  Recent studies on dwarf galaxies reveal that some of them harbor a massive
black hole (BH), which is believed to have a similar mass of the Supermassive
BH "seeds" at early times. The origin and growth of the primitive BHs are still
open questions, since these BH seeds are hardly observed at high redshifts.
Therefore, massive BH of dwarf galaxies can be the perfect candidates to
untangle BH "seeds" properties and their influence on their host galaxy
evolution, since massive BH may preserve their initial conditions due to its
quiet merger and accretion histories. We use optical integral field unit
observations, obtained with the Gemini GMOS-IFU, to study the gas emission and
kinematics in four dwarf galaxies, candidates to host massive BH, based on the
analysis of their [Fe X] luminosities measured from SDSS spectra. The [Fe X]
emission line is not detected in our GMOS in any of the galaxies, prompting
speculation that its absence in our recent data may stem from a past tidal
disruption event coinciding with the observation period of the SDSS data. All
galaxies exhibit extended gas emissions, and the spatially resolved
emission-line ratio diagnostic diagrams present values that suggest AGN
photoionization from the [S II] - BPT diagram. The gas velocity fields of all
galaxies are indicative of disturbed rotation patterns, with no detection of
gas outflows in any of the sources. Although the [S II] - BPT diagrams indicate
AGN photoionization, further confirmation through multi-wavelength observations
is required to validate this scenario.
