## However this bound is extremely strong and should motivate further work to better model the interaction of charged dark matter with ordered and disordered magnetic fields in galaxies and clusters of galaxies; to develop precise tests for the presence of charged dark matter based on better estimates of angular momentum exchange; and also to better understand how charged dark matter might modify the growth of magnetic fields, and the formation and interaction histories of galaxies, galaxy groups, and clusters.

New Limits on Charged Dark Matter from Large-Scale Coherent Magnetic Fields

## However, with appropriate means of reconstruction, such visualisation can also be used to bring out the inherent 3D structure that exists in 2D observations of known galaxies, providing new views of these galaxies and visually illustrating the spatial relationships within galaxy groups that are not obvious in 2D.

A New View of Observed Galaxies through 3D Modelling and Visualisation

## We present analysis on three intervening H I-C IV absorption systems tracing gas within galaxy group/cluster environments, identified in the $HST$/COS far-UV spectra of the background quasars PG $1148+549$ ($z_{abs}=0. C IV absorbers tracing cool gas in dense galaxy group/cluster environments ## Galaxy Group sentence examples within Ray Galaxy Group ## We use a set of 111 radio-selected AGN at 3 GHz VLA-COSMOS within the X-ray galaxy groups in the COSMOS field. The M *–M halo Relation at 0.08 < z < 1.53 in COSMOS: The Role of Active Galactic Nucleus Radio-mode Feedback ## We present a weak-lensing analysis of X-ray galaxy groups and clusters selected from the XMM-XXL survey using the first-year data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program. Weak lensing Analysis of X-Ray-selected XXL Galaxy Groups and Clusters with Subaru HSC Data ## Learn more from Galaxy Group ## Galaxy Group sentence examples within Simulated Galaxy Group ## Using the BAHAMAS and MACSIS simulations to obtain$>10,000$simulated galaxy groups and clusters, we compute three temperature measures and quantify the differences between them. Relativistic SZ temperature scaling relations of groups and clusters derived from the BAHAMAS and MACSIS simulations. ## In this study we quantify the properties of the gas and dark matter around active galactic nuclei (AGN) in simulated galaxy groups and clusters and analyze the effect of AGN feedback on the surrounding intra-cluster (group) medium. Cosmological Simulation of Galaxy Groups and Clusters-I: Global Effect of Feedback from Active Galactic Nuclei ## Galaxy Group sentence examples within Isolated Galaxy Group ## Then we carry out a series of idealized numerical simulations to model the collision of two initially isolated galaxy groups by using the TreePM-SPH GADGET-3 code. A Study of the Merger History of the Galaxy Group HCG 62 Based on X-Ray Observations and Smoothed Particle Hydrodynamic Simulations ## Its group atmosphere appears truncated and deficient when compared with isolated galaxy groups of similar temperatures. Extended X-Ray Study of M49: The Frontier of the Virgo Cluster ## Galaxy Group sentence examples within Around Galaxy Group ## We apply a spectral stacking technique to Westerbork Synthesis Radio Telescope observations to measure the neutral atomic hydrogen content (H i) of nearby galaxies in and around galaxy groups at z < 0. The atomic hydrogen content of galaxies as a function of group-centric radius ## We analyse the presence of dust around galaxy group members through the reddening of background quasars. Following the crumbs: Statistical effects of Ram Pressure in Galaxies ## Galaxy Group sentence examples within Nearby Galaxy Group ## We present deep (250 ks) Chandra observations of the nearby galaxy group NGC 1600, which has at its centre an ultramassive black hole (17±1. Probing within the Bondi radius of the ultramassive black hole in NGC 1600 ## We study a sample of 207 nearby galaxy groups and clusters observed with XMM-Newton. The non-uniformity of galaxy cluster metallicity profiles ## Galaxy Group sentence examples within galaxy group environment ## 26}$, similar to galaxy group environments and in line with previous studies for moderate-luminosity X-ray selected AGN.

The XMM-Newton Wide Field Survey in the COSMOS Field: Clustering Dependence of X-ray Selected AGN on Host Galaxy Properties

## We construct a catalog of nearby ultra-diffuse galaxies in galaxy group environments, and set upper and lower limits for the possible velocity dispersion allowed in MOND, taking into account possible variations in the mass-to-light ratio of the dwarf and in the distance to the galaxy group.

Predicted MOND velocity dispersions for a catalog of ultra-diffuse galaxies in group environments

## We run a galaxy group finder and mimic the H i stacking procedure adopted by different surveys and find we can reproduce their observationally derived HIHM relation.

Unveiling the atomic hydrogen–halo mass relation via spectral stacking

## We present a proof of concept of a new galaxy group finder method, Markov graph CLustering (MCL) that naturally handles probabilistic linking criteria.

A new approach to finding galaxy groups using Markov Clustering.

## 91 galaxy group RO-1001.

An Ancient Massive Quiescent Galaxy Found in a Gas-rich z ∼ 3 Group

## We have discovered a 300 kpc-wide giant Lyman-α (Lyα) nebula centered on the massive galaxy group RO-1001 at z = 2.

Three Lyman-α-emitting filaments converging to a massive galaxy group at z = 2.91: discussing the case for cold gas infall

10.1093/mnras/stz2483

## Galaxies and galaxy groups located along the line of sight towards gravitationally lensed quasars produce high-order perturbations of the gravitational potential at the lens position.

H0LiCOW XI: Spectroscopic/imaging survey and galaxy-group identification around the strong gravitational lens system WFI2033-4723

10.3847/1538-4357/aaf566

## The DLA is associated with an interacting galaxy pair within a galaxy group.

Discovery of a Damped Lyα System in a Low-z Galaxy Group: Possible Evidence for Gas Inflow and Nuclear Star Formation

10.1051/0004-6361/201935375

## We combined this catalog with the BCGs of galaxy groups and clusters extracted from the deeper AEGIS, CDFS, COSMOS, XMM-CFHTLS, and XMM-XXL surveys to study the stellar mass - halo mass relation using the largest sample of X-ray groups and clusters known to date.

Stellar mass-halo mass relation for the brightest central galaxies of X-ray clusters since z~0.65

10.1140/epjp/i2019-12418-4

## The data of galaxy groups of the Hercules-Bootes region are also shown to support the $\Lambda$Λ-gravity nature of the dark matter, i.

On the common nature of dark matter and dark energy: Galaxy groups

10.1002/asna.202023779

## Accurate chemical abundance measurements of X-ray-emitting atmospheres pervading massive galaxies, galaxy groups, and clusters provide essential information on the star formation and chemical enrichment histories of these large-scale structures.

How do atomic code uncertainties affect abundance measurements in the intracluster medium

10.3847/2041-8213/ab25ec

## This DLA was known to be associated with a galaxy group of dynamical mass M_group ~3e12 M_sun, but its physical origin remained ambiguous.

A Giant Intragroup Nebula Hosting a Damped $\mathrm{Ly}\alpha$ Absorber at z = 0.313

10.1051/0004-6361/201935186

## 26}$, similar to galaxy group environments and in line with previous studies for moderate-luminosity X-ray selected AGN. The XMM-Newton Wide Field Survey in the COSMOS Field: Clustering Dependence of X-ray Selected AGN on Host Galaxy Properties 10.18727/0722-6691/5126 ## At intermediate length scales (10 kpc-1 Mpc) WAVES will probe the size and mass distribution of galaxy groups, as well as the galaxy merger rates, in order to directly measure the assembly of dark matter halos and stellar mass. 4MOST Consortium Survey 7: Wide-Area VISTA Extragalactic Survey (WAVES) 10.3847/1538-4357/ab3288 ## The faintness of satellite systems in galaxy groups has contributed to the widely discussed "missing satellite" and "too big to fail" issues. MIND THE GAP: Is The Too Big To Fail Problem Resolved? 10.1051/0004-6361/201937283 ## This is a combination of increasing number of galaxy groups and their selection as identification of an X-ray sources either by chance or due to groups hosting an AGN. CODEX clusters. The Survey, the Catalog, and Cosmology of the X-ray Luminosity Function 10.1051/0004-6361/201936022 ## 3+3026 that follows the X-ray emission from the cluster center to the remnant of a galaxy group in the SW. Particle acceleration in a nearby galaxy cluster pair: the role of cluster dynamics 10.1051/0004-6361/201936467 ## We found evidence of a galaxy group infalling on RXC J1825. Growth and disruption in the Lyra complex 10.1051/0004-6361/201936114 ## We present MeerKAT observations of neutral hydrogen gas (H I) in the nearby merger remnant NGC 1316 (Fornax A), the brightest member of a galaxy group which is falling into the Fornax cluster. Neutral hydrogen gas within and around NGC 1316 10.1093/mnras/staa2235 ## We study the gas and stellar mass content of galaxy groups and clusters in the FABLE suite of cosmological hydrodynamical simulations, including the evolution of their central brightest cluster galaxies (BCGs), satellite galaxies and intracluster light (ICL). The baryon content of groups and clusters of galaxies in the FABLE simulations 10.3847/1538-4357/ab4f6d ## In addition to the clear application to the Milky Way and similar galaxies, our method can be extended to galaxy groups or clusters. A Versatile and Accurate Method for Halo Mass Determination from Phase-Space Distribution of Satellite Galaxies 10.1093/mnrasl/slz143 ## The gravitational field of a galaxy group or cluster slows down the Hubble stream and turns it speed to zero at some radius$R_0$. The radius, at which a galaxy group stops the Hubble stream, and the group mass: an exact analytical solution. 10.18727/0722-6691/5124 ## 2$, eROSITA will also detect X-ray emission from galaxy groups and filaments.

4MOST Consortium Survey 5: eROSITA Galaxy Cluster Redshift Survey

10.1093/mnras/stz1711

## 3 or greater, making this one of the most violent mergers yet observed between galaxy groups.

Building a cluster: shocks, cavities, and cooling filaments in the group–group merger NGC 6338

10.1093/mnras/stz2490

## Cosmic filaments are the channel through which galaxy groups assemble their mass.

Group connectivity in COSMOS: a tracer of mass assembly history

10.1093/mnras/stz2501

## We present an H I study of the galaxy group LGG 351 using Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY) early science data observed with the Australian Square Kilometre Array Pathfinder (ASKAP).

WALLABY early science - V. ASKAP H I imaging of the Lyon Group of Galaxies 351

10.3847/1538-4357/ab0419

## As a detection of a rare dwarf-dwarf pair beyond the Local Universe, this system provides an uncommon opportunity to explore the properties of galaxy groups in the low-galaxy mass regime as a function of redshift.

The Next Generation Fornax Survey (NGFS): V. Discovery of a dwarf-dwarf galaxy pair at z=0.30 and its characterization using deep VLT/MUSE observations

10.1051/0004-6361/201936435

## The main goal of this work is to investigate the photometric properties of the IC1459 group, and to compare our results with those obtained for other galaxy groups studied in VEGAS, in order to provide a first view of the variation of their properties as a function of the evolution of the system.

VEGAS: VST Early-type GAlaxy Survey. V. IC 1459 group: Mass assembly history in low density environments.

10.1051/0004-6361/201935394

## We characterised galaxy populations in these structures to study the influence of "pre-processing" by cosmic filaments and galaxy groups on star-formation quenching.

Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS

10.3847/2041-8213/ab412e

## We report the first detection obtained with ALMA of the [N II] 122$\mu$m line emission from a galaxy group BRI 1202-0725 at $z=4. First [NII]122$\mu$m line detection in a QSO-SMG pair BRI 1202-0725 at$z=4.69$. 10.1093/mnras/staa200 ## We created candidate lists based on a) galaxy group and cluster samples and b) photometrically selected galaxy samples. Observation and Confirmation of Nine Strong Lensing Systems in Dark Energy Survey Year 1 Data 10.1093/mnras/stz1199 ## We run two zoom-in simulations of galaxy groups with$M_{halo}>10^{13}M_\odotat z=0, selected to have quiet merger histories. mufasa: Time-scales for H i consumption and SFR depletion of satellite galaxies in groups 10.1093/mnras/stz2301 ## We study the redshift evolution of the X-ray and Sunyaev-Zel'dovich (SZ) scaling relations for galaxy groups and clusters in the FABLE suite of cosmological hydrodynamical simulations. The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations 10.3847/1538-4357/ab2ece ## We explore the interrelationships between the galaxy group halo mass and various observable group properties. The Fundamental Relation between Halo Mass and Galaxy Group Properties 10.1140/epjc/s10052-019-7081-0 ## This conclusion is drawn within modified weak-field General Relativity where the accelerated expansion of the Universe and the dynamics of galaxy groups and clusters are described by the same parameter, the cosmological constant. $$H_0$$H0 tension: clue to common nature of dark sector? 10.1093/mnras/stz1764 ## We find that the resulting luminosity dependence of the satellite red fraction is significantly shallower than corresponding measurements from galaxy group catalogues, and we provide a simple fitting function to describe this dependence. Global analysis of luminosity- and colour-dependent galaxy clustering in the Sloan Digital Sky Survey 10.1051/0004-6361/201834206 ## galaxy group catalog, finding a very good agreement with the sample of groups with 2 members. Weak-lensing analysis of galaxy pairs using CS82 data 10.3847/2041-8213/ab4885 ## The effect of black hole feedback is expected to be a strong function of halo mass, and galaxy groups and clusters are among the most massive structures in the Universe. Quantifying the effect of black hole feedback from the central galaxy on the satellite populations of groups and clusters 10.1051/0004-6361/201935810 ## In this work, we measure the alignment of shapes of satellite galaxies, in galaxy groups, with respect to the brightest group galaxy (BGG), as well as alignments of the BGG shape with the satellite positions, using the highly complete Galaxy And Mass Assembly (GAMA) spectroscopic survey and deep imaging from the Kilo Degree Survey. GAMA+KiDS: Alignment of galaxies in galaxy groups and its dependence on galaxy scale 10.1093/mnras/stz1142 ## We perform detailed mass modeling of this system using archival imaging data, and find that the unusually large shear responsible for the diamond-like configuration can be attributed mainly to a faint companion\sim 4''$away, and to a galaxy group/cluster$\sim 30''$away. A Search for Gravitationally Lensed Quasars and Quasar Pairs in Pan-STARRS1: Spectroscopy and Sources of Shear in the Diamond 2M1134$-\$2103.

10.1051/0004-6361/201629174

## Our test measures the systematic variations of the Hubble flow towards distant galaxies groups as a function of the matter distribution in the lines of sight to those galaxy groups.

Hubble flow variations as a test for inhomogeneous cosmology

10.3847/2041-8213/aafee6

## It has recently been suggested that the nearby galaxies Maffei 1 and 2 are further in distance than previously thought, such that they no longer are members of the same galaxy group as IC 342.

The Distance and Motion of the Maffei Group

## Galaxy clusters are the most massive gravitationally bound systems in the universe which grow through mergers with other clusters, galaxy groups, and accretion of gas.

Extended diffuse radio emission in galaxy clusters

10.1093/mnrasl/slz139

## We report on observations of ESO156−G029, member of a galaxy group which is positioned at the virial radius of cluster Abell 3193.

Group pre-processing versus cluster ram-pressure stripping: the case of ESO156-G029

10.1051/0004-6361/201834914

## We construct a catalog of nearby ultra-diffuse galaxies in galaxy group environments, and set upper and lower limits for the possible velocity dispersion allowed in MOND, taking into account possible variations in the mass-to-light ratio of the dwarf and in the distance to the galaxy group.

Predicted MOND velocity dispersions for a catalog of ultra-diffuse galaxies in group environments