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We present a novel approach to disentangle two key contributions to thelargest-scale anisotropy of the galaxy distribution: (i) the intrinsic dipoledue to clustering and anisotropic geometry, and (ii) the kinematic dipole dueto our peculiar velocity. Including the redshift and angular size of galaxies,in addition to their fluxes and positions allows us to measure both thedirection and amplitude of our velocity independently of the intrinsic dipoleof the source distribution. We find that this new approach applied to futuregalaxy surveys (LSST and Euclid) and a SKA radio continuum survey will allow tomeasure our velocity ($\beta = v/c$) with a relative error in the amplitude$\sigma(\beta)/\beta \sim (1.3 - 4.5)\%$ and in direction, $\theta_{\beta} \sim0.9^\circ - 3.9^\circ$, well beyond what can be achieved when analysing onlythe number count dipole. We also find that galaxy surveys are able to measurethe intrinsic large-scale anisotropy with a relative uncertainty of $\lesssim5\%$ (measurement error, not including cosmic variance). Our method enables twosimultaneous tests of the Cosmological Principle: comparing the observations ofour peculiar velocity with the CMB dipole, and testing for a significantintrinsic anisotropy on large scales which would indicate effects beyond thestandard cosmological model.

A new way to test the Cosmological Principle: measuring our peculiar velocity and the large scale anisotropy independently