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arxiv: 2604.19744 · v1 · submitted 2026-04-21 · 🌌 astro-ph.CO · astro-ph.GA

Recognition: unknown

Precision Kinematic Sunyaev--Zel'dovich Measurements Across Halo Mass and Redshift with DESI DR2 and ACT DR6: Part I. Luminous Red Galaxies

F. J. Qu , B. Ried Guachalla , E. Schaan , B. Hadzhiyska , S. Ferraro , J. Aguilar , S. Ahlen , A. Baleato Lizancos
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D. Bianchi D. Brooks R. Canning F. J. Castander E. Chaussidon T. Claybaugh A. Cuceu A. de la Macorra B. Dey P. Doel A. Font-Ribera J. E. Forero-Romero E. Gazta\~naga S. Gontcho A Gontcho G. Gutierrez H. K. Herrera-Alcantar K. Honscheid C. Howlett D. Huterer M. Ishak R. Kehoe T. Kisner A. Kremin O. Lahav M. Landriau L. Le Guillou M. E. Levi M. Manera A. Meisner R. Miquel S. Nadathur J. A. Newman W. J. Percival I. P'erez-R`afols G. Rossi L. Samushia E. Sanchez E. F. Schlafly D. Schlegel M. Schubnell H. Seo J. Silber D. Sprayberry G. Tarl'e B. A. Weaver R. Zhou
Authors on Pith no claims yet

Pith reviewed 2026-05-10 01:24 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords kinetic Sunyaev-Zel'dovich effectluminous red galaxieshalo gas profilesbaryonic feedbackcircumgalactic mediumDESIACTgas redistribution
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The pith

Precise kSZ measurements around luminous red galaxies show that gas profiles deviate from dark matter, indicating redistribution by feedback beyond gravitational collapse.

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

The paper measures the kinetic Sunyaev-Zel'dovich effect by cross-correlating 2.4 million spectroscopic luminous red galaxies from DESI DR2 with ACT DR6 data, achieving 18 sigma detection in both harmonic and configuration space. A new harmonic-space method using momentum-weighted templates produces nearly uncorrelated bandpowers, which are then converted to halo gas profiles via the LRG halo occupation distribution. The resulting generalized Navarro-Frenk-White fits demonstrate that gas does not trace dark matter, and comparison to hydrodynamical simulations favors feedback efficiencies higher than the Battaglia profile. The analysis also splits the signal by redshift and stellar mass to track evolution consistent with changing halo masses.

Core claim

The measurements establish that hot gas in halos around luminous red galaxies is redistributed beyond what gravitational collapse alone would produce, with the inferred profiles requiring more efficient gas ejection than assumed in the Battaglia feedback model. This is obtained by converting observed galaxy-centered kSZ signals into halo-centered profiles and fitting them with generalized Navarro-Frenk-White forms that deviate systematically from dark-matter expectations.

What carries the argument

Momentum-weighted kSZ templates in harmonic space for cross-correlation, combined with halo occupation distribution modeling to convert galaxy gas profiles into halo gas profiles.

If this is right

  • Hydrodynamical simulations must adopt higher feedback efficiencies in group-scale halos to match the observed gas redistribution.
  • Baryonic modeling for large-scale structure analyses should incorporate more extended gas profiles than standard dark-matter tracing assumes.
  • The kSZ signal amplitude declines with redshift in a manner consistent with the expected drop in mean halo mass at fixed comoving number density.
  • Splitting by stellar mass reveals how kSZ amplitude scales with galaxy properties across the luminous red galaxy population.

Where Pith is reading between the lines

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

  • The same spectroscopic kSZ approach applied to other tracers such as emission-line galaxies could map feedback across a wider range of halo masses and environments.
  • The measured deviation supplies an empirical target that can be used to calibrate subgrid feedback prescriptions in simulations without relying solely on internal simulation diagnostics.
  • If the higher feedback efficiency persists in other galaxy samples, it would tighten constraints on the total baryon budget available for star formation and on the thermal history of the circumgalactic medium.

Load-bearing premise

The conversion from measured galaxy-centered signals to halo-centered gas profiles relies on the adopted luminous red galaxy halo occupation distribution being accurate enough that modeling uncertainties do not dominate the inferred deviation from dark matter.

What would settle it

Repeating the profile conversion with an independent halo occupation distribution that differs by more than the quoted uncertainty and finding that the deviation from dark matter disappears or reverses sign.

Figures

Figures reproduced from arXiv: 2604.19744 by A. Baleato Lizancos, A. Cuceu, A. de la Macorra, A. Font-Ribera, A. Kremin, A. Meisner, B. A. Weaver, B. Dey, B. Hadzhiyska, B. Ried Guachalla, C. Howlett, D. Bianchi, D. Brooks, D. Huterer, D. Schlegel, D. Sprayberry, E. Chaussidon, E. F. Schlafly, E. Gazta\~naga, E. Sanchez, E. Schaan, F. J. Castander, F. J. Qu, G. Gutierrez, G. Rossi, G. Tarl'e, H. K. Herrera-Alcantar, H. Seo, I. P'erez-R`afols, J. Aguilar, J. A. Newman, J. E. Forero-Romero, J. Silber, K. Honscheid, L. Le Guillou, L. Samushia, M. E. Levi, M. Ishak, M. Landriau, M. Manera, M. Schubnell, O. Lahav, P. Doel, R. Canning, R. Kehoe, R. Miquel, R. Zhou, S. Ahlen, S. Ferraro, S. Gontcho A Gontcho, S. Nadathur, T. Claybaugh, T. Kisner, W. J. Percival.

Figure 1
Figure 1. Figure 1: FIG. 1. Sky coverage of the DESI LRG DR2 sample (blue) [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Stellar mass distribution of the DESI LRG Year 3 [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Redshift distribution of the DESI LRG Year 3 sample [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Distribution of reconstructed line-of-sight velocities [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Sensitivity of the GNFW gas profile and the kSZ-galaxy correlation to the three sampled shape parameters. [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Correlation coefficient matrix between kSZ measure [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Measured kSZ-galaxy power spectrum from cross-correlating DESI galaxies with ACT CMB temperature maps across [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10. Null test using random velocity templates in har [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11. Stacked CMB temperature map around galaxy po [PITH_FULL_IMAGE:figures/full_fig_p017_11.png] view at source ↗
Figure 13
Figure 13. Figure 13: FIG. 13. Mean kSZ temperature profiles as a function of [PITH_FULL_IMAGE:figures/full_fig_p018_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: shows the fractional amplitude Abf(z)/Abf 1 2 3 4 5 6 [arcmin] 10 1 10 0 10 1 [ K a r c min ] z1 SNR=10 z2 SNR=9 z3 SNR=9 z4 SNR=5 FIG. 13. Mean kSZ temperature profiles as a function of projected radius for DESI LRGs in four redshift bins: z1 (0.4 < z < 0.6, dark blue), z2 (0.6 < z < 0.7, light blue), z3 (0.7 < z < 0.8, dark green), and z4 (0.8 < z < 1.1, light green). The detection significance correspo… view at source ↗
Figure 16
Figure 16. Figure 16: FIG. 16. Comparison between the real-space CAP measure [PITH_FULL_IMAGE:figures/full_fig_p020_16.png] view at source ↗
Figure 15
Figure 15. Figure 15: FIG. 15 [PITH_FULL_IMAGE:figures/full_fig_p020_15.png] view at source ↗
Figure 18
Figure 18. Figure 18: FIG. 18. Stacked kSZ signal versus angular scale in four red [PITH_FULL_IMAGE:figures/full_fig_p021_18.png] view at source ↗
Figure 17
Figure 17. Figure 17: FIG. 17. Stacked kSZ signal versus angular scale comparison [PITH_FULL_IMAGE:figures/full_fig_p021_17.png] view at source ↗
Figure 19
Figure 19. Figure 19: FIG. 19. Comparison of kSZ measurements using DESI DR2 [PITH_FULL_IMAGE:figures/full_fig_p022_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: FIG. 20. Foreground test for the kSZ signal. [PITH_FULL_IMAGE:figures/full_fig_p025_20.png] view at source ↗
Figure 22
Figure 22. Figure 22: FIG. 22. Null test for systematic errors in the kSZ measure [PITH_FULL_IMAGE:figures/full_fig_p026_22.png] view at source ↗
Figure 24
Figure 24. Figure 24: FIG. 24. Comparison of our DR1 reanalysis (red, SNR = 9.6) [PITH_FULL_IMAGE:figures/full_fig_p026_24.png] view at source ↗
Figure 26
Figure 26. Figure 26: FIG. 26. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p027_26.png] view at source ↗
Figure 25
Figure 25. Figure 25: FIG. 25. Cumulative significance for simulation gas profiles [PITH_FULL_IMAGE:figures/full_fig_p027_25.png] view at source ↗
Figure 27
Figure 27. Figure 27: FIG. 27. Robustness to pixelization. Ratio of the auto [PITH_FULL_IMAGE:figures/full_fig_p029_27.png] view at source ↗
Figure 28
Figure 28. Figure 28: FIG. 28. Impact of cosmological parameter uncertainty on the [PITH_FULL_IMAGE:figures/full_fig_p030_28.png] view at source ↗
read the original abstract

We present the most precise measurements of the kinetic Sunyaev-Zel'dovich (kSZ) effect around luminous red galaxies to date, detecting the signal at $18\sigma$ significance in both harmonic and configuration space. Our analysis cross-correlates 2.4 million spectroscopic LRGs from the Dark Energy Spectroscopic Instrument (DESI) DR2 sample with Data Release 6 (DR6) of the Atacama Cosmology Telescope (ACT). We develop a novel harmonic-space cross-correlation approach using momentum-weighted kSZ templates, yielding nearly uncorrelated bandpowers within a framework consistent with other large-scale structure analyses. By incorporating the LRG halo occupation distribution (HOD) and its uncertainty, we convert measured galaxy gas profiles into halo gas profiles and provide generalized Navarro-Frenk-White (GNFW) fitting profiles, providing empirical targets for tuning feedback efficiency in hydrodynamical simulations and for baryonic modeling in large-scale structure analyses. We find strong evidence that gas profiles do not trace dark matter, providing direct evidence for gas redistribution beyond gravitational collapse. Comparing to hydrodynamical simulations, our measurements favor feedback efficiencies exceeding those in the Battaglia profile, suggesting more efficient gas ejection in group-scale halos than previously predicted. Splitting by redshift, we detect the kSZ signal at SNR $\approx 5$--$10$ in each of four bins and find amplitude evolution consistent with the expected decline in mean halo mass at fixed comoving number density. Splitting by stellar mass, we study the scaling of kSZ amplitude with galaxy properties. Together with BGS and ELG measurements in Paper II, these results span $0.1 \lesssim z \lesssim 1.6$ across three galaxy populations, demonstrating the potential of spectroscopic kSZ to map circumgalactic gas and constrain baryonic feedback.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper reports an 18σ detection of the kinetic Sunyaev-Zel'dovich (kSZ) effect around 2.4 million luminous red galaxies (LRGs) from DESI DR2 cross-correlated with ACT DR6. It introduces a novel harmonic-space cross-correlation estimator using momentum-weighted kSZ templates, converts the measured galaxy gas profiles to halo-centric profiles by incorporating the LRG halo occupation distribution (HOD) and its uncertainty, performs generalized Navarro-Frenk-White (GNFW) fits, and claims strong evidence that gas does not trace dark matter, favoring feedback efficiencies higher than in the Battaglia profile. Results are also split by redshift (SNR ≈5–10 in four bins) and stellar mass.

Significance. If the HOD conversion holds, the high-significance detection and GNFW constraints provide valuable empirical targets for baryonic feedback in hydrodynamical simulations and for modeling in large-scale structure analyses. The large sample size, redshift and mass splits, and consistency with expected evolution are strengths; the novel estimator and direct cross-correlation approach add technical value.

major comments (2)
  1. [HOD conversion and halo gas profile section (methods and results)] The central interpretive claims—that gas profiles do not trace dark matter and that measurements favor feedback efficiencies exceeding the Battaglia profile—rest on converting the observed galaxy-kSZ cross-correlation into halo gas profiles. This step uses the adopted LRG HOD to account for central/satellite fractions, mass distribution, and one-halo/two-halo terms. While the abstract states that HOD uncertainty is incorporated, it is not demonstrated that residual mismatches between the assumed HOD parametrization and the true distribution (e.g., from alternative clustering or weak-lensing constraints) do not rescale or distort the inferred halo gas density enough to affect the deviation from NFW or the GNFW parameter comparison. This modeling choice is load-bearing for the strongest claims.
  2. [Abstract and estimator validation] The abstract states an 18σ detection in both harmonic and configuration space but provides no quantitative summary of residual systematics, covariance validation, or robustness tests for the novel momentum-weighted estimator. Given that the subsequent GNFW fitting and simulation comparison are used to claim higher feedback, explicit tests showing that the deviation from dark-matter tracing persists under reasonable HOD variations and estimator choices are needed to support the interpretation.
minor comments (2)
  1. [Abstract] The abstract is information-dense; consider separating the detection significance, the HOD conversion step, and the feedback comparison into clearer sentences for readability.
  2. [Methods] Notation for the GNFW parameters and the exact definition of the momentum-weighted templates could be clarified with a dedicated equation or table in the methods.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address each major comment below in turn and have revised the paper accordingly to strengthen the presentation of our results on the HOD conversion and estimator validation.

read point-by-point responses

  1. Referee: [HOD conversion and halo gas profile section (methods and results)] The central interpretive claims—that gas profiles do not trace dark matter and that measurements favor feedback efficiencies exceeding the Battaglia profile—rest on converting the observed galaxy-kSZ cross-correlation into halo gas profiles. This step uses the adopted LRG HOD to account for central/satellite fractions, mass distribution, and one-halo/two-halo terms. While the abstract states that HOD uncertainty is incorporated, it is not demonstrated that residual mismatches between the assumed HOD parametrization and the true distribution (e.g., from alternative clustering or weak-lensing constraints) do not rescale or distort the inferred halo gas density enough to affect the deviation from NFW or the GNFW parameter comparison. This modeling choice is load-bearing for the strongest claims.

    Authors: We agree that an explicit demonstration of robustness against residual HOD mismatches is necessary to support the load-bearing interpretive claims. In the revised manuscript we have added a new subsection that systematically varies the HOD parameters within the range allowed by alternative clustering and weak-lensing constraints. We show that the resulting halo-centric gas profiles and GNFW parameters remain consistent within the quoted uncertainties, preserving both the deviation from NFW and the preference for feedback efficiencies higher than the Battaglia profile. These tests are now summarized in the text and illustrated in an additional figure. revision: yes

  2. Referee: [Abstract and estimator validation] The abstract states an 18σ detection in both harmonic and configuration space but provides no quantitative summary of residual systematics, covariance validation, or robustness tests for the novel momentum-weighted estimator. Given that the subsequent GNFW fitting and simulation comparison are used to claim higher feedback, explicit tests showing that the deviation from dark-matter tracing persists under reasonable HOD variations and estimator choices are needed to support the interpretation.

    Authors: We accept that the abstract and validation sections would benefit from more quantitative detail. We have revised the abstract to include a concise statement on the robustness tests performed. In addition, we have expanded the estimator validation discussion to report quantitative summaries of residual systematics, covariance validation, and explicit checks confirming that the deviation from dark-matter tracing and the higher-feedback conclusion remain stable under reasonable HOD variations and alternative estimator choices. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the kSZ derivation chain

full rationale

The paper's core results are direct cross-correlations between independent datasets (DESI DR2 spectroscopic LRGs and ACT DR6 kSZ maps), producing an 18σ detection in harmonic and configuration space. Conversion of galaxy gas profiles to halo-centric profiles via incorporation of the LRG HOD (and its uncertainty) is a post-measurement modeling step using separately determined occupation parameters, not a self-definitional loop or fitted input renamed as prediction. GNFW profile fitting and hydrodynamical simulation comparisons are interpretive post-processing that do not force the primary detection or the claim of gas redistribution by construction. No load-bearing self-citations, uniqueness theorems, or ansatz smuggling are required for the central measurement; the analysis remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard cosmological assumptions for converting redshifts and angular scales into halo masses, plus the accuracy of the LRG HOD model used to map galaxy to halo quantities. No new particles or forces are introduced.

free parameters (1)
  • GNFW profile parameters
    The generalized Navarro-Frenk-White parameters are fitted to the measured gas profiles after the cross-correlation step.
axioms (2)
  • domain assumption Standard flat Lambda-CDM cosmology for distance and halo mass conversions
    Invoked when interpreting the kSZ signal in terms of physical halo properties and redshift evolution.
  • domain assumption LRG halo occupation distribution model and its uncertainty are sufficiently accurate
    Used to convert galaxy-centered measurements into halo gas profiles.

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Reference graph

Works this paper leans on

96 extracted references · 49 canonical work pages · 4 internal anchors

  1. [1]

    29 ˆπ(θ) = Z l.o.s

    Building the kSZ momentum template ˆπ(θ) = X i∈pixel(θ) vr,i c (C12) ˆπ(θ) = ˆπ2D(θ)×Ω pix (C13) here, note that ˆπis an extensive quantity and depends on the size of the pixel. 29 ˆπ(θ) = Z l.o.s. n3D g (χ,θ) vr(χ,θ) c dV(C14) = Ωpix Z n3D g (z,θ) vr(z,θ) c χ2(z) c H(z) dz(C15) = Ωpix Z n3D g (χ,θ) vr(χ,θ) c χ2 dχ(C16) = Ωpix Z ¯n3D g (χ) [1 +δg(χ,θ)] vr...

  2. [2]

    Robustness in building the template We verified that our kSZ template is insensitive to the choice of sky pixelization by constructing it in two in- dependent ways: (i) on the sphere using an equal–area HEALPixgrid (after projecting the CAR maps and mask toHEALPix), and (ii) directly on a CAR grid using pixell, enforcing the same declination cut (δ >−20 ◦...

  3. [3]

    L. D. E. S. Collaboration, Large synoptic survey telescope: Dark energy science collaboration (2012), arXiv:https://arxiv.org/abs/1211.0310 arXiv:1211.0310 [astro-ph.CO]

    work page Pith review arXiv 2012

  4. [4]

    Ivezic, S

    Z. Ivezic, S. M. Kahn, J. A. Tyson, B. Abel, E. Acosta, R. Allsman, D. Alonso, Y. AlSayyad, S. F. Anderson, J. Andrew, J. R. P. Angel, G. Z. Angeli, R. Ansari, P. Antilogus, C. Araujo, R. Armstrong, K. T. Arndt, P. Astier, ´E. Aubourg, N. Auza, T. S. Axelrod, D. J. Bard, J. D. Barr, A. Barrau, J. G. Bartlett, A. E. Bauer, B. J. Bauman, S. Baumont, E. Bech...

    2019

  5. [5]

    Euclid Collaborationet al., Euclid preparation. I. The Euclid Wide Survey, A&A662, A112 (2022), arXiv:https://arxiv.org/abs/2108.01201 arXiv:2108.01201 [astro-ph.CO]

    work page arXiv 2022

  6. [6]

    Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report

    D. Spergel, N. Gehrels, C. Baltay, D. Bennett, J. Breckin- ridge, M. Donahue, A. Dressler, B. S. Gaudi, T. Greene, O. Guyon, C. Hirata, J. Kalirai, N. J. Kasdin, B. Macin- tosh, W. Moos, S. Perlmutter, M. Postman, B. Rauscher, J. Rhodes, Y. Wang, D. Weinberg, D. Benford, M. Hud- son, W. S. Jeong, Y. Mellier, W. Traub, T. Yamada, P. Capak, J. Colbert, D. M...

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  7. [7]

    Cen and J

    R. Cen and J. P. Ostriker, Where Are the Baryons? II. Feedback Effects, Astrophys. J.650, 560 (2006), arXiv:https://arxiv.org/abs/astro-ph/0601008 arXiv:astro-ph/0601008 [astro-ph]

    work page arXiv 2006

  8. [8]

    Birkinshaw, The sunyaev–zeldovich effect, Physics Reports310, 97 (1999)

    M. Birkinshaw, The sunyaev–zeldovich effect, Physics Reports310, 97 (1999)

    1999

  9. [9]

    doi:10.1007/s11214-019-0581-2 , archiveprefix =

    T. Mroczkowski, D. Nagai, K. Basu, J. Chluba, J. Say- ers, R. Adam, E. Churazov, A. Crites, L. Di Mas- colo, D. Eckert, J. Macias-Perez, F. Mayet, L. Perotto, E. Pointecouteau, C. Romero, F. Ruppin, E. Scanna- pieco, and J. ZuHone, Astrophysics with the spatially and spectrally resolved sunyaev-zeldovich effects: A millime- tre/submillimetre probe of the ...

    work page doi:10.1007/s11214-019-0581-2 2019

  10. [10]

    N. Hand, G. E. Addison, E. Aubourg, N. Battaglia, E. S. Battistelli, D. Bizyaev, J. R. Bond, H. Brew- ington, J. Brinkmann, B. R. Brown, S. Das, K. S. Dawson, M. J. Devlin, J. Dunkley, R. Dunner, D. J. Eisenstein, J. W. Fowler, M. B. Gralla, A. Hajian, M. Halpern, M. Hilton, A. D. Hincks, R. Hlozek, J. P. Hughes, L. Infante, K. D. Irwin, A. Kosowsky, Y.-T...

    2012

  11. [11]

    Hern´ andez-Monteagudo, Y.-Z

    C. Hern´ andez-Monteagudo, Y.-Z. Ma, F. S. Kitaura, W. Wang, R. G´ enova-Santos, J. Mac´ ıas-P´ erez, and D. Herranz, Evidence of the missing baryons from the kinematic sunyaev-zeldovich effect in planck data, Phys. Rev. Lett.115, 191301 (2015)

    2015

  12. [12]

    F. D. Bernardis, S. Aiola, E. Vavagiakis, N. Battaglia, M. Niemack, J. Beall, D. Becker, J. Bond, E. Calabrese, H. Cho, K. Coughlin, R. Datta, M. Devlin, J. Dunkley, R. Dunner, S. Ferraro, A. Fox, P. Gallardo, M. Halpern, N. Hand, M. Hasselfield, S. Henderson, J. Hill, G. Hilton, M. Hilton, A. Hincks, R. Hlozek, J. Hubmayr, K. Huffen- berger, J. Hughes, K...

  13. [13]

    Soergel, S

    B. Soergel, S. Flender, K. T. Story, L. Bleem, T. Gi- annantonio, G. Efstathiou, E. Rykoff, B. A. Benson, T. Crawford, S. Dodelson, S. Habib, K. Heitmann, G. Holder, B. Jain, E. Rozo, A. Saro, J. Weller, F. B. Ab- dalla, S. Allam, J. Annis, R. Armstrong, A. Benoit-L´ evy, G. M. Bernstein, J. E. Carlstrom, A. Carnero Rosell, M. Carrasco Kind, F. J. Castand...

    2016

  14. [14]

    N. S. Sugiyama, T. Okumura, and D. N. Spergel, A direct measure of free electron gas via the kinematic sunyaev– zeldovich effect in fourier-space analysis, Monthly Notices of the Royal Astronomical Society475, 3764 (2018)

    2018

  15. [15]

    Calafut, P

    V. Calafut, P. A. Gallardo, E. M. Vavagiakis, S. Amodeo, S. Aiola, J. E. Austermann, N. Battaglia, E. S. Battis- telli, J. A. Beall, R. Bean, J. R. Bond, E. Calabrese, S. K. Choi, N. F. Cothard, M. J. Devlin, C. J. Duell, S. M. Duff, A. J. Duivenvoorden, J. Dunkley, R. Dunner, S. Ferraro, Y. Guan, J. C. Hill, G. C. Hilton, M. Hilton, R. Hloˇ zek, Z. B. Hu...

    2021

  16. [16]

    S. Li, Y. Zheng, Z. Chen, H. Xu, and X. Yang, Detection of pairwise kinetic sunyaev-zel’dovich ef- fect with desi galaxy groups and planck in fourier space (2024), arXiv:https://arxiv.org/abs/2401.03507 arXiv:2401.03507 [astro-ph.CO]

    work page arXiv 2024

  17. [17]

    B. Hadzhiyskaet al., Probing cosmic velocities with the pairwise kinematic Sunyaev-Zel’dovich sig- nal in DESI Bright Galaxy Sample DR1 and ACT DR6 (2025), arXiv:https://arxiv.org/abs/2510.14135 arXiv:2510.14135 [astro-ph.CO]

    work page arXiv 2025

  18. [18]

    Harscouet, K

    L. Harscouet, K. Wolz, A. Wayland, D. Alonso, and B. Hadzhiyska, ksz for ev- eryone: the pseudo-cl approach to stacking (2025), arXiv:https://arxiv.org/abs/2512.14625 arXiv:2512.14625 [astro-ph.CO]

    work page arXiv 2025

  19. [19]

    J. C. Hill, S. Ferraro, N. Battaglia, J. Liu, and D. N. Spergel, Kinematic sunyaev-zel’dovich effect with pro- jected fields: A novel probe of the baryon distribution with planck, wmap, and wise data, Phys. Rev. Lett.117, 051301 (2016)

    2016

  20. [20]

    Ferraro, J

    S. Ferraro, J. C. Hill, N. Battaglia, J. Liu, and D. N. Spergel, Kinematic sunyaev-zel’dovich effect with pro- jected fields. ii. prospects, challenges, and comparison with simulations, Phys. Rev. D94, 123526 (2016)

    2016

  21. [21]

    Kusiak, B

    A. Kusiak, B. Bolliet, S. Ferraro, J. C. Hill, and A. Krolewski, Constraining the baryon abundance with the kinematic sunyaev-zel’dovich effect: Projected-field detection usingplanck,wmap, andunwise, Phys. Rev. D104, 043518 (2021)

    2021

  22. [22]

    Bolliet, J

    B. Bolliet, J. Colin Hill, S. Ferraro, A. Kusiak, and A. Krolewski, Projected-field kinetic sunyaev-zeldovich cross-correlations: halo model and forecasts, Journal of Cosmology and Astroparticle Physics2023(03), 039

  23. [23]

    Schaan, S

    E. Schaan, S. Ferraro, M. Vargas-Maga˜ na, K. M. Smith, S. Ho, S. Aiola, N. Battaglia, J. R. Bond, F. De Bernardis, E. Calabrese, H.-M. Cho, M. J. Devlin, J. Dunkley, P. A. Gallardo, M. Hasselfield, S. Hender- son, J. C. Hill, A. D. Hincks, R. Hlozek, J. Hubmayr, J. P. Hughes, K. D. Irwin, B. Koopman, A. Kosowsky, D. Li, T. Louis, M. Lungu, M. Madhavacher...

    2016

  24. [24]

    Schaan, S

    E. Schaan, S. Ferraro, S. Amodeo, N. Battaglia, S. Aiola, J. E. Austermann, J. A. Beall, R. Bean, D. T. Becker, R. J. Bond, E. Calabrese, V. Calafut, S. K. Choi, E. V. Denison, M. J. Devlin, S. M. Duff, A. J. Duivenvoorden, J. Dunkley, R. D¨ unner, P. A. Gallardo, Y. Guan, D. Han, J. C. Hill, G. C. Hilton, M. Hilton, R. Hloˇ zek, J. Hub- mayr, K. M. Huffe...

    2021

  25. [25]

    Mallaby-Kay, S

    M. Mallaby-Kay, S. Amodeo, J. C. Hill, M. Aguena, S. Allam, O. Alves, J. Annis, N. Battaglia, E. S. Battis- telli, E. J. Baxter, K. Bechtol, M. R. Becker, E. Bertin, J. R. Bond, D. Brooks, E. Calabrese, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, A. Choi, M. Crocce, L. N. da Costa, M. E. S. Pereira, J. De Vicente, S. De- sai, J. P. Dietrich, P. Doe...

    2023

  26. [26]

    Hadzhiyska, S

    B. Hadzhiyska, S. Ferraro, B. R. Guachalla, E. Schaan, J. Aguilar, N. Battaglia, J. R. Bond, D. Brooks, E. Cal- abrese, S. K. Choi, T. Claybaugh, W. R. Coulton, K. Dawson, M. Devlin, B. Dey, P. Doel, A. J. Duiv- envoorden, J. Dunkley, G. S. Farren, A. Font-Ribera, J. E. Forero-Romero, P. A. Gallardo, E. Gazta˜ naga, S. G. Gontcho, M. Gralla, L. L. Guillou...

    work page arXiv 2025

  27. [27]

    B. R. Guachalla, E. Schaan, B. Hadzhiyska, S. Fer- raro, J. N. Aguilar, S. Ahlen, N. Battaglia, D. Bianchi, R. Bond, D. Brooks, T. Claybaugh, W. R. Coulton, A. de la Macorra, M. J. Devlin, A. Dey, P. Doel, J. Dunk- ley, K. Fanning, J. Forero-Romero, E. Gazta˜ naga, S. G. A. Gontcho, G. Gutierrez, J. Guy, J. C. Hill, K. Honscheid, S. Juneau, T. Kisner, A. ...

    work page arXiv 2025

  28. [28]

    McCarthy, N

    F. McCarthy, N. Battaglia, R. Bean, J. R. Bond, H. Cai, E. Calabrese, W. R. Coulton, M. J. Devlin, J. Dunkley, S. Ferraro, V. Gluscevic, Y. Guan, J. C. Hill, M. C. Johnson, A. Kusiak, A. Lagu¨ e, N. Mac- Crann, M. S. Madhavacheril, K. Moodley, S. Naess, F. J. Qu, B. R. Guachalla, N. Sehgal, B. D. Sherwin, C. Sif´ on, K. M. Smith, S. T. Staggs, A. van Enge...

    work page arXiv 2024

  29. [29]

    McCarthy, B

    F. McCarthy, B. Hadzhiyska, J. R. Bond, W. R. Coulton, J. Dunkley, C. E. Villagra, M. C. John- son, K. Moodley, T. Namikawa, B. R. Guachalla, B. D. Sherwin, C. Sif´ on, A. van Engelen, E. M. Vavagiakis, and E. J. Wollack, The atacama cosmol- ogy telescope: Cross-correlation of ksz and continu- ity equation velocity reconstruction with photometric desi lrg...

    work page arXiv 2025

  30. [30]

    S. C. Hotinli, K. M. Smith, and S. Ferraro, Velocity reconstruction from ksz: Measuringf N L with act and desils (2025), arXiv:https://arxiv.org/abs/2506.21657 arXiv:2506.21657 [astro-ph.CO]

    work page arXiv 2025

  31. [31]

    A. C. M. Lai, Y. Kvasiuk, and M. M¨ unchmeyer, Ksz velocity reconstruction with act and desi-ls using a tomographic qml power spectrum esti- mator (2025), arXiv:https://arxiv.org/abs/2506.21684 arXiv:2506.21684 [astro-ph.CO]

    work page arXiv 2025

  32. [32]

    Lagu¨ e, M

    A. Lagu¨ e, M. S. Madhavacheril, K. M. Smith, S. Ferraro, and E. Schaan, Constraints on local primordial non-gaussianity with 3d velocity recon- struction from the kinetic sunyaev-zeldovich ef- fect (2024), arXiv:https://arxiv.org/abs/2411.08240 arXiv:2411.08240 [astro-ph.CO]

    work page arXiv 2024

  33. [33]

    Coulton, M

    W. Coulton, M. S. Madhavacheril, A. J. Duivenvoor- den, J. C. Hill, I. Abril-Cabezas, P. A. R. Ade, S. Aiola, T. Alford, M. Amiri, S. Amodeo, R. An, Z. Atkins, J. E. Austermann, N. Battaglia, E. S. Battistelli, J. A. Beall, R. Bean, B. Beringue, T. Bhandarkar, E. Biermann, B. Bolliet, J. R. Bond, H. Cai, E. Calabrese, V. Cala- fut, V. Capalbo, F. Carrero,...

    2024

  34. [34]

    Schneider, S

    A. Schneider, S. K. Giri, S. Amodeo, and A. Refregier, Constraining baryonic feedback and cosmology with weak-lensing, x-ray, and kinematic sunyaev–zeldovich ob- servations, Monthly Notices of the Royal Astronomical Society514, 3802–3814 (2022)

    2022

  35. [37]

    The kinetic sunyaev zeldovich effect as a benchmark for agn feedback models in hydrodynamical simulations: insights from desi + act,

    L. Bigwood, M. Yamamoto, J. Siegel, A. Amon, I. G. McCarthy, R. Dave, J. Salcido, M. Schaller, J. Schaye, and T. Yang, The kinetic sunyaev zel- dovich effect as a benchmark for agn feedback mod- els in hydrodynamical simulations: insights from desi + act (2025), arXiv:https://arxiv.org/abs/2510.15822 arXiv:2510.15822 [astro-ph.CO]

    work page arXiv 2025

  36. [38]

    Siegel, L

    J. Siegel, L. Bigwood, A. Amon, J. McCullough, M. Ya- mamoto, I. G. McCarthy, M. Schaller, A. Schnei- der, and J. Schaye, The suppression of the mat- ter power spectrum: strong feedback from X-ray gas mass fractions, kSZ effect profiles, and galaxy-galaxy lensing (2025), arXiv:https://arxiv.org/abs/2512.02954 arXiv:2512.02954 [astro-ph.CO]

    work page arXiv 2025

  37. [39]

    Salcido and I

    J. Salcido and I. G. McCarthy, Implications of feedback solutions to thes 8 tension for the baryon fractions of galaxy groups and clusters (2025), arXiv:https://arxiv.org/abs/2409.05716 arXiv:2409.05716 [astro-ph.CO]

    work page arXiv 2025

  38. [40]

    I. G. McCarthy, A. Amon, J. Schaye, E. Schaan, R. E. Angulo, J. Salcido, M. Schaller, L. Bigwood, W. Elbers, R. Kugel, J. C. Helly, V. J. F. Moreno, C. S. Frenk, R. J. McGibbon, L. Ondaro-Mallea, and M. P. van Daalen, Flamingo: combining kinetic 36 sz effect and galaxy-galaxy lensing measurements to gauge the impact of feedback on large-scale struc- ture ...

    work page arXiv 2025

  39. [41]

    Lagu¨ e, M

    A. Lagu¨ e, M. S. Madhavacheril, J. Borrow, K. M. Smith, X. Chen, M. Schaller, and J. Schaye, In- ferring the Impacts of Baryonic Feedback from Kinetic Sunyaev-Zeldovich Cross-Correlations (2025), arXiv:https://arxiv.org/abs/2511.20595 arXiv:2511.20595 [astro-ph.CO]

    work page arXiv 2025

  40. [42]

    Kovaˇ c, A

    M. Kovaˇ c, A. Nicola, J. Bucko, A. Schneider, R. Reis- chke, S. K. Giri, R. Teyssier, M. Schaller, and J. Schaye, Baryonification ii: Constraining feedback with x-ray and kinematic sunyaev-zel’dovich obser- vations (2025), arXiv:https://arxiv.org/abs/2507.07991 arXiv:2507.07991 [astro-ph.CO]

    work page arXiv 2025

  41. [43]

    Hadzhiyska, S

    B. Hadzhiyska, S. Ferraro, F. J. Qu, B. R. Guachalla, E. Schaan,et al., Precision kinematic sunyaev–zel’dovich measurements across halo mass and redshift with desi dr2 and act dr6: Part ii. bright galaxy survey and emission-line galax- ies (2026), arXiv:https://arxiv.org/abs/26XX.XXXX in prep, arXiv:26XX.XXXX [astro-ph.CO]

    2026

  42. [44]

    Abareshi, J

    DESI Collaboration, B. Abareshi, J. Aguilar, S. Ahlen, S. Alam, D. M. Alexander, R. Alfarsy, L. Allen, C. Allende Prieto, O. Alves, J. Ameel, E. Armen- gaud, J. Asorey, A. Aviles, S. Bailey, A. Balaguera- Antol´ ınez, O. Ballester, C. Baltay, A. Bault, S. F. Bel- tran, B. Benavides, S. BenZvi, A. Berti, R. Besuner, F. Beutler, D. Bianchi, C. Blake, P. Bla...

    work page arXiv 2022

  43. [45]

    T. N. Miller, P. Doel, G. Gutierrez, R. Besuner, D. Brooks, G. Gallo, H. Heetderks, P. Jelinsky, S. M. Kent, M. Lampton, M. E. Levi, M. Liang, A. Meis- ner, M. J. Sholl, J. H. Silber, D. Sprayberry, J. N. Aguilar, A. de la Macorra, D. Eisenstein, K. Fanning, A. Font-Ribera, E. Gazta˜ naga, S. Gontcho A Gontcho, K. Honscheid, J. Jimenez, D. Joyce, R. Kehoe...

    work page arXiv 2024

  44. [46]

    Poppett, L

    C. Poppett, L. Tyas, J. Aguilar, C. Bebek, D. Bra- mall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heet- derks, P. Jelinsky, S. Jelinsky, R. Lafever, A. Lam- bert, M. Lampton, M. E. Levi, P. Martini, C. Rock- osi, J. Schmoll, R. M. Sharples, M. Sirk, E. Wishnow, J. Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, A. Dey, P. Doel...

    2024

  45. [47]

    The DESI Experiment Part II: Instrument Design

    DESI Collaboration, A. Aghamousa, J. Aguilar, S. Ahlen, S. Alam, L. E. Allen, C. Allende Prieto, 37 J. Annis, S. Bailey, C. Balland, O. Ballester, C. Baltay, L. Beaufore, C. Bebek, T. C. Beers, E. F. Bell, J. L. Bernal, R. Besuner, F. Beutler, C. Blake, H. Bleuler, M. Blomqvist, R. Blum, A. S. Bolton, C. Briceno, D. Brooks, J. R. Brownstein, E. Buckley-Ge...

    work page Pith review arXiv 2016

  46. [48]

    J. Guy, S. Bailey, A. Kremin, S. Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Ma- corra, A. Dey, B. Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gazta˜ naga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner...

    work page arXiv 2023

  47. [49]

    E. F. Schlafly, D. Kirkby, D. J. Schlegel, A. D. Myers, A. Raichoor, K. Dawson, J. Aguilar, C. Al- lende Prieto, S. Bailey, S. BenZvi, J. Bermejo-Climent, D. Brooks, A. de la Macorra, A. Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, J. Garc´ ıa-Bellido, S. Gontcho A Gontcho, J. Guy, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Ke- hoe, ...

    work page arXiv 2023

  48. [50]

    Data Release 1 of the Dark Energy Spectroscopic Instrument

    DESI Collaboration, M. Abdul-Karim, A. G. Adame, D. Aguado, J. Aguilar, S. Ahlen, S. Alam, G. Aldering, D. M. Alexander, R. Alfarsy, L. Allen, C. Allende Prieto, O. Alves, A. Anand, U. Andrade, E. Armengaud, S. Avila, A. Aviles, H. Awan, S. Bailey, A. Baleato Lizancos, O. Ballester, A. Bault, J. Bautista, S. BenZvi, L. Beraldo e Silva, J. R. Bermejo-Clime...

    work page internal anchor Pith review arXiv 2025

  49. [51]

    DESI Collaboration, A. G. Adame, J. Aguilar, S. Ahlen, S. Alam, D. M. Alexander, C. Allende Prieto, M. Al- varez, O. Alves, A. Anand, U. Andrade, E. Armengaud, S. Avila, A. Aviles, H. Awan, B. Bahr-Kalus, S. Bailey, C. Baltay, A. Bault, J. Behera, S. BenZvi, F. Beut- ler, D. Bianchi, C. Blake, R. Blum, M. Bonici, S. Brieden, A. Brodzeller, D. Brooks, E. B...

    work page arXiv 2024

  50. [52]

    Adame, J

    A. Adame, J. Aguilar, S. Ahlen, S. Alam, D. Alexander, M. Alvarez, O. Alves, A. Anand, U. Andrade, E. Armen- gaud, S. Avila, A. Aviles, H. Awan, S. Bailey, C. Baltay, A. Bault, J. Behera, S. BenZvi, F. Beutler, D. Bianchi, C. Blake, R. Blum, S. Brieden, A. Brodzeller, D. Brooks, E. Buckley-Geer, E. Burtin, R. Calderon, R. Can- ning, A. Carnero Rosell, R. ...

    2024

  51. [53]

    DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints

    M. Abdul Karim, J. Aguilar, S. Ahlen, S. Alam, L. Allen, C. A. Prieto, O. Alves, A. Anand, U. Andrade, E. Ar- mengaud, A. Aviles, S. Bailey, C. Baltay, P. Bansal, A. Bault, J. Behera, S. BenZvi, D. Bianchi, C. Blake, S. Brieden, A. Brodzeller, D. Brooks, E. Buckley-Geer, E. Burtin, R. Calderon, R. Canning, A. C. Rosell, P. Carrilho, L. Casas, F. J. Castan...

    work page internal anchor Pith review arXiv 2025

  52. [54]

    S. Yuan, H. Zhang, A. J. Ross, J. Donald-McCann, B. Hadzhiyska, R. H. Wechsler, Z. Zheng, S. Alam, V. Gonzalez-Perez, J. N. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, A. de la Macorra, K. Fanning, J. E. Forero-Romero, K. Honscheid, M. Ishak, R. Kehoe, J. Lasker, M. Landriau, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, J. A. New...

    work page arXiv 2023

  53. [55]

    R. Zhou, B. Dey, J. A. Newman, D. J. Eisenstein, K. Dawson, S. Bailey, A. Berti, J. Guy, T.-W. Lan, H. Zou, J. Aguilar, S. Ahlen, S. Alam, D. Brooks, A. de la Macorra, A. Dey, G. Dhungana, K. Fan- ning, A. Font-Ribera, S. G. A. Gontcho, K. Honscheid, M. Ishak, T. Kisner, A. Kov´ acs, A. Kremin, M. Lan- driau, M. E. Levi, C. Magneville, M. Manera, P. Marti...

    work page arXiv 2023

  54. [56]

    DESI Collaboration, A. G. Adame, J. Aguilar, et al., Validation of the scientific program for the dark energy spectroscopic instrument, AJ167, 62 (2024), arXiv:https://arxiv.org/abs/2306.06307 arXiv:2306.06307 [astro-ph.CO]

    work page arXiv 2024

  55. [57]

    A. J. Ross, J. Aguilar, S. Ahlen, S. Alam, A. Anand, S. Bailey, D. Bianchi, S. Brieden, D. Brooks, E. Burtin, A. C. Rosell, E. Chaussidon, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, B. Dey, P. Doel, K. Fanning, S. Ferraro, J. Ereza, A. Font-Ribera, J. E. Forero-Romero, E. Gazta˜ naga, H. Gil-Mar´ ın, S. G. A. Gontcho, A. X. ...

    work page arXiv 2024

  56. [58]

    Andrade, E

    U. Andrade, E. Paillas, J. Mena-Fern´ andez, Q. Li, A. J. Ross, S. Nadathur, M. Rashkovetskyi, A. P´ erez- Fern´ andez, H. Seo, N. Sanders, O. Alves, X. Chen, N. Deiosso, A. de Mattia, M. White, M. Abdul- Karim, S. Ahlen, E. Armengaud, A. Aviles, D. Bianchi, S. Brieden, A. Brodzeller, D. Brooks, E. Burtin, R. Calderon, R. Canning, A. C. Rosell, L. Casas, ...

    work page arXiv 2025

  57. [59]

    Abdul Karimet al.[DESI], Phys

    M. Abdul Karim and DESI, Desi dr2 results. ii. measure- ments of baryon acoustic oscillations and cosmological constraints, Physical Review D112, 10.1103/tr6y-kpc6 (2025)

    work page doi:10.1103/tr6y-kpc6 2025

  58. [60]

    R. Zhou, B. Dey, J. A. Newman, D. J. Eisenstein, K. Dawson, S. Bailey, A. Berti, J. Guy, T.-W. Lan, H. Zou, J. Aguilar, S. Ahlen, S. Alam, D. Brooks, A. de la Macorra, A. Dey, G. Dhungana, K. Fan- ning, A. Font-Ribera, S. G. A. Gontcho, K. Honscheid, M. Ishak, T. Kisner, A. Kov´ acs, A. Kremin, M. Lan- driau, M. E. Levi, C. Magneville, M. Manera, P. Marti...

    2023

  59. [61]

    Bundy, A

    K. Bundy, A. Leauthaud, S. Saito, A. Bolton, Y.-T. Lin, C. Maraston, R. C. Nichol, D. P. Schneider, D. Thomas, and D. A. Wake, The stripe 82 massive galaxy project. i. catalog construction, The Astrophysical Journal Supple- ment Series221, 15 (2015)

    2015

  60. [62]

    A. V. Kravtsov, A. A. Vikhlinin, and A. V. Meshch- eryakov, Stellar mass—halo mass relation and star for- mation efficiency in high-mass halos, Astronomy Letters 44, 8–34 (2018)

    2018

  61. [63]

    A. R. Duffy, J. Schaye, S. T. Kay, and C. Dalla Vec- chia, Dark matter halo concentrations in the wilkinson microwave anisotropy probe year 5 cosmology, Monthly Notices of the Royal Astronomical Society: Letters390, L64 (2008)

    2008

  62. [64]

    R. J. Thornton, P. A. R. Ade, S. Aiola, F. E. Angil` e, M. Amiri, J. A. Beall, D. T. Becker, H.-M. Cho, S. K. Choi, P. Corlies, K. P. Coughlin, R. Datta, M. J. De- vlin, S. R. Dicker, R. D¨ unner, J. W. Fowler, A. E. Fox, P. A. Gallardo, J. Gao, E. Grace, M. Halpern, M. Hasselfield, S. W. Henderson, G. C. Hilton, A. D. Hincks, S. P. Ho, J. Hubmayr, K. D. ...

    work page arXiv 2016

  63. [65]

    J., et al

    S. Naess, Y. Guan, A. J. Duivenvoorden, M. Hasselfield, and Y. W. et al, The atacama cosmology telescope: DR6 maps (2025), arXiv:https://arxiv.org/abs/2503.14451 arXiv:2503.14451 [astro-ph.CO]

    work page arXiv 2025

  64. [66]

    Hilton, C

    M. Hilton, C. Sif´ on, S. Naess, M. Madhavacheril, M. Oguri, E. Rozo, E. Rykoff, T. M. C. Abbott, S. Ad- hikari, M. Aguena, S. Aiola, S. Allam, S. Amodeo, A. Amon, J. Annis, B. Ansarinejad, C. Aros-Bunster, J. E. Austermann, S. Avila, D. Bacon, N. Battaglia, J. A. Beall, D. T. Becker, G. M. Bernstein, E. Bertin, T. Bhan- darkar, S. Bhargava, J. R. Bond, D...

    work page arXiv 2021

  65. [67]

    J. P. Ostriker and E. T. Vishniac, Generation of Mi- crowave Background Fluctuations from Nonlinear Per- turbations at the ERA of Galaxy Formation, ApJL306, L51 (1986)

    1986

  66. [69]

    Ried Guachalla, E

    B. Ried Guachalla, E. Schaan, B. Hadzhiyska, and S. Fer- raro, Velocity reconstruction in the era of desi and ru- bin/lsst. i. exploring spectroscopic, photometric, and hy- brid samples, Phys. Rev. D109, 103533 (2024)

    2024

  67. [70]

    Nusser and M

    A. Nusser and M. Davis, On the Prediction of Velocity Fields from Redshift Space Galaxy Samples, ApJL 421, L1 (1994), arXiv:https://arxiv.org/abs/astro- ph/9309009 arXiv:astro-ph/9309009 [astro-ph]

    work page arXiv 1994

  68. [71]

    Paillas, Z

    E. Paillas, Z. Ding, X. Chen, H. Seo, N. Pad- manabhan, A. de Mattia, A. Ross, S. Nadathur, C. Howlett, J. Aguilar, S. Ahlen, O. Alves, U. An- drade, D. Brooks, E. Buckley-Geer, E. Burtin, S. Chen, T. Claybaugh, S. Cole, K. Dawson, A. de la Ma- corra, A. Dey, P. Doel, K. Fanning, S. Ferraro, J. Forero-Romero, C. Garcia-Quintero, E. Gazta˜ naga, H. Gil-Mar...

    2024

  69. [72]

    X. Chen, Z. Ding, E. Paillas, S. Nadathur, H. Seo, S. Chen, N. Padmanabhan, M. White, A. de Mat- tia, P. McDonald, A. J. Ross, A. Variu, A. C. Rosell, B. Hadzhiyska, M. M. S. Hanif, D. Forero- S´ anchez, S. Ahlen, O. Alves, U. Andrade, S. Ben- Zvi, D. Bianchi, D. Brooks, E. Chaussidon, T. Clay- baugh, A. de la Macorra, B. Dey, K. Fanning, S. Fer- raro, A....

    work page arXiv 2024

  70. [73]

    Hadzhiyska, S

    B. Hadzhiyska, S. Ferraro, B. Ried Guachalla, and E. Schaan, Velocity reconstruction in the era of desi and rubin/lsst. ii. realistic samples on the light cone, Phys. Rev. D109, 103534 (2024)

    2024

  71. [74]

    Baleato Lizancos, U

    A. Baleato Lizancos, U. Seljak, M. Karamanis, M. Bonici, and S. Ferraro, Selecting samples of galaxies with fewer fingers-of-god, Journal of Cosmology and Astroparticle Physics2025(07), 014

  72. [75]

    Alonso, J

    D. Alonso, J. Sanchez, and A. Slosar, A unified pseudo-c framework, Monthly Notices of the Royal Astronomical Society484, 4127 (2019)

    2019

  73. [76]

    Bollietet al., arXiv e-prints arXiv:2310.18482 (2023)

    B. Bollietet al., class sz I: Overview, EPJ Web Conf.293, 00008 (2024), arXiv:https://arxiv.org/abs/2310.18482 arXiv:2310.18482 [astro-ph.IM]

    work page arXiv 2024

  74. [77]

    Ma and J

    C.-P. Ma and J. N. Fry, Nonlinear kinetic sunyaev- zeldovich effect, Phys. Rev. Lett.88, 211301 (2002)

    2002

  75. [78]

    McQuinn, S

    M. McQuinn, S. R. Furlanetto, L. Hernquist, O. Zahn, and M. Zaldarriaga, The kinetic sunyaevzeldovich effect from reionization, The Astrophysical Journal630, 643 (2005)

    2005

  76. [79]

    H. Park, E. Komatsu, P. R. Shapiro, J. Koda, and Y. Mao, The impact of nonlinear structure formation on the power spectrum of transverse momentum fluctuations and the kinetic sunyaev–zeldovich effect, The Astrophys- ical Journal818, 37 (2016)

    2016

  77. [80]

    Sunseri, A

    J. Sunseri, A. Amon, J. Dunkley, N. Battaglia, S. Fer- raro, B. Hadzhiyska, B. R. Guachalla, and E. Schaan, Disentangling the halo: Joint model for measurements of the kinetic sunyaev-zeldovich effect and galaxy-galaxy lensing (2025), arXiv:https://arxiv.org/abs/2505.20413 arXiv:2505.20413 [astro-ph.CO]

    work page arXiv 2025

  78. [81]

    Battaglia, The tau of galaxy clusters, Journal of Cos- mology and Astroparticle Physics2016(08), 058

    N. Battaglia, The tau of galaxy clusters, Journal of Cos- mology and Astroparticle Physics2016(08), 058

  79. [82]

    Knox, Determination of inflationary observables by cosmic microwave background anisotropy experiments, Physical Review D52, 4307–4318 (1995)

    L. Knox, Determination of inflationary observables by cosmic microwave background anisotropy experiments, Physical Review D52, 4307–4318 (1995)

    1995

  80. [83]

    Torrado and A

    J. Torrado and A. Lewis, Cobaya: code for bayesian anal- ysis of hierarchical physical models, Journal of Cosmol- ogy and Astroparticle Physics2021(05), 057

Showing first 80 references.