Characterising bars in low surface brightness galaxies
  In this paper, we use $\textit{B}$-band, $\textit{I}$-band, and 3.6 $\mu$m
azimuthal light profiles of four low surface brightness (LSB) galaxies (UGC
628, F568-1, F568-3, F563-V2) to characterise three bar parameters: length,
strength, and corotation radius. We employ three techniques to measure the
radius of the bars, including a new method using the azimuthal light profiles.
We find comparable bar radii between the $\textit{I}$-band and 3.6 $\mu$m for
all four galaxies when using our azimuthal light profile method, and that our
bar lengths are comparable to those in high surface brightness galaxies (HSBs).
In addition, we find the bar strengths for our galaxies to be smaller than
those for HSBs. Finally, we use Fourier transforms of the $\textit{B}$-band,
$\textit{I}$-band, and 3.6 $\mu$m images to characterise the bars as either
`fast' or `slow' by measuring the corotation radius via phase profiles. When
using the $\textit{B}$ and $\textit{I}$-band phase crossings, we find three of
our galaxies have faster than expected relative bar pattern speeds for galaxies
expected to be embedded in centrally-dense cold dark matter haloes. When using
the $\textit{B}$-band and 3.6 $\mu$m phase crossings, we find more ambiguous
results, although the relative bar pattern speeds are still faster than
expected. Since we find a very slow bar in F563-V2, we are confident that we
are able to differentiate between fast and slow bars. Finally, we find no
relation between bar strength and relative bar pattern speed when comparing our
LSBs to HSBs.
