J/A+A/604/A128      S abundances for 1301 stars from GES       (Duffau+, 2017)
The Gaia-ESO Survey: Galactic evolution of sulphur and zinc.
    Duffau S., Caffau E., Sbordone L., Bonifacio P., Andrievsky S.,
    Korotin S., Babusiaux C., Salvadori S., Monaco L., Francois P.,
    Skuladottir A., Bragaglia A., Donati P., Spina L., Gallagher A.J.,
    Ludwig H.-G., Christlieb N., Hansen C.J., Mott A., Steffen M., Zaggia S.,
    Blanco-Cuaresma S., Calura F., Friel E., Jimenez-Esteban F.M., Koch A.,
    Magrini L., Pancino E., Tang B., Tautvaisiene G., Vallenari A.,
    Hawkins K., Gilmore G., Randich S., Feltzing S., Bensby T., Flaccomio E.,
    Smiljanic R., Bayo A., Carraro G., Casey A. R., Costado M. T., Damiani F.,
    Franciosini E., Hourihane A., Jofre P., Lardo C., Lewis J., Morbidelli L.,
    Sousa S.G., Worley C.C.
    <Astron. Astrophys. 604, A128 (2017)>
    =2017A&A...604A.128D        (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Stars, dwarfs ; Stars, giant ; Abundances ;
              Spectroscopy
Keywords: Galaxy: abundances - Galaxy: evolution - Galaxy: disk -
          stars: abundances - open clusters and associations: general -
          globular clusters: general

Abstract:
    Due to their volatile nature, when sulphur and zinc are observed in
    external galaxies, their determined abundances represent the gas-phase
    abundances in the interstellar medium. This implies that they can be
    used as tracers of the chemical enrichment of matter in the Universe
    at high redshift. Comparable observations in stars are more difficult
    and, until recently, plagued by small number statistics. We wish to
    exploit the Gaia ESO Survey (GES) data to study the behaviour of
    sulphur and zinc abundances of a large number of Galactic stars, in a
    homogeneous way. By using the UVES spectra of the GES sample, we are
    able to assemble a sample of 1301 Galactic stars, including stars in
    open and globular clusters in which both sulphur and zinc were
    measured. We confirm the results from the literature that sulphur
    behaves as an alpha-element. We find a large scatter in [Zn/Fe] ratios
    among giant stars around solar metallicity. The lower ratios are
    observed in giant stars at Galactocentric distances less than 7.5kpc.
    No such effect is observed among dwarf stars, since they do not extend
    to that radius. Given the sample selection, giants and dwarfs are
    observed at different Galactic locations, and it is plausible, and
    compatible with simple calculations, that Zn-poor giants trace a
    younger population more polluted by SN Ia yields. It is necessary to
    extend observations in order to observe both giants and dwarfs at the
    same Galactic location. Further theoretical work on the evolution of
    zinc is also necessary.

Description:
    GES internal star identifier (CNAME), Sulphur abundances and NLTE
    corrections to the Sulphur abundances for 1301 stars. Sulphur
    abundances are expressed in the customary logarithmic form:
    A(S)=log_10(N(S)/N(H))+12.
    The abundances delivered are the LTE ones. NLTEabundances can be
    determined by directly summing the NLTE correction delivered:
    A(S)_NLTE = A(S) + NLTE_C.
    So that a negative NLTE correction indicates that the NLTE abundance
    is lower than the LTE one.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
ges_s_du.dat      37     1301   Sulphur abundances


See also:
   J/A+A/572/A33    : Abundances from Gaia-ESO Survey (Mikolaitis+, 2014)
   J/A+A/589/A115   : Na and Al abundances of 1303 stars (Smiljanic+, 2016)
   J/A+A/603/A2     : GES abundances radial distribution (Magrini+, 2017)
   J/MNRAS/441/3127 : FeI oscillator strengths for Gaia-ESO (Ruffoni+, 2014)


Byte-by-byte Description of file: ges_s_du.dat

   Bytes Format Units   Label     Explanations

   1- 16  A16   ---     Cname     GES star unique identifier (HHMMSSss+DDMMSSs)
  19- 25  F7.4  ---     A(S)      Sulphur abundance (LTE)
  28- 37  E10.3 ---     NLTEc     NLTE corrections


Acknowledgements:
    Sonia Duffau, sonia.duffau(at)gmail.com
(End) Sonia Duffau [Universidad Andres Bello] Patricia Vannier [CDS] 03-Jul-2017