  Emission signatures from galactic winds provide an opportunity to directly
map the outflowing gas, but this is traditionally challenging because of the
low surface brightness. Using deep observations (27 hours) of the Hubble Deep
Field South from the Multi Unit Spectroscopic Explorer (MUSE) instrument, we
identify signatures of an outflow in both emission and absorption from a
spatially resolved galaxy at z = 1.29 with a stellar mass M* = 8 x 10^9 Msun,
star formation rate SFR = 77 Msun/yr, and star formation rate surface
brightness 1.6 Msun/kpc^2 within the [OII] half-light radius R_1/2,[OII] = 2.76
+- 0.17 kpc. From a component of the strong resonant MgII and FeII absorptions
at -350 km/s, we infer a mass outflow rate that is comparable to the star
formation rate. We detect non-resonant FeII* emission, at lambda 2626, 2612,
2396, and 2365, at 1.2-2.4-1.5-2.7 x 10^-18 egs s-1 cm-2 respectively. These
flux ratios are consistent with the expectations for optically thick gas. By
combining the four non-resonant FeII* emission lines, we spatially map the
FeII* emission from an individual galaxy for the first time. The FeII* emission
has an elliptical morphology that is roughly aligned with the galaxy minor
kinematic axis, and its integrated half-light radius R_1/2,FeII* = 4.1 +- 0.4
kpc is 50% larger than the stellar continuum (R_1/2,* = 2.34 +- 0.17 kpc) or
the [OII] nebular line. Moreover, the FeII* emission shows a blue wing
extending up to -400 km/s, which is more pronounced along the galaxy minor
kinematic axis and reveals a C-shaped pattern in a p-v diagram along that axis.
These features are consistent with a bi-conical outflow.
