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We investigate the kinematic signatures induced by spiral and bar structurein a set of simulations of Milky Way-sized spiral disc galaxies. The setincludes test particle simulations that follow a quasi-stationary densitywave-like scenario with rigidly rotating spiral arms, and $N$-body simulationsthat host a bar and transient, co-rotating spiral arms. From a location similarto that of the Sun, we calculate the radial, tangential and line-of-sightpeculiar velocity fields of a patch of the disc and quantify the fluctuationsby computing the power spectrum from a two-dimensional Fourier transform. Wefind that the peculiar velocity power spectrum of the simulation with a bar andtransient, co-rotating spiral arms fits very well to that of APOGEE red clumpstar data, while the quasi-stationary density wave spiral model without a bardoes not. We determine that the power spectrum is sensitive to the number ofspiral arms, spiral arm pitch angle and position with respect to the spiralarm. However, it is necessary to go beyond the line of sight velocity field inorder to distinguish fully between the various spiral models with this method.We compute the power spectrum for different regions of the spiral discs, anddiscuss the application of this analysis technique to external galaxies.

Spiral and bar driven peculiar velocities in Milky Way sized galaxy simulations