Kinematic Sunyaev-Zel'dovich Cosmic Microwave Background Temperature Anisotropies Generated by Gas in Cosmic Structures

Atrio-Barandela, F.; Mücket, J. P.; Génova-Santos, R. T.

doi:10.1086/529139

Cited by 20 publications

(33 citation statements)

References 25 publications

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“…As explained in Atrio-Barandela et al (2008a), the distribution of the effect is rather skewed and 9% of all lines of sight will produce an effect 1.8-6 times larger than the estimate from eq. (7).…”

Section: The Thermal and Kinematic Sz Effect From The Igm/whimmentioning

confidence: 81%

“…Similar arguments can be used to compute the correlation function of the kSZ effect due to two filaments located at distances l and l ′ along two lines of sight separated by an angle α (see Atrio-Barandela et al (2008a) for further details):…”

Section: The Thermal and Kinematic Sz Effect From The Igm/whimmentioning

confidence: 99%

“…The predicted power spectrum of the tSZ effect peaks at ℓ ∼ 2000-4000, with an amplitude similar to the tSZ from galaxy clusters. More recently, in Atrio-Barandela et al (2008a) we studied the contribution of the kinematic SZ (kSZ, Sunyaev & Zeldovich 1980) effect. We found that the kSZ power spectrum had a maximum at ℓ ∼ 400-600.…”

Section: Introductionmentioning

confidence: 99%

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THE CONTRIBUTION OF THE KINEMATIC SUNYAEV-ZEL'DOVICH EFFECT FROM THE WARM-HOT INTERGALACTIC MEDIUM TO THE FIVE-YEARWILKINSON MICROWAVE ANISOTROPY PROBEDATA

Génova-Santos¹,

Atrio-Barandela²,

Mücket³

et al. 2009

ApJ

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We study the contribution of the kinematic Sunyaev-Zel'dovich (kSZ) effect, generated by the warm-hot intergalactic medium (WHIM), to the cosmic microwave background (CMB) temperature anisotropies in the Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) data. We explore the concordance ΛCDM cosmological model, with and without this kSZ contribution, using a Markov chain Monte Carlo algorithm. Our model requires a single extra parameter to describe this new component. Our results show that the inclusion of the kSZ signal improves the fit to the data without significantly altering the best-fit cosmological parameters except Ω b h 2 . The improvement is localized at the ℓ 500 multipoles. For the best-fit model, this extra component peaks at ℓ ∼ 450 with an amplitude of 129 µK 2 , and represents 3.1% of the total power measured by the Wilkinson Microwave Anisotropy Probe. Nevertheless, at the 2σ level a null kSZ contribution is still compatible with the data. Part of the detected signal could arise from unmasked point sources and/or Poissonianly distributed foreground residuals. A statistically more significant detection requires the wider frequency coverage and angular resolution of the forthcoming Planck mission.

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Section: The Thermal and Kinematic Sz Effect From The Igm/whimmentioning

confidence: 81%

Section: The Thermal and Kinematic Sz Effect From The Igm/whimmentioning

confidence: 99%

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THE CONTRIBUTION OF THE KINEMATIC SUNYAEV-ZEL'DOVICH EFFECT FROM THE WARM-HOT INTERGALACTIC MEDIUM TO THE FIVE-YEARWILKINSON MICROWAVE ANISOTROPY PROBEDATA

Génova-Santos¹,

Atrio-Barandela²,

Mücket³

et al. 2009

ApJ

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“…However, at lower electron temperatures, like those of the WHIM, both components become comparable. In a recent work, Atrio‐Barandela, Mücket & Génova‐Santos (2008) argued that the kinetic SZ effect generated in WHIM structures could have an important contribution. They estimate that 1 per cent of all WHIM filaments of size ∼5 Mpc, aligned with the line of sight, produce a combined thermal and kinetic SZ effect that could account for the total flux density observed in decrement H. In particular, a filament of size L ≈ 5 Mpc and electron density n e ≈ 10 3 m −3 could produce a combined thermal and kinetic SZ signal of ≈− 200 μK.…”

Section: Origin Of the Decrementmentioning

confidence: 99%

Observations of the Corona Borealis supercluster with the superextended Very Small Array: further constraints on the nature of the non-Gaussian cosmic microwave background cold spot

Génova-Santos¹,

Rubiño-Martín²,

Rebolo³

et al. 2008

Monthly Notices of the Royal Astronomical Society

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We present interferometric imaging at 33 GHz, with the new superextended configuration of the Very Small Array (VSA), of a very deep decrement in the cosmic microwave background (CMB) temperature. This decrement is located in the direction of the Corona Borealis supercluster, at a position with no known galaxy clusters, and was discovered by a previous VSA survey. A total area of 3 deg2 has now been imaged, with an angular resolution of 7 arcmin and a flux sensitivity of 5 mJy beam−1. These observations confirm the presence of this strong and resolved negative spot at −37 ± 5 mJy beam−1(−229 ± 32 μK). This structure is also present in the Wilkinson Microwave Anisotropy Probe 5‐year data. The temperature of the W‐band (94 GHz) data at the position of the decrement agrees within 0.3σn with that observed by the VSA at 33 GHz and within 0.2σn with the Sunyaev–Zel'dovich (SZ) spectrum. Our analyses show that it is a non‐Gaussian feature in the CMB at a level of 4.4σ, where sigma accounts for primordial CMB fluctuations, thermal noise and residual radio source contributions. The probability of finding such a deviation or larger in simulations including Gaussian CMB is only 0.63 per cent. Therefore, an explanation other than primordial Gaussian CMB is required. We have considered the possibility of an SZ effect generated in a diffuse, extended warm/hot gas distribution. This hypothesis is especially relevant, as the presence of such structures, if confirmed, could provide the location for a significant fraction of the missing baryons in the Local Universe. However, from the absence of X‐ray emission in this region we conclude that the whole decrement cannot be generated solely via the SZ effect in such structure. Therefore, the most plausible scenario is a combination between a negative CMB feature and a SZ effect, probably generated by a warm/hot gas distribution.

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“…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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Kinematic Sunyaev-Zel'dovich Cosmic Microwave Background Temperature Anisotropies Generated by Gas in Cosmic Structures

Cited by 20 publications

References 25 publications

THE CONTRIBUTION OF THE KINEMATIC SUNYAEV-ZEL'DOVICH EFFECT FROM THE WARM-HOT INTERGALACTIC MEDIUM TO THE FIVE-YEARWILKINSON MICROWAVE ANISOTROPY PROBEDATA

THE CONTRIBUTION OF THE KINEMATIC SUNYAEV-ZEL'DOVICH EFFECT FROM THE WARM-HOT INTERGALACTIC MEDIUM TO THE FIVE-YEARWILKINSON MICROWAVE ANISOTROPY PROBEDATA

Observations of the Corona Borealis supercluster with the superextended Very Small Array: further constraints on the nature of the non-Gaussian cosmic microwave background cold spot

Lensing and the Warm-hot Intergalactic Medium

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