  We study the properties of one of the most luminous hinge clumps, located on
the compact group of galaxies NGC6845. Using IFS from GMOS/Gemini, complemented
with archival MUSE data, we obtain oxygen abundances, ages, star formation
rates, velocity fields and we also performed a single stellar populations
modeling to understand the SFH of the hinge clump localized in NGC6845. We
found that the hinge clump sits in a tail, having a SFR of
3.4$M_{\odot}yr^{-1}$, which is comparable with a few other extreme cases,
e.g., the star clusters in the Antennae galaxy and other reported hinge clumps
in the literature. In fact, this clump represents ~15\% of total SFR of
NGC6845A. Large-scale modeling of the observed velocity field of NGC6845A rules
out the scenario on which this hinge clump was a satellite galaxy. Indeed, its
kinematics is compatible with the galactic disk of NGC6845A. Its abundance,
mean value of 0.4Z$_{\odot}$, is also consistent with the metallicity gradient
of the galaxy. Our analysis, suggest that the hinge clump is formed by multiple
stellar populations instead of a single burst, thus having a large range of
ages. We found that central clump is encompassed by a ring-like structure,
suggesting that the ring-like structure represents a second-generation of star
formation. In addition, the analysis of the diagnostic diagram indicates that
this central region can also be being ionized by shock from stellar and
supernovae winds. Finally, the derived SFR density
$\Sigma=9.7M_{\odot}yr^{-1}kpc^{-2}$ of the central clump, place it in
starburst regime, where gas inflows should provide gas to maintain the star
formation. This work shows a resolved example of an extreme localized starburst
in a compact group of galaxies.
