Found 32 talks width keyword large-scale structure

Wednesday January 28, 2009
Dr. Francesco Sylos Labini
Institute for Complex Systems, CNR, Italy


The Sloan Digital Sky Survey is currently the largest spectroscopic survey of extragalactic objects and one of the most ambitious observational programs ever undertaken in astronomy, measuring about 1 million redshifts and thus providing a three dimensional mapping of the local universe up to a depth of several hundreds of Mpc. The main characteristic of galaxy distribution in this survey, and in the Two degree Field Galaxy redshift Survey completed few years ago, is that large scale structures have been found to extend to scales of the order of hundreds of mega parsecs. However the standard determination of a characteristic length scale, statistically describing galaxy correlations, is of only few mega parsecs: the standard explanation of this apparent mismatch is that large scale structures have small amplitude relative to the average density. We show that, in the newest galaxy samples, large scale structures are quite typical and correspond to large fluctuation in the galaxy density field, making the standard interpretation untenable. We show that the standard statistical analysis is affected by systematics which are due to inconsistent assumptions. We point out that standard theoretical models of structure formation are unable to explain the existence of the large fluctuations in the galaxy density field detected in these samples. This conclusion is reached in two ways: by considering the scale, determined by a linear perturbation analysis of a self-gravitating fluid, below which large fluctuations are expected in standard models and through the determination of statistical properties of mock galaxy catalogs generated from cosmological N-body simulations. Finally we discuss the implications of this results in relation to recent attempts to describe inhomogeneous models in general relativity and to the recent discoveries of large scale coherent bulk flows.

Tuesday November 18, 2008
Dr. Carlos Hernández-Monteagudo
Max Planck Institute for Astrophysics, Germany


The amount of baryons seen in the local Universe falls short by a factor2-5 if compared to the amount of detected baryons at intermediate (z~2)or high (z~1,100) redshift. This is the so called "missing baryon" problem in Cosmology. Hydrodynamical simulations of the large scale structure predict that most of those missing baryons should be in the form of ionized gas present in slightly overdense regions, at a temperature ranging from 10^5 to 10^7 K, conforming the "Warm Hot Intergalactic Medium" (WHIM). This WHIM would not form stars, and would not emit or absorb either in the IR, optical or UV. However, it should interact with the photons of the Cosmic Microwave Background (CMB) through two different channels: (i) Thompson scattering (where there is no energy exchange) and (ii) Compton scattering (where hot electrons transfer energy to the CMB photons, distorting their black body spectrum). I shall review the status of the search for missing baryons in the context of CMB observations and the currently most favored cosmological model. I shall also outline new methods and prospects for detecting this missing gas with upcoming CMB experiments and address the link between the cosmic baryon problem and the search for (so far undetected) bulk flows at scales of ~10 Mpc/h.

<< First 1 | 2 | 3 | 4 Older »

Upcoming talks

Featured talks