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tokens: jet emanating from Sgr A*: the jet collides with the Eastern arm of the Sgr A West H ii region, driving a shock front which is observable in infrared and radio, and accelerating relativistic electrons which are seen in X-ray. The long axis of the hypothetical jet path corresponds to an azimuthal angle φ ∼ (−35 ± 2)°. If the jet propagates along the rotation axis, this measurement is consistent with our finding that φ ∼ (−32 ± 23)°. The rotation axis is also similar to that inferred by jet models of Markoff, Bower Falcke ( 2007 ), θ ≳ 75°, φ ∼ −25°, and model-dependent constraints on the spin axis by Meyer et al. ( 2007 ), φ ∼ − 25°. Surprisingly, this rotation axis is also nearly coincident with the Galaxy's rotation axis, φ = −317 (Reid Brunthaler 2004 ). Since we find a rotation axis misaligned with both the stellar clockwise disc (by ∼90°), and with G2 (by ∼60°), our model argues against scenarios in which gas in the accretion flow originates from either of these sources. The rotation axis we identify does align quite closely with the circumnuclear disc, a massive torus of molecular gas with an inner edge ∼1.5 pc from Sgr A* (θ = 118° ± 15°, φ = −25° ± 15°; Jackson et al. 1993 ). Our analysis suggests that the gas in the accretion flow hails from the circumnuclear disc, rather than from the young clockwise stellar disc as is commonly assumed. In addition to constraining the rotation axis of the accretion flow, we find degenerate relationships between the gas density and magnetic field strength, and between the rotation profile and the shape of the G2 cloud. These degeneracies could be broken with further observations, yielding first measurements of the gas density and rotation speed at radii of 100s of au in the Galactic centre. This is an exciting possibility, because these measurements would constrain the thermodynamics and momentum transport within the accretion flow, providing important information about the physics of black hole accretion in low-luminosity systems such as Sgr A*. We find that G2's motion is with the accretion flow rather than against it (Fig. 8 ; cf. Sadowski et al. 2013a ). With a relative inclination of ∼60° between G2's pre-pericentre orbit and the accretion flow, this is similar to the M3 simulation of Abarca, Sadowski Sironi ( 2014 ). This lowers the relative velocity somewhat, and may help explain non-detections of the bow-shock ahead of the cloud (e.g. Bower et al. 2015 ; Tsuboi et al. 2015 ). A potentially important effect we have not included in our analysis is the back-reaction of the drag force on to the accretion flow; since the combined mass of G1 and G2 is comparable to the total amount of gas in the accretion flow, the drag force acting on the clouds could also influence the evolution of the accretion flow. This is a complex process, as the back-reaction depends on angular momentum transport in the accretion flow and could be affected by magnetic fields, turbulent transport, and viscosity; we have