The Contribution of the Intergalactic Medium to Cosmic Microwave Background Anisotropies

Atrio-Barandela, F.; Mücket, J. P.

doi:10.1086/502709

Cited by 19 publications

(30 citation statements)

References 36 publications

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“…In our first-year analysis we reported detections of an SZ signal from the Coma cluster and from an aggregate sample of X-ray-selected Abell clusters, the XBAC catalog. Since then, there have been numerous additional reports of SZ signal detection in the first-year WMAP data (Fosalba & Gaztañaga 2004;Fosalba et al 2003;Myers et al 2004;Afshordi et al 2004Afshordi et al , 2005Hernández-Monteagudo & Rubiño-Martín 2004;Hansen et al 2005;Atrio-Barandela & Muecket 2006). In this section, we update our results for the Coma cluster and the XBAC catalog; in subsequent cosmological studies, we mask these clusters from the data.…”

Section: Sunyaev-zeldovich (Sz ) Effectmentioning

confidence: 95%

Three‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Temperature Analysis

Hinshaw

Nolta

Bennett

et al. 2007

ASTROPHYS J SUPPL S

1,181

1,209

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We present new full-sky temperature maps in five frequency bands from 23 to 94 GHz, based on data from the first 3 years of the WMAP sky survey. The new maps are consistent with the first-year maps and are more sensitive. The 3 year maps incorporate several improvements in data processing made possible by the additional years of data and by a more complete analysis of the polarization signal. These include several new consistency tests as well as refinements in the gain calibration and beam response models. We employ two forms of multifrequency analysis to separate astrophysical foreground signals from the CMB, each of which improves on our first-year analyses. First, we form an improved ''Internal Linear Combination'' (ILC) map, based solely on WMAP data, by adding a bias-correction step and by quantifying residual uncertainties in the resulting map. Second, we fit and subtract new spatial templates that trace Galactic emission; in particular, we now use low-frequency WMAP data to trace synchrotron emission instead of the 408 MHz sky survey. The WMAP point source catalog is updated to include 115 new sources whose detection is made possible by the improved sky map sensitivity. We derive the angular power spectrum of the temperature anisotropy using a hybrid approach that combines a maximum likelihood estimate at low l (large angular scales) with a quadratic cross-power estimate for l > 30. The resulting multifrequency spectra are analyzed for residual point source contamination. At 94 GHz the unmasked sources contribute 128 AE 27 K 2 to l(l þ 1)C l /2 at l ¼ 1000. After subtracting this contribution, our best estimate of the CMB power spectrum is derived by averaging cross-power spectra from 153 statistically independent channel pairs. The combined spectrum is cosmic variance limited to l ¼ 400, and the signal-to-noise ratio per l-mode exceeds unity up to l ¼ 850. For bins of width Ál/l ¼ 3%, the signal-to-noise ratio exceeds unity up to l ¼ 1000. The first two acoustic peaks are seen at l ¼ 220:8 AE 0:7 and l ¼ 530:9 AE 3:8, respectively, while the first two troughs are seen at l ¼ 412:4 AE 1:9 and l ¼ 675:2 AE 11:1. The rise to the third peak is unambiguous; when the WMAP data are combined with higher resolution CMB measurements, the existence of a third acoustic peak is well established. Spergel et al. use the 3 year temperature and polarization data to constrain cosmological model parameters. A simple six-parameter ÃCDM model continues to fit CMB data and other measures of large-scale structure remarkably well. The new polarization data produce a better measurement of the optical depth to reionization, ¼ 0:089 AE 0:03. This new and tighter constraint on helps break a degeneracy with the scalar spectral index, which is now found to be n s ¼ 0:960 AE 0:016. If additional cosmological data sets are included in the analysis, the spectral index is found to be n s ¼ 0:947 AE 0:015.

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Section: Sunyaev-zeldovich (Sz ) Effectmentioning

confidence: 95%

Three‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Temperature Analysis

Hinshaw

Nolta

Bennett

et al. 2007

ASTROPHYS J SUPPL S

1,181

1,209

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“…Although the density contrast of the WHIM is moderate (δ < 100), its temperature is high (10 5 K < T < 10 7 K), and it is supposed to make a significant contribution to the cosmic baryon budget of ≈50%. Estimates provided by Atrio-Barandela & Mücket (2006), AtrioBarandela et al (2008), and Génova-Santos et al (2009) indicate on a non-negligible contribution, which under certain conditions might be even comparable with the overall SZ contribution of clusters of galaxies. Thus the SZ effect could serve as an additional detection channel for the WHIM.…”

Section: Introductionmentioning

confidence: 82%

A detailed view of filaments and sheets in the warm-hot intergalactic medium

Klar

Mücket

2010

A&A

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Context. Numerical simulations predict that a considerable fraction of the missing baryons at redshift z ≈ 0 rest in the so-called warmhot intergalactic medium (WHIM). The filaments and sheets of the WHIM have high temperatures (10 5 −10 7 K) and a high degree of ionization but only low to intermediate densities. Therefore, their reliable detection is a challenging task for today's observational cosmology. The particular physical conditions of the WHIM structures, e.g. density and temperature profiles, or velocity fields, are expected to leave their special imprint on spectroscopic observations. Aims. In order to get further insight into these conditions, we performed hydrodynamical simulations of the WHIM. Instead of analyzing extensive simulations of cosmological structure formation, we simulate certain well-defined structures and studied the impact of different physical processes as well as of the scale dependencies. Methods. We started with a comprehensive study of the one-dimensional collapse (pancake) and examined the influence of radiative cooling, heating due to an UV background, and thermal conduction. We investigated the effect of small-scale perturbations given by the cosmological power spectrum. Results. If the initial perturbation length scale L exceeds ≈2 Mpc the collapse leads to shock-confined structures. As a result of radiative cooling and of heating due to an UV background a relatively cold and dense core forms in the one-dimensional case. The properties of the core (extension, density, and temperature) are correlated with L. For longer L the core sizes are more concentrated. Thermal conduction enhances this trend and may even result in an evaporation of the core. Our estimates predict that a core may start to evaporate for perturbation lengths longer than L ≈ 30 Mpc. Though the physics in the corresponding three-dimensional case is much more complex, one might expect a similar regulation mechanism with respect to the cold streams along filaments, too. However, this question will be addressed in a forthcoming paper. The obtained detailed profiles for density and temperature for prototype WHIM structures allow for the determination of possible spectral signatures by the WHIM.

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“…The non-linear baryon density contrast ξ in units of the baryon mean density should not be confused with δ or δ B , respectively the matter and IGM baryon overdensities in the linear regime; ξ is given in terms of the gaussian distributed variable δ B (Choudhury et al 2001, Atrio-Barandela & Mücket 2006 …”

Section: Lensing-tsz Correlation In the Filament Modelmentioning

confidence: 99%

“…Since the WHIM is highly ionized, there has been an extensive search on the thermal and kinematic SunyaevZel'dovich CMB temperature anisotropies (hereafter tSZ and kSZ, Sunyaev & Zeldovich 1970;Sunyaev & Zeldovich 1972) generated by this baryon component (Atrio-Barandela & Mücket 2006;Atrio-Barandela et al 2008). Crosscorrelation of CMB temperature data from WMAP or Planck with matter templates produced only marginal evidence of tSZ anisotropies due to the WHIM (Suarez-Velásquez et al 2013b, Génova-Santos et al 2013.…”

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confidence: 99%

Lensing and the Warm-hot Intergalactic Medium

Atrio-Barandela

Mücket

2017

ApJ

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The correlation of weak lensing and Cosmic Microwave Anisotropy (CMB) data traces the pressure distribution of the hot, ionized gas and the underlying matter density field. The measured correlation is dominated by baryons residing in halos. Detecting the contribution from unbound gas by measuring the residual cross-correlation after masking all known halos requires a theoretical understanding of this correlation and its dependence with model parameters. Our model assumes that the gas in filaments is well described by a log-normal probability distribution function, with temperatures 10 5−7 K and overdensities ξ ≤ 100. The lensing-comptonization cross-correlation is dominated by gas with overdensities in the range ξ ≈ [3 − 33]; the signal is generated at redshifts z ≤ 1. If only 10% of the measured cross-correlation is due to unbound gas, then the most recent measurements set an upper limit ofT e < ∼ 10 6 K on the mean temperature of Inter Galactic Medium. The amplitude is proportional to the baryon fraction stored in filaments. The lensing-comptonization power spectrum peaks at a different scale than the gas in halos making it possible to distinguish both contributions. To trace the distribution of the low density and low temperature plasma on cosmological scales, the effect of halos will have to be subtracted from the data, requiring observations with larger signal-to-noise ratio than currently available.

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The Contribution of the Intergalactic Medium to Cosmic Microwave Background Anisotropies

Cited by 19 publications

References 36 publications

Three‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Temperature Analysis

Three‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Temperature Analysis

A detailed view of filaments and sheets in the warm-hot intergalactic medium

Lensing and the Warm-hot Intergalactic Medium

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