C1951p186 | Baade (1928) with 1925 RA and dec C1951p186 | Sawyer (1952) pointed out that these two variables were within the C1951p186 | limits of the cluster NGC 6838 and Sawyer (1953) assigned the numbers C1951p186 | V1 and 2 C1951p186 | V3-4 C1951p186 | Sawyer (1953) with x,y coordinates and an ID chart for V1-4 C1951p186 | V5-6 = AH1-29, S142 [V6 is also known as V0345 Sge.] C1951p186 | Welty (1985) recognized that these two stars were variable and C1951p186 | derived periods and x,y coordinates (offset by -5,+11 from Sawyer C1951p186 | Hogg's x,y system). Frogel et al. (1979) had previously pointed out C1951p186 | that AH1-29 was a small amplitude variable near the RG tip and C1951p186 | in 1977, there was some private correspondence between Cohen and C1951p186 | Sawyer Hogg concerning this star. C1951p186 | AH1-29 was identified on a chart by Arp & Hartwick (1971). C1951p186 | S142 was identified by Sanders (1971). C1951p186 | The numbers V5 and V6 were assigned by Clement (1997) in the first C1951p186 | electronic update of the Sawyer Hogg (1973) catalogue. C1951p186 | P1-5 = short period variables V1-5 of Yan & Mateo (1994) C1951p186 | = faint variables v1-5 of Park & Nemec (2000) C1951p186 | Yan & Mateo listed their 1950 RA and Dec and published ID charts. C1951p186 | Park & Nemec listed their 2000 RA and dec and published ID charts C1951p186 | for V1, V2, V4 and V5. C1951p186 | Yan & Mateo's V3 and V4 had been previously announced by Hodder et C1951p186 | al. (1992) who designated them as H3 and H4 and published X,Y C1951p186 | pixel numbers and an ID chart. C1951p186 | Rucinski (2000) analysed the observations of the 4 contact binaries C1951p186 | (Yan & Mateo V1,2,3,5 ) and concluded that they were all cluster C1951p186 | members based on their photometric properties. C1951p186 | In the Clement et al. (2001) catalogue, the numbers V7-11 were C1951p186 | assigned to these stars and Samus et al. (2009) followed the C1951p186 | Clement numbering system. However, subsequent investigators have C1951p186 | followed the numbering system of Yan & Mateo. Therefore in this C1951p186 | electronic catalogue, these stars are numbered P1-5 to distinguish C1951p186 | them from the original V1-5 in NGC 6838 (M71). C1951p186 | P6-7 = faint variables v6-7 of Park & Nemec (2000), previously C1951p186 | announced by Hodder et al. (1992) who designated them as H1 and H2 C1951p186 | and published X,Y pixel numbers and an ID chart. C1951p186 | In the Clement et al. (2001) catalogue, the numbers V12-13 were C1951p186 | assigned to these stars and Samus et al. (2009) followed the C1951p186 | Clement numbering system. However, subsequent investigators have C1951p186 | followed the numbering scheme that Park & Nemec (2000) set up for C1951p186 | the faint variables in M71 so they have been numbered P6-7 in this C1951p186 | catalogue. C1951p186 | P8-23 = v8-23 of Park & Nemec (2000) who listed RA, dec and published C1951p186 | ID charts. C1951p186 | In the Clement et al. (2001) catalogue, the numbers V14-29 were C1951p186 | assigned to these stars and Samus et al. (2009) followed the C1951p186 | Clement numbering system. However, in a subsequent paper, McCormac C1951p186 | et al. (2014) followed the numbering system of Park & Nemec. C1951p186 | Therefore in this electronic catalogue, the stars are designated C1951p186 | "P" to indicate the numbering system of Park & Nemec. C1951p186 | P24-40 = V24-40 of McCormac et al. (2014) C1951p186 | who published finding charts and 2000 RA and dec C1951p186 | PSR = PSR J1953=1846A, a binary millisecond pulsar with a low mass C1951p186 | companion (Hessels et al. 2007): rotation P= 4.888 ms and C1951p186 | orbital P = 4.24 hours C1951p186 |------------------------------------------------------------------- C1951p186 |Jeon et al. (2004) announced the discovery of a double-radial-mode C1951p186 |SX Phe star which they named D6, but no identification was provided C1951p186 |and the star was not mentioned in their subsequent paper (Jeon et al. C1951p186 |2006) on SX Phe variables in M71. C1951p186 |------------------------ C1951p186 |Jeon et al. (2007) announced the detection of 24 eclipsing binaries, 10 C1951p186 |of them new discoveries and 16 other variables, most of which have long C1951p186 |periods. This was a poster paper and only the abstract was published. C1951p186 |----------------------- C1951p186 |Elsner et al. (2008) observed the cluster with Chandra and detected C1951p186 |29 X-ray sources within the half-mass radius (r_h) and another 34 C1951p186 |between r_h and 2r_h. Their source s08 coincideed with the MSP. For C1951p186 |some of the other sources, they listed possible optical and infrared C1951p186 |counterparts. C1951p186 |----------------------- C1951p186 |Pietrukowicz (2009) imaged five of the X-ray sources in H-alpha and C1951p186 |concluded that s57 of Elsner et al. (2008) might be a CV. C1951p186 |----------------------- C1951p186 |Huang etal. (2010) searched for HST counterparts to Chandra X-ray sources C1951p186 |in M71 and concluded that source #29 is a CV and that source #02 and #20 C1951p186 |are chromospherically active binaries. There were not successful in C1951p186 |identifying the optical counterpart for the MSP. # C2003m220 |V1-12 C2003m220 | Shapley (1920) with x,y coordinates and an ID chart C2003m220 | He also announced suspected variables V13-16, but Sawyer Hogg did C2003m220 | not include these four stars in any of her catalogues. Shapley's C2003m220 | V13-16 were referred to as S1-4 by Pinto et al. (1982) and also C2003m220 | by Samus et al. (2009) who derived their RA and dec. Pinto et al. C2003m220 | noted that they were probably not variable and this result was C2003m220 | confirmed by Corwin et al. (2003). C2003m220 |V13-17 C2003m220 | Pinto et al. (1982) with x,y coordinates and an ID chart C2003m220 |V18-47 = Corwin NV1-NV30 C2003m220 | Corwin et al (2003) with x,y coordinates C2003m220 |V48-51 = Scott NV1-NV4 C2003m220 | Scott et al. (2006) with x,y coordinates # C2031p072 |V1-51 C2031p072 | Sawyer, H. B. (1938) with x,y coordinates and an ID chart C2031p072 | Preliminary results were announced by Sawyer (1933, 1936) C2031p072 |V52-86 C2031p072 | Kaluzny et al. (2001) with RA, dec and indiviual finder charts # C2050m127 |V1-34 (V6, V19, V33 were supsected variables) C2050m127 | discovered by Ritchie and announced by Shapley (1920) with x,y C2050m127 | coordinates and an ID chart. C2050m127 | Kadla et al. (1995) later showed that V6, V19 and V33 are giant C2050m127 | branch stars. C2050m127 |V35-41 C2050m127 | Sawyer (1953) with x,y coordinates and an ID chart C2050m127 | In the course of deriving the RA and dec for V14, V29, V33, V41, C2050m127 | Samus et al. (2009) and Kadla et al. (1998) noted that there C2050m127 | were errors in the published positions for these variables in C2050m127 | earlier versions of our GC variable star catalogues. C2050m127 |V42 C2050m127 | Dickens & Flinn (1973) noted that they had discovered a new red C2050m127 | variable near the cluster centre. The number 42 was assigned and C2050m127 | x,y coordinates were listed by Sawyer Hogg (1973) in her 3rd C2050m127 | catalog, based on unpublished correspondence with Dickens. C2050m127 |V43-V49 = S3, S5, S7, S8, S9, R3, R4 C2050m127 | Kadla et al. (1995, 1996) with x,y coordinates in arcsec and an ID C2050m127 | chart in the 1996 paper. Approximately 33 of variables V1-42 were C2050m127 | also labelled on the ID charts by Kadla et al. (1996). C2050m127 | The numbers V43-49 were assigned by Bramich et al. (2011). C2050m127 | In their papers, Kadla et al. listed 9 suspected variables (S1-9) C2050m127 | and 7 possible RR Lyrae variables (R1-7), all based on their location C2050m127 | in the CMD. They did not detect any variations because their study was C2050m127 | based on one B frame and one V frame taken simultaneously. With their C2050m127 | more extensive data set, Bramich et al. detected variation only in the C2050m127 | seven listed here. The others are considered to be non-variable. C2050m127 |V50-56 C2050m127 | Bramich et al. (2011) with RA, dec and ID charts. They also published C2050m127 | RA, dec and ID charts for the other variables they analysed in their C2050m127 | study. C2050m127 |V57-58 C2050m127 | Skottfelt et al. (2013a) with RA, dec and an ID chart C2050m127 | Skottfelt et al. (2013b) later pointed out that the coordinates for C2050m127 | V57 and V58 had been switched in their original paper (2013a). The C2050m127 | corrected coordinates are listed in the table above. C2050m127 |V59-60 C2050m127 | Amigo et al. (2013) with RA and dec C2050m127 | (These two variables were outside the field of view of the study by C2050m127 | Bramich et al. 2011). C2050m127 |------------------------------------------------------------------------- C2050m127 |Lynch & Ransom (2011) conducted a search for pulsars, but did not find C2050m127 |any in NGC 6981. # C2059p160 | V1-11 C2059p160 | Shapley & Mayberry (1921) with x,y coordinates C2059p160 | They noted that V2 and V5 had been announced previously by C2059p160 | Shapley (1920). In the earlier study, V5 was numbered V1. C2059p160 | V12-43 C2059p160 | Discovered by Hubble and reported by Sandage (1954) with x,y C2059p160 | coordinates and an ID chart, based on Hubble's unpublished notes C2059p160 | The origin of his x,y coordinate system differed from that of C2059p160 | Shapley & Mayberry by a small amount. Sawyer (1955) published the C2059p160 | conversion. C2059p160 | Hubble also recovered 8 of Shapley's 11 variables. He concluded that C2059p160 | V4 and V7 were not variable and that the variabiity of V9 was C2059p160 | questionable. C2059p160 | V44-52 C2059p160 | Rosino & Mannino (1955) with x,y coordinates and an ID chart C2059p160 | Mannino (1957) derived periods for many of the variables, but did not C2059p160 | discover any new ones C2059p160 | V53-54 C2059p160 | Sandage & Wildey (1967) with ID chart C2059p160 | Many of the other known variables were also labelled on their chart. C2059p160 | Rosino & Ciatti (1967) published x,y coordinates for V53-54 C2059p160 | V55-75 C2059p160 | Rosino & Ciatti, Asiago Contr 199 (1967) C2059p160 | V76 C2059p160 | Wehlau et al. (1992) with ID chart C2059p160 | x,y coordinates were later derived by Gerashchenko (1999). C2059p160 |--------------------------------------------------------------------- C2059p160 | Gerashchenko (2006) announced two additional RR Lyrae candidates C2059p160 | based on their location in the BV and VR CM diagrams. He derived C2059p160 | their x,y, coordinates and published an ID chart. C2059p160 | He assigned the numbers V77 and V78 and listed V amplitudes of C2059p160 | 0.2 and 0.25 mag respectively. No periods were determined. # C2127p119 | V1-51 C2127p119 | Bailey (1902) with ID chart C2127p119 | V52-66 C2127p119 | Bailey et al. (1919) with x,y positions and ID chart for V1-66 C2127p119 | V67-95 C2127p119 | Rosino (1950) with x,y positions and ID chart C2127p119 | V96-98 C2127p119 | Izsak (1952) with Kustner numbers, x,y positions and ID chart C2127p119 | V99=Kustner 717 C2127p119 | Mannino (1956) with x,y position and Kustner number C2127p119 | V100-102 C2127p119 | Notni & Oleak (1958) with x,y positions for V100, 101, 102 and C2127p119 | Kustner numbers (626 and 867) for V100 and V102 C2127p119 | V103-105 C2127p119 | Tsoo (1961) with x,y positions and ID chart C2127p119 | Note: Tsoo (1961) and Chu (1977) are the same person. C2127p119 | V106-112 = Kustner 438, 424, 425, 633, 726, 777, 822 C2127p119 | Rosino (1969) with x,y positions and Kustner numbers C2127p119 | He also listed magnitude ranges and concluded that these C2127p119 | variables were all RR Lyrae type. C2127p119 | V113 C2127p119 | Silbermann & Smith (1995) with x,y position (on p707) and an ID C2127p119 | chart C2127p119 | When Kadla et al. (1984a) announced the discovery of V114-121, they C2127p119 | designated Kustner #1082, a variable announced by Chu (1977) as C2127p119 | V113, but in this catalogue, Chu's variable has been designated as C2127p119 | V122. C2127p119 | V114-121 C2127p119 | Kadla et al. (1984a) with x,y positions C2127p119 | They also pointed out that V114=Kustner 537, V118=K657, V120=K715, C2127p119 | and V121= K431. However, the x,y coordinates (0.91, 49.93) that C2127p119 | they listed for V114 were not the coordinates that Kustner published C2127p119 | for K537 ( wich were -8.56, -23.94). Later they published an erratum C2127p119 | (Kadla et al. 1984b) and noted that V114 should have been Kustner #579. C2127p119 | V114 in the above table is the variable that Corwin et al. (2008) C2127p119 | discovered at a position 2.69 arcseconds from the x,y position C2127p119 | originally listed for V114 by Kadla et al. (1984a). The "other V114" C2127p119 | (Kadla et al. 1984b) is Corwin's NV3. C2127p119 | V122=Kustner 1082 C2127p119 | Chu (1977) with x,y position and ID chart C2127p119 | He noted that x,y were measured relative to RA 21:27.6 C2127p119 | and dec +11:57 (1950) C2127p119 | The number V122 was assigned in the original electronic version of C2127p119 | this catalogue (Clement 1997). C2127p119 | V123&124 = Kustner 64 & 152 C2127p119 | Chu et al. (1984) with ID chart C2127p119 | The numbers V123 and V124 were assigned in the electronic C2127p119 | (Clement et al. 2001). C2127p119 | V125 = AC211 C2127p119 | Auriere et al. (1984) showed that this star was the optical C2127p119 | counterpart of the M15 X-ray source: X2127+119 C2127p119 | The number V125 was assigned in the electronic (Clement et al. 2001). C2127p119 | V126 =Kustner 1040 = S6 in ID chart of Sandage (1970) C2127p119 | Its variability was discovered by Yao (1990). C2127p119 | The number V126 was assigned in the electronic (Clement et al. 2001). C2127p119 | V127 = Kustner 1098 C2127p119 | Yao & Qin (1993) with x,y position C2127p119 | The number V127 was assigned in the electronic (Clement et al. 2001). C2127p119 | V128-142 = HST V1-11 and HST V13-16 C2127p119 | Ferraro & Paresce (1993) with x,y pixel positions C2127p119 | The variability of HST V12 was not confirmed by Butler et al. C2127p119 | (1998) or by Tuairisg et al. (2003). C2127p119 | The numbers V128-142 were assigned to these stars in our electronic C2127p119 | catalog (Clement et al. 2001). Zheleznyak & Kravtsov (2003) later C2127p119 | pointed out that the x-y (arcsec) coordinates we listed for these C2127p119 | stars were erroneous and published the correct values. C2127p119 | V143-155 = Butler #135, 1856, 2283, 2411, 2954, 7229, 7516, C2127p119 | 7600, 7964, 8807, 9245, 10039 & 10837 C2127p119 | Butler et al. (1998) with x,y pixel positions C2127p119 | The numbers V143-155 were assigned to these stars in our electronic C2127p119 | catalog (Clement et al. 2001). Zheleznyak & Kravtsov (2003) later C2127p119 | pointed out that the x-y (arcsec) coordinates listed for these C2127p119 | stars in the electronic catalogue were erroneous and published the C2127p119 | correct values. C2127p119 | V156 = SX1 C2127p119 | Jeon et al. (2000) with RA, dec and ID chart C2127p119 | The number V156 was assigned to this star in our 2001 C2127p119 | electronic catalog. C2127p119 | V157 & 158 = W1 & W2 C2127p119 | Jeon et al. (2001b) with RA, Dec and ID chart C2127p119 | The numbers V157 & 158 were assigned to these stars in our C2127p119 | 2002 update to the electronic catalog. C2127p119 | V159-181 C2127p119 | Tuairisg et al. (2003, MNRAS 345, 960) with RA, dec and C2127p119 | ID chart. C2127p119 | V159 is a blend of V17, 18 & 19 of Ferraro & Paresce (1993). C2127p119 | ZK variables C2127p119 | Zheleznyak & Kravtsov (2003) with x,y positions C2127p119 | Corwin et al. (2008, AJ 135, 1459) found that some of the ZK C2127p119 | variables were announced by Tuairisg et al.: C2127p119 | ZK6=V175, ZK10 = V174, ZK11=V173, ZK13=V172, ZK14= V181, ZK18=V162, C2127p119 | ZK22=V166, ZK23=V169, ZK32=V165, ZK37=V164, ZK39= V161, ZK44=V139, C2127p119 | ZK52=V160, ZK55=V178 and ZK64=V177. C2127p119 | For these stars, we have adopted the Tuairisg numbering system C2127p119 | and the ZK numbers are listed in the "Remarks" column. C2127p119 | NV variables C2127p119 | Corwin et al. (2008) with RA & dec C2127p119 | They listed 14 variables: NV1-14 C2127p119 | A comparison of RA and dec derived by Samus et al. (2009) for C2127p119 | previously known variables indicates that NV2=V107, NV5=V116, C2127p119 | NV7=V120, NV10=V102, NV12=V100, and NV14=V109. C2127p119 | K757, K825 C2127p119 | McDonald et al. (2010) with RA, dec and Kustner number C2127p119 | X-2 C2127p119 | White & Angelini (2001) with RA and dec C2127p119 | CV1 C2127p119 | Charles et al. New Astron. 7, 21 (2002) with ID chart C2127p119 | These authors discovered two additional variables thought to be RR C2127p119 | Lyrae variables. They labelled them on their ID chart. C2127p119 | CV2= Source C C2127p119 | Hannikainen et al. (2005) with RA & dec and ID chart C2127p119 | PSR: According to Paulo Freire's website, there are 8 millisecond C2127p119 | pulsars in M15. (www.naic.edu/~pfreire/GCpsr.html) C2127p119 |------------------ C2127p119 | Additional variables: C2127p119 | Dieball et al. (2007) detected 4 known (+ 13 candidate) RR Lyrae, C2127p119 | 1 known (+ 6 candidate) Cepheids, 1 known (+ 1 candidate) SXPHE C2127p119 | near the centre of M15 from FUV and NUV observations obtained C2127p119 | with HST. They labelled them all on an ID chart. C2127p119 | A number of these variables have also been detected by Diaz-Sanchez et C2127p119 | al. (2012) from high-resolution I-band imaging of the core. C2127p119 |------------------ C2127p119 |Kraemer et al. (2013) announced that they are making optical and C2127p119 |near-infrared observations in order to identify the long period variables C2127p119 |on the AGB. # C2130m010 | V1-10 C2130m010 | Bailey (1902) with x,y positions (p 244) and ID chart C2130m010 | (Plate XII, Fig. 3) C2130m010 | V11 C2130m010 | announced by Chevremont (1897) with ID chart (1898) C2130m010 | This star was designated V11 by Sawyer (1935) C2130m010 | V12-17 C2130m010 | Sawyer (1935) with ID chart for V1-17 C2130m010 | and x,y positions for V11-17 listed by Sawyer (1938) C2130m010 | V18-21 C2130m010 | Margoni & Stagni (1967) with x,y positions and (1969) with ID C2130m010 | chart C2130m010 | V22-34 C2130m010 | Lee & Carney (1999) with ID chart C2130m010 | V22-34 = LC 184, 301, 450, 456, 608, 651, 708, C2130m010 | 715, 733, 798, 864, 939, 1047 respectively C2130m010 | The numbers V22-34 were assigned in our electronic catalogue ------------------------------------------------------------------------------------------------ #***Output truncated to 3728 records