Evidence of the Missing Baryons from the Kinematic Sunyaev-Zeldovich Effect in Planck Data

Hernández-Monteagudo, C.; Ma, Yin-Zhe; Kitaura, Francisco-Shu; Wang, Wenting; Génova-Santos, R. T.; Macías-Pérez, J. F.; Herranz, D.

doi:10.1103/physrevlett.115.191301

Cited by 78 publications

(100 citation statements)

References 24 publications

(57 reference statements)

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“…The kSZ effect, on the other hand, while much more difficult to detect, is affected by all ionized gas regardless of its temperature, providing a more global and unbiased view of the universe during and after reionization. The next generation of ground based CMB surveys, such as the Simons Observatory (SO 1 ) and CMB-S4 2 (Abazajian et al 2016) will use the kSZ effect both as a probe of the intergalactic medium (Hernández-Monteagudo et al 2015;Schaan et al 2016;Hill et al 2016;Soergel et al 2016;De Bernardis et al 2017;: cosmology with large-scale velocity flows (Mueller et al 2015a;Sugiyama et al 2017;Mueller et al 2015b;) will soon become a reality. The kSZ effect can be detected in the cosmic microwave background alone or by cross-correlating it with tracers of large-scale structure such as galaxies and clusters.…”

Section: Introductionmentioning

confidence: 99%

The Impact of Baryonic Physics on the Kinetic Sunyaev–Zel’dovich Effect

Park

Alvarez

Bond

2018

ApJ

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Poorly understood "baryonic physics" impacts our ability to predict the power spectrum of the kinetic Sunyaev-Zel'dovich (kSZ) effect. We study this in one sample high resolution simulation of galaxy formation and feedback, Illustris. The high resolution of Illustris allows us to probe the kSZ power spectrum on multipoles = 10 3 − 3 × 10 4 . Strong AGN feedback in Illustris nearly wipes out gas fluctuations at k 1 h Mpc −1 and at late times, likely somewhat under predicting the kSZ power generated at z 1. The post-reionization kSZ power spectrum for Illustris is well-fit by D z<6 = 1.38[ /3000] 0.21 µK 2 over 3000 10000, somewhat lower than most other reported values but consistent with the analysis of Shaw et al. Our analysis of the bias of free electrons reveals subtle effects associated with the multi-phase gas physics and stellar fractions that affect even linear scales. In particular there are fewer electrons in biased galaxies, due to gas cooling and star formation, and this leads to an electron bias less than one even at low wavenumbers. The combination of bias and electron fraction that determines the overall suppression is relatively constant, f 2 e b 2 e0 ∼ 0.7, but more simulations are needed to see if this is Illustris-specific. By separating the kSZ power into different terms, we find at least 6 (10)% of the signal at = 3000 (10000) comes from non-Gaussian connected four-point density and velocity correlations, δvδv c , even without correcting for the Illustris simulation box size. A challenge going forward will be to accurately model long-wave velocity modes simultaneously with Illustris-like high resolution to capture the complexities of galaxy formation and its correlations with large scale flows. Subject headings:1. INTRODUCTION The cosmic microwave background (CMB) is a powerful probe of cosmic history through secondary anisotropies generated by free electrons in the intergalactic medium, resulting in a spectral distortion and cluster-concentrated anisotropies from inverse Compton scattering off of hot gas in galaxy clusters, the thermal Sunyaev-Zel'dovich (tSZ) effect (e.g., Sunyaev and Zeldovich 1972), and spectrally undistorted temperature anisotropies from Thompson scattering from moving electrons participating in the bulk flow of the medium, the kinetic Sunyeav-Zel'dovich (kSZ) (e.g., Sunyaev and Zeldovich 1980) effect.Of these two, the tSZ effect is much easier to detect because it is determined by electron pressure, which is much higher in clusters. The distinct spectral signature allows it to be separated from other sky signals if observations are made in multiple frequency bands. Because the tSZ effect is dominated by massive clusters, however, it gives a rather biased view of the intergalactic medium, concentrated towards the rarest peaks at relatively late times, z 1.5 (e.g., Komatsu and Seljak 2002). The kSZ effect, on the other hand, while much more difficult to detect, is affected by all ionized gas regardless of its temperature, providing a more global and unbiased view o...

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Section: Introductionmentioning

confidence: 99%

The Impact of Baryonic Physics on the Kinetic Sunyaev–Zel’dovich Effect

Park

Alvarez

Bond

2018

ApJ

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“…Hernández-Monteagudo et al 2015;Nevalainen et al 2015;Planck Collaboration XXXVII 2015), we have designed a program to detect the putative filaments connecting cluster pairs in absorption. This technique has several advantages over attempts to detect the gas in emission.…”

Section: Introductionmentioning

confidence: 99%

Towards the statistical detection of the warm–hot intergalactic medium in intercluster filaments of the cosmic web

Tejos

Prochaska

Crighton

et al. 2015

Mon. Not. R. Astron. Soc.

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Modern analyses of structure formation predict a universe tangled in a 'cosmic web' of dark matter and diffuse baryons. These theories further predict that at low-z, a significant fraction of the baryons will be shock-heated to T ∼ 10 5 − 10 7 K yielding a warm-hot intergalactic medium (WHIM), but whose actual existence has eluded a firm observational confirmation. We present a novel experiment to detect the WHIM, by targeting the putative filaments connecting galaxy clusters. We use HST/COS to observe a remarkable QSO sightline that passes within ∆d = 3 Mpc from the 7 inter-cluster axes connecting 7 independent cluster-pairs at redshifts 0.1 z 0.5. We find tentative excesses of total H I, narrow H I (NLA; Doppler parameters b < 50 km s −1 ), broad H I (BLA; b 50 km s −1 ) and O VI absorption lines within rest-frame velocities of ∆v 1000 km s −1 from the cluster-pairs redshifts, corresponding to ∼ 2, ∼ 1.7, ∼ 6 and ∼ 4 times their field expectations, respectively. Although the excess of O VI likely comes from gas close to individual galaxies, we conclude that most of the excesses of NLAs and BLAs are truly intergalactic. We find the covering fractions, f c , of BLAs close to cluster-pairs are ∼ 4 − 7 times higher than the random expectation (at the ∼ 2σ c.l.), whereas the f c of NLAs and O VI are not significantly enhanced. We argue that a larger relative excess of BLAs compared to those of NLAs close to cluster-pairs may be a signature of the WHIM in inter-cluster filaments. By extending the present analysis to tens of sightlines our experiment offers a promising route to detect the WHIM.

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“…We obtain τ T = (1.39 ± 0.46) × 10 −4 (i.e., at the 3σ level) for the SEVEM map, with very similar values for all other foreground-cleaned maps. We defer the physical interpretation of the kSZ measurements of this paper to an external publication, (Hernández-Monteagudo et al 2015).…”

Section: Cross-correlation Analysis With Estimated Peculiar Velocitiesmentioning

confidence: 99%

Planckintermediate results

Ade

Aghanim

Arnaud

et al. 2016

A&A

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By looking at the kinetic Sunyaev-Zeldovich effect (kSZ) in Planck nominal mission data, we present a significant detection of baryons participating in large-scale bulk flows around central galaxies (CGs) at redshift z ≈ 0.1. We estimate the pairwise momentum of the kSZ temperature fluctuations at the positions of the Central Galaxy Catalogue (CGC) samples extracted from Sloan Digital Sky Survey (SDSS-DR7) data. For the foreground-cleaned SEVEM, SMICA, NILC, and COMMANDER maps, we find 1.8-2.5σ detections of the kSZ signal, which are consistent with the kSZ evidence found in individual Planck raw frequency maps, although lower than found in the WMAP-9yr W-band (3.3σ). We further reconstruct the peculiar velocity field from the CG density field, and compute for the first time the cross-correlation function between kSZ temperature fluctuations and estimates of CG radial peculiar velocities. This correlation function yields a 3.0-3.7σ detection of the peculiar motion of extended gas on Mpc scales in flows correlated up to distances of 80-100 h −1 Mpc. Both the pairwise momentum estimates and the kSZ temperature-velocity field correlation find evidence for kSZ signatures out to apertures of 8 arcmin and beyond, corresponding to a physical radius of >1 Mpc, more than twice the mean virial radius of halos. This is consistent with the predictions from hydrodynamical simulations that most of the baryons are outside the virialized halos. We fit a simple model, in which the temperature-velocity cross-correlation is proportional to the signal seen in a semi-analytic model built upon N-body simulations, and interpret the proportionality constant as an effective optical depth to Thomson scattering. We find τ T = (1.4 ± 0.5) × 10 −4 ; the simplest interpretation of this measurement is that much of the gas is in a diffuse phase, which contributes little signal to X-ray or thermal Sunyaev-Zeldovich observations.

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Evidence of the Missing Baryons from the Kinematic Sunyaev-Zeldovich Effect in Planck Data

Cited by 78 publications

References 24 publications

The Impact of Baryonic Physics on the Kinetic Sunyaev–Zel’dovich Effect

The Impact of Baryonic Physics on the Kinetic Sunyaev–Zel’dovich Effect

Towards the statistical detection of the warm–hot intergalactic medium in intercluster filaments of the cosmic web

Planckintermediate results

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