N-body and semianalytic simulations indicate that globular cluster distributions in UDG1 and Fornax require dark matter halos via dynamical friction, while DF44 yields no strong constraint.
Probing dark matter with star clusters: a dark matter core in the ultra-faint dwarf Eridanus II
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abstract
We present a new technique to probe the central dark matter (DM) density profile of galaxies that harnesses both the survival and observed properties of star clusters. As a first application, we apply our method to the `ultra-faint' dwarf Eridanus II (Eri II) that has a lone star cluster ~45 pc from its centre. Using a grid of collisional $N$-body simulations, incorporating the effects of stellar evolution, external tides and dynamical friction, we show that a DM core for Eri II naturally reproduces the size and the projected position of its star cluster. By contrast, a dense cusped galaxy requires the cluster to lie implausibly far from the centre of Eri II (>1 kpc), with a high inclination orbit that must be observed at a particular orbital phase. Our results, therefore, favour a dark matter core. This implies that either a cold DM cusp was `heated up' at the centre of Eri II by bursty star formation, or we are seeing an evidence for physics beyond cold DM.
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Globular cluster distributions as a dynamical probe of dark matter
N-body and semianalytic simulations indicate that globular cluster distributions in UDG1 and Fornax require dark matter halos via dynamical friction, while DF44 yields no strong constraint.