SAMI and TNG-Cluster: tracing galaxy spin and environmental transformation across cluster phase-space and cosmic time
4 affiliations
- 1Departamento Acadêmico de Física, Universidade Tecnológica Federal do Paraná , Rua Sete de Setembro 3165, Curitiba, PR ,
- 2European Southern Observatory , Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München ,
- 3Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo , Rua do Matão 1226, São Paulo, SP ,
- 4Department of Physics, College of Natural and Mathematical Sciences, University of Dodoma , 1 Benjamin Mkapa Road, 41218 Iyumbu, Dodoma ,
Abstract
The dense environment of galaxy clusters suppresses star formation and alters the kinematic properties of infalling satellites through gas stripping, tidal interactions, gravitational harassment, and starvation. Projected phase-space diagrams connect the present-day distribution of cluster galaxies to their accretion histories. We combine Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey integral field spectroscopy with the TNG-Cluster simulation to investigate how the stellar spin parameter (λ R), (g−i) colour, and specific star formation rate (sSFR) vary across projected phase-space infall regions. At z = 0, TNG-Cluster reproduces the direction and broad strength of the phase-space trends observed in SAMI, including the weak yet significant λ R–clustercentric distance correlation. Leveraging this agreement, we extend the analysis across the last 8 Gyr, tracing the statistical evolution of galaxy properties within each infall region, and complement this with individual orbital histories of representative satellites. While colour and sSFR show clear monotonic gradients with both phase-space position and cosmic time, λ R behaves differently: It remains largely uniform across the outer infall regions, with only the virialized core exhibiting systematically lower values, and displays a slow monotonic decline towards the present day across all regions. We find that angular momentum suppression driven by the cluster environment is a slow, cumulative process requiring several Gyr of exposure to the cluster core, modulated by orbital history and stellar mass. This gradual nature explains why the λ R–environment correlation appears weak across phase-space regions in statistical samples; the effect emerges when individual satellite histories are tracked, revealing a sustained dynamical response to prolonged cluster residence.
Versions
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BibTeX
@article{goncalves2026sami,
title = {{SAMI and TNG-Cluster: tracing galaxy spin and environmental transformation across cluster phase-space and cosmic time}},
author = {Gustavo F Gonçalves and Ilaria Marini and A Fraser-McKelvie and Natan de Isídio and Rubens E G Machado and Richards P Albuquerque and Daudi T Mazengo},
journal = {Monthly Notices of the Royal Astronomical Society},
year = {2026},
month = oct,
doi = {10.1093/mnras/stag1960},
url = {https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1960/8917826},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - SAMI and TNG-Cluster: tracing galaxy spin and environmental transformation across cluster phase-space and cosmic time
AU - Gustavo F Gonçalves
AU - Ilaria Marini
AU - A Fraser-McKelvie
AU - Natan de Isídio
AU - Rubens E G Machado
AU - Richards P Albuquerque
AU - Daudi T Mazengo
PY - 2026
DA - 2026/10/15
JO - Monthly Notices of the Royal Astronomical Society
DO - 10.1093/mnras/stag1960
UR - https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1960/8917826
AB - The dense environment of galaxy clusters suppresses star formation and alters the kinematic properties of infalling satellites through gas stripping, tidal interactions, gravitational harassment, and starvation. Projected phase-space diagrams connect the present-day distribution of cluster galaxies to their accretion histories. We combine Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey integral field spectroscopy with the TNG-Cluster simulation to investigate how the stellar spin parameter (λ _R), (g−i) colour, and specific star formation rate (sSFR) vary across projected phase-space infall regions. At z = 0, TNG-Cluster reproduces the direction and broad strength of the phase-space trends observed in SAMI, including the weak yet significant λ _R–clustercentric distance correlation. Leveraging this agreement, we extend the analysis across the last 8 Gyr, tracing the statistical evolution of galaxy properties within each infall region, and complement this with individual orbital histories of representative satellites. While colour and sSFR show clear monotonic gradients with both phase-space position and cosmic time, λ _R behaves differently: It remains largely uniform across the outer infall regions, with only the virialized core exhibiting systematically lower values, and displays a slow monotonic decline towards the present day across all regions. We find that angular momentum suppression driven by the cluster environment is a slow, cumulative process requiring several Gyr of exposure to the cluster core, modulated by orbital history and stellar mass. This gradual nature explains why the λ _R–environment correlation appears weak across phase-space regions in statistical samples; the effect emerges when individual satellite histories are tracked, revealing a sustained dynamical response to prolonged cluster residence.
SN - 0035-8711
SN - 1365-2966
ER -