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Table 1

Observed sample of GCs and main parameters.

Cluster [Fe/H]d (m − M)0 a E(B − V)a [M/H]b HBc t exp d
NGC 288 −1.07 14.73 0.03 −1.00 E 1.10 h
NGC 362 −1.15 14.68 0.05 −0.94 N 1.10 h
NGC 1851 −1.08 15.46 0.02 −0.87 E 2.05 h
NGC 2808 −1.15 14.90 0.23 −0.94 E 2.05 h
NGC 5272 (M3) −1.34 15.03 0.01 −1.13 N 2.05 h
NGC 6093 (M80) −1.41 14.96 0.18 −1.20 E 2.05 h
NGC 6205 (M13) −1.39 14.43 0.02 −1.18 E 1.10 h
NGC 6341 (M92) −2.16 14.78 0.02 −1.95 N 1.10 h
NGC 6388 −0.61 15.30 0.44 −0.40 E 2.05 h
NGC 6539 −0.66 e 14.62 1.08 −0.45 N 1.10 h
NGC 6440 −0.56 e 14.48 1.15 −0.35 N 1.10 h
NGC 6441 −0.50 e 15.26 0.52 −0.29 E 2.05 h
NGC 6752 −1.42 13.18 0.04 −1.21 E 0.90 h
NGC 7078 (M15) −2.12 15.15 0.09 −1.91 E 2.05 h
NGC 7099 (M 30) −1.91 14.71 0.03 −1.00 N 1.10 h

Notes.

(a)

Cluster metallicity, reddening, and distance modulus from Ferraro et al. (1999a, 2000) and Valenti et al. (2007).

(b)

Cluster global metallicity computed using the formula ([ M / H ] = [ Fe / H ] + log 10(0.638 × fα + 0.362), by assuming an overall [α/ Fe ] = + 0.3 enhancement (i.e., fα = 2) (see Salaris et al. 1993; Ferraro et al. 1999a).

(c)

HB morphology: N = normal (red and blue if metal-poor clumps), E = extended (blue tails).

(d)

Total exposure time for our IRAC mapping, according to the AOR duration estimated with SPOT–v11.07.

(e)

Cluster metallicity from high-resolution IR spectroscopy by Origlia et al. (2005) and Origlia et al. (2008).

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