We present near-infrared emission-line flux distributions , excitation and kinematics , as well as stellar kinematics , of the inner 520 \times 520 ~ { } { pc ^ { 2 } } of the Seyfert 2 galaxy NGC 5929 . The observations were performed with the Gemini ’ s Near-Infrared Integral Field Spectrograph ( NIFS ) at a spatial resolution of \sim 20 ~ { } pc and spectral resolution of 40 ~ { } km s ^ { -1 } in the J- and K _ { l } -bands . The flux distributions of H _ { 2 } , [ Fe ii ] , [ P ii ] , and H recombination lines are extended over most of the field of view , with the highest intensity levels observed along PA = 60 / 240 ^ { \circ } , and well correlated with the radio emission . The H _ { 2 } and [ Fe ii ] line emission are originated in thermal processes , mainly due to heating of the gas by X-rays from the central Active Galactic Nucleus ( AGN ) . Contribution of shocks due to the radio jet is observed at locations co-spatial with the radio hotspots at 0 \aas@@fstack { \prime \prime } 50 northeast and 0 \aas@@fstack { \prime \prime } 60 southwest of the nucleus , as evidenced by the emission-line ratio and gas kinematics . The stellar kinematics shows rotation with an amplitude at 250pc from the nucleus of \sim 200 km s ^ { -1 } after corrected for the inferred inclination of 18.3 ^ { \circ } . The stellar velocity dispersion obtained from the integrated K-band spectrum is \sigma _ { * } = 133 \pm 8 km s ^ { -1 } , which implying on a mass for the supermassive black hole of M _ { \bullet } = 5.2 ^ { 1.6 } _ { -1.2 } \times 10 ^ { 7 } ~ { } { M _ { \odot } } , using the M _ { \bullet } - \sigma _ { * } relation . The gas kinematics present three components : ( 1 ) gas in the plane of the galaxy in counter-rotation relative to the stars ; ( 2 ) an outflow perpendicular to the radio jet that seems to be due to an equatorial AGN outflow ; ( 3 ) turbulence of the gas observed in association with the radio hot spots , supporting an interaction of the radio jet with the gas of the disk . We estimated the mass of ionized and warm molecular gas of \sim 1.3 \times 10 ^ { 6 } { M _ { \odot } } and \sim 470 ~ { } { M _ { \odot } } , respectively .