Cosmic microwave background anisotropies resulting from feedback-regulated inhomogeneous reionization

Bruscoli, M.; Ferrara, Andrea; Fabbri, R.; Ciardi, B.

doi:10.1046/j.1365-8711.2000.03671.x

Cited by 27 publications

(40 citation statements)

References 22 publications

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“…We would like to note here that a recent similar analysis by Bruscoli et al (2000) did not use randomization in calculating the CMB anisotropies, and by adopting a periodic universe, overestimated the correct result by a factor of 3È10.…”

Section: Then For All Boxes Between Andmentioning

confidence: 86%

“…Workers in the Ðeld have considered models for the distribution of the ionization fraction in the linear regime (e.g., Knox et al 1998 ;Gruzinov & Hu 1998), as well as full simulations or semianalytic models of the ionized gas, as in this work (see also Bruscoli et al 2000 ;Benson et al 2001 ;Springel et al 2001). …”

Section: T Erminology For Secondary Anisotropiesmentioning

confidence: 99%

“…with provided we make a usual cos h \ (r 1 AE r 2 )/(r 1 r 2 ), assumption (e.g., Bruscoli et al 2000) that the electron density and velocity are uncorrelated, i.e.,…”

Section: Introductionmentioning

confidence: 99%

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Secondary Cosmic Microwave Background Anisotropies from Cosmological Reionization

Gnedin

Jaffe

2001

ApJ

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We use numerical simulations of cosmological reionization to calculate the secondary CMB anisotropies in a representative Ñat low-density cosmological model. We show that the kinetic SunyaevZeldovich e †ect (scattering o † of moving electrons in the ionized intergalactic medium) is dominated by the nonlinear hydrodynamic and gravitational evolution of the density and velocity Ðelds, rather than the detailed distribution of the ionization fraction ("" patchy reionization ÏÏ) on all angular scales. Combining our results with the recent calculation of secondary CMB anisotropies by Springel et al., we are able to accurately predict the power spectrum of the kinetic SZ e †ect on almost all angular scales.

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Section: Then For All Boxes Between Andmentioning

confidence: 86%

Section: T Erminology For Secondary Anisotropiesmentioning

confidence: 99%

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Secondary Cosmic Microwave Background Anisotropies from Cosmological Reionization

Gnedin

Jaffe

2001

ApJ

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“…Gnedin & Jaffe (2000) used a numerical simulation to show that, in the case of stellar reionization, the effect on the CMB of patchy reionization is indeed sub-dominant compared to the contribution of non-linear density and velocity fluctuations. Nevertheless, a signature of reionization could still be detected in future measurements of CMB angular fluctuations on the scale of a few arcseconds (see also Bruscoli et al 2000, who find a somewhat higher power spectrum due to patchy reionization).…”

Section: Effect Of Reionization On Cmb Anisotropiesmentioning

confidence: 91%

In the beginning: the first sources of light and the reionization of the universe

2001

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The formation of the first stars and quasars marks the transformation of the universe from its smooth initial state to its clumpy current state. In popular cosmological models, the first sources of light began to form at a redshift z = 30 and reionized most of the hydrogen in the universe by z = 7. Current observations are at the threshold of probing the hydrogen reionization epoch. The study of high-redshift sources is likely to attract major attention in observational and theoretical cosmology over the next decade.

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“…The secondary anisotropies produced by inhomogeneous reionization which we study in this article have also been computed by means of numerical simulations in Bruscoli et al (2000), Gnedin & Jaffe (2000) and Springel et al (2000), using different cosmologies and astrophysical models. These authors find a broad maximum for the power-spectra C l and S l of C l ∼ 10 −13 −10 −12 around l ∼ 10 4 .…”

Section: Comparison With Numerical Simulationsmentioning

confidence: 99%

Secondary CMB anisotropies from the kinetic SZ effect

Valageas

Balbi

Silk

2001

A&A

102

136

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Abstract. The reionization of the universe by stars and quasars is expected to be a highly inhomogeneous process. Moreover, the fluctuations of the matter density field also lead to inhomogeneities of the free electron distribution. These patterns gave rise to secondary CMB anisotropies through Thomson scattering of photons by free electrons. In this article we present an analytic model, based on our previous work which tackled the reionization history of the universe, which allows us to describe the generation of these secondary CMB anisotropies. We take into account the "patchy pattern" of reionization (HII bubbles), the cross-correlations of these ionized regions, the small-scale fluctuations of the matter density field and the contribution from collapsed objects. For an open universe, we find that the angular correlation function C(θ) displays a very slow decline from C(0) ∼ 6 10 −13 up to the scale θ ∼ 10−3 rad where it shows a sharp drop. On the other hand, the power-spectrum l(l + 1)C l /(2π) (and the "local average" S l ) exhibits a plateau of height ∼10 −13 in the range 10 3 < l < 10 6 . We find that for large wavenumbers l > 10 4 the signal is dominated by the contribution from collapsed halos while for l < 10 4 it is governed by the large-scale correlations of HII bubbles. This implies that one cannot discriminate reionization by stars from a quasar-driven scenario since the size of ionized regions never dominates the behaviour of the anisotropies. Moreover, the secondary CMB anisotropies arise from a broad range of redshifts (7.5 < z < 10 for the IGM and 0 < z < 7 for galactic halos). Thus, we find that the generation of these anisotropies involves several intricate processes and they are close to the resolution limit of current numerical simulations. The signal expected in our model might bias the cosmological parameter estimation from CMB experiments such as Planck or MAP, and could be detected by future mm-wavelength interferometers (e.g., ALMA).

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Cosmic microwave background anisotropies resulting from feedback-regulated inhomogeneous reionization

Cited by 27 publications

References 22 publications

Secondary Cosmic Microwave Background Anisotropies from Cosmological Reionization

Secondary Cosmic Microwave Background Anisotropies from Cosmological Reionization

In the beginning: the first sources of light and the reionization of the universe

Secondary CMB anisotropies from the kinetic SZ effect

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