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Title: Thermal and non-thermal production of dark matter via Z{sup ′}-portal(s)

Abstract

We study the genesis of dark matter in the primordial Universe for representative classes of Z{sup ′}-portals models. For weak-scale Z{sup ′} mediators we compute the range of values of the kinetic mixing allowed by WMAP/PLANCK experiments corresponding to a FIMP regime. We show that very small values of δ (10{sup −12}≲δ≲10{sup −11}) are sufficient to produce the right amount of dark matter. We also analyse the case of very massive gauge mediators, whose mass m{sub Z{sup ′}} is larger than the reheating temperature, T{sub RH}, with a weak-scale coupling g{sub D} to ordinary matter. Relic abundance constraints then impose a direct correlation between T{sub RH} and the effective scale Λ of the interactions: Λ∼10{sup 3}−10{sup 5}×T{sub RH}. Finally we describe in some detail the process of dark thermalisation and study its consequences on the computation of the relic abundance.

Authors:
 [1]; ;  [2];  [3]
  1. Service de Physique Théorique Université Libre de Bruxelles,Brussels, 1050 (Belgium)
  2. Laboratoire de Physique Théorique Université Paris-Sud,Orsay, F-91405 (France)
  3. Instituto de Fisica Teorica, IFT-UAM/CSIC,Madrid, 28049 (Spain)
Publication Date:
Sponsoring Org.:
SCOAP3, CERN, Geneva (Switzerland)
OSTI Identifier:
22458432
Resource Type:
Journal Article
Resource Relation:
Journal Name: Journal of Cosmology and Astroparticle Physics; Journal Volume: 2014; Journal Issue: 01; Other Information: PUBLISHER-ID: JCAP01(2014)034; OAI: oai:repo.scoap3.org:1043; cc-by Article funded by SCOAP3. Content from this work may be used under the terms of the Creative Commons Attribution 3.0 License. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.; Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; ABUNDANCE; CALCULATION METHODS; GAUGE INVARIANCE; INTERACTIONS; LIMITING VALUES; NONLUMINOUS MATTER; RELICT RADIATION; UNIVERSE

Citation Formats

Chu, Xiaoyong, Mambrini, Yann, Quevillon, Jérémie, and Zaldívar, Bryan. Thermal and non-thermal production of dark matter via Z{sup ′}-portal(s). United States: N. p., 2014. Web. doi:10.1088/1475-7516/2014/01/034.
Chu, Xiaoyong, Mambrini, Yann, Quevillon, Jérémie, & Zaldívar, Bryan. Thermal and non-thermal production of dark matter via Z{sup ′}-portal(s). United States. doi:10.1088/1475-7516/2014/01/034.
Chu, Xiaoyong, Mambrini, Yann, Quevillon, Jérémie, and Zaldívar, Bryan. Thu . "Thermal and non-thermal production of dark matter via Z{sup ′}-portal(s)". United States. doi:10.1088/1475-7516/2014/01/034.
@article{osti_22458432,
title = {Thermal and non-thermal production of dark matter via Z{sup ′}-portal(s)},
author = {Chu, Xiaoyong and Mambrini, Yann and Quevillon, Jérémie and Zaldívar, Bryan},
abstractNote = {We study the genesis of dark matter in the primordial Universe for representative classes of Z{sup ′}-portals models. For weak-scale Z{sup ′} mediators we compute the range of values of the kinetic mixing allowed by WMAP/PLANCK experiments corresponding to a FIMP regime. We show that very small values of δ (10{sup −12}≲δ≲10{sup −11}) are sufficient to produce the right amount of dark matter. We also analyse the case of very massive gauge mediators, whose mass m{sub Z{sup ′}} is larger than the reheating temperature, T{sub RH}, with a weak-scale coupling g{sub D} to ordinary matter. Relic abundance constraints then impose a direct correlation between T{sub RH} and the effective scale Λ of the interactions: Λ∼10{sup 3}−10{sup 5}×T{sub RH}. Finally we describe in some detail the process of dark thermalisation and study its consequences on the computation of the relic abundance.},
doi = {10.1088/1475-7516/2014/01/034},
journal = {Journal of Cosmology and Astroparticle Physics},
number = 01,
volume = 2014,
place = {United States},
year = {Thu Jan 23 00:00:00 EST 2014},
month = {Thu Jan 23 00:00:00 EST 2014}
}