Hubble Space Telescope (HST) spectroscopy has revealed a remarkable 
population of dwarf Seyferts with an unusually large broad-line region (BLR). 
These objects are remarkable for two reasons. Firstly, the size of the BLR 
can, in some cases, rival those seen in the most luminous quasars. Secondly, 
the size of the BLR is not correlated with the AGN luminosity, an observation 
that distinguishes them from reverberating active galactic nuclei. 
Collectively, these early results suggest that non-reverberating dwarf 
Seyferts are a very heterogeneous group, and not simply scaled versions of 
their reverberating counterparts. Close inspection with HST reveals broad H 
Balmer emission lines with single peaks, double peaks, and a combination of 
the two, suggesting that the broad emission lines are produced in 
kinematically distinct regions centered on the black hole (BH). Since the 
gravitational field strength is already known for these objects, by virtue of 
knowing their BH mass, the relationship between velocity, and radius may be 
established, given a kinematic model for the BLR gas. In this way, one can 
determine the inner, and outer radii of the BLRs by modeling the shape of 
their broad emission line profiles. High quality spectra obtained with the 
Space Telescope Imaging Spectrograph will be presented for M81, NGC 3998, 
NGC 4203, NGC 3227, NGC 4051, and NGC 3516 enabling a determination of the 
size, structure, and ionization of the BLR in these dwarf Seyfert galaxies.