Constraints on the fuzzy dark matter mass using globular clusters in dwarf galaxies from Euclid ERO data
Abstract
We constrain the particle mass of the fuzzy dark matter model using globular cluster candidates in dwarf galaxies, from the Euclid Early Release Observations, within the Fornax and Perseus galaxy clusters. We model the orbital evolution of globular clusters by combining fuzzy dark matter density profiles with the corresponding dynamical friction formalism, and integrate their orbits using galpy. In the fuzzy dark matter framework, both the halo density profile and the dynamical friction force are modified by the wave-like nature of the ultra-light dark matter particle, whose mass is parameterized as m22=mχ/10−22,eV and explored over the range 0.1 ≤ m22 ≤ 100. This framework naturally alleviates the long-standing globular cluster timing problem originally identified in the Fornax dSph. We find that globular clusters no longer experience orbital decay toward the centers of their host galaxies for m22≤1.46+0.51−0.32 in the Fornax cluster and m22≤1.09+0.14−0.21 in the Perseus cluster. Future Euclid data releases, providing substantially larger samples of globular cluster candidates, will enable significantly tighter constraints on the dark matter particle mass within the fuzzy dark matter scenario.
Related
- SHARP(ening the) view of unresolved globular clusters in ultra diffuse galaxies
- Isochrone fitting of Galactic globular clusters - IX. Tip of the red-giant branch for 27 clusters and constraints on new particle physics
- Euclid: Quick Data Release (Q1) -- Exploring the detailed visual morphology of galaxies in clusters
- Euclid Quick Data Release (Q1). Mass-to-light ratio of elliptical galaxies: constraints from strong lensing
- Tighter dark-matter constraints from the projected mass method: A neural-network-enhanced method for galaxy groups and clusters
BibTeX
@misc{besnard2026constraints,
title = {{Constraints on the fuzzy dark matter mass using globular clusters in dwarf galaxies from Euclid ERO data}},
author = {Lisa Besnard and Pierre Boldrini and Paola Di Matteo and Chervin Laporte and Teymoor Saifollahi},
howpublished = {HAL},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.11328},
eprint = {2609.11328},
archivePrefix = {arXiv},
url = {https://hal.science/hal-05761205v1},
}
RIS
TY - UNPB
TI - Constraints on the fuzzy dark matter mass using globular clusters in dwarf galaxies from Euclid ERO data
AU - Lisa Besnard
AU - Pierre Boldrini
AU - Paola Di Matteo
AU - Chervin Laporte
AU - Teymoor Saifollahi
PY - 2026
DA - 2026/09/10
PB - HAL
DO - 10.48550/arxiv.2609.11328
UR - https://hal.science/hal-05761205v1
AB - We constrain the particle mass of the fuzzy dark matter model using globular cluster candidates in dwarf galaxies, from the Euclid Early Release Observations, within the Fornax and Perseus galaxy clusters. We model the orbital evolution of globular clusters by combining fuzzy dark matter density profiles with the corresponding dynamical friction formalism, and integrate their orbits using galpy. In the fuzzy dark matter framework, both the halo density profile and the dynamical friction force are modified by the wave-like nature of the ultra-light dark matter particle, whose mass is parameterized as m_22=m_χ/10^−22,eV and explored over the range 0.1 ≤ m_22 ≤ 100. This framework naturally alleviates the long-standing globular cluster timing problem originally identified in the Fornax dSph. We find that globular clusters no longer experience orbital decay toward the centers of their host galaxies for m_22≤1.46^+0.51_−0.32 in the Fornax cluster and m_22≤1.09^+0.14_−0.21 in the Perseus cluster. Future Euclid data releases, providing substantially larger samples of globular cluster candidates, will enable significantly tighter constraints on the dark matter particle mass within the fuzzy dark matter scenario.
ER -