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We present a numerical code for continuum radiative transfer that is based onthe idea of a `library' describing the relation between the intensity of thelocal radiation field and the resulting dust emission. With this informationand local intensities at a few reference wavelengths, the radiative transferequation can be integrated through the source and an approximation of theemission spectrum is obtained. Tests with small models for which the radiativetransfer problem can be solved directly show that with our method one caneasily obtain an accuracy of a few per cent. We show spectra computed fromthree-dimensional MHD simulations containing up to 128^3 cells. The modelsrepresent starless, inhomogeneous interstellar clouds embedded in the normalinterstellar radiation field. The intensity ratios between IRAS bands showlarge variations that follow the filamentary density distribution. The powerlaw index of the spatial power spectrum of the column density map is -2.8. Ininfrared maps temperature variations increase the power at high spatialfrequencies, and the index varies between -2.5 and -2.7. Assuming constant dustproperties throughout the cloud, the IRAS ratio <I_60/I_100> decreases indensest cores only by a factor of ~4 compared with the value in diffuse medium.In observations the ratio can decrease twice as much even in optically thinnerclouds. This requires that most of the small grains are removed in theseregions, and possibly a modification of the properties of large grains.Comment: 12 pages, 10 figures. Revised version, accepted to A&

Dust emission from inhomogeneous interstellar clouds: Radiative transfer in 3D with transiently heated particles