The full Boltzmann hierarchy for dark matter-massive neutrino interactions

被引：17

作者：

Mosbech, Markus R. ^{[1
]}

Boehm, Celine ^{[1
]}

Hannestad, Steen ^{[2
]}

Mena, Olga ^{[3
]}

Stadler, Julia ^{[4
]}

Wong, Yvonne Y. Y. ^{[5
]}

机构：

[1] Univ Sydney, Sch Phys, Camperdown, NSW 2006, Australia

[2] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark

[3] Univ Valencia, IFIC, CSIC, Valencia 46071, Spain

[4] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany

[5] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2021年 / 03期

基金：

欧盟地平线“2020”;

关键词：

cosmological perturbation theory; dark matter theory; neutrino properties; particle physics - cosmology connection; BARYON ACOUSTIC-OSCILLATIONS; INTERACTION CROSS-SECTION; LY-ALPHA ABSORPTION; STERILE NEUTRINOS; COSMOLOGICAL SIMULATIONS; RADIATION INTERACTIONS; CONSTRAINTS; SIGNATURES; CONSTANT; I;

D O I：

10.1088/1475-7516/2021/03/066

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The impact of dark matter-neutrino interactions on the measurement of the cosmological parameters has been investigated in the past in the context of massless neutrinos exclusively. Here we revisit the role of a neutrino-dark matter coupling in light of ongoing cosmological tensions by implementing the full Boltzmann hierarchy for three massive neutrinos. Our tightest 95% CL upper limit on the strength of the interactions, parameterized via u(chi) = sigma(0)/sigma(Th) (m(chi)/100GeV)(-1), is u(chi) <= 3.34 . 10(-4), arising from a combination of Planck TTTEEE data, Planck lensing data and SDSS BAO data. This upper bound is, as expected, slightly higher than previous results for interacting massless neutrinos, due to the correction factor associated with neutrino masses. We find that these interactions significantly relax the lower bounds on the value of sigma 8 that is inferred in the context of Lambda CDM from the Planck data, leading to agreement within 1-2 sigma with weak lensing estimates of sigma 8, as those from KiDS1000. However, the presence of these interactions barely affects the value of the Hubble constant H-0.

引用

页数：31

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