Massive Neutrinos and the Halo Model of Large Scale Structure

2005 ◽  
Vol 143 ◽  
pp. 571
Author(s):  
Eric Switzer ◽  
Kev Abazajian ◽  
Scott Dodelson ◽  
Salman Habib ◽  
Katrin Heitmann
Keyword(s):  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Massive Neutrinos

scholarly journals Constraints on neutrino masses from the study of the nearby large-scale structure and galaxy cluster counts

2016 ◽  
Vol 31 (21) ◽  
pp. 1640008 ◽  
Author(s):  
Hans Böhringer ◽  
Gayoung Chon
Keyword(s):  
Large Scale ◽  
Cosmological Parameters ◽  
Large Scale Structure ◽  
Matter Density ◽  
Density Fluctuations ◽  
Scale Structure ◽  
Neutrino Masses ◽  
Microwave Background ◽  
X Ray ◽  
Massive Neutrinos

The high precision measurements of the cosmic microwave background by the Planck survey yielded tight constraints on cosmological parameters and the statistics of the density fluctuations at the time of recombination. This provides the means for a critical study of structure formation in the Universe by comparing the microwave background results with present epoch measurements of the cosmic large-scale structure. It can reveal subtle effects such as how different forms of Dark Matter may modify structure growth. Currently most interesting is the damping effect of structure growth by massive neutrinos. Different observations of low redshift matter density fluctuations provided evidence for a signature of massive neutrinos. Here we discuss the study of the cosmic large-scale structure with a complete sample of nearby, X-ray luminous clusters from our REFLEX cluster survey. From the observed X-ray luminosity function and its reproduction for different cosmological models, we obtain tight constraints on the cosmological parameters describing the matter density, [Formula: see text], and the density fluctuation amplitude, [Formula: see text]. A comparison of these constraints with the Planck results shows a discrepancy in the framework of a pure [Formula: see text]CDM model, but the results can be reconciled, if we allow for a neutrino mass in the range of 0.17 eV to 0.7 eV. Also some others, but not all of the observations of the nearby large-scale structure provide evidence or trends for signatures of massive neutrinos. With further improvement in the systematics and future survey projects, these indications will develop into a definitive measurement of neutrino masses.

scholarly journals Large-scale structure formation with massive neutrinos and dynamical dark energy

2014 ◽  
Vol 89 (10) ◽  
Author(s):  
Amol Upadhye ◽  
Rahul Biswas ◽  
Adrian Pope ◽  
Katrin Heitmann ◽  
Salman Habib ◽  
...  
Keyword(s):  
Dark Energy ◽  
Structure Formation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Massive Neutrinos ◽  
Dynamical Dark Energy ◽  
Large Scale Structure Formation

scholarly journals Effects of massive neutrinos on the large-scale structure of the Universe

2011 ◽  
Vol 418 (1) ◽  
pp. 346-356 ◽  
Author(s):  
Federico Marulli ◽  
Carmelita Carbone ◽  
Matteo Viel ◽  
Lauro Moscardini ◽  
Andrea Cimatti
Keyword(s):  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Massive Neutrinos ◽  
The Universe

scholarly journals Non-linear description of massive neutrinos in the framework of large-scale structure formation

2014 ◽  
Vol 11 (S308) ◽  
pp. 121-124
Author(s):  
Hélène Dupuy
Keyword(s):  
Large Scale ◽  
Cold Dark Matter ◽  
Dynamical Evolution ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Linear Regime ◽  
Non Linear ◽  
Massive Neutrinos ◽  
Single Flow ◽  
The Universe

AbstractThere is now no doubt that neutrinos are massive particles fully involved in the non-linear growth of the large-scale structure of the universe. A problem is that they are particularly difficult to include in cosmological models because the equations describing their behavior in the non-linear regime are cumbersome and difficult to handle. In this manuscript I present a new method allowing to deal with massive neutrinos in a very simple way, based on basic conservation laws. This method is still valid in the non-linear regime. The key idea is to describe neutrinos as a collection of single-flow fluids instead of seeing them as a single hot multi-flow fluid. In this framework, the time evolution of neutrinos is encoded in fluid equations describing macroscopic fields, just as what is done for cold dark matter. Although valid up to shell-crossing only, this approach is a further step towards a fully non-linear treatment of the dynamical evolution of neutrinos in the framework of large-scale structure growth.

scholarly journals The BAHAMAS project: the CMB–large-scale structure tension and the roles of massive neutrinos and galaxy formation

2018 ◽  
Vol 476 (3) ◽  
pp. 2999-3030 ◽  
Author(s):  
Ian G McCarthy ◽  
Simeon Bird ◽  
Joop Schaye ◽  
Joachim Harnois-Deraps ◽  
Andreea S Font ◽  
...  
Keyword(s):  
Galaxy Formation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Bahamas ◽  
Massive Neutrinos

scholarly journals Fast simulations of cosmic large-scale structure with massive neutrinos

2020 ◽  
Vol 2020 (09) ◽  
pp. 018-018 ◽  
Author(s):  
Christian Partmann ◽  
Christian Fidler ◽  
Cornelius Rampf ◽  
Oliver Hahn
Keyword(s):  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Massive Neutrinos

scholarly journals Accelerating Large-Scale-Structure data analyses by emulating Boltzmann solvers and Lagrangian Perturbation Theory

2021 ◽  
Vol 1 ◽  
pp. 152
Author(s):  
Giovanni Arico' ◽  
Raul Angulo ◽  
Matteo Zennaro
Keyword(s):  
Perturbation Theory ◽  
Power Spectrum ◽  
Large Scale ◽  
Theoretical Models ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Matter Power Spectrum ◽  
Linear Spectrum ◽  
Massive Neutrinos ◽  
Cold Matter

The linear matter power spectrum is an essential ingredient in all theoretical models for interpreting large-scale-structure observables. Although Boltzmann codes such as CLASS or CAMB are very efficient at computing the linear spectrum, the analysis of data usually requires 104-106 evaluations, which means this task can be the most computationally expensive aspect of data analysis. Here, we address this problem by building a neural network emulator that provides the linear theory (total and cold) matter power spectrum in about one millisecond with ≈0.2%(0.5%) accuracy over redshifts z ≤ 3 (z ≤ 9), and scales10-4 ≤ k [h Mpc-1] < 50. We train this emulator with more than 200,000 measurements, spanning a broad cosmological parameter space that includes massive neutrinos and dynamical dark energy. We show that the parameter range and accuracy of our emulator is enough to get unbiased cosmological constraints in the analysis of a Euclid-like weak lensing survey. Complementing this emulator, we train 15 other emulators for the cross-spectra of various linear fields in Eulerian space, as predicted by 2nd-order Lagrangian Perturbation theory, which can be used to accelerate perturbative bias descriptions of galaxy clustering. Our emulators are specially designed to be used in combination with emulators for the nonlinear matter power spectrum and for baryonic effects, all of which are publicly available at http://www.dipc.org/bacco.

Sign in / Sign up

Export Citation Format

Share Document