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arxiv: 2607.01175 · v1 · pith:NM7DBVGJnew · submitted 2026-07-01 · 🌌 astro-ph.CO · astro-ph.GA

Galaxy Clusters Selected via the Sunyaev-Zel'dovich Effect in 5 year data from the SPT-3G Main Survey

L. E. Bleem , M. Klein , K. Kornoelje , S. Bocquet , J. A. Sobrin , M. Aguena , E. Anderes , A. J. Anderson
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F. Andrade-Oliveira B. Ansarinejad M. Archipley L. Balkenhol D. R. Barron P. S. Barry M. Bayliss K. Benabed A. N. Bender B. A. Benson F. Bianchini F. R. Bouchet D. Brooks D. L. Burke M. Calzadilla R. Camilleri E. Camphuis M. G. Campitiello J. E. Carlstrom A. Carnero Rosell J. Carretero J. Carron C. L. Chang P. M. Chichura A. Chokshi T.-L. Chou A. Coerver M. Costanzi T. M. Crawford L. N. da Costa C. Daley T. M. Davis T. de Haan J. De Vicente S. Desai K. R. Dibert H. T. Diehl M. A. Dobbs M. Doohan D. Dutcher S. Everett G. Evrard C. Feng K. R. Ferguson N. C. Ferree K. Fichman B. Flaugher B. Floyd K. Fosdick A. Foster S. Galli A. E. Gambrel A. K. Gao J. Garc\'ia-Bellido F. Ge M. D. Gladders S. Grandis F. Guidi S. Guns G. Gutierrez N. W. Halverson S. R. Hinton E. Hivon G. P. Holder D. L. Hollowood W. L. Holzapfel J. C. Hood A. Hryciuk N. Huang T. Jhaveri S. Kent F. K\'eruzor\'e A. R. Khalife G. Khullar L. Knox K. Kuehn C.-L. Kuo O. Lahav K. Levy Y. Li A. E. Lowitz C. Lu G. P. Lynch T. J. Maccarone G. Mahler A. S. Maniyar J. L. Marshall E. S. Martsen M. McDonald J. Mena-Fern\'andez F. Menanteau M. Millea R. Miquel J. J. Mohr J. Montgomery J. Myles Y. Nakato T. Natoli R. C. Nichol V. Novosad R. L. C. Ogando Y. Omori A. Ouellette Z. Pan K. A. Phadke A. A. Plazas Malag\'on A. W. Pollak A. Porredon K. Prabhu J. Prat W. Quan S. Raghunathan M. Rahimi A. Rahlin C. L. Reichardt A. K. Romer M. Rouble J. E. Ruhl E. Sanchez D. Sanchez Cid T. Schrabback I. Sevilla-Noarbe A. C. Silva Oliveira A. Simpson T. Somboonpanyakul A. A. Stark E. Suchyta M. E. C. Swanson C. Tandoi C. To C. Trendafilova J. D. Vieira A. G. Vieregg V. Vikram A. Vitrier Y. Wan N. Weaverdyck J. Weller N. Whitehorn W. L. K. Wu M. R. Young J. A. Zebrowski J. Zhan
This is my paper

Pith reviewed 2026-07-02 06:17 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords galaxy clustersSunyaev-Zel'dovich effectSPT-3Gcluster cataloghigh-redshift clusterscosmology
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The pith

The paper presents a catalog of 7190 confirmed galaxy clusters selected via the Sunyaev-Zel'dovich effect from five years of SPT-3G observations.

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

This work constructs a new sample of galaxy clusters by detecting their thermal imprint on the cosmic microwave background in high-resolution millimeter-wave maps. The resulting catalog reaches lower masses and higher redshifts than earlier SZ surveys while maintaining high purity after optical and infrared confirmation. Such a large, uniformly selected sample supports statistical studies of cluster abundance, mass calibration, and evolution across cosmic time. The data also enable direct comparisons with X-ray observations from eROSITA and internal tests for astrophysical contaminants.

Core claim

The central claim is a catalog of 8892 SZ cluster candidates above detection significance ξ=4 (expected purity >82 percent), with 7190 confirmed as real clusters; the sample covers masses 7.9×10^13 to 1.6×10^15 solar masses per h70 and redshifts 0.037 to roughly 2, achieving a surface density of 4.5 confirmed clusters per square degree and 2-4 times higher per-cluster signal-to-noise than prior SPT or ACT catalogs.

What carries the argument

Detection of the thermal Sunyaev-Zel'dovich effect, which produces a frequency-dependent temperature decrement in the cosmic microwave background proportional to the integrated electron pressure along the line of sight through a cluster.

If this is right

  • The catalog contains 1780 clusters above redshift 1 and 271 above redshift 1.5, extending the reach of SZ selection into the epoch when clusters first assembled.
  • Cross-matches yield 1279 clusters in common with the eRASS1 X-ray catalog, with mass estimates in relatively good agreement.
  • Validation tests reveal a seventeen-fold increase in 220 GHz emission for clusters at z approximately 1.5 compared with z approximately 0.25, indicating stronger correlated dusty emission at higher redshift.
  • A subset of clusters is identified as candidate strong gravitational lenses for follow-up study.

Where Pith is reading between the lines

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

  • The higher cluster density and improved mass reach could tighten cosmological constraints on structure growth when combined with weak-lensing or velocity-dispersion mass calibration.
  • The redshift-dependent dusty emission trend suggests that multi-frequency modeling will become increasingly important for SZ surveys targeting z greater than 1.
  • The flagged lens candidates provide a ready target list for high-resolution imaging to measure cluster masses independently of the SZ signal.

Load-bearing premise

Optical and infrared imaging reliably distinguishes true clusters from false detections across the full redshift range, especially above redshift 1.

What would settle it

Finding that the number of clusters confirmed at z greater than 1.5 falls well below the expected count from the purity estimates, or that SPT and eROSITA mass estimates show large systematic offsets for the same objects.

Figures

Figures reproduced from arXiv: 2607.01175 by A. A. Plazas Malag\'on, A. A. Stark, A. Carnero Rosell, A. Chokshi, A. Coerver, A. C. Silva Oliveira, A. E. Gambrel, A. E. Lowitz, A. Foster, A. G. Vieregg, A. Hryciuk, A. J. Anderson, A. K. Gao, A. K. Romer, A. N. Bender, A. Ouellette, A. Porredon, A. Rahlin, A. R. Khalife, A. Simpson, A. S. Maniyar, A. Vitrier, A. W. Pollak, B. A. Benson, B. Ansarinejad, B. Flaugher, B. Floyd, C. Daley, C. Feng, C. L. Chang, C.-L. Kuo, C. L. Reichardt, C. Lu, C. Tandoi, C. To, C. Trendafilova, D. Brooks, D. Dutcher, D. L. Burke, D. L. Hollowood, D. R. Barron, D. Sanchez Cid, E. Anderes, E. Camphuis, E. Hivon, E. Sanchez, E. S. Martsen, E. Suchyta, F. Andrade-Oliveira, F. Bianchini, F. Ge, F. Guidi, F. K\'eruzor\'e, F. Menanteau, F. R. Bouchet, G. Evrard, G. Gutierrez, G. Khullar, G. Mahler, G. P. Holder, G. P. Lynch, H. T. Diehl, I. Sevilla-Noarbe, J. A. Sobrin, J. A. Zebrowski, J. Carretero, J. Carron, J. C. Hood, J. De Vicente, J. D. Vieira, J. E. Carlstrom, J. E. Ruhl, J. Garc\'ia-Bellido, J. J. Mohr, J. L. Marshall, J. Mena-Fern\'andez, J. Montgomery, J. Myles, J. Prat, J. Weller, J. Zhan, K. A. Phadke, K. Benabed, K. Fichman, K. Fosdick, K. Kornoelje, K. Kuehn, K. Levy, K. Prabhu, K. R. Dibert, K. R. Ferguson, L. Balkenhol, L. E. Bleem, L. Knox, L. N. da Costa, M. A. Dobbs, M. Aguena, M. Archipley, M. Bayliss, M. Calzadilla, M. Costanzi, M. D. Gladders, M. Doohan, M. E. C. Swanson, M. G. Campitiello, M. Klein, M. McDonald, M. Millea, M. Rahimi, M. Rouble, M. R. Young, N. C. Ferree, N. Huang, N. Weaverdyck, N. W. Halverson, N. Whitehorn, O. Lahav, P. M. Chichura, P. S. Barry, R. Camilleri, R. C. Nichol, R. L. C. Ogando, R. Miquel, S. Bocquet, S. Desai, S. Everett, S. Galli, S. Grandis, S. Guns, S. Kent, S. Raghunathan, S. R. Hinton, T. de Haan, T. Jhaveri, T. J. Maccarone, T.-L. Chou, T. M. Crawford, T. M. Davis, T. Natoli, T. Schrabback, T. Somboonpanyakul, V. Novosad, V. Vikram, W. L. Holzapfel, W. L. K. Wu, W. Quan, Y. Li, Y. Nakato, Y. Omori, Y. Wan, Z. Pan.

Figure 1
Figure 1. Figure 1: — Footprint of the SPT-3G survey plotted with those of several other multi-wavelength surveys discussed in this work. The footprints are overlaid on a dust map from Planck Collaboration et al. (2016a). The full SPT-3G 10,000 deg2 survey is shown in pale blue, the boundaries of the SPT-Euclid Deep field South (Archipley et al. 2026) and SPT 100d Deep field (Kornoelje et al. 2026) are white-dashed, and the S… view at source ↗
Figure 2
Figure 2. Figure 2: — (Left) Cutout of 3o × 6.5 o of SPT-3G Main field survey data (approximately 1.2% of the Main field survey area). The rgb image is constructed using the 95 (red), 150 GHz (green), and 220 (blue) GHz data with peak-to-peak fluctuations in each channel of ±110µKCMB. This figure illustrates the main constituents of the SPT-3G temperature maps. As the maps are calibrated in µKCMB units, CMB fluctuations have … view at source ↗
Figure 3
Figure 3. Figure 3: — Distribution of cluster sample properties in terms of detection significance, ξ, (top) and corresponding filter scales (bot￾tom). In orange we show the full sample and, over-plotted in blue, the clusters confirmed by the optical analysis as discussed in Sec. 4. In the top panel we also highlight several massive well-known clusters in the SPT footprint. The distribution in θc of the pre￾dominately low-ξ u… view at source ↗
Figure 4
Figure 4. Figure 4: — Top: The expected purity (orange) and number of false detections (green) for the SPT-3G Main field cluster catalog as a function of minimum ξ without additional optical follow-up. We find an expected purity of 82% above ξmin = 4, and 99% above ξmin = 5. Bottom: The expected purity of the cluster sample as a function of filter core size, θc. Here the label “Peak Core Size” reflects that the simulated clus… view at source ↗
Figure 5
Figure 5. Figure 5: — MCMF richness λ vs. redshift for the SPT-3G candi￾date list at ξ > 4. In solid lines we overplot the richness confirma￾tion thresholds of fmax cont =0.2 for the LS-DR10 and WISE datasets. In blue we plot clusters confirmed by MCMF in the sample, in black we mark clusters confirmed using other datasets (see Sec. 4.5.), and in gray SPT candidates with optical associations below our confirmation threshold. … view at source ↗
Figure 6
Figure 6. Figure 6: — SPT-CL J2128.4−5658.0, a ξ = 10 cluster at z ≳ 1.6 confirmed using the combination of WISE and Magellan/FourStar data. The 3′ diameter rgb image is constructed from FourStar/J￾band and LS-DR10 z- and r-band data; SZ detection countours are overlaid on the image. solved for by SCAMP (Bertin 2006) based on source po￾sitions extracted using SExtractor (Bertin & Arnouts 1996). Images are then resampled and r… view at source ↗
Figure 7
Figure 7. Figure 7: — DECam imaging of SPT-3G clusters from the LS-DR10 release (Dey et al. 2019) with SZ detection contours overlaid. The rgb images were created from z−, r−, g−band data and are 3. ′8 in diameter. Clusters were selected to illustrate the SZ significance and redshift reach of the sample. The highest-redshift clusters were confirmed with additional observations from Spitzer, FourStar (Sec. 4.3), and WISE. scal… view at source ↗
Figure 8
Figure 8. Figure 8: — Redshift distribution of the 7,190 confirmed clusters in the SPT-3G Main field sample confirmed using optical-IR data as discussed in Sec. 4. As noted in Sec. 4.5, owing to color degeneracies in the IR, we assign clusters with redshifts estimated at z > 1.6 using the 1.6 µm bump method to a value of z = 1.6 in the catalog table, but we use their raw best-fit redshifts in the histogram here to illustrate … view at source ↗
Figure 9
Figure 9. Figure 9: — Parameters of the SZ and richness observable-mass relations assuming a fixed reference cosmology (68% and 95% credibility). Gold contours show an analysis of the cluster counts where we model the sample selection in detection significance ξ and redshift z (we fix σln ζ = 0.2 in this case as shown by the dashed line). Blue contours show an analysis of the cluster counts where we model the sample selection… view at source ↗
Figure 10
Figure 10. Figure 10: — Distribution of the (ξ > 5, 0.25 < z < 1) subsample of SPT-3G clusters in the space of SPT significance and optical richness. The straight line shows the mean model and contours show the expected distribution. We find 27 out of 3,005 clusters outside of the 99% contour, in line with the expectation. Clusters whose richness estimates are likely to be affected by masking are shown with gray crosses and ar… view at source ↗
Figure 11
Figure 11. Figure 11: — The mass-redshift distribution of the five-year SPT-3G Main field sample compared to other recent large ICM-selected cluster samples, including those from ACT (ACTDESHSC Collaboration et al. 2026), eROSITA (Bulbul et al. 2024), Planck (Planck Collaboration et al. 2016b), and previously published samples from the SPT-SZ, SPTpol, and SPT-3G collaborations (Bleem et al. 2015, 2020, 2024; Klein et al. 2024b… view at source ↗
Figure 12
Figure 12. Figure 12: — Estimated completeness of the SPT-3G Main cluster sample above ξ = 4 at several different redshifts. As discussed in Sec. 6, the sample has a declining mass threshold as a function of redshift. The sample is expected to be > 90% complete for masses M500c ≳ 2 × 1014 M⊙/h70 at z > 0.25. SPT-3G cluster sample using DECALS and archival SPT follow-up data. We additionally flag potential lenses in Sec. 10.1.1… view at source ↗
Figure 13
Figure 13. Figure 13: — Redshift-scaled (Sec. 5) SPT detection significance, ξ, vs. X-ray mass for clusters at z > 0.25 in the eRASS1 cosmol￾ogy sample (Bulbul et al. 2024). In bold we plot eRASS1 clusters that have counterparts within the SPT-3G catalog (89%), while in pale gray we plot force-photometered ξ values for clusters with￾out matches; note that the y-axis scaling transitions from log to linear below the SPT detectio… view at source ↗
Figure 14
Figure 14. Figure 14: — Optical richness vs. SZ-inferred mass for the subset of 1,909 clusters at 0.2 < z < 0.95 found in all four (SPT-3G, redMaPPer Y3, MaDCoWS2, and WH24) cluster samples. MCMF, our baseline confirmation method (Sec. 4) shows the smallest scatter with SZ mass, followed by the redMaPPer sample. The WH24 sample, while having large scatter, is the most complete (∼ 78%) of the external catalogs. peaking in the s… view at source ↗
Figure 15
Figure 15. Figure 15: — [PITH_FULL_IMAGE:figures/full_fig_p030_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: — Redshift evolution of the median correlated 220 GHz emission at SPT-3G cluster locations; this emission increases by over an order of magnitude over the redshift range probed by the SPT sample (0.25 < z ≲ 2), while the median Compton-y value in each bin is comparable. As above, the region z > 1.6 is shaded to denote higher redshift uncertainties; the plotted redshifts in each bin are the median of the b… view at source ↗
read the original abstract

We report a new galaxy cluster catalog, selected using the thermal Sunyaev-Zel'dovich (SZ) effect, from 5 years of observations of the SPT-3G Main field. Drawn from arcminute-resolution data with white noise levels of 3.2, 2.5, and 8.9 $\mu$K-arcmin at 95, 150, and 220 GHz, respectively, the sample consists of 8,892 cluster candidates detected above significance $\xi=4$, with an expected purity of $>82\%$ (4,480 at $\xi\ge5$ with purity $>99\%$). Using optical and infrared data we have confirmed 7,190 candidates as clusters. The sample spans a mass range $7.9 \times 10^{13}$ $M_\odot/h_{70}$ \ $< M_\textrm{500c} < $ $1.6 \times 10^{15}$ $M_\odot/h_{70}$ with a median mass of $1.65 \times 10^{14}$ $M_\odot/h_{70}$, and a redshift range of $0.037<z\lesssim 2$ with a median redshift of $z_{\textrm{med}}$ = 0.73; 1,780 clusters are at $z>1$ and 271 at $z>1.5$. Compared to previous SZ cluster samples from South Pole Telescope and Atacama Cosmology Telescope data, the SPT-3G sample is highly consistent in mass and redshift but is significantly deeper, with per-cluster detection signal-to-noise 2-4 times higher and a cluster density of 4.5 confirmed clusters/deg$^2$. We cross match with eRASS1 cluster and point source catalogs, finding 1,279 and 1,319 matches, respectively. The SPT and eROSITA cluster mass estimates are in relatively good agreement. We perform a series of validation checks using both internal data splits and comparisons to external samples. These tests show increasing correlated (dusty) emission with redshift, with a $\sim17\times$ larger 220 GHz temperature increment for clusters at $z\sim1.5$ than $z\sim0.25$, but only weak evidence for correlated synchrotron emission. Finally, a number of clusters are flagged as candidate strong gravitational lenses.

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

0 major / 3 minor

Summary. The manuscript reports a new SZ-selected galaxy cluster catalog from 5 years of SPT-3G Main Survey observations. It contains 8,892 candidates detected at ξ ≥ 4 (expected purity >82%) and 4,480 at ξ ≥ 5 (purity >99%), with 7,190 confirmed as clusters via optical and infrared data. The sample spans 7.9×10^13 M⊙/h70 < M500c < 1.6×10^15 M⊙/h70 (median 1.65×10^14 M⊙/h70) and 0.037 < z ≲ 2 (median z=0.73), including 1,780 clusters at z>1. It includes cross-matches with eRASS1 (1,279 clusters, 1,319 point sources), internal validation splits, and notes on redshift-dependent dusty emission.

Significance. If the reported purities and confirmations hold, this catalog is a substantial advance over prior SPT and ACT SZ samples due to its greater depth, 2-4× higher per-cluster S/N, and cluster density of 4.5 confirmed clusters/deg². The large high-redshift subsample and eRASS1 cross-matches support improved cosmological constraints and studies of cluster astrophysics at z>1. The validation checks using data splits and external comparisons add credibility to the catalog's utility.

minor comments (3)
  1. The abstract and text use ξ for detection significance without an explicit definition or reference to its construction in the methods section; adding a brief equation or citation to prior SPT papers would improve clarity for readers.
  2. Mass and redshift ranges are reported with h70 and M500c; ensure consistent notation and units are used throughout all tables and figures.
  3. The statement on increasing correlated dusty emission (∼17× larger 220 GHz increment at z∼1.5 vs z∼0.25) is presented without an accompanying figure or table quantifying the trend; a supplemental plot would strengthen the validation section.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript and their recommendation to accept. We are pleased that the referee finds the catalog to be a substantial advance and that the validation checks add credibility.

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

This is an observational catalog paper reporting counts of SZ-selected cluster candidates, confirmation statistics via optical/IR data, mass/redshift ranges, and validation checks against external catalogs. No equations, fitted parameters, or self-citation chains are invoked to derive the headline numbers; the reported quantities are direct outputs of the detection and confirmation pipeline rather than predictions that reduce to inputs by construction. The paper is self-contained against external benchmarks with no load-bearing self-referential steps.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on the SZ detection pipeline and optical/IR confirmation, which rely on standard field assumptions rather than new derivations or invented entities.

free parameters (2)
  • significance threshold ξ=4
    Chosen to achieve stated purity of >82%; value is a selection cut.
  • purity estimates from simulations
    Expected purity values are simulation-derived and affect the reported sample.
axioms (2)
  • domain assumption The thermal SZ effect dominates the detected signal in galaxy clusters
    Standard assumption invoked for all SZ cluster selection.
  • domain assumption Optical and infrared data provide reliable cluster confirmation
    Directly invoked to convert candidates to confirmed clusters.

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