Volume 537, January 2012
|Number of page(s)||19|
|Section||Galactic structure, stellar clusters and populations|
|Published online||17 January 2012|
The VMC survey
1 Osservatorio Astronomico di Padova – INAF, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
2 Dipartimento di Astronomia, Università di Padova, Vicolo dell’Osservatorio 2, 35122 Padova, Italy
3 Universidade Estadual de Santa Cruz, Rodovia Ilhéus-Itabuna, km. 16 – 45662-000 Ilhéus, Bahia, Brazil
4 University of Hertfordshire, Physics Astronomy and Mathematics, Hatfield AL10 9AB, UK
5 University Observatory Munich, Scheinerstrasse 1, 81679 München, Germany
6 ICRAR M468, The University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia
7 Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Lu 5, Hai Dian District, 100871 Beijing, China
8 Department of Astronomy and Space Science, Kyung Hee University, Yongin-shi, 449-701 Kyungki-do, Republic of Korea
9 Astronomy Unit, Queen Mary University of London, Mile End Road, London E1 4NS, UK
10 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium
11 European Southern Observatory, Av. Alonso de Córdoba 3107, Casilla 19, Santiago, Chile
12 South African Astronomical Observatory, PO Box 9, 7935 Observatory, South Africa
13 Southern African Large Telescope Foundation, PO Box 9, 7935 Observatory, South Africa
14 Lennard-Jones Laboratories, Keele University, ST5 5BG, UK
Received: 9 August 2011
Accepted: 24 October 2011
We 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.
Key words: Magellanic Clouds / galaxies: evolution / infrared: stars / Hertzsprung-Russell and C-M diagrams
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2012
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