Dark matter in Hidden Valley models with stable and unstable light dark mesons
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Springer
Received: October 6, Revised: March 18, Accepted: April 15, Published: April 18,
2018 2019 2019 2019
Hugues Beauchesne,a,b Enrico Bertuzzoa and Giovanni Grilli di Cortonaa a
Instituto de F´ısica, Universidade de S˜ ao Paulo, C.P. 66.318, 05315-970 S˜ ao Paulo, Brazil b Department of Physics, Ben-Gurion University, Beer-Sheva 8410501, Israel
E-mail: [email protected], [email protected], [email protected] Abstract: It is a distinct possibility that a Hidden Valley sector would have a spectrum of light particles consisting of both stable and unstable dark mesons. The simultaneous presence of these two types of particles can lead to novel mechanisms for generating the correct dark matter relic abundance, which in turn can reflect themselves into new exotic signatures at colliders. We study the viability of such sectors for various Hidden Valley models and map the valid parameter space to possible collider signatures. Mediators studied include various scalar bifundamentals and a heavy Z 0 . It is shown that in general bounds from direct and indirect detection can easily be avoided. In most of the allowed parameter space, the relic density is determined by stable mesons annihilating to unstable ones which in turn decay quickly to Standard Model particles. Dark mesons that decay mainly to heavier Standard Model fermions allow for more valid parameter space, though dark mesons are still allowed to decay exclusively to some of the lighter fermions. Possible exotic collider signatures include displaced vertices, emerging jets and semivisible jets. Keywords: Cosmology of Theories beyond the SM, Beyond Standard Model ArXiv ePrint: 1809.10152
c The Authors. Open Access, Article funded by SCOAP3 .
https://doi.org/10.1007/JHEP04(2019)118
JHEP04(2019)118
Dark matter in Hidden Valley models with stable and unstable light dark mesons
Contents 1
2 General setup and overview of the mechanism
3
3 Overview of constraints 3.1 Direct detection 3.2 Indirect detection
5 5 6
4 Constraints for benchmark models 4.1 Scalar mediators interacting only with down-type quarks 4.2 Multiple scalar mediators interacting only with down-type quarks 4.3 Z 0 model
7 7 11 13
5 Additional comments
13
6 Conclusion
16
A Calculations of the dark matter relic density A.1 Lagrangian A.2 3 → 2 processes A.3 Energy exchange A.4 Boltzmann equation and approximations
16 16 17 17 18
1
Introduction
The existence of dark matter (DM) is for all intents and purposes an established fact. A multitude of astrophysical observations such as anisotropies in the Cosmic Microwave Background (CMB), large scale structures of the Universe and galactic rotational curves all point toward the presence of a long-lived and non-baryonic dark matter component with a density roughly five times that of visible matter [1]. For the past few decades, the leading dark matter candidates have been Weakly Interacting Massive Particles (WIMP), which are assumed to generate the correct relic abundance via thermal freeze-out [2–4]. In contrast to astrophysical
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