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If the Galaxy is axisymmetric and in dynamical equilibrium, we expectnegligible fluctuations in the residual line-of-sight velocity field. Recentresults using the \apg{} survey find significant fluctuations in velocity forstars in the midplane ($|z|<$0.25 kpc) out to 5 kpc, suggesting that thedynamical influence of non-axisymmetric features i.e., the Milky Way's bar,spiral arms and merger events extends out to the Solar neighborhood. Theirmeasured power spectrum has a characteristic amplitude of 11 \kms{} on a scaleof 2.5 kpc. The existence of such large-scale streaming motions has importantimplications for determining the Sun's motion about the Galactic Centre. UsingRed Clump stars from \glh{} and \apg{}, we map the line-of-sight velocitiesaround the Sun (d$<$5 kpc), and $|z|<$1.25 kpc from the midplane. Bysubtracting a smooth axisymmetric model for the velocity field, we study theresidual fluctuations and compare our findings with mock survey generated by\glx{}. We find negligible large-scale fluctuations away from the plane. In themid-plane, we reproduce the earlier \apg{} power spectrum but with 20\% smalleramplitude (9.3 \kms{}) after taking into account a few systematics (e.g.,volume completeness). Using a flexible axisymmetric model the power-amplitudeis further reduced to 6.3 \kms{}. Additionally, our simulations show that, inthe plane, distances are underestimated for high-mass Red Clump stars which canlead to spurious power-amplitude of about 5.2 \kms{}. Taking this into account,we estimate the amplitude of real fluctuations to be $<$4.6 \kms{}, about afactor of three less than the \apg{} result.

The GALAH Survey: Velocity fluctuations in the Milky Way using red clump giants