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C. Halliday, D. Carter, Z.C. Jackson (Liverpool John Moores University)
Measuring the distribution of dynamical mass within galaxies offers a powerful constraint on their evolution. We present radial velocity measurements for 300 planetary nebulae within M31 obtained using [OIII] emission line observations to constrain the kinematical and dynamical structure of the galaxy halo. We plan to apply non-parametric models by Merritt and collaborators to allow the measurement of the dynamical structure without restrictive assumptions about the galaxy potential and distribution function.
We will compare these data with radial velocities for 200 globular clusters in M31 to test whether the globular clusters and planetary nebulae populations trace similar populations. If these two populations are both found to trace the old bulge stellar population, these data will be used together to better constrain the models.
We gratefully acknowledge the support of a PPARC Grant no. PPA/G/S/1998/00114. ZCJ acknowledeges support of a LJM University fellowship.
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