On the Non-Thermal Energy Content of Cosmic Structures

Vazza, Franco; Wittor, Denis; Brüggen, M.; Gheller, C.

doi:10.3390/galaxies4040060

Cited by 9 publications

(4 citation statements)

References 67 publications

(126 reference statements)

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“…If non-physical calibration issues are negligible, the excess of B from unity can be attributed to non-thermal pressure support in halos. The magnitude of B we found is con-sistent with that in cosmological hydrodynamical simulations and analytic predictions of structure formation where halos are additionally supported by internal bulk motions and turbulence sourced by hierarchical mass assembly (Dolag et al 2005;Iapichino & Niemeyer 2008;Vazza et al 2006Vazza et al , 2009Vazza et al , 2016Vazza et al , 2018Lau et al 2009;Maier et al 2009;Shaw et al 2010;Iapichino et al 2011;Battaglia et al 2012b;Nelson et al 2014;Shi & Komatsu 2014;Shi et al 2015Shi et al , 2016Angelinelli et al 2020). This implies that additional kinetic energy injections from baryonic feedback, mostly from active galactic nucleus activities, are either small (because, e.g., they are confined in the small volume of galaxy cluster cores) or largely thermalized.…”

Section: Interpreting the Mass Biassupporting

confidence: 84%

The Cosmic Thermal History Probed by Sunyaev-Zeldovich Effect Tomography

Chiang,

Makiya,

Ménard

et al. 2020

Preprint

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The cosmic thermal history, quantified by the evolution of the mean thermal energy density in the universe, is driven by the growth of structures as baryons get shock-heated in collapsing dark matter halos. This process can be probed by redshift-dependent amplitudes of the thermal Sunyaev-Zeldovich (SZ) effect background. To do so, we cross-correlate eight sky intensity maps in the Planck and Infrared Astronomical Satellite missions with two million spectroscopic-redshift references in the Sloan Digital Sky Surveys. This delivers snapshot spectra for the far-infrared to microwave background light as a function of redshift up to z ∼ 3. We decompose them into the SZ and thermal dust components. Our SZ measurements directly constrain 〈bP e 〉, the halo bias-weighted mean electron pressure, up to z ∼ 1. This is the highest redshift achieved to date, with uncorrelated redshift bins thanks to the spectroscopic references. We detect a threefold increase in the density-weighted mean electron temperature T e from 7 × 10 5 K at z = 1 to 2 × 10 6 K today. Over z = 1-0, we witness the build up of nearly 70% of the present-day mean thermal energy density ρ th , with the corresponding density parameter Ω th reaching 1.5 × 10 −8 . We find the mass bias parameter of Planck's universal pressure profile of B = 1.27 (or 1 − b = 1/B = 0.79), consistent with the magnitude of nonthermal pressure in gas motion and turbulence from mass assembly. We estimate the redshift-integrated mean Compton parameter y ∼ 1.2 × 10 −6 , which will be tested by future spectral distortion experiments. More than half of which originates from large-scale structure at z < 1, which we detect directly.

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Section: Interpreting the Mass Biassupporting

confidence: 84%

The Cosmic Thermal History Probed by Sunyaev-Zeldovich Effect Tomography

Chiang,

Makiya,

Ménard

et al. 2020

Preprint

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“…At the same time, the techniques used to analyse the simulations and compare them to observational data, including mock images, have further enhanced their predictive power. Still, the level of the above mass bias for simulated clusters considered 'dynamically relaxed' has always been consistently found to be around 10-20 percent (Rasia et al 2006;Nagai et al 2007a;Jeltema et al 2008;Piffaretti & Valdarnini 2008;Lau et al 2009;Meneghetti et al 2010;Nelson et al 2012;Battaglia et al 2012;Rasia et al 2012;Shi et al 2015;Biffi et al 2016;Vazza et al 2016;Henson et al 2017; Barnes et al 2017a;Vazza et al 2018;Cialone et al 2018;Angelinelli et al 2019). Thanks to simulations, we understand that the main sources of the HE bias are the residual, non-thermalized gas velocity, in the form of both bulk motion and turbulence, and intra-cluster medium (ICM) inhomogeneities.…”

Section: Introductionmentioning

confidence: 96%

The Three Hundred Project: Correcting for the hydrostatic-equilibrium mass bias in X-ray and SZ surveys

Ansarifard

Rasia

Biffi

et al. 2020

A&A

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Accurate and precise measurements of masses of galaxy clusters are key to derive robust constraints on cosmological parameters. Rising evidence from observations, however, confirms that X-ray masses, obtained under the assumption of hydrostatic equilibrium, might be underestimated, as previously predicted by cosmological simulations. We analyse more than 300 simulated massive clusters, from 'The Three Hundred Project', and investigate the connection between mass bias and several diagnostics extracted from synthetic X-ray images of these simulated clusters. We find that the azimuthal scatter measured in 12 sectors of the X-ray flux maps is a statistically significant indication of the presence of an intrinsic (i.e. 3D) clumpy gas distribution. We verify that a robust correction to the hydrostatic mass bias can be inferred when estimates of the gas inhomogeneity from X-ray maps (such as the azimuthal scatter or the gas ellipticity) are combined with the asymptotic external slope of the gas density or pressure profiles, which can be respectively derived from X-ray and millimetric (Sunyaev-Zeldovich effect) observations. We also obtain that mass measurements based on either gas density and temperature or gas density and pressure result in similar distributions of the mass bias. In both cases, we provide corrections that help reduce both the dispersion and skewness of the mass bias distribution. These are effective even when irregular clusters are included leading to interesting implications for the modelling and correction of hydrostatic mass bias in cosmological analyses of current and future X-ray and SZ cluster surveys.

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“…Now, what accounts for this? A promising candidate for non-thermal pressure quantified by Ω non−th is the bulk and turbulent motion of gas sourced by mass accretion and structure formation (Dolag et al 2005;Iapichino & Niemeyer 2008;Vazza et al 2006Vazza et al , 2009Vazza et al , 2016Vazza et al , 2018Lau et al 2009;Maier et al 2009;Shaw et al 2010;Iapichino et al 2011;Battaglia et al 2012;Nelson et al 2014a;Shi & Komatsu 2014;Shi et al 2015;Angelinelli et al 2020). An analytical model (Shi & Komatsu 2014) validated by cosmological hydrodynamical simulations (Shi et al 2015) suggests the following picture: the non-thermal energy is sourced by the mass growth of halos via mergers and accretion, and dissipates with a time-scale determined by the turnover time of the largest turbulence eddies.…”

Section: Discussionmentioning

confidence: 99%

The thermal and gravitational energy densities in the large-scale structure of the Universe

Chiang,

Makiya,

Komatsu

et al. 2020

Preprint

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As cosmic structures form, matter density fluctuations collapse gravitationally and baryonic matter is shock-heated and thermalized. We therefore expect a connection between the mean gravitational potential energy density of collapsed halos, Ω halo W , and the mean thermal energy density of baryons, Ω th . These quantities can be obtained using two fundamentally different estimates: we compute Ω halo W using the theoretical framework of the halo model which is driven by dark matter statistics, and measure Ω th using the Sunyaev-Zeldovich (SZ) effect which probes the mean thermal pressure of baryons. First, we derive that, at the present time, about 90% of Ω halo W originates from massive halos with M > 10 13 M . Then, using our measurements of the SZ background, we find that Ω th accounts for about 80% of the kinetic energy of the baryons available for pressure in halos at z 0.5. This constrains the amount of non-thermal pressure, e.g., due to bulk and turbulent gas motion sourced by mass accretion, to be about Ω non−th 0.4 × 10 −8 at z = 0.

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On the Non-Thermal Energy Content of Cosmic Structures

Cited by 9 publications

References 67 publications

The Cosmic Thermal History Probed by Sunyaev-Zeldovich Effect Tomography

The Cosmic Thermal History Probed by Sunyaev-Zeldovich Effect Tomography

The Three Hundred Project: Correcting for the hydrostatic-equilibrium mass bias in X-ray and SZ surveys

The thermal and gravitational energy densities in the large-scale structure of the Universe

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