S-Z power spectrum produced by primordial magnetic fields

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 < 2.0 nGauss for n=-2.9 or B < 1.0 nGauss for n=-2.6, where B is the comoving amplitude of magnetic fields at h^-1 Mpc and n is the power law index. Future S-Z measurements have the potential to give constraints tighter than those from temperature anisotropies and polarization of cosmic microwave background induced by the magnetic fields at the recombination epoch.

9 pages, 6 figures. accepted by MNRAS

References in corpus (5)

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• The evolution of primordial magnetic field since its generation
• Constraints on Primordial Magnetic Fields from their impact on the ionization history with Planck 2018
• Generation of large-scale magnetic fields, non-Gaussianity, and primordial gravitational waves in inflationary cosmology
• Thermal Sunyaev-Zel'dovich effect in the intergalactic medium with primordial magnetic fields
• Probing the primordial Universe with 21-cm line from cosmic dawn/epoch of reionization
• Primordial magnetic fields generated by the non-adiabatic fluctuations at pre-recombination era
• Primordial magnetic fields with X-ray and S-Z cluster survey
• LiteBIRD Science Goals and Forecasts: Primordial Magnetic Fields
• Secondary CMB anisotropies from bulk motions in the presence of stochastic magnetic fields
• Implications of baryon-dark matter interaction on IGM temperature and tSZ effect with magnetic field