Small-scale fluctuations of relic radiation

Sunyaev, R.; Zel’dovich, Ya. B.

doi:10.1007/bf00653471

Cited by 1,172 publications

(899 citation statements)

References 12 publications

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“…(i) Integrated electron pressure: CMB photons are scattered by high energy electrons in the plasma inside clusters due to inverse Compton scattering. This phenomenon is knows as the thermal Sunyaev-Zeldovich (tSZ) effect and it induces a shift in the energy of the scattered CMB photons (Sunyaev & Zeldovich 1970). Such a shift is typically parameterized by the integrated Compton-y parameter (Y SZ ) and can be directly measured in SZ surveys.…”

Section: Cluster Data and Propertiesmentioning

confidence: 99%

Augmenting astrophysical scaling relations with machine learning: application to reducing the Sunyaev-Zeldovich flux-mass scatter

Wadekar¹,

Thiele²,

Villaescusa-Navarro³

et al. 2022

Preprint

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Complex systems (stars, supernovae, galaxies, and clusters) often exhibit low scatter relations between observable properties (e.g., luminosity, velocity dispersion, oscillation period, temperature). These scaling relations can illuminate the underlying physics and can provide observational tools for estimating masses and distances. Machine learning can provide a fast and systematic way to search for new scaling relations (or for simple extensions to existing relations) in abstract high-dimensional parameter spaces. We use a machine learning tool called symbolic regression (SR), which models the patterns in a given dataset in the form of analytic equations. We focus on the Sunyaev-Zeldovich flux−cluster mass relation (Y SZ − M ), the scatter in which affects inference of cosmological parameters from cluster abundance data. Using SR on the data from the IllustrisTNG hydrodynamical simulation, we find a new proxy for cluster mass which combines Y SZ and concentration of ionized gas (c gas ):SZ (1 − A c gas ). Y conc reduces the scatter in the predicted M by ∼ 20 − 30% for large clusters (M 10 14 h −1 M ) at both high and low redshifts, as compared to using just Y SZ . We show that the dependence on c gas is linked to cores of clusters exhibiting larger scatter than their outskirts. Finally, we test Y conc on clusters from simulations of the CAMELS project and show that Y conc is robust against variations in cosmology, astrophysics, subgrid physics, and cosmic variance. Our results and methodology can be useful for accurate multiwavelength cluster mass estimation from current and upcoming CMB and X-ray surveys like ACT, SO, SPT, eROSITA and CMB-S4.1. INTRODUCTION Astrophysical scaling relations are simple low-scatter relationships (generally power laws) between properties of astrophysical systems which hold over a wide range of parameter values. Some notable examples of such relations are the Phillips relation for supernovae (Phillips 1993), the Color-Magnitude Relation, the Leavitt period luminosity relation for Cepheids (Leavitt & Pickering 1912;Riess et al. 2016Riess et al. , 2019, the Tully Fisher relation (Tully & Fisher 1977) and its baryonic analogue (McGaugh et al. 2000) for spiral galaxies, the

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Section: Cluster Data and Propertiesmentioning

confidence: 99%

Augmenting astrophysical scaling relations with machine learning: application to reducing the Sunyaev-Zeldovich flux-mass scatter

Wadekar¹,

Thiele²,

Villaescusa-Navarro³

et al. 2022

Preprint

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“…The CMB photons get scattered off the hot electron gas present in the halos, which causes additional anisotropies in CMB temperature (Sunyaev & Zeldovich 1970, 1972. The temperature fluctuation due to the tSZ effect can be expressed as…”

Section: Compton Y Parametermentioning

confidence: 99%

Probing the circumgalactic medium with CMB polarization statistical anisotropy

Roy¹,

Engelen²,

Gluscevic³

et al. 2022

Preprint

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As cosmic microwave background (CMB) photons traverse the Universe, anisotropies can be induced via Thomson scattering (proportional to the integrated electron density; optical depth) and inverse Compton scattering (proportional to the integrated electron pressure; thermal Sunyaev-Zel'dovich effect). Measurements of anisotropy in optical depth τ and Compton y parameter are imprinted by the galaxies and galaxy clusters and are thus sensitive to the thermodynamic properties of circumgalactic medium and intergalactic medium. We use an analytic halo model to predict the power spectrum of the optical depth (τ τ ), the cross-correlation between the optical depth and the Compton y parameter (τ y), as well as the cross-correlation between the optical depth and galaxy clustering (τ g), and compare this model to cosmological simulations. We constrain the optical depths of halos at z 3 using a technique originally devised to constrain patchy reionization at a much higher redshift range. The forecasted signal-to-noise ratio is 2.6, 8.5, and 13, respectively, for a CMB-S4-like experiment and a VRO-like optical survey. We show that a joint analysis of these probes can constrain the amplitude of the density profiles of halos to 6.5% and the pressure profile to 13%, marginalizing over the outer slope of the pressure profile. These constraints translate to astrophysical parameters related to the physics of galaxy evolution, such as the gas mass fraction, f g , which can be constrained to 5.3% uncertainty at z ∼ 0, assuming an underlying model for the shape of the density profile. The cross-correlations presented here are complementary to other CMB and galaxy cross-correlations since they do not require spectroscopic galaxy redshifts and are another example of how such correlations are a powerful probe of the astrophysics of galaxy evolution.

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“…disentangle them observationally. 3 The non-relativistic contribution is determined by a line-of-sight integral over electron pressure, 4 y ≡ y(n) n = dn 4π…”

Section: Introductionmentioning

confidence: 99%

“…All these signals can be accurately modeled using SZpack[14] 4. We set the speed of light and Boltzmann's constant to one.…”

mentioning

confidence: 99%

Percent-level constraints on baryonic feedback with spectral distortion measurements

Thiele,

Wadekar,

Hill

et al. 2022

Preprint

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High-significance measurements of the monopole thermal Sunyaev-Zel'dovich CMB spectral distortions have the potential to tightly constrain poorly understood baryonic feedback processes. The sky-averaged Compton-y distortion and its relativistic correction are measures of the total thermal energy in electrons in the observable universe and their mean temperature.We use the CAMELS suite of hydrodynamic simulations to explore possible constraints on parameters describing the subgrid implementation of feedback from active galactic nuclei and supernovae, assuming a PIXIE-like measurement.The small 25 h −1 Mpc CAMELS boxes present challenges due to the significant cosmic variance. We utilize machine learning to construct interpolators through the noisy simulation data. Using the halo model, we translate the simulation halo mass functions into correction factors to reduce cosmic variance where required.Our results depend on the subgrid model. In the case of IllustrisTNG, we find that the bestdetermined parameter combination can be measured to 2 % and corresponds to a product of AGN and SN feedback. In the case of SIMBA, the tightest constraint is 0.2 % on a ratio between AGN and SN feedback. A second orthogonal parameter combination can be measured to 8 %. Our results demonstrate the significant constraining power a measurement of the late-time spectral distortion monopoles would have for baryonic feedback models.

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Small-scale fluctuations of relic radiation

Cited by 1,172 publications

References 12 publications

Augmenting astrophysical scaling relations with machine learning: application to reducing the Sunyaev-Zeldovich flux-mass scatter

Augmenting astrophysical scaling relations with machine learning: application to reducing the Sunyaev-Zeldovich flux-mass scatter

Probing the circumgalactic medium with CMB polarization statistical anisotropy

Percent-level constraints on baryonic feedback with spectral distortion measurements

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