We present Gemini Multiobject Spectrograph integral field spectroscopy of the extended emission-line region associated with quasar 3C 249.1 .
The kinematics of the ionized gas measured from the [ O iii ] \lambda 5007 line is rather complex and can not be explained globally by a simple dynamical model , but some clouds can be modeled individually as having locally linear velocity gradients .
The temperatures of the ionized gas appear uniform ( varying from \sim 12000 to 15000 K ) , while the densities vary from a few tens to a few hundreds cm ^ { -3 } .
The emission mechanism of all of the emission clouds , as indicated by the line-ratio diagnostics , is consistent both with “ shock + precursor ” and pure photoionization models .
The total mass of the ionized gas is on the order of 10 ^ { 9 } M _ { \odot } .
We estimate the bulk kinetic energy and momentum of the extended emission-line region of 2.5 \times 10 ^ { 57 } ergs and 10 ^ { 50 } dyne s , and a dynamical timescale of \sim 10 Myr .
By comparing the injection rates of kinetic energy and momentum of different galactic wind models with the observation , we argue that the emission-line clouds are most likely a direct result from the feedback of the quasar .
We also discuss the nature of the extended X-ray emission surrounding the quasar .