  In this paper, we report a detailed study with a variety of data from
optical, near-infrared, X-ray, and radio telescopes of the nuclear region of
the galaxy NGC 613 with the aim of understanding its complexity. We detected an
extended stellar emission in the nucleus that, at first, appears to be, in the
optical band, two stellar nuclei separated by a stream of dust. The active
galactic nucleus (AGN) is identified as a variable point-like source between
these two stellar components. There is a central hard X-ray emission and an
extended soft X-ray emission that closely coincides with the ionization cone,
as seen in the [O III]$\lambda$5007 emission. The centroid of the [O
I]$\lambda$6300 emission does not coincide with the AGN, being shifted by 0.24
arcsec towards the ionization cone; this shift is probably caused by a
combination of differential dust extinction together with emission and
reflection in the ionization cone. The optical spectra extracted from the
central region are typical of low-ionization nuclear emission-line regions. We
also identify 10 H II regions, eight of them in a star forming ring that is
visible in Br$\gamma$, [Fe II]$\lambda$16436 and molecular CO(3-2) images
observed in previous studies. Such a ring also presents weak hard X-ray
emission, probably associated with supernova remnants, not detected in other
studies. The position of the AGN coincides with the centre of a nuclear spiral
(detected in previous works) that brings gas and dust from the bar to the
nucleus, causing the high extinction in this area.
