Abstract
Galactic Archaeology, i.e. the use of chemo-dynamical information for stellar samples covering large portions of the Milky Way to infer the dominant processes involved in its formation and evolution, is now a powerful method thanks to the large recently completed and ongoing spectroscopic surveys. It is now important to ask the right questions when analyzing and interpreting the information contained in these rich datasets. To this aim, we have developed a chemodynamical model for the Milky Way that provides quantitative predictions to be compared with the chemo-kinematical properties extracted from the stellar spectra. Three key parameters are needed to make the comparison between data and model predictions useful in order to advance in the field, namely: precise proper-motions, distances and ages. The uncertainties involved in the estimate of ages and distances for field stars are currently the main obstacles in the Galactic Archaeology method. Two important developments might change this situation in the near future: asteroseismology and the now launched Gaia. When combined with the large datasets from surveys like RAVE, SEGUE, LAMOST, Gaia-ESO, APOGEE, HERMES and the future 4MOST we will have the basic ingredients for the reconstruction of the MW history in hands. In the light of these observational advances, the development of detailed chemo-dynamical models tailored to the Milky Way is urgently needed in the field. Here we show the steps we have taken, both in terms of data analysis and modelling. The examples shown here illustrate how powerful can the Galactic Archaeology method become once ages and distances are known with better precision than what is currently feasible.
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Notes
- 1.
Which is different from the fact that in different samples there are some stars wandering from other regions due to eccentric orbits—those can be easily identified by calculating their orbital parameters—see, for instance Anders et al. 2014).
- 2.
Even though, only in the particular fields observed by CoRoT and Kepler. Hopefully, with Plato much the same data can be obtained for a larger portion of the Galaxy—see Rauer and the PLATO 2.0 collaboration (2013).
- 3.
The simulation builds up a galactic disk self-consistently by gas inflow from filaments and mergers and naturally takes into account radial migration processes due to early merger activity and internal disk evolution at low redshift. A central bar is developed early on, similar in size at the final simulation time to that of the MW.
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Acknowledgements
C.C. would like to thank SDSS-III (and in particular the Brazilian and German Participation Groups) for the work done in APOGEE and SEGUE, and in particular Basilio Santiago and Leo Girardi. The RAVE collaboration is greatly acknowledged as well. Finally, I would like to thank the organizers for the invitation and for the patience in waiting for this contribution.
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Chiappini, C., Minchev, I., Anders, F., Brauer, D., Boeche, C., Martig, M. (2015). New Observational Constraints to Milky Way Chemodynamical Models. In: Miglio, A., Eggenberger, P., Girardi, L., Montalbán, J. (eds) Asteroseismology of Stellar Populations in the Milky Way. Astrophysics and Space Science Proceedings, vol 39. Springer, Cham. https://doi.org/10.1007/978-3-319-10993-0_13
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