We present the first stellar density profile of the Milky Way bulge reaching latitude \(b=0^\circ\). It is derived by counting red clump stars within the colour\--magnitude diagram constructed with the new PSF-fitting photometry from VISTA Variables in the V\'\i a L\'actea (VVV) survey data. The new stellar density map covers the area between \(|l|\leq 10^\circ\) and \(|b|\leq 4.5^\circ\) with unprecedented accuracy, allowing to establish a direct link between the stellar kinematics from the Giraffe Inner Bulge Spectroscopic Survey (GIBS) and the stellar mass density distribution. In particular, the location of the central velocity dispersion peak from GIBS matches a high overdensity in the VVV star count map. By scaling the total luminosity function (LF) obtained from all VVV fields to the LF from Zoccali et al.(2003), we obtain the first fully empirical estimate of the mass in stars and remnants of the Galactic bulge. The Milky Way bulge stellar mass within (\(|b|<9.5^\circ\), \(|l|<10^\circ\)) is \(2.0\pm0.3\times 10^{10}M_{\odot}\).