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The paper claims that the higher-order angular moments of oriented thermal Sunyaev-Zel'dovich stacks around supercluster halos respond to cosmological parameters almost as strongly as the isotropic signal but much less to gas-pressure varia

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2026-08-04 10:45 UTC pith:MUWT6DE6

load-bearing objection Higher multipoles of oriented tSZ stacks are a promising cosmological handle, but the degeneracy-breaking claim is demonstrated only for isotropic gas models. the 3 major comments →

arxiv 2510.08331 v2 pith:MUWT6DE6 submitted 2025-10-09 astro-ph.CO

The superclustering of hot gas: cosmological sensitivity in the Websky simulations

M. Lokken , J. R. Bond , R. Hlo\v{z}ek , N. J. Carlson , Z. Li , A. van Engelen This is my paper
classification astro-ph.CO
keywords thermal Sunyaev-Zel'dovich effectoriented stackingsuperclusterscosmic webCompton-y mapscosmological parameter sensitivitygas feedback degeneracyWebsky simulations
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper asks whether directional, environmentally-selected stacks of the hot-gas signal in cosmic superclusters can serve as a cosmological probe rather than just a gas-physics probe. It runs nine fast simulations with different matter densities and two matter–dark-energy trajectories, plus six gas-pressure models, and finds that cosmology shifts all multipole moments of the oriented stacks similarly, while gas-model variations mostly shift only the monopole. The conclusion is that the higher multipoles carry cosmologically sensitive information that is relatively robust to gas uncertainties, so combining moments can disentangle cosmology from feedback. This matters because standard SZ-galaxy cross-correlations are directionless and heavily degenerate with gas physics, while the oriented higher moments are also observationally cleaner, since they are insensitive to the mean y-signal and to isotropic contamination.

Core claim

The central claim is that oriented stacking of the thermal Sunyaev-Zel'dovich signal in supercluster regions adds genuinely new cosmological information beyond unoriented stacking, and that this information can be isolated from gas physics. In simulations with Omega_M varied from 0.22 to 0.42 and sigma_8 fixed at z=0.5, the first five cosine multipoles of the stacked y-images all respond to cosmology in a similar amplitude-scaling way, while the pressure-profile variations—BBPS profile extent and a broken-power-law AGN-feedback model—affect m=0 much more than m>0. Because the higher-order moments retain cosmological sensitivity but are less affected by gas modeling, the paper concludes that

What carries the argument

The central statistic is the constrained oriented stack: cutouts of a Compton-y map are centered on massive halos (M > 5e13 solar masses) that lie in overdense, elongated regions of a smoothed halo-density map, then rotated so the local filament axis is horizontal, gradient-flipped, and averaged. The signal is decomposed into cosine and sine multipole moments C_m(r) and S_m(r), and the summary measure is integrated multipole power P_m = integral of (C_m^2 + S_m^2) r dr. The key comparison is the ratio A_m(r) = C_m/C_0, which the paper finds to be largely cosmology-independent, so the shape of the multipole spectrum—rather than its overall amplitude—carries the gas-robust cosmological signal.

Load-bearing premise

The results assume that isotropic halo-pasted pressure profiles, with a plausible range of amplitude variations, bracket the real range of gas physics for every multipole—including anisotropic feedback correlated with large-scale structure—an assumption the authors explicitly flag as uncertain.

What would settle it

Run two hydrodynamical simulations with identical cosmology but different feedback models, one with AGN jets preferentially aligned with filaments and one with isotropic thermal feedback, and apply the same oriented stacking; if the m=2/m=0 power ratio changes by as much as the change between adjacent Omega_M runs, the proposed degeneracy breaking would not survive in real data.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Combining m=0 with higher moments should yield cosmological constraints that are far less sensitive to AGN feedback modeling than monopole-only stacks.
  • The m>0 moments can be measured in the far-field regime without the need to subtract the true mean y-signal, avoiding a major systematic that hampers isotropic stacking.
  • Oriented stacks can distinguish cosmologies that differ mainly in the matter-lambda-H0 plane, which are nearly identical in the one-halo regime of unoriented stacks.
  • Environmental constraints raise the per-halo signal and cosmological sensitivity but shrink the sample; the trade-off leaves net sensitivity roughly unchanged while reducing computational cost.
  • Wider sky overlap between CMB and galaxy surveys will increase stack sample sizes and make the demonstrated cosmological sensitivity observationally accessible.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The paper's own A_m(r) analysis suggests a potential shape-only statistic, e.g., ratios of higher-moment power to monopole power, that could separate cosmology from gas parameters without needing to model feedback amplitude at all—an extension the authors do not explicitly build.
  • A stronger test than the isotropic halo-pasting used here would be hydrodynamical simulations with AGN jets aligned or anti-aligned with filaments; if those alter m>0 moments in a cosmology-dependent way, the degeneracy breaking could weaken in real data.
  • The same oriented-multipole machinery could plausibly be applied to other tracers of the cosmic web—kinematic SZ, weak lensing, or galaxy density—where the moment spectrum may similarly isolate cosmology from astrophysical nuisance parameters.
  • The Cosmo2 suite effectively isolates geometry and growth effects from matter-density amplitude, so a future cosmological inference using these moments could target the matter–dark-energy balance and H0 rather than just Omega_M.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper investigates whether multipole moments of constrained, oriented stacks of the thermal Sunyaev-Zel'dovich effect around massive halos are sensitive to cosmological and gas-physics parameters. It uses the Websky/Peak Patch algorithm to build nine 2.4 Gpc lightcone simulations: a fiducial Planck cosmology; four Cosmo1 runs varying Omega_M with H0 and Omega_b fixed; and four Cosmo2 runs varying Omega_M and H0 with Omega_M h^2 and Omega_b h^2 fixed. sigma8(z=0.5) is renormalized across runs. Oriented stacks are constructed for halos M>5e13 Msun in supercluster environments (nu>2, e>0.3) at z~0.5, and cosine/sine multipoles C_m(r), integrated power P_m, and normalized shapes A_m(r)=C_m/C_0 are compared. Six gas variations are applied to the fiducial cosmology: BBPS pressure-profile cutoff radii 2R200, 4R200, 6R200 and break-model variations with different M_br and alpha_br. The main claim is that gas variations affect m=0 more than m>0, while cosmology variations affect all moments similarly; hence higher-order moments can help break the gas-cosmology degeneracy. The paper is explicitly a proof-of-concept and does not attempt parameter inference or a full experimental forecast.

Significance. If the degeneracy-breaking claim survives further testing, the paper makes a useful case for adding directional statistics to SZ cross-correlation analyses. The analysis is transparent: it uses the public Websky framework, carefully isolates cosmology from the sigma8 amplitude, compares oriented to unoriented stacks with a noise floor from random orientations, and explicitly enumerates its limitations. The conclusion that higher multipoles carry additional cosmological information beyond the monopole is supported by the noiseless simulation comparisons. However, the central mechanism for breaking the gas-cosmology degeneracy rests on the assumption that gas variations relevant to m>0 are captured by isotropic, halo-pasted profile rescalings. This assumption is untested, and the paper itself states that coherent anisotropic feedback is not modeled. The significance is therefore conditional: the paper motivates, but does not yet establish, the degeneracy-breaking power of higher moments.

major comments (3)
  1. [Section 5 / 5.4] The main claim that higher-order moments can break the gas-cosmology degeneracy is only tested against isotropic halo-pasted gas variations. Section 5 explicitly states 'we do not model asymmetric halo profiles nor the inter-halo gas' and that 'feedback processes that act in a coherent, anisotropic way with respect to the large-scale structure... cannot be captured by our modeling.' Since the m>0 multipoles are specifically directional, rescaling an isotropic profile changes only the amplitude of an already-oriented halo field; it cannot generate or suppress gas anisotropy that is coherently aligned with the large-scale structure. If AGN jets or anisotropic shock heating deposit extra pressure along filament axes, that signal projects into m=2 and m=4 in a way that may track the same orientation field as the cosmological signal, restoring the degeneracy. Section 5.4 concedes that the gas
  2. [Section 4.1] The error budget relies on a single realization per cosmology, with covariance estimated from 40 spatially clustered sub-samples of the same realization. The text says 'we do not run multiple realizations' and that the sub-samples are 'mostly (but not completely) independent' because they are clustered on the sky. Clustered sub-samples of one realization do not provide independent samples of the large-scale modes that dominate the two-halo regime, so the 1-sigma bands in Figures 4 and 6 and the statement that A_m(r) is 'consistent across most of the simulations within 2-sigma' are not a reliable substitute for realization-level variance. This limits the strength of the 'cosmology affects all moments similarly' claim. The paper is appropriately hedged as a proof-of-concept, but the covariance treatment should be stated as an approximation and, ideally, supplemented by at least one indepen
  3. [Section 2.5, 5.1, and 4] The cosmological sensitivity is not independent of the gas prescription. The BBPS model enters through rho_cr(z) and f_b (Eq. 5.1), and in Cosmo1 f_b varies with Omega_M by construction. The paper itself notes in Section 2.3 that at fixed mass lower-Omega_M runs have higher pressure because f_b is larger. Thus the observed 'cosmology variations affect all moments similarly' includes the response of the assumed pressure model to cosmology, not just the response of the halo distribution. Section 2.5 admits it is 'not entirely clear whether the prescriptions used in this work can be accurately used to create y maps for such broad cosmological parameter variations.' This should be treated as a systematic uncertainty in the interpretation of Figures 4, 5, and 10, not merely as a numerical caveat. A useful check would be to repeat one or two cosmology variations with a cosmology-independent pr
minor comments (4)
  1. [References / Sec. 5.2] The text attributes the break-model constraints to '[85] (hereafter P22)', but reference [85] is the DES Y3 galaxy clustering/weak lensing paper; the ACT+Planck tSZ cross-correlation paper that tests the break model appears to be [87]. Please correct the citation.
  2. [Figure 4] The upper axis 'r [Mpc]' is computed for the fiducial cosmology only, but in Cosmo2 the distance-redshift relation varies significantly across runs (Table 1). The text notes this for the images but not for the multipole profiles; a reader may misinterpret the Mpc scale as common to all curves. State explicitly that the Mpc conversion differs per cosmology.
  3. [Section 4.4] Equation (4.6) is a rough sensitivity heuristic, but the denominator uses 1/N and 1/N' as if the noise in integrated power scales as 1/N with no covariance between radial bins. Since the covariance is already estimated from sub-samples, a more direct comparison would use that covariance. As written, the 0.8-1.2x sensitivity ratios in Section 4.4 should be interpreted as indicative only.
  4. [Section 5.3] The 'Span of gas variations' shaded band in Figures 9 and 10 is defined by the minimum and maximum of the explored models rather than by a statistical confidence interval. The caption in Figure 9 correctly calls it a rough estimate, but the text at the end of Section 5.3 says 'this constitutes a rough estimate of the range within which ~68% of gas model trajectories would fall'; the 68% wording is not justified by the two-model family explored.

Circularity Check

0 steps flagged

No significant circularity: the multipole sensitivity result is an output of new simulations, not an input.

full rationale

The paper's derivation chain is not circular. The central result—that higher-order cosine moments of constrained oriented tSZ stacks respond similarly to cosmological variations but less strongly to the adopted gas-pressure variations—is a measured output of mock maps generated from new Websky realizations. The inputs are set independently: the cosmological trajectories (Omega_M, Omega_Lambda, H0, As with sigma8 fixed at z=0.5) and the gas prescriptions (BBPS profile, radius cuts, and P22-motivated break-model parameters) are external calibration choices, not functions of the multipole moments C_m(r) or integrated powers P_m. The BBPS profile and oriented-stacking technique are cited from prior work that includes some of the same authors, but those citations supply the method and fiducial model, not the conclusion; no equation defines the moments in terms of the gas-model parameters in a way that forces the reported ordering. The paper explicitly acknowledges in Sections 5 and 6 that it only explores isotropic halo-pasted gas variations and that anisotropic feedback correlated with large-scale structure could change the higher-order moments; this is a physical scope limitation, not a circular reduction of the conclusion to an input.

Axiom & Free-Parameter Ledger

5 free parameters · 6 axioms · 0 invented entities

The central claim rests on several hand-chosen simulation and analysis parameters (sigma8 normalization, environmental cuts, smoothing scale, BBPS parameters, break-model parameters) and on the domain assumption that Websky halo-pasting remains valid across broad cosmology and gas variations. The paper is transparent about most of these, but none are independently validated in this work.

free parameters (5)
  • sigma8(z*=0.5) normalization = 0.62
    Hand-chosen fixed amplitude at z=0.5; Eq. 2.1 rescales As for each cosmology. The suite is designed around this choice, so all sensitivity results are conditional on it.
  • environmental thresholds (nu, e) = nu>2, e>0.3
    Sub-selection of stacking halos in supercluster regions (Sec 3). The signal amplitude and sensitivity change with these thresholds, which are taken from prior work and not varied here.
  • orientation smoothing scale = 35 arcmin FWHM
    Gaussian smoothing of the halo density map sets the peak radius of m>0 moments (Sec 3/4.1); fixed across all runs.
  • BBPS gas pressure parameters = P0, xc, beta, alpha_m, alpha_z from Table 1 of Battaglia et al. 2012
    Fiducial gas model pasted onto halos in every cosmology run; calibrated externally to hydrodynamic simulations, not re-fit here.
  • break-model parameters = alpha_br^m = 0.398, 0.972, 1.718; M_br = 5e13 and 2e14 h^-1 M_sun
    Gas variation range from Pandey et al. 2022 constraints; defines the shaded span of gas variations used to argue higher-order moments break degeneracy.
axioms (6)
  • domain assumption Websky mass-Peak Patch (2LPT + ellipsoidal collapse + exclusion) is accurate enough on quasi-linear scales for this analysis
    Invoked throughout; validated against N-body only in prior work, not revalidated for these cosmology variations.
  • domain assumption BBPS pressure profiles calibrated around 1e14-1.7e14 M_sun can be extrapolated to 1e13 M_sun and 4R200, and remain valid across broad Omega_M and H0 variations
    Section 2.5 admits this is 'not entirely clear'; it is load-bearing for the cosmology sensitivity comparison.
  • domain assumption Fixing sigma8 at z=0.5 removes the dominant tSZ amplitude dependence and isolates the effects of Omega_M and Omega_Lambda on superclustering
    Section 2.2 design; the known tSZ power dependence on sigma8 motivates this, but residual mass-function and pressure-profile effects remain.
  • domain assumption Isotropic halo-pasted gas models span the realistic range of stacked multipole responses to feedback
    Section 5 and Conclusions caveat that AGN jets aligned with filaments or anisotropic shock heating are not modeled; if anisotropic feedback couples to m>0, the degeneracy-breaking claim weakens.
  • domain assumption Cosmic variance can be approximated by 40 spatial sub-samples of one realization
    Section 4.1; sub-samples are not fully independent and there is only one seed/realization per cosmology.
  • domain assumption Flat LCDM with two massless and one massive neutrino (m_nu=0.06 eV) is the background model
    Section 2.1; all variations stay in this model class.

pith-pipeline@v1.3.0-alltime-deepseek · 27671 in / 14907 out tokens · 122558 ms · 2026-08-04T10:45:59.940707+00:00 · methodology

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Combinations of galaxy surveys and cosmic microwave background secondaries, such as the thermal Sunyaev-Zel'dovich (tSZ) effect, are increasingly being used to jointly constrain cosmology and astrophysical properties of the gas within and beyond halos. Standard cross-correlations measure a directionless correlation between the microwave maps and galaxy catalogs. However, more information about the cosmic web structure can be captured by summary statistics which include environmental constraints and measure oriented correlations along axes of structure, such as filaments or superclusters. This work studies the sensitivity of multipole moments of constrained oriented stacks, a directional and environmentally-dependent statistic, to variations in cosmological and astrophysical parameters. We run nine different 2.4 Gpc-per-side simulations with the Websky algorithm, varying the matter density within flat $\Lambda$CDM, and create mock tSZ maps with each. We also apply six different gas prescriptions, imitating AGN feedback variations, to the fiducial cosmology. We analyze oriented stacks of the tSZ signal in supercluster regions in each simulation, focusing on signal out to $\sim20$ transverse Mpc from massive ($M>5\times10^{13}~M_\odot$) halos. The cosmology variations affect anisotropic and isotropic measurements similarly, while the halo-pasted gas variations mostly affect the isotropic signal. Our results suggest it is worthwhile to incorporate directional information into SZ-galaxy cross-correlations to increase cosmological sensitivity and help break degeneracies with gas physics.

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Reference graph

Works this paper leans on

89 extracted references · 79 linked inside Pith

  1. [1]

    van de Weygaert and J.R

    R. van de Weygaert and J.R. Bond,Clusters and the Theory of the Cosmic Web, inA Pan-Chromatic View of Clusters of Galaxies and the Large-Scale Structure, M. Plionis, O. L´ opez-Cruz and D. Hughes, eds., vol. 740, p. 335, Dordrecht: Springer (2008), DOI. – 25 –

    2008

  2. [2]

    Cen,The Local Supercluster as a Test of Cosmological Models, ApJ424(1994) 22

    R. Cen,The Local Supercluster as a Test of Cosmological Models, ApJ424(1994) 22

    1994

  3. [3]

    Frisch, J

    P. Frisch, J. Einasto, M. Einasto, W. Freudling, K.J. Fricke, M. Gramann et al.,Evolution of the supercluster-void network., A&A296(1995) 611 [astro-ph/9503037]

    Pith/arXiv arXiv 1995

  4. [4]

    Basilakos, M

    S. Basilakos, M. Plionis and M. Rowan-Robinson,PSCz superclusters: detection, shapes and cosmological implications, MNRAS323(2001) 47 [astro-ph/0007155]

    Pith/arXiv arXiv 2001

  5. [5]

    Kolokotronis, S

    V. Kolokotronis, S. Basilakos and M. Plionis,Supercluster properties as a cosmological probe, MNRAS331(2002) 1020 [astro-ph/0111044]

    Pith/arXiv arXiv 2002

  6. [6]

    Bharadwaj and B

    S. Bharadwaj and B. Pandey,Using the Filaments in the Las Campanas Redshift Survey to Test theΛCDM Model, ApJ615(2004) 1 [astro-ph/0405059]

    Pith/arXiv arXiv 2004

  7. [7]

    Hopkins, N.A

    P.F. Hopkins, N.A. Bahcall and P. Bode,Cluster Alignments and Ellipticities inΛCDM Cosmology, ApJ618(2005) 1 [astro-ph/0409652]

    Pith/arXiv arXiv 2005

  8. [8]

    Bagchi, S

    J. Bagchi, S. Sankhyayan, P. Sarkar, S. Raychaudhury, J. Jacob and P. Dabhade,Saraswati: An Extremely Massive∼200 Megaparsec Scale Supercluster, ApJ844(2017) 25 [1707.03082]

    Pith/arXiv arXiv 2017

  9. [9]

    A. Ho, M. Gronke, B. Falck and D.F. Mota,Probing modified gravity in cosmic filaments, A&A 619(2018) A122 [1807.07287]

    Pith/arXiv arXiv 2018

  10. [10]

    Z. Xu, S. Adachi, P. Ade, J.A. Beall, T. Bhandarkar, J.R. Bond et al.,The Simons Observatory: The Large Aperture Telescope (LAT),Research Notes of the American Astronomical Society5(2021) 100 [2104.09511]

    Pith/arXiv arXiv 2021

  11. [11]

    Aghamousa, J

    DESI Collaboration, A. Aghamousa, J. Aguilar, S. Ahlen, S. Alam, L.E. Allen et al.,The DESI Experiment Part I: Science,Targeting, and Survey Design,arXiv e-prints(2016) arXiv:1611.00036 [1611.00036]

    Pith/arXiv arXiv 2016

  12. [12]

    Ivezi´ c, S.M

    ˇZ. Ivezi´ c, S.M. Kahn, J.A. Tyson, B. Abel, E. Acosta, R. Allsman et al.,LSST: From Science Drivers to Reference Design and Anticipated Data Products, ApJ873(2019) 111 [0805.2366]

    Pith/arXiv arXiv 2019

  13. [13]

    Melnyk, A.A

    O.V. Melnyk, A.A. Elyiv and I.B. Vavilova,The structure of the Local Supercluster of galaxies detected by three-dimensional Voronoi’s tessellation method,Kinematika i Fizika Nebesnykh Tel 22(2006) 283 [0712.1297]

    Pith/arXiv arXiv 2006

  14. [14]

    Forero-Romero, Y

    J.E. Forero-Romero, Y. Hoffman, S. Gottl¨ ober, A. Klypin and G. Yepes,A dynamical classification of the cosmic web, MNRAS396(2009) 1815 [0809.4135]

    Pith/arXiv arXiv 2009

  15. [15]

    Sousbie,DisPerSE: robust structure identification in 2D and 3D,arXiv e-prints(2013) arXiv:1302.6221 [1302.6221]

    T. Sousbie,DisPerSE: robust structure identification in 2D and 3D,arXiv e-prints(2013) arXiv:1302.6221 [1302.6221]

    Pith/arXiv arXiv 2013

  16. [16]

    G. Chon, H. B¨ ohringer and N. Nowak,The extended ROSAT-ESO Flux-Limited X-ray Galaxy Cluster Survey (REFLEX II) - III. Construction of the first flux-limited supercluster sample, MNRAS429(2013) 3272 [1212.1597]

    Pith/arXiv arXiv 2013

  17. [17]

    Tully, H

    R.B. Tully, H. Courtois, Y. Hoffman and D. Pomar` ede,The Laniakea supercluster of galaxies, Nature513(2014) 71 [1409.0880]

    Pith/arXiv arXiv 2014

  18. [18]

    Chow-Mart ´ ınez, H

    M. Chow-Mart ´ ınez, H. Andernach, C.A. Caretta and J.J. Trejo-Alonso,Two new catalogues of superclusters of Abell/ACO galaxy clusters out to redshift 0.15, MNRAS445(2014) 4073 [1409.5152]

    Pith/arXiv arXiv 2014

  19. [19]

    Kraljic, C

    K. Kraljic, C. Pichon, Y. Dubois, S. Codis, C. Cadiou, J. Devriendt et al.,Galaxies flowing in the oriented saddle frame of the cosmic web, MNRAS483(2019) 3227 [1810.05211]

    Pith/arXiv arXiv 2019

  20. [20]

    Pe˜ naranda-Rivera, D.L

    J.D. Pe˜ naranda-Rivera, D.L. Paipa-Le´ on, S.D. Hern´ andez-Charpak and J.E. Forero-Romero, Superclusters from velocity divergence fields,arXiv e-prints(2020) arXiv:2010.05160 [2010.05160]

    Pith/arXiv arXiv 2020

  21. [21]

    Read and N

    J. Read and N. Trentham,The baryonic mass function of galaxies,Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences363(2005) 2693 [https://royalsocietypublishing.org/doi/pdf/10.1098/rsta.2005.1648]. – 26 –

    arXiv 2005

  22. [22]

    Tumlinson, M.S

    J. Tumlinson, M.S. Peeples and J.K. Werk,The Circumgalactic Medium, ARA&A55(2017) 389 [1709.09180]

    Pith/arXiv arXiv 2017

  23. [23]

    A. Rost, U. Kuchner, C. Welker, F. Pearce, F. Stasyszyn, M. Gray et al.,The ThreeHundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters, MNRAS502 (2021) 714 [2012.02850]

    Pith/arXiv arXiv 2021

  24. [24]

    Lokken, R

    M. Lokken, R. Hloˇ zek, A. van Engelen, M. Madhavacheril, E. Baxter, J. DeRose et al., Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. I. Evidence for Thermal Energy Anisotropy Using Oriented Stacking, ApJ933(2022) 134 [2107.05523]

    Pith/arXiv arXiv 2022

  25. [25]

    Henderson, R

    S.W. Henderson, R. Allison, J. Austermann, T. Baildon, N. Battaglia, J.A. Beall et al., Advanced ACTPol Cryogenic Detector Arrays and Readout,Journal of Low Temperature Physics184(2016) 772 [1510.02809]

    Pith/arXiv arXiv 2016

  26. [26]

    The Dark Energy Survey Collaboration,The Dark Energy Survey,arXiv e-prints(2005) [astro-ph/0510346]

    Pith/arXiv arXiv 2005

  27. [27]

    Lokken, A

    M. Lokken, A. van Engelen, M. Aguena, S.S. Allam, D. Anbajagane, D. Bacon et al., Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. II. Anisotropic Large-scale Coherence in Hot Gas, Galaxies, and Dark Matter, ApJ982(2025) 186 [2409.04535]

    Pith/arXiv arXiv 2025

  28. [28]

    Bond and S.T

    J.R. Bond and S.T. Myers,The Peak-Patch Picture of Cosmic Catalogs. I. Algorithms, ApJS 103(1996) 1

    1996

  29. [29]

    Stein, M.A

    G. Stein, M.A. Alvarez and J.R. Bond,The mass-Peak Patch algorithm for fast generation of deep all-sky dark matter halo catalogues and its N-body validation, MNRAS483(2019) 2236 [1810.07727]

    Pith/arXiv arXiv 2019

  30. [30]

    Stein, M.A

    G. Stein, M.A. Alvarez, J.R. Bond, A. van Engelen and N. Battaglia,The Websky extragalactic CMB simulations, J. Cosmology Astropart. Phys.2020(2020) 012 [2001.08787]

    Pith/arXiv arXiv 2020

  31. [31]

    Sunyaev and Y.B

    R.A. Sunyaev and Y.B. Zeldovich,The Spectrum of Primordial Radiation, its Distortions and their Significance,Comments on Astrophysics and Space Physics2(1970) 66

    1970

  32. [32]

    Sunyaev and Y.B

    R.A. Sunyaev and Y.B. Zeldovich,The Observations of Relic Radiation as a Test of the Nature of X-Ray Radiation from the Clusters of Galaxies,Comments on Astrophysics and Space Physics4(1972) 173

    1972

  33. [33]

    Mroczkowski, D

    T. Mroczkowski, D. Nagai, K. Basu, J. Chluba, J. Sayers, R. Adam et al.,Astrophysics with the Spatially and Spectrally Resolved Sunyaev-Zeldovich Effects. A Millimetre/Submillimetre Probe of the Warm and Hot Universe, Space Sci. Rev.215(2019) 17 [1811.02310]

    Pith/arXiv arXiv 2019

  34. [34]

    Chiang, R

    Y.-K. Chiang, R. Makiya, B. M´ enard and E. Komatsu,The Cosmic Thermal History Probed by Sunyaev-Zeldovich Effect Tomography, ApJ902(2020) 56 [2006.14650]

    Pith/arXiv arXiv 2020

  35. [35]

    Z. Chen, P. Zhang and X. Yang,Thermal Energy Census with the Sunyaev-Zel’dovich Effect of DESI Galaxy Clusters/Groups and Its Implication on the Weak-lensing Power Spectrum, ApJ 953(2023) 188 [2201.12591]

    Pith/arXiv arXiv 2023

  36. [36]

    Di Mascolo, Y

    L. Di Mascolo, Y. Perrott, T. Mroczkowski, S. Andreon, S. Ettori, A. Simionescu et al., Atacama Large Aperture Submillimeter Telescope (AtLAST) Science: Resolving the Hot and Ionized Universe through the Sunyaev-Zeldovich effect,arXiv e-prints(2024) arXiv:2403.00909 [2403.00909]

    Pith/arXiv arXiv 2024

  37. [37]

    Komatsu and U

    E. Komatsu and U. Seljak,The Sunyaev-Zel’dovich angular power spectrum as a probe of cosmological parameters, MNRAS336(2002) 1256 [astro-ph/0205468]

    Pith/arXiv arXiv 2002

  38. [38]

    Bhattacharya, D

    S. Bhattacharya, D. Nagai, L. Shaw, T. Crawford and G.P. Holder,Bispectrum of the Sunyaev-Zel’dovich Effect, ApJ760(2012) 5 [1203.6368]. – 27 –

    Pith/arXiv arXiv 2012

  39. [39]

    Hill and E

    J.C. Hill and E. Pajer,Cosmology from the thermal Sunyaev-Zel’dovich power spectrum: Primordial non-Gaussianity and massive neutrinos, Phys. Rev. D88(2013) 063526 [1303.4726]

    Pith/arXiv arXiv 2013

  40. [40]

    Hill and B.D

    J.C. Hill and B.D. Sherwin,Cosmological constraints from moments of the thermal Sunyaev-Zel’dovich effect, Phys. Rev. D87(2013) 023527 [1205.5794]

    Pith/arXiv arXiv 2013

  41. [41]

    Hojjati, T

    A. Hojjati, T. Tr¨ oster, J. Harnois-D´ eraps, I.G. McCarthy, L. van Waerbeke, A. Choi et al., Cross-correlating Planck tSZ with RCSLenS weak lensing: implications for cosmology and AGN feedback, MNRAS471(2017) 1565 [1608.07581]

    Pith/arXiv arXiv 2017

  42. [42]

    Hill, E.J

    J.C. Hill, E.J. Baxter, A. Lidz, J.P. Greco and B. Jain,Two-halo term in stacked thermal Sunyaev-Zel’dovich measurements: Implications for self-similarity, Phys. Rev. D97(2018) 083501 [1706.03753]

    Pith/arXiv arXiv 2018

  43. [43]

    Lippich, A.G

    M. Lippich, A.G. S´ anchez, M. Colavincenzo, E. Sefusatti, P. Monaco, L. Blot et al.,Comparing approximate methods for mock catalogues and covariance matrices - I. Correlation function, MNRAS482(2019) 1786 [1806.09477]

    Pith/arXiv arXiv 2019

  44. [44]

    L. Blot, M. Crocce, E. Sefusatti, M. Lippich, A.G. S´ anchez, M. Colavincenzo et al.,Comparing approximate methods for mock catalogues and covariance matrices II: power spectrum multipoles, MNRAS485(2019) 2806 [1806.09497]

    Pith/arXiv arXiv 2019

  45. [45]

    Colavincenzo, E

    M. Colavincenzo, E. Sefusatti, P. Monaco, L. Blot, M. Crocce, M. Lippich et al.,Comparing approximate methods for mock catalogues and covariance matrices - III: bispectrum, MNRAS 482(2019) 4883 [1806.09499]

    Pith/arXiv arXiv 2019

  46. [46]

    L. Kuhn, Z. Li and W.R. Coulton,Forecasts and Simulations for Relativistic Corrections to the Sunyaev-Zeldovich Effect,arXiv e-prints(2025) arXiv:2504.18637 [2504.18637]

    arXiv 2025

  47. [47]

    Battaglia, J.R

    N. Battaglia, J.R. Bond, C. Pfrommer and J.L. Sievers,On the Cluster Physics of Sunyaev-Zel’dovich and X-Ray Surveys. II. Deconstructing the Thermal SZ Power Spectrum, ApJ758(2012) 75 [1109.3711]

    Pith/arXiv arXiv 2012

  48. [48]

    Aghanim, Y

    Planck Collaboration, N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi et al., Planck 2018 results. VI. Cosmological parameters, A&A641(2020) A6 [1807.06209]

    Pith/arXiv arXiv 2018

  49. [49]

    Abbott, M

    T.M.C. Abbott, M. Aguena, A. Alarcon, S. Allam, O. Alves, A. Amon et al.,Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing, Phys. Rev. D105(2022) 023520 [2105.13549]

    Pith/arXiv arXiv 2022

  50. [50]

    Komatsu and T

    E. Komatsu and T. Kitayama,Sunyaev-Zeldovich Fluctuations from Spatial Correlations between Clusters of Galaxies, ApJ526(1999) L1 [astro-ph/9908087]

    Pith/arXiv arXiv 1999

  51. [51]

    Bolliet, B

    B. Bolliet, B. Comis, E. Komatsu and J.F. Mac ´ ıas-P´ erez,Dark energy constraints from the thermal Sunyaev-Zeldovich power spectrum, MNRAS477(2018) 4957 [1712.00788]

    Pith/arXiv arXiv 2018

  52. [52]

    Lewis, A

    A. Lewis, A. Challinor and A. Lasenby,Efficient Computation of Cosmic Microwave Background Anisotropies in Closed Friedmann-Robertson-Walker Models, ApJ538(2000) 473 [astro-ph/9911177]

    Pith/arXiv arXiv 2000

  53. [53]

    Hogg,Distance measures in cosmology,arXiv e-prints(1999) [astro-ph/9905116]

    D.W. Hogg,Distance measures in cosmology,arXiv e-prints(1999) [astro-ph/9905116]

    Pith/arXiv arXiv 1999

  54. [54]

    Kaiser,Evolution and clustering of rich clusters., MNRAS222(1986) 323

    N. Kaiser,Evolution and clustering of rich clusters., MNRAS222(1986) 323

    1986

  55. [55]

    Dav´ e, R

    R. Dav´ e, R. Cen, J.P. Ostriker, G.L. Bryan, L. Hernquist, N. Katz et al.,Baryons in the Warm-Hot Intergalactic Medium, ApJ552(2001) 473 [astro-ph/0007217]

    Pith/arXiv arXiv 2001

  56. [56]

    McQuinn,The Evolution of the Intergalactic Medium, ARA&A54(2016) 313 [1512.00086]

    M. McQuinn,The Evolution of the Intergalactic Medium, ARA&A54(2016) 313 [1512.00086]

    Pith/arXiv arXiv 2016

  57. [57]

    Cuciti, F

    V. Cuciti, F. de Gasperin, M. Br¨ uggen, F. Vazza, G. Brunetti, T.W. Shimwell et al.,Galaxy clusters enveloped by vast volumes of relativistic electrons,Nature609(2022) 911

    2022

  58. [58]

    Osato and D

    K. Osato and D. Nagai,Baryon pasting algorithm: halo-based and particle-based pasting methods, MNRAS519(2023) 2069 [2201.02632]. – 28 –

    Pith/arXiv arXiv 2023

  59. [59]

    Greco, J.C

    J.P. Greco, J.C. Hill, D.N. Spergel and N. Battaglia,The Stacked Thermal Sunyaev-Zel’dovich Signal of Locally Brightest Galaxies in Planck Full Mission Data: Evidence for Galaxy Feedback?, ApJ808(2015) 151 [1409.6747]

    Pith/arXiv arXiv 2015

  60. [60]

    Aghanim, M

    Planck Collaboration, N. Aghanim, M. Arnaud, M. Ashdown, J. Aumont, C. Baccigalupi et al., Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect, A&A594(2016) A22 [1502.01596]

    Pith/arXiv arXiv 2015

  61. [61]

    Horowitz and U

    B. Horowitz and U. Seljak,Cosmological constraints from thermal Sunyaev-Zeldovich power spectrum revisited, MNRAS469(2017) 394 [1609.01850]

    Pith/arXiv arXiv 2017

  62. [62]

    Gong, Y.-Z

    Y. Gong, Y.-Z. Ma and H. Tanimura,Probing galaxy cluster and intra-cluster gas with luminous red galaxies, MNRAS486(2019) 4904 [1904.12089]

    Pith/arXiv arXiv 2019

  63. [63]

    Singh, A

    P. Singh, A. Saro, M. Costanzi and K. Dolag,Cosmology dependence of galaxy cluster scaling relations, MNRAS494(2020) 3728 [1911.05751]

    Pith/arXiv arXiv 2020

  64. [64]

    Schaye, R

    J. Schaye, R. Kugel, M. Schaller, J.C. Helly, J. Braspenning, W. Elbers et al.,The FLAMINGO project: cosmological hydrodynamical simulations for large-scale structure and galaxy cluster surveys, MNRAS526(2023) 4978 [2306.04024]

    Pith/arXiv arXiv 2023

  65. [65]

    Lokken, W

    M. Lokken, W. Cui, J.R. Bond, R. Hloˇ zek, N. Murray, R. Dav´ e et al.,Boundless baryons: how diffuse gas contributes to anisotropic tSZ signal around simulated Three Hundred clusters, MNRAS523(2023) 1346 [2211.00242]

    Pith/arXiv arXiv 2023

  66. [66]

    Regaldo-Saint Blancard, S

    B. Regaldo-Saint Blancard, S. Codis, J.R. Bond and G. Stein,Statistical exploration of halo anisotropic clustering and intrinsic alignments with the mass-Peak Patch algorithm, MNRAS 504(2021) 1694 [2101.01455]

    Pith/arXiv arXiv 2021

  67. [67]

    McClintock, T.N

    T. McClintock, T.N. Varga, D. Gruen, E. Rozo, E.S. Rykoff, T. Shin et al.,Dark Energy Survey Year 1 results: weak lensing mass calibration of redMaPPer galaxy clusters, MNRAS 482(2019) 1352 [1805.00039]

    Pith/arXiv arXiv 2019

  68. [68]

    G´ orski, E

    K.M. G´ orski, E. Hivon, A.J. Banday, B.D. Wandelt, F.K. Hansen, M. Reinecke et al., HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere, ApJ622(2005) 759 [arXiv:astro-ph/0409513]

    Pith/arXiv arXiv 2005

  69. [69]

    Anbajagane, H

    D. Anbajagane, H. Aung, A.E. Evrard, A. Farahi, D. Nagai, D.J. Barnes et al.,Galaxy velocity bias in cosmological simulations: towards per cent-level calibration, MNRAS510(2022) 2980 [2110.01683]

    Pith/arXiv arXiv 2022

  70. [70]

    Schaan, S

    E. Schaan, S. Ferraro, S. Amodeo, N. Battaglia, S. Aiola, J.E. Austermann et al.,The Atacama Cosmology Telescope: Combined kinematic and thermal Sunyaev-Zel’dovich measurements from BOSS CMASS and LOWZ halos,arXiv e-prints(2020) arXiv:2009.05557 [2009.05557]

    Pith/arXiv arXiv 2020

  71. [71]

    R. Li, H.J. Mo, Z. Fan, F.C. van den Bosch and X. Yang,Probing hot gas in galaxy groups through the Sunyaev-Zeldovich effect, MNRAS413(2011) 3039 [1006.4760]

    Pith/arXiv arXiv 2011

  72. [72]

    W. Fang, K. Kadota and M. Takada,Cross-correlating the thermal Sunyaev-Zel’dovich effect and the distribution of galaxy clusters, Phys. Rev. D85(2012) 023007 [1109.4934]

    Pith/arXiv arXiv 2012

  73. [73]

    Vikram, A

    V. Vikram, A. Lidz and B. Jain,A Measurement of the Galaxy Group-Thermal Sunyaev-Zel’dovich Effect Cross-Correlation Function, MNRAS467(2017) 2315 [1608.04160]

    Pith/arXiv arXiv 2017

  74. [74]

    Pandey, E.J

    S. Pandey, E.J. Baxter, Z. Xu, J. Orlowski-Scherer, N. Zhu, A. Lidz et al.,Constraints on the redshift evolution of astrophysical feedback with Sunyaev-Zel’dovich effect cross-correlations, Phys. Rev. D100(2019) 063519 [1904.13347]

    Pith/arXiv arXiv 2019

  75. [75]

    Schimd, K

    C. Schimd, K. Kraljic, R. Dav´ e and C. Pichon,Large-scale geometry and topology of gas fields: Effects of AGN and stellar feedback, A&A689(2024) A311 [2406.04430]

    Pith/arXiv arXiv 2024

  76. [76]

    Anbajagane, S

    D. Anbajagane, S. Pandey and C. Chang,Map-level baryonification: Efficient modelling of – 29 – higher-order correlations in the weak lensing and thermal Sunyaev-Zeldovich fields,The Open Journal of Astrophysics7(2024) 108 [2409.03822]

    Pith/arXiv arXiv 2024

  77. [77]

    Aric` o and R.E

    G. Aric` o and R.E. Angulo,Baryonification extended to thermal Sunyaev Zel’dovich, A&A690 (2024) A188 [2406.01672]

    Pith/arXiv arXiv 2024

  78. [78]

    Yang, Y.-C

    T. Yang, Y.-C. Cai, W. Cui, R. Dav´ e, J.A. Peacock and D. Sorini,Understanding the relation between thermal Sunyaev-Zeldovich decrement and halo mass using the SIMBA and TNG simulations, MNRAS516(2022) 4084 [2202.11430]

    Pith/arXiv arXiv 2022

  79. [79]

    Sorini, R

    D. Sorini, R. Dav´ e, W. Cui and S. Appleby,How baryons affect haloes and large-scale structure: a unified picture from the SIMBA simulation, MNRAS (2022) [2111.13708]

    Pith/arXiv arXiv 2022

  80. [80]

    Ayromlou, D

    M. Ayromlou, D. Nelson and A. Pillepich,Feedback reshapes the baryon distribution within haloes, in halo outskirts, and beyond: the closure radius from dwarfs to massive clusters, MNRAS524(2023) 5391 [2211.07659]

    Pith/arXiv arXiv 2023

Showing first 80 references.