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Galactic Archeology with 4MOST

Published online by Cambridge University Press:  02 August 2018

S. Feltzing ,
T. Bensby ,
M. Bergemann ,
C. Chiappini ,
N. Christlieb ,
M.-R. Cioni ,
A. Helmi ,
M. Irwin ,
I. Minchev  and
E. Starkenburg
...Show all authors
S. Feltzing
Affiliation:
Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, SE-221 00, Lund, Sweden, email: sofia@astro.lu.se
T. Bensby
Affiliation:
Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, SE-221 00, Lund, Sweden, email: sofia@astro.lu.se
M. Bergemann
Affiliation:
Max-Planck-Institut für Astronomie, Heidelberg, Germany
C. Chiappini
Affiliation:
Leibniz-Institute for Astrophysics Potsdam, Potsdam, Germany
N. Christlieb
Affiliation:
ZAH, Landessternwarte, Heidelberg, Germany
M.-R. Cioni
Affiliation:
Leibniz-Institute for Astrophysics Potsdam, Potsdam, Germany
A. Helmi
Affiliation:
Kapteyn Astronomical Institute, Groningen, The Netherlands
M. Irwin
Affiliation:
Institute of Astronomy, Cambridge, UK
I. Minchev
Affiliation:
Leibniz-Institute for Astrophysics Potsdam, Potsdam, Germany
E. Starkenburg
Affiliation:
Leibniz-Institute for Astrophysics Potsdam, Potsdam, Germany
R. de Jong
Affiliation:
Leibniz-Institute for Astrophysics Potsdam, Potsdam, Germany
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Abstract

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4MOST is a new wide-field, high-multiplex spectroscopic survey facility for the VISTA telescope of ESO. Starting in 2022, 4MOST will deploy 2400 fibres in a 4.1 square degree field-of-view using a positioner based on the tilting spine principle. In this contribution we give an outline of the major science goals we wish to achieve with 4MOST in the area of Galactic Archeology. The 4MOST Galactic Archeology surveys have been designed to address long-standing and far-reaching problems in Galactic science. They are focused on four major themes: 1) Near-field cosmology tests, 2) Chemo-dynamical characterisation of the major Milky Way stellar components, 3) The Galactic Halo and beyond, and 4) Discovery and characterisation of extremely metal-poor stars. In addition to a top-level description of the Galactic surveys we provide information about how the community will be able to join 4MOST via a call for Public Spectroscopic Surveys that ESO will launch.

Keywords

Galaxy: haloGalaxy: diskGalaxy: bulgeGalaxy: evolutionGalaxy: structureGalaxy: abundancesMagellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 225 - 232
Copyright
Copyright © International Astronomical Union 2018 

References

Belokurov, V., et al. 2017, MNRAS, 466, 4711Google Scholar
Bergemann, M., et al. 2012, MNRAS, 427, 27Google Scholar
Bland-Hawthorn, J. & Gerhard, O., 2016, ARA&A, 54, 529Google Scholar
Caffau, E., et al. 2013, AN, 334, 197Google Scholar
Cioni, M-R., et al. 2011, A&A, 527, A116Google Scholar
Dalton, G. et al. 2016, Final design and progress of WEAVE: the next generation wide-field spectroscopy facility for the William Herschel Telescope, Proc. SPIE Vol. 9908, 99081GGoogle Scholar
de Jong, R. S. et al. 2016a, SPIE, 4MOST: the 4-metre Multi-Object Spectroscopic Telescope project at preliminary design review Proc. SPIE Vol. 9908, 99081OGoogle Scholar
de Jong, R. S., et al. 2016b, AN, 337, 964Google Scholar
Deason, C., et al. 2017, MNRAS, 467, 2636Google Scholar
DESI collaboration, 2016, arXiv:1611.00036Google Scholar
Freeman, K. & Bland-Hawthorn, J., 2002, ARA&A, 40, 487Google Scholar
Gilmore, G., et al. 2012, Msngr, 147, 25Google Scholar
Hansen, C., et al. 2015, AN, 336, 665Google Scholar
Heiter, C., et al. 2015, A&A, 582, A49Google Scholar
Laurent, F. et al. 2016, 4MOST low-resolution spectrograph: design and performances Proc. SPIE Vol. 9908, 99087VGoogle Scholar
Lind, K., et al. 2012, MNRAS, 427, 50Google Scholar
Martell, G., et al. 2017, MNRAS, 465, 3203Google Scholar
Miglio, A. et al. 2017, arXiv:1706.03778Google Scholar
Ness, M., et al. 2015, ApJ, 808, 16Google Scholar
Pancino, E., et al. 2017, A&A, 598, A5Google Scholar
Ripepi, V. et al. 2017, arXiv:1707.04500Google Scholar
Ructhi, G., et al. 2016, MNRAS, 461, 2174Google Scholar
Seifert, W. et al. 2016, 4MOST: the high-resolution spectrograph Proc. SPIE Vol. 9908, 990890Google Scholar
Turon, C. et al. 2008, ESA-ESO Working Group on Galactic Populations, Chemistry and Dynamics http://www.stecf.org/coordination/eso-esa/galpops.phpGoogle Scholar
Valentini, M., et al. 2017, A&A, 600, A66Google Scholar
Walcher, J. C. et al. 2016, 4MOST: science operations for a large spectroscopic survey program with multiple science cases executed in parallel Proc. SPIE Vol. 9910, 99101NGoogle Scholar