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We have used the capabilities of ALMA to probe the ionized gas towards theGalactic center with the H30alpha mm hydrogen recombination line within 30'' ofthe Galaxy's dynamical center. The observations are made with spatial andspectral resolutions of 0.46'' X 0.35'' and 3 km/s, respectively. Multiplecompact and extended sources are detected in the mini-cavity region withextreme negative radial velocities ranging from -480 to -300 km/s, 2-3''(0.08-0.12 pc) from Sgr A*. This is the highest radial velocity of ionized gasdetected beyond the inner 1'' of Sgr A*. This new component is kinematicallyisolated from the orbiting ionized gas. The detected gas has a velocitygradient ranging from -50 to -200 km/s per arcsecond located to the southwestof Sgr A* at a position angle of roughly -160 degrees. Previous proper motionmeasurements in the immediate vicinity of these extreme high-velocity ionizedcomponents have been measured and show transverse velocities that range from313 - 865 km/s. If we assume that they are associated with each other, then thetotal velocity implies these components are gravitationally unbound. Inaddition, we report the kinematics of cometary radio and infrared sources.These sources are diagonally distributed with a position angle of roughly 50degrees within 14'' of Sgr A*. We interpret the highly blue-shifted features tothe SW where the mini-cavity is located and red-shifted cometary sources to theNE in terms of the interaction of a collimated outflow with an opening angle ofroughly 30 degrees. An expected mass outflow rate of 2E-7 or 4E-5 solar massper yr is estimated by a relativistic jet-driven outflow or collimated stellarwinds, respectively.

ALMA Detection of Extreme Blue-Shifted Ionized Gas Within 0.2 pc of Sgr A* from -480 to -300 km/s