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 observed with XMM–Newton spanning 31 epochs .
Parametric fits to X-ray spectra helps constrain the possible location of transition from the high energy end of the synchrotron 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 external Compton ( EC ; disk , broad line region , torus ) mechanisms are used to estimate magnetic field strength \leq 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 .