Johnson C.I.Rich R.M.Simion I.T.Young M.D.Clarkson W.I.Pilachowski C.A.Michael S.Marchetti T.Mario Soto VicencioKunder A.Koch-Hansen A.J.Katherina Vivas A.Joyce M.Shen J.Osmond A.2025-03-142025-03-142022https://hdl.handle.net/20.500.12740/17132We present photometric metallicity measurements for a sample of 2.6 million bulge red clump stars extracted from the Blanco DECam Bulge Survey (BDBS). Similar to previous studies, we find that the bulge exhibits a strong vertical metallicity gradient, and that at least two peaks in the metallicity distribution functions appear at b < -5°. We can discern a metal-poor ([Fe/H] ∼-0.3) and metal-rich ([Fe/H] ∼+0.2) abundance distribution that each show clear systematic trends with latitude, and may be best understood by changes in the bulge's star formation/enrichment processes. Both groups exhibit asymmetric tails, and as a result we argue that the proximity of a star to either peak in [Fe/H] space is not necessarily an affirmation of group membership. The metal-poor peak shifts to lower [Fe/H] values at larger distances from the plane while the metal-rich tail truncates. Close to the plane, the metal-rich tail appears broader along the minor axis than in off-axis fields. We also posit that the bulge has two metal-poor populations - one that belongs to the metal-poor tail of the low latitude and predominantly metal-rich group, and another belonging to the metal-poor group that dominates in the outer bulge. We detect the X-shape structure in fields withPDFGalaxy: bulgeArtículohttp://dx.doi.org/10.1093/mnras/stac1840