Francesco Montanari

The CLASSgal code for relativistic cosmological large scale structure

We present accurate and efficient computations of large scale structure observables, obtained with a modified version of the c l ass code which is made publicly available. This code includes all relativistic corrections and computes both the power spectrum C-l(z(1), z(2)) and the corresponding correlation function xi(theta, z(1), z(2)) of the matter density and the galaxy number fluctuations in linear perturbation theory. For Gaussian initial perturbations, these quantities contain the full information encoded in the large scale matter distribution at the level of linear perturbation theory. We illustrate the usefulness of our code for cosmological parameter estimation through a few simple examples.

Cosmological parameter estimation with large scale structure observations

We estimate the sensitivity of future galaxy surveys to cosmological parameters, using the redshift dependent angular power spectra of galaxy number counts, C-l(z(1), z(2)), calculated with all relativistic corrections at first order in perturbation theory. We pay special attention to the redshift dependence of the non-linearity scale and present Fisher matrix forecasts for Euclid-like and DES-like galaxy surveys. We compare the standard P(k) analysis with the new C-l(z(1), z(2)) method. We show that for surveys with photometric redshifts the new analysis performs significantly better than the P(k) analysis. For spectroscopic redshifts, however, the large number of redshift bins which would be needed to fully profit from the redshift information, is severely limited by shot noise. We also identify surveys which can measure the lensing contribution and we study the monopole, C-0(z(1), z(2)).

Measuring the lensing potential with tomographic galaxy number counts

We investigate how the lensing potential can be measured tomographically with future galaxy surveys using their number counts. Such a measurement is an independent test of the standard

A new method for the Alcock-Paczynski test

\Lambda

Curvature constraints from Large Scale Structure

CDM framework and can be used to discern modified theories of gravity. We perform a Fisher matrix forecast based on galaxy angular-redshift power spectra, assuming specifications consistent with future photometric Euclid-like surveys and spectroscopic SKA-like surveys. For the Euclid-like survey we derive a fitting formula for the magnification bias. Our analysis suggests that the cross correlation between different redshift bins is very sensitive to the lensing potential such that the survey can measure the amplitude of the lensing potential at the same level of precision as other standard

Lensing convergence and the neutrino mass scale in galaxy redshift surveys

\Lambda

An analytic approach to baryon acoustic oscillations

CDM cosmological parameters.

Backreaction and FRW consistency conditions

We argue that from observations alone, only the transverse power spectrum

Erratum: Galaxy number counts to second order and their bispectrum

C_\ell(z_1,z_2)

Evaluating backreaction with the ellipsoidal collapse model

and the corresponding correlation function