Chemical Gradients in the Milky Way from the Rave Chemical Abundances Catalogue

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The RAVE project is an ongoing large spectroscopic survey which aims at observing up to 1 million stars of the Milky Way in order to measure radial velocities, stellar parameters and chemical abundances. RAVE spectra cover the wavelength region between 8410 and 8795 Angstrom with spectral resolution of R 7500. We present the RAVE chemical catalogue which currently holds chemical abundances for up to 12 elements of 88000 RAVE stars. For these stars we have also estimated distances, absolute velocities and galactic orbit parameters. This is currently the richest data set for chemo-kinematic investigations of the Milky Way.
We focused our first investigation on the present structure of the Galaxy, investigating its chemical evolution by measuring the chemical gradients along the galactic radius. By using a sample of 3549 dwarf stars we measured the chemical gradients for 6 elements (Mg, Al, Si, Ca Ti, Fe). We found that stars with low vertical velocities |W| (which stay close to the galactic plane) show an iron gradient in agreement with previous works. However, stars with larger |W|, which are able to reach larger altitudes (Zmax) above the galactic plane, show progressively flatter gradients as function of |Zmax|. The gradients of the other elements follow this trend. In particular, stars with higher |W| that kinematically are classified as thick disk stars, exhibit a chemical composition typical of thin disk stars. The picture coming from the RAVE data does not easily fit the Milky Way formation scenario commonly accepted today. We suggest the possibility that these ``transition stars" having thick disk kinematic and thin disk chemical composition (already detected by other authors) might be an evolutionary connection between the thin and thick disk of the Milky Way.

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