Templates for the Sunyaev-Zel’dovich Angular Power Spectrum

Trac, Hy; Bode, Paul; Ostriker, Jeremiah P.

doi:10.1088/0004-637x/727/2/94

Cited by 109 publications

(195 citation statements)

References 69 publications

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“…Kinetic SZ: the kSZ template used here is from Trac et al (2011). We solve for the amplitude A kSZ (in units of µK 2 ):…”

Section: Model Of Unresolved Foregrounds and "Nuisance" Parametersmentioning

confidence: 99%

“…We have not investigated extensively the impact of varying the tSZ and kSZ templates. A variety of different approaches (analytic, semi-analytic and numerical) have been used to estimate tSZ templates (e.g., Komatsu & Seljak 2002;Sehgal et al 2010;Trac et al 2011;Battaglia et al 2010Battaglia et al , 2012. These have similar shapes at multipoles < ∼ 3000, relevant to Planck and to the tSZ template used here.…”

Section: C1 Impact Of Foreground Priorsmentioning

confidence: 99%

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Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

4,999

163

2,253

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This paper presents the first cosmological results based on Planck measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra. We find that the Planck spectra at high multipoles ( > ∼ 40) are extremely well described by the standard spatiallyflat six-parameter ΛCDM cosmology with a power-law spectrum of adiabatic scalar perturbations. Within the context of this cosmology, the Planck data determine the cosmological parameters to high precision: the angular size of the sound horizon at recombination, the physical densities of baryons and cold dark matter, and the scalar spectral index are estimated to be θ * = (1.04147 ± 0.00062) × 10 −2 , Ω b h 2 = 0.02205 ± 0.00028, Ω c h 2 = 0.1199 ± 0.0027, and n s = 0.9603 ± 0.0073, respectively (note that in this abstract we quote 68% errors on measured parameters and 95% upper limits on other parameters). For this cosmology, we find a low value of the Hubble constant, H 0 = (67.3 ± 1.2) km s −1 Mpc −1 , and a high value of the matter density parameter, Ω m = 0.315 ± 0.017. These values are in tension with recent direct measurements of H 0 and the magnituderedshift relation for Type Ia supernovae, but are in excellent agreement with geometrical constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent level precision using Planck CMB data alone. We use high-resolution CMB data together with Planck to provide greater control on extragalactic foreground components in an investigation of extensions to the six-parameter ΛCDM model. We present selected results from a large grid of cosmological models, using a range of additional astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured over the standard six-parameter ΛCDM cosmology. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find an upper limit of r 0.002 < 0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles beyond the three families of neutrinos in the standard model. Using BAO and CMB data, we find N eff = 3.30 ± 0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the sum of neutrino masses. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of N eff = 3.046. We find no evidence for dynamical dark energy; using BAO and CMB data, the dark energy equation of state parameter is constrained to be w = −1.13 +0.13 −0.10 . We also use the Planck data to set limits on a possible variation of the fine-structure constant, dark matter annihilation and primordial magnetic fields. Despite the success of the six-parameter ΛCDM model in describing the Planck data at high multipoles, we note that this cosmology does not provide a good fit to the temperature power spectrum at low multipoles. T...

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“…Kinetic SZ: the kSZ template used here is from Trac et al (2011). We solve for the amplitude A kSZ (in units of µK 2 ):…”

Section: Model Of Unresolved Foregrounds and "Nuisance" Parametersmentioning

confidence: 99%

Section: C1 Impact Of Foreground Priorsmentioning

confidence: 99%

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

4,999

163

2,253

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“…Second, for the kinetic SZ effect we adopt the template described by Trac et al (2011), and as in Eq. (14) we treat the dimensionless amplitude of the template, A kSZ , as a free parameter,…”

Section: Unresolved Sunyaev-zeldovich Effectsmentioning

confidence: 99%

Planck2013 results. XV. CMB power spectra and likelihood

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

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263

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This paper presents the Planck 2013 likelihood, a complete statistical description of the two-point correlation function of the CMB temperature fluctuations that accounts for all known relevant uncertainties, both instrumental and astrophysical in nature. We use this likelihood to derive our best estimate of the CMB angular power spectrum from Planck over three decades in multipole moment, , covering 2 ≤ ≤ 2500. The main source of uncertainty at < ∼ 1500 is cosmic variance. Uncertainties in small-scale foreground modelling and instrumental noise dominate the error budget at higher s. For < 50, our likelihood exploits all Planck frequency channels from 30 to 353 GHz, separating the cosmological CMB signal from diffuse Galactic foregrounds through a physically motivated Bayesian component separation technique. At ≥ 50, we employ a correlated Gaussian likelihood approximation based on a fine-grained set of angular cross-spectra derived from multiple detector combinations between the 100, 143, and 217 GHz frequency channels, marginalising over power spectrum foreground templates. We validate our likelihood through an extensive suite of consistency tests, and assess the impact of residual foreground and instrumental uncertainties on the final cosmological parameters. We find good internal agreement among the high-cross-spectra with residuals below a few µK 2 at < ∼ 1000, in agreement with estimated calibration uncertainties. We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. We further show that the best-fit ΛCDM cosmology is in excellent agreement with preliminary Planck EE and T E polarisation spectra. We find that the standard ΛCDM cosmology is well constrained by Planck from the measurements at < ∼ 1500. One specific example is the spectral index of scalar perturbations, for which we report a 5.4σ deviation from scale invariance, n s = 1. Increasing the multipole range beyond 1500 does not increase our accuracy for the ΛCDM parameters, but instead allows us to study extensions beyond the standard model. We find no indication of significant departures from the ΛCDM framework. Finally, we report a tension between the Planck best-fit ΛCDM model and the low-spectrum in the form of a power deficit of 5-10% at < ∼ 40, with a statistical significance of 2.5-3σ. Without a theoretically motivated model for this power deficit, we do not elaborate further on its cosmological implications, but note that this is our most puzzling finding in an otherwise remarkably consistent data set.

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“…Besides this UPP model procedure, three other approaches have been adopted by the ACT team to study the scaling relations that allow us to estimate M 500 from the cluster SZ signal strength. These are based on (i) structure formation simulations (Bode et al 2012), where the density and temperature of the intracluster are modeled as a virialized ideal gas (M B12 500 ); (ii) a nonthermal pressure and adiabatic model for the gas (M non-thermal 500 ; Trac et al 2011); and (iii) a dynamical estimate of the cluster mass using the galaxy velocity dispersions (M dyn 500 ; Sifon et al 2013). It is worth mentioning that, when assuming the so-called concordance cosmology (a flat ΛCDM model with Ω m = 0.3), the scaling from UPP is nearly identical to the adiabatic nonthermal model, while a model incorporating non-thermal pressure is in better agreement with dynamical mass measurements .…”

Section: F Gasmentioning

confidence: 99%

Constraints on the duality relation from ACT cluster data

Gonçalves

Bernui

Holanda

et al. 2014

A&A

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Aims. The cosmic distance-duality relation, d L (z)/d A (z)(1 + z) 2 = η, where d L (z) and d A (z) are, respectively, the luminosity and the angular diameter distances and where η = 1 holds as long as the number of photons is conserved and gravity is described by a metric theory. Testing such hypotheses is, therefore, an important task for both cosmology and fundamental physics. Methods. We estimated the gas mass fraction of 91 galaxy clusters (GC) from current measurements of the GC total mass recently reported by the Atacama Cosmology Telescope collaboration. We use these data, along with type Ia supernovae observations of the Union 2.1 compilation, to test a possible deviation from the value η = 1. Results. Although they agree with the standard hypothesis, we find that this combination of both data tends to favor values of η less than 1, which might be associated with some physical processes that increase the number of photons and modifying the above relation to d L < (1 + z) 2 d A .

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Templates for the Sunyaev-Zel’dovich Angular Power Spectrum

Cited by 109 publications

References 69 publications

Planck2013 results. XVI. Cosmological parameters

Planck2013 results. XVI. Cosmological parameters

Planck2013 results. XV. CMB power spectra and likelihood

Constraints on the duality relation from ACT cluster data

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