/ftp/cats/aliases/K/./KHI2013



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J/A+A/555/A12       Foreground Galactic stars properties     (Kordopatis+, 2013)
The following files can be converted to FITS (extension .fit or fit.gz)
	table2.dat table4.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/555/A12
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Beginning of ReadMe : J/A+A/555/A12 Foreground Galactic stars properties (Kordopatis+, 2013) ================================================================================ Through thick and thin: Structure of the Galactic thick disc from extragalactic surveys. Kordopatis G., Hill V., Irwin M., Gilmore G., Wyse R.F.G., Tolstoy E., de Laverny P., Recio-Blanco A., Battaglia G., Starkenburg E. <Astron. Astrophys. 555, A12 (2013)> =2013A&A...555A..12K ================================================================================ ADC_Keywords: Milky Way ; Stars, distances ; Effective temperatures ; Abundances, [Fe/H] ; Radial velocities Keywords: Galaxy: evolution - Galaxy: structure - Galaxy: disk - stars: abundances - methods: observational - Galaxy: stellar content Abstract: We study the chemical and kinematic properties of roughly a thousand FLAMES-GIRAFFE LR8 spectra of faint magnitude foreground Galactic stars observed serendipitously during extra-galactic surveys in four lines-of-sight: three in the southern Galactic hemisphere (surveys of the Carina, Fornax and Sculptor dwarf spheroidal galaxies) and one in the northern Galactic hemisphere (a survey of the Sextans dwarf spheroidal galaxy). The foreground stars span distances up to  3kpc from the Galactic plane and Galactocentric radii up to 11kpc. The stellar atmospheric parameters (effective temperature, surface gravity, metallicity) are obtained by an automated parameterisation pipeline and the distances of the stars are then derived by a projection of the atmospheric parameters on a set of theoretical isochrones using a Bayesian approach. The metallicity gradients are estimated for each line-of-sight and compared with predictions from the Besancon model of the Galaxy, in order to test the chemical structure of the thick disc. Finally, we use the radial velocities in each line-of-sight to derive a proxy for either the azimuthal or the vertical component of the orbital velocity of the stars. Only three lines-of-sight have a sufficient number of foreground stars for a robust analysis. Towards Sextans in the Northern Galactic hemisphere and Sculptor in the South, we measure a consistent decrease in mean metallicity with height from the Galactic plane, suggesting a chemically symmetric thick disc. This decrease can either be due to an intrinsic thick disc metallicity gradient, or simply due to a change in the thin disc/thick disc population ratio and no intrinsic metallicity gradients for the thick disc. We favour the latter explanation. In contrast, we find evidence of an unpredicted metal-poor population in the direction of Carina. This population was earlier detected by Wyse et al. (2006ApJ...639L..13W), but our more detailed analysis provides robust estimates of its location (|Z|<1kpc), metallicity (-2<[M/H]<-1dex) and azimuthal orbital velocity (V_phi_ 120km/s). Description: These tables contain all the parameters that have been computed, based on the LR8 spectra of targets selected as being foreground Galactic members. The atmospheric parameters were computed using the pipeline presented in Kordopatis et al. (2011A&A...535A.106K). The line-of-sight distances and the projected atmospheric parameters were computed by projecting the pipeline atmospheric parameters on the Yonsei-Yale isochrones as in Kordopatis et al. (2011A&A...535A.106K). The calibrated metallicities are obtained by applying the corrections established in Kordopatis et al. (2013b, in prep.) for the 4th data release of the RAVE survey. The radial velocities, the photometric values and the positions are taken from Battaglia et al. (2008, Cat. J/MNRAS/383/183) and Koch et al. (2006, Cat. J/AJ/131/895).