CMB temperature anisotropy

Cosmology ◽  
2017 ◽  
pp. 279-308
Author(s):  
Nicola Vittorio
Keyword(s):  
Temperature Anisotropy ◽  
Cmb Temperature

Maps of the CMB Temperature Anisotropy: from the Time-Ordered Data to the Maximum-Likelihood Solution

2003 ◽  
pp. 414-420
Author(s):  
Radek Stompor ◽  
Amedeo Balbi ◽  
Julian Borrill ◽  
Pedro Ferreira ◽  
Shaul Hanany ◽  
...  
Keyword(s):  
Maximum Likelihood ◽  
Temperature Anisotropy ◽  
Ordered Data ◽  
Cmb Temperature

scholarly journals A Measurement of the Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of BOOMERANG

2006 ◽  
Vol 647 (2) ◽  
pp. 823-832 ◽  
Author(s):  
W. C. Jones ◽  
P. A. R. Ade ◽  
J. J. Bock ◽  
J. R. Bond ◽  
J. Borrill ◽  
...  
Keyword(s):  
Power Spectrum ◽  
Temperature Anisotropy ◽  
Angular Power Spectrum ◽  
Cmb Temperature

Observations and simulations of the CMB temperature anisotropy at very small angular scales

2012 ◽  
Author(s):  
Màrius Josep Fullana i Alfonso ◽  
Josep Vicent Arnau i Córdoba ◽  
Robert J. Thacker ◽  
Hugh M. P. Couchman ◽  
Diego P. Sáez
Keyword(s):  
Temperature Anisotropy ◽  
Cmb Temperature

scholarly journals Cosmological constraints on matter density perturbations amplitude, neutrino mass and number of relativistic species

2018 ◽  
Vol 191 ◽  
pp. 01009
Author(s):  
Rodion Burenin
Keyword(s):  
Neutrino Mass ◽  
Large Scale ◽  
Hubble Constant ◽  
Density Perturbation ◽  
Matter Density ◽  
Temperature Anisotropy ◽  
Perturbation Amplitude ◽  
High Multipoles ◽  
Density Perturbations ◽  
Cmb Temperature

It is shown that Planck CMB temperature anisotropy data at high multipoles, ℓ > 1000, produce the measurement of matter density perturbations amplitude that contradict to all other constraints obtained both from remaining Planck CMB anisotropy data and from other cosmological data, at about 3:7σ significance level. With the exception of Planck CMB temperature anisotropy data at high multipoles, all other measurements of density perturbation amplitude are in good agreement between each other and give the following measurements of linear density perturbation amplitude: σ8 = 0:792 ± 0:006, mean density of the Universe: Ωm = 0:287 ± 0:007, and Hubble constant: H0 = 69:4 ± 0:6 km s-1 Mpc-1. Therefore, in this case the tensions in H0 constraints between Planck+BAO data and direct H0 measurements are weaken, and the tensions in σ8 measurements between Planck CMB data and large scale structure data disappear completely. Taking in account the data on baryon acoustic oscillations and (or) direct measurements of the Hubble constant, one can obtain different constraints on sum of neutrino mass and number of relativistic species.

scholarly journals Do we have any hope of detecting scattering between dark energy and baryons through cosmology?

2020 ◽  
Vol 493 (1) ◽  
pp. 1139-1152 ◽  
Author(s):  
Sunny Vagnozzi ◽  
Luca Visinelli ◽  
Olga Mena ◽  
David F Mota
Keyword(s):  
Dark Energy ◽  
Power Spectrum ◽  
Cross Sections ◽  
Direct Detection ◽  
Late Time ◽  
Temperature Anisotropy ◽  
Momentum Exchange ◽  
Microwave Background ◽  
Matter Power Spectrum ◽  
Cmb Temperature

ABSTRACT We consider the possibility that dark energy and baryons might scatter off each other. The type of interaction we consider leads to a pure momentum exchange, and does not affect the background evolution of the expansion history. We parametrize this interaction in an effective way at the level of Boltzmann equations. We compute the effect of dark energy-baryon scattering on cosmological observables, focusing on the cosmic microwave background (CMB) temperature anisotropy power spectrum and the matter power spectrum. Surprisingly, we find that even huge dark energy-baryon cross-sections $\sigma _{xb} \sim {\cal O}({\rm b})$, which are generically excluded by non-cosmological probes such as collider searches or precision gravity tests, only leave an insignificant imprint on the observables considered. In the case of the CMB temperature power spectrum, the only imprint consists in a sub-per cent enhancement or depletion of power (depending whether or not the dark energy equation of state lies above or below −1) at very low multipoles, which is thus swamped by cosmic variance. These effects are explained in terms of differences in how gravitational potentials decay in the presence of a dark energy-baryon scattering, which ultimately lead to an increase or decrease in the late-time integrated Sachs–Wolfe power. Even smaller related effects are imprinted on the matter power spectrum. The imprints on the CMB are not expected to be degenerate with the effects due to altering the dark energy sound speed. We conclude that, while strongly appealing, the prospects for a direct detection of dark energy through cosmology do not seem feasible when considering realistic dark energy-baryon cross-sections. As a caveat, our results hold to linear order in perturbation theory.

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