  We present a study of the mechanical power generated by both winds and jets
across the black hole mass scale. We begin with the study of ionized X-ray
winds and present a uniform analysis using Chandra grating spectra. The high
quality grating spectra facilitate the characterization of the outflow
velocity, ionization and column density of the absorbing gas. We find that the
kinetic power of the winds scales with increasing bolometric luminosity as
log(L_wind) \propto (1.58 \pm 0.07) log(L_Bol). This means that SMBH may be
more efficient than stellar-mass black holes in launching winds. In addition,
the simplicity of the scaling may suggest common driving mechanisms across the
mass scale. For comparison, we next examine jet production, estimating jet
power based on the energy required to inflate local bubbles. The jet relation
is log(L_Jet)\propto (1.18\pm0.24) log(L_Bol). The energetics of the bubble
associated with Cygnus X-1 are particularly difficult to determine, and the
bubble could be a background SNR. If we exclude Cygnus X-1, then the jets
follow a consistent relation to the winds within errors but with a higher
normalization, log(L_Jet) \propto (1.34 \pm 0.50) log(L_Bol). The formal
consistency in the wind and jet scaling relations suggests that a common
launching mechanism may drive both flows; magnetic processes are viable
possibilities. We also examine winds with especially high velocities, v >
0.01c. These ultra-fast outflows tend to resemble the jets more than the winds,
indicating we may be observing a regime in which winds become jets. This study
allows for the total power from black hole accretion, both mechanical and
radiative, to be characterized in a simple manner and suggests a possible
connection between winds and jets. Finally, we find at low Eddington fractions,
the jet power is dominant, and at high Eddington fractions the wind power is
dominant.
