  Blazars are classified into high, intermediate and low energy peaked sources
based on the location of their synchrotron peak. This lies in infra-red/optical
to ultra-violet bands for low and intermediate peaked blazars. The transition
from synchrotron to inverse Compton emission falls in the X-ray bands for such
sources. We present the spectral and timing analysis of 14 low and intermediate
energy peaked blazars ob- served with XMMNewton spanning 31 epochs. Parametric
fits to X-ray spectra helps constrain the possible location of transition from
the high energy end of the syn- chrotron to the low energy end of the inverse
Compton emission. In seven sources in our sample, we infer such a transition
and constrain the break energy in the range 0.6 10 keV. The Lomb-Scargle
periodogram is used to estimate the power spectral density (PSD) shape. It is
well described by a power law in a majority of light curves, the index being
flatter compared to general expectation from AGN, ranging here between 0.01 and
1.12, possibly due to short observation durations resulting in an absence of
long term trends. A toy model involving synchrotron self-Compton (SSC) and
exter- nal Compton (EC; disk, broad line region, torus) mechanisms are used to
estimate magnetic field strength 6 0.03 - 0.88 G in sources displaying the
energy break and infer a prominent EC contribution. The timescale for
variability being shorter than synchrotron cooling implies steeper PSD slopes
which are inferred in these sources.
