The Power Spectrum of the Sunyaev-Zel'dovich Effect

2); (2) Princeton; (3) CITA); A. Refregier (1; D.N. Spergel (2); E. Komatsu (2); U.-L. Pen (3) ((1) Cambridge

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The Power Spectrum of the Sunyaev-Zel'dovich Effect

A. Refregier (1, 2), E. Komatsu (2), D.N. Spergel (2), U.-L. Pen (3) ((1) Cambridge, (2) Princeton, (3) CITA)

Astrophysics · Submitted 9 Dec 1999

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim For cluster- normalized CDM models, the SZ power spectrum is comparable to the primordial power spectrum around l=2000.

how it is stated · asserted 1.00 read the record →

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arXiv IDastro-ph/9912180 (version 2)

Pith IDZ32VSTK2, Pith's permanent record of this paper and its review

Citation2), (2) Princeton, (3) CITA), A. Refregier (1, D.N. Spergel (2), E. Komatsu (2), U.-L. Pen (3) ((1) Cambridge. "The Power Spectrum of the Sunyaev-Zel'dovich Effect." arXiv:astro-ph/9912180 (1999). https://pith.science/paper/Z32VSTK2

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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.98 · human participants 0.01 · controlled comparison 0.22 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.97 · mentions code or data availability 0.02.

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arXiv listing abstract v2. Results and the main claim are underlined; show every role.

(Abridged) The hot gas in the IGM produces anisotropies in the Cosmic Microwave Background (CMB) through the thermal Sunyaev-Zel'dovich (SZ) effect. The SZ effect is a powerful probe of large-scale structure in the universe and must be carefully subtracted from measurements of the primary CMB anisotropies. We use moving-mesh hydrodynamical simulations to study the 3-dimensional statistics of the gas, and compute the mean comptonization parameter and the angular power spectrum of the SZ fluctuations, for different cosmologies. We compare these results with predictions using the Press-Schechter formalism. We find that the two methods agree approximately, but differ in details. We discuss this discrepancy, and show that resolution limits the reliability of our results to the 200<l<2000 range. For cluster- normalized CDM models, the SZ power spectrum is comparable to the primordial power spectrum around l=2000. We show that groups and filaments (kT<5 keV) contribute about 50% of the SZ power spectrum at l=500. About half of the SZ power spectrum on these scales is produced at redshifts z<0.1, and can thus be detected and removed using existing catalogs of galaxies and X-ray clusters. We discuss the implications of these results for the future MAP and Planck Surveyor missions.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	(Abridged) The hot gas in the IGM produces anisotropies in the Cosmic Microwave Background (CMB) through the thermal Sunyaev-Zel'dovich (SZ) effect.	background 1.00	0.05	0.04	asserted 1.00
s1	The SZ effect is a powerful probe of large-scale structure in the universe and must be carefully subtracted from measurements of the primary CMB anisotropies.	background 1.00	0.06	0.05	asserted 1.00
s2	We use moving-mesh hydrodynamical simulations to study the 3-dimensional statistics of the gas, and compute the mean comptonization parameter and the angular power spectrum of the SZ fluctuations, for different cosmologies.	method 0.72	0.97	0.06	asserted 0.98
s3	We compare these results with predictions using the Press-Schechter formalism.	method 0.90	0.87	0.03	asserted 0.74
s4	We find that the two methods agree approximately, but differ in details.	result 1.00	0.94	0.11	asserted 0.99
s5	We discuss this discrepancy, and show that resolution limits the reliability of our results to the 200<l<2000 range.	limitation 1.00	0.91	0.07	asserted 1.00
s6	For cluster- normalized CDM models, the SZ power spectrum is comparable to the primordial power spectrum around l=2000.	result 1.00	0.88	0.29	asserted 1.00
s7	We show that groups and filaments (kT<5 keV) contribute about 50% of the SZ power spectrum at l=500.	result 1.00	0.94	0.13	asserted 1.00
s8	About half of the SZ power spectrum on these scales is produced at redshifts z<0.1, and can thus be detected and removed using existing catalogs of galaxies and X-ray clusters.	result 0.78	0.88	0.15	asserted 0.99
s9	We discuss the implications of these results for the future MAP and Planck Surveyor missions.	interpretation 0.90	0.42	0.05	unclear 0.90

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

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arXiv listing abstract v2

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full text
figures and tables
references and citing sentences
relations to other papers

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P abstract

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T body sentences
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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

(Abridged) The hot gas in the IGM produces anisotropies in the Cosmic Microwave Background (CMB) through the thermal Sunyaev-Zel'dovich (SZ) effect. The SZ effect is a powerful probe of large-scale structure in the universe and must be carefully subtracted from measurements of the primary CMB anisotropies. We use moving-mesh hydrodynamical simulations to study the 3-dimensional statistics of the gas, and compute the mean comptonization parameter and the angular power spectrum of the SZ fluctuations, for different cosmologies. We compare these results with predictions using the Press-Schechter formalism. We find that the two methods agree approximately, but differ in details. We discuss this discrepancy, and show that resolution limits the reliability of our results to the 200<l<2000 range. For cluster- normalized CDM models, the SZ power spectrum is comparable to the primordial power spectrum around l=2000. We show that groups and filaments (kT<5 keV) contribute about 50% of the SZ power spectrum at l=500. About half of the SZ power spectrum on these scales is produced at redshifts z<0.1, and can thus be detected and removed using existing catalogs of galaxies and X-ray clusters. We discuss the implications of these results for the future MAP and Planck Surveyor missions.

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References

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Revisiting Constraints on Resonant Axion-Photon Conversions from CMB Spectral Distortions
astro-ph.CO 2024-11 conditional novelty 6.0 of 10

Resonant conversion of CMB photons into axions in a primordial magnetic field creates a characteristic spectral distortion, and the updated calculations tighten axion-photon coupling constraints and reach previously u...
Scale-dependent bias of galaxies and mu-type distortion of the cosmic microwave background spectrum from single-field inflation with a modified initial state
astro-ph.CO 2012-04 conditional novelty 5.0 of 10

Single-field inflation with a non-Bunch-Davies initial state yields a k^-3 scale-dependent halo bias and a mu-distortion-temperature cross-correlation that PIXIE could detect at occupation number near 0.5.
The Cosmic Microwave Background: Spectral Distortions
astro-ph.CO 2025-01 unverdicted novelty 1.0 of 10

A review of CMB spectral distortion theory and prospects, covering the standard y and mu distortions, guaranteed Lambda-CDM signals, and future spectrometer experiments.

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16 arXiv papers cite this in 21 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 13 sentences without a confident label

Uses its data or values 2 papers

The amplitude of these signals is more uncertain, but even within our standard cosmological paradigm, one expects an average $y$-parameter of $y≃10^-7-10^-6$ due to the large-scale structure and the reionization epoch [ref] , with the most recent computations giving $y≃2-6$ [ref] .

Spectral distortions of the CMB dipole · Introduction · 0.91
Several estimates for this contribution were obtained, yielding values for the total $y$-parameter at the level $y≃few-6$ [ref] .

The Cosmic Microwave Background: Spectral Distortions · Reionization and structure formation · 0.88

Cites it as background 5 papers

The mean electron pressure $⟨P_e⟩$ is related to the density-weighted mean temperature of electrons in the universe, defined as $T̅_e ≡⟨n_eT_e⟩/⟨n_e⟩$ [ref] .

Testing the SZ-based tomographic approach to the thermal history of the universe with pressure-density cross-correlations: Insights from the Magneticum simulation · The density-weighted mean electron temperature Te · 0.96
The contribution from the peaks in the large scale structure and the effect of baryonic physics to the $y$-type distortion fluctuations has been studied by many groups using numerical simulations as well as analytically [ref] .

Limits on the fluctuating part of $y$-type distortion monopole from Planck and SPT results · Introduction · 0.87
However, we have many astrophyscial/cosmological sources inducing spectral distortions: decaying or annihilating particles [ref] , reionization and structure formation [ref] , primordial black holes [ref] , cosmic strings [ref] , small-scale magnetic fields [ref] , the adiabatic cooling of matter [ref] , cosmological recombination [ref] , gravitino decay [ref] , and the dissipation of primordial density perturbations [ref] which is the main concern of this paper.

CMB Spectral $\mu$-Distortion of Multiple Inflation Scenario · Introduction · 0.94

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