and one strongly prolate. Overall, we find that the many assumptions required make this type of analysis susceptible to errors.'
author:
- |
    S. P. C. Peters$^{1}$, P. C. van der Kruit$^{1}$[^1], R. J. Allen$^{2}$ and K. C. Freeman$^{3}$\
    $^{1}$Kapteyn Astronomical Institute, University of Groningen, P.O.Box 800, 9700AV Groningen, the Netherlands\
    $^{2}$Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA\
    $^{3}$Research School of Astronomy and Astrophysics The Australian National University, Cotter Road Weston Creek, ACT 2611,\
    Australia
bibliography:
- 'refsV.bib'
date: 'Accepted 2015 month xx. Received 2015 Month xx; in original form 2015 Month xx'
title: |
    The Shape of Dark Matter Haloes\
    V. Analysis of observations of edge-on galaxies
---

\[firstpage\]

galaxies: haloes, galaxies: kinematics and dynamics, galaxies: photometry, galaxies: spiral, galaxies: structure

Introduction {#sec:dmintro}
============

Modern day cosmological dark matter simulations predict that dark matter has a significant impact on the formation and evolution of galaxies. The dark matter clumps into haloes, which serve as gravitational sinks for baryonic matter to fall in to. Once inside, these baryons form the galaxies and other visible structures in the universe. The size and shape of these haloes is influenced by the type of dark matter particle and 