C$^3$-Cluster Clustering Cosmology II. First detection of the BAO peak in the three-point correlation function of galaxy clusters

Moresco, Michele; Veropalumbo, Alfonso; Marulli, Federico; Moscardini, Lauro; Cimatti, Andrea

doi:10.48550/arxiv.2011.04665

Cited by 5 publications

(5 citation statements)

References 99 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Galaxy clusters are hosted by the most massive virialised CDM haloes, and their redshift evolution (number density and spatial distribution) is highly sensitive to different cosmological parameters (see e.g. Planck Collaboration XXIV 2016; Vikhlinin et al 2009;Veropalumbo et al 2014Veropalumbo et al , 2016Pacaud et al 2018;Marulli et al 2018Marulli et al , 2020Costanzi et al 2019;Moresco et al 2020;Lesci et al 2020;Nanni et al, in prep. ).…”

Section: Introductionmentioning

confidence: 99%

AMICO galaxy clusters in KiDS-DR3

Giocoli

Marulli

Moscardini

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Introductionmentioning

confidence: 99%

AMICO galaxy clusters in KiDS-DR3

Giocoli

Marulli

Moscardini

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…As a simple method, two-dimensional three-point angular statistics have been observed from the dawn of the study of cosmological three-point statistics to the present (Peebles & Groth 1975;Peebles 1975;Groth & Peebles 1977;Fry & Peebles 1980;Fry & Seldner 1982;Sharp et al 1984;Jing & Zhang 1989;Jing et al 1991;Toth et al 1989;Frieman & Gaztañaga 1999;Szapudi et al 2001;de Carvalho et al 2020). Eventually, with the development of spectroscopic observations of galaxies, three-dimensional three-point statistics have become the primary targets observed in configuration space (Bean et al 1983;Efstathiou & Jedrzejewski 1994;Hale-Sutton et al 1989;Gott et al 1991;Jing & Borner 1998;Jing & Börner 2004;Kayo et al 2004;Wang et al 2004;Nichol et al 2006;Kulkarni et al 2007;Gaztañaga et al 2009;Marin 2011;McBride et al 2011a,b;Marin et al 2013;Guo et al 2014;Moresco et al 2017a;Slepian et al 2017a;Slepian et al 2017b;Moresco et al 2017bMoresco et al , 2020 or in Fourier space (Baumgart & Fry 1991;Scoccimarro et al 2001a;Feldman et al 2001;Verde et al 2002;Nishimichi et al 2007;Gil-Marín et al 2...…”

Section: Developments In the Study Of Galaxy Three-point Statisticsmentioning

confidence: 99%

New constraints on cosmological modified gravity theories from anisotropic three-point correlation functions of BOSS DR12 galaxies

Sugiyama¹,

Yamauchi²,

Kobayashi³

et al. 2023

Preprint

View full text Add to dashboard Cite

We report a new test of modified gravity theories using the large-scale structure of the Universe. This paper is the first attempt to (1) apply a joint analysis of the anisotropic components of galaxy two-and three-point correlation functions (2 and 3PCFs) to actual galaxy data and (2) constrain the nonlinear effects of degenerate higher-order scalar-tensor (DHOST) theories on cosmological scales. Applying this analysis to the Baryon Oscillation Spectroscopic Survey (BOSS) data release 12, we obtain the lower bounds of −1.655 < ξ t and −0.504 < ξ s at the 95% confidence level on the parameters characterising the time evolution of the tidal and shift terms of the second-order velocity field. These constraints are consistent with GR predictions of ξ t = 15/1144 and ξ s = 0. Moreover, they represent a 35-fold and 20-fold improvement, respectively, over the joint analysis with only the isotropic 3PCF. We ensure the validity of our results by investigating various quantities, including theoretical models of the 3PCF, window function corrections, cumulative S/N, Fisher matrices, and statistical scattering effects of mock simulation data. We also find statistically significant discrepancies between the BOSS data and the Patchy mocks for the 3PCF measurement. Finally, we package all of our 3PCF analysis codes under the name HITOMI and make them publicly available so that readers can reproduce all the results of this paper and easily apply them to ongoing future galaxy surveys.

show abstract

“…Examples in the literature include estimates from the 2dFGRS (Jing & Börner 2004), various releases of the SDSS main sample (Kayo et al 2004;Nichol et al 2006;Kulkarni et al 2007;McBride et al 2011a,b;Marín 2011;Guo et al 2014), the BOSS CMASS (Guo et al 2015) and the first Public Data Release (PDR1) of the VIPERS survey (Moresco et al 2017). Only recently, however, thanks to a breakthrough in the efficiency of available estimators, it has become possible to push measurements of the 3PCF to scales comparable to those of the BAO peak (Slepian & Eisenstein 2015;Slepian et al 2017a,b), also using galaxy clusters as tracers (Moresco et al 2020). Finally, combined 2PCF and 3PCF analyses in configuration space were performed by Marín et al (2013) using the WiggleZ spectroscopic galaxy survey.…”

Section: Introductionmentioning

confidence: 99%

A joint 2- and 3-point clustering analysis of the VIPERS PDR2 catalogue at z~1: breaking the degeneracy of cosmological parameters

Veropalumbo,

Casares,

Branchini

et al. 2021

Preprint

View full text Add to dashboard Cite

We measure the galaxy 2-and 3-point correlation functions at 𝑧 = [0.5, 0.7] and 𝑧 = [0.7, 0.9], from the final data release of the VIPERS survey (PDR2). We model the two statistics including a nonlinear 1-loop model for the 2-point function and a tree-level model for the 3-point function, and perform a joint likelihood analysis. The entire process and nonlinear corrections are tested and validated through the use of the 153 highly realistic VIPERS mock catalogues, showing that they are robust down to scales as small as 10 ℎ −1 Mpc. The mocks are also adopted to compute the covariance matrix that we use for the joint 2-and 3-point analysis. Despite the limited statistics of the two (volume-limited) sub-samples analysed, we demonstrate that such a combination successfully breaks the degeneracy existing at 2-point level between clustering amplitude 𝜎 8 , linear bias 𝑏 1 and the linear growth rate of fluctuations 𝑓 . For the latter, in particular, we measure 𝑓 (𝑧 = 0.61) = 0.64 +0.55 −0.37 and 𝑓 (𝑧 = 0.8) = 1.0 ± 1.0, while the amplitude of clustering is found to be 𝜎 8 (𝑧 = 0.61) = 0.50 ± 0.12 and 𝜎 8 (𝑧 = 0.8) = 0.39 +0.11 −0.13 . These values are in excellent agreement with the extrapolation of a Planck cosmology.

show abstract

C$^3$-Cluster Clustering Cosmology II. First detection of the BAO peak in the three-point correlation function of galaxy clusters

Cited by 5 publications

References 99 publications

AMICO galaxy clusters in KiDS-DR3

AMICO galaxy clusters in KiDS-DR3

New constraints on cosmological modified gravity theories from anisotropic three-point correlation functions of BOSS DR12 galaxies

A joint 2- and 3-point clustering analysis of the VIPERS PDR2 catalogue at z~1: breaking the degeneracy of cosmological parameters

Contact Info

Product

Resources

About