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

We present a numerical code for continuum radiative transfer that is based on the idea of a `library' describing the relation between the intensity of the local radiation field and the resulting dust emission. With this information and local intensities at a few reference wavelengths, the radiative transfer equation can be integrated through the source and an approximation of the emission spectrum is obtained. Tests with small models for which the radiative transfer problem can be solved directly show that with our method one can easily obtain an accuracy of a few per cent. We show spectra computed from three-dimensional MHD simulations containing up to 128^3 cells. The models represent starless, inhomogeneous interstellar clouds embedded in the normal interstellar radiation field. The intensity ratios between IRAS bands show large variations that follow the filamentary density distribution. The power law index of the spatial power spectrum of the column density map is -2.8. In infrared maps temperature variations increase the power at high spatial frequencies, and the index varies between -2.5 and -2.7. Assuming constant dust properties throughout the cloud, the IRAS ratio <I_60/I_100> decreases in densest 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 thinner clouds. This requires that most of the small grains are removed in these regions, and possibly a modification of the properties of large grains.