First measurement of the characteristic depletion radius of dark matter haloes from weak lensing

Fong, Matthew; Han, Jiaxin; Zhang, Jun; Yang, Xiaohu; Gao, Hongyu; Wang, Jiaqi; Li, Hekun; Katsianis, Antonios; Pedro, Alonso,

doi:10.1093/mnras/stac1263

“…Recent works have measured 𝑅 id and 𝑅 cd from observations. Fong et al (2022) made the first measurements of 𝑅 cd using weak lensing observations. Li & Han (2021) measured the 𝑅 id of the Milky Way using the motion of nearby dwarf galaxies.…”

Section: Introductionmentioning

confidence: 99%

A physical and concise halo model based on the depletion radius

Zhou¹,

Han²

2023

Preprint

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0

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We develop a self-consistent and accurate halo model by partitioning matter according to the depletion radii of haloes. Unlike conventional models that define haloes with the virial radius while relying on a separate exclusion radius or ad-hoc fixes to account for halo exclusion, our model distributes mass across all scales self-consistently. Using a cosmological simulation, we show that our halo definition leads to very simple and intuitive model components, with the one-halo term given by the Einasto profile with no truncation needed, and the halo-halo correlation function following a universal power-law form down to the halo boundary. The universal halo-halo correlation also allows us to easily model the distribution of unresolved haloes as well as diffuse matter. Convolving the halo profile with the halo-halo correlation function, we obtain a complete description of the halo-matter correlation across all scales, which self-consistently accounts for halo exclusion on the transition scale. Mass conservation is explicitly maintained in our model, and the scale dependence of the classical halo bias is easily reproduced. Our model can successfully reconstruct the halo-matter correlation function with percent level accuracy for halo virial masses in the range of 10 11.5 ℎ −1 M < 𝑀 vir < 10 15.35 ℎ −1 M at 𝑧 = 0, and covers the radial range of 0.01ℎ −1 Mpc < 𝑟 < 20ℎ −1 Mpc. We also show that our model profile can accurately predict the characteristic depletion radius at the minimum bias and the splash-back radius at the steepest density slope locations.

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“…A few recent works have used this shear measurement method and have calculated the lensing signals with it. 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

¹

,

Wang

²

,

Zhang

³

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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“…where M h is the halo mass and f (x) bears the following form with x = R/r s : On the other hand, if the candidate lens galaxy is not located at the center of the host halo, but with an off-center distance R off , the projected surface density will change from an NFW profile Σ NFW (R) to In the halo model, if we consider the mass or galaxy outside the host halo, which we call the two-halo term, we need to take into the halo exclusion effect (Wang et al 2004). Here, we use the following function to describe this effect in the halo matter In addition to the halo exclusion effect, to accurately model the cross-correlation functions at large scales, one needs to take into account the scale dependence of the halo bias, ζ(r, z) (see Fong et al 2022 for a more sophisticated treatment at this scale). Following van den Bosch et al (2013), we start from the one obtained by Tinker et al (2005), given by…”

Section: 0637mentioning

confidence: 99%

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

Wang

¹

,

Yang

²

,

Zhang

³

et al. 2022

ApJ

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Based on a large group/cluster catalog recently constructed from the DESI Legacy Imaging Surveys DR9 using an extended halo-based group finder, we measure and model the group–galaxy weak-lensing signals for groups/clusters in a few redshift bins within redshift range 0.1 ≤ z < 0.6. Here, the background shear signals are obtained based on the DECaLS survey shape catalog, derived with the Fourier_Quad method. We divide the lens samples into five equispaced redshift bins and seven mass bins, which allow us to probe the redshift and mass dependence of the lensing signals, and hence the resulting halo properties. In addition to these sample selections, we also check the signals around different group centers, e.g., the brightest central galaxy, the luminosity-weighted center, and the number-weighted center. We use a lensing model that includes off-centering to describe the lensing signals that we measure for all mass and redshift bins. The results demonstrate that our model predictions for the halo masses, biases, and concentrations are stable and self-consistent among different samples for different group centers. Taking advantage of the very large and complete sample of groups/clusters, as well as the reliable estimations of their halo masses, we provide measurements of the cumulative halo mass functions up to redshift z = 0.6, with a mass precision at 0.03 ∼ 0.09 dex.

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First measurement of the characteristic depletion radius of dark matter haloes from weak lensing

Cited by 20 publications

References 115 publications

A physical and concise halo model based on the depletion radius

A physical and concise halo model based on the depletion radius

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

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

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