Springer : Connecting between inflation and dark matter in models with gauged Z$_{3}$ symmetry

Choi, Soo-Min; Zhu, Bin; Kim, Jinsu; Lee, Hyun Min

doi:10.1007/JHEP06(2020)135

Article
Report number	arXiv:2003.11823
Title	Connecting between inflation and dark matter in models with gauged Z$_{3}$ symmetry
Author(s)	Choi, Soo-Min (Chung-Ang U. ; CERN) ; Kim, Jinsu (Gottingen U.) ; Lee, Hyun Min (Chung-Ang U. ; CERN) ; Zhu, Bin (Chung-Ang U. ; Yantai U.)
Publication	2020-06-22
Imprint	2020-03-26
Number of pages	40
Note	40 pages, 9 figures, Accepted to JHEP, Discussion on heavy degrees of freedom during inflation added
In:	JHEP 2006 (2020) 135
DOI	10.1007/JHEP06(2020)135
Subject category	hep-ph ; Particle Physics - Phenomenology
Abstract	We investigate the possibility of unifying the inflation and dark matter physics in the minimal model for a complex scalar dark matter with gauged $Z_3$ symmetry. The dark local $U(1)$ symmetry is broken spontaneously into the $Z_3$ symmetry by the dark Higgs mechanism. As compared to dark matter models with $Z_2$ parity, the dark matter cubic self-interaction restricts the inflation with non-minimal couplings to take place beyond the pure dark matter direction and plays an important role in the loop corrections for the inflationary predictions as well as determining the correct dark matter relic density. Considering either of $2\rightarrow 2$, $3\rightarrow 2$ or forbidden channels to be a dominant production mechanism for dark matter, we show the viable parameter space of the model that is consistent with the theoretical and phenomenological constraints combined from inflation and dark matter.
Copyright/License	preprint: (License: arXiv nonexclusive-distrib 1.0) publication: © 2020-2025 The Authors (License: CC-BY-4.0), sponsored by SCOAP³

$Parameter space for WIMP dark matter scenario with $\xi_\chi/\xi_\phi=1$ (left) and $0.01$ (right) for the quartic self-couplings with $\lambda_\chi=\lambda_\phi$ versus the quartic mixing couplings with $\lambda_{\phi\chi}=\lambda_{\chi H}$. The parameters shown here are set at low-energy scale. The rest input parameters are chosen as $\zeta = 0.05$, $g_X =0.1, \, \sin\theta = 0.01$, $\varepsilon=10^{-4}$, $m_{h^\prime} = 100$ GeV and $m_\chi = 500$ GeV. Constraints from dark matter physics and cosmic inflation are shown. The green region represents the correct dark matter relic abundance within 3$\sigma$ range \cite{planck}. The hatched and black regions are disfavored due to stability, unitarity and perturbativity. The dark Higgs (mixed) inflation is not allowed in the red-colored (blue-colored) region. The black points are our benchmark points shown in Table \ref{tab:BPWIMPinput}.$ $Parameter space for WIMP dark matter scenario with $\xi_\chi/\xi_\phi=1$ (left) and $0.01$ (right) for the quartic self-couplings with $\lambda_\chi=\lambda_\phi$ versus the quartic mixing couplings with $\lambda_{\phi\chi}=\lambda_{\chi H}$. The parameters shown here are set at low-energy scale. The rest input parameters are chosen as $\zeta = 0.05$, $g_X =0.1, \, \sin\theta = 0.01$, $\varepsilon=10^{-4}$, $m_{h^\prime} = 100$ GeV and $m_\chi = 500$ GeV. Constraints from dark matter physics and cosmic inflation are shown. The green region represents the correct dark matter relic abundance within 3$\sigma$ range \cite{planck}. The hatched and black regions are disfavored due to stability, unitarity and perturbativity. The dark Higgs (mixed) inflation is not allowed in the red-colored (blue-colored) region. The black points are our benchmark points shown in Table \ref{tab:BPWIMPinput}.$ $Parameter space for WIMP dark matter scenario with $\xi_\chi/\xi_\phi=1$ (left) and $0.01$ (right) for the quartic couplings with $\lambda_\chi=\lambda_\phi=\lambda_{\phi\chi}=\lambda_{\chi H}$ versus the dark matter cubic coupling $\zeta$. The rest input parameters and color codes are as in Fig.~\ref{fig:WIMP1}, except that $\zeta$ is varying.$ Show more plots

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