) Intermediate mass black holes ( 10 ^ { 3 } –10 ^ { 5 } M _ { \odot } ) in the center of dwarf galaxies are believed to be analogous to growing Active Galactic Nuclei ( AGN ) in the early Universe .
Their characterization can provide insight about the early galaxies .
We present optical and near-infrared integral field spectroscopy of the inner \sim 50 pc of the dwarf galaxy NGC 4395 , known to harbor an AGN .
NGC 4395 is an ideal candidate to investigate the nature of dwarf AGN , as it is nearby ( d \approx 4.4 Mpc ) enough to allow a close look at its nucleus .
The optical data were obtained with the Gemini GMOS-IFU covering the 4500 Å to 7300 Å spectral range at a spatial resolution of 10 pc .
The J and K-band spectra were obtained with the Gemini NIFS at spatial resolutions of \sim 5 pc .
The gas kinematics show a compact , rotation disk component with a projected velocity amplitude of 25 km s ^ { -1 } .
We estimate a mass of 7.7 \times 10 ^ { 5 } M _ { \odot } inside a radius of 10 pc .
From the H \alpha broad line component , we estimate the AGN bolometric luminosity as L _ { bol } = ( 9.9 \pm 1.4 ) \times 10 ^ { 40 } erg s ^ { -1 } and a mass M _ { BH } = ( 2.5 ^ { +1.0 } _ { -0.8 } ) \times 10 ^ { 5 } M _ { \odot } for the central black hole .
The mean surface mass densities for the ionized and molecular gas are in the ranges ( 1–2 ) M _ { \odot } pc ^ { -2 } and ( 1–4 ) \times 10 ^ { -3 } M { { } _ { \odot } } pc ^ { -2 } and the average ratio between ionized and hot molecular gas masses is \sim 500 .
The emission-line flux distributions reveal an elongated structure at 24 pc west of the nucleus , which is blueshifted relative to the systemic velocity of the galaxy by \approx 30 km s ^ { -1 } .
We speculate that this structure is originated by the accretion of a gas-rich small satellite or by a low metallicity cosmic cloud .