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[abridged] We used J and Ks band images acquired with the VISTA telescope aspart of the science verification to quantify the structures in the stellar diskof the barred Sc galaxy NGC253. Moving outward from the galaxy center, we finda nuclear ring within the bright 1 kpc diameter nucleus, then a bar, a ringwith 2.9 kpc radius. From the Ks image we obtain a new measure of thedeprojected length of the bar of 2.5 kpc. The bar's strength, as derived fromthe curvature of the dust lanes in the J-Ks image, is typical of weak bars.From the deprojected length of the bar, we establish the corotation radius(R_CR=3 kpc) and bar pattern speed (Omega_b = 61.3 km /s kpc), which providesthe connection between the high-frequency structures in the disk and theorbital resonances induced by the bar. The nuclear ring is located at the innerLindblad resonance. The second ring does not have a resonant origin, but itcould be a merger remnant or a transient structure formed during anintermediate stage of the bar formation. The inferred bar pattern speed placesthe outer Lindblad resonance within the optical disk at 4.9 kpc, in the sameradial range as the peak in the HI surface density. The disk of NGC253 has adown-bending profile with a break at R~9.3 kpc, which corresponds to about 3times the scale length of the inner disk. We discuss the evidence for athreshold in star formation efficiency as a possible explanation of the steepgradient in the surface brightness profile at large radii. The NIR photometryunveils the dynamical response of the NGC253 stellar disk to its central bar.The formation of the bar may be related to the merger event that determined thetruncation of stars and gas at large radii and the perturbation of the disk'souter edge.

The NIR structure of the barred galaxy NGC253 from VISTA