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arxiv: 2605.15444 · v1 · pith:5GGEKKBPnew · submitted 2026-05-14 · 🌌 astro-ph.CO · astro-ph.GA

Clusters Hiding Under Millimeter Sources (CHUMS) I: Extreme CHUMS

Harshda Saxena , Adam B. Mantz , Jack Sayers , Denise G. Yudovich , Steve W. Allen This is my paper

Pith reviewed 2026-05-19 14:46 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords galaxy clustersSunyaev-Zeldovich effectactive galactic nucleimillimeter surveyscosmology
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The pith

Subtracting central AGN emission from millimeter maps reveals previously hidden galaxy clusters.

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

This paper shows that bright emission from active galactic nuclei in the centers of galaxy clusters can mask the Sunyaev-Zeldovich signal in millimeter surveys, turning potential detections into non-detections. By using targeted observations at 30 and 90 GHz to measure the AGN flux and subtract it from wider survey maps at 90 GHz, the cluster signals become detectable at high significance. This approach matters because cluster counts constrain the expansion history and structure growth in the universe, and missing clusters due to contamination can bias those constraints. The work demonstrates the method on three specific clusters and finds that the AGN emission varies little over time, supporting the subtraction across different observation epochs.

Core claim

For three galaxy clusters whose central AGN emission overwhelms the SZ signal at 90 GHz, leading to non-detections in the ACT survey, measurements of the AGN with CARMA at 30 and 90 GHz allow subtraction of that contaminating signal from the ACT maps, resulting in high SNR detections of the clusters. Pressure profiles from X-ray data are used to estimate the AGN contribution at 150 GHz. Low variability in the AGN emission across observation epochs supports the validity of the subtraction.

What carries the argument

AGN flux subtraction from CARMA 30 and 90 GHz measurements applied to ACT survey maps to recover the underlying SZ cluster signal.

If this is right

  • Recovered high-SNR detections allow these clusters to be added to cosmological samples.
  • Improved completeness reduces biases in cluster abundance statistics used for cosmology.
  • Low AGN variability justifies time-asynchronous subtraction in future analyses.
  • Modeling AGN contamination becomes essential for accurate SZ survey results.

Where Pith is reading between the lines

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

  • This technique may help recover clusters in other ongoing mm-wave surveys.
  • Future large surveys could incorporate routine AGN flux monitoring to avoid missing objects.
  • The method highlights the need for multi-wavelength data to fully exploit SZ cluster catalogs for precision cosmology.

Load-bearing premise

The AGN emission level measured at one time with CARMA remains stable enough to subtract accurately from ACT maps taken at different times.

What would settle it

Observing the AGN flux at 90 GHz at the same time as the ACT data and finding a significantly different value than used in the subtraction, or finding no cluster signal after subtraction.

Figures

Figures reproduced from arXiv: 2605.15444 by Adam B. Mantz, Denise G. Yudovich, Harshda Saxena, Jack Sayers, Steve W. Allen.

Figure 1
Figure 1. Figure 1: Left: CARMA data for long-baselines (≥ 3kλ) for MACS0242, dominated by AGN emission. Middle : CARMA short-baseline (≤ 3kλ) data for MACS0242. Right: Residual CARMA short-baseline map, after subtracting the AGN emission and revealing the SZ decrement from the cluster. 40.91° 40.78° 40.64° 40.51° 40.38° RA (J2000) -21.79° -21.67° -21.55° -21.42° -21.30° Dec (J2000) 40.91° 40.78° 40.64° 40.51° 40.38° RA (J200… view at source ↗
Figure 2
Figure 2. Figure 2: Left: ACT 98 GHz map at the position of MACS0242. Right: ACT map after subtraction of the AGN emission, revealing the SZ decrement from the cluster. then fit a Gaussian profile to this residual and adopt the resulting best-fit flux density as our measurement of the 150 GHz AGN emission. For MACS0242, the flux density obtained after cluster subtraction is 55.8 ± 6.8 mJy, fully consistent with the extrapolat… view at source ↗
Figure 3
Figure 3. Figure 3: Histograms in blue show the SNR distribution from mock observations of the cluster SZ signal based on the X-ray-derived pressure profile plus the bright central AGN, with the actual SNR from the location of the cluster shown in the red line. Histograms in purple show the SNR distribution from mock observations that include only the SZ signal (i.e., no central AGN), with the actual SNR from the location of … view at source ↗
Figure 4
Figure 4. Figure 4: SED fits in blue to the flux densities of the AGN cores in the CGs of MACS0242 and RXJ0439 using Eqn. 1, with black points corresponding to previous measurements from the literature, and red stars corresponding to our measurements, including those obtained at 150 GHz from the ACT data based on subtracting an X-ray-derived model of the SZ signal. We note that for some archival points we do not have measurem… view at source ↗
Figure 5
Figure 5. Figure 5: Lightcurves of the AGN cores within the CGs of MACS0242 and RXJ0439, spanning our observations from April 2012 - October 2013 and October 2011-October2013 respectively. uncertainties, and so there is no statistically significant evidence for variability. This behavior is in agreement with the findings of M. T. Hogan et al. (2015), who similarly report a lack of strong variability for this source between Ap… view at source ↗
Figure 6
Figure 6. Figure 6: 1.5 GHz emission from Hercules A, at the center of RXJ1615, as observed by R. Timmerman et al. (2022). We overlay 10σ, 30σ and 100σ (30 GHz only) contours from our CLEAN maps of the CARMA data at 30 and 90 GHz in red and cyan respectively. We also add elliptical dashed patches showing the synthesized beam at 30 and 90 GHz in red and cyan respectively in the bottom corners. surement, we instead follow the a… view at source ↗
read the original abstract

Galaxy cluster abundance provides a powerful probe of the $\Lambda$CDM model and enables precise constraints on cosmological parameters. Millimeter-wavelength surveys detect clusters through the Sunyaev-Zeldovich (SZ) effect, and are particularly effective at high redshifts. However, the SZ signal can be significantly contaminated by emission from Active Galactic Nuclei (AGN), particularly AGN within the Central Galaxies (CGs). This contamination reduces the SZ signal strength at the frequencies most accessible from the ground, which reduces detection significances or converts cluster detections to non-detections, thereby diminishing survey completeness and introducing biases in cosmological analyses. In this work, we analyze three clusters that host bright AGN in their CGs using 30 and 90 GHz observations from the Combined Array for Research in Millimeter-wave Astronomy (CARMA). In each case the AGN emission overwhelms the cluster SZ signal, resulting in non-detections in the Atacama Cosmology Telescope (ACT) survey. We present signal to noise ratio (SNR) estimates for the clusters after subtracting the AGN signal from 90 GHz ACT maps using the CARMA measurements, demonstrating high SNR cluster detections once this contaminating emission is removed. Using cluster pressure profiles derived from Chandra X-ray data, we subtract the expected SZ signal from the 150 GHz ACT maps to estimate the flux density of the AGN in that band. Leveraging the time-asynchronous CARMA observations, we also assess temporal variability in the AGN emission, and find low fractional variability for our sample. Finally, we discuss the importance of modeling and mitigating AGN contamination in SZ cluster surveys.

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

3 major / 2 minor

Summary. The paper analyzes three galaxy clusters with bright central AGN that appear as non-detections in ACT SZ surveys. Using CARMA 30/90 GHz data, the authors subtract the AGN contribution from 90 GHz ACT maps to recover high-SNR SZ signals. They employ Chandra-derived pressure profiles to estimate AGN flux at 150 GHz and use time-asynchronous CARMA observations to report low fractional variability in the AGN emission, arguing that AGN contamination can be mitigated to improve cluster detection completeness.

Significance. If the cross-epoch subtraction holds, the result demonstrates a viable path to recover clusters hidden by central AGN, directly addressing completeness and bias issues in millimeter SZ surveys used for cosmology. The multi-wavelength approach combining CARMA, ACT, and X-ray data is a strength, as is the explicit variability check; however, the absence of quantitative error budgets and simulation validation limits the immediate impact on survey pipelines.

major comments (3)
  1. [Abstract / variability assessment] Abstract and variability assessment section: the central claim of high-SNR cluster detections after CARMA subtraction from ACT 90 GHz maps assumes that single-epoch CARMA AGN fluxes can be subtracted from maps taken at different times. The reported low fractional variability does not include a quantitative bound showing that the maximum epoch-to-epoch flux difference is smaller than the SZ amplitude or post-subtraction noise, leaving the recovered SNR vulnerable to unaccounted residuals from variability, spectral-index mismatch, or beam differences.
  2. [Method / results] Method and results sections: no error budget, Monte Carlo propagation, or simulation validation is presented for the subtracted maps. Uncertainties in CARMA flux, ACT beam/response, and the X-ray-derived 150 GHz AGN estimate are not folded into the final SNR values, which is load-bearing for the claim that the clusters are now detected at high significance.
  3. [Sample / introduction] Sample description: explicit selection criteria for the three clusters and any completeness or bias assessment relative to the parent ACT sample are not provided, making it difficult to assess how representative the recovered detections are for broader survey corrections.
minor comments (2)
  1. Notation for frequencies (30 GHz, 90 GHz, 150 GHz) and instruments should be standardized in all figure captions and equations for clarity.
  2. Add references to prior works on AGN contamination in SZ surveys (e.g., recent ACT or SPT analyses) to better contextualize the novelty of the CHUMS approach.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful reading and valuable comments, which have helped us improve the manuscript. We address each major comment below and plan to incorporate revisions accordingly.

read point-by-point responses

  1. Referee: Abstract and variability assessment section: the central claim of high-SNR cluster detections after CARMA subtraction from ACT 90 GHz maps assumes that single-epoch CARMA AGN fluxes can be subtracted from maps taken at different times. The reported low fractional variability does not include a quantitative bound showing that the maximum epoch-to-epoch flux difference is smaller than the SZ amplitude or post-subtraction noise, leaving the recovered SNR vulnerable to unaccounted residuals from variability, spectral-index mismatch, or beam differences.

    Authors: We thank the referee for highlighting this important point. While we report low fractional variability based on the asynchronous CARMA observations, we agree that a quantitative assessment relative to the SZ signal and noise is necessary to fully support the subtraction validity. In the revised manuscript, we will add a calculation comparing the observed flux variations to the expected SZ decrement and the map noise levels, demonstrating that variability-induced residuals are negligible compared to the recovered signals. revision: yes

  2. Referee: Method and results sections: no error budget, Monte Carlo propagation, or simulation validation is presented for the subtracted maps. Uncertainties in CARMA flux, ACT beam/response, and the X-ray-derived 150 GHz AGN estimate are not folded into the final SNR values, which is load-bearing for the claim that the clusters are now detected at high significance.

    Authors: We acknowledge the lack of a detailed error budget in the current version. To address this, we will include an expanded methods section with a full error propagation analysis. This will involve Monte Carlo simulations that incorporate uncertainties from the CARMA flux measurements, assumptions in the ACT beam and response functions, and the extrapolation of the AGN flux from the Chandra-derived pressure profiles to 150 GHz. The resulting uncertainties will be reflected in the reported SNR values for the subtracted maps. revision: yes

  3. Referee: Sample description: explicit selection criteria for the three clusters and any completeness or bias assessment relative to the parent ACT sample are not provided, making it difficult to assess how representative the recovered detections are for broader survey corrections.

    Authors: The three clusters were chosen as illustrative examples of systems where bright central AGN lead to non-detections in the ACT SZ survey, identified through cross-correlation with X-ray observations. We recognize that explicit criteria and a discussion of representativeness would improve the paper. In the revision, we will add a dedicated subsection in the introduction or methods detailing the selection process and noting the limitations in generalizing to the full ACT sample, as this work focuses on demonstrating the mitigation technique rather than providing a complete statistical correction. revision: yes

Circularity Check

0 steps flagged

No circularity: data-driven subtraction using independent multi-epoch and X-ray observations

full rationale

The paper's central results are SNR estimates obtained by direct subtraction of measured CARMA AGN fluxes from ACT 90 GHz maps, with AGN flux at 150 GHz estimated via independent Chandra-derived pressure profiles. Variability is quantified from the time-asynchronous CARMA data themselves without any fitted parameter being redefined as a prediction. No equations, self-citations, or ansatzes reduce the claimed detections to the inputs by construction. The analysis is externally benchmarked against X-ray and millimeter data and does not invoke uniqueness theorems or rename known results.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard assumptions from SZ and X-ray cluster literature (thermal pressure profiles, negligible non-thermal pressure, point-source subtraction validity) plus the observational premise that CARMA and ACT epochs can be aligned despite time separation. No new free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption X-ray derived pressure profiles accurately predict the SZ signal at 150 GHz for subtraction purposes
    Invoked when estimating AGN flux density from 150 GHz ACT maps after removing expected cluster contribution.
  • domain assumption AGN emission is dominated by a compact source whose flux can be measured and subtracted as a point source at 90 GHz
    Central to the CARMA-based subtraction step that produces the high-SNR cluster detections.

pith-pipeline@v0.9.0 · 5841 in / 1590 out tokens · 76803 ms · 2026-05-19T14:46:47.230748+00:00 · methodology

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Works this paper leans on

79 extracted references · 79 canonical work pages · 4 internal anchors

  1. [1]

    Abbott, T. M. C., Aguena, M., Alarcon, A., et al. 2020, PhRvD, 102, 023509, doi: 10.1103/PhysRevD.102.023509

    work page doi:10.1103/physrevd.102.023509 2020

  2. [2]

    Ade, P. A. R., Aghanim, N., Armitage-Caplan, C., et al. 2014, Astronomy & Astrophysics, 571, A8, doi: 10.1051/0004-6361/201321538 10 T able 3.List of targets with details of the archival CARMA data Cluster T rack ID Obs. date (mm/dd/yy) On time (mins) F req. (GHz) Flux cal. RXJ0439 c0769Z.4SH 30RXJ043.2 08/23/11 75 34.9 Mars RXJ0439 c0769Z.4SH 30RXJ04...

    work page doi:10.1051/0004-6361/201321538 2014

  3. [3]

    The Open Journal of Astrophysics , keywords =

    Aguena, M., Aiola, S., Allam, S., et al. 2026, The Open Journal of Astrophysics, 9, 55863, doi: 10.33232/001c.155863

    work page doi:10.33232/001c.155863 2026

  4. [4]

    2017, Astronomy & Astrophysics, 607, A122, doi: 10.1051/0004-6361/201630311

    Akrami, Y., Ashdown, M., Aumont, J., et al. 2017, Astronomy & Astrophysics, 607, A122, doi: 10.1051/0004-6361/201630311

    work page doi:10.1051/0004-6361/201630311 2017

  5. [5]

    W., Evrard A

    Allen, S. W., Evrard, A. E., & Mantz, A. B. 2011, ARA&A, 49, 409, doi: 10.1146/annurev-astro-081710-102514

    work page doi:10.1146/annurev-astro-081710-102514 2011

  6. [6]

    Mignone and Jonathan C

    Allen, S. W., Rapetti, D. A., Schmidt, R. W., et al. 2007, Monthly Notices of the Royal Astronomical Society, 383, 879–896, doi: 10.1111/j.1365-2966.2007.12610.x

    work page doi:10.1111/j.1365-2966.2007.12610.x 2007

  7. [7]

    M., Papadakis I

    Allen, S. W., Schmidt, R. W., Ebeling, H., Fabian, A. C., & van Speybroeck, L. 2004, Monthly Notices of the Royal Astronomical Society, 353, 457–467, doi: 10.1111/j.1365-2966.2004.08080.x

    work page doi:10.1111/j.1365-2966.2004.08080.x 2004

  8. [8]

    W., Piffaretti, R., et al

    Arnaud, M., Pratt, G. W., Piffaretti, R., et al. 2010, A&A, 517, A92, doi: 10.1051/0004-6361/200913416

    work page doi:10.1051/0004-6361/200913416 2010

  9. [9]

    E., et al., 2015, @doi [ ] 10.1088/0067-0049/216/2/27 , https://ui.adsabs.harvard.edu/abs/2015ApJS..216...27B 216, 27

    Bleem, L. E., Stalder, B., de Haan, T., et al. 2015, ApJS, 216, 27, doi: 10.1088/0067-0049/216/2/27

    work page doi:10.1088/0067-0049/216/2/27 2015

  10. [10]

    E., Klein, M., Abbot, T

    Bleem, L. E., Klein, M., Abbot, T. M. C., et al. 2024, The Open Journal of Astrophysics, 7, doi: 10.21105/astro.2311.07512

    work page doi:10.21105/astro.2311.07512 2024

  11. [11]

    E., et al

    Bocquet, S., Grandis, S., Bleem, L. E., et al. 2024, PhRvD, 110, 083510, doi: 10.1103/PhysRevD.110.083510

    work page doi:10.1103/physrevd.110.083510 2024

  12. [12]

    2012, New Journal of Physics, 14, 025010, doi: 10.1088/1367-2630/14/2/025010

    Bonamente, M., Hasler, N., Bulbul, E., et al. 2012, New Journal of Physics, 14, 025010, doi: 10.1088/1367-2630/14/2/025010

    work page doi:10.1088/1367-2630/14/2/025010 2012

  13. [13]

    The first catalog of galaxy clusters and groups in the Western Galactic Hemisphere

    Bulbul, E., Liu, A., Kluge, M., et al. 2024, A&A, 685, A106, doi: 10.1051/0004-6361/202348264 B¨ ohringer, H., Schuecker, P., Guzzo, L., et al. 2004, Astronomy & Astrophysics, 425, 367–383, doi: 10.1051/0004-6361:20034484

    work page doi:10.1051/0004-6361/202348264 2024

  14. [14]

    E., Holder G

    Carlstrom, J. E., Holder, G. P., & Reese, E. D. 2002, Annual Review of Astronomy and Astrophysics, 40, 643–680, doi: 10.1146/annurev.astro.40.060401.093803

    work page doi:10.1146/annurev.astro.40.060401.093803 2002

  15. [15]

    arXiv , author =:2007.07289 , journal =

    Choi, S. K., Hasselfield, M., Ho, S.-P. P., et al. 2020, Journal of Cosmology and Astroparticle Physics, 2020, 045–045, doi: 10.1088/1475-7516/2020/12/045

    work page doi:10.1088/1475-7516/2020/12/045 2020

  16. [16]

    E., et al

    Coble, K., Bonamente, M., Carlstrom, J. E., et al. 2007, The Astronomical Journal, 134, 897, doi: 10.1086/519973

    work page doi:10.1086/519973 2007

  17. [17]

    Abitbol et al.,The Simons Observatory: Science Goals and Forecasts for the Enhanced Large Aperture Telescope, arXiv:2503.00636

    Collaboration, S. O., Abitbol, M., Abril-Cabezas, I., et al. 2025, https://arxiv.org/abs/2503.00636

    work page arXiv 2025

  18. [18]

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package

    Collaboration, T. A., Price-Whelan, A. M., Lim, P. L., et al. 2022, The Astrophysical Journal, 935, 167, doi: 10.3847/1538-4357/ac7c74

    work page internal anchor Pith review doi:10.3847/1538-4357/ac7c74 2022

  19. [19]

    , keywords =

    Condon, J. J., Cotton, W. D., Greisen, E. W., et al. 1998, AJ, 115, 1693, doi: 10.1086/300337

    work page doi:10.1086/300337 1998

  20. [20]

    J., & Dressel, L

    Condon, J. J., & Dressel, L. L. 1978, ApJ, 221, 456, doi: 10.1086/156047 DES Collaboration, Abbott, T. M. C., Aguena, M., et al. 2025, arXiv e-prints, arXiv:2503.13632, doi: 10.48550/arXiv.2503.13632 Dupourqu´ e, S., Clerc, N., Pointecouteau, E., et al. 2024, Astronomy & Astrophysics, 687, A58, doi: 10.1051/0004-6361/202348701

    work page doi:10.1086/156047 1978

  21. [21]

    A., De Marco O., Barlow M

    Ebeling, H., Edge, A. C., Bohringer, H., et al. 1998, MNRAS, 301, 881, doi: 10.1046/j.1365-8711.1998.01949.x

    work page doi:10.1046/j.1365-8711.1998.01949.x 1998

  22. [22]

    C., & Henry, J

    Ebeling, H., Edge, A. C., & Henry, J. P. 2001, ApJ, 553, 668, doi: 10.1086/320958

    work page doi:10.1086/320958 2001

  23. [23]

    J., Reeves J

    Ebeling, H., Edge, A. C., Mantz, A., et al. 2010, Monthly Notices of the Royal Astronomical Society, 407, 83–93, doi: 10.1111/j.1365-2966.2010.16920.x

    work page doi:10.1111/j.1365-2966.2010.16920.x 2010

  24. [24]

    2019, A&A, 621, A40, doi: 10.1051/0004-6361/201833324

    Eckert, D., Ghirardini, V., Ettori, S., et al. 2019, A&A, 621, A40, doi: 10.1051/0004-6361/201833324

    work page doi:10.1051/0004-6361/201833324 2019

  25. [25]

    Fabian, A. C. 2012, ARA&A, 50, 455, doi: 10.1146/annurev-astro-081811-125521

    work page internal anchor Pith review doi:10.1146/annurev-astro-081811-125521 2012

  26. [26]

    C., Iwasawa, K., Reynolds, C

    Fabian, A. C., Iwasawa, K., Reynolds, C. S., & Young, A. J. 2000, PASP, 112, 1145, doi: 10.1086/316610

    work page doi:10.1086/316610 2000

  27. [27]

    Jiang, F

    Fabian, A. C., Sanders, J. S., Allen, S. W., et al. 2003, Mon. Not. Roy. Astron. Soc., 344, L43, doi: 10.1046/j.1365-8711.2003.06902.x

    work page doi:10.1046/j.1365-8711.2003.06902.x 2003

  28. [28]

    2005, The Astrophysical Journal, 635, 894, doi: 10.1086/429746

    Forman, W., Nulsen, P., Heinz, S., et al. 2005, The Astrophysical Journal, 635, 894, doi: 10.1086/429746

    work page doi:10.1086/429746 2005

  29. [29]

    2007, ApJ, 665, 1057, doi: 10.1086/519480

    Forman, W., Jones, C., Churazov, E., et al. 2007, The Astrophysical Journal, 665, 1057, doi: 10.1086/519480

    work page doi:10.1086/519480 2007

  30. [30]

    2024, Astronomy & Astrophysics, 689, A298, doi: 10.1051/0004-6361/202348852

    Ghirardini, V., Bulbul, E., Artis, E., et al. 2024, Astronomy & Astrophysics, 689, A298, doi: 10.1051/0004-6361/202348852

    work page doi:10.1051/0004-6361/202348852 2024

  31. [31]

    B., Crichton, D., Marriage, T

    Gralla, M. B., Crichton, D., Marriage, T. A., et al. 2014, Monthly Notices of the Royal Astronomical Society, 445, 460–478, doi: 10.1093/mnras/stu1592

    work page doi:10.1093/mnras/stu1592 2014

  32. [32]

    R., & Wright, A

    Griffith, M. R., & Wright, A. E. 1993, AJ, 105, 1666, doi: 10.1086/116545

    work page doi:10.1086/116545 1993

  33. [33]

    J., et al

    Gupta, N., Saro, A., Mohr, J. J., et al. 2017, MNRAS, 467, 3737, doi: 10.1093/mnras/stx095

    work page doi:10.1093/mnras/stx095 2017

  34. [34]

    T., Ogilvie G

    Hardcastle, M. J., & Looney, L. W. 2008, MNRAS, 388, 176, doi: 10.1111/j.1365-2966.2008.13370.x

    work page doi:10.1111/j.1365-2966.2008.13370.x 2008

  35. [35]

    Hart, B. C. 2008, https://arxiv.org/abs/0801.4093

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  36. [36]

    E., Romani, R

    Healey, S. E., Romani, R. W., Taylor, G. B., et al. 2007, ApJS, 171, 61, doi: 10.1086/513742

    work page doi:10.1086/513742 2007

  37. [37]

    2024, MNRAS, 528, 7274, doi: 10.1093/mnras/stae208

    Heinrich, A., Zhuravleva, I., Zhang, C., et al. 2024, MNRAS, 528, 7274, doi: 10.1093/mnras/stae208

    work page doi:10.1093/mnras/stae208 2024

  38. [38]

    2021, ApJS, 253, 3, doi: 10.3847/1538-4365/abd023

    Hilton, M., Sif´ on, C., Naess, S., et al. 2021, ApJS, 253, 3, doi: 10.3847/1538-4365/abd023 Hitomi Collaboration, Aharonian, F., Akamatsu, H., et al. 2016, Nature, 535, 117, doi: 10.1038/nature18627 12

    work page doi:10.3847/1538-4365/abd023 2021

  39. [39]

    Hogan, M. T. 2012, Monthly Notices of the Royal Astronomical Society, 424, 224–231, doi: 10.1111/j.1365-2966.2012.21187.x

    work page doi:10.1111/j.1365-2966.2012.21187.x 2012

  40. [40]

    T., Edge, A

    Hogan, M. T., Edge, A. C., Geach, J. E., et al. 2015, MNRAS, 453, 1223, doi: 10.1093/mnras/stv1518 H¨ ogbom, J. A. 1974, A&AS, 15, 417

    work page doi:10.1093/mnras/stv1518 2015

  41. [41]

    Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90, doi: 10.1109/MCSE.2007.55

    work page doi:10.1109/mcse.2007.55 2007

  42. [42]

    A., Chandler, C

    Lacy, M., Baum, S. A., Chandler, C. J., et al. 2020, PASP, 132, 035001, doi: 10.1088/1538-3873/ab63eb

    work page doi:10.1088/1538-3873/ab63eb 2020

  43. [43]

    F., Marulli, F., Moscardini, L., et al

    Lesci, G. F., Marulli, F., Moscardini, L., et al. 2022, Astronomy & Astrophysics, 659, A88, doi: 10.1051/0004-6361/202040194

    work page doi:10.1051/0004-6361/202040194 2022

  44. [44]

    F., Veropalumbo, A., Sereno, M., et al

    Lesci, G. F., Veropalumbo, A., Sereno, M., et al. 2023, A&A, 674, A80, doi: 10.1051/0004-6361/202346261

    work page doi:10.1051/0004-6361/202346261 2023

  45. [45]

    P., & Ziegler, B

    Maier, C., Haines, C. P., & Ziegler, B. L. 2022, A&A, 658, A190, doi: 10.1051/0004-6361/202141498

    work page doi:10.1051/0004-6361/202141498 2022

  46. [46]

    Mantz, A. B. 2019, MNRAS, 485, 4863, doi: 10.1093/mnras/stz320

    work page doi:10.1093/mnras/stz320 2019

  47. [47]

    B., Allen, S

    Mantz, A. B., Allen, S. W., Morris, R. G., & Schmidt, R. W. 2016, Monthly Notices of the Royal Astronomical Society, 456, 4020–4039, doi: 10.1093/mnras/stv2899

    work page doi:10.1093/mnras/stv2899 2016

  48. [48]

    B., von der Linden, A., Allen, S

    Mantz, A. B., von der Linden, A., Allen, S. W., et al. 2015, MNRAS, 446, 2205, doi: 10.1093/mnras/stu2096

    work page doi:10.1093/mnras/stu2096 2015

  49. [49]

    2021, Astronomy & Astrophysics, 647, A104, doi: 10.1051/0004-6361/202037788 Mart´ ınez-Ram´ ırez, L

    Maris, M., Romelli, E., Tomasi, M., et al. 2021, Astronomy & Astrophysics, 647, A104, doi: 10.1051/0004-6361/202037788 Mart´ ınez-Ram´ ırez, L. N., Rivera, G. C., Lusso, E., et al. 2024, https://arxiv.org/abs/2405.12111

    work page doi:10.1051/0004-6361/202037788 2021

  50. [50]

    R., Nulsen P

    McNamara, B. R., & Nulsen, P. E. J. 2012, New Journal of Physics, 14, 055023, doi: 10.1088/1367-2630/14/5/055023

    work page doi:10.1088/1367-2630/14/5/055023 2012

  51. [51]

    R., et al., 2000, @doi [ ] 10.1086/312662 , http://adsabs.harvard.edu/abs/2000ApJ...534L.135M 534, L135

    McNamara, B. R., Wise, M., Nulsen, P. E. J., et al. 2000, The Astrophysical Journal, 534, L135, doi: 10.1086/312662

    work page doi:10.1086/312662 2000

  52. [52]

    G., & Delabrouille, J

    Melin, J.-B., Bartlett, J. G., & Delabrouille, J. 2005, Astron. Astrophys., 429, 417, doi: 10.1051/0004-6361:20048093

    work page doi:10.1051/0004-6361:20048093 2005

  53. [53]

    2020, ApJ, 901, 131, doi: 10.3847/1538-4357/abb08d

    Mo, W., Gonzalez, A., Brodwin, M., et al. 2020, ApJ, 901, 131, doi: 10.3847/1538-4357/abb08d

    work page doi:10.3847/1538-4357/abb08d 2020

  54. [54]

    E., et al

    Muchovej, S., Mroczkowski, T., Carlstrom, J. E., et al. 2007, The Astrophysical Journal, 663, 708, doi: 10.1086/511971

    work page doi:10.1086/511971 2007

  55. [55]

    R., 2009, @doi [ ] 10.1111/j.1365-2966.2009.15167.x , http://adsabs.harvard.edu/abs/2009MNRAS.398..607V 398, 607

    Murphy, T., Sadler, E. M., Ekers, R. D., et al. 2010, MNRAS, 402, 2403, doi: 10.1111/j.1365-2966.2009.15961.x

    work page doi:10.1111/j.1365-2966.2009.15961.x 2010

  56. [56]

    TheAtacamaCosmologyTelescope: DR6 Maps

    Naess, S., Guan, Y., Duivenvoorden, A. J., et al. 2025, https://arxiv.org/abs/2503.14451

    work page arXiv 2025

  57. [57]

    V., & Vikhlinin, A

    Nagai, D., Kravtsov, A. V., & Vikhlinin, A. 2007, ApJ, 668, 1, doi: 10.1086/521328

    work page doi:10.1086/521328 2007

  58. [58]

    B., Sebastian, B., Seth, R., & Raychaudhury, S

    Pandge, M. B., Sebastian, B., Seth, R., & Raychaudhury, S. 2021, Monthly Notices of the Royal Astronomical Society, 504, 1644, doi: 10.1093/mnras/stab384

    work page doi:10.1093/mnras/stab384 2021

  59. [59]

    J., Shepherd, M

    Pearson, T. J., Shepherd, M. C., Taylor, G. B., & Myers, S. T. 1994, in American Astronomical Society Meeting

    work page 1994

  60. [60]

    , keywords =

    Piotrowska, J. M., Bluck, A. F. L., Maiolino, R., & Peng, Y. 2021, Monthly Notices of the Royal Astronomical Society, 512, 1052, doi: 10.1093/mnras/stab3673 Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2016a, A&A, 594, A24, doi: 10.1051/0004-6361/201525833 Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2016b, A&A, 594, A27, doi: 10.1...

    work page doi:10.1093/mnras/stab3673 2021

  61. [61]

    2026, https://arxiv.org/abs/2603.20163 Rodr´ ıguez-Pascual, P

    Quan, W., Camphuis, E., Daley, C., et al. 2026, https://arxiv.org/abs/2603.20163 Rodr´ ıguez-Pascual, P. M., Alloin, D., Clavel, J., et al. 1997, ApJS, 110, 9, doi: 10.1086/312996

    work page doi:10.1086/312996 2026

  62. [62]

    S., et al., 2014, @doi [ ] 10.1088/0004-637X/785/2/104 , http://adsabs.harvard.edu/abs/2014ApJ...785..104R 785, 104

    Rykoff, E. S., Rozo, E., Busha, M. T., et al. 2014, ApJ, 785, 104, doi: 10.1088/0004-637X/785/2/104

    work page doi:10.1088/0004-637x/785/2/104 2014

  63. [63]

    S., et al., 2016, @doi [ ] 10.3847/0067-0049/224/1/1 , https://ui.adsabs.harvard.edu/abs/2016ApJS..224....1R 224, 1

    Rykoff, E. S., Rozo, E., Hollowood, D., et al. 2016, ApJS, 224, 1, doi: 10.3847/0067-0049/224/1/1

    work page doi:10.3847/0067-0049/224/1/1 2016

  64. [64]

    A retrospective view of Miriad

    Sault, R. J., Teuben, P. J., & Wright, M. C. H. 1995, in Astronomical Society of the Pacific Conference Series, Vol. 77, Astronomical Data Analysis Software and Systems IV, ed. R. A. Shaw, H. E. Payne, & J. J. E. Hayes, 433, doi: 10.48550/arXiv.astro-ph/0612759

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0612759 1995

  65. [65]

    2025, Astronomy & Astrophysics, 700, A128, doi: 10.1051/0004-6361/202555719

    Saxena, H., Sayers, J., Gavidia, A., et al. 2025, Astronomy & Astrophysics, 700, A128, doi: 10.1051/0004-6361/202555719

    work page doi:10.1051/0004-6361/202555719 2025

  66. [66]

    G., et al

    Sayers, J., Mroczkowski, T., Czakon, N. G., et al. 2013, ApJ, 764, 152, doi: 10.1088/0004-637X/764/2/152

    work page doi:10.1088/0004-637x/764/2/152 2013

  67. [67]

    Somerville, R

    Schaye, J., Crain, R. A., Bower, R. G., et al. 2015, MNRAS, 446, 521, doi: 10.1093/mnras/stu2058

    work page doi:10.1093/mnras/stu2058 2015

  68. [68]

    2022, The Astronomical Journal, 163, 146, doi: 10.3847/1538-3881/ac5030

    Somboonpanyakul, T., McDonald, M., Noble, A., et al. 2022, The Astronomical Journal, 163, 146, doi: 10.3847/1538-3881/ac5030

    work page doi:10.3847/1538-3881/ac5030 2022

  69. [69]

    J., Callingham, J

    Timmerman, R., van Weeren, R. J., Callingham, J. R., et al. 2022, A&A, 658, A5, doi: 10.1051/0004-6361/202140880

    work page doi:10.1051/0004-6361/202140880 2022

  70. [70]

    J., & de Kool, M

    Tingay, S. J., & de Kool, M. 2003, AJ, 126, 723, doi: 10.1086/376600 13

    work page doi:10.1086/376600 2003

  71. [71]

    W., et al

    Vazza, F., Angelinelli, M., Jones, T. W., et al. 2018, MNRAS, 481, L120, doi: 10.1093/mnrasl/sly172

    work page doi:10.1093/mnrasl/sly172 2018

  72. [72]

    Oliphant, Matt Haberland, Tyler Reddy, David Cournapeau, Evgeni Burovski, Pearu Peterson, Warren Weckesser, Jonathan Bright, St´ efan J

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261, doi: 10.1038/s41592-019-0686-2 von der Linden, A., Mantz, A., Allen, S. W., et al. 2014, Monthly Notices of the Royal Astronomical Society, 443, 1973–1978, doi: 10.1093/mnras/stu1423

    work page doi:10.1038/s41592-019-0686-2 2020

  73. [73]

    2018, Space Science Reviews, 215, doi: 10.1007/s11214-018-0571-9

    Scannapieco, E. 2018, Space Science Reviews, 215, doi: 10.1007/s11214-018-0571-9

    work page doi:10.1007/s11214-018-0571-9 2018

  74. [74]

    P., Oguri, M., Ramos-Ceja, M

    Willis, J. P., Oguri, M., Ramos-Ceja, M. E., et al. 2021, Monthly Notices of the Royal Astronomical Society, 503, 5624, doi: 10.1093/mnras/stab873

    work page doi:10.1093/mnras/stab873 2021

  75. [75]

    2022, MNRAS, 515, 4471, doi: 10.1093/mnras/stac2048

    Wu, H.-Y., Costanzi, M., To, C.-H., et al. 2022, MNRAS, 515, 4471, doi: 10.1093/mnras/stac2048

    work page doi:10.1093/mnras/stac2048 2022

  76. [76]

    W., Mantz, A., & Werner, N

    Zhuravleva, I., Allen, S. W., Mantz, A., & Werner, N. 2018, ApJ, 865, 53, doi: 10.3847/1538-4357/aadae3

    work page doi:10.3847/1538-4357/aadae3 2018

  77. [77]

    C., Churazov, E., et al

    Zhuravleva, I., Chen, M. C., Churazov, E., et al. 2023, MNRAS, 520, 5157, doi: 10.1093/mnras/stad470

    work page doi:10.1093/mnras/stad470 2023

  78. [78]

    A., et al

    Zhuravleva, I., Churazov, E., Schekochihin, A. A., et al. 2014, Nature, 515, 85, doi: 10.1038/nature13830

    work page doi:10.1038/nature13830 2014

  79. [79]

    2019, Monthly Notices of the Royal Astronomical Society, 489, 401–419, doi: 10.1093/mnras/stz2153

    Zubeldia, I., & Challinor, A. 2019, Monthly Notices of the Royal Astronomical Society, 489, 401–419, doi: 10.1093/mnras/stz2153

    work page doi:10.1093/mnras/stz2153 2019