2025/08/19 by Tang, Xiao-xiao, Wang, Peng, Rong, Yu +2
#Astrophysics of Galaxies (astro-ph.GA) #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences
paper · doi:10.48550/arxiv.2508.13597
The spin of galaxy clusters encodes key information about their formation, dynamics, and the influence of large-scale structure. However, whether clusters possess statistically significant spin and how to measure it observationally remain open questions. Here, we present the first observational, statistical detection of coherent spin in galaxy clusters, using two samples of 2,170 and 1,329 systems with M > 1014 M_\odot, selected from two publicly available group catalogs (\citet2017A&A...602A.100T and \citet2012ApJ...752...41Y) constructed with two different algorithms and but both based primarily on SDSS galaxies. Cluster spin is quantified by identifying the orientation in the projected plane that maximizes the redshift difference (ΔZ\rm max) between member galaxies in two regions divided by a trial axis. We find compelling statistical evidence for coherent rotation, as the observed ΔZ\rm max distribution departs markedly from the randomized controls, exhibiting pronounced deviations near 380 \mathrmkm s-1. Stacked visualizations confirm the spatial segregation of redshifted and blueshifted galaxies across the rotation axis. The radial profile of the rotational velocity indicates that it increases as a function of radius. The cluster rotation speed increases with mass, from ∼360~km s-1 at 1014 M_\odot to ∼693~km s-1 at 1015 M_\odot. Additionally, cluster spin tends to align parallel with the central galaxy spin and perpendicular to the nearest cosmic filament, particularly in richer systems. These results reveal significant coherent spin in galaxy clusters, shaped by both internal dynamics and large-scale structure.