KiDS+GAMA: The weak lensing calibrated stellar-to-halo mass relation of central and satellite galaxies

Dvornik, Andrej; Hoekstra, Henk; Kuijken, Konrad; Wright, Angus H.; Asgari, Marika; Bilicki, Maciej; Erben, T.; Giblin, Benjamin; Graham, Alister W.; Heymans, Catherine; Hildebrandt, Hendrik; Hopkins, A. M.; Kannawadi, Arun; Lin, Chieh Yu; Taylor, Edward N.; Tröster, Tilman

doi:10.1051/0004-6361/202038693

Cited by 18 publications

(11 citation statements)

References 72 publications

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“…Figure D1 shows that, at the same M , massive satellite galaxies show very different ∆Σ profiles with centrals due to the strong impact from their host dark matter halos. Despite the small impact on the stacked ∆Σ profiles due to the low satellite fraction value, the ∆Σ profile of massive satellite galaxies alone contains valuable information about the galaxy-halo connection of massive galaxies (e.g., Sifón et al 2015;Li et al 2016b;Dvornik et al 2020). We will aim to understand it more so that we can deal with satellites better when using M -based Mvir proxies.…”

Section: Appendix D: ∆σ Profiles Of Massive Satellite Galaxiesmentioning

confidence: 99%

The Outer Stellar Mass of Massive Galaxies: A Simple Tracer of Halo Mass with Scatter Comparable to Richness and Reduced Projection Effects

Huang,

Leauthaud,

Bradshaw

et al. 2021

Preprint

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Using the weak gravitational lensing data from the Hyper Suprime-Cam Subaru Strategic Program (HSC survey), we study the potential of different stellar mass estimates in tracing halo mass. We consider galaxies with log 10 (M /M )> 11.5 at 0.2 < z < 0.5 with carefully measured light profiles, and clusters from the redMaP-Per and CAMIRA richness-based algorithms. We devise a method (the "Top-N test") to evaluate the scatter in the halo mass-observable relation for different tracers, and to inter-compare halo mass proxies in four number density bins using stacked galaxygalaxy lensing profiles. This test reveals three key findings. Stellar masses based on CModel photometry and aperture luminosity within R <30 kpc are poor proxies of halo mass. In contrast, the stellar mass of the outer envelope is an excellent halo mass proxy. The stellar mass within R = [50, 100] kpc, M ,[50,100] , has performance comparable to the state-of-the-art richness-based cluster finders at log 10 M vir 14.0 and could be a better halo mass tracer at lower halo masses. Finally, using N-body simulations, we find that the lensing profiles of massive halos selected by M , [50,100] are consistent with the expectation for a sample without projection or mis-centering effects. Richness-selected clusters, on the other hand, display an excess at R ∼ 1 Mpc in their lensing profiles, which may suggest a more significant impact from selection biases. These results suggest that M -based tracers have distinct advantages in identifying massive halos, which could open up new avenues for cluster cosmology. The codes and data used in this work can be found here:

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Section: Appendix D: ∆σ Profiles Of Massive Satellite Galaxiesmentioning

confidence: 99%

The Outer Stellar Mass of Massive Galaxies: A Simple Tracer of Halo Mass with Scatter Comparable to Richness and Reduced Projection Effects

Huang,

Leauthaud,

Bradshaw

et al. 2021

Preprint

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“…This inference might be unfeasible in practice due to the highdimensional parameter space. Third, HODs are important tools to constrain the stellar-to-halo mass ratio, traditionally obtained from second-order statistics, such as galaxy-galaxy-lensing (Velander et al 2014;van Uitert et al 2018;Dvornik et al 2020). Combining these measurements with the HOD constraints from G3L could lead to tighter constraints on the relationship between baryonic and dark matter.…”

Section: Discussionmentioning

confidence: 99%

KiDS+VIKING+GAMA: Halo occupation distributions and correlations of satellite numbers with a new halo model of the galaxy-matter bispectrum for galaxy-galaxy-galaxy lensing

Linke,

Simon,

Schneider

et al. 2022

Preprint

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Context. Halo models and halo occupation distributions (HODs) are important tools to model the distribution of galaxies and matter. Aims. We present and assess a new method for constraining the parameters of HODs using the mean gravitational lensing shear around galaxy pairs, so-called galaxy-galaxy-galaxy-lensing (G3L). In contrast to galaxy-galaxy-lensing, G3L is also sensitive to the correlations between the per-halo numbers of galaxies from different populations. We employ our G3L halo model to probe these correlations and test the default hypothesis that they are negligible. Methods. We derive a halo model for G3L and validate it with realistic mock data from the Millennium Simulation and a semianalytic galaxy model. Then, we analyse public data from the Kilo-Degree Survey (KiDS), the VISTA Infrared Kilo-Degree Galaxy Survey (VIKING) and data from the Galaxy And Mass Assembly Survey (GAMA) to infer the HODs of galaxies at z < 0.5 in five different stellar mass bins between 10 8.5 h −2 M and 10 11.5 h −2 M and two colours (red and blue), as well as correlations between satellite numbers. Results. The analysis accurately recovers the true HODs in the simulated data for all galaxy samples within the 68% credibility range. The model best-fits agree with the observed G3L signal on the 95% confidence level. The inferred HODs vary significantly with colour and stellar mass. In particular red galaxies prefer more massive halos 10 12 M , while blue galaxies are present in halos 10 11 M . There is strong evidence (> 3σ) for a high correlation, increasing with halo mass, between the numbers of red and blue satellites and between galaxies with stellar masses below 10 10 M . Conclusions. Our G3L halo model accurately constrains galaxy HODs for lensing surveys of up to 10 3 deg 2 and redshift below 0.5 probed here. Analyses of future surveys may need to include non-Poisson variances of satellite numbers or a revised model for central galaxies. Correlations between satellite numbers are ubiquitous between various galaxy samples and are relevant for halos with masses 10 13 M , that is, of galaxy group scale and more massive. Possible causes of these correlations are the selection of similar galaxies in different samples, the survey flux limit, or physical mechanisms like a fixed ratio between the satellite numbers of distinct populations. The decorrelation for halos with smaller masses is probably an effect of shot noise by low-occupancy halos. The inferred HODs can be used to complement galaxy-galaxy-lensing or galaxy clustering HOD studies or as input to cosmological analyses and improved mock galaxy catalogues.

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“…Weak gravitational lensing is a very useful technique to get the halo masses for groups/clusters sample selected according to their observable properties (for e.g. Mandelbaum et al 2006b;Okabe et al 2010;Gruen et al 2014;Viola et al 2015;Simet et al 2016;Dvornik et al 2017;Sereno et al 2017;Luo et al 2018;Murata et al 2018;Bellagamba et al 2019;Miyatake et al 2019;Murata et al 2019;Taylor et al 2020;Renneby et al 2020;Umetsu 2020;Dvornik et al 2020;Giocoli et al 2021). In contrast to other methods, the weak gravitational lensing gives a halo mass estimate independent of assumptions and uncertainties on the physical properties of the groups/clusters.…”

Section: Introductionmentioning

confidence: 99%

The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

Rana,

More,

Miyatake

et al. 2021

Preprint

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We utilize the galaxy shape catalogue from the first year data release of the Subaru Hyper Suprime-cam Survey (HSC) to study the dark matter content of galaxy groups in the Universe using weak gravitational lensing. As our lens sample, we use galaxy groups that have been spectroscopically selected from the Galaxy Mass and Assembly (GAMA) galaxy survey in approximately 100 sq. degrees of the sky that overlap with the HSC survey. We restrict our analysis to the 1587 groups with at least five group members. We divide these galaxy groups into six bins each of galaxy group luminosity and group member velocity dispersion and measure the coherent tangential ellipticity pattern on background HSC galaxies imprinted by weak gravitational lensing. We measure the weak lensing signal with a total signal-to-noise ratio of 55 and 51 for these two different selections, respectively. We use a Bayesian halo model framework to infer the halo mass distribution of our galaxy groups binned in the two different observable properties and obtain constraints on the power law scaling relation between mean halo masses and the two group observable properties. We obtain a 5 percent constraint on the amplitude of the scaling relation between halo mass and group luminosity with 𝑀 = (0.81 ± 0.04) × 10 14 ℎ −1 𝑀 for 𝐿 grp = 10 11.5 ℎ −2 𝐿 , and a power law index of 𝛼 = 1.01 ± 0.07. We also obtain a 5 percent constraint on the amplitude of the scaling relation between halo mass and velocity dispersion with 𝑀 = (0.93 ± 0.05) × 10 14 ℎ −1 𝑀 for 𝜎 = 500km s −1 and a power law index 𝛼 = 1.52 ± 0.10, although these scaling relations are sensitive to the exact cuts applied to the number of group members. Comparisons with similar scaling relations from the literature indicate that our results are consistent, but have significantly reduced errors.

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KiDS+GAMA: The weak lensing calibrated stellar-to-halo mass relation of central and satellite galaxies

Cited by 18 publications

References 72 publications

The Outer Stellar Mass of Massive Galaxies: A Simple Tracer of Halo Mass with Scatter Comparable to Richness and Reduced Projection Effects

The Outer Stellar Mass of Massive Galaxies: A Simple Tracer of Halo Mass with Scatter Comparable to Richness and Reduced Projection Effects

KiDS+VIKING+GAMA: Halo occupation distributions and correlations of satellite numbers with a new halo model of the galaxy-matter bispectrum for galaxy-galaxy-galaxy lensing

The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

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