| Abstract : | For LSP and ISP blazars, X-ray emission is probably due to inverse Compton emissions from lower energy electrons. The emission mechanism is not well understood, and variability could have imprints of an accretion disc component. Therefore, flux distribution studies of LSPs and ISPs are important, as such studies are useful for testing models of blazars, which are almost entirely dominated by the emission of relativistic jets, contrary to the majority of AGNs where the emission is mostly dominated by the accretion disc. Therefore, the non-Gaussian flux distribution of blazars, if found on IDV timescales, can be used to test additive models, such as mini jets-in-a-jet and other scenarios in blazar jets. We present our work on the study of the flux distribution of a sample of 15 Intermediate and Low-energy peaked blazars using XMM-Newton observations on short-term timescales. We characterise the X-ray variability of all of the light curves using excess fractional variability amplitude. In order to characterise the origin of X-ray variability in these blazars, we fit the flux distributions of all these light curves using Gaussian and lognormal distributions, as any non-Gaussian perturbation could indicate the imprints of fluctuations in the accretion disc, which could be Doppler boosted through the relativistic jets in blazars. However, intra-day variability, as seen in our observations, is difficult to reconcile using disc components as the emissions in such sources are mostly dominated by jets. In 11 observations of 4 blazars, namely, ON 231, 3C 273, PKS 0235+164 and PKS 0521-365, both models equally fit the flux distributions. In two sources, namely, BL Lacertae and S4 0954+650, the lognormal distribution is preferred over the normal distribution, which could arise from non-Gaussian perturbations from relativistic jets or linear Gaussian perturbation in the particle time scale leading to such flux distributions. |
