Prospects for Determining the Mass Distributions of Galaxy Clusters on Large Scales Using Weak Gravitational Lensing

Fong, Matthew; Bowyer, Rachel; Whitehead, Alfred J.; Lee, B; King, Lindsay J.; Applegate, Douglas; McCarthy, Ian G.

doi:10.1093/mnras/sty1339

Cited by 15 publications

(8 citation statements)

References 42 publications

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“…The depletion radius is located in between the halo scale and the linear scale of matter growth. This intermediate scale has already been studied in many previous works both theoretically and observationally (e.g., Cooray & Sheth 2002;Tasitsiomi et al 2004;Weinberg et al 2004;Sheldon et al 2004;Mandelbaum et al 2005;Prada et al 2006;Hayashi & White 2008;Fong et al 2018;Garcia et al 2020;Fong & Han 2021;Diemer 2021). However, the characterization of the depletion region is new and the potential uses have yet to be fully realized.…”

Section: Introductionmentioning

confidence: 79%

“…Recently a natural and physically meaningful halo radius has been introduced, relating halo accretion to the halo boundary, called the splashback radius (Diemer & Kravtsov 2014; ★ matthew.fong@sjtu.edu.cn † jiaxin.han@sjtu.edu.cn ‡ betajzhang@sjtu.edu.cn 2014; More et al 2015;Shi 2016). It has proven to be a powerful tool that can potentially probe halo properties that have previously been hidden and has been measured in observations (More et al 2016;Snaith et al 2017;Umetsu & Diemer 2017;Baxter et al 2017;Mansfield et al 2017;Okumura et al 2017;Fong et al 2018;Chang et al 2018;Okumura et al 2018;Contigiani et al 2019;Xhakaj et al 2020;Sugiura et al 2020;Aung et al 2021;Murata et al 2020;Deason et al 2020a,b;Zhang et al 2021;O'Neil et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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

Fong,

Han,

Zhang

et al. 2022

Preprint

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We use weak lensing observations to make the first measurement of the characteristic depletion radius, one of the three radii that characterize the region where matter is being depleted by growing haloes. The lenses are taken from the halo catalog produced by the extended halo-based group/cluster finder applied to DESI Legacy Imaging Surveys DR9, while the sources are extracted from the DECaLS DR8 imaging data with the F _Q pipeline. We study halo masses 12 < log(𝑀 grp [M /ℎ]) ≤ 15.3 within redshifts 0.2 ≤ 𝑧 ≤ 0.3. The virial and splashback radii are also measured and used to test the original findings on the depletion region. When binning haloes by mass, we find consistency between most of our measurements and predictions from the C G simulation, with exceptions to the lowest mass bins. The characteristic depletion radius is found to be roughly 2.5 times the virial radius and 1.7 − 3 times the splashback radius, in line with an approximately universal outer density profile, and the average enclosed density within the characteristic depletion radius is found to be roughly 29 times the mean matter density of the Universe in our sample. When binning haloes by both mass and a proxy for halo concentration, we do not detect a significant variation of the depletion radius with concentration, on which the simulation prediction is also sensitive to the choice of concentration proxy. We also confirm that the measured splashback radius varies with concentration differently from simulation predictions.

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Section: Introductionmentioning

confidence: 79%

Section: Introductionmentioning

confidence: 99%

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

Fong,

Han,

Zhang

et al. 2022

Preprint

View full text Add to dashboard Cite

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“…The proposed density profile has been used to find the steepest point in spherically averaged dark matter, stellar and subhalo profiles in simulations (e.g. More et al 2015;Fong et al 2018;Xhakaj et al 2020;Deason et al 2020b) and in observational work using galaxies as traces of dark matter density (More et al 2016;Baxter et al 2017;Chang et al 2018;Shin et al 2019;Murata et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The splashback boundary of haloes in hydrodynamic simulations

O'Neil,

Barnes,

Vogelsberger

et al. 2020

Preprint

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The splashback radius, R sp , is a physically motivated halo boundary that separates infalling and collapsed matter of haloes. We study R sp in the hydrodynamic and dark matter only IllustrisTNG simulations. The most commonly adopted signature of R sp is the radius at which the radial density profiles are steepest. Therefore, we explicitly optimise our density profile fit to the profile slope and find that this leads to a ∼ 5% larger radius compared to other optimisations. We calculate R sp for haloes with masses between 10 13−15 M as a function of halo mass, accretion rate and redshift. R sp decreases with mass and with redshift for haloes of similar M 200m in agreement with previous work. We also find that R sp /R 200m decreases with halo accretion rate. We apply our analysis to dark matter, gas and satellite galaxies associated with haloes to investigate the observational potential of R sp . The radius of steepest slope in gas profiles is consistently smaller than the value calculated from dark matter profiles. The steepest slope in galaxy profiles, which are often used in observations, tends to agree with dark matter profiles but is lower for less massive haloes. We compare R sp in hydrodynamic and N-body dark matter only simulations and do not find a significant difference caused by the addition of baryonic physics. Thus, results from dark matter only simulations should be applicable to realistic haloes.

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“…The gravitational interplay between dark matter and baryons plays a crucial role in describing the structures of galaxy clusters. Generally speaking, most of the studies for galaxy clusters rely on X-ray observations (Reiprich et al 2013;Balogh et al 2011;Chan 2014Chan , 2020, numerical simulations (Munari et al 2016;Henden, Puchwein & Sijacki 2020;Qiu et al 2020) and gravitational lensing (Fong et al 2018;Jauzac, Harvey & Massey 2018;Meneghetti et al 2020). In particular, X-ray observation of the hot gas is the most conventional way to study galaxy clusters, which can tell us about the hot gas distribution and probe the dark matter content.…”

Section: Introductionmentioning

confidence: 99%

Two analytic relations connecting the hot gas astrophysics with the cold dark matter model for galaxy clusters

Chan

2021

Preprint

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Galaxy clusters are good targets for examining our understanding of cosmology. Apart from numerical simulations and gravitational lensing, X-ray observation is the most common and conventional way to analyze the gravitational structures of galaxy clusters. Therefore, it is valuable to have simple analytical relations that can connect the observed distribution of the hot, X-ray emitting gas to the structure of the dark matter in the clusters as derived from simulations. In this article, we apply a simple framework that can analytically connect the hot gas empirical parameters with the standard parameters in the cosmological cold dark matter model. We have theoretically derived two important analytic relations, r s ≈ √ 3r c and ρ s ≈ 9βkT /8πGm g r 2 c , which can easily relate the dark matter properties in galaxy clusters with the hot gas properties. This can give a consistent picture describing gravitational astrophysics for galaxy clusters by the hot gas and cold dark matter models.

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Prospects for Determining the Mass Distributions of Galaxy Clusters on Large Scales Using Weak Gravitational Lensing

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Cited by 15 publications

References 42 publications

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

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

The splashback boundary of haloes in hydrodynamic simulations

Two analytic relations connecting the hot gas astrophysics with the cold dark matter model for galaxy clusters

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