language: en

arXiv:0908.0113v1 [astro-ph.CO] 2 Aug 2009

[Mon. Not. R. Astron. Soc. 000, 000?000 (0000)]

[Printed]

2 August 2009

(MN L A T E X style file v2.2)

S-Z power spectrum produced by primordial magnetic fields

Hiroyuki Tashiro 1 , and Naoshi Sugiyama 23
1 Institut d'Astrophysique Spatiale (IAS),
Batiment 121, Université Paris-Sud 11, Orsay, F-91405, France
2 Department of Physics and Astrophysics, Nagoya University,
Chikusa, Nagoya 464-8602, Japan
3 Institute for Physics and Mathematics of the Universe, University of Tokyo,
5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba, 277-8582, Japan
2 August 2009

ABSTRACT Primordial magnetic fields generated in the very early universe are one of the candidates for the origin of magnetic fields observed in galaxy clusters. After recombination, the Lorentz force acts on the residual ions and electrons to generate density fluctuations of baryons. Accordingly these fluctuations induce the early formation of dark halos which cause the Sunyaev-Zel'dovich (S-Z) effect in cosmic microwave background radiation. This additional S-Z effect due to primordial magnetic fields amplifies the angular power spectrum of cosmic microwave temperature anisotropies on small scales. This amplification depends on the comoving amplitude and the power law index of the primordial magnetic fields spectrum. Comparing with the small scale CMB observations, we obtained the constraints on the primordial magnetic fields, i.e., B < 0.7 nGauss for n = ?2.9 or B < 0.3 nGauss for n = ?2.5 , where B is the comoving amplitude of magnetic fields at 1 Mpc and n is the power law index. These constraints are tighter than those from temperature anisotropies and polarization of cosmic microwave background induced by the magnetic fields at the recombination epoch.

Key words: cosmology: theory ? magnetic fields ? large-scale structure of universe

1 INTRODUCTION