2017ApJ...848...78F

We utilize the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope to search for extended Lyα emission around the z ∼ 6.6 QSO J0305-3150. After carefully subtracting the point spread function, we reach a nominal 5σ surface-brightness limit of SB_5σ = 1.9 x 10^–18 erg s^–1 cm^–2 arcsec^–2 over a 1 arcsec² aperture, collapsing five wavelength slices centered at the expected location of the redshifted Lyα emission (i.e., at 9256 Å). Current data suggest the presence (5σ accounting for systematics) of a Lyα nebula that extends for 9 kpc around the QSO. This emission is displaced and redshifted by 155 km s^–1 with respect to the location of the QSO host galaxy traced by the [C II] 158 µm emission line. The total luminosity is L(Lyα) = (3.0 ± 0.4) x 10⁴² erg s^–1. Our analysis suggests that this emission is unlikely to rise from optically thick clouds illuminated by the ionizing radiation of the QSO. It is more plausible that the Lyα emission is due to the fluorescence of the highly ionized optically thin gas. This scenario implies a high hydrogen volume density of n_H∼6 cm^–3. In addition, we detect a Lyα emitter (LAE) in the immediate vicinity of the QSO, i.e., with a projected separation of ∼12.5 kpc and a line-of-sight velocity difference of 560 km s^–1. The luminosity of the LAE is L(Lyα) = (2.1 ± 0.2) x 10⁴² erg s^–1 and its inferred star-formation rate is SFR ∼ 1.3 M_☉ yr^–1. The probability of finding such a close LAE is one order of magnitude above the expectations based on the QSO-galaxy cross-correlation function. This discovery is in agreement with a scenario where dissipative interactions favor the rapid build-up of supermassive black holes at early cosmic times.