Table 3
Clusters sample intrinsic properties and structural parameters.
| Name | [Fe/H] | HBR |  ) |
Agel | ε | σ o | c | r t | rh/rJp |
|
|
M/L | ||||||
| (dex) | (oK) | (Gyr) | (km s-1) | (′) | (′) | (mag) | (dex) | (M⊙  ) |
||||||||||
|
|
||||||||||||||||||
| NGC 104 (47 Tuc) | −0.75a | −0.99 | 3.756i | 13.06 | 0.09 | 11.5n | 2.03 | 42.86 | − | −9.42 | 6.05q | 1.33q | ||||||
| NGC 288 | −1.26a | 0.98 | 4.221j | 10.62 | 0.09m | 2.9n | 0.96 | 12.94 | 0.093 | −6.74 | 4.85q | 2.15q | ||||||
| NGC 362 | −1.33b | −0.87h | 4.079i | 10.37 | 0.01 | 6.4n | 1.94 | 16.11 | 0.023 | −8.41 | 5.53q | 0.90r | ||||||
| NGC 1851 | −1.22c | −0.32h | 4.097i | 9.98 | 0.05 | 10.4n | 2.32 | 11.70 | 0.015 | −8.33 | 5.49q | 1.61q | ||||||
| NGC 5927 | −0.67d | −1.00 | 3.724i | 12.67 | 0.04 | 4.3o | 1.60 | 16.68 | − | −7.80 | 5.32r | − | ||||||
| NGC 6352 | −0.55e | −1.00 | − | 12.67 | 0.07 | 5.4o | 1.10 | 10.51 | − | −6.48 | 4.57r | − | ||||||
| NGC 6388 | −0.41a | −0.69h | 4.255i | 12.03 | 0.01 | 18.9n | 1.70 | 6.21 | − | −9.42 | 6.02q | 1.89q | ||||||
| NGC 6656 (M 22) | −1.76f | 0.91h | − | 12.67 | 0.14 | 9.0n | 1.31 | 28.97 | − | −8.50 | 5.56q | 2.07q | ||||||
| NGC 6752 | −1.56a | 1.00 | 4.471j | 11.78 | 0.04 | 4.5n | 2.50 | 55.34 | − | −7.73 | 5.16r | − | ||||||
| NGC 6809 (M 55) | −1.97a | 0.87 | 4.153j | 12.29 | 0.02 | 4.9n | 0.76 | 16.28 | − | −7.55 | 4.99q | 3.23q | ||||||
| NGC 7078 (M 15) | −2.34a | 0.67h | 4.477i | 12.93 | 0.05 | 12.0n | 2.50 | 21.50 | 0.027 | −9.17 | 5.84r | − | ||||||
| Pal 12 | −0.80g | −1.00 | − | 8.83 | − | 1.3o | 1.94 | 17.42 | 0.193 | −4.48 | 3.75q | − | ||||||
Notes. All parameters are derived from the 2003 revision of the Harris (1996) GGC catalogue except:
relative ages by Marín-Franch et al. (2009) converted to absolute ages multiplying by 12.8 Gyr;
Meaning of columns. (1) Cluster name (alternate name in parenthesis); (2) mean iron abundance ratio; (3) HB morphology, where HBR = (B − R)/(B + V + R), being B the number of stars bluer than the instability strip, R redder, and V the number of variables in the strip; (4) the maximum temperature of the HB; (5) the age in Gyr; (6) the isophotal ellipticity ϵ = 1 − (b/a); (7) the central radial velocity dispersion; (8) the concentration (2.5 means core collapsed cluster); (9) the tidal radius; (10) the ratio between the half-light and the Jacobi radius; (11) the integrated V magnitude; (12) the logarithm of the total mass in solar units; (12) the mass-to-light radius in solar units.
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