Nowadays it is enough accepted that active galaxies are formed by a super massive black holes in the nucleus, which is surrounded by an accretion disk, a dusty torus, and in some cases by two collimated jets. The orientation of the dusty torus respect to the observer, have been key to explain much of the differences observed in the optical spectrum of the large family of active galaxies. However, it have failed explaining others: for example, the existence of “pure” Seyfert 2 galaxies. Because the emission of the dust peaks at mid-infrared (MIR), around 20-30 um, recent studies have used high angular resolution (subarcseconds) data to characterize the physical and geometrical properties of this structure. In this talk, I am going to present the results that we have obtained from studying the dusty torus in low and high luminosity AGNs using high angular resolution data at MIR, and how these results are changing the classical view of the unification scheme of AGNs.
