Astrophysics with the Spatially and Spectrally Resolved Sunyaev-Zeldovich Effects

Mroczkowski, Tony; Nagai, Daisuke; Basu, Kaustuv; Chluba, Jens; Sayers, Jack; Adam, R.; Churazov, E.; Crites, A. T.; Mascolo, Luca Di; Eckert, D.; Macías-Pérez, J. F.; Mayet, F.; Perotto, L.; Pointecouteau, É.; Romero, C.; Ruppin, F.; Scannapieco, Evan; ZuHone, John

doi:10.1007/s11214-019-0581-2

Cited by 176 publications

(125 citation statements)

References 361 publications

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“…Estimating turbulent velocities is again important in calculating the hydrostatic mass bias of clusters (Schuecker et al 2004;George et al 2009;Bautz et al 2009;Cavaliere et al 2011;Nelson et al 2014). On these scales, pressure fluctuations obtained from Sunyaev-Zeldovich effect (SZ) observations can also be used to estimate gas velocities (Zeldovich & Sunyaev 1969;Khatri & Gaspari 2016;Mroczkowski et al 2019). Thus, a detailed study of density, pressure and velocity fluctuations in a stratified medium is important to obtain reliable scaling relations between different observables and velocities (see Simionescu et al 2019 for a review on ICM gas velocities).…”

Section: Introductionmentioning

confidence: 99%

Turbulence in stratified atmospheres: implications for the intracluster medium

Mohapatra

Federrath

Sharma

2020

Monthly Notices of the Royal Astronomical Society

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The gas motions in the intracluster medium (ICM) are governed by turbulence. However, since the ICM has a radial profile with the centre being denser than the outskirts, ICM turbulence is stratified. Stratified turbulence is fundamentally different from Kolmogorov (isotropic, homogeneous) turbulence; kinetic energy not only cascades from large to small scales, but it is also converted into buoyancy potential energy. To understand the density and velocity fluctuations in the ICM, we conduct high-resolution (1024 2 × 1536 grid points) hydrodynamical simulations of subsonic turbulence (with rms Mach number M ≈ 0.25) and different levels of stratification, quantified by the Richardson number Ri, from Ri = 0 (no stratification) to Ri = 13 (strong stratification). We quantify the density, pressure and velocity fields for varying stratification because observational studies often use surface brightness fluctuations to infer the turbulent gas velocities of the ICM. We find that the standard deviation of the logarithmic density fluctuations (σ s ), where s = ln(ρ/ ρ(z) ), increases with Ri. For weakly stratified subsonic turbulence (Ri 10, M < 1), we derive a new σ s -M-Ri relation, σ 2 s = ln 1 + b 2 M 4 + 0.09M 2 RiH P /H S , where b = 1/3-1 is the turbulence driving parameter, and H P and H S are the pressure and entropy scale heights respectively. We further find that the power spectrum of density fluctuations, P(ρ k / ρ ), increases in magnitude with increasing Ri. Its slope in k-space flattens with increasing Ri before steepening again for Ri 1. In contrast to the density spectrum, the velocity power spectrum is invariant to changes in the stratification. Thus, we find that the ratio between density and velocity power spectra strongly depends on Ri, with the total power in density and velocity fluctuations described by our σ s -M-Ri relation. Pressure fluctuations, on the other hand, are independent of stratification and only depend on M.

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Section: Introductionmentioning

confidence: 99%

Turbulence in stratified atmospheres: implications for the intracluster medium

Mohapatra

Federrath

Sharma

2020

Monthly Notices of the Royal Astronomical Society

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“…To date, X-ray and microwave measurements of the thermodynamic and metallicity profiles of the ICM have been critical towards determining the physics governing structure formation (Walker et al 2019;Mroczkowski et al 2019, for reviews), chemical enrichment of the ICM (Werner et al 2013;Urban et al 2017;Mernier et al 2018, for a review), and cosmological models (Allen et al 2011;Pratt et al 2019, for reviews). Modern cosmological simulations of galaxy cluster formation predict that the outskirts of galaxy clusters is a cosmic-melting pot, where the structure formation processes, such as mergers and gas accretion (Lau et al 2015;Zinger et al 2016), generate clumpy (Nagai & Lau 2011;Zhuravleva et al 2013;Vazza et al 2013;Rasia et al 2014) and turbulent (Lau et al 2009;Nagai et al 2013;Nelson et al 2014) hot X-ray emitting ICM in the outskirts of galaxy clusters.…”

Section: Introductionmentioning

confidence: 99%

Ultraviolet signatures of the multiphase intracluster and circumgalactic media in the romulusc simulation

Butsky

Burchett

Nagai

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Quasar absorption-line studies in the ultraviolet (UV) can uniquely probe the nature of the multiphase cool-warm (10 4 < T < 10 6 K) gas in and around galaxy clusters, promising to provide unprecedented insights into 1) interactions between the circumgalactic medium (CGM) associated with infalling galaxies and the hot (T > 10 6 K) X-ray emitting intracluster medium (ICM), 2) the stripping of metal-rich gas from the CGM, and 3) a multiphase structure of the ICM with a wide range of temperatures and metallicities. In this work, we present results from a high-resolution simulation of a ∼ 10 14 M galaxy cluster to study the physical properties and observable signatures of this cool-warm gas in galaxy clusters. We show that the ICM becomes increasingly multiphased at large radii, with the cool-warm gas becoming dominant in cluster outskirts. The diffuse cool-warm gas also exhibits a wider range of metallicity than the hot X-ray emitting gas. We make predictions for the covering fractions of key absorptionline tracers, both in the ICM and in the CGM of cluster galaxies, typically observed with the Cosmic Origins Spectrograph aboard the Hubble Space Telescope (HST). We further extract synthetic spectra to demonstrate the feasibility of detecting and characterizing the thermal, kinematic, and chemical composition of the cool-warm gas using H i, O vi, and C iv lines, and we predict an enhanced population of broad Lyα absorbers tracing the warm gas. Lastly, we discuss future prospects of probing the multiphase structure of the ICM beyond HST.

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“…Briefly, the Sunyaev-Zeldovich (SZ; Sunyaev & Zeldovich 1972) effect is a faint, extended decrement in the Cosmic Microwave Background (CMB) which has a redshift-independent surface brightness that traces the warm and hot gas in large scale structures, such as groups and clusters of galaxies (for a recent review, see Mroczkowski et al 2019b). High-resolution observations of the SZ effect have become nearly routine using ALMA and the Atacama Compact Array (ACA) in Band 3 (Basu et al 2016;Kitayama et al 2016;Ueda et al 2017;Di Mascolo et al 2019a,b;Gobat et al 2019).…”

Section: The Sunyaev-zeldovich Effectmentioning

confidence: 99%

Wideband 67−116 GHz receiver development for ALMA Band 2

Yagoubov

Mroczkowski

Belitsky

et al. 2020

A&A

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Context. The Atacama Large Millimeter/submillimeter Array (ALMA) has been in operation since 2011, but it has not yet been populated with the full suite of its planned frequency bands. In particular, ALMA Band 2 (67-90 GHz) is the final band in the original ALMA band definition to be approved for production. Aims. We aim to produce a wideband, tuneable, sideband-separating receiver with 28 GHz of instantaneous bandwidth per polarisation operating in the sky frequency range of 67-116 GHz. Our design anticipates new ALMA requirements following the recommendations of the 2030 ALMA Development Roadmap. Methods. The cryogenic cartridge is designed to be compatible with the ALMA Band 2 cartridge slot, where the coldest components -the feedhorns, orthomode transducers, and cryogenic low noise amplifiers -operate at a temperature of 15 K. We use multiple simulation methods and tools to optimise our designs for both the passive optics and the active components. The cryogenic cartridge is interfaced with a room-temperature (warm) cartridge hosting the local oscillator and the downconverter module. This warm cartridge is largely based on GaAs semiconductor technology and is optimised to match the cryogenic receiver bandwidth with the required instantaneous local oscillator frequency tuning range. Results. Our collaboration has resulted in the design, fabrication, and testing of multiple technical solutions for each of the receiver components, producing a state-of-the-art receiver covering the full ALMA Band 2 and 3 atmospheric window. The receiver is suitable for deployment on ALMA in the coming years and it is capable of dual-polarisation, sideband-separating observations in intermediate frequency bands spanning 4-18 GHz for a total of 28 GHz on-sky bandwidth per polarisation channel. Conclusions. We conclude that the 67-116 GHz wideband implementation for ALMA Band 2 is now feasible and that this receiver provides a compelling instrumental upgrade for ALMA that will enhance observational capabilities and scientific reach. 1 https://www.almaobservatory.org of construction. Recent technological developments in cryogenic monolithic microwave integrated circuits (MMICs) and optical components, such as wide bandwidth feedhorns, orthomode transducers (OMT), and lens designs -have opened up the opportunity to extend the originally-planned radio-frequency (RF) bandwidth of this receiver, to cover the 67-116 GHz frequency range on-sky with a single receiver. This holds the potential for combining ALMA Band 2 (67-90 GHz) with ALMA Band 3 (84-116 GHz), serving as an upgrade that paves the way for wider bandwidth ALMA operations. As discussed in Mroczkowski et al. 2019a, this approach offers several opera-Article number, page 1 of 23

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Astrophysics with the Spatially and Spectrally Resolved Sunyaev-Zeldovich Effects

Cited by 176 publications

References 361 publications

Turbulence in stratified atmospheres: implications for the intracluster medium

Turbulence in stratified atmospheres: implications for the intracluster medium

Ultraviolet signatures of the multiphase intracluster and circumgalactic media in the romulusc simulation

Wideband 67−116 GHz receiver development for ALMA Band 2

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