000002228 001__ 2228
000002228 005__ 20160706143210.0
000002228 0247_ $$2DOI$$a10.1051/0004-6361/201117863
000002228 037__ $$aASTROimport-385
000002228 100__ $$aRubele, S.
000002228 245__ $$aThe VMC survey. IV. The LMC star formation history and disk geometry from four VMC tiles
000002228 260__ $$c2012
000002228 520__ $$aWe derive the star formation history (SFH) for several regions of the Large Magellanic Cloud (LMC), using deep near-infrared data from the VISTA near-infrared YJKs survey of the Magellanic system (VMC). The regions include three almost-complete 1.4 deg2 tiles located ~3.5° away from the LMC centre in distinct directions. They are split into 21.0' × 21.5' (0.12 deg2) subregions, and each of these is analysed independently. To this dataset, we add two 11.3' × 11.3' (0.036 deg2) subregions selected based on their small and uniform extinction inside the 30 Doradus tile. The SFH is derived from the simultaneous reconstruction of two different colour-magnitude diagrams (CMDs), using the minimization code StarFISH together with a database of "partial models" representing the CMDs of LMC populations of various ages and metallicities, plus a partial model for the CMD of the Milky Way foreground. The distance modulus and extinction AV is varied within intervals ~0.2 and ~0.5 mag wide, respectively, within which we identify the best-fitting star formation rate SFR(t) as a function of lookback time t, age-metallicity relation (AMR), and AV. Our results demonstrate that VMC data, due to the combination of depth and little sensitivity to differential reddening, allow the derivation of the space-resolved SFH of the LMC with unprecedented quality compared to previous wide-area surveys. In particular, the data clearly reveal the presence of peaks in the SFR(t) at ages log (t/yr) ? 9.3 and 9.7, which appear in most of the subregions. The most recent SFR(t) is found to vary greatly from subregion to subregion, with the general trend of being more intense in the innermost LMC, except for the tile next to the N11 complex. In the bar region, the SFR(t) seems remarkably constant over the time interval from log (t/yr) ? 8.4 to 9.7. The AMRs, instead, turn out to be remarkably similar across the LMC. Thanks to the accuracy in determining the distance modulus for every subregion - with typical errors of just ~0.03 mag - we make a first attempt to derive a spatial model of the LMC disk. The fields studied so far are fit extremely well by a single disk of inclination i = 26.2 ± 2.0°, position angle of the line of nodes θ0 = 129.1 ± 13.0°, and distance modulus of mag (random errors only) up to the LMC centre. We show that once the values or each subregion are assumed to be identical to those derived from this best-fittingplane, systematic errors in the SFR(t) and AMR are reduced by a factor of about two. Based on observations made with VISTA at ESO under program ID 179.B-2003.Appendix A is available in electronic form at http://www.aanda.org
000002228 700__ $$aKerber, L.
000002228 700__ $$aGirardi, L.
000002228 700__ $$aCioni, M.-R.
000002228 700__ $$aMarigo, P.
000002228 700__ $$aZaggia, S.
000002228 700__ $$aBekki, K.
000002228 700__ $$ade Grijs, R.
000002228 700__ $$aEmerson, J.
000002228 700__ $$aGroenewegen, M. A. T.
000002228 700__ $$aGullieuszik, M.
000002228 700__ $$aIvanov, V.
000002228 700__ $$aMiszalski, B.
000002228 700__ $$aOliveira, J. M.
000002228 700__ $$aTatton, B.
000002228 700__ $$avan Loon, J. T.
000002228 773__ $$cA106$$pAstronomy and Astrophysics$$v537$$y2012
000002228 85642 $$ahttp://esoads.eso.org/abs/2012A%26A...537A.106R
000002228 905__ $$apublished in
000002228 980__ $$aREFERD