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Table B.1

Data for star clusters that have been searched for the Na-O anti-correlation or multiple populations in the colour-magnitude diagram.

Class Object Alt. name M r h a C 5 b Age [Fe/H] MPsc Ref.
(105 M) (pc) (Gyr)

GC NGC 104 47 Tuc 6.46 7.1 0.92 12.8 –0.76 Y 1, 2, 3, 4
GC NGC 288 Melotte 3 0.46 9.8 0.05 12.2 –1.32 Y 1, 2, 3, 4
GC NGC 362 Dunlop 62 2.5 3.5 0.72 10 –1.26 Y 2, 3, 4, 5
GC NGC 1261 Caldwell 87 3.41 5.5 0.62 10.24 –1.08 Y 2, 4, 6, 7
GC NGC 1851 Dunlop 508 5.51 3.05 1.81 7.64 –1.13 Y 2, 4, 6, 8
GC NGC 1904 M79 1.45 4.1 0.50 12.0 –1.58 Y 1, 2, 9
GC NGC 2298 Dunlop 578 0.85 3.1 0.16 12.4 –1.98 Y 2, 4, 6, 8
GC NGC 2808 Dunlop 265 12.3 3.8 3.24 11.2 –1.18 Y 1, 2, 3, 4
GC NGC 3201 Dunlop 445 1.1 7.5 0.15 11.1 –1.51 Y 1, 2, 4, 10
GC NGC 4590 M68 1.07 7.7 0.14 12.7 –2.27 Y 1, 2, 3, 4
GC NGC 4833 Dunlop 164 4.10 7.9 0.52 12.5 –1.71 Y 2, 4, 6, 7
GC NGC 5024 M53 8.26 11.6 0.71 12.7 –1.86 Y 2, 4, 6, 7
GC NGC 5053 1.25 22.5 0.056 12.3 –1.98 Y 2, 4, 6, 7
GC NGC 5272 M3 4.68 11.7 0.40 11.4 –1.34 Y 2, 3, 4, 7
GC NGC 5286 7.13 4.2 1.69 12.5 –1.41 Y 2, 3, 4, 7
GC NGC 5466 1.79 18.2 0.098 13.6 –2.20 Y 2, 4, 6, 7
GC NGC 5897 2.11 12.7 0.17 12.3 –1.73 Y 2, 4, 6, 7
GC NGC 5904 M5 3.89 6.6 0.59 11.5 –1.33 Y 1, 2, 3, 4
GC NGC 5927 3.38 4.2 0.81 12.7 –0.64 Y 2, 4, 6, 7
GC NGC 5986 5.99 5.04 1.19 12.2 –1.35 Y 2, 4, 6, 7
GC NGC 6093 M80 5.02 3.02 1.66 12.5 –1.47 Y 2, 4, 6, 7
GC NGC 6101 Caldwell 107 1.0 8.00 0.13 12.5 –1.76 Y 2, 4, 7, 11
GC NGC 6121 M4 1.17 4.7 0.25 13.1 –1.98 Y 1, 2, 3, 4
GC NGC 6139 3.80 4.2 0.90 11.6 –1.58 Y 1, 2, 12
GC NGC 6144 1.69 7.17 0.24 13.8 –1.56 Y 2, 4, 6, 7
GC NGC 6171 M107 1.17 5.5 0.21 13.4 –1.03 Y 1, 2, 4, 13, 14,
GC NGC 6205 M13 7.75 5.93 1.31 11.7 –1.33 Y 2, 4, 6, 7
GC NGC 6218 M12 0.74 4.2 0.18 13.4 –1.43 Y 1, 2, 3, 4
GC NGC 6254 M10 1.53 4.2 0.36 12.4 –1.57 Y 1, 2, 4, 15
GC NGC 6304 2.17 4.14 0.52 13.6 –0.66 Y 2, 4, 6, 7
GC NGC 6341 M92 4.89 4.19 1.17 13.2 –2.16 Y 2, 4, 6, 7
GC NGC 6352 0.37 5.68 0.065 12.7 –0.70 Y 2, 4, 7, 16
GC NGC 6362 0.81 7.70 0.11 13.6 –0.99 Y 2, 4, 7, 16
GC NGC 6366 0.30 5.05 0.058 13.3 –0.73 Y 2, 4, 7, 16
GC NGC 6388 12 2.5 4.8 11.7 –0.45 Y 1, 2, 4, 17
GC NGC 6397 1.1 3.3 0.33 13.4 –1.99 Y 1, 2, 4, 18
GC NGC 6441 9.55 3.3 2.92 11.2 –0.44 Y 1, 2, 3, 4
GC NGC 6496 2.00 5.70 0.35 12.4 –0.70 Y 2, 4, 6, 7
GC NGC 6535 0.20 2.86 0.070 10.5 –1.51 Y 2, 4, 6, 7
GC NGC 6541 5.72 3.93 1.45 12.9 –1.53 Y 2, 4, 6, 7
GC NGC 6584 3.03 4.87 0.62 11.3 –1.30 Y 2, 4, 6, 7
GC NGC 6624 2.57 3.20 0.80 12.5 –0.70 Y 2, 4, 6, 7
GC NGC 6637 M69 2.00 3.66 0.55 13.1 –0.78 Y 2, 4, 7, 19
GC NGC 6652 1.09 2.37 0.46 12.0 –0.97 Y 2, 4, 6, 7
GC NGC 6656 M22 6.44 5.32 1.21 12.7 –1.49 Y 2, 4, 6, 7
GC NGC 6681 M70 1.79 3.16 0.57 12.8 –1.35 Y 2, 4, 6, 7
GC NGC 6715 M54 12.9 10.7 1.20 10.8 –1.25 Y 2, 3, 4, 7
GC NGC 6717 0.48 2.39 0.20 13.2 –1.09 Y 2, 4, 6, 7
GC NGC 6723 3.57 6.58 0.54 13.1 –0.96 Y 2, 4, 6, 7
GC NGC 6752 2.82 3.8 0.75 13.8 –1.55 Y 1, 2, 3, 4
GC NGC 6779 M56 2.30 5.11 0.45 13.7 –2.00 Y 2, 4, 6, 7
GC NGC 6809 M55 0.55 7.6 0.07 13.8 –1.93 Y 1, 2, 3, 4
GC NGC 6838 M71 0.20 3.3 0.06 12.7 –0.82 Y 1, 2, 3, 4
GC NGC 6934 2.95 5.32 0.55 11.1 –1.32 Y 2, 4, 6, 7
GC NGC 6981 M72 1.68 7.82 0.21 10.9 –1.21 Y 2, 4, 6, 7
GC NGC 7078 M15 5.13 5.1 1.00 13.6 –2.33 Y 1, 2, 3, 4
GC NGC 7089 M2 5.75 6.03 0.95 11.8 –1.31 Y 2, 3, 4, 7
GC NGC 7099 M30 1.45 4.1 0.35 14.6 –2.33 Y 1, 2, 3, 4
GC Ruprecht 106 0.68 11 0.06 12 –1.5 N 2, 20
GC Terzan 7 0.39 8.7 0.04 7.4 –0.12 N 1, 2, 21, 22
GC Palomar 12 0.28 16 0.024 8.6 –0.81 N 1, 2, 21
OC Berkley 39 0.2 11 0.018 6 –0.21 N 23, 24
OC Collinder 261 0.01 2d 0.005 6 –0.03 N 24, 25, 26
OC Melotte 25 Hyades 0.004 3.7 0.001 0.6 +0.13 N 27, 28, 29, 30
OC Melotte 111 Coma Berenices 0.001 3.5 0.0003 0.5 +0.07 N 27, 29, 31, 32
OC NGC 752 0.001 1.4 0.0009 1.12 –0.02 N 29, 33, 34
OC NGC 1817 Collinder 4a 0.02 7 0.002 1 –0.11 N 27, 32, 34, 35, 36
OC NGC 2360 Melotte 64 0.018 2 0.009 0.56 –0.07 N 29, 34, 37
OC NGC 2506 Collinder 170 0.03 15 0.002 1.11 –0.19 N 29, 34, 38, 39
OC NGC 2682 M67 0.01 2.5 0.004 4.4 +0.05 N 29, 40, 41
OC NGC 3114 0.0016 8 0.0002 0.16 –0.01 N 24, 29, 36, 42
OC NGC 6134 0.0008 2 0.0004 0.7 + 0.12 N 24, 29, 43, 44
OC NGC 6253 Melotte 156 0.007 2 0.0035 4 +0.4 N 24, 26, 29
OC NGC 6475 M 7 0.007 6 0.001 0.3 +0.14 N 29, 32, 36
OC NGC 6705 0.1 1.2 0.08 0.3 +0.10 N 21
OC NGC 6791 Berkeley 46 0.5 5 0.1 7.5 +0.30 N 29, 45, 46
OC NGC 7789 Melotte 245 0.06 5 0.01 1.6 +0.04 N 29, 36, 41, 47
OC IC 4651 Melotte 169 0.006 2 0.003 1.1 +0.15 N 24, 29, 36, 48
Fornax For 3 5.2 7.2 0.72 13 –2.33 Y 49
Fornax For 5 3.2 8.5 0.38 13 –2.09 Y 49
LMC NGC 1651 0.8 22 0.04 1.5 –0.3 N 50, 51, 52
LMC NGC 1783 2.5 19 0.13 1.4 –0.3 N 50, 51, 52
LMC NGC 1786 3.7 6.0 0.62 13 –1.75 Y 53, 54, 55
LMC NGC 1806 1.3 15 0.08 1.4 –0.3 N 50, 56, 57
LMC NGC 1846 1.7 15 0.11 1.4 –0.3 N 50, 56, 58
LMC NGC 1866 0.8 19 0.04 0.2 –0.3 N 50, 59, 60, 61
LMC NGC 1978 2.0 8.7 0.23 2.0 –0.3 N 50, 51, 62, 63, 64, 65
LMC NGC 2173 0.5 11 0.05 1.6 –0.3 N 50, 51, 52
LMC NGC 2210 3.0 5.9 0.51 13 –1.65 Y 53, 54, 55
LMC NGC 2257 2.6 19 0.14 13 –1.95 Y 53, 54, 55
Scutum red supergiant cluster 1 0.32 2.6 0.12 0.012 –0.15 N 66, 67
Scutum red supergiant cluster 2 0.40 4.6 0.087 0.017 –0.15 N 66, 67

Notes.

(a)

Half-mass radii were computed from the half-light radii (apparent size was taken as equivalent to half-light radii) from the literature, assuming a Plummer model for the cluster.

(b)

Compactness M/rh in units of 105 M/pc.

(c)

Y: possesses multiple populations; N: multiple populations have been searched for, but not found.

(d)

Estimated from Fig. 5 in Ref. (16).

Reference. (1) Carretta et al. (2010); (2) Harris (1996, 2010 edition); (3) Kimmig et al. (2015); (4) Piotto et al. (2015): (5) Lebzelter & Wood (2011); (6) Boyles et al. (2011); (7) Forbes & Bridges (2010); (8) Koleva et al. (2008); (9) Lützgendorf et al. (2013); (10) Mucciarelli et al. (2015); (11) Caloi & D’Antona (2011); (12) Bragaglia et al. (2015) (13) Conroy (2012); (14) Piatek et al. (1994); (15) Zocchi et al. (2012) (16) Mandushev et al. (1991); (17) Lanzoni et al. (2013); (18) Heyl et al. (2012); (19) Miocchi (2007) (20) Villanova et al. (2013); (21) Cantat-Gaudin et al. (2014); (22) Salaris & Weiss (2002); (23) Bragaglia et al. (2012); (24) Tadross (2001) (25) Bragaglia & Tosi (2006) (26) Mikolaitis et al. (2012); (27) Casewell et al. (2014); (28) Lodieu et al. (2014); (29) MacLean et al. (2015); (30) Portegies Zwart et al. (2001) (31) Gebran et al. (2008) (32) Becker & Fenkart (1971); (33) Francic (1989); (34) Reddy et al. (2012); (35) Donati et al. (2014); (36) Gozha et al. (2012); (37) Güneş et al. (2012); (38) Lee et al. (2013); (39) Marconi et al. (1997); (40) Hurley et al. (2005); (41) Pancino et al. (2010); (42) Santrich et al. (2013); (43) Smiljanic et al. (2009) (44) Mikolaitis et al. (2010) (45) Bragaglia et al. (2014) (46) Platais et al. (2011); (47) Wu et al. (2009) (48) Mikolaitis et al. (2011); (49) Larsen et al. (2012); (50) Goudfrooij et al. (2014); (51) Mucciarelli et al. (2008); (52) Niederhofer et al. in prep; (53) Mackey & Gilmore (2003) (54) Mucciarelli et al. (2009); (55) Mucciarelli et al. (2010) (56) Bastian & Niederhofer (2015); (57) Mucciarelli et al. (2014); (58) Mackey et al. (in prep.); (59) Bastian & Silva-Villa (2013); (60) Mucciarelli et al. (2011); (61) Niederhofer et al. (2015); (62) Ferraro et al. (2006); (63) Miloneet al. (2009); (64) Mucciarelli et al. (2007); (65) Werchan & Zaritsky (2011); (66) Davies et al. (2009); (67) Portegies Zwart et al. (2010).

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