  We have obtained near-IR spectra of five Active Galactic Nuclei that exhibit
double-peaked Balmer Emission Lines (NGC 1097, Pictor A, PKS 0921-213, 1E
0450.30-1817, and IRAS 0236.6-3101). The stellar velocity dispersions of the
host galaxies were measured from the Ca II 8494,8542,8662 Angstrom absorption
lines and were found to range from 140 to 200 km/s. Using the well-known
correlation between the black hole mass and the stellar velocity dispersion,
the black hole masses in these galaxies were estimated to range from 4x10^7 to
1.2x10^8 solar masses. We supplement the observations presented here with
estimates of the black holes masses for five additional double-peaked emitters
(Arp 102B, 3C 390.3, NGC 4579, NGC 4203, and M81) obtained by other authors
using similar methods. Using these black hole masses, we infer the ratio of the
bolometric luminosity to the Eddington luminosity, L_bol/L_Edd. We find that
two objects (Pictor A and PKS 0921--213) have L_bol/L_Edd ~ 0.2, whereas the
other objects have L_bol/L_Edd <~ 10^-2 (nearby, low-luminosity double-peaked
emitters are the most extreme, with L_bol/L_Edd <~ 10^-4). The physical time
scales in the outer regions of the accretion disks (at r ~ 10^3 GM/c^2) in
these objects were also estimated and range from a few months, for the
dynamical time scale, to several decades for the sound crossing time scale. The
profile variability in these objects are typically an order of magnitude longer
than the dynamical time, but we note that variability occurring on the
dynamical time scale has not been ruled out by the observations.
