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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 742434.0, MPI für Astronomie / Publikationen_mpia
The Pristine survey - I. Mining the Galaxy for the most metal-poor stars
Authors:Starkenburg, E.; Martin, N.; Youakim, K.; Aguado, D. S.; Allende Prieto, C.; Arentsen, A.; Bernard, E. J.; Bonifacio, P.; Caffau, E.; Carlberg, R. G.; Côté, P.; Fouesneau, M.; François, P.; Franke, O.; González Hernández, J. I.; Gwyn, S. D. J.; Hill, V.; Ibata, R. A.; Jablonka, P.; Longeard, N.; McConnachie, A. W.; Navarro, J. F.; Sánchez-Janssen, R.; Tolstoy, E.; Venn, K. A.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:Monthly Notices of the Royal Astronomical Society
Volume:471
Issue / Number:3
Start Page:2587
End Page:2604
Audience:Not Specified
Abstract / Description:We present the Pristine survey, a new narrow-band photometric survey focused on the metallicity-sensitive Ca H&K lines and conducted in the Northern hemisphere with the wide-field imager MegaCam on the Canada-France-Hawaii Telescope. This paper reviews our overall survey strategy and discusses the data processing and metallicity calibration. Additionally we review the application of these data to the main aims of the survey, which are to gather a large sample of the most metal-poor stars in the Galaxy, to further characterize the faintest Milky Way satellites, and to map the (metal-poor) substructure in the Galactic halo. The current Pristine footprint comprises over 1000 deg2 in the Galactic halo ranging from b ˜ 30° to ˜78° and covers many known stellar substructures. We demonstrate that, for Sloan Digital Sky Survey (SDSS) stellar objects, we can calibrate the photometry at the 0.02-mag level. The comparison with existing spectroscopic metallicities from SDSS/Sloan Extension for Galactic Understanding and Exploration (SEGUE) and Large Sky Area Multi-Object Fiber Spectroscopic Telescope shows that, when combined with SDSS broad-band g and I photometry, we can use the CaHK photometry to infer photometric metallicities with an accuracy of ˜0.2 dex from [Fe/H] = -0.5 down to the extremely metal-poor regime ([Fe/H] < -3.0). After the removal of various contaminants, we can efficiently select metal-poor stars and build a very complete sample with high purity. The success rate of uncovering [Fe/H]SEGUE < -3.0 stars among [Fe/H]Pristine < -3.0 selected stars is 24 per cent, and 85 per cent of the remaining candidates are still very metal poor ([Fe/H]<-2.0). We further demonstrate that Pristine is well suited to identify the very rare and pristine Galactic stars with [Fe/H] < -4.0, which can teach us valuable lessons about the early Universe.
Free Keywords:stars: abundances; Galaxy: abundances; Galaxy: evolution; Galaxy: formation; Galaxy: halo; galaxies: dwarf
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711
URL:http://adsabs.harvard.edu/abs/2017MNRAS.471.2587S
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