PROBING THE DUSTY ACCRETION TORUS OF SEYFERT-GALAXIES

We show that the IRAS colors of Seyfert galaxies can be understood in terms of a model in which we see emission by hot dust near its sublima tion temperature emitting a spectrum that varies little from object to object. For objects observed through the dusty accretion torus, which is optically thick at 12 mu m, this dust emission is absorbed to vari ous degrees. In addition, in many objects, this spectrum is veiled by a component produced by a circumnuclear starburst. The hidden broad-li ne objects all lie along the reddening line in IRAS color-color plots, and the dust extinction at 12 mu m lies in the range 0.5-2.5, which i mplies an H I column density of similar to 5 x 10(22) cm(-2) for the h ot circumnuclear dust located at about 3 pc from the central engine. F or these objects we can also estimate the true luminosities of the cen tral active nuclei from the dereddened IR fluxes. If the simple accret ion flow model is correct, then typical accretion rates are on the ord er of 10 M. yr(-1). The radiation pressure of the central active galac tic nucleus acting on the inner portions of the dust torus is likely t o play a critical role in controlling the accretion how toward the nuc leus and in forming the ''ionization'' cones seen in the narrow-line r egions of Seyfert galaxies.