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REVIEW 2 major objections 5 minor 297 references

A probabilistic matching of optical groups to eROSITA X-ray contours recovers low-mass systems more completely than red-sequence methods while letting purity be set by the user.

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2026-07-12 07:35 UTC pith:OXGLADOA

load-bearing objection Solid multi-wavelength catalog paper that carefully maps purity–completeness trade-offs for S-PLUS + eRASS1 groups and shows PZWav+AME recovers more low-mass systems than identically matched redMaPPer. the 2 major comments →

arxiv 2607.02706 v1 pith:OXGLADOA submitted 2026-07-02 astro-ph.CO

S-PLUS Clusters And Large-scale Environments (SCALE): II. PZWav versus redMaPPer identification of eRosita groups

L. Doubrawa , A. Finoguenov , E. S. Cypriano , C. Mendes de Oliveira , E. V. Lima , L. Nakazono , G. Souza , J. Comparat
show 5 more authors
A. Gonzalez R. Demarco A. Kanaan T. Ribeiro W. Schoenell
This is my paper
classification astro-ph.CO
keywords galaxy clustersgalaxy groupseROSITAS-PLUScluster findersX-ray luminosity functionphotometric redshiftsmulti-wavelength catalogs
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper builds multi-wavelength catalogs of galaxy groups and clusters by linking S-PLUS optical overdensities (found with PZWav and membership-weighted by AME) to extended X-ray contours from eRASS1. Matching uses a probabilistic form of the modified Hausdorff distance that folds in photometric-redshift probability distributions and can be tuned for purity levels of 80–95 percent. Fainter absolute-magnitude cuts recover more low-mass, low-luminosity groups; brighter cuts favor massive clusters and enlarge the surveyed volume at higher redshift. The resulting X-ray luminosity functions match earlier determinations, the logN–logS distributions show high recovery of luminous systems, and a side-by-side comparison with an identically matched redMaPPer sample confirms that the PZWav+AME route is more complete at the group scale because it retains blue galaxies. The catalogs are released so that cosmological and galaxy-evolution studies can trade purity against completeness in a controlled way.

Core claim

Probabilistic modified-Hausdorff matching of PZWav+AME optical systems to eRASS1 X-ray contours yields multi-wavelength catalogs whose X-ray luminosity functions agree with prior work and that recover low-mass groups more completely than an identically matched redMaPPer sample, while giving explicit control of purity (80–95 %) versus completeness.

What carries the argument

The probabilistic modified Hausdorff distance that associates X-ray surface-brightness contours with galaxy membership probabilities drawn from photometric-redshift PDFs; purity is defined as one minus the ratio of random (RA-shifted) to real matches and is sampled over a grid of membership thresholds and contour-coverage fractions.

Load-bearing premise

The claim that shifting every optical system by ten degrees in right ascension produces a random catalog free of residual large-scale-structure bias, so that the quoted purity levels truly measure chance superpositions.

What would settle it

Recompute the purity fractions with an independent randomization (for example, random sky rotations or mock light-cones that preserve clustering) and check whether the X-ray luminosity functions and group recovery fractions remain unchanged within the quoted uncertainties.

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

If this is right

  • Users can select magnitude cut and purity level to optimize a catalog for either group-scale galaxy evolution or high-mass cosmological probes.
  • Inclusion of blue members systematically raises completeness below ~10^43 erg s^{-1} relative to red-sequence finders.
  • The released eSCALE and eRedMaPPer catalogs supply a ready multi-wavelength sample for weak-lensing mass calibration and environmental studies inside the S-PLUS footprint.
  • Deeper eROSITA releases can reuse the same matching pipeline without redesign.

Where Pith is reading between the lines

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

  • The same purity-tunable Hausdorff machinery could be applied to any photometric survey that supplies galaxy PDFs, not only S-PLUS.
  • If residual large-scale-structure bias in the RA-shift randoms is non-negligible, the true purity of the lowest-luminosity bins may be lower than reported, affecting cosmological number counts.
  • Combining PZWav and redMaPPer memberships before matching may yield a still more complete group catalog without sacrificing the purity dial.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The paper constructs multi-wavelength group/cluster catalogs by probabilistically matching PZWav+AME optical systems from S-PLUS (0.08<z<0.25) to eRASS1 extended X-ray contours via a modified Hausdorff-distance framework that incorporates photometric-redshift PDFs and membership probabilities. It systematically varies absolute-magnitude cuts (Mr < −18.5 to −20) and purity thresholds (80–95 %), quantifies the resulting completeness–purity trade-offs, derives purity-corrected X-ray luminosity functions and logN–logS distributions that agree with COSMOS/RASS benchmarks, and shows that the same matching applied to redMaPPer yields consistent high-mass trends while PZWav+AME recovers more low-mass, blue-member systems.

Significance. If the purity control and XLF agreement hold, the work supplies a practical, tunable multi-wavelength catalog (eSCALE) and a reusable matching pipeline for eROSITA–optical studies of groups, where AGN feedback is expected to be most efficient. Strengths include explicit random-catalog purity definition, purity-corrected XLFs, dual matching of an independent redMaPPer sample, and appendices testing full versus cleaned luminosities and an independent Klein-style random-superposition cut. The catalogs are released at CDS, supporting immediate follow-up.

major comments (2)
  1. Section 3 defines purity as 1 − N_random/N_real from a +10° RA-shifted catalog and states that residual clustering enhancement is only ~0.0005. While Appendix B applies an independent P(λ/z) cut that removes the ~1.7 excess at LX ~ 10^43 erg s^−1, the main-text XLFs (Fig. 5) and incompleteness thresholds still rest on the primary randoms. A short quantitative test (e.g., alternative shifts or a shuffled-redshift random) would confirm that the reported purity levels and the group-scale completeness gain versus eRedMaPPer are robust to residual large-scale-structure bias.
  2. Section 4.2 and Fig. 3 convert richness to a group/cluster boundary using mass–richness relations fitted only on the 95 % purity subsample. Because the same relations are then applied to the 80 % and 90 % samples, any purity-dependent change in the richness–mass scatter could bias the reported group fractions. Reporting the scatter or refitting per purity level would strengthen the claim that the group fraction is stable.
minor comments (5)
  1. Fig. 1 caption and color legend: the four absolute-magnitude cuts are listed but the mapping of light-blue/red/purple/dark-blue is easy to misread; a single legend panel would help.
  2. Section 2.2.1: the S/N threshold of 4 and the cylindrical volume (dr_lim = 1500 kpc, dz_m = 0.03) are stated without a brief justification or reference to the forthcoming Doubrawa et al. catalog paper; a sentence on how these choices affect purity would aid reproducibility.
  3. Appendix A, Fig. A.1: the “Purity 70 %” label appears inconsistent with the main-text 80/90/95 % grid; clarify whether this is a different selection or a typographical remnant.
  4. Throughout: “eRosita” / “eROSITA” capitalization is inconsistent in the title and abstract; standardize to the official eROSITA spelling.
  5. Section 4.5: the redshift cut for eRedMaPPer is stated as z < 0.2 while the parent optical sample extends to 0.25; a one-sentence note on why the stricter cut is required (catalog volume) would avoid confusion.

Circularity Check

1 steps flagged

No significant circularity: purity is measured against an independent RA-shifted random catalog, XLFs are compared to external literature, and redMaPPer is an independent optical finder; self-citations supply the optical catalog but do not force the X-ray matching results.

specific steps
  1. self citation load bearing [Section 2.2.1–2.2.2 and Introduction (optical catalog construction)]
    "The S-PLUS cluster and group catalog (Doubrawa et al., in prep.) was constructed using the cluster-finder algorithm PZWav. ... To further characterize the detected systems, we employ the Adaptive Membership Estimator (AME) algorithm (Doubrawa et al. 2023)."

    The optical systems and membership probabilities that enter the matching are taken from the authors’ own prior/in-prep work. This is ordinary self-citation of the input catalog; it does not force the subsequent X-ray matching purity, completeness, or XLF results, which are measured against independent randoms and external literature. Score contribution is therefore minimal (1).

full rationale

The paper constructs multi-wavelength catalogs by matching PZWav+AME optical systems to eRASS1 X-ray contours via a probabilistic modified-Hausdorff procedure. Purity is defined operationally as 1 minus the ratio of random-to-real identifications, where the random catalog is generated by shifting RA by +10° (modulo 360°) and is corrected for the 15% area difference; the paper quantifies residual clustering enhancement as ~0.0005. Completeness and XLF results are then reported at fixed purity levels (80/90/95%) and compared to external benchmarks (Finoguenov et al. 2007 COSMOS XLF; Vikhlinin et al. 1998 ROSAT logN–logS). The redMaPPer comparison uses an identically matched independent optical catalog (eRedMaPPer). Self-citations to prior PZWav/AME papers (Doubrawa et al. 2023, 2024; Werner et al. 2023) merely supply the input optical catalog and membership probabilities; they do not define the matching criteria or the purity metric. Masses use the published Leauthaud et al. (2010) Lx–M200 relation (validated externally by Pederneiras et al. 2025). Appendix B applies an independent Klein-style P(λ/z) cut that removes the low-luminosity excess while preserving the same incompleteness thresholds and the group-scale completeness gain. No step reduces a claimed prediction or first-principles result to its own fitted inputs by construction. The single minor self-citation dependence is not load-bearing for the central claims.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The central results rest on standard cosmological and survey assumptions plus a small set of free matching thresholds that are scanned rather than fitted to a target science result. No new physical entities are postulated; the method inherits optical finders and X-ray scaling relations from prior work.

free parameters (4)
  • summed membership-probability threshold = typically 2–5 depending on purity
    Sampled over {2,3,4,5,6,8,10}; the value that maximizes matches at fixed purity is retained (Section 3).
  • fraction of X-ray contour points required for a match = 50–100 %
    Sampled 10–100 %; higher fractions preferred for 95 % purity catalogs.
  • target purity levels = 80/90/95 %
    User-chosen operating points (80 %, 90 %, 95 %) that define the distance cut via the random-to-real ratio.
  • absolute-magnitude cuts = −18.5, −19, −19.5, −20
    Four discrete depth choices (Mr < −18.5/−19/−19.5/−20) that set the optical galaxy sample used for matching.
axioms (4)
  • domain assumption Flat ΛCDM cosmology with H0 = 70 km s−1 Mpc−1, Ωm = 0.3
    Adopted throughout for distances, absolute magnitudes and volumes (Section 1).
  • domain assumption Lx–M200 relation of Leauthaud et al. (2010) and L–T relation of Markevitch (1998) remain valid for the eRASS1 sample
    Used to convert fluxes to masses and temperatures (Section 3); consistency checked only via Pederneiras et al. (2025).
  • ad hoc to paper RA +10° shift produces an unbiased random catalog of chance superpositions
    Defines purity; residual clustering bias is claimed to be ~0.0005 but not independently verified (Section 3).
  • domain assumption Photometric-redshift PDFs and AME membership probabilities correctly represent galaxy association probabilities
    Inherited from prior PZWav/AME papers and used as weights in the Hausdorff matching.

pith-pipeline@v1.1.0-grok45 · 24953 in / 2647 out tokens · 18527 ms · 2026-07-12T07:35:01.385053+00:00 · methodology

0 comments
read the original abstract

We present the construction and characterization of a multi-wavelength catalog of galaxy groups and clusters by matching optical detections from the Southern Photometric Local Universe Survey (S-PLUS) with extended X-ray emission from the first eROSITA all-sky survey data release (eRASS1). We employ a probabilistic matching framework, based on the modified Hausdorff distance, to associate galaxy systems identified by the PZWav cluster finder and characterized by the AME membership estimator with X-ray surface brightness contours. This method explicitly accounts for the photometric redshift probability distribution of galaxies and allows us to explore the critical trade-off between catalog completeness and purity. We investigate how the matched sample changes with different optical selection depths, defined by absolute magnitude cuts of $M_r$ < -18.5, -19, -19.5, and -20 sampling redshifts within 0.08 < z < 0.25, and across purity levels of 80%, 90%, and 95%. We find that fainter optical cuts enhance the recovery of low-mass, low-luminosity groups, while brighter cuts favor more massive clusters and increase the effective survey volume at higher redshifts. Stricter purity requirements reduce contamination but systematically lower completeness, particularly for low-luminosity systems. The derived X-ray luminosity functions agree well with previous determinations, and the logN-logS distributions confirm the high recovery rate of luminous clusters. Comparisons with the redMaPPer cluster catalog validate our approach, showing consistent trends and significant overlap, while our method offers improved completeness at the group scale. This work demonstrates a robust, flexible methodology for creating reliable multi-wavelength cluster catalogs, essential for cosmological studies and investigations of galaxy evolution in dense environments.

Figures

Figures reproduced from arXiv: 2607.02706 by A. Finoguenov, A. Gonzalez, A. Kanaan, C. Mendes de Oliveira, E. S. Cypriano, E. V. Lima, G. Souza, J. Comparat, L. Doubrawa, L. Nakazono, R. Demarco, T. Ribeiro, W. Schoenell.

Figure 1
Figure 1. Figure 1: Examples of detected clusters, along with their associated member galaxies. Colors indicate the adopted absolute magnitude [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Top panel: Redshift distribution of the cluster catalog at [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Fractions of clusters (triangles) and groups (circles) in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: log N–log S distribution of cluster counts as a function of X-ray flux. Symbols represent different absolute-magnitude cuts. The gray dot-dashed curve shows all X-ray sources within the S￾PLUS footprint. Red shaded regions represent the eRedMaPPer catalog over the redshift range 0.08 < z < 0.2. Star symbols indi￾cate the combined contribution of the eSCALE and eRedMaPPer catalogs. The gray solid line shows… view at source ↗
Figure 6
Figure 6. Figure 6: Recovery fraction as a function of the cluster richness, [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 5
Figure 5. Figure 5: Cluster X-ray luminosity functions for three di [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: Top panel: Fraction of X-ray sources missed by each cata [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Incompleteness rate as a function of richness for the [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗

discussion (0)

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Works this paper leans on

297 extracted references · 83 canonical work pages · 59 internal anchors

  1. [1]

    and Cardoso, N

    Mendes de Oliveira, C. and Cardoso, N. M. and Lopes, P. A. A. and Ribeiro, A. L. B. and Olave-Rojas, D. E. and Krabbe, A. and Sodr. S-PLUS Clusters And Large-scale Environments (SCALE): I. A catalog of known clusters and groups in DR5 and a pilot study of Abell 4038 , note =

  2. [2]

    and Oliveira Schwarz, Gustavo and Herpich, Fabio R

    Rodrigues de Lima, Erik V. and Oliveira Schwarz, Gustavo and Herpich, Fabio R. and Almeida-Fernandes, Felipe D. and Nakazono, Lilianne and Lacerda, Eduardo A. and Santos, Andr. The S-PLUS Fifth Data-Release: Over 4500 square degrees of the Southern Sky and a multicolor view of the Hydra and Antlia galaxy clusters , note =

  3. [3]

    and Mendes de Oliveira, Claudia and Krabbe, Angela C

    Cardoso, Natanael M. and Mendes de Oliveira, Claudia and Krabbe, Angela C. and Castelli, Analía V. Smith and Oliveira Schwarz, Gustavo B. and Nakazono, Lilianne and Demarco, Ricardo and Carvalho, Maiara S. and Schoenell, William and Ribeiro, Tiago and Kanaan, Antonio and Saraiva, Antonio M. , title =. 2026 , month =. doi:10.3847/1538-3881/ae4fb1 , url =

    doi:10.3847/1538-3881/ae4fb1 2026

  4. [4]

    The Lx-T Relation and Temperature Function for Nearby Clusters Revisited

    The L _ X -T Relation and Temperature Function for Nearby Clusters Revisited. , keywords =. doi:10.1086/306080 , archivePrefix =. astro-ph/9802059 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/306080

  5. [5]

    MNRAS , volume=

    Cosmological constraints from CODEX galaxy clusters spectroscopically confirmed by SDSS-IV/SPIDERS DR16 , author=. MNRAS , volume=. 2020 , publisher=

    2020

  6. [6]

    AJ , volume=

    Overview of the DESI legacy imaging surveys , author=. AJ , volume=. 2019 , publisher=

    2019

  7. [7]

    Optical identification and properties of galaxy clusters and groups in the western galactic hemisphere

    The SRG/eROSITA All-Sky Survey. Optical identification and properties of galaxy clusters and groups in the western galactic hemisphere. , keywords =. doi:10.1051/0004-6361/202349031 , archivePrefix =. 2402.08453 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202349031

  8. [8]

    AXES-2MRS: A new all-sky catalogue of extended X-ray galaxy groups

    AXES-2MRS: A new all-sky catalogue of extended X-ray galaxy groups. , keywords =. doi:10.1051/0004-6361/202450060 , archivePrefix =. 2403.17061 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202450060

  9. [9]

    AXES-SDSS: comparison of SDSS galaxy groups with all-sky X-ray extended sources

    AXES-SDSS: Comparison of SDSS galaxy groups with all-sky X-ray extended sources. , keywords =. doi:10.1051/0004-6361/202449591 , archivePrefix =. 2403.17055 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202449591

  10. [10]

    First X-ray catalogues and data release of the western Galactic hemisphere

    The SRG/eROSITA all-sky survey. First X-ray catalogues and data release of the western Galactic hemisphere. , keywords =. doi:10.1051/0004-6361/202347165 , archivePrefix =. 2401.17274 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202347165

  11. [11]

    Handbook of X-ray and Gamma-ray Astrophysics , year = 2023, eid =

    X-Ray Cluster Cosmology. Handbook of X-ray and Gamma-ray Astrophysics , year = 2023, eid =. doi:10.1007/978-981-16-4544-0_117-1 , adsurl =

    work page doi:10.1007/978-981-16-4544-0_117-1 2023

  12. [12]

    MNRAS , fjournal=

    Sereno, Mauro , title=. MNRAS , fjournal=

  13. [13]

    , keywords =

    A Universal Density Profile from Hierarchical Clustering. , keywords =. doi:10.1086/304888 , archivePrefix =. astro-ph/9611107 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/304888

  14. [14]

    2019 , publisher=

    Introduction to Research Methods 5th Edition: A Practical Guide for Anyone Undertaking a Research Project , author=. 2019 , publisher=

    2019

  15. [15]

    2017 , publisher=

    Statistics , author=. 2017 , publisher=

    2017

  16. [16]

    , keywords =

    Cosmic variance of the galaxy cluster weak lensing signal. , keywords =. doi:10.1093/mnras/stv532 , archivePrefix =. 1501.01632 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv532

  17. [17]

    A Bayesian approach to linear regression in astronomy

    A Bayesian approach to linear regression in astronomy. , keywords =. doi:10.1093/mnras/stv2374 , archivePrefix =. 1509.05778 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2374

  18. [18]

    , keywords =

    Weak Lensing Calibrated M-T Scaling Relation of Galaxy Groups in the COSMOS Field ^ sstarf. , keywords =. doi:10.1088/0004-637X/778/1/74 , archivePrefix =. 1309.3891 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/778/1/74

  19. [20]

    Testing the Low-Mass End of X-Ray Scaling Relations with a Sample of Chandra Galaxy Groups

    Testing the low-mass end of X-ray scaling relations with a sample of Chandra galaxy groups. , keywords =. doi:10.1051/0004-6361/201116734 , archivePrefix =. 1109.6498 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201116734

  20. [21]

    , keywords =

    Some Aspects of Measurement Error in Linear Regression of Astronomical Data. , keywords =. doi:10.1086/519947 , archivePrefix =. 0705.2774 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/519947

  21. [22]

    , keywords =

    Evolution and clustering of rich clusters. , keywords =. doi:10.1093/mnras/222.2.323 , adsurl =

    doi:10.1093/mnras/222.2.323

  22. [23]

    , keywords =

    The Impact of Galaxy Formation on the Sunyaev-Zel'dovich Effect of Galaxy Clusters. , keywords =. doi:10.1086/506467 , archivePrefix =. astro-ph/0512208 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/506467

  23. [24]

    , keywords =

    Galaxy cluster X-ray luminosity scaling relations from a representative local sample (REXCESS). , keywords =. doi:10.1051/0004-6361/200810994 , archivePrefix =. 0809.3784 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/200810994

  24. [25]

    , keywords =

    Large-Scale Structure Formation: From the First Non-linear Objects to Massive Galaxy Clusters. , keywords =. doi:10.1007/s11214-014-0045-7 , archivePrefix =. 1404.3956 , primaryClass =

    Pith/arXiv arXiv doi:10.1007/s11214-014-0045-7

  25. [26]

    , year = 1974, month = feb, volume =

    Formation of Galaxies and Clusters of Galaxies by Self-Similar Gravitational Condensation. , year = 1974, month = feb, volume =. doi:10.1086/152650 , adsurl =

    doi:10.1086/152650 1974

  26. [27]

    , keywords =

    Statistics of X-ray observables for the cooling-core and non-cooling core galaxy clusters. , keywords =. doi:10.1051/0004-6361:20066471 , archivePrefix =. astro-ph/0702482 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361:20066471

  27. [28]

    , keywords =

    X-Ray Properties of SPT-selected Galaxy Clusters at 0.2 < z < 1.5 Observed with XMM-Newton. , keywords =. doi:10.3847/1538-4357/aaf230 , archivePrefix =. 1807.02556 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aaf230

  28. [29]

    X-ray scaling relations for a representative sample of Planck selected clusters observed with XMM-Newton

    X-Ray Scaling Relations for a Representative Sample of Planck-selected Clusters Observed with XMM-Newton. , keywords =. doi:10.3847/1538-4357/ab7997 , archivePrefix =. 2002.11740 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab7997 2002

  29. [30]

    and Babu, J

    Feigelson, E. and Babu, J. , title =. 2012 , publisher =

    2012

  30. [31]

    , keywords =

    Formation of Galaxy Clusters. , keywords =. doi:10.1146/annurev-astro-081811-125502 , archivePrefix =. 1205.5556 , primaryClass =

    Pith/arXiv arXiv doi:10.1146/annurev-astro-081811-125502

  31. [32]

    The Astrophysical Journal , abstract =

    Yutaka Fujita and Han Aung , title =. The Astrophysical Journal , abstract =. 2019 , month =. doi:10.3847/1538-4357/ab0e02 , url =

    work page doi:10.3847/1538-4357/ab0e02 2019

  32. [33]

    Chandra Cluster Cosmology Project. II. Samples and X-Ray Data Reduction. , keywords =. doi:10.1088/0004-637X/692/2/1033 , archivePrefix =. 0805.2207 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/692/2/1033

  33. [34]

    arXiv e-prints , keywords =

    Lectures on Gravitational Lensing. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/9606001 , archivePrefix =. astro-ph/9606001 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9606001

  34. [35]

    , keywords =

    Formation of galaxies and large-scale structure with cold dark matter. , keywords =. doi:10.1038/311517a0 , adsurl =

    doi:10.1038/311517a0

  35. [36]

    , keywords =

    Core condensation in heavy halos: a two-stage theory for galaxy formation and clustering. , keywords =. doi:10.1093/mnras/183.3.341 , adsurl =

    doi:10.1093/mnras/183.3.341

  36. [37]

    arXiv e-prints , keywords =

    The FLAMINGO Project: Galaxy clusters in comparison to X-ray observations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2312.08277 , archivePrefix =. 2312.08277 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2312.08277

  37. [38]

    , title =

    Gregory, P. , title =. 2005 , publisher =

    2005

  38. [39]

    CODEX: Role of velocity substructure in the scaling relations of galaxy clusters

    CODEX: Role of velocity substructure in the scaling relations of galaxy clusters. , keywords =. doi:10.1051/0004-6361/202245308 , archivePrefix =. 2307.08749 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202245308

  39. [40]

    CODEX Weak Lensing Mass Catalogue and implications on the mass-richness relation

    CODEX weak lensing mass catalogue and implications on the mass-richness relation. , keywords =. doi:10.1093/mnras/staa3936 , archivePrefix =. 2101.02257 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa3936

  40. [41]

    Scaling Properties of Galaxy Groups

    Scaling Properties of Galaxy Groups. Universe , keywords =. doi:10.3390/universe7050139 , archivePrefix =. 2106.13256 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3390/universe7050139

  41. [42]

    CODEX clusters. The Survey, the Catalog, and Cosmology of the X-ray Luminosity Function

    CODEX clusters. Survey, catalog, and cosmology of the X-ray luminosity function. , keywords =. doi:10.1051/0004-6361/201937283 , archivePrefix =. 1912.03262 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201937283 1912

  42. [43]

    Mass Calibration of the CODEX Cluster Sample using SPIDERS Spectroscopy -- I. The Richness-Mass Relation

    Mass calibration of the CODEX cluster sample using SPIDERS spectroscopy - I. The richness-mass relation. , keywords =. doi:10.1093/mnras/stz931 , archivePrefix =. 1812.06094 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz931

  43. [44]

    , keywords =

    CODEX weak lensing: concentration of galaxy clusters at z 0.5. , keywords =. doi:10.1093/mnras/stx484 , archivePrefix =. 1612.06871 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx484

  44. [45]

    CCCP and MENeaCS: (updated) weak-lensing masses for 100 galaxy clusters

    CCCP and MENeaCS: (updated) weak-lensing masses for 100 galaxy clusters. , keywords =. doi:10.1093/mnras/staa2303 , archivePrefix =. 1912.04414 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa2303 1912

  45. [46]

    , keywords =

    The Canadian Cluster Comparison Project: detailed study of systematics and updated weak lensing masses. , keywords =. doi:10.1093/mnras/stv275 , archivePrefix =. 1502.01883 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv275

  46. [47]

    , keywords =

    Adiabatic scaling relations of galaxy clusters. , keywords =. doi:10.1111/j.1365-2966.2006.10596.x , archivePrefix =. astro-ph/0605720 , primaryClass =

    doi:10.1111/j.1365-2966.2006.10596.x 2006

  47. [48]

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

    The SRG/eROSITA All-Sky Survey. The first catalog of galaxy clusters and groups in the Western Galactic Hemisphere. , keywords =. doi:10.1051/0004-6361/202348264 , archivePrefix =. 2402.08452 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202348264

  48. [49]

    L. R. Jones and C. Scharf and H. Ebeling and E. Perlman and G. Wegner and M. Malkan and D. Horner , title =. The Astrophysical Journal , abstract =. 1998 , month =. doi:10.1086/305283 , url =

    work page doi:10.1086/305283 1998

  49. [50]

    , keywords =

    Accurate Universal Models for the Mass Accretion Histories and Concentrations of Dark Matter Halos. , keywords =. doi:10.1088/0004-637X/707/1/354 , archivePrefix =. 0811.0828 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/707/1/354

  50. [51]

    , keywords =

    The ROSAT all-sky survey bright source catalogue. , keywords =. doi:10.48550/arXiv.astro-ph/9909315 , archivePrefix =. astro-ph/9909315 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9909315

  51. [52]

    A Catalog of 200 Galaxy Clusters Serendipitously Detected in the ROSAT PSPC Pointed Observations

    A Catalog of 200 Galaxy Clusters Serendipitously Detected in the ROSAT PSPC Pointed Observations. , keywords =. doi:10.1086/305951 , archivePrefix =. astro-ph/9803099 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/305951

  52. [53]

    Annual Review of Astronomy and Astrophysics , volume =

    Veilleux, Sylvain and Cecil, Gerald and Bland-Hawthorn, Joss , title =. Annual Review of Astronomy and Astrophysics , volume =. 2005 , doi =. https://doi.org/10.1146/annurev.astro.43.072103.150610 , abstract =

    Pith/arXiv arXiv doi:10.1146/annurev.astro.43.072103.150610 2005

  53. [54]

    redMaPPer. I. Algorithm and SDSS DR8 Catalog. , keywords =. doi:10.1088/0004-637X/785/2/104 , archivePrefix =. 1303.3562 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/785/2/104

  54. [55]

    , keywords =

    A Weak Lensing Study of X-ray Groups in the Cosmos Survey: Form and Evolution of the Mass-Luminosity Relation. , keywords =. doi:10.1088/0004-637X/709/1/97 , archivePrefix =. 0910.5219 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/709/1/97

  55. [56]

    , keywords =

    CFHTLenS: weak lensing calibrated scaling relations for low-mass clusters of galaxies. , keywords =. doi:10.1093/mnras/stv923 , archivePrefix =. 1410.8769 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv923

  56. [57]

    , keywords =

    The Sloan Digital Sky Survey: Technical Summary. , keywords =. doi:10.1086/301513 , archivePrefix =. astro-ph/0006396 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/301513

  57. [58]

    Brightest X-ray clusters of galaxies in the CFHTLS wide fields: Catalog and optical mass estimator

    Brightest X-Ray Clusters of Galaxies in the CFHTLS Wide Fields: Catalog and Optical Mass Estimator. , keywords =. doi:10.1088/0004-637X/799/1/60 , archivePrefix =. 1411.3326 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/799/1/60

  58. [59]

    , keywords =

    Toward a Halo Mass Function for Precision Cosmology: The Limits of Universality. , keywords =. doi:10.1086/591439 , archivePrefix =. 0803.2706 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/591439

  59. [60]

    Communications in Applied Mathematics and Computational Science , keywords =

    Ensemble samplers with affine invariance. Communications in Applied Mathematics and Computational Science , keywords =. doi:10.2140/camcos.2010.5.65 , adsurl =

    doi:10.2140/camcos.2010.5.65 2010

  60. [61]

    , keywords =

    emcee: The MCMC Hammer. , keywords =. doi:10.1086/670067 , archivePrefix =. 1202.3665 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/670067

  61. [62]

    , keywords =

    Hundreds of weak lensing shear-selected clusters from the Hyper Suprime-Cam Subaru Strategic Program S19A data. , keywords =. doi:10.1093/pasj/psab047 , archivePrefix =. 2103.15016 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/pasj/psab047

  62. [64]

    Unified weak lensing constraints on the evolution of the mass -- X-ray luminosity relation for galaxy clusters

    Unified Weak Lensing Constraints on the Evolution of the Mass X-Ray Luminosity Relation for Galaxy Clusters. , keywords =. doi:10.3847/1538-4357/ade793 , archivePrefix =. 2505.21659 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ade793

  63. [66]

    MAR: A Multiband Astronomical Reduction package. Astron. Comput. , keywords =. doi:10.1016/j.ascom.2024.100899 , adsurl =

    work page doi:10.1016/j.ascom.2024.100899 2024

  64. [67]

    ASR , keywords =

    The ROSAT all-sky survey. ASR , keywords =. doi:10.1016/0273-1177(93)90147-4 , adsurl =

    doi:10.1016/0273-1177(93)90147-4

  65. [68]

    , year = 1968, month = feb, volume =

    Space Distribution and Luminosity Functions of Quasi-Stellar Radio Sources. , year = 1968, month = feb, volume =. doi:10.1086/149446 , adsurl =

    doi:10.1086/149446 1968

  66. [69]

    doi:10.5281/zenodo.12728524 , url =

    Erik Vinicius Rodrigues de Lima , title =. doi:10.5281/zenodo.12728524 , url =

    work page doi:10.5281/zenodo.12728524

  67. [70]

    Feedback from Active Galactic Nuclei in Galaxy Groups

    Feedback from Active Galactic Nuclei in Galaxy Groups. Universe , keywords =. doi:10.3390/universe7050142 , archivePrefix =. 2106.13259 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3390/universe7050142

  68. [71]

    10.1051/0004-6361/202453464

    AXES-SDSS: Solving the puzzle of X-ray emission of optical galaxy groups via a modified Hausdorff distance , DOI= "10.1051/0004-6361/202453464", url= "https://doi.org/10.1051/0004-6361/202453464", journal =

    work page doi:10.1051/0004-6361/202453464

  69. [72]

    Galaxy groups and clusters and their brightest galaxies within the cosmic web

    Galaxy groups and clusters and their brightest galaxies within the cosmic web. , keywords =. doi:10.1051/0004-6361/202347504 , archivePrefix =. 2311.01868 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202347504

  70. [73]

    Bulge-disc decomposition of the Hydra cluster galaxies in 12 bands

    Bulge-disc decomposition of the Hydra cluster galaxies in 12 bands. , keywords =. doi:10.1093/mnras/stad3571 , archivePrefix =. 2311.09313 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad3571

  71. [74]

    Structure and large scale environment of galaxy pairs in the S-PLUS DR4

    Structure and large-scale environment of galaxy pairs in the S-PLUS DR4. , keywords =. doi:10.1093/mnras/stae334 , archivePrefix =. 2402.00120 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stae334

  72. [75]

    , keywords =

    CALSAGOS: Clustering algorithms applied to galaxies in overdense systems. , keywords =. doi:10.1093/mnras/stac3762 , archivePrefix =. 2212.09451 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stac3762

  73. [76]

    10.1051/0004-6361/201731606

    The XXL Survey - XX. The 365 cluster catalogue★★★ , DOI= "10.1051/0004-6361/201731606", url= "https://doi.org/10.1051/0004-6361/201731606", journal =

    doi:10.1051/0004-6361/201731606

  74. [77]

    The XXL Survey. I. Scientific motivations - XMM-Newton observing plan - Follow-up observations and simulation programme. , keywords =. doi:10.1051/0004-6361/201526766 , archivePrefix =. 1512.04317 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201526766

  75. [78]

    arXiv e-prints , keywords =

    The DESI Experiment Part II: Instrument Design. arXiv e-prints , keywords =. doi:10.48550/arXiv.1611.00037 , archivePrefix =. 1611.00037 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1611.00037

  76. [79]

    , year = 1936, month = jan, volume =

    The Mass of the Virgo Cluster. , year = 1936, month = jan, volume =. doi:10.1086/143697 , adsurl =

    doi:10.1086/143697 1936

  77. [80]

    , year = 1937, month = oct, volume =

    On the Masses of Nebulae and of Clusters of Nebulae. , year = 1937, month = oct, volume =. doi:10.1086/143864 , adsurl =

    doi:10.1086/143864 1937

  78. [81]

    The Chandra X-Ray Observatory (CXO): An Overview

    The Chandra X-Ray Observatory (CXO): An Overview. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/9912097 , archivePrefix =. astro-ph/9912097 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9912097

  79. [82]

    Space Optics 1994: Earth Observation and Astronomy , year = 1994, editor =

    X-ray spectroscopy mission (XMM) telescope development. Space Optics 1994: Earth Observation and Astronomy , year = 1994, editor =. doi:10.1117/12.185278 , adsurl =

    work page doi:10.1117/12.185278 1994

  80. [83]

    , keywords =

    The eROSITA X-ray telescope on SRG. , keywords =. doi:10.1051/0004-6361/202039313 , archivePrefix =. 2010.03477 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202039313 2010

Showing first 80 references.