  We study the dynamical evolution of the putative gas clouds G1 and G2
recently discovered in the Galactic center. Following earlier studies
suggesting that these two clouds are part of a larger gas streamer, we combine
their orbits into a single trajectory. Since the gas clouds experience a drag
force from background gas, this trajectory is not exactly Keplerian. By
assuming the G1 and G2 clouds trace this trajectory, we fit for the drag force
they experience and thus extract information about the accretion flow at a
distance of thousands of Schwarzschild radii from the black hole. This range of
radii is important for theories of black hole accretion, but is currently
unconstrained by observations.
  In this paper we extend our previous work by accounting for radial forces due
to possible inflow or outflow of the background gas. Such radial forces drive
precession in the orbital plane, allowing a slightly better fit to the G1 and
G2 data. This precession delays the pericenter passage of G2 by 4-5 months
relative to estimates derived from a Keplerian orbital fit; if it proves
possible to identify the pericenter time observationally, this enables an
immediate test of whether G1 and G2 are gas clouds part of a larger gas
streamer. If G2 is indeed a gas cloud, its closest approach likely occurred in
late summer 2014, after many of the observing campaigns monitoring G2's
anticipated pericenter passage ended. We discuss how this affects
interpretation of the G2 observations.
