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The most metal-deficient stars hold important clues about the early build-upand chemical evolution of the Milky Way, and carbon-enhanced metal-poor (CEMP)stars are of special interest. However, little is known about CEMP stars in theGalactic bulge. In this paper, we use the large spectroscopic sample ofmetal-poor stars from the Pristine Inner Galaxy Survey (PIGS) to identify CEMPstars ([C/Fe] > +0.7) in the bulge region and to derive a CEMP fraction. Weidentify 96 new CEMP stars in the inner Galaxy, of which 62 are very metal-poor([Fe/H] < -2.0); this is more than a ten-fold increase compared to the sevenpreviously known bulge CEMP stars. The cumulative fraction of CEMP stars inPIGS is $42^{\,+14\,}_{\,-13} \%$ for stars with [Fe/H] < -3.0, and decreasesto $16^{\,+3\,}_{\,-3} \%$ for [Fe/H] < -2.5 and $5.7^{\,+0.6\,}_{\,-0.5} \%$for [Fe/H] < -2.0. The PIGS inner Galaxy CEMP fraction for [Fe/H] < -3.0 isconsistent with the halo fraction found in the literature, but at highermetallicities the PIGS fraction is substantially lower. While this can partlybe attributed to a photometric selection bias, such bias is unlikely to fullyexplain the low CEMP fraction at higher metallicities. Considering the typicalcarbon excesses and metallicity ranges for halo CEMP-s and CEMP-no stars, ourresults point to a possible deficiency of both CEMP-s and CEMP-no stars(especially the more metal-rich) in the inner Galaxy. The former is potentiallyrelated to a difference in the binary fraction, whereas the latter may be theresult of a fast chemical enrichment in the early building blocks of the innerGalaxy.

The Pristine Inner Galaxy Survey (PIGS) III: carbon-enhanced metal-poor stars in the bulge