The Pristine survey I: Mining the Galaxy for the most metal-poor stars
  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 (CFHT). 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
characterise the faintest Milky Way satellites, and to map the (metal-poor)
substructure in the Galactic halo. The current Pristine footprint comprises
over 1,000 deg2 in the Galactic halo ranging from b~30 to 78 and covers many
known stellar substructures. We demonstrate that, for SDSS stellar objects, we
can calibrate the photometry at the 0.02-magnitude level. The comparison with
existing spectroscopic metallicities from SDSS/SEGUE and LAMOST 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% and 85%
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.
