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Aims. We study the forward shock in the oxygen-rich young supernova remnant(SNR) 1E0102.2-7219 (1E0102 in short) via optical coronal emission from [FeXIV] and [Fe XI]: emission lines which offer an alternative method to X-rays todo so.  Methods. We have used the Multi-Unit Spectroscopic Explorer (MUSE) opticalintegral field spectrograph at the Very Large Telescope (VLT) on Cerro Paranalto obtain deep observations of SNR 1E0102 in the Small Magellanic Cloud. Ourobservations cover the entire extent of the remnant with a seeing limitedspatial resolution of 0.7" = 0.2 pc at the distance of 1E 0102.  Results. Our MUSE observations unambiguously reveal the presence of [Fe XIV]and [Fe XI] emission in 1E0102. The emission largely arises from a thin,partial ring of filaments surrounding the fast moving O-rich ejecta in thesystem. The brightest [Fe XIV] and [Fe XI] emission is found along the easternand north-western sides of 1E0102, where shocks are driven into denser ISMmaterial, while fainter emission along the northern edge reveals the locationof the forward shock in lower density gas, possibly the relic stellar windcavity. Modeling of the eastern shocks and the photoionization precursorsurrounding 1E0102, we derive a pre-shock density $n_H$ = (7.4 +-1.5)cm$^{-3}$, and a shock velocity 330 km/s < $v_s$ < 350 km/s.

[Fe XIV] and [Fe XI] reveal the forward shock in SNR 1E0102.2-7219