  A photometric and spectroscopic investigation is performed on five W Ursae
Majoris eclipsing binaries (EWs) J015818.6+260247 (hereinafter as J0158b),
J073248.4+405538 (hereinafter as J0732), J101330.8+494846 (hereinafter as
J1013), J132439.8+130747 (hereinafter as J1324) and J152450.7+245943
(hereinafter as J1524). The photometric data are collected with the help of the
1.3\,m Devasthal Fast Optical Telescope (DFOT), the 1.04\,m Sampurnanand
Telescope (ST) and the TESS space mission. The low-resolution spectra of the
4\,m Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) are
used for spectroscopic analysis. The orbital period change of these systems is
determined using our and previously available photometric data from different
surveys. The orbital period of J1013 and J1524 is changing with a rate of
$-2.552(\pm0.249)\times 10^{-7}$ days $yr^{-1}$ and $-6.792(\pm0.952)\times
10^{-8}$ days $yr^{-1}$, respectively, while others do not show any orbital
period change. The orbital period change of J1013 and J1524 corresponds to a
mass transfer rate of $2.199\times10^{-7} M_{\odot}\,yr^{-1}$ and
$6.151\times10^{-8}M_{\odot}\,yr^{-1}$ from the primary to the secondary
component in these systems. It is likely that angular momentum loss via
magnetic braking may also be responsible for the observed orbital period change
in the case of J1524. All systems have a mass-ratio lower than 0.5, except
J0158b with a mass-ratio of 0.71. All the systems are shallow type contact
binaries. The J0158b and J1524 are A-subtype while others are W-subtype. The
$H_{\alpha}$ emission line region is compared with template spectra prepared
using two inactive stars with the help of STARMOD program. The J0158, J1324 and
J1524 systems show excess emission in the residual spectra after subtraction of
the template.
