The stellar content of the S0 galaxy NGC 5102 is investigated using deep r ^ { \prime } and i ^ { \prime } images obtained with GMOS-S. A modest population of bright main sequence stars and red supergiants ( RSGs ) is detected throughout the western portion of the disk .
Based on the numbers of main sequence stars , the star formation rate ( SFR ) in NGC 5102 during the past ten million years is estimated to have been 0.02 M _ { \odot } year ^ { -1 } .
The majority of red giant branch ( RGB ) stars in the disk of NGC 5102 have [ M/H ] between –0.9 and –0.1 , and the metallicity distribution of RGB stars at intermediate galactocentric radii peaks near [ M/H ] \sim - 0.6 .
RGB stars are traced out to galactocentric distances of 10 kpc , which corresponds to \sim 14 disk scale lengths .
A large population of bright asymptotic giant branch ( AGB ) stars are seen throughout the western portion of the disk , and the youngest of these have log ( t _ { yr } ) \sim 8.1 .
It is concluded that ( 1 ) stars that formed within the past Gyr comprise \sim 20 \% of the total stellar disk mass , and ( 2 ) the SFR during intermediate epochs in the disk of NGC 5102 was at least 1.4 M _ { \odot } year ^ { -1 } .
Thus , large-scale star formation occured throughout the disk of NGC 5102 at approximately the same time that similar elevated levels of star formation occured in the bulge .
It is suggested that NGC 5102 was a spiral galaxy that experienced a galaxy-wide episode of star formation that terminated a few hundred Myr in the past , and that much of its interstellar medium was ejected in an outflow .