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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., Comment: Minor changes to match the version in press in MNRAS

In the last decade, several ultra faint objects (UFOs, $M_V\gtrsim-3.5$) have been discovered in the outer halo of the Milky Way. For some of these objects it is not clear whether they are star clusters or (ultra-faint) dwarf galaxies. In this work we quantify the contribution of star clusters to the population of UFOs. We extrapolated the mass and Galactocentric radius distribution of the globular clusters using a population model, finding that the Milky Way contains about $3.3^{+7.3}_{-1.6}$ star clusters with $M_V\gtrsim-3.5$ and Galactocentric radius $\geq20\,$kpc. To understand whether dissolving clusters can appear as UFOs, we run a suite of direct $N$-body models, varying the orbit, the Galactic potential, the binary fraction and the black hole (BH) natal kick velocities. In the analyses, we consider observational biases such as: luminosity limit, field stars, and line-of-sight projection. We find that star clusters contribute to both the compact and the extended population of UFOs: clusters without BHs appear compact with radii $\sim5\,$pc, while clusters that retain their BHs after formation have radii $\gtrsim20\,$pc. The properties of the extended clusters are remarkably similar to those of dwarf galaxies: high inferred mass-to-light ratios due to binaries; binary properties mildly affected by dynamical evolution; no observable mass segregation; and flattened stellar mass function. We conclude that the slope of the stellar mass function as a function of Galactocentric radius and the presence/absence of cold streams can discriminate between DM free and DM dominated UFOs., Comment: 17 pages, 17 figures; added a comment+reference in the discussion; Accepted for publication in MNRAS

We investigate the dynamical evolution of a star cluster in an external tidal field by using N-body simulations, with focus on the effects of the presence or absence of neutron star natal velocity kicks.We show that, even if neutron stars typically represent less than 2% of the total bound mass of a star cluster, their primordial kinematic properties may affect the lifetime of the system by up to almost a factor of four. We interpret this result in the light of two known modes of star cluster dissolution, dominated by either early stellar evolution mass loss or two-body relaxation. The competition between these effects shapes the mass loss profile of star clusters, which may either dissolve abruptly ("jumping"), in the pre-core-collapse phase, or gradually ("skiing"), after having reached core collapse., Comment: 5 pages, 5 figures, 1 table. Accepted for publication in MNRAS Letters

We report on a survey of astronomers asking questions at the most recent National Astronomy Meeting (NAM2014). The gender balance of both speakers and session chairs at NAM (31% and 29% women respectively) closely matched that of attendees (28% female). However, we find that women were under-represented among question askers (just 18% female). Women were especially under-represented in asking the first question (only 14% of first questions asked by women), but when the Q&A session reached four or more questions, women and men were observed to ask roughly equal numbers of questions. We found a small, but statistically insignificant, increase in the fraction of questions from women in sessions where the chair was also female. On average $2.2\pm0.1$ questions were asked per talk, with no detectable difference in the number of questions asked of female and male speakers, but on average female chairs solicited slightly fewer questions than male chairs. We compare these results to a similar study by Davenport et al. (2014) for the AAS, who also found under-representation of women amongst question askers, but saw more pronounced gender effects when a session chair or speaker were female. We conclude with suggestions for improving the balance of questions at future astronomy meetings., Comment: 15 pages, 7 figures, comments welcome