Spatial segregation of massive clusters in dwarf galaxies
Bruce G. Elmegreen, A. Adamo, M. Boquien, F. Bournaud, D. Calzetti, D., O. Cook, D.A. Dale, P.-A. Duc, D. M. Elmegreen, J. Fensch, K. Grasha, Hwi, Kim, L. Kahre, M. Messa, J. E. Ryon, E. Sabbi, and L.J. Smith
TL;DR
This study investigates how star clusters of different masses are spatially distributed in dwarf galaxies, revealing mass segregation in low-mass galaxies but not in high-mass ones, influenced by formation and gravitational effects.
Contribution
It provides the first evidence of mass segregation of star clusters in dwarf galaxies and explores potential causes related to galaxy mass and cluster structure.
Findings
Mass segregation observed in low-mass galaxies for irregular clusters.
No mass segregation detected in high-mass galaxies or for symmetric clusters.
Potential causes include formation differences and gravitational scattering.
Abstract
The relative average minimum projected separations of star clusters in the Legacy ExtraGalactic UV Survey (LEGUS) and in tidal dwarfs around the interacting galaxy NGC 5291 are determined as a function of cluster mass to look for cluster-cluster mass segregation. Class 2 and 3 LEGUS clusters, which have a more irregular internal structure than the compact and symmetric class 1 clusters, are found to be mass segregated in low mass galaxies, which means that the more massive clusters are systematically bunched together compared to the lower mass clusters. This mass segregation is not present in high-mass galaxies nor for class 1 clusters. We consider possible causes for this segregation including differences in cluster formation and scattering in the shallow gravitational potentials of low mass galaxies.
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