2017MNRAS.467..836S

Abell 1201 is a massive galaxy cluster at z = 0.169 with a brightest cluster galaxy (BCG) that acts as a gravitational lens to a background source at z = 0.451. The lensing configuration is unusual, with a single bright arc formed at small radius (∼2 arcsec), where stars and dark matter are both expected to contribute substantially to the total lensing mass. Here, we present deep spectroscopic observations of the Abell 1201 BCG with MUSE (Multi-Unit Spectroscopic Explorer), which reveal emission lines from a faint counterimage, opposite to the main arc, at a radius of 0.6 arcsec. We explore models in which the lensing mass is described by a combination of stellar mass and a standard dark matter halo. The counterimage is not predicted in such models, unless the dark matter component is negligible, which would imply an extremely heavy stellar initial mass function (IMF) in this galaxy. We consider two modifications to the model, which can produce the observed configuration without resorting to extreme IMFs. Imposing a radial gradient in the stellar mass-to-light ratio, U, can generate a counterimage close to the observed position if U increases by >= 60 per cent within the inner ∼1 arcsec (e.g. variation from a Milky Way-like to a Salpeter-like IMF). Alternatively, the counterimage can be produced by introducing a central supermassive black hole. The required mass is M_BH = (1.3 ± 0.6) x 10¹⁰ M_☉, which is comparable to the largest black holes known to date, several of which are also hosted by BCGs. We comment on future observations that promise to distinguish between these alternatives.