Triple Experiment Spectrum of the Sunyaev-Zel'dovich Effect in the Coma Cluster:
                    <i>H</i>
                    <sub>0</sub>

Battistelli, E. S.; Petris, M. De; Lamagna, L.; Luzzi, G.; Maoli, R.; Melchiorri, A.; Melchiorri, F.; Orlando, A.; Palladino, Emilia; Savini, G.; Rephaeli, Yoel; Shimon, Meir; Signore, M.; Colafrancesco, S.

doi:10.1086/380778

Cited by 35 publications

(29 citation statements)

References 29 publications

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“…Using the same θ c and β as above, Battistelli et al (2003) found ΔT SZ (0) = −184 ± 39, −32 ± 79, and +172±36μK (68% CL) at 143, 214, and 272 GHz, respectively, in units of thermodynamic temperatures. As MITO has three frequencies, they were able to separate SZ, CMB, and the atmospheric fluctuation.…”

Section: −1mentioning

confidence: 79%

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Komatsu¹,

Smith²,

Dunkley³

et al. 2011

ApJS

7,710

472

6,429

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The combination of seven-year data from WMAP and improved astrophysical data rigorously tests the standard cosmological model and places new constraints on its basic parameters and extensions. By combining the WMAP data with the latest distance measurements from the baryon acoustic oscillations (BAO) in the distribution of galaxies and the Hubble constant (H 0 ) measurement, we determine the parameters of the simplest six-parameter ΛCDM model. The power-law index of the primordial power spectrum is n s = 0.968 ± 0.012 (68% CL) for this data combination, a measurement that excludes the Harrison-Zel'dovich-Peebles spectrum by 99.5% CL. The other parameters, including those beyond the minimal set, are also consistent with, and improved from, the five-year results. We find no convincing deviations from the minimal model. The seven-year temperature power spectrum gives a better determination of the third acoustic peak, which results in a better determination of the redshift of the matter-radiation equality epoch. Notable examples of improved parameters are the total mass of neutrinos, m ν < 0.58 eV (95% CL), and the effective number of neutrino species, N eff = 4.34 +0.86 −0.88 (68% CL), which benefit from better determinations of the third peak and H 0 . The limit on a constant dark energy equation of state parameter from WMAP+BAO+H 0 , without high-redshift Type Ia supernovae, is w = −1.10 ± 0.14 (68% CL). We detect the effect of primordial helium on the temperature power spectrum and provide a new test of big bang nucleosynthesis by measuring Y p = 0.326 ± 0.075 (68% CL). We detect, and show on the map for the first time, the tangential and radial polarization patterns around hot and cold spots of temperature fluctuations, an important test of physical processes at z = 1090 and the dominance of adiabatic scalar fluctuations. The seven-year polarization data have significantly improved: we now detect the temperature-E-mode polarization cross power spectrum at 21σ , compared with 13σ from the five-year data. With the seven-year temperature-B-mode cross power spectrum, the limit on a rotation of the polarization plane due to potential parity-violating effects has improved by 38% to Δα = −1.• 1 ± 1.• 4(statistical) ± 1.• 5(systematic) (68% CL). We report significant detections of the Sunyaev-Zel'dovich (SZ) effect at the locations of known clusters of galaxies. The measured SZ signal agrees well with the expected signal from the X-ray data on a cluster-by-cluster basis. However, it is a factor of 0.5-0.7 times the predictions from "universal profile" of Arnaud et al., analytical models, and hydrodynamical simulations. We find, for the first time in the SZ effect, a significant difference between the cooling-flow and non-cooling-flow clusters (or relaxed and non-relaxed clusters), which can explain some of the discrepancy. This lower amplitude is consistent with the lower-than-theoretically expected SZ power spectrum recently measured by the South Pole Telescope Collaboration.

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Section: −1mentioning

confidence: 79%

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Komatsu¹,

Smith²,

Dunkley³

et al. 2011

ApJS

7,710

472

6,429

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“…The spectral signature of the SZ effect can in principle probe the electron gas distribution and constrain any non-thermal electron population in the intracluster medium. Moreover multi-frequency SZ measurements might provide a novel way of constraining the CMB temperature and its evolution with redshift (Battistelli et al 2003, Horellou et al 2005). To achieve these goals, high precision measurements of the SZ effect will be needed over large areas of the sky.…”

Section: Discussionmentioning

confidence: 99%

Secondary anisotropies of the CMB

Aghanim¹,

Majumdar²,

Silk³

2008

Rep. Prog. Phys.

104

101

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Abstract.The Cosmic Microwave Background fluctuations provide a powerful probe of the dark ages of the universe through the imprint of the secondary anisotropies associated with the reionisation of the universe and the growth of structure. We review the relation between the secondary anisotropies and and the primary anisotropies that are directly generated by quantum fluctuations in the very early universe. The physics of secondary fluctuations is described, with emphasis on the ionisation history and the evolution of structure. We discuss the different signatures arising from the secondary effects in terms of their induced temperature fluctuations, polarisation and statistics. The secondary anisotropies are being actively pursued at present, and we review the future and current observational status.

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“…In this paper, we only fit for the thermal SZ effect in two separate regions around the Coma and Virgo clusters, which are by far the two strongest SZ objects on the sky, in order to prevent these from contaminating the other components. While the SZ decrement for the Coma cluster is as large as −400 µK below 100 GHz on an angular scale of a few arcminutes (Battistelli et al 2003;Planck Collaboration Int. X 2013), and for the Virgo cluster a few tens of microkelvin on a few degrees scale (Diego & Ascasibar 2008), it is only a few microkelvin for most other objects after convolution with the large beams considered in this paper.…”

mentioning

confidence: 99%

Planck2015 results

Adam¹,

Ade²,

Aghanim³

et al. 2016

A&A

Self Cite

426

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Planck has mapped the microwave sky in temperature over nine frequency bands between 30 and 857 GHz and in polarization over seven frequency bands between 30 and 353 GHz in polarization. In this paper we consider the problem of diffuse astrophysical component separation, and process these maps within a Bayesian framework to derive an internally consistent set of full-sky astrophysical component maps. Component separation dedicated to cosmic microwave background (CMB) reconstruction is described in a companion paper. For the temperature analysis, we combine the Planck observations with the 9-yr Wilkinson Microwave Anisotropy Probe (WMAP) sky maps and the Haslam et al. 408 MHz map, to derive a joint model of CMB, synchrotron, free-free, spinning dust, CO, line emission in the 94 and 100 GHz channels, and thermal dust emission. Full-sky maps are provided for each component, with an angular resolution varying between 7. 5 and 1 • . Global parameters (monopoles, dipoles, relative calibration, and bandpass errors) are fitted jointly with the sky model, and best-fit values are tabulated. For polarization, the model includes CMB, synchrotron, and thermal dust emission. These models provide excellent fits to the observed data, with rms temperature residuals smaller than 4 µK over 93% of the sky for all Planck frequencies up to 353 GHz, and fractional errors smaller than 1% in the remaining 7% of the sky. The main limitations of the temperature model at the lower frequencies are internal degeneracies among the spinning dust, free-free, and synchrotron components; additional observations from external low-frequency experiments will be essential to break these degeneracies. The main limitations of the temperature model at the higher frequencies are uncertainties in the 545 and 857 GHz calibration and zero-points. For polarization, the main outstanding issues are instrumental systematics in the 100-353 GHz bands on large angular scales in the form of temperature-to-polarization leakage, uncertainties in the analogue-to-digital conversion, and corrections for the very long time constant of the bolometer detectors, all of which are expected to improve in the near future.

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Triple Experiment Spectrum of the Sunyaev-Zel'dovich Effect in the Coma Cluster: H ₀

Cited by 35 publications

References 29 publications

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Secondary anisotropies of the CMB

Planck2015 results

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Triple Experiment Spectrum of the Sunyaev-Zel'dovich Effect in the Coma Cluster: H 0

Cited by 35 publications

References 29 publications

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Secondary anisotropies of the CMB

Planck2015 results

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Product

Resources

About

Triple Experiment Spectrum of the Sunyaev-Zel'dovich Effect in the Coma Cluster: H ₀