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We present the first metallicity gradient measurement for a grand-designface-on spiral galaxy at z~1.5. This galaxy has been magnified by a factor of22$\times$ by a massive, X-ray luminous galaxy cluster MACS\,J1149.5+2223 atz=0.544. Using the Laser Guide Star Adaptive Optics aided integral fieldspectrograph OSIRIS on KECK II, we target the Halpha emission and achieve aspatial resolution of 0.1", corresponding to a source plane resolution of 170pc. The galaxy has well-developed spiral arms and the nebular emission linedynamics clearly indicate a rotationally supported disk with V_{rot}/\sigma~4.The best-fit disk velocity field model yields a maximum rotation of V_{rot}sin{i}=150$\pm$15 km s^{-1}, and a dynamical mass ofM_{dyn}=1.3$\pm0.2\times10^{10}csc^2(i) M_{\odot} (within 2.5\,kpc), where theinclination angle i=45$\pm10^{\circ}$. Based on the [NII] and Halpha ratios, wemeasured the radial chemical abundance gradient from the inner hundreds ofparsecs out to ~5 kpc. The slope of the gradient is -0.16$\pm$0.02 dexkpc$^{-1}$, significantly steeper than the gradient of late-type or early-typegalaxies in the local universe. If representative of disk galaxies at z~1.5,our results support an "inside-out" disk formation scenario in which earlyinfall/collapse in the galaxy center builds a chemically enriched nucleus,followed by slow enrichment of the disk over the next 9 Gyr.

Metallicity Gradient of a Lensed Face-on Spiral Galaxy at Redshift 1.49