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(abridged) Within the Orion A molecular cloud, the integral-shaped filament(ISF) is a prominent, degree-long structure of dense gas and dust, with clearsigns of recent and on-going high-mass star formation. We used the ArTeMiSbolometer camera at APEX to map a 0.6x0.2 deg^2 region covering OMC-1, OMC-2,OMC-3 at 350 and 450 micron. We combined these data with Herschel-SPIRE maps torecover extended emission. The combined Herschel-ArTeMiS maps provide detailson the distribution of dense, cold material, with a high spatial dynamic range,from our 8'' resolution (0.016 pc) up to the size of the map ~10-15 deg. Bycombining Herschel and ArTeMiS data at 160, 250, 350 and 450 micron, weconstructed high-resolution temperature and H2 column density maps. Weextracted radial profiles from the column density map in several,representative portions of the ISF, that we fitted with Gaussian and Plummermodels to derive their intrinsic widths. We also compared the distribution ofmaterial traced by ArTeMiS with that seen in the higher density tracerN2H+(1-0) recently observed with the ALMA interferometer. All the radialprofiles that we extracted show clear deviation from a Gaussian, with evidencefor an inner plateau, previously not seen using Herschel-only data. We measureintrinsic half-power widths in the range 0.06 to 0.11 pc. This is significantlylarger than the Gaussian widths measured for fibers seen in N2H+, whichprobably traces only the dense innermost regions of the large-scale filament.These half-power widths are within a factor of two of the value of 0.1 pc foundfor a large sample of nearby filaments in various low-mass star-formingregions, which tends to indicate that the physical conditions governing thefragmentation of prestellar cores within transcritical or supercriticalfilaments are the same over a large range of masses per unit length.

Probing the structure of a massive filament: ArTeMiS 350 and 450 micron mapping of the integral-shaped filament in Orion A