Galactic Dynamics and Evolution in Cluster Environments
Summary
Clusters of galaxies represent the most massive bound structures in the Universe, where the high galaxy density and hot intracluster medium foster a variety of processes that drive galactic evolution. The gravitational potential of a cluster and the hydrodynamic pressure of its gas act in concert to strip and heat the interstellar medium of member galaxies, quenching star formation and transforming late-type systems into early-type morphologies. Tidal forces from close encounters and the overall cluster potential can distort stellar distributions, create diffuse streams and substructures, and reshape galaxy kinematics. Meanwhile, the dark matter halo plays a critical role by anchoring the galaxy against disruptive influences and setting the stage for long-term dynamical stability. Observations across the electromagnetic spectrum have characterised the removal of atomic and molecular gas, the onset of morphological transformations, and the varying timescales over which different mass regimes respond to environmental effects. Pre-processing in groups and filaments prior to cluster infall further complicates this picture, seeding galaxies with altered gas reservoirs and dynamical signatures that persist in the main cluster. This multifaceted interplay of gravitational and hydrodynamic interactions underpins the transformation pathways of galaxies in dense environments, with implications for large-scale structure formation and the baryon cycle on cosmological scales.
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Galactic Dynamics and Evolution in Cluster Environments publication trend
The graph below shows the total number of articles in galactic dynamics and evolution in cluster environments across all publications each year (not limited to Nature Index journals).
Technical terms
Ram pressure stripping: Removal of a galaxy’s gas by the pressure exerted by the hot intracluster medium as the galaxy moves through it.
Tidal interactions: Gravitational perturbations from close encounters or the cluster potential that distort stellar and gas distributions.
Pre-processing: Evolutionary alterations experienced by galaxies in groups or filaments prior to infall into the main cluster.
Atomic hydrogen (HI): Neutral hydrogen gas detectable via its 21 cm emission line, serving as a tracer of the cold interstellar medium.
Molecular gas (H2): Cold molecular hydrogen, often traced by CO emission, which directly fuels star formation.
Fundamental Plane: Empirical relation linking galaxy size, surface brightness and velocity dispersion, used to probe structural and dynamical properties.
Dark matter fraction: The proportion of a galaxy’s total mass attributed to dark matter within a given radius.
Dwarf early-type galaxies (dEs): Low-mass galaxies with smooth light profiles and little ongoing star formation, often found in clusters.
References
- The MeerKAT Fornax Survey. Astronomy & Astrophysics (2023).
- CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array. The Astrophysical Journal Supplement Series (2022).
- Witnessing a Transformation to Blue-cored Dwarf Early-type Galaxies in Filaments and the Cluster Outskirts: Gas-phase Abundances and Internal Kinematics Perspectives. The Astrophysical Journal (2023).
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