In this review, I will discuss the comparison between model results and observational data for the Milky Way, the predictive power of such models as well as their limits. Such a comparison, known as Galactic archaeology, allows us to impose constraints on stellar nucleosynthesis and timescales of formation of the various Galactic components (halo, bulge, thick disk and thin disk).

Modeling the chemical evolution of the Milky Way

In this review I will discuss the comparison between model results and observational data for the Milky Way, the predictive power of such models as well as their limits. Such a comparison, known as Galactic archaeology, allows us to impose constraints on stellar nucleosynthesis and timescales of formation of the various Galactic components (halo, bulge, thick disk and thin disk).

Modelling the chemical evolution of the Milky Way

Searches of large scale surveys have resulted in the discovery of over 1000 brown dwarfs in the Solar neighbourhood. In this chapter we review the progress in finding brown dwarfs in large datasets, highlighting the key science goals, and summarising the surveys that have contributed most significantly to the current sample.

Large Scale Searches for Brown Dwarfs and Free-Floating Planets

We describe a proposal for a public IR variability survey of the entire Milky Way Bulge and a large portion of the Southern Galactic Plane with VISTA at ESO Paranal Observatory The survey will take about 180 nights, covering 5�0^8 point sources within an area of about 600 sq deg, including 40 known globular clusters and more than one hundred known open clusters The final products of our VVV survey will be a deep IR atlas of the bulge and inner disk, along with a catalogue of more than a million variable point sources These will allow to map the 3-D structure of the bulge and inner disk (unlike single epoch surveys that only give 2-D maps) using well understood primary distance indicators such as RR-Lyrae stars, and to obtain important information on the age of the Milky Way stellar populations The survey will also detect hundreds of star formation regions, and allow to examine the environmental dependence of star formation The VISTA observations will be combined with data from MACHO, OGLE, EROS, 2MASS, DENIS, VST, SPITZER, HST, CHANDRA, INTEGRAL and ALMA for a complete understanding of the variable sources in the inner Milky Way Several important implications for the history of the Milky Way, for globular cluster evolution, for the population census of the bulge and center, and for pulsation theory would follow from this survey

Vista Variables in the Via Lactea (VVV)

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