Spectral distortions in the cosmic microwave background polarization

Renaux‐Petel, Sébastien; Fidler, Christian; Pitrou, Cyril; Pettinari, Guido Walter

doi:10.1088/1475-7516/2014/03/033

Cited by 17 publications

(27 citation statements)

References 58 publications

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“…Different authors have concentrated on following only specific moments. The most commonly used are the Rayleigh-Jeans temperature,T RJ ≡T (1) (Chluba and Sunyaev, 2003); the number density temperature,T n ≡ T (3) (Naruko et al, 2013;Pitrou et al, 2010a;Renaux-Petel et al, 2014); and the bolometric temperaturē Huang and Vernizzi, 2013;Pitrou et al, 2010b); giving respectively the low frequency brightness, the number density of photons, and the energy density in photons. Indeed, using Eq.…”

Section: Temperature Transformmentioning

confidence: 99%

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Radiative transport of relativistic species in cosmology

Pitrou

2021

Astroparticle Physics

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Je résume les étapes essentielles de la construction d'une fonction de distribution pour les gaz de fermions et de bosons (photons), en mettant en exergue les points communs et les différences entre ces deux cas. L'objet central qui caractérise la polarisation des photons est une fonction de distribution à valeurs tensorielles, tandis que pour les fermions elle prend des valeurs vectorielles. Les termes de collision des équations de Boltzmann associées aux fermions et aux bosons possèdent également une structure semblable, et ils ne diffèrent essentiellement qu'à cause des effets quantiques associés à l'état final des réactions considérées. En particulier, les réactions de conversion entre neutrons et protons dans l'univers primordial, qui déterminent l'abondance de l'Helium, ont de nombreux points communs avec les diffusions Compton qui déterminent la forme du fond diffus cosmologique, et je montre que ces deux classes de réactions peuvent être calculées avec un développement de type Fokker-Planck. Pour les conversions neutronsprotons, cela permet d'obtenir les corrections dues à la masse finie des nucléons et qui s'avèrent être cruciales pour obtenir des prédictions théoriques précises, tandis que dans le cas des diffusions Compton cela permet d'obtenir les effets thermaux et de recul des électrons qui sont pris en compte dans la célèbre équation de Kompaneets. Dans ce mémoire, je généralise celle-ci au cas d'une distribution de radiation anisotrope et potentiellement polarisée. Enfin, je discute une paramétrisation du spectre des photons basée sur l'utilisation de moments logarithmiques, ce qui permet de séparer proprement les effets qui induisent une variation de température de ceux qui génèrent une distorsion du spectre de corps noir.

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Section: Temperature Transformmentioning

confidence: 99%

“…Indeed it also shifts ln E by a constant quantity, and therefore d 1 is affected by a boost but not the centered moments u ab n . , and this distortion, known in this context as the non-linear kinetic SZ effect (Pitrou et al, 2010a;Renaux-Petel et al, 2014), is generated by the r.h.s. of (8.27) with p = 2.…”

Section: General Form Of the Boltzmann Equationmentioning

confidence: 99%

Radiative transport of relativistic species in cosmology

Pitrou

2021

Astroparticle Physics

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“…Another source of contamination comes from the cross-correlation of E with the quadratic Doppler effect (see [35,36] and references therein). Being proportional to the velocity of the baryons squared, this observable tracks the primordial density squared y reio ∼ ζ(k) 2 .…”

Section: Y-distortion From Reionizationmentioning

confidence: 99%

“…The authors of [35] provide an analytic expression for y (2) reio . The second order transfer function for CMB polarization anisotropies can instead be obtained numerically, using the…”

Section: Y-distortion From Reionizationmentioning

confidence: 99%

Primordial non-Gaussianity with μ-type andy-type spectral distortions: exploiting Cosmic Microwave Background polarization and dealing with secondary sources

Ravenni¹,

Bartolo²,

Shiraishi³

2017

J. Cosmol. Astropart. Phys.

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Cross-correlations between Cosmic Microwave Background (CMB) temperature and y-spectral distortions anisotropies have been previously proposed as a way to measure the local bispectrum parameter f loc.NL in a range of scales inaccessible to either CMB (T , E) bispectra or T -µ correlations. This is useful e.g. to test scale dependence of primordial non-Gaussianity. Unfortunately, the primordial y-T signal is strongly contaminated by the late-time correlation between the Integrated Sachs Wolfe and Sunyaev-Zel'dovich (SZ) effects. Moreover, SZ itself generates a large noise contribution in the y-parameter map. We consider two original ways to address these issues. In order to remove the bias due to the SZ-CMB temperature coupling, while also adding new signal, we include in the analysis the crosscorrelation between y-distortions and CMB polarization. In order to reduce the noise, we propose to clean the y-map by subtracting a SZ template, reconstructed via cross-correlation with external tracers (CMB and galaxy-lensing signals). We combine this SZ template subtraction with the previously adopted solution of directly masking detected clusters. Our final forecasts show that, using y-distortions, a PRISM-like survey can achieve 1σ(f loc. NL ) = 300, while an ideal experiment will achieve 1σ(f loc. NL ) = 130, with improvements of a factor ∼ 3 from adding the y-E signal, and a further 20 − 30% from template cleaning. These forecasts are much worse than current f loc.NL boundaries from Planck, but we stress again that they refer to completely different scales.

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“…Note that −(ln p) does not have the zeroth order part but have both the first and the second order terms which describe the gravitational redshift since p is the comoving momentum. On the other hand, using (3.10) we can write the time derivative of G by 25) and Y can be neglected since this is the first order quantity which is multiplied by the second order perturbations in the equation. Combining (3.23), (3.24) and (3.25) up to second order, we obtain…”

Section: Boltzmann Equationsmentioning

confidence: 99%

CMB spectral distortions as solutions to the Boltzmann equations

Ota

2017

J. Cosmol. Astropart. Phys.

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Abstract. We propose to re-interpret the cosmic microwave background spectral distortions as solutions to the Boltzmann equation. This approach makes it possible to solve the second order Boltzmann equation explicitly, with the spectral y distortion and the momentum independent second order temperature perturbation, while generation of µ distortion cannot be explained even at second order in this framework. We also extend our method to higher order Boltzmann equations systematically and find new type spectral distortions, assuming that the collision term is linear in the photon distribution functions, namely, in the Thomson scattering limit. As an example, we concretely construct solutions to the cubic order Boltzmann equation and show that the equations are closed with additional three parameters composed of a cubic order temperature perturbation and two cubic order spectral distortions. The linear Sunyaev-Zel'dovich effect whose momentum dependence is different from the usual y distortion is also discussed in the presence of the next leading order Kompaneets terms, and we show that higher order spectral distortions are also generated as a result of the diffusion process in a framework of higher order Boltzmann equations. The method may be applicable to a wider class of problems and has potential to give a general prescription to non-equilibrium physics.

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Spectral distortions in the cosmic microwave background polarization

Cited by 17 publications

References 58 publications

Radiative transport of relativistic species in cosmology

Radiative transport of relativistic species in cosmology

Primordial non-Gaussianity with μ-type andy-type spectral distortions: exploiting Cosmic Microwave Background polarization and dealing with secondary sources

CMB spectral distortions as solutions to the Boltzmann equations

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