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 \lambda \lambda 8494 , 8542 , 8662 ~ { } \AA absorption lines and were found to range from 140 to 200 { km s ^ { -1 } } .
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 4 \times 10 ^ { 7 } to 1.2 \times 10 ^ { 8 } ~ { } { M _ { \odot } } .
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 } \sim 0.2 , whereas the other objects have L _ { bol } / L _ { Edd } \lesssim 10 ^ { -2 } ( nearby , low-luminosity double-peaked emitters are the most extreme , with L _ { bol } / L _ { Edd } \lesssim 10 ^ { -4 } ) .
The physical time scales in the outer regions of the accretion disks ( at r \sim 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 .