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We derive the star formation history for several regions of the LMC, usingdeep near-infrared data from the VISTA near-infrared YJKs survey of theMagellanic system (VMC). The regions include three almost-complete 1.4 sqdegtiles located 3.5 deg away from the LMC centre in distinct directions. To thisdataset, we add two 0.036 sqdeg subregions inside the 30 Doradus tile. The SFHis derived from the simultaneous reconstruction of two different CMDs, usingthe minimization code StarFISH. The distance modulus (m-M)_0 and extinction Avis varied within intervals 0.2 and 0.5 mag wide, respectively, within which weidentify the best-fitting star formation rate SFR(t), age-metallicity relation(AMR), (m-M)_0 and Av. Our results demonstrate that VMC data, due to thecombination of depth and little sensitivity to differential reddening, allowthe derivation of the space-resolved SFH of the LMC with unprecedented qualitycompared to previous wide-area surveys. In particular, the data clearly revealthe presence of peaks in the SFR(t) at ages log(t/yr)=9.3 and 9.7, which appearin most of the subregions. The most recent SFR is found to vary greatly fromsubregion to subregion, with the general trend of being more intense in theinnermost LMC, except for the tile next to the N11 complex. In the bar region,the SFR seems remarkably constant over the time interval from 8.4 to 9.7. TheAMRs, instead, turn out to be remarkably similar across the LMC. The fieldsstudied so far are fit extremely well by a single disk of inclination 26.2+-2.0deg, position angle of the line of nodes 129.1+-13.0 deg, and distance modulusof 18.470+-0.006 mag (random errors only) up to the LMC centre.

The VMC Survey IV. The LMC star formation history and disk geometry from four VMC tiles