The center image is the dust temperature distribution of the inner CMZ derived from Herschel HI-GAL 70–350 μm images (Molinari et al. 2011). It has a doughnut shaped distribution as seen in projection marking a warm dust bubble (Molinari et al. 2011, 2014). On the left is the radio continuum map generated by Simpson et al. (2007) based on the data of Yusef-Zadeh & Morris (1987) of the central portion of the bubble (the hole in the doughnut) containing the Radio Arc and arched filaments. The [C ii] integrated intensity, I([C ii]) (K km s^-1), strip scans as a function of longitude and latitude are plotted to the bottom and the right, respectively, and are aligned with the temperature map of the inner CMZ. These plots show the velocity-integrated [C ii] intensity profiles as functions of longitude or latitude: the black lines represent the total intensity in the velocity range V_LSR = −200 to +140 km s^-1, the red and blue lines represent I([C ii]) integrated emission in the high-velocity red and blue wings from V_LSR = + 80 to +130 km s^-1 and −80 to −130 km s^-1, respectively.