We present V and I photometry of a 9.4 \arcmin \times 9.4 \arcmin field centered on the dwarf spheroidal galaxy Leo II .
The Tip of the Red Giant Branch is identified at I ^ { TRGB } = 17.83 \pm 0.03 and adopting \langle [ M / H ] \rangle = -1.53 \pm 0.2 from the comparison of RGB stars with Galactic templates , we obtain a distance modulus ( m - M ) _ { 0 } = 21.84 \pm 0.13 , corresponding to a distance D = 233 \pm 15 Kpc .
Two significant bumps have been detected in the Luminosity Function of the Red Giant Branch .
The fainter bump ( B1 , at V = 21.76 \pm 0.05 ) is the RGB bump of the dominant stellar population while the actual nature of the brightest one ( B2 , at V = 21.35 \pm 0.05 ) can not be firmly assessed on the basis of the available data , it can be due to the Asymptotic Giant Branch Clump of the main population or it may be a secondary RGB bump .
The luminosity of the main RGB bump ( B1 ) suggests that the majority of RGB stars in Leo II belongs to a population that is \ga 4 gyr younger than the classical Galactic globular clusters .
The stars belonging to the He-burning Red Clump are shown to be significantly more centrally concentrated than RR Lyrae and Blue Horizontal Branch stars , probing the existence of an age/metallicity radial gradient in this remote dwarf spheroidal .