Soft X-ray excess in the Coma cluster from a Cosmic Axion Background

被引：45

作者：

Angus, Stephen ^{[1
]}

Conlon, Joseph P. ^{[1
]}

Marsh, M. C. David ^{[1
]}

Powell, Andrew J. ^{[1
]}

Witkowski, Lukas T. ^{[1
,2
]}

机构：

[1] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England

[2] Heidelberg Univ, Inst Theoret Phys, D-69120 Heidelberg, Germany

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2014年 / 09期

基金：

欧洲研究理事会;

关键词：

axions; string theory and cosmology; galaxy clusters; particle physics - cosmology connection; EXTREME-ULTRAVIOLET EMISSION; MAGNETIC-FIELD; XMM-NEWTON; COSMOLOGICAL IMPLICATIONS; NONTHERMAL EMISSION; FARADAY-ROTATION; GALAXY CLUSTERS; ABELL; 2199; SN; 1987A; ROSAT;

D O I：

10.1088/1475-7516/2014/09/026

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We show that the soft X-ray excess in the Coma cluster can be explained by a cosmic background of relativistic axion-like particles (ALPs) converting into photons in the cluster magnetic field. We provide a detailed self-contained review of the cluster soft X-ray excess, the proposed astrophysical explanations and the problems they face, and explain how a 0.1-1 keV axion background naturally arises at reheating in many string theory models of the early universe. We study the morphology of the soft excess by numerically propagating axions through stochastic, multi-scale magnetic field models that are consistent with observations of Faraday rotation measures from Coma. By comparing to ROSAT observations of the 0.2-0.4 keV soft excess, we find that the overall excess luminosity is easily reproduced for g(a gamma gamma) similar to 2 x 10(-13) GeV-1. The resulting morphology is highly sensitive to the magnetic field power spectrum. For Gaussian magnetic field models, the observed soft excess morphology prefers magnetic field spectra with most power in coherence lengths on O(3 kpc) scales over those with most power on O(12 kpc) scales. Within this scenario, we bound the mean energy of the axion background to 50 eV less than or similar to < E-a > less than or similar to 250 eV, the axion mass to m(a) less than or similar to 10(-12) eV, and derive a lower bound on the axion-photon coupling g(a gamma gamma) greater than or similar to root 0.5/Delta N-eff 1.4 x 10(-13) GeV-1.

引用

页数：49

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