Left: distribution of number of emission-line objects as a function of S/N of the lead line for each of the three confidence levels we employ for classification. Objects at the S/N limit are dominated by confidence 1 objects and may include some spurious lines, while for objects with S/N above 10, we expect hardly any misclassifications. Right: redshift histogram of the emission line sources classified by their strongest line. The redshift desert, where there are no strong emission lines in the MUSE wavelength range between 1.5 <  z <  2.9, is clearly visible. We are able to find 479 LAEs, reaching densities of almost 12 LAEs/arcmin².