Analyzing the Hubble tension through hidden sector dynamics in the early universe

被引：18

作者：

Aboubrahim, Amin ^{[1
]}

Klasen, Michael ^{[1
]}

Nath, Pran ^{[2
]}

机构：

[1] Westfalische Wilhelms Univ Munster, Inst Theoret Phys, Wilhelm Klemm Str 9, D-48149 Munster, Germany

[2] Northeastern Univ, Dept Phys, 111 Forsyth St, Boston, MA 02115 USA

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2022年 / 04期

关键词：

particle physics - cosmology connection; cosmology of theories beyond the SM; dark matter theory; DARK GAUGE FORCES; EXCLUSION LIMITS; PARTICLES;

D O I：

10.1088/1475-7516/2022/04/042

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The recent analysis from the SHOES collaboration has confirmed the existence of a Hubble tension between measurements at high redshift (z > 1000) and at low redshift (z < 1) at the 5 sigma level with the low redshift measurement giving a higher value. In this work we propose a particle physics model that can help alleviate the Hubble tension via an out-of-equilibrium hidden sector coupled to the visible sector. The particles that populate the dark sector consist of a dark fermion, which acts as dark matter, a dark photon, a massive scalar and a massless pseudo-scalar. Assuming no initial population of particles in the dark sector, feeble couplings between the visible and the hidden sectors via kinetic mixing populate the dark sector even though the number densities of hidden sector particles never reach their equilibrium distribution and the two sectors remain at different temperatures. A cosmologically consistent analysis is presented where a correlated evolution of the visible and the hidden sectors with coupled Boltzmann equations involving two temperatures, one for the visible sector and the other for the hidden sector, is carried out. The relic density of the dark matter constituted of dark fermions is computed in this two-temperature formalism. As a consequence, BBN predictions are upheld with a minimal contribution to Delta N-eff. However, the out-of-equilibrium decay of the massive scalar to the massless pseudo-scalar close to the recombination time causes an increase in Delta N-eff that can help weaken the Hubble tension.

引用

页数：26

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