Outflows in black hole accreting systems are not yet fully understood.  Some of the open
questions are what is the driving mechanism, where is the wind located, what are the
abundances in the wind. These outflows are observed near black holes, from supermassive
ones at the center of galaxies to galactic stellar mass X-ray binaries. Although these
black holes differ by orders of magnitude in scale, there are similarities regarding the
physical process of mass accretion and outflows. In this talk, I will report on
Chandra/HETG grating observations over the past two decades characterizing similarities
and differences between these systems. Starting with a sample of outflows in nine active
galaxies (AGNs) for which we find a universal dependence of outflow column density, NH,
on the ionization parameter, xi. I will demonstrate the importance of the XRISM/Resolve
spectrometer in constraining the column density of the high-xi components better than
HETG, and with much shorter observations. When applying the same analysis to the outflow
of the X-ray binary GRO J1655-40 we find a complex ionization structure of the wind,
different in nature from that of AGNs. We use this structure to measure abundances of
seventeen different elements in the wind, leading to inferences about the historical
supernova explosion. The outflow is characterized by supersolar abundances of odd-Z
elements, which have never before been observed in the X-ray, and originate in a massive
type II supernova with supersolar metallicity.