A multisimulation study of relativistic SZ temperature scalings in galaxy clusters and groups

Lee, Elizabeth; Anbajagane, Dhayaa; Singh, Priyanka; Chluba, Jens; Nagai, Daisuke; Kay, Scott T.; Cui, Weiguang; Dolag, K.; Yepes, Gustavo

doi:10.1093/mnras/stac2781

Cited by 19 publications

(4 citation statements)

References 130 publications

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“…They found that the spectroscopic temperature derived from MOCK-X in a more massive sample (𝑀 500 > 10 13 M , 𝑇 X,spec > 0.5 keV where spectroscopic template fitting is reliable) is systematically underestimated by a factor ∼ 2, which is consistent with the ∼ 0.3 dex underestimation seen in our sample at the high-𝑇 sl end. The spectroscopic-like temperature definition further enhances the underestimation due to the 𝑇 −3/4 weighting, and that underestimation is actually a bit stronger in IllustrisTNG compared to other cosmological hydrodynamic simulations (see Figure A5 in Lee et al 2022).…”

Section: X-ray Scaling Relations Of the Simulated Etgsmentioning

confidence: 89%

X-ray scaling relations of early-type galaxies in IllustrisTNG and a new way of identifying backsplash objects

Wang¹,

Vogelsberger²,

Kim³

et al. 2023

Preprint

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We investigate how feedback and environment shapes the X-ray scaling relations of early-type galaxies (ETGs), especially at the low-mass end. We select central-ETGs from the IllustrisTNG-100 box that have stellar masses log 10 (𝑀 * /M ) ∈ [10.7, 11.9]. We derive mock X-ray luminosity (𝐿 X,500 ) and spectroscopic-like temperature (𝑇 sl,500 ) of hot gas within 𝑅 500 of the ETG haloes using the MOCK-X pipeline. The scaling between 𝐿 X,500 and the total mass within 5 effective radii (𝑀 5𝑅 e ) agrees well with observed ETGs from Chandra. IllustrisTNG reproduces the observed increase in scatter of 𝐿 X,500 towards lower masses, and we find that ETGs with log 10 (𝑀 5𝑅 e /M ) 11.5 with above-average 𝐿 X,500 experienced systematically lower cumulative kinetic AGN feedback energy historically (vice versa for below-average ETGs). This leads to larger gas mass fractions and younger stellar populations with stronger stellar feedback heating, concertedly resulting in the above-average 𝐿 X,500 . The 𝐿 X,500 -𝑇 sl,500 relation shows a similar slope to the observed ETGs but the simulation systematically underestimates the gas temperature. Three outliers that lie far below the 𝐿 X -𝑇 sl relation all interacted with larger galaxy clusters recently and demonstrate clear features of environmental heating. We propose that the distinct location of these backsplash ETGs in the 𝐿 X -𝑇 sl plane could provide a new way of identifying backsplash galaxies in future X-ray surveys.

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Section: X-ray Scaling Relations Of the Simulated Etgsmentioning

confidence: 89%

X-ray scaling relations of early-type galaxies in IllustrisTNG and a new way of identifying backsplash objects

Wang¹,

Vogelsberger²,

Kim³

et al. 2023

Preprint

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show abstract

“…Given the range of possible, allowed assumptions, the simulations manifest a variety of halo property behaviors. Comparative studies show the predictions agree in the overall trends but differ in specific details [e.g., 113,[115][116][117][118][119][120]. Studies on the thermodynamic properties of gas also find differences between the measurements from data and the predictions from these hydrodynamic simulations [e.g., [121][122][123][124][125].…”

Section: Jcap03(2024)062mentioning

confidence: 99%

Primordial non-Gaussianities with weak lensing: information on non-linear scales in the Ulagam full-sky simulations

Anbajagane,

Chang,

Lee

et al. 2024

J. Cosmol. Astropart. Phys.

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Primordial non-Gaussianities (PNGs) are signatures in the density field that encode particle physics processes from the inflationary epoch. Such signatures have been extensively studied using the Cosmic Microwave Background, through constraining their amplitudes, fX NL, with future improvements expected from large-scale structure surveys; specifically, the galaxy correlation functions. We show that weak lensing fields can be used to achieve competitive and complementary constraints. This is shown via the Ulagam suite of N-body simulations, a subset of which evolves primordial fields with four types of PNGs. We create full-sky lensing maps and estimate the Fisher information from three summary statistics measured on the maps: the moments, the cumulative distribution function, and the 3-point correlation function. We find that the year 10 sample from the Rubin Observatory Legacy Survey of Space and Time (LSST) can constrain PNGs to σ(f NL eq) ≈ 110, σ(f NL or, lss) ≈ 120, σ(f NL loc) ≈ 40. For the former two, this is better than or comparable to expected galaxy clustering-based constraints from the Dark Energy Spectroscopic Instrument (DESI). The PNG information in lensing fields is on non-linear scales and at low redshifts (z ≲ 1.25), with a clear origin in the evolution history of massive halos. The constraining power degrades by ∼60% under scale cuts of ≳ 20 Mpc, showing there is still significant information on scales mostly insensitive to small-scale systematic effects (e.g., baryons). We publicly release the Ulagam suite to enable more survey-focused analyses.

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“…Furthermore, observations of the SZ effect can constrain astrophysical processes occurring in galaxy groups and clusters and their thermodynamic properties (Battaglia et al 2017;Mroczkowski et al 2019;Schaan et al 2021;Moser et al 2022;Hadzhiyska et al 2023a, for review). Similarly, observed X-ray emission and spectra from galaxy groups and clusters can aid in constraining the complex feedback and formation processes in the multiphase intracluster medium (ICM) and Intragroup Medium (IGrM; Singh et al 2018;McCabe et al 2021;Lee et al 2022;Singh et al 2022;Lovisari et al 2024).…”

Section: Introductionmentioning

confidence: 99%

Zooming by in the CARPoolGP Lane: New CAMELS-TNG Simulations of Zoomed-in Massive Halos

Lee,

Genel,

Wandelt

et al. 2024

ApJ

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Galaxy formation models within cosmological hydrodynamical simulations contain numerous parameters with nontrivial influences over the resulting properties of simulated cosmic structures and galaxy populations. It is computationally challenging to sample these high dimensional parameter spaces with simulations, in particular for halos in the high-mass end of the mass function. In this work, we develop a novel sampling and reduced variance regression method, CARPoolGP, which leverages built-in correlations between samples in different locations of high dimensional parameter spaces to provide an efficient way to explore parameter space and generate low-variance emulations of summary statistics. We use this method to extend the Cosmology and Astrophysics with machinE Learning Simulations to include a set of 768 zoom-in simulations of halos in the mass range of 1013–1014.5 M ⊙ h −1 that span a 28-dimensional parameter space in the IllustrisTNG model. With these simulations and the CARPoolGP emulation method, we explore parameter trends in the Compton Y–M, black hole mass–halo mass, and metallicity–mass relations, as well as thermodynamic profiles and quenched fractions of satellite galaxies. We use these emulations to provide a physical picture of the complex interplay between supernova and active galactic nuclei feedback. We then use emulations of the Y–M relation of massive halos to perform Fisher forecasts on astrophysical parameters for future Sunyaev–Zeldovich observations and find a significant improvement in forecasted constraints. We publicly release both the simulation suite and CARPoolGP software package.

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A multisimulation study of relativistic SZ temperature scalings in galaxy clusters and groups

Cited by 19 publications

References 130 publications

X-ray scaling relations of early-type galaxies in IllustrisTNG and a new way of identifying backsplash objects

X-ray scaling relations of early-type galaxies in IllustrisTNG and a new way of identifying backsplash objects

Primordial non-Gaussianities with weak lensing: information on non-linear scales in the Ulagam full-sky simulations

Zooming by in the CARPoolGP Lane: New CAMELS-TNG Simulations of Zoomed-in Massive Halos

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