We present two wide-field ( \approx 5 \arcmin \times 3.5 \arcmin ) , diffraction limited ( \lambda / D \simeq 0.5 \arcsec at 10 µm ) , broad-band 10 µm and 20 \mu m images of the Orion Nebula , plus six 7–13 µm narrow-band ( \lambda / \Delta \lambda \simeq 1 ) images of the BN/KL complex taken at the 3.8m UKIRT The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the U.K . Particle Physics and Astronomy Research Council . telescope with the MPIA MAX camera . The wide field images , centered on the Trapezium and BN/KL regions , are mosaics of 35 \arcsec \times 35 \arcsec frames obtained with standard chopping and nodding technique and reconstructed using a new restoration method developed for this project . They show the filamentary structure of the dust emission from the walls of the HII region and reveal a new remarkable group of arc-like structures \approx 1 \arcmin to the South of the Trapezium . The morphology of the Ney-Allen nebula , produced by wind-wind interaction in the vicinity of the Trapezium stars , suggests a complex kinematical structure at the center of the Cluster . We find indications that one of the most massive members of the cluster , the B0.5V star \theta ^ { 1 } Ori-D , is surrounded by a photoevaporated circumstellar disk . Among the four historic Trapezium OB stars , this is the only one without a binary companion , suggesting that stellar multiplicity and the presence of massive circumstellar disks may be mutually exclusive . In what concerns the BN/KL complex , we find evidence for extended optically thin silicate emission on top of the deep 10 µm absorption feature . Assuming a simple two component model , we map with \simeq 0 \farcs 5 spatial resolution the foreground optical depth , color temperature and mid-IR luminosity of the embedded sources . We resolve a conspicuous point source at the location of the IRc2-A knot , approximately 0 \farcs 5 north of the deeply embedded HII region “ I ” . We analyze the spectral profile of the 10 µm silicate absorption feature and find indication for grain crystallization in the harsh nebular environment . In the OMC-1 South region , we detect several point sources and discuss their association with the mass loss phenomenology observed at optical and millimeter wavelengths . Finally , we list the position and photometry of 177 point sources , the large majority of which detected for the first time in the mid-IR . Twenty two of them lack a counterpart at shorter wavelengths , and are , therefore , candidates for deeply embedded protostars . The comparison of photometric data obtained at two different epochs reveals that source variability at 10 \mu m is present up to \approx 1  mag level on a time-scale \sim 2  yr. With the possible exception of a pair of OB stars , all point sources detected at shorter wavelengths display 10 \mu m emission well above the photospheric level , that we attribute to disks circumstellar emission . The model of Robberto , Beckwith , & Panagia ( 2002 , ApJ . 578 , 897 ) provides the simplest explanation for the observed mid-IR excess .