Rain Kipper will defend his doctoral thesis titled “Galaxy modelling: dynamical methods and applications” on 31. August 2016 at 14.15 at W. Ostwaldi 1, room B103.
Elmo Tempel, Tartu Observatory
Peeter Tenjes, Institute of Physics, University of Tartu
Pekka Heinämäki,Tuorla Observatory, Finland
Gert Hütsi, Tartu Observatory
The aim of the present Thesis was to develop a method to study the dynamics of galaxies and vari-ous effects that could affect the comparison of the model calculations with observations. Measured kinematic quantities provide us with a possibility to constrain the mass distribution of galaxies. A common way for it is to model the kinematics via solving the Jeans equations – the equations de-rived from collisionless Boltzmann equation to describe the stellar motions. From the classical point of view, the task is degenerated: one cannot distinguish the distortions of velocities from different mass distributions. In addition, a shortcoming of using the Jeans equations is that there are more variables than equations, and therefore the problem is not solvable by itself – we must use additional constraints. One possible source of constraints is a non-classical conserved quantity (third integral of motion) – a variable that is constant along the stellar orbit. This Thesis provided a new solution by choosing a specific form for the third integral of motion, which allows us to solve the Jeans equations. In the Thesis, we also studied various effects influencing the model input and output. We studied how well the stellar density distribution that is needed for the model input can be found from pho-tometric observations. Most parameters can be restored well, except the flatness of the component, for which the accuracy is moderate. For making the output of the model comparable with observa-tions, one has to take into account all the points on sightline and the convolution due to atmosphere and spectrograph slit. In case of high redshift galaxies, the effect can be very important. Our kinematic model allowed us to study an interesting topic – how much the presence of dust af-fects the kinematic parameters. The dust in galaxies hinders the visibility of the far side of galaxy, and therefore suppresses the influence of the kinematic parameters of that region.