Discovery of an optical counterpart to the hyperluminous X-ray source in ESO 243-49

The existence of black holes of masses � 10 2 -10 5 Mhas important implications for the formation and evolution of star clusters and supermassive black holes. One of the strongest candidates to date is the hyperluminous X-ray source HLX1, possibly located in the S0-a galaxy ESO243-49, but the lack of an identifiable optical counterpart had hampered its interpretation. Using the Magellan telescope, we have discovered an unresolved optical source with R = 23:80 ± 0:25 mag and V = 24:5 ± 0:3 mag within HLX1's positional error circle. This implies an average X-ray/optical flux ratio � 500. Taking the same distance as ESO243-49, we obtain an intrinsic brightness MR = 11:0±0:3 mag, comparable to that of a massive globular cluster. Alternatively, the optical source is consistent with a main-sequence M star in the Galactic halo (for example an M4.4 star at � 2:5 kpc). We also examined the properties of ESO243-49 by combining Swift/UVOT observations with stellar population modelling. We found that the overall emission is dominated by a � 5 Gyr old stellar population, but the UV emission at � 2000 u is mostly due to ongoing star-formation at a rate of � 0:03M� yr −1 . The UV emission is more intense (at least a 9� enhancement above the mean) North East of the nucleus, in the same quadrant as HLX1. With the combined optical and X-ray measurements, we put constraints on the nature of HLX1. We rule out a foreground star and a background AGN. Two alternative scenarios are still viable. HLX1 could be an accreting intermediate mass black hole in a star cluster, which may itself be the stripped nucleus of a dwarf galaxy that passed through ESO243-49, an event which might have caused the current episode of star formation. Or, it could be a neutron star in the Galactic halo, accreting from an M4-M5 donor star.