Stavros Pastras, Reinhard Genzel, Linda J. Tacconi, Karl Schuster, Roberto Neri, Natascha M. Förster Schreiber, Thorsten Naab, Capucine Barfety, Andreas Burkert, Yixian Cao, Jianhang Chen, Françoise Combes, Ric Davies, Frank Eisenhauer, Juan M. Espejo Salcedo, Santiago García-Burillo, Rodrigo Herrera-Camus, Jean-Baptiste Jolly, Lilian L. Lee, Minju M. Lee, Daizhong Liu, Dieter Lutz, Amit Nestor Shachar, Eleonora Parlanti, Sedona H. Price, Claudia Pulsoni, Alvio Renzini, Letizia Scaloni, Taro T. Shimizu, Volker Springel, Amiel Sternberg, Eckhard Sturm, Giulia Tozzi, Stijn Wuyts, Hannah Übler

We present a very deep CO(3-2) observation of a massive, gas-rich, main sequence, barred spiral galaxy at $z\approx1.52$. Our data were taken with the IRAM-NOEMA interferometer for a 12-antenna equivalent on-source integration time of $\sim$ 50 hours. We fit the major axis kinematics using forward modelling of a rotating disk, and then subtract the two-dimensional beam convolved best-fit model revealing signatures of planar non-circular motions in the residuals. The inferred in-plane radial velocities are remarkably large, of the order of $\approx60$ km/s. Direct comparisons with a high-resolution, simulated, gas-rich, barred galaxy, obtained with the moving mesh code AREPO and the TNG sub-grid model, show that the observed non-circular gas flows can be explained as radial flows driven by the central bar, with an inferred net inflow rate of the order of the SFR. Given the recent evidence for a higher-than-expected fraction of barred disk galaxies at cosmic noon, our results suggest that rapid gas inflows due to bars could be important evolutionary drivers for the dominant population of star-forming galaxies at the peak epoch of star and galaxy formation.