Secondary Cosmic Microwave Background Anisotropies from Cosmological Reionization

Gnedin, Nickolay Y.; Jaffe, A. H.

doi:10.1086/320076

Cited by 55 publications

(75 citation statements)

References 34 publications

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“…However, the smaller bubbles expected for mini-quasars or for star-forming dwarf galaxies would produce an anisotropy signal which is weaker and at smaller angular scales, likely outside the range of the upcoming satellites (see, e.g., Haiman & Knox 1999 for discussion). 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: 99%

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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Section: Effect Of Reionization On Cmb Anisotropiesmentioning

confidence: 99%

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

2001

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“…Because these regimes are difficult to describe analytically, a more appropriate tool is numerical simulations (e.g. Gnedin & Jaffe 2001, Zhang, Pen & Trac 2004, see also Figure 4. However, one can also use the halo model (see review by Cooray & Sheth 2002) to model analytically the mildly non-linear regime as done for example by Santos et al (2003) or Ma & Fry (2000, 2002.…”

Section: Secondary Anisotropies From Reionisationmentioning

confidence: 99%

Secondary anisotropies of the CMB

Aghanim¹,

Majumdar²,

Silk³

2008

Rep. Prog. Phys.

104

101

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Abstract.The Cosmic Microwave Background fluctuations provide a powerful probe of the dark ages of the universe through the imprint of the secondary anisotropies associated with the reionisation of the universe and the growth of structure. We review the relation between the secondary anisotropies and and the primary anisotropies that are directly generated by quantum fluctuations in the very early universe. The physics of secondary fluctuations is described, with emphasis on the ionisation history and the evolution of structure. We discuss the different signatures arising from the secondary effects in terms of their induced temperature fluctuations, polarisation and statistics. The secondary anisotropies are being actively pursued at present, and we review the future and current observational status.

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“…At second order in perturbation theory, this is known as the Ostriker-Vishniac effect (Ostriker & Vishniac 1986;Vishniac 1987;Dodelson & Jubas 1995;Hu & White 1996), whereas the full nonlinear signal is referred to as the kSZ effect. This full nonlinear contribution has been studied in detail both analytically (Hu 2000a;Ma & Fry 2002;Zhang, Pen, & Trac 2004) and numerically (Gnedin & Jaffe 2001;Springel, White, & Hernquist 2001;da Silva et al 2001;Zhang et al 2004).…”

Section: The Ksz Effectmentioning

confidence: 99%

Beyond the Damping Tail: Cross‐Correlating the Kinetic Sunyaev‐Zel’dovich Effect with Cosmic Shear

Doré

Spergel

2004

ApJ

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Secondary anisotropies of the cosmic microwave background (CMB) have the potential to reveal intricate details about the history of our universe between the present and recombination epochs. However, because the CMB we observe is the projected sum of a multitude of effects, the interpretation of small-scale anisotropies by future high-resolution experiments will be marred by uncertainty and speculation without the handles provided by other observations. The recent controversy over the excess small-scale anisotropy detected by CBI and the BIMA array is a foretaste of potential challenges that will be faced when interpreting future experiments. In this paper we show that cross-correlating the CMB with an overlapping weak-lensing survey will isolate the elusive kinetic Sunyaev-Zel'dovich (kSZ) effect from secondary anisotropies generated at higher redshifts. We show that if upcoming high angular resolution CMB experiments, like Planck /ACT/SPT, cover the same area of sky as current and future weak-lensing surveys, like CFTHLS/SNAP/ LSST, the cross-correlation of cosmic shear with the kSZ effect will be detected with high signal-to-noise ratio, increasing the potential science accessible to both sets of surveys. For example, if ACT and a CFHTLS-like survey were to overlap, this cross-correlation would be detected with a total signal-to-noise ratio greater than 220, reaching 1.8 per individual multipole around l $ 5000. Furthermore, this cross-correlation probes the three-point coupling between the underlying dark matter and the momentum of the ionized baryons in the densest regions of the universe at intermediate redshifts. Similar to the thermal Sunyaev-Zel'dovich (tSZ) power spectrum, its strength is extremely sensitive to the power spectrum normalization parameter, 8 , scaling roughly as 7 8 . It provides an effective mechanism to isolate any component of anisotropy due to patchy reionization and rule out primordial small-scale anisotropy.

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Secondary Cosmic Microwave Background Anisotropies from Cosmological Reionization

Cited by 55 publications

References 34 publications

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

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

Secondary anisotropies of the CMB

Beyond the Damping Tail: Cross‐Correlating the Kinetic Sunyaev‐Zel’dovich Effect with Cosmic Shear

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