|Authors||L. Prisinzano(1), G. Micela(2), S. Sciortino(2) and F. Favata(3)|
|Affiliation||(1) Dipartimento di Scienze Fisiche ed Astronomiche, UniversitÓ di Palermo, Piazza del Parlamento 1, I-90134 Palermo Italy|
(2) INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo Italy
(3) Astrophysics Division - Space Science Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands
|Accepted by||Astronomy & Astrophysics|
In order to minimize field star contamination, their number has been statistically subtracted based on the surface density map. The empirical cluster main sequence has been recovered in the V vs. V-I and in the J vs. J-K_S planes, using optical and infrared data, respectively. From these empirical cluster main sequences, two samples of candidate cluster members were derived in order to obtain the luminosity distributions as a function of the V and J magnitudes. The Luminosity Functions have been transformed into the corresponding Mass Functions; for M > 1 Mo, the two distributions have been fitted with a power law of index alpha_V = 2.95 ± 0.53 and alpha_J = 2.81 ± 0.84 in V and in J, respectively, while the Salpeter Mass Function in this notation has index alpha = 2.35.