scholarly journals Footprints of Doppler and aberration effects in cosmic microwave background experiments: statistical and cosmological implications

2020 ◽  
Vol 493 (2) ◽  
pp. 1708-1724
Author(s):  
Siavash Yasini ◽  
Elena Pierpaoli
Keyword(s):  
Solar System ◽  
Cosmic Microwave Background ◽  
Cosmological Parameters ◽  
Power Spectra ◽  
Additional Term ◽  
Local Motion ◽  
Microwave Background ◽  
Wide Range ◽  
Cmb Temperature ◽  
Polarization Power

ABSTRACT In the frame of the Solar system, the Doppler and aberration effects cause distortions in the form of mode couplings in the cosmic microwave background (CMB) temperature and polarization power spectra and, hence, impose biases on the statistics derived by the moving observer. We explore several aspects of such biases and pay close attention to their effects on CMB polarization, which, previously, have not been examined in detail. A potentially important bias that we introduce here is boost variance—an additional term in cosmic variance, induced by the observer’s motion. Although this additional term is negligible for whole-sky experiments, in partial-sky experiments it can reach 10 per cent (temperature) to 20 per cent (polarization) of the standard cosmic variance (σ). Furthermore, we investigate the significance of motion-induced power and parity asymmetries in TT, EE, and TE as well as potential biases induced in cosmological parameter estimation performed with whole-sky TTTEEE. Using Planck-like simulations, we find that our local motion induces $\sim 1\!-\!2 {{\ \rm per\ cent}}$ hemispherical asymmetry in a wide range of angular scales in the CMB temperature and polarization power spectra; however, it does not imply any significant amount of parity asymmetry or shift in cosmological parameters. Finally, we examine the prospects of measuring the velocity of the Solar system w.r.t. the CMB with future experiments via the mode coupling induced by the Doppler and aberration effects. Using the CMB TT, EE, and TE power spectra up to ℓ = 4000, the Simons Observatory and CMB-S4 can make a dipole-independent measurement of our local velocity, respectively, at 8.5σ and 20σ.

scholarly journals Planck 2013 Cosmology Results: a Review

2014 ◽  
Vol 1 (1) ◽  
pp. 49-55
Author(s):  
José Alberto Rubino-Martín
Keyword(s):  
Cosmic Microwave Background ◽  
Galaxy Clusters ◽  
Cosmological Parameters ◽  
Power Spectra ◽  
Microwave Background ◽  
Statistical Characterization ◽  
Number Counts ◽  
Cmb Temperature

This talk presents an overview of the cosmological results derived from the first 15.5 months of observations of the ESA’s <em>Planck</em> mission. These cosmological results are mainly based on the <em>Planck </em>measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra, although we also briefly discuss other aspects of the <em>Planck</em> data, as the statistical characterization of the reconstructed CMB maps, or the constraints on cosmological parameters using the number counts of galaxy clusters detected by means of the Sunyaev-Zeldovich effect in the <em>Planck</em> maps. All these results are described in detail in a series of papers released by ESA and the <em>Planck</em> collaboration in March 2013.

scholarly journals Determination of miscalibrated polarization angles from observed cosmic microwave background and foreground EB power spectra: Application to partial-sky observation

2020 ◽  
Vol 2020 (6) ◽  
Author(s):  
Yuto Minami
Keyword(s):  
Power Spectrum ◽  
Cosmic Microwave Background ◽  
Simultaneous Determination ◽  
Unbiased Estimate ◽  
Dust Emission ◽  
Power Spectra ◽  
Microwave Background ◽  
The Public ◽  
Polarization Power

Abstract We study a strategy to determine miscalibrated polarization angles of cosmic microwave background (CMB) experiments using the observed $EB$ polarization power spectra of CMB and Galactic foreground emission. We apply the methodology of Y. Minami et al. (Prog. Theor. Exp. Phys. 2019, 083E02, 2019), developed for full-sky observations to ground-based experiments such as Simons Observatory. We take into account the $E$-to-$B$ leakage and $\ell$-to-$\ell$ covariance due to partial sky coverage using the public code NaMaster. We show that our method yields an unbiased estimate of miscalibrated angles. Our method also enables simultaneous determination of miscalibrated angles and the intrinsic $EB$ power spectrum of polarized dust emission when the latter is proportional to $\sqrt{C_\ell^{EE}C_\ell^{BB}}$ and $C_\ell^{BB}$ is proportional to $C_\ell^{EE}$.

scholarly journals Cosmology with the cosmic microwave background temperature-polarization correlation

2017 ◽  
Vol 602 ◽  
pp. A41 ◽  
Author(s):  
F. Couchot ◽  
S. Henrot-Versillé ◽  
O. Perdereau ◽  
S. Plaszczynski ◽  
B. Rouillé d’Orfeuil ◽  
...  
Keyword(s):  
Cosmic Microwave Background ◽  
Cosmological Parameters ◽  
Power Spectra ◽  
Microwave Background ◽  
Instrumental Noise ◽  
Cosmic Microwave Background Temperature ◽  
Temperature Polarization ◽  
Background Temperature ◽  
The Impact ◽  
Polarization Correlation

We demonstrate that the cosmic microwave background (CMB) temperature-polarization cross-correlation provides accurate and robust constraints on cosmological parameters. We compare them with the results from temperature or polarization and investigate the impact of foregrounds, cosmic variance, and instrumental noise. This analysis makes use of the Planck high-ℓ HiLLiPOP likelihood based on angular power spectra, which takes into account systematics from the instrument and foreground residuals directly modelled using Planck measurements. The temperature-polarization correlation (TE) spectrum is less contaminated by astrophysical emissions than the temperature power spectrum (TT), allowing constraints that are less sensitive to foreground uncertainties to be derived. For ΛCDM parameters, TE gives very competitive results compared to TT. For basic ΛCDM model extensions (such as AL, ∑mν, or Neff), it is still limited by the instrumental noise level in the polarization maps.

scholarly journals Simultaneous determination of the cosmic birefringence and miscalibrated polarization angles II: Including cross-frequency spectra

2020 ◽  
Vol 2020 (10) ◽  
Author(s):  
Yuto Minami ◽  
Eiichiro Komatsu
Keyword(s):  
Cosmic Microwave Background ◽  
Simultaneous Determination ◽  
Power Spectra ◽  
Microwave Background ◽  
Frequency Spectra ◽  
Frequency Bands ◽  
Frequency Power ◽  
Polarization Power

Abstract We develop a strategy to determine the cosmic birefringence and miscalibrated polarization angles simultaneously using the observed $EB$ polarization power spectra of the cosmic microwave background and the Galactic foreground emission. We extend the methodology of Y. Minami et al. (Prog. Theor. Exp. Phys. 2019, 083E02, 2019), which was developed for auto-frequency power spectra, by including cross-frequency spectra. By fitting one global birefringence angle and independent miscalibration angles at different frequency bands, we determine both angles with significantly smaller uncertainties (by more than a factor of two) compared to the auto spectra.

scholarly journals COSMOLOGY WITH MIRROR DARK MATTER II: COSMIC MICROWAVE BACKGROUND AND LARGE SCALE STRUCTURE

2005 ◽  
Vol 14 (02) ◽  
pp. 223-256 ◽  
Author(s):  
PAOLO CIARCELLUTI
Keyword(s):  
Dark Matter ◽  
Power Spectrum ◽  
Cosmic Microwave Background ◽  
Large Scale ◽  
Cosmological Parameters ◽  
Power Spectra ◽  
Linear Regime ◽  
Microwave Background ◽  
Primordial Nucleosynthesis ◽  
Standard Cosmology

This is the second paper of a series devoted to the study of the cosmological implications of the existence of mirror dark matter. The parallel hidden mirror world has the same microphysics as the observable one and couples the latter only gravitationally. The primordial nucleosynthesis bounds demand that the mirror sector should have a smaller temperature T′ than the ordinary one T, and by this reason its evolution can be substantially deviated from the standard cosmology. In this paper we take scalar adiabatic perturbations as the input in a flat Universe, and compute the power spectra for ordinary and mirror CMB and LSS, changing the cosmological parameters, and always comparing with the CDM case. We find differences in both the CMB and LSS power spectra, and we demonstrate that the LSS spectrum is particularly sensitive to the mirror parameters, due to the presence of both the oscillatory features of mirror baryons and the collisional mirror Silk damping. For x<0.3 the mirror baryon–photon decoupling happens before the matter–radiation equality, so that CMB and LSS power spectra in linear regime are equivalent for mirror and CDM cases. For higher x-values the LSS spectra strongly depend on the amount of mirror baryons. Finally, qualitatively comparing with the present observational limits on the CMB and LSS spectra, we show that for x<0.3 the entire dark matter could be made of mirror baryons, while in the case x≳0.3 the pattern of the LSS power spectrum excludes the possibility of dark matter consisting entirely of mirror baryons, but they could present as admixture (up to ~50%) to the conventional CDM.

scholarly journals MEASUREMENT OF COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRA FROM TWO YEARS OF BICEP DATA

2010 ◽  
Vol 711 (2) ◽  
pp. 1123-1140 ◽  
Author(s):  
H. C. Chiang ◽  
P. A. R. Ade ◽  
D. Barkats ◽  
J. O. Battle ◽  
E. M. Bierman ◽  
...  
Keyword(s):  
Cosmic Microwave Background ◽  
Power Spectra ◽  
Microwave Background ◽  
Cosmic Microwave Background Polarization ◽  
Polarization Power
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