the dusty gas is launched as a hydromagnetic wind [@Konigl1994; @Keating2012]. Heating of the ISM from stellar feedback might support the dusty gas in a puffy disk [@Hopkins2012-1]. The disk might be simultaneously supported by infrared radiation pressure [@Pier1992-1; @Krolik2007], or the infrared radiation pressure may generate a failed wind [@Dorodnitsyn2011-1; @Dorodnitsyn2012].

Regardless of what supports the torus, gas continues to be drawn in to the black hole accretion disk at small radii ($< 10^{17}$ cm), where it powers an active galactic nucleus (AGN). The radiation emitted from SMBH accretion disks influences the dynamics of the torus itself, along with the dynamics of the host galaxy. This feedback may act through a number of channels that include radiative heating [e.g. @DiMatteo2005], jets [@Silk2005; @Croton2006; @McNamara2007], and winds driven by radiation pressure on resonant ultraviolet lines [@Murray1995; @Proga2000] and dust [@Konigl1994; @Murray2005; @Keating2012]. Our challenge is to understand the combined effect of all these modes of interaction. Improving our understanding of this connection will be crucial for answering questions about the growth of SMBHs, observations of AGN, and the star formation histories in galaxies.

Recent observations have begun to reveal the violent impact that AGN may have on their host galaxies. 