Images spanning the 0.5 to 2.3 \mu m wavelength interval are used to probe the stellar content in the disk and halo of the Sculptor Group galaxy NGC 247 .
The main sequence turn-off ( MSTO ) in the inner 12 kpc of the disk corresponds to an age of \sim 6 Myr .
A mean star formation rate ( SFR ) of 0.1 M _ { \odot } year ^ { -1 } during the past 16 Myr is computed from star counts ; this is qualitatively consistent with the relatively low SFR computed from other indicators .
The color of the red supergiant plume does not change with radius , suggesting that the mean metallicity of young stars does not vary by more than \sim 0.1 dex throughout the disk .
However , the number of bright main sequence stars per local stellar mass density climbs towards larger radii out to a distance of 12 kpc ; the scale lengths that characterize the radial distributions of young and old stars thus differ throughout much of the disk .
For comparison , the density of bright main sequence stars with respect to projected HI mass gradually drops with increasing radius .
At distances in excess of 12 kpc the population of very young stars disappears ; the MSTO at galactocentric radii between 12 and 15 kpc corresponds to \sim 16 Myr , while between 15 and 18 kpc the MSTO age is \geq 40 Myr .
Stars evolving on the red giant branch are resolved in an extraplanar region that has a projected galactocentric distance along the minor axis of \sim 12 kpc .
The r ^ { \prime } - i ^ { \prime } colors of the RGB population indicate that there is a broad spread in metallicity , with a mean [ M/H ] \sim - 1.2 .
The RGB-tip occurs at i ^ { \prime } = 24.5 \pm 0.1 , and a distance modulus of 27.9 \pm 0.1 is computed .
Luminous AGB stars are also seen in this field , and the brightnesses of these objects is consistent with an age \sim 3 Gyr .
Possible origins of such a population of intermediate aged stars well off of the disk plane are discussed .