Webpage: GES (Gaia-ESO spectroscopic Survey)
Description of the project:
- The Gaia-ESO Public Spectroscopic Survey
Gilmore et al., 2012Msngr.147...25G
- "The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars",
Smiljanic et al. 2014A&A...570A.122S
- “Gaia-ESO Survey: Analysis of pre-main sequence stellar spectra”,
Lanzafame et al., 2015A&A...576A..80L
Gaia-ESO is a public spectroscopic survey, targeting ≥ 105 stars, systematically covering all major components of the MilkyWay, from halo to star forming regions, providing the first homogeneous overview of the distributions of kinematics and elemental abundances. This alone will revolutionise knowledge of Galactic and stellar evolution: when combined with Gaia astrometry the survey will quantify the formation history and evolution of young, mature and ancient Galactic populations. With well-defined samples, we will survey the bulge, thick and thin discs and halo components, and open star clusters of all ages and masses. The Fibre Large Array Multi Element Spectrograph (FLAMES) spectra will: quantify individual elemental abundances in each star; yield precise radial velocities for a 4-D kinematic phase-space; map kinematic gradients and abundance - phase-space structure throughout the Galaxy; follow the formation, evolution and dissolution of open clusters as they populate the disc, and provide a legacy dataset that adds enormous value to the Gaia mission and ongoing ESO imaging surveys.
David Montes is the institutional representative of UCM node in the GES working groups (WG). The SEEF group participate in the WG 11 (UVES FGK stars) and WG 12 (pre-main sequence stars) and has developed (Tabernero 2014, PhD. Thesis UCM) automatic tools to derive stellar atmospheric parameters: effective temperature (Teff), surface gravity (logg), metallicity ([Fe/H]), and the microturbulent velocity (ξ ) as well as abundances (i.e., [X/H], [X/Fe]) for 20 different chemical elements (Na, Mg, Al, Si, Ca, Ti, V, Cr, Mn, Co, Fe, Ni, Cu, Zn, Y, Zr, Ba, Ce, and Nd) of FGK stars using the equivalent width (EW) method. The automatics codes StePar and SteAbu developed have been tested with well known stars (benchmarks stars) providing very accuracy results and used to apply the “Chemical Tagging” technique to test the common origin of two young stellar kinematic groups. Thismethodology has been used to analyse in an automatic way the large amount of UVES spectra coming from the Gaia-ESO spectroscopic Survey (GES) from FGK field stars and member of open clusters of different ages. This collaboration with GES results in several papers recently published about the methodology (Sousa et al. 2014, A&A, 561, A21; Smiljanic et al. 2014, A&A, 570, A122; Lanzafame et al. 2015, A&A., 576, A80), the benchmark stars tests (Jofré et al. 2014, A&A, 564, A133; 2015, A&A, 582, A81), the particular analysis of two young open clusters: gamma Velorum (Spina et al., 2014, A&A, 567, A55: Frasca et al. 2015, A&A, 575, A4) and Chamaeleon I (Spina et al., 2014, A&A, 568, A2) and the test of the chemical tagging technique with open clusters (Blanco-Cuaresma et al. 2015, A&A, 577, A47). In addition a new PhD student (M.L. Gutiérrez Albarran) is working with the detailed analysis of the lithium abundances to derive a calibration of the Li-age relation (2017hsa9.conf..507G) using the information of all the open clusters observed within GES.