The G2+G2t complex as a fast and massive outflow?
  Observations of the gas component of the cloud G2 in the Galactic Center have
revealed its connection to a tail (G2t) lying on the same orbit. More recent
studies indicate a connection between G2 and G1, another cloud detected on the
blueshifted side of G2's orbit, suggesting a scenario in which G2 is a denser
clump in a stream of gas. In this Letter we show that a simulation of an
outflow by a central source (possibly a T Tauri star) moving on G2's orbit and
interacting with a hot atmosphere surrounding SgrA* can have G2 and G2t as a
byproduct. G2 would be the bow-shock formed in the head of the source, while
G2t might be the result of the stripping of the rest of the shocked material by
the ram pressure of the surrounding hot gas and of its successive accumulation
in the trailing region. Mock position-velocity diagrams for the Br$\gamma$
emission for this simulation can indeed reproduce the correct position and
velocity of G2t, as well as the more tenuous material in between. Though some
tension between the observations and the simulated model remains, we argue that
this might be due to issues in the construction of observed position-velocity
(PV) diagrams and/or to a poor treatment of some physical processes - like
hydrodynamic mixing - in our simulation.
