Table 9
Information on MW GCs and OCs for which multiple populations have been studied.
| Cluster | [Fe/H] | M V | Age | Log M | MP? | Ref. for MPs |
|
|
||||||
| NGC 104 | –0.72 | –9.42 | 0.98 | 6.05 | Y | 1, 2 |
| NGC 288 | –1.32 | –6.75 | 0.94 | 4.85 | Y | 1, 2 |
| NGC 362 | –1.26 | –8.43 | 0.84 | 5.53 | Y | 3 |
| NGC 1851 | –1.18 | –8.33 | 0.85 | 5.49 | Y | 4, 5 |
| NGC 1904 | –1.60 | –7.86 | 0.92 | 5.20 | Y | 1, 2 |
| NGC 2808 | –1.14 | –9.39 | 0.87 | 5.93 | Y | 6 |
| NGC 3201 | –1.59 | –7.45 | 0.85 | 5.04 | Y | 1, 2 |
| NGC 4147 | –1.80 | –6.17 | 0.97 | 4.66 | Y | 7 |
| NGC 4372 | –2.17 | –7.79 | 0.98 | Y | 8 | |
| NGC 4590 | –2.23 | –7.37 | 0.91 | 4.96 | Y | 1, 2 |
| NGC 4833 | –1.85 | –8.17 | 1.01 | Y | 9 | |
| NGC 5024 | –2.10 | –8.71 | 1.02 | 5.65 | Y | 10, 11 |
| NGC 5053 | –2.27 | –6.76 | 0.98 | 4.80 | Y | 12 |
| NGC 5139 | –1.53 | –10.26 | 0.89 | 6.37 | Y | 13, 14 |
| NGC 5272 | –1.50 | –8.88 | 0.90 | 5.58 | Y | 15, 16, 17 |
| NGC 5286 | –1.69 | –8.74 | 1.04 | 5.65 | Y | 18 |
| Pal5 | –1.41 | –5.17 | 0.85 | 4.17 | Y | 19 |
| NGC 5466 | –1.98 | –6.98 | 1.03 | 4.77 | Y | 10 |
| NGC 5634 | –1.88 | –7.69 | 0.96 | 5.14 | Y | 20 |
| NGC 5694 | –1.98 | –7.83 | 1.05 | 5.33 | Y | 21 |
| NGC 5824 | –1.91 | –8.85 | 1.00 | 5.81 | Y | 22 |
| NGC 5927 | –0.49 | –7.81 | 0.90 | Y | 23 | |
| NGC 5897 | –1.90 | –7.23 | 1.04 | 5.01 | Y | 24 |
| NGC 5904 | –1.29 | –8.81 | 0.89 | 5.65 | Y | 1, 2 |
| NGC 5986 | –1.59 | –8.44 | 0.99 | Y | 25 | |
| NGC 6093 | –1.75 | –8.23 | 1.03 | 5.44 | Y | 26 |
| NGC 6121 | –1.16 | –7.19 | 1.01 | 5.06 | Y | 1, 2 |
| NGC 6139 | –1.65 | –8.36 | 0.92 | 5.51 | Y | 27 |
| NGC 6171 | –1.02 | –7.12 | 1.03 | 4.90 | Y | 1, 2 |
| NGC 6205 | –1.53 | –8.55 | 1.04 | 5.57 | Y | 16, 17 |
| NGC 6218 | –1.37 | –7.31 | 1.03 | 4.95 | Y | 28 |
| NGC 6254 | –1.56 | –7.48 | 0.95 | 5.18 | Y | 1, 2 |
| NGC 6266 | –1.18 | –9.18 | 0.93 | 5.86 | Y | 29, 30 |
| NGC 6273 | –1.74 | –9.13 | 1.01 | 5.84 | Y | 31 |
| NGC 6341 | –2.31 | –8.21 | 1.06 | 5.43 | Y | 10 |
| NGC 6352 | –0.64 | –6.47 | 0.88 | Y | 32 | |
| NGC 6362 | –0.99 | –6.95 | 0.98 | 5.03 | Y | 33 |
| NGC 6366 | –0.59 | –5.74 | 0.93 | 4.78 | Y | 34 |
| NGC 6388 | –0.55 | –9.41 | 0.90 | 6.02 | Y | 35, 1 |
| NGC 6397 | –2.02 | –6.64 | 1.00 | Y | 1, 2 | |
| NGC 6440 | –0.36 | –8.75 | 0.74 | 5.77 | Y | 36 |
| NGC 6441 | –0.46 | –9.63 | 0.85 | 6.16 | Y | 37, 38 |
| NGC 6528 | –0.11 | –6.57 | 0.89 | 5.08 | Y | 39 |
| NGC 6535 | –1.79 | –4.75 | 0.87 | 3.53 | Y | This paper |
| NGC 6553 | –0.18 | –7.77 | 0.93 | 5.50 | Y | 39, 40 |
| NGC 6626 | –1.32 | –8.16 | 1.04 | Y | 41 | |
| NGC 6637 | –0.64 | –7.64 | 0.94 | 5.39 | Y | 42 |
| NGC 6656 | –1.70 | –8.50 | 1.08 | 5.56 | Y | 43, 44 |
| NGC 6681 | –1.62 | –7.12 | 0.99 | Y | 45, 46 | |
| NGC 6712 | –1.02 | –7.50 | 0.89 | 5.23 | Y | 47 |
| NGC 6715 | –1.49 | –9.98 | 0.90 | 6.29 | Y | 48, 49 |
| NGC 6723 | –1.10 | –7.83 | 1.05 | 5.28 | Y | 50 |
| NGC 6752 | –1.54 | –7.73 | 1.05 | Y | 51 | |
| NGC 6809 | –1.94 | –7.57 | 1.03 | 4.99 | Y | 1, 2 |
| NGC 6838 | –0.78 | –5.61 | 0.96 | Y | 1, 2 | |
| NGC 6864 | –1.29 | –8.57 | 0.85 | 5.65 | Y | 52 |
| Terzan8 | –2.16 | –5.07 | 0.96 | Y | 53 | |
| NGC 7006 | –1.52 | –7.67 | 0.91 | 5.20 | Y | 54 |
| NGC 7078 | –2.37 | –9.19 | 0.98 | Y | 1, 2 | |
| NGC 7089 | –1.65 | –9.03 | 0.99 | 5.84 | Y | 55 |
| NGC 7099 | –2.27 | –7.45 | 1.06 | Y | 1, 2 | |
| NGC 7492 | –1.78 | –5.81 | 0.96 | 4.44 | Y | 56 |
| Terzan5 | –0.23 | –7.42 | 0.89 | Y | 39 | |
| NGC 1261 | –1.27 | –7.80 | 0.83 | 5.20 | P | 46, 57 |
| NGC 2298 | –1.92 | –6.31 | 1.01 | 4.49 | P | 46, 57 |
| NGC 2419 | –2.15 | –9.42 | 0.89 | 5.96 | P | 58, 59, 60, 61 |
| NGC 6101 | –1.98 | –6.94 | 1.00 | 4.76 | P | 46, 57 |
| NGC 6304 | –0.45 | –7.30 | 0.83 | P | 46, 57 | |
| NGC 6496 | –0.46 | –7.20 | 0.88 | 4.76 | P | 46, 57 |
| NGC 6541 | –1.81 | –8.52 | 1.06 | 5.32 | P | 62, 46, 57 |
| NGC 6584 | –1.50 | –7.69 | 0.92 | 5.02 | P | 46, 57 |
| NGC 6624 | –0.44 | –7.49 | 0.89 | P | 46, 57 | |
| NGC 6652 | –0.81 | –6.66 | 0.95 | 4.76 | P | 46, 57 |
| NGC 6717 | –1.26 | –5.66 | 1.04 | P | 46, 57 | |
| NGC 6779 | –1.98 | –7.41 | 1.10 | 5.17 | P | 46, 57 |
| NGC 6934 | –1.47 | –7.45 | 0.91 | 5.20 | P | 63, 46, 57 |
| NGC 6981 | –1.42 | –7.04 | 0.90 | 5.00 | P | 46, 57 |
| Pal6 | –0.91 | –6.79 | Y? | 39 | ||
| NGC 6333 | –1.77 | –7.95 | 0.89 | 5.53 | Y? | 64 |
| NGC 6426 | –2.15 | –6.67 | 0.96 | Y? | 65 | |
| NGC 6522 | –1.34 | –7.65 | 1.00 | Y? | 39 | |
| NGC 6342 | –0.55 | –6.42 | 0.94 | Y? | 34 | |
| HP1 | –1.00 | –6.46 | 1.01 | Y? | 66 | |
| Pal3 | –1.63 | –5.69 | 0.85 | 4.65 | Y? | 67 |
| Pal14 | –1.62 | –4.80 | 0.78 | 4.09 | N? | 68 |
| Pal12 | –0.85 | –4.47 | 0.67 | 3.75 | N/P | 69, 70 |
| E3 | –0.83 | –4.12 | 0.95 | N | 71 | |
| Terzan7 | –0.32 | –5.01 | 0.55 | 4.74 | N | 72, 73 |
| Rup106 | –1.68 | –6.35 | 0.81 | N | 74 | |
| Pal1 | –0.65 | –2.52 | 0.54 | 3.67 | N | 75 |
|
|
||||||
| NGC 6791 | +0.40 | –4.14 | 0.59 | N | 76, 77, 78 | |
| Berkeley39 | –0.20 | –4.24 | 0.48 | N | 79 | |
| Trumpler20 | +0.17 | 0.11 | N | 80 | ||
| NGC 6705 | +0.10 | –6.00 | 0.02 | N | 81 | |
| Berkeley81 | +0.23 | –4.70 | 0.07 | N | 82 | |
| Trumpler23 | +0.14 | 0.06 | N | 83 | ||
| NGC 6802 | +0.10 | 0.07 | N | 84 | ||
| NGC 2420 | –0.16 | –3.44 | 0.15 | N | 85 | |
| NGC 7789 | +0.03 | 0.12 | N | 86 | ||
| Collinder261 | –0.03 | –2.87 | 0.44 | N | 87 | |
| NGC 752 | –0.02 | 0.12 | N | 88 | ||
| NGC 2682 | +0.03 | –3.16 | 0.30 | N | 89 | |
Notes. Metallicity and MV for GCs come from Harris (1996); Age = relative age come from Carretta et al. (2010a) or from individual papers; Log M = Log(mass) come from McLaughlin & van der Marel (2005). The reference for presence of multiple stellar populations is to our homogeneous FLAMES survey or to the first paper(s) presenting evidence for this survey. The codes for multiple populations are Y = evidence from high-resolution spectroscopy (i.e. O, Na; Mg, Al); Y? = dubious but probable; N? = dubious but improbable; N = not present; P = present, on the basis of low-resolution spectroscopy or photometric data (i.e. CN, CH; split/spread sequences). Values for MV for OCs come from Lata et al. (2002), relative age and metallicity from the individual papers. APO stands for APOGEE, GES for Gaia-ESO survey.
Reference. (1) Carretta et al. (2009a); (2) Carretta et al. (2009b); (3) Carretta et al. (2013b); (4) Carretta et al. (2010d); (5) Carretta et al. (2011a); (6) Carretta (2006); (7) Villanova et al. (2016); (8) San Roman et al. (2015); (9) Carretta et al. (2014b); (10) Mészáros et al. (2015); (11) Boberg et al. (2016); (12) Boberg et al. (2015); (13) Johnson & Pilachowski (2010); (14) Marino et al. (2011); (15) Cohen (1978); (16) Kraft et al. (1992); (17) Cohen & Meléndez (2005b); (18) Marino et al. (2015); (19) Smith et al. (2002); (20) Carretta et al. (2017); (21) Mucciarelli et al. (2013); (22) Roederer et al. (2016); (23) Pancino et al. (2017); (24) Koch & McWilliam (2014); (25) Johnson et al. (2017); (26) Carretta et al. (2015); (27) Bragaglia et al. (2015); (28) Carretta et al. (2007b); (29) Yong et al. (2014a); (30) Lapenna et al. (2015); (31) Johnson et al. (2015); (32) Feltzing et al. (2009); (33) Mucciarelli et al. (2016); (34) Johnson et al. (2016); (35) Carretta et al. (2007c); (36) Muñoz et al. (2017); (37) Gratton et al. (2006); (38) Gratton et al. (2007); (39) Schiavon et al. (2017); (40) Tang et al. (2017a); (41) Villanova et al. (2017); (42) Lee (2007); (43) Cohen (1981); (44) Marino et al. (2009); (45) O’Malley et al. (2017); (46) Soto et al. (2017); (47) Yong et al. (2008); (48) Carretta et al. (2010b); (49) Carretta et al. (2010c); (50) Gratton et al. (2015); (51) Carretta et al. (2007a); (52) Kacharov et al. (2014); (53) Carretta et al. (2014a); (54) Kraftet al. (1998); (55) Yong et al. (2014b); (56) Cohen & Melendez (2005a); (57) Milone et al. (2017); (58) Cohen & Kirby (2012) (59) Mucciarelli et al. (2012); (60) Beccari et al. (2013); (61) Frank et al. (2015); (62) Geisler (1988); (63) Smith & Bell (1986); (64) Johnson et al. (2013); (65) Hanke et al. (2017); (66) Barbuy et al. (2016); (67) Koch et al. (2009); (68) Çalışkan et al. (2012); (69) Cohen (2004); (70) Pancino et al. (2010); (71) Salinas & Strader (2015); (72) Tautvaišienė et al. (2004); (73) Sbordone et al. (2005); (74) Villanova et al. (2013); (75) Sakari et al. (2011); (76) Bragaglia et al. (2014); (77) Cunha et al. (2015) (APO); (78) Geisler et al. (2012); (79) Bragaglia et al. (2012); (80) Donati et al. (2014) (GES); (81) Cantat-Gaudin et al. (2014b) (GES); (82) Magrini et al. (2015) (GES); (83) Overbeek et al. (2017) (GES); (84) Tang et al. (2017b) (GES); (85) Souto et al. (2016) (APO); (86) Overbeek et al. (2015); (87) De Silva et al. (2007); (88) Böcek Topcu et al. (2015); (89) Randich et al. (2006).
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