The eROSITA Final Equatorial-Depth Survey (eFEDS)

Liu, Ang; Bülbül, Esra; Ghirardini, Vittorio; Liu, T.; Klein, Matthias; Clerc, N.; Özsoy, Y.; Ramos-Ceja, M. E.; Pacaud, F.; Comparat, Johan; Okabe, Nobuhiko; Bahar, Y. E.; Biffi, V.; Brunner, H.; Brüggen, M.; Buchner, Johannes; Chitham, J. Ider; Chiu, I-Non; Dolag, K.; Gatuzz, E.; González, J. D. Remolina; Hoang, D. N.; Lamer, G.; Merloni, A.; Nandra, K.; Oguri, Masamune; Ota, Naomi; Predehl, P.; Reiprich, T. H.; Salvato, M.; Schrabback, T.; Sanders, Jeremy; Seppi, R.; Thibaud, Q.

doi:10.1051/0004-6361/202141120

“…Galaxy clusters can be detected in different wavelengths. In recent years, several experiments produced large catalogs of clusters to be used for the cosmological analysis, such as the Planck survey (Planck Collaboration et al 2016a;Planck Collaboration et al 2016b), the South Pole Telescope (SPT hereafter) (Bleem et al 2015;de Haan et al 2016;Bocquet et al 2019), and the Atacama Cosmology Telescope (Hilton et al 2021) in the millimeter wavelengths; the Kilo-Degree Survey (Maturi et al 2019) and the Dark Energy Survey (Drlica-Wagner et al 2018;Abbott et al 2020) in the optical; and the ROSAT survey (Böhringer et al 2017), the XXL survey (Pacaud et al 2018;Adami et al 2018), and the first eROSITA observations (Liu et al 2022) in X-rays. In particular, the abundance of galaxy clusters (galaxy cluster number counts) has emerged as a fundamental cosmological probe.…”

Section: Introductionmentioning

confidence: 99%

Combining Planck and SPT Cluster Catalogs: Cosmological Analysis and Impact on the Planck Scaling Relation Calibration

Salvati

¹

,

Saro

²

,

Bocquet

³

et al. 2022

ApJ

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We provide the first combined cosmological analysis of the South Pole Telescope (SPT) and Planck cluster catalogs. The aim is to provide an independent calibration for Planck scaling relations, exploiting the cosmological constraining power of the SPT-SZ cluster catalog and its dedicated weak lensing (WL) and X-ray follow-up observations. We build a new version of the Planck cluster likelihood. In the νΛ CDM scenario, focusing on the mass slope and mass bias of Planck scaling relations, we find α SZ = 1.49 − 0.10 + 0.07 and 1 − b SZ = 0.69 − 0.14 + 0.07 , respectively. The results for the mass slope show a ∼4 σ departure from the self-similar evolution, α SZ ∼ 1.8. This shift is mainly driven by the matter density value preferred by SPT data, Ω m = 0.30 ± 0.03, lower than the one obtained by Planck data alone, Ω m = 0.37 − 0.06 + 0.02 . The mass bias constraints are consistent both with outcomes of hydrodynamical simulations and external WL calibrations, (1 − b) ∼ 0.8, and with results required by the Planck cosmic microwave background cosmology, (1 − b) ∼ 0.6. From this analysis, we obtain a new catalog of Planck cluster masses M 500. We estimate the ratio between the published Planck M SZ masses and our derived masses M 500, as a “measured mass bias,” 1 − b M . We analyze the mass, redshift, and detection noise dependence of 1 − b M , finding an increasing trend toward high redshift and low mass. These results mimic the effect of departure from self-similarity in cluster evolution, showing different dependencies for the low-mass, high-mass, low-z, and high-z regimes.

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“…The richness range N > 15 corresponds to the cluster mass M 500 5 × 10 13 M (Okabe et al 2019). We cross-matched the CAMIRA catalog with the eFEDS X-ray cluster catalog (Liu et al 2022) to find there are 211 optical clusters that have at least one spatially-extended Xray source within the scale radius R 500 from the optical centers. Here R 500 was estimated from the mass-richness relation (Okabe et al 2019) and the cluster richness (Oguri et al 2018).…”

Section: Samplementioning

confidence: 99%

The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray properties of Subaru optically-selected clusters

Ota¹,

Nguyen-Dang²,

Mitsuishi³

et al. 2022

Preprint

Self Cite

0

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Context. We present the results from a systematic X-ray analysis of Subaru optically-selected clusters with high cluster richness in the eROSITA Final Equatorial-Depth Survey (eFEDS) field. Aims. By a joint analysis of SRG(Spectrum Roentgen Gamma)/eROSITA and Subaru/HSC surveys, we aim to investigate the dynamical status of the optically-selected clusters and derive the cluster scaling relations. Methods. The sample consists of 43 optically-selected galaxy clusters with richness > 40 in the redshift range of 0.16-0.89. We systematically analyzed X-ray images and emission spectra using the eROSITA data. We identified the brightest cluster galaxy (BCG) using the optical and far-infrared databases and measured the offset between X-ray peak and BCG position as an indicator of the dynamical status. We investigated the luminosity-temperature and mass-luminosity relations based on eROSITA X-ray spectra and HSC weak-lensing data analyses.Results. The fraction of relaxed clusters is estimated to be 2(< 39)%, which is smaller than that of the X-ray-selected cluster samples. After correcting for a selection bias due to the richness cut, we obtained a shallow L − T slope of 2.0 ± 0.4, which is consistent with the predictions of the self-similar model and the new baseline model by Fujita & Aung (2019). The L − M slope of 1.5 ± 0.3 agrees with the above theoretical models and that of the shear-selected clusters in the eFEDs field. Conclusions. Our analysis of the high-richness optical clusters yielded a small fraction of relaxed clusters and a shallow slope of the luminositytemperature relation. This suggests that the average X-ray properties of the optical clusters are likely to be different from those observed in the X-ray samples. Thus, the joint eROSITA and HSC observations are powerful in extending the analysis to a larger sample and understanding the selection effect towards establishing the cluster scaling relations.

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“…Prior to the all-sky survey, the eROSITA Final Equatorial Depth Survey (eFEDS) was first carried out as part of the performance verification phase of the eROSITA mission. There are 540 X-ray selected clusters in eFEDS with a survey area of ≈ 140 deg 2 with systems extending to redshift 𝑧 ≈ 1.3 (Liu et al 2022a;Klein et al 2022). The data products and catalogs have been entirely released in the Early Data Release 1 of the eROSITA mission with a series of studies on the characterization of X-ray properties (e.g., Liu et al 2022a;Ghirardini et al 2021;Bahar et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Cosmological Constraints from Galaxy Clusters and Groups in the eROSITA Final Equatorial Depth Survey

Chiu¹,

Klein²,

Mohr³

et al. 2022

Preprint

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We present the first cosmological study of a sample of eROSITA clusters, which were identified in the eROSITA Final Equatorial Depth Survey (eFEDS). In a joint selection on X-ray and optical observables, the sample contains 455 clusters within a redshift range of 0.1 < 𝑧 < 1.2, of which 177 systems are covered by the public data from the Hyper Suprime-Cam (HSC) survey that enables uniform weak-lensing cluster mass constraints. With minimal assumptions, at each cluster redshift 𝑧 we empirically model (1) the scaling relations between the cluster halo mass 𝑀 and the observables, which include the X-ray count rate 𝜂, the optical richness 𝜆, and the weak-lensing mass 𝑀 WL , and (2) the X-ray selection in terms of the completeness function C. Using the richness distribution of the clusters, we directly measure the X-ray completeness and adopt those measurements as informative priors for the parameters of C. We validate our cosmology analysis framework using mock data, and then in a blinded analysis of the real data we further validate the joint modeling of the cluster abundance and the weak-lensing mass calibration with a set of consistency tests. After unblinding, we obtain the cosmological constraints Ω m = 0.245 +0.048 −0.058 , 𝜎 8 = 0.833 +0.075 −0.063 and 𝑆 8 ≡ 𝜎 8 (Ω m /0.3) 0.3 = 0.791 +0.028 −0.031 in a flat ΛCDM cosmology. Extending to a flat 𝑤CDM cosmology leads to the constraint on the equation of state parameter of the dark energy of 𝑤 = −1.25 ± 0.47. The eFEDS constraints are in good agreement with the results from the Planck mission, the galaxy-galaxy lensing and clustering analysis of the Dark Energy Survey, and the cluster abundance analysis of the SPT-SZ survey at a level of 1𝜎. Through extensive testing we find that the eFEDS results are robust with respect to the informative priors applied to the parameters of C, the assumed functional form of the mass scaling of the count rate, and the different subsample selections. Our results suggest an X-ray completeness without a significant redshift dependence. No strong evidence of a broken power-law mass scaling of the count rate is supported by the eFEDS sample of galaxy clusters and groups. This work not only presents the first fully self-consistent cosmological constraints obtained in a synergy between wide-field X-ray and weak lensing surveys, but also demonstrates the success of the empirical modeling in X-ray cluster cosmology studies. We provide updated estimates of individual cluster masses.

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The eROSITA Final Equatorial-Depth Survey (eFEDS)

Cited by 96 publications

References 125 publications

Combining Planck and SPT Cluster Catalogs: Cosmological Analysis and Impact on the Planck Scaling Relation Calibration

Combining Planck and SPT Cluster Catalogs: Cosmological Analysis and Impact on the Planck Scaling Relation Calibration

The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray properties of Subaru optically-selected clusters

Cosmological Constraints from Galaxy Clusters and Groups in the eROSITA Final Equatorial Depth Survey

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