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Context. The star formation rates and stellar densities found in youngmassive clusters suggest that these stellar systems originate from gas atdensities n(H$_2$) $>10^7$ cm$^{-3}$. Until today, however, the physicalcharacterization of this ultra high density material remains largelyunconstrained in observations. Aims. We investigated the density properties ofthe star-forming gas in the OMC-1 region located in the vicinity of the OrionNebula Cluster (ONC). Methods. We mapped the molecular emission at 652 GHz inOMC-1 as part of the APEX-SEPIA660 Early Science. Results. We detect bright andextended N$_2$H$^+$ (J=7-6) line emission along the entire OMC-1 region.Comparisons with previous ALMA data of the (J=1-0) transition and radiativetransfer models indicate that the line intensities observed in this N$_2$H$^+$(7-6) line are produced by large mass reservoirs of gas at densities n(H$_2$)$>10^7$ cm$^{-3}$. Conclusions. The first detection of this N$_2$H$^+$ (7-6)line at parsec-scales demonstrates the extreme density conditions of thestar-forming gas in young massive clusters such as the ONC. Our resultshighlight the unique combination of sensitivity and mapping capabilities of thenew SEPIA660 receiver for the study of the ISM properties at high frequencies.

APEX-SEPIA660 Early Science: Gas at densities above $10^7$ cm$^{-3}$ towards OMC-1