CFHTLenS: weak lensing constraints on the ellipticity of galaxy-scale matter haloes and the galaxy-halo misalignment

We simultaneously present constraints on the stellar-to-halo mass relation for central and satellite galaxies through a weak lensing analysis of spectroscopically classified galaxies. Using overlapping data from the fourth data release of the Kilo-Degree Survey (KiDS), and the Galaxy And Mass Assembly survey (GAMA), we find that satellite galaxies are hosted by halo masses that are 0.53 ± 0.39 dex (68% confidence, 3σ detection) smaller than those of central galaxies of the same stellar mass (for a stellar mass of log(M⋆/M⊙) = 10.6). This is consistent with galaxy formation models, whereby infalling satellite galaxies are preferentially stripped of their dark matter. We find consistent results with similar uncertainties when comparing constraints from a standard azimuthally averaged galaxy-galaxy lensing analysis and a two-dimensional likelihood analysis of the full shear field. As the latter approach is somewhat biased due to the lens incompleteness and as it does not provide any improvement to the precision when applied to actual data, we conclude that stacked tangential shear measurements are best-suited for studies of the galaxy-halo connection.

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Maturing satellite kinematics into a competitive probe of the galaxy–halo connection

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/sty2950 ◽

2018 ◽

Vol 482 (4) ◽

pp. 4824-4845 ◽

Cited By ~ 7

Author(s):

Johannes U Lange ◽

Frank C van den Bosch ◽

Andrew R Zentner ◽

Kuan Wang ◽

Antonio S Villarreal

Keyword(s):

The Galaxy ◽

Galaxy Halo

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Halo cluster shapes: insights from simulated galaxies and ICL with prospects for weak lensing applications

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab2585 ◽

2021 ◽

Vol 508 (1) ◽

pp. 1280-1295

Author(s):

Elizabeth J Gonzalez ◽

Cinthia Ragone-Figueroa ◽

Carlos J Donzelli ◽

Martín Makler ◽

Diego García Lambas ◽

...

Keyword(s):

Observational Studies ◽

Semimajor Axis ◽

Galaxy Cluster ◽

Weak Lensing ◽

Cluster Galaxy ◽

Surface Mass ◽

Cluster Shape ◽

The Galaxy ◽

Hydrodynamical Simulations ◽

Intracluster Light

ABSTRACT We present a detailed study of the shapes and alignments of different galaxy cluster components using hydrodynamical simulations. We compute shape parameters from the dark matter (DM) distribution, the galaxy members and the intracluster light (ICL). We assess how well the DM cluster shape can be constrained by means of the identified galaxy member positions and the ICL. Further, we address the dilution factor introduced when estimating the cluster elongation using weak-lensing stacking techniques, which arises due to the misalignment between the total surface mass distribution and the distribution of luminous tracers. The dilution is computed considering the alignment between the DM and the brightest cluster galaxy, the galaxy members and the ICL. Our study shows that distributions of galaxy members and ICL are less spherical than the DM component, although both are well aligned with the semimajor axis of the latter. We find that the distribution of galaxy members hosted in more concentrated subhaloes is more elongated than the distribution of the DM. Moreover, these galaxies are better aligned with the DM component compared to the distribution of galaxies hosted in less concentrated subhaloes. We conclude that the positions of galaxy members can be used as suitable tracers to estimate the cluster surface density orientation, even when a low number of members is considered. Our results provide useful information for interpreting the constraints on the shapes of galaxy clusters in observational studies.

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The weak lensing radial acceleration relation: Constraining modified gravity and cold dark matter theories with KiDS-1000

Astronomy and Astrophysics ◽

10.1051/0004-6361/202040108 ◽

2021 ◽

Vol 650 ◽

pp. A113

Author(s):

Margot M. Brouwer ◽

Kyle A. Oman ◽

Edwin A. Valentijn ◽

Maciej Bilicki ◽

Catherine Heymans ◽

...

Keyword(s):

Dark Matter ◽

Galaxy Formation ◽

Modified Gravity ◽

Cold Dark Matter ◽

Weak Lensing ◽

Mass Relation ◽

Gravitational Acceleration ◽

Radial Acceleration ◽

The Galaxy ◽

The Difference

We present measurements of the radial gravitational acceleration around isolated galaxies, comparing the expected gravitational acceleration given the baryonic matter (gbar) with the observed gravitational acceleration (gobs), using weak lensing measurements from the fourth data release of the Kilo-Degree Survey (KiDS-1000). These measurements extend the radial acceleration relation (RAR), traditionally measured using galaxy rotation curves, by 2 decades in gobs into the low-acceleration regime beyond the outskirts of the observable galaxy. We compare our RAR measurements to the predictions of two modified gravity (MG) theories: modified Newtonian dynamics and Verlinde’s emergent gravity (EG). We find that the measured relation between gobs and gbar agrees well with the MG predictions. In addition, we find a difference of at least 6σ between the RARs of early- and late-type galaxies (split by Sérsic index and u − r colour) with the same stellar mass. Current MG theories involve a gravity modification that is independent of other galaxy properties, which would be unable to explain this behaviour, although the EG theory is still limited to spherically symmetric static mass models. The difference might be explained if only the early-type galaxies have significant (Mgas ≈ M⋆) circumgalactic gaseous haloes. The observed behaviour is also expected in Λ-cold dark matter (ΛCDM) models where the galaxy-to-halo mass relation depends on the galaxy formation history. We find that MICE, a ΛCDM simulation with hybrid halo occupation distribution modelling and abundance matching, reproduces the observed RAR but significantly differs from BAHAMAS, a hydrodynamical cosmological galaxy formation simulation. Our results are sensitive to the amount of circumgalactic gas; current observational constraints indicate that the resulting corrections are likely moderate. Measurements of the lensing RAR with future cosmological surveys (such as Euclid) will be able to further distinguish between MG and ΛCDM models if systematic uncertainties in the baryonic mass distribution around galaxies are reduced.

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Calibrating the Galaxy Halo – Black Hole Relation Based on the Clustering of Quasars

Growing Black Holes: Accretion in a Cosmological Context - ESO Astrophysics Symposia ◽

10.1007/11403913_6 ◽

2006 ◽

pp. 56-59

Author(s):

S. Wyithe

Keyword(s):

Black Hole ◽

The Galaxy ◽

Galaxy Halo

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The Galaxy–Halo Connection in Low-mass Halos

The Astrophysical Journal ◽

10.3847/2041-8213/aafe80 ◽

2019 ◽

Vol 871 (2) ◽

pp. L21 ◽

Cited By ~ 6

Author(s):

Robert Feldmann ◽

Claude-André Faucher-Giguère ◽

Dušan Kereš

Keyword(s):

The Galaxy ◽

Low Mass ◽

Galaxy Halo

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CoMaLit – VI. Intrinsic scatter in stacked relations. The weak lensing AMICO galaxy clusters in KiDS-DR3

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1902 ◽

2020 ◽

Vol 497 (1) ◽

pp. 894-905

Author(s):

Mauro Sereno ◽

Stefano Ettori ◽

Giorgio F Lesci ◽

Federico Marulli ◽

Matteo Maturi ◽

...

Keyword(s):

Galaxy Clusters ◽

Weak Lensing ◽

Inference Method ◽

The Third ◽

Data Release ◽

The Galaxy ◽

Bayesian Inference Method ◽

Mass Calibration ◽

The Individual ◽

Intrinsic Scatter

ABSTRACT Unbiased and precise mass calibration of galaxy clusters is crucial to fully exploit galaxy clusters as cosmological probes. Stacking of weak lensing (WL) signal allows us to measure observable–mass relations down to less massive haloes without extrapolation. We propose a Bayesian inference method to constrain the intrinsic scatter of the mass proxy in stacked analyses. The scatter of the stacked data is rescaled with respect to the individual scatter based on the number of binned clusters. We apply this method to the galaxy clusters detected with the AMICO (Adaptive Matched Identifier of Clustered Objects) algorithm in the third data release of the Kilo-Degree Survey. The results confirm the optical richness as a low-scatter mass proxy. Based on the optical richness and the calibrated WL mass–richness relation, mass of individual objects down to $\sim\! 10^{13}\, \mathrm{M}_\odot$ can be estimated with a precision of ∼20 per cent.

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Weak lensing mass reconstruction of the galaxy cluster Abell 209

Astronomy and Astrophysics ◽

10.1051/0004-6361:20066994 ◽

2007 ◽

Vol 467 (2) ◽

pp. 427-436 ◽

Cited By ~ 17

Author(s):

S. Paulin-Henriksson ◽

V. Antonuccio-Delogu ◽

C. P. Haines ◽

M. Radovich ◽

A. Mercurio ◽

...

Keyword(s):

Galaxy Cluster ◽

Weak Lensing ◽

The Galaxy ◽

Mass Reconstruction

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The galaxy–halo connection in modified gravity cosmologies: environment dependence of galaxy luminosity function

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1664 ◽

2019 ◽

Vol 488 (1) ◽

pp. 782-802 ◽

Cited By ~ 1

Author(s):

N Chandrachani Devi ◽

Aldo Rodríguez-Puebla ◽

O Valenzuela ◽

Vladimir Avila-Reese ◽

César Hernández-Aguayo ◽

...

Keyword(s):

Modified Gravity ◽

Luminosity Function ◽

Cold Dark Matter ◽

Density Field ◽

High Density ◽

Gravity Models ◽

The Galaxy ◽

Galaxy Halo ◽

Environment Dependence ◽

Galaxy Luminosity Function

Abstract We investigate the dependence of the galaxy–halo connection and galaxy density field in modified gravity models using the N-body simulations for f(R) and nDGP models at z = 0. Because of the screening mechanisms employed by these models, chameleon and Vainshtein, haloes are clustered differently in the non-linear regime of structure formation. We quantify their deviations in the galaxy density field from the standard Λ cold dark matter (ΛCDM) model under different environments. We populate galaxies in haloes via the (sub)halo abundance matching. Our main results are as follows: (1) The galaxy–halo connection strongly depends on the gravity model; a maximum variation of ${\sim }40{{\ \rm per\ cent}}$ is observed between halo occupational distribution (HOD) parameters; (2) f(R) gravity models predict an excess of galaxies in low-density environments of ${\sim }10{{\ \rm per\ cent}}$ but predict a deficit of ${\sim }10{{\ \rm per\ cent}}$ at high-density environments for |fR0| = 10−4 and 10−6 while |fR0| = 10−5 predicts more high-density structures; nDGP models are consistent with ΛCDM; (3) different gravity models predict different dependences of the galaxy luminosity function (GLF) with the environment, especially in void-like regions we find differences around ${\sim }10{{\ \rm per\ cent}}$ for the f(R) models while nDPG models remain closer to ΛCDM for low-luminosity galaxies but there is a deficit of ${\sim }11{{\ \rm per\ cent}}$ for high-luminosity galaxies in all environments. We conclude that the dependence of the GLF with environment might provide a test to distinguish between gravity models and their screening mechanisms from the ΛCDM. We provide HOD parameters for the gravity models analysed in this paper.

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The Three Hundred project: shapes and radial alignment of satellite, infalling, and backsplash galaxies

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1407 ◽

2020 ◽

Vol 495 (3) ◽

pp. 3002-3013 ◽

Cited By ~ 2

Author(s):

Alexander Knebe ◽

Matías Gámez-Marín ◽

Frazer R Pearce ◽

Weiguang Cui ◽

Kai Hoffmann ◽

...

Keyword(s):

Dark Matter ◽

Galaxy Clusters ◽

Galaxy Cluster ◽

Cluster Radius ◽

Dynamical State ◽

The Galaxy ◽

Radial Orbit ◽

Galaxy Halo ◽

Satellite Galaxies

ABSTRACT Using 324 numerically modelled galaxy clusters, we investigate the radial and galaxy–halo alignment of dark matter subhaloes and satellite galaxies orbiting within and around them. We find that radial alignment depends on distance to the centre of the galaxy cluster but appears independent of the dynamical state of the central host cluster. Furthermore, we cannot find a relation between radial alignment of the halo or galaxy shape with its own mass. We report that backsplash galaxies, i.e. objects that have already passed through the cluster radius but are now located in the outskirts, show a stronger radial alignment than infalling objects. We further find that there exists a population of well radially aligned objects passing very close to the central cluster’s centre that were found to be on highly radial orbit.

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