In this work is based on recent work on detection of the gravitational wave by the interaction with the electromagnetic waves (arXiv:1711.04657). Here we take the source of gravitational waves for the two cases of (i) an astrophysical binary star and (ii) a binary blackhole before merging. We investigate the interaction of the electromagnetic radiation with each of the gravity wave sources. The effect is the time variation in the light curve of a distant source such as quasar in the wave optics regime. We study the probability of detection of this event and the observational features of this interaction. Finally, the observational prospect for the detection of this event is proposed for (a) the gravity wave sourced by the astrophysical binaries and (b) the follow-up observations in the radio and visual wavelengths for detecting the gravity wave of merging binary black holes that are already alerted by LIGO/VIRGO detectors.

We will browse through the physics of CMB, what we learned from it and what is left.

I discuss some of the cosmological consequences of the recent classical nonlocal extension of the general theory of relativity. This is done within the regime of nonlocal Newtonian cosmology.

In my talk, I will start off by a short review of cosmology and then I will move on to the idea of cosmic inflation as the widely accepted description of the early universe cosmology. Afterwards, I will present a review of cosmological perturbation theory and some of its applications for calculating cosmological observable such as the scalar and tensor power spectra.

I will introduce the formalism of stochastic inflation, as well as some techniques for computing observables within that framework.

This talk is dedicated to a modern review on Topological and geometrical measures inspired by stochasticity behavior of Cosmological random fields. Stochasticity is ubiquitous in cosmology ranging from initial conditions to large-scale structures at the late time. On the other hand, there are many theoretical approaches and observational datasets attempting to explain the mysteries of our cosmos. An interesting question is: how one can extract science from big-data and discriminate between different models?

In this presentation, I expect to give a clue from this point of view which most probably has an important impact on future attempts for clarifying the nature of our Universe.

The large scale structure (LSS) observations like the statistics and clustering of galaxies are one set of the main observations to test the cosmological models. However the distribution of the galaxies is a biased tracer of the dark matter distribution in large scales. Accordingly the knowledge that how the baryonic matter traces the dark matter distribution (known as bias parameter) is a key ingredient to use LSS observation to constrain the cosmological models.

In this lecture I will first introduce the concept of galaxy clustering and galaxy count as a cosmological tool and then I will present the ideas in non-linear structure formation like Excursion set theory in order to find the clustering and bias of galaxies in non-linear scales.