Chandra spectroscopy of transient stellar-mass black holes in outburst has clearly revealed accretion disk winds in soft , disk–dominated states , in apparent anti-correlation with relativistic jets in low/hard states .
These disk winds are observed to be highly ionized , dense , and to have typical velocities of \sim 1000 km/s or less projected along our line of sight .
Here , we present an analysis of two Chandra High Energy Transmission Grating spectra of the Galactic black hole candidate IGR J17091 - 3624 and contemporaneous EVLA radio observations , obtained in 2011 .
The second Chandra observation reveals an absorption line at 6.91 \pm 0.01 keV ; associating this line with He-like Fe XXV requires a blue-shift of 9300 ^ { +500 } _ { -400 } km/s ( 0.03 c , or the escape velocity at 1000 R _ { Schw } ) .
This projected outflow velocity is an order of magnitude higher than has previously been observed in stellar-mass black holes , and is broadly consistent with some of the fastest winds detected in 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 putative feature is marginal .
Photoionization modeling suggests that the accretion disk wind in IGR J17091 - 3624 may originate within 43,300 Schwarzschild radii of the black hole , and may be expelling more gas than accretes .
The contemporaneous EVLA observations strongly indicate that jet activity was indeed quenched at the time of our Chandra observations .
We discuss the results in the context of disk winds , jets , and basic accretion disk physics in accreting black hole systems .