Mg II line properties in lobe-dominated quasars
  We investigate the relationships between Mg ii {\lambda}2798 emission line
properties, as well as between these properties and inclination angle and Fe ii
strength, in a lobe-dominated quasar sample. We find no correlation between Mg
ii line width and inclination, unlike previous studies of the general quasar
population. This suggests that the Mg ii emission region in these objects is
not of a thin disk geometry, however the average equivalent width of the line
negates a spherical alternative. A positive correlation between Mg ii
equivalent width and inclination cannot be ruled out, meaning there is no
strong evidence that Mg ii emission is anisotropic. Since thin disk emission
would be highly directional, the geometric implications of these two findings
are compatible. The lack of line width correlation with inclination may also
indicate that Mg ii is useful for estimating black hole masses in
lobe-dominated quasar samples, since it is unbiased by orientation. Some
quasars in our sample have almost edge-on viewing angles and therefore cannot
have a smooth toroidal obscurer co-planar with the accretion disk. Alternatives
may be a distorted dusty disk or a clumpy obscurer. This could result from the
sample selection bias towards high inclination objects, rather than intrinsic
differences between lobe-dominated and typical quasars. Five objects have
visible [O iii] allowing equivalent width calculation, revealing it to be
higher than in typical quasars. Since these objects are of high inclination,
this finding supports the positive correlation between [O iii] equivalent width
and inclination found in a previous study.
