Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9

Wang, Jiaqi; Yang, Xiaohu; Zhang, Jun; Li, Hekun; Fong, Matthew; Xu, Haojie; He, Min; Gu, Yizhou; Luo, Wentao; Dong, Fuyu; Wang, Yirong; Li, Qingyang; Katsianis, Antonios; Wang, Haoran; Shen, Zhi Xiang; Alonso, Vaquero, Pedro; Liu, Cong; Yiqi, Huang,; Liu, Zhenjie

doi:10.3847/1538-4357/ac8986

Cited by 15 publications

(16 citation statements)

References 111 publications

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“…This may cause a large uncertainty in the estimate of the mean value of δlgM and the total PDF at large lgM t . In addition, Wang et al (2022) shows that there is a slight difference between halo masses determined by their ESD model and those provided by Yang et al (2021) when lgM L ∼ 14.8. Therefore we abandon the most massive bin in redshift 0.2 < z < 0.4 and 0.4 < z < 0.6, whose M L 10 14.9 M e h −1 , in fitting relation of f gas and halo mass M.…”

Section: Appendix a Relationship Between The True Mass And The Observ...mentioning

confidence: 90%

“…On the other hand, it means that the current data are not accurate enough to constrain the halo concentration. Stacking cosmic shear around these groups will constrain not only the total mass but also the concentration-mass relation (Wang et al 2022). 4.…”

Section: Discussionmentioning

confidence: 99%

“…With more accurate measurements with the upcoming surveys, the concentration (or the shape of the density profile) may become a nonnegligible ingredient. Fortunately, the sheargroup correlation could put a constraint on the halo concentration as a function of the redshift and halo mass (Wang et al 2022). In the mass bin 14.5 < lgM L < 15, the number of clusters in the mock catalog is too small to construct a precise description of the PDF.…”

Section: Discussionmentioning

confidence: 99%

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Thermal Energy Census with the Sunyaev–Zel’dovich Effect of DESI Galaxy Clusters/Groups and Its Implication on the Weak-lensing Power Spectrum

Chen,

Zhang,

Yang

2023

ApJ

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We carry out a thermal energy census of hot baryons at z < 1, by cross correlating the Planck Modified Internal Linear Combination Algorithm (MILCA) y map with 0.8 million clusters/groups selected from the Yang et al. catalog. The thermal Sunyaev–Zel’dovich effect around these clusters/groups is reliably obtained, which enables us to make our model constraints based on one-halo (1h) and two-halo (2h) contributions, respectively. (1) The total measurement signal-to-noise (S/N) of the one-halo term is 63. We constrain the Y–M relation over the halo mass range of 1013–1015 M ⊙ h −1, and find Y ∝ M α with α = 1.8 at z = 0.14 (α = 2.1 at z = 0.75). The total thermal energy of gas bound to clusters/groups increases from 0.1 meV cm−3 at z = 0.14 to 0.22 meV cm−3 at z = 0.75. (2) The 2h term is used to constrain the bias-weighted electron pressure 〈b y P e 〉. We find that 〈b y P e 〉 (in units of meV cm−3) increases from 0.24 ± 0.02 at z = 0.14 to 0.45 ± 0.02 at z = 0.75. These results lead to several implications. (i) The hot gas fraction f gas in clusters/groups monotonically increase with the halo mass, where f gas of a 1014 M ⊙ h −1 halo is ∼50% (25%) of the cosmic mean at z = 0.14 (0.75). (ii) By comparing the 1h and 2h terms, we obtain a tentative constraint on the thermal energy of unbound gas. (iii) The above results lead to significant suppression of the matter and weak-lensing power spectrum at small scales. These implications are important for astrophysics and cosmology, and we will further investigate them with improved data and gas modeling.

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Section: Appendix a Relationship Between The True Mass And The Observ...mentioning

confidence: 90%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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Thermal Energy Census with the Sunyaev–Zel’dovich Effect of DESI Galaxy Clusters/Groups and Its Implication on the Weak-lensing Power Spectrum

Chen,

Zhang,

Yang

2023

ApJ

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“…For example, Fong et al (2022) performed the first measurements of the so-called characteristic depletion radius using weak lensing data. Wang et al (2022) made use of the same weak lensing data to study halo properties of different lens samples.…”

Section: The Observed Lensing Signalsmentioning

confidence: 99%

Dark against Luminous Matter around Isolated Central Galaxies: A Comparative Study between Modern Surveys and IllustrisTNG

Pedro

Wang

Zhang

et al. 2023

ApJ

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Based on independent shear measurements using the Dark Energy Camera Legacy Survey/DR8 imaging data, we measure the weak lensing signals around isolated central galaxies (ICGs) from Sloan Digital Sky Survey/DR7 at z ∼ 0.1. The projected stellar mass density profiles of satellite galaxies are further deduced, using photometric sources from the Hyper Suprime-cam survey. The signals of ICGs + their extended stellar halos are taken from Wang et al. All measurements are compared with predictions by the IllustrisTNG300-1 simulation. We find, overall, a good agreement between observation and TNG300. In particular, a correction to the stellar mass of massive observed ICGs is applied based on the calibration of He et al., which brings a much better agreement with TNG300 predicted lensing signals at log 10 M * / M ⊙ > 11.1 . In real observation, red ICGs are hosted by more massive dark matter halos and have more satellites and more extended stellar halos than blue ICGs at fixed stellar mass. However, in TNG300 there are more satellites around blue ICGs at fixed stellar mass, and the outer stellar halos of red and blue ICGs are similar. The stellar halos of TNG galaxies are more extended compared with real observed galaxies, especially for blue ICGs with log 10 M * / M ⊙ > 10.8 . We find the same trend for TNG100 galaxies and for true halo central galaxies. The tensions between TNG and real galaxies indicate that satellite disruptions are stronger in TNG. In both TNG300 and observation, satellites approximately trace the underlying dark matter distribution beyond 0.1R 200, but the fraction of total stellar mass in TNG300 does not show the same radial distribution as real galaxies.

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“…Cosmic shear refers to the coherent shape distortion of the background galaxies due to the gravitational lensing effect by the foreground large scale density fluctuation (Kaiser 1992;Bacon et al 2000;Kaiser et al 2000;Wittman et al 2000;Bartelmann & Schneider 2001;Hoekstra & Jain 2008;Mandelbaum 2018). It has been routinely measured in galaxy surveys for the purpose of not only constraining the cosmological parameters (Schrabback et al 2010;Heymans et al 2013;Kilbinger et al 2013;Fu et al 2014;Hikage et al 2019;Heymans et al 2021;Asgari et al 2021;Doux et al 2022) , but also reconstructing density profiles of the dark matter halos, voids, filaments (Mandelbaum et al 2006;Melchior et al 2014;Clampitt et al 2016;Sánchez et al 2016;Luo et al 2018;Dong et al 2019;Schrabback et al 2021;Xu et al 2021;Fong et al 2022;Wang et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Towards Optimal Reconstruction of Shear Field with PDF-Folding

Wang¹,

Zhang²,

Li³

et al. 2023

Preprint

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Weak lensing provides a direct way of mapping the density distribution in the universe. To reconstruct the density field from the shear catalog, an important step is to build the shear field from the shear catalog, which can be quite nontrivial due to the inhomogeneity of the background galaxy distribution and the shape noise. We propose the PDF Folding method as a statistically optimal way of reconstructing the shear field. It is an extention of the PDF SYM method, which is previously designed for optimizing the stacked shear signal as well as the shear-shear correlation. PDF Folding does not require smoothing kernels as in traditional methods, therefore it suffers less information loss on small scales, and avoids possible biases due to the spatial variation of shear on the scale of the kernel. We show with analytic reasoning as well as numerical examples that the new method can reach the optimal signal-to-noise ratio on the reconstructed shear map under general observing conditions, i.e., with inhomogeneous background densities or masks. We also show the performance of the new method with real shear data around foreground galaxy clusters.

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Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9

Cited by 15 publications

References 111 publications

Thermal Energy Census with the Sunyaev–Zel’dovich Effect of DESI Galaxy Clusters/Groups and Its Implication on the Weak-lensing Power Spectrum

Thermal Energy Census with the Sunyaev–Zel’dovich Effect of DESI Galaxy Clusters/Groups and Its Implication on the Weak-lensing Power Spectrum

Dark against Luminous Matter around Isolated Central Galaxies: A Comparative Study between Modern Surveys and IllustrisTNG

Towards Optimal Reconstruction of Shear Field with PDF-Folding

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