Linear velocity fields in non-Gaussian models for large-scale structure

1992 ◽  
Vol 390 ◽  
pp. 330 ◽  
Author(s):  
Robert J. Scherrer
Keyword(s):  
Large Scale ◽  
Large Scale Structure ◽  
Velocity Fields ◽  
Linear Velocity ◽  
Scale Structure ◽  
Gaussian Models ◽  
Non Gaussian

scholarly journals Fast and easy super-sample covariance of large-scale structure observables

2019 ◽  
Vol 624 ◽  
pp. A61 ◽  
Author(s):  
Fabien Lacasa ◽  
Julien Grain
Keyword(s):  
Large Scale ◽  
Signal To Noise Ratio ◽  
Cosmological Parameters ◽  
Power Spectra ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Numerical Application ◽  
Sample Covariance ◽  
Non Gaussian ◽  
Fast Prediction

We present a numerically cheap approximation to super-sample covariance (SSC) of large-scale structure cosmological probes, first in the case of angular power spectra. No new elements are needed besides those used to predict the considered probes, thus relieving analysis pipelines from having to develop a full SSC modeling, and reducing the computational load. The approximation is asymptotically exact for fine redshift bins Δz → 0. We furthermore show how it can be implemented at the level of a Gaussian likelihood or a Fisher matrix forecast as a fast correction to the Gaussian case without needing to build large covariance matrices. Numerical application to a Euclid-like survey show that, compared to a full SSC computation, the approximation nicely recovers the signal-to-noise ratio and the Fisher forecasts on cosmological parameters of the wCDM cosmological model. Moreover, it allows for a fast prediction of which parameters are going to be the most affected by SSC and at what level. In the case of photometric galaxy clustering with Euclid-like specifications, we find that σ8, ns, and the dark energy equation of state w are particularly heavily affected. We finally show how to generalize the approximation for probes other than angular spectra (correlation functions, number counts, and bispectra) and at the likelihood level, allowing for the latter to be non-Gaussian if necessary. We release publicly a Python module allowing the implementation of the SSC approximation and a notebook reproducing the plots of the article.

The topology of large-scale structure. II - Nonlinear evolution of Gaussian models

1988 ◽  
Vol 328 ◽  
pp. 50 ◽  
Author(s):  
Adrian L. Melott ◽  
David H. Weinberg ◽  
J. Richard, III Gott
Keyword(s):  
Large Scale ◽  
Nonlinear Evolution ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Gaussian Models

scholarly journals Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure

2010 ◽  
Vol 2010 ◽  
pp. 1-64 ◽  
Author(s):  
Michele Liguori ◽  
Emiliano Sefusatti ◽  
James R. Fergusson ◽  
E. P. S. Shellard
Keyword(s):  
Cosmic Microwave Background ◽  
Large Scale ◽  
Initial Conditions ◽  
Temperature Fluctuations ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Future Prospects ◽  
Microwave Background ◽  
Galaxy Distribution ◽  
Non Gaussian

The most direct probe of non-Gaussian initial conditions has come from bispectrum measurements of temperature fluctuations in the Cosmic Microwave Background and of the matter and galaxy distribution at large scales. Such bispectrum estimators are expected to continue to provide the best constraints on the non-Gaussian parameters in future observations. We review and compare the theoretical and observational problems, current results, and future prospects for the detection of a nonvanishing primordial component in the bispectrum of the Cosmic Microwave Background and large-scale structure, and the relation to specific predictions from different inflationary models.

scholarly journals Non-Gaussian stochastic gravitational waves from phase transitions

2021 ◽  
Vol 2021 (11) ◽  
Author(s):  
Soubhik Kumar ◽  
Raman Sundrum ◽  
Yuhsin Tsai
Keyword(s):  
Phase Transitions ◽  
Cosmic Microwave Background ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Microwave Background ◽  
Gravitational Wave Detectors ◽  
Non Gaussian

Abstract Cosmological phase transitions in the primordial universe can produce anisotropic stochastic gravitational wave backgrounds (GWB), similar to the cosmic microwave background (CMB). For adiabatic perturbations, the fluctuations in GWB follow those in the CMB, but if primordial fluctuations carry an isocurvature component, this need no longer be true. It is shown that in non-minimal inflationary and reheating settings, primordial isocurvature can survive in GWB and exhibit significant non-Gaussianity (NG) in contrast to the CMB, while obeying current observational bounds. While probing such NG GWB is at best a marginal possibility at LISA, there is much greater scope at future proposed detectors such as DECIGO and BBO. It is even possible that the first observations of inflation-era NG could be made with gravitational wave detectors as opposed to the CMB or Large-Scale Structure surveys.

Sign in / Sign up

Export Citation Format

Share Document