B-mode power spectrum of CMB via polarized Compton scattering

Khodagholizadeh, Jafar; Mohammadi, Rohoollah; Sadegh, Mahdi; Vahedi, Ali

doi:10.1088/1475-7516/2020/01/051

Cited by 5 publications

(4 citation statements)

References 126 publications

(165 reference statements)

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“…Before ending this section, it should be mentioned that we only considered the contribution of the CνB and ALPs interactions to discuss the constraint placed on the parameter space of axion. Some other mechanisms including polarized (2024) 84:619 Compton scattering [70], dipole asymmetry of CMB temperature anisotropy [71], and various sorts of new physics interaction leading to produce CMB B mode polarization [25] that generates EB power spectrum, can contribute to the generation of the CB angle. However, by upgrading data on EB-cross power spectrum along with the theoretical and experimental studies in the future we will be able to get more information about the origin of the reported CB angle.…”

Section: Cb Angle Due To Cνb and Alpmentioning

confidence: 99%

Generation of the CMB cosmic birefringence through axion-like particles, sterile and active neutrinos

Mahmoudi,

Sadegh,

Khodagholizadeh

et al. 2024

Eur. Phys. J. C

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The cosmic birefringence (CB) angle refers to the rotation of the linear polarization plane of Cosmic Microwave Background (CMB) radiations when parity-violating theories are considered. We analyzed the Quantum Boltzmann equation for an ensemble of CMB photons interacting with the right-handed sterile neutrino dark matter (DM) and axion-like particles (ALPs) DM in the presence of the scalar metric perturbation. We used the birefringence angle of CMB to study those probable candidates of DM. It is shown that the CB angle contribution of sterile neutrino is much less that two other sources considered here. Next, we combined the results of the cosmic neutrinos’ contribution and the contribution of the ALPs to producing the CMB birefringence and discussed the uncertainty on the parameter space of axions caused by the share of CMB-cosmic neutrino interaction in generating this effect. Finally, we plotted the EB power spectrum of the CMB and showed that this spectrum behaves differently in the presence of cosmic neutrinos and ALPs interactions in small l. Hence, future observed data for $$C^{l}_{EB},$$ C EB l , will help us to distinguish the CB angle value due to the various sources of its production.

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Section: Cb Angle Due To Cνb and Alpmentioning

confidence: 99%

Generation of the CMB cosmic birefringence through axion-like particles, sterile and active neutrinos

Mahmoudi,

Sadegh,

Khodagholizadeh

et al. 2024

Eur. Phys. J. C

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“…There may be some other mechanisms generating the EB power spectrum that can suppress the contribution of photon-neutrino interaction and CB angle. among these mechanisms are Chern-Simons Axion coupling to the electromagnetic field [39], scattering of CMB photons off polarized electrons [65,66], and dipole asymmetry of temperature anisotropy of CMB [67]. Large-scale magnetic fields and other Lorentz-violating interactions can also play roles as birefringence mediums.…”

Section: Big Inconsistency Between Cb Angle Generated Via Majorana Cν...mentioning

confidence: 99%

Cross-correlation power spectra and cosmic birefringence of the CMB via photon-neutrino interaction

Khodagholizadeh

Mohammadi

Sadegh

et al. 2023

J. Cosmol. Astropart. Phys.

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In the context of the standard model of particles, the weak interaction of cosmic microwave background (CMB) and cosmic neutrino background (CνB), can generate non-vanishing TB and EB power spectra in the order of one loop forward scattering, in the presence of scalar perturbation, which is in contrast with the standard scenario cosmology. Comparing our results with the current experimental data may provide, significant information about the nature of CνB, including CMB-CνB forward scattering for TB, TE, and EB power spectra. To this end, different cases were studied, including Majorana CνB and Dirac CνB. On the other hand, it was shown that the mean opacity due to cosmic neutrino background could behave as an anisotropic birefringent medium and change the linear polarization rotation angle. Considering the contributions from neutrino and anti-neutrino forward scattering with CMB photons (in the case of Dirac neutrino), we introduce relative neutrino and anti-neutrino density asymmetry (δν = Δnν /nν = nν -nν̅ /nν ). Then, using the cosmic birefringence angle reported by the Planck data release β = 0.30° ± 0.11° (68%C.L.), some constraints can be put on δν . Also, the value of cosmic birefringence due to Majorana CνB medium is estimated at about β| ν ≃ 0.2 rad. In this respect, since Majorana neutrino and anti-neutrino are exactly the same, both CB contributions will be added together. However, this value is at least two orders larger than the cosmic birefringence angle reported by the Planck data release, β = 0.30° ± 0.11° (68%C.L.). Finally, we shortly discussed this big inconsistency. It is noteworthy that to calculate the contribution of photon-neutrino forward scattering for cosmic birefringence, we just consider the standard model of particles and the standard scenario of cosmology.

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“…Let us consider a small fraction δ L of left-handed polarization for ingoing cosmic electrons while we do not apply any constraint on the outgoing electrons due to their interaction with CMB photons. A reason for this asymmetry between left-handed and right-handed electrons is the cosmic magnetic field, which enforces the lowest Landau level fill just by left-handed electrons (See [50,61]). The chiral asymmetry is also discussed in the inflation models which is generated from chiral coupling between the axion and the fermion axial current (See [30]).…”

Section: Jcap01(2019)052mentioning

confidence: 99%

“…As shown in eqs. (2.25)-(2.27), the polarized Compton scattering can generate the B-mode polarization in the presence of the scalar perturbation, thereby affecting the value of E-mode polarization and the anisotropy of CMB temperature [61].…”

Section: Jcap01(2019)052 4 Conclusionmentioning

confidence: 99%

Generation of circular polarization of CMB via polarized Compton scattering

Vahedi

Khodagholizadeh

Mohammadi

et al. 2019

J. Cosmol. Astropart. Phys.

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The standard scenario of cosmology predicts a measurable amount for linear polarization of the Cosmic Microwave Background radiation (CMB) via Thomson scattering, while through this scenario, the generation of circular polarization is excluded. On the another hand, the circular polarization of CMB has not been excluded in observational evidence. The generation of CMB photons circular polarization via their Compton scattering with polarized cosmic electrons is considered in this paper. Our motivation for considering polarized Compton scattering comes from the effects of the external magnetic field in large scale, the chiral magnetic instability and new physics interactions of the cosmic electrons. It is shown that damping term of polarized Compton scattering in the presence of scalar perturbation can generate circular polarization in CMB radiation, so that the power spectrum of circular polarization of CMB C V (S) l is proportional to the power spectrum of temperature anisotropy of CMB C

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B-mode power spectrum of CMB via polarized Compton scattering

Cited by 5 publications

References 126 publications

Generation of the CMB cosmic birefringence through axion-like particles, sterile and active neutrinos

Generation of the CMB cosmic birefringence through axion-like particles, sterile and active neutrinos

Cross-correlation power spectra and cosmic birefringence of the CMB via photon-neutrino interaction

Generation of circular polarization of CMB via polarized Compton scattering

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