Dmitri Pogosyan

CITA

Title:   Cosmic Structure on Large and Small Scales

Analysis of random inhomogeneities is one of main underlying threads
in modern theoretical cosmology. Statistical observables of the random
fields associated with primary CMB temperature fluctuations, galaxy
number density, Sunyaev-Zeldovich fluctuations, weak-lensing shear
(to name a few examples of random fields) carry information on the
global parameters which define our Universe. The very geometry of tiny
density perturbations produced in early Universe explains the morphology
of predominately filamentary Web-like pattern of galaxy distribution
on large scales.  The subject is not restricted to cosmology and large
scales. Another example is provided by the fluctuations of radio emission
from neutral hydrogen in the disk of our Galaxy.  The 21 cm emission
carries information about density and velocity distribution of HI and,
ultimately, about the nature of the turbulence in the ISM.  In my recent
work, HI studies have been shown to benefit from statistical techniques
similar to the ones used in cosmology.  I  shall discuss my work in the
field, first reviewing the Cosmic Web theory for the Large-Scale Structure
but also highlighting my recent results in analyzing HI and CMB data.