  We present uvbybeta CCD photometry of the central region of the double
cluster h and chi Persei. We identify 350 stars, of which 214 were not included
in Oosterhof catalogue. Our magnitude limit V=16.5 allows us to reach early F
spectral type and obtain very accurate fits to the ZAMS. We derive reddening
values of E(b-y)=0.44+-0.02 for h Persei and E(b-y)=0.39+-0.05 for chi Persei.
  From the ZAMS fitting, we derive distance moduli V0-Mv=11.66+-0.20 and
V0-Mv=11.56+-0.20 for h and chi Persei respectively. These values are perfectly
compatible with both clusters being placed at the same distance and having
identical reddenings. The shift in the main-sequence turnoff and isochrone
fitting, however, show that there is a significant age difference between both
clusters, with the bulk of stars in h Persei being older than chi Persei. There
is, however, a significant population of stars in h Persei which are younger
than chi Persei. All this argues for at least three different epochs of star
formation, corresponding approximately to log t=7.0, 7.15 and 7.3.
