2021MNRAS.507.4294Z

Using deep (11.2 h) VLT/MUSE data from the MEGAFLOW survey, we report the first detection of extended Mg II emission from a galaxy's halo that is probed by a quasar sightline. The Mg II λλ2796, 2803 emission around the z = 0.702 galaxy (log(M_*/M☉_)=10.05-0.11_^+0.15) is detected out to ~25 \hboxkpc from the central galaxy and covers 1.0×10³ kpc^2^ above a surface brightness of 14×10^–19 erg s^–1 cm^–2 arcsec^–2 (2 σ; integrated over 1200 km s^–1= 19Åand averaged over 1.5 arcsec²). The Mg II emission around this highly inclined galaxy (i ≃ 75 deg) is strongest along the galaxy's projected minor axis, consistent with the Mg II gas having been ejected from the galaxy into a bi-conical structure. The quasar sightline, which is aligned with the galaxy's minor axis, shows strong Mg II absorption (\hboxEW_0^λ2796^=1.8 Å) at an impact parameter of 39 \hboxkpc from the galaxy. Comparing the kinematics of both the emission and the absorption - probed with VLT/UVES - to the expectation from a simple toy model of a bi-conical outflow, we find good consistency when assuming a relatively slow outflow (v_out=130 km s^–1). We investigate potential origins of the extended Mg II emission using simple toy models. With continuum scattering models we encounter serious difficulties in explaining the luminosity of the Mg II halo and in reconciling density estimates from emission and absorption. Instead, we find that shocks might be a more viable source to power the extended Mg II (and non-resonant [O II]) emission.