We have used ESO telescopes at La Silla and the Hubble Space Telescope (HST
) in order to obtain accurate B, V, I CCD photometry for the stars located
within 200" (similar or equal to2 half-mass radii, r(h) = 1.71') from the c
enter of the cluster NGC 6101. Color-Magnitude Diagrams (CMDs) extending fr
om the red-giant tip to about 5 magnitudes below the main-sequence turnoff
MSTO (V = 20.05 +/- 0.05) have been constructed. The following results have
been obtained from the analysis of the CMDs: a) The overall morphology of
the main branches confirms previous results from the literature, in particu
lar the existence of a sizeable population of 73 "blue stragglers" (BSS), w
hich had been already partly detected (27). They are considerably more conc
entrated than either the subgiant branch (SGB) or the main sequence (MS) st
ars, and have the same spatial distribution as the horizontal branch (HB) s
tars (84% probability from K-S test). An hypothesis on the possible BSS pro
geny is also presented. b) The HB is narrow and the bulk of stars is blue,
as expected for a typical metal-poor globular cluster. c) The derived magni
tudes for the HB and the MSTO, V-ZAHB = 16.59 +/- 0.10, V-TO = 20.05 +/- 0.
05, coupled with the values E(B - V) = 0.1, [Fe/H] = -1.80, Y = 0.23 yield
a distance modulus (m - M)(v) = 16.23 and an age similar to other "old" met
al-poor globular clusters. In particular, from the comparison with theoreti
cal isochrones, we derive for this cluster an age of 13 Gyrs. d) By using t
he large statistical sample of Red Giant Branch (RGB) stars, we detected wi
th high accuracy the position of the bump in the RGB luminosity function. T
his observational feature has been compared with theoretical prescriptions,
yielding a good agreement within the current theoretical and observational
uncertainties.