AMICO galaxy clusters in KiDS-DR3: Constraints on cosmological parameters and on the normalisation of the mass-richness relation from clustering

Lesci, Giorgio F.; Nanni, Lorenza; Marulli, F.; Moscardini, L.; Veropalumbo, Alfonso; Maturi, M.; Sereno, Mauro; Radovich, M.; Bellagamba, F.; Roncarelli, M.; Bardelli, S.; Castignani, G.; Covone, G.; Giocoli, Carlo; Ingoglia, Lorenzo; Puddu, E.

doi:10.1051/0004-6361/202243538

Cited by 25 publications

(11 citation statements)

References 72 publications

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“…The cluster catalogue used in this work is the same one exploited in previous works (Bellagamba et al 2018(Bellagamba et al , 2019Radovich et al 2020;Puddu et al 2021;Lesci et al 2022b;Ingoglia et al 2022;Romanello et al 2024) and validated by Maturi et al (2019). All systems belonging to the KiDS-DR3 footprints that are heavily affected by satellite tracks, haloes created by bright stars, and images or artefacts are rejected (Maturi et al 2019).…”

Section: Amico Kids-dr3 Cluster Cataloguementioning

confidence: 99%

AMICO galaxy clusters in KiDS-DR3

Giocoli

Marulli

Moscardini

et al. 2021

A&A

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Context. The large-scale mass distribution around dark matter haloes hosting galaxy clusters provides sensitive cosmological information. Aims. In this work we make use of a large photometric galaxy cluster sample, constructed from the public Third Data Release of the Kilo-Degree Survey, and the corresponding shear signal, to assess cluster masses and test the concordance Λ-cold dark matter (ΛCDM) model. In particular, we study the weak gravitational lensing effects on scales beyond the cluster virial radius, where the signal is dominated by correlated and uncorrelated matter density distributions along the line of sight. The analysed catalogue consists of 6962 galaxy clusters, in the redshift range 0.1 ≤ z ≤ 0.6 and with signal-to-noise ratios higher than 3.5. Methods. We perform a full Bayesian analysis to model the stacked shear profiles of these clusters. The adopted likelihood function considers both the small-scale one-halo term, used primarily to constrain the cluster structural properties, and the two-halo term, that can be used to constrain cosmological parameters. Results. We find that the adopted modelling is successful in assessing both the cluster masses and the total matter density parameter, ΩM, when fitting shear profiles up to the largest available scales of 35 Mpc h−1. Moreover, our results provide a strong observational evidence of the two-halo signal in the stacked gravitational lensing of galaxy clusters, further demonstrating the reliability of this probe for cosmological studies. The main result of this work is a robust constraint on ΩM, assuming a flat ΛCDM cosmology. We get ΩM = 0.29 ± 0.02, estimated from the full posterior probability distribution, consistent with the estimates from cosmic microwave background experiments.

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Section: Amico Kids-dr3 Cluster Cataloguementioning

confidence: 99%

AMICO galaxy clusters in KiDS-DR3

Giocoli

Marulli

Moscardini

et al. 2021

A&A

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“…The grey band represents Planck18 constraints. The CMB lensing data are in black [151,171,533], the galaxy WL data are in blue [133,165,166], while the galaxy clustering [425,534,535] in red, galaxy clusters [536][537][538][539][540] in yellow, and tSZ [541][542][543] are in purple. Extensive research has been conducted on systematics related to various probes, aiming to understand the possible systematic-induced tension between the early-time and multiple late-time measurements (see, e.g., review [544]).…”

Section: Insights Into Mg From Current Surveysmentioning

confidence: 99%

“…However, if this discrepancy is attributed to exotic physics, the proposed model must reconcile the effects in both early and late stages and successfully pass scrutiny from cosmological probes. √ Ω m /0.3 for CMB lensing (black) [151,171,533], galaxy WL data (blue) [133,135,136,549], galaxy clustering (red) [425,534,535], galaxy clusters (yellow) [536][537][538][539][540], and tSZ (purple) [541][542][543]. The grey band is from Planck using TT+TE+EE+lowE [182].…”

Section: Insights Into Mg From Current Surveysmentioning

confidence: 99%

Cosmological Probes of Structure Growth and Tests of Gravity

et al. 2023

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The current standard cosmological model is constructed within the framework of general relativity with a cosmological constant Λ, which is often associated with dark energy, and phenomenologically explains the accelerated cosmic expansion. Understanding the nature of dark energy is one of the most appealing questions in achieving a self-consistent physical model at cosmological scales. Modification of general relativity could potentially provide a more natural and physical solution to the accelerated expansion. The growth of the cosmic structure is sensitive in constraining gravity models. In this paper, we aim to provide a concise introductory review of modified gravity models from an observational point of view. We will discuss various mainstream cosmological observables, and their potential advantages and limitations as probes of gravity models.

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“…It can therefore help to calibrate these relations and reduce the uncertainties in the mass estimation. It can furthermore improve the constraints on cosmological parameters (Majumdar & Mohr 2004;Mana et al 2013;To et al 2021a;Lesci et al 2022). The correlation function of galaxy clusters has also been used to identify baryonic acoustic oscillations (BAOs) independently of the cosmic microwave background (CMB, Miller et al 2001;Angulo et al 2005;Huetsi 2010;Veropalumbo et al 2014;Moresco et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Euclid preparation

Fumagalli,

Saro,

Borgani

et al. 2024

A&A

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We validate a semi-analytical model for the covariance of the real-space two-point correlation function of galaxy clusters. Using 1000 PINOCCHIO light cones mimicking the expected sample of galaxy clusters, we calibrated a simple model to accurately describe the clustering covariance. Then, we used this model to quantify the likelihood-analysis response to variations in the covariance, and we investigated the impact of a cosmology-dependent matrix at the level of statistics expected for the survey of galaxy clusters. We find that a Gaussian model with Poissonian shot-noise does not correctly predict the covariance of the two-point correlation function of galaxy clusters. By introducing a few additional parameters fitted from simulations, the proposed model reproduces the numerical covariance with an accuracy of 10\,<!PCT!>, with differences of about 5\,<!PCT!> on the figure of merit of the cosmological parameters $ m $ and $ We also find that the covariance contains additional valuable information that is not present in the mean value, and the constraining power of cluster clustering can improve significantly when its cosmology dependence is accounted for. Finally, we find that the cosmological figure of merit can be further improved when mass binning is taken into account. Our results have significant implications for the derivation of cosmological constraints from the two-point clustering statistics of the survey of galaxy clusters.

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AMICO galaxy clusters in KiDS-DR3: Constraints on cosmological parameters and on the normalisation of the mass-richness relation from clustering

Cited by 25 publications

References 72 publications

AMICO galaxy clusters in KiDS-DR3

AMICO galaxy clusters in KiDS-DR3

Cosmological Probes of Structure Growth and Tests of Gravity

Euclid preparation

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