  The aim of this paper is to present the results of photometric investigations
of the central cluster of the W5 E region as well as a follow-up study of the
triggered star formation in and around bright-rimmed clouds (BRCs). We have
carried out wide field $UBVI_c$ and deep $VI_c$ photometry of the W5 E H{\sc
ii} region. A distance of $\sim$2.1 kpc and a mean age of $\sim$1.3 Myr have
been obtained for the central cluster. The young stellar objects (YSOs)
associated with the region are identified on the basis of near-infrared and
mid-infrared observations. We confirmed our earlier results that the average
age of the YSOs lying on/inside the rim are younger than those lying outside
the rim. The global distribution of the YSOs shows an aligned distribution from
the ionising source to the BRCs. These facts indicate that a series of
radiation driven implosion processes proceeded from near the central ionising
source towards the periphery of the W5 E H{\sc ii} region. We found that, in
general, the age distributions of the Class II and Class III sources are the
same. This result is apparently in contradiction with the conclusion by
Bertout, Siess & Cabrit (2007) and Chauhan et al. (2009) that classical T Tauri
stars evolve to weak-line T Tauri stars. The initial mass function of the
central cluster region in the mass range $0.4 \le M/M_\odot \le 30$ can be
represented by $\Gamma = -1.29 \pm 0.03$. The cumulative mass functions
indicate that in the mass range $0.2 \le M/M_\odot \le 0.8$, the cluster region
and BRC NW have more low mass YSOs in comparison to BRCs 13 and 14.
