  We present the photometric and spectroscopic analysis of four W UMa binaries
J015829.5+260333 (hereinafter as J0158), J030505.1+293443 (hereinafter as
J0305), J102211.7+310022 (hereinafter as J1022) and KW Psc. The VRcIc band
photometric observations are carried out with the 1.3-m Devasthal Fast Optical
Telescope. For low resolution spectroscopy, we used 2-m Himalayan Chandra
Telescope as well as the archival data from 4-m LAMOST survey. The systems
J0158 and J0305 show a period increase rate of 5.26(+/-1.72)x10^-7 days/yr and
1.78(+/-1.52)x10^-6 days/yr, respectively. The period of J1022 is found to be
decreasing with a rate of 4.22(+/-1.67)x10^-6 days/yr. The period analysis of
KW Psc displays no change in its period. PHOEBE package is used for the light
curve modeling and basic parameters are evaluated with the help of GAIA
parallax. The asymmetry of light curves is explained with the assumption of
cool spots at specific positions on one of the components of the system. On the
basis of temperatures, mass ratios, fill-out factors and periods, the system
J1022 is identified as W-subtype systems while the others show some mixed
properties. To probe the chromospheric activities in these W UMa binaries,
their spectra are compared with the known inactive stars spectra. The
comparison shows emission in H\alpha, H\beta and CaII. To understand the
evolutionary status of these systems, the components are drawn in mass-radius
and mass-luminosity planes with other well characterized binary systems. The
secondary components of all the systems are away from ZAMS which indicates that
secondary is more evolved than the primary component.
