Events · Journal Talk
Journal Talk 21: Md Fardin Islam (2026)
Tracing the Evolution of the Morphology–Density Relation Across z ~ 1.5 to z = 0 in Cosmological Hydrodynamical Simulations.
Tracing the Evolution of the Morphology–Density Relation Across z ~ 1.5 to z = 0 in Cosmological Hydrodynamical Simulations.
Abstract
Galaxies do not evolve in isolation. Their properties are strongly influenced by the environments in which they live. In the present day (z = 0) Universe, dense environments such as galaxy groups and clusters contain a larger fraction of early-type and quenched galaxies, while lower-density field environments contain more star-forming disk galaxies. This connection between galaxy morphology and environment is known as the morphology–density relation. Although this relation is well known at low redshift, it is still important to understand when it first became established and how it developed over cosmic time.
In this work, we aim to study the emergence of the morphology–density relation from z ~ 1.5 to z = 0 using cosmological hydrodynamical simulation data. We plan to select galaxies from simulation catalogues at different redshift snapshots and compare their properties in different environments, such as field regions, groups, and cluster environments. The galaxies will be studied in terms of stellar mass, star-formation rate (SFR), and morphology (sersic index, CAS, M20 and other identifiers).
The main goal of this work is to investigate whether galaxies in dense environments become morphologically different from galaxies in low-density environments gradually over time, and to identify the redshift range where this relation becomes significant. Galaxy morphology may be studied using structural indicators such as Sersic index, concentration, asymmetry, Gini coefficient, M20, ellipticity, or particle-based morphology. We will also examine how the quenched galaxy population changes with environment and redshift, in order to understand whether morphological transformation and star-formation quenching occur together or on different timescales. This study will help explore how environment, halo growth, and quenching processes contribute to the formation of the present-day galaxy population.
Presenter: Md Fardin Islam (Undergraduate Research Assistant at CASSA; B.Sc. (ongoing) in Physics, Independent University, Bangladesh)
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