Individual Estimates of the Virial Factor in 10 Quasars: Implications on
  the Kinematics of the Broad Line Region
  Assuming a gravitational origin for the Fe III$\lambda\lambda$2039-2113
redshift and using microlensing based estimates of the size of the region
emitting this feature, we obtain individual measurements of the virial factor,
$f$, in 10 quasars. The average values for the Balmer lines, $\langle
f_{H\beta}\rangle={\bf 0.43\pm 0.20}$ and $\langle f_{H\alpha}\rangle={\bf
0.50\pm 0.24}$, are in good agreement with the results of previous studies for
objects with lines of comparable widths. In the case of Mg II, consistent
results, $f_{Mg II} \sim {\bf 0.44}$, can be also obtained accepting a
reasonable scaling for the size of the emitting region. The modeling of the
cumulative histograms of individual measurements, $CDF(f)$, indicates a
{relatively} high value for the ratio between isotropic and cylindrical
motions, $a\sim {\bf 0.4}-0.7$. On the contrary, we find very large values of
the virial factor associated to the Fe III$\lambda\lambda$2039-2113 blend,
$f_{FeIII}=14.3\pm2.4$, which can be explained if this feature arises from a
flattened nearly face-on structure, similar to the accretion disk.
