To investigate AGN outflows as a tracer of AGN feedback on star-formation , we perform integral-field spectroscopy of 20 type 2 AGNs at z < 0.1 , which are luminous AGNs with the [ O iii ] luminosity > 10 ^ { 41.5 } erg s ^ { -1 } , and exhibit strong outflow signatures in the [ O iii ] kinematics .
By decomposing the emission-line profile , we obtain the maps of the narrow and broad components of [ O iii ] and H \alpha lines , respectively .
The broad components in both [ O iii ] and H \alpha represent the non-gravitational kinematics , i.e. , gas outflows , while the narrow components , especially in H \alpha , represent the gravitational kinematics , i.e. , rotational disk .
By using the integrated spectra within the flux-weighted size of the narrow-line region , we estimate the energetics of the gas outflows .
The ionized gas mass is 1.0–38.5 \times 10 ^ { 5 } M _ { \odot } , and the mean mass outflow rate is 4.6 \pm 4.3 M _ { \odot } yr ^ { -1 } , which is a factor of \sim 260 higher than the mean mass accretion rate 0.02 \pm 0.01 M _ { \odot } yr ^ { -1 } .
The mean energy injection rate of the sample is 0.8 \pm 0.6 % of the AGN bolometric luminosity , while the momentum flux is ( 5.4 \pm 3.6 ) \times L _ { \text { bol } } / c on average , except for two most kinematically energetic AGNs with low L _ { \text { bol } } , which are possibly due to the dynamical timescale of the outflows .
The estimated outflow energetics are consistent with the theoretical expectations for energy-conserving outflows from AGNs , yet we find no supporting evidence of instantaneous quenching of star formation due to the outflows .