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{\it Chandra} spectroscopy of transient stellar-mass black holes in outbursthas clearly revealed accretion disk winds in soft, disk--dominated states, inapparent anti-correlation with relativistic jets in low/hard states. These diskwinds are observed to be highly ionized, dense, and to have typical velocitiesof $\sim$1000 km/s or less projected along our line of sight. Here, we presentan analysis of two {\it Chandra} High Energy Transmission Grating spectra ofthe Galactic black hole candidate IGR J17091$-$3624 and contemporaneous EVLAradio observations, obtained in 2011. The second {\it Chandra} observationreveals an absorption line at 6.91$\pm$0.01 keV; associating this line withHe-like Fe XXV requires a blue-shift of $9300^{+500}_{-400}$ km/s (0.03$c$, orthe escape velocity at 1000 R$_{Schw}$). This projected outflow velocity is anorder of magnitude higher than has previously been observed in stellar-massblack holes, and is broadly consistent with some of the fastest winds detectedin active galactic nuclei. A potential feature at 7.32 keV, if due to Fe XXVI,would imply a velocity of $\sim 14600$ km/s (0.05$c$), but this putativefeature is marginal. Photoionization modeling suggests that the accretion diskwind in IGR J17091$-$3624 may originate within 43,300 Schwarzschild radii ofthe black hole, and may be expelling more gas than accretes. Thecontemporaneous EVLA observations strongly indicate that jet activity wasindeed quenched at the time of our {\it Chandra} observations. We discuss theresults in the context of disk winds, jets, and basic accretion disk physics inaccreting black hole systems.

An Extreme X-ray Disk Wind in the Black Hole Candidate IGR J17091-3624