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We construct dynamical models of the Milky Way's Box/Peanut (B/P) bulge,using the recently measured 3D density of Red Clump Giants (RCGs) as well askinematic data from the BRAVA survey. We match these data using the NMAGICMade-to-Measure method, starting with N-body models for barred discs indifferent dark matter haloes. We determine the total mass in the bulge volumeof the RCGs measurement (+-2.2 x +- 1.4 x +- 1.2 kpc) with unprecedentedaccuracy and robustness to be 1.84 +- 0.07 x10^10 Msun. The stellar mass inthis volume varies between 1.25-1.6 x10^10 Msun, depending on the amount ofdark matter in the bulge. We evaluate the mass-to-light and mass-to-clumpratios in the bulge and compare them to theoretical predictions from populationsynthesis models. We find a mass-to-light ratio in the K-band in the range0.8-1.1. The models are consistent with a Kroupa or Chabrier IMF, but aSalpeter IMF is ruled out for stellar ages of 10 Gyr. To match predictions fromthe Zoccali IMF derived from the bulge stellar luminosity function requiresabout 40% or 0.7 x10^10 Msun dark matter in the bulge region. The BRAVA datatogether with the RCGs 3D density imply a low pattern speed for the GalacticB/P bulge of 25-30 km.s-1.kpc-1. This would place the Galaxy among the slowrotators (R >= 1.5). Finally, we show that the Milky Way's B/P bulge has anoff-centred X structure, and that the stellar mass involved in the peanut shapeaccounts for at least 20% of the stellar mass of the bulge, significantlylarger than previously thought.

Made-to-Measure models of the Galactic Box/Peanut bulge: stellar and total mass in the bulge region