Cluster |
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3
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Ref. |
mag | ![]() |
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||
NGC 2477 | 17.00 | 95 | 1.0 | 152 |
NGC 2477 | 17.00 | 95 | 1.0 | 152 |
NGC 7044 | 21.75 | 95 | 1.0 | 62 |
NGC 2266 | 18.75 | 95 | 1.5 | 41 |
Berkeley 32 | 20.25 | 95 | 1.5 | 40 |
NGC 2682 | 18.00 | 98 | 1.5 | 335 |
18.00 | 99 | 1.5 | 31 | |
18.00 | 98 | 1.5 | 54 | |
NGC 2506 | 18.00 | 98 | 1.5 | 284 |
17.75 | 98 | 1.5 | 163 | |
NGC 2355 | 19.75 | 98 | 1.0 | 217 |
18.25 | 98 | 1.0 | 44 | |
Melotte 105 | 16.75 | 98 | 1.5 | 289 |
16.75 | 98 | 1.5 | 32 | |
Trumpler 1 | 19.00 | 85 | 1.5 | 320 |
19.00 | 95 | 1.5 | 86 |
Notes.
is the adopted cut-off in magnitude in V,
is the density of stars in the observed field as a function of radius determined from the cluster center and 3
is the photometric error as described in the text.
References. 152 = Kassis et al. (1997); 62 = Aparicio et al. (1993);
41 = Kaluzny & Mazur (1991); 40 = Kaluzny & Mazur (1991);
335 = Henden 2003; 31 = Gilliland et al. (1991);
54 = Montgomery et al. (1993) (adopted
);
284 = Kim et al. (2001) (adopted mean values: see Table 5 of the paper);
163 = Marconi et al. (1997); 217 = Ann et al. (1999); 44 = Kaluzny & Mazur (1991); 289 = Sagar et al. (2001); 32 = Kjeldsen & Frandsen (1991); 320 = Yadav & Sagar (2002); 86 = Phelps & Janes (1994).
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