Constraining the Neutrino Mass with the Drifting Coefficient of the Field Cluster Mass Function

Abstract

We present a numerical analysis supporting the evidence that the redshift evolution of the drifting coefficient of the field cluster mass function is capable of breaking several cosmic degeneracies. This evidence is based on the data from the CoDECS and DUSTGRAIN-pathfinder simulations performed separately for various non-standard cosmologies including coupled dark energy, f (R) gravity and combinations of f (R) gravity with massive neutrinos as well as for the standard ΛCDM cosmology. We first numerically determine the field cluster mass functions at various redshifts in the range of 0 ≤ z ≤ 1 for each cosmology. Then, we compare the analytic formula developed in previous works with the numerically obtained field cluster mass functions by adjusting its drifting coefficient, β, at each redshift. It is found that the analytic formula with the best-fit coefficient provides a good match to the numerical results at all redshifts for all of the cosmologies. The empirically determined redshift evolution of the drifting coefficient, β(z), turns out to significantly differ among different cosmologies. It is also shown that even without using any prior information on the background cosmology the drifting coefficient, β(z), can discriminate with high statistical significance the degenerate non-standard cosmologies not only from the ΛCDM but also from one another. It is concluded that the evolution of the departure from the Einstein-de Sitter state and spherically symmetric collapse processes quantified by β(z) is a powerful probe of gravity and dark sector physics.

Quantification of High-dimensional Non-Gaussianities and Its Implication to Fisher Analysis in Cosmology

“…Recently, different methods and statistics have been developed to efficiently extract the cosmological information hidden in the matter, halo, and galaxy density fields (Neyrinck et al 2009 ; Simpson et al 2011 , 2013 ; Coulton et al 2019 ; Liu & Madhavacheril 2019 ; Li et al 2019 ; Marques et al 2019 ; Vicinanza et al 2019 ; Ajani et al 2020 ; Allys et al 2020 ; Banerjee et al 2020 ; Dai et al 2020 ; de la Bella et al 2021 ; Friedrich et al 2020 ; Giri & Smith 2022 ; Gualdi et al 2021a , 2021b ; Hahn et al 2020 ; Lee & Ryu 2020 ; Ryu & Lee 2020 ; Villaescusa-Navarro et al 2020 ; Valogiannis & Dvorkin 2022 ; Uhlemann et al 2020 ; Zhang et al 2020 ; Banerjee & Abel 2021a , 2021b ; Bayer et al 2021 ; Cheng & Menard 2021a ; Hahn & Villaescusa-Navarro 2021 ; Harnois-Deraps et al 2021 , 2022 ; Kuruvilla 2022 ; Kuruvilla & Aghanim 2021 ; Massara et al 2021 ; Naidoo et al 2022 ; Porth et al 2023 ; Samushia et al 2021 ; Liu et al 2022 ). For instance, Hahn et al ( 2020 ) uses the halo bispectrum to break the parameter degeneracy between σ 8 and M ν and shows that the sum of neutrino masses can be measured with ∼5× higher precision than just using the power spectrum.…”

Weighing the Neutrinos with the Galaxy Shape-Shape Correlations

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