A Measurement of Secondary Cosmic Microwave Background Anisotropies From the 2500 Square-Degree SPT-Sz Survey

George, E. M.; Reichardt, Christian; Aird, K. A.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Cho, H-M.; Crawford, T. M.; Crites, A. T.; Haan, T. de; Dobbs, M.; Dudley, J. P.; Halverson, N. W.; Harrington, N. L.; Holder, G. P.; Holzapfel, W. L.; Hou, Z.; Hrubes, J. D.; Keisler, R.; Knox, L.; Lee, A. T.; Leitch, E. M.; Lueker, M.; Luong-Van, D.; McMahon, Jeff; Mehl, J.; Meyer, S. S.; Millea, M.; Mocanu, L. M.; Mohr, J. J.; Montroy, T. E.; Padin, S.; Plagge, T.; Pryke, C.; Ruhl, J. E.; Schaffer, K. K.; Shaw, L.; Shirokoff, E.; Spieler, H.; Staniszewski, Z.; Stark, A. A.; Story, K. T.; Engelen, Alexander van; Vanderlinde, K.; Vieira, J. D.; Williamson, A. R.; Zahn, O.

doi:10.1088/0004-637x/799/2/177

Cited by 229 publications

(275 citation statements)

References 103 publications

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“…From the evolution of volume filling factor QHII for HII regions, one can see that reionization is almost completed (QHII ∼ 1) around 5.8 z 8.5 (2-σ limits) for Planck model. The mean ionized fraction evolves rapidly in 5.8 z 10.6, in good agreement with other recent works (George et al 2015;Robertson et al 2015), whereas the mean WMAP model favors a relatively gradual or extended reionization (spanning 5.8 z 13). This is reflected in the evolution of the neutral hydrogen fraction xHI: the mean value for Planck model goes from xHI ∼ 0.8 to xHI ∼ 10 −4 between z = 10.6 (z = 13 for WMAP model) and z = 5.8.…”

Section: Mcmc-pca Constraints From Planck Datasupporting

confidence: 90%

Cosmic reionization after Planck

Mitra

Choudhury

Ferrara

2015

Monthly Notices of the Royal Astronomical Society: Letters

138

103

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Cosmic reionization holds the key to understand structure formation in the Universe, and can inform us about the properties of the first sources, as their star formation efficiency and escape fraction of ionizing photons. By combining the recent release of Planck electron scattering optical depth data with observations of high-redshift quasar absorption spectra, we obtain strong constraints on viable reionization histories. We show that inclusion of Planck data favors a reionization scenario with a single stellar population. The mean x HI drops from ∼ 0.8 at z = 10.6 to ∼ 10 −4 at z = 5.8 and reionization is completed around 5.8 z 8.5 (2-σ), thus indicating a significant reduction in contributions to reionization from high redshift sources. We can put independent constraints on the escape fraction f esc of ionizing photons by incorporating the high-redshift galaxy luminosity function data into our analysis. We find a non-evolving f esc of ∼ 10% in the redshift range z = 6 − 9.

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Section: Mcmc-pca Constraints From Planck Datasupporting

confidence: 90%

Cosmic reionization after Planck

Mitra

Choudhury

Ferrara

2015

Monthly Notices of the Royal Astronomical Society: Letters

138

103

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“…In the temperature skies we add several components: the thermal Sunyaev-Zel'dovich (tSZ), the clustered and unclustered components of the CIB (dusty sources), and radio point sources (active galactic nuclei; AGNs). The tSZ component is modeled by a tSZ power spectrum template taken from Shaw et al (George et al 2015). We neglect the correlation between these CIB components at 150 and 95 GHz and the simulated CIB map at 500 μm.…”

Section: Pipelinementioning

confidence: 99%

“…Power from unclustered point sources is by definition flat in C ℓ , so p=2 for unclustered sources. With the adopted threshold for point source masking of 50mJy at 150 GHz, the residual dusty sources power spectrum amplitudes are m = A 9 K (Mocanu et al 2013;George et al 2015). We need the foreground component in the temperature maps to properly account for T/E → B leakage that is removed through the convolutional cleaning step of the power spectrum analysis of the B-mode map (Section 4.4).…”

Section: Pipelinementioning

confidence: 99%

CMB Polarization B-mode Delensing with SPTpol and Herschel

Manzotti

Story

et al. 2017

ApJ

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We present a demonstration of delensing the observed cosmic microwave background (CMB) B-mode polarization anisotropy. This process of reducing the gravitational-lensing-generated B-mode component will become increasingly important for improving searches for the B modes produced by primordial gravitational waves. In this work, we delens B-mode maps constructed from multi-frequency SPTpol observations of a 90 deg 2 patch of sky by subtracting a B-mode template constructed from two inputs: SPTpol E-mode maps and a lensing potential map estimated from the Herschel 500 μm map of the cosmic infrared background. We find that our delensing procedure reduces the measured B-mode power spectrum by 28% in the multipole range < < ℓ 300 2300; this is shown to be consistent with expectations from simulations and to be robust against systematics. The null hypothesis of no delensing is rejected at s 6.9 . Furthermore, we build and use a suite of realistic simulations to study the general properties of the delensing process and find that the delensing efficiency achieved in this work is limited primarily by the noise in the lensing potential map. We demonstrate the importance of including realistic experimental nonidealities in the delensing forecasts used to inform instrument and survey-strategy planning of upcoming lowernoise experiments, such as CMB-S4.

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“…These measurements were calibrated using WMAP 7yr data. A more recent analysis from the complete ∼2500 deg 2 area of the SPT-SZ survey is presented in George et al (2015), dubbed SPT high2014 hereafter. In this later release, cross spectra cover a somewhat broader range, between 2000 and 13000.…”

Section: Datasetsmentioning

confidence: 99%

“…We thus prefer to use Reichardt et al (2012) dataset as a baseline in our analyses, with free calibration parameters to match other datasets. We have checked that all results presented in this paper are stable when switching to George et al (2015), in which case we have to set strict priors on recalibration parameters owing to the form of the associated covariance matrix.…”

Section: Datasetsmentioning

confidence: 99%

Relieving tensions related to the lensing of the cosmic microwave background temperature power spectra

Couchot

Henrot-Versillé

Perdereau

et al. 2017

A&A

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The angular power spectra of the cosmic microwave background (CMB) temperature anisotropies reconstructed from Planck data seem to present 'too much' gravitational lensing distortion. This is quantified by the control parameter A L that should be compatible with unity for a standard cosmology. With the class Boltzmann solver and the profile-likelihood method, for this parameter we measure a 2.6σ shift from 1 using the Planck public likelihoods. We show that, owing to strong correlations with the reionization optical depth τ and the primordial perturbation amplitude A s , a ∼ 2σ tension on τ also appears between the results obtained with the low ( ≤ 30) and high (30 < 2500) multipoles likelihoods. With Hillipop, another high-likelihood built from Planck data, this difference is lowered to 1.3σ. In this case, the A L value is still in disagreement with unity by 2.2σ, suggesting a non-trivial effect of the correlations between cosmological and nuisance parameters. To better constrain the nuisance foregrounds parameters, we include the very-high-measurements of the Atacama Cosmology Telescope (ACT) and South Pole Telescope (SPT) experiments and obtain A L = 1.03 ± 0.08. The Hillipop+ACT+SPT likelihood estimate of the optical depth is τ = 0.052 ± 0.035, which is now fully compatible with the low-likelihood determination. After showing the robustness of our results with various combinations, we investigate the reasons for this improvement that results from a better determination of the whole set of foregrounds parameters. We finally provide estimates of the ΛCDM parameters with our combined CMB data likelihood.

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A Measurement of Secondary Cosmic Microwave Background Anisotropies From the 2500 Square-Degree SPT-Sz Survey

Cited by 229 publications

References 103 publications

Cosmic reionization after Planck

Cosmic reionization after Planck

CMB Polarization B-mode Delensing with SPTpol and Herschel

Relieving tensions related to the lensing of the cosmic microwave background temperature power spectra

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