We present the first stellar density profile of the Milky Way bulge that reaches latitude b = 0°. The profile was derived by counting red clump stars within the colour-magnitude diagram that was constructed using the new PSF-fitting photometry from VISTA Variables in the Vía Láctea (VVV) survey data. The new stellar density map covers the area between | l | ≤ 10° and | b | ≤ 4.5° with unprecedented accuracy, allowing the stellar kinematics from the Giraffe Inner Bulge Spectroscopic Survey (GIBS) to be linked to the stellar mass density distribution. In particular, the location of the central velocity-dispersion peak from GIBS matches a high over-density 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 in remnants of the Galactic bulge. Within (| b | < 9.5°, | l | < 10°), the Milky Way bulge stellar mass is 2.0 ± 0.3 × 1010M⊙.
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机译：我们介绍了到达纬度b = 0°的银河系凸起的第一个恒星密度分布。该轮廓是通过对色度图中的红色块状星进行计数而得出的，该色度图是使用来自VíaLáctea（VVV）调查数据中VISTA Variables的新型PSF拟合光度法构建的。新的恒星密度图覆盖了|之间的区域。 l | ≤10°和| b | ≤4.5°，具有前所未有的精度，使长颈鹿内膨胀光谱调查（GIBS）的恒星运动学与恒星质量密度分布相关联。特别是，来自GIBS的中心速度色散峰的位置与VVV星数图中的高过密度匹配。通过将从所有VVV场获得的总光度函数（LF）缩放到Zoccali等人（2003）的LF，我们获得了第一个完全实证的质量估计，包括恒星和银河膨胀隆起部分的质量。在（| b | <9.5°，| l | <10°）范围内，银河系凸起的恒星质量为2.0±0.3×1010M⊙。
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