I am interested in the formation, evolution, and dynamics of galaxies ranging from our own Milky Way to the most massive galaxies found at the centres of galaxy clusters. In my PhD research I started using Planetary Nebulae (PNe) as kinematic tracers for the build-up of the extended halos of massive early-type galaxies. Below is a selection of current and past research projects that I have been involved in.
The halo of M105 and its group environment as traced by planetary nebulae populations
The galaxy M105 in the Leo I group has been at the centre of a long-standing debate on the dark matter (DM) content of early-type galaxies and is one of the poster children of the Planetary Nebula Spectrograph (PN.S) early-type galaxy survey. We have recently obtained more extended photometric and kinematic data to place better constraints on the assembly history of M105 and its group environment. The figure on the left shows the PNe detected in M105 and its companion spiral galaxy NGC 3384 colour-coded by their velocity.
We have performed a novel photo-kinematic decomposition of of our sample into two subcomponents associated with NGC 3384 and M105 using Gaussian Mixture Models and are currently investigating the presence and dynamics of intra-group light in this loose group of galaxies. These new data will also allow us to better constrain the matter content of M105 at large radii. First results are presented in Chapter 4 of my PhD thesis.
Three dynamically distinct stellar populations in the halo of M49
For the second project of my PhD, I investigated the kinematics in the outer halo of the early-type galaxy M49, the brightest galaxy in the Virgo Cluster. As kinematic tracers, we used planetary nebulae. We employed a multi-Gaussian model for the velocity distribution to identify stellar populations with distinct kinematics and histories
We detected stellar-kinematic substructure associated with the interaction of M49 with the dwarf irregular galaxy VCC 1249. We find two kinematically distinct PN populations associated with the main M49 halo and the extended intra-group light (IGL). The dispersion of the PNe associated with the IGL joins onto that of the satellite galaxies in subcluster B at 100 kpc radius. This is the first time that the transition from halo to IGL is observed based on the velocities of individual stars (see Figure on the right). Therefore the halo of M49, consisting of at least three distinct components, has undergone an extended accretion history within its parent group potential.
The halo of M 49 and its environment as traced by planetary nebulae populations
Prior to our work on the kinematics of M49, we carried out a photometric survey with the aim to detect PNe in the halo of this galaxy. PNe were identified based on their bright [OIII]5007 Å emission and absence of a broad-band continuum through automated detection techniques. We identified 738 PNe out to a radius of 155 kpc from M 49's centre from which we define a complete sample of 624 PNe.
Comparing the PN number density to the broad-band stellar surface brightness profile, we find a variation of the PN-specific frequency (α-parameter) with radius. The outer halo beyond 60 kpc has a 3.2 times higher α-parameter compared to the main galaxy halo, which is likely due to contribution from the surrounding blue IGL.
Dynamical modelling of the dwarf spheroidal galaxies Ursa Minor and Draco
For my Master Research project, I studied the two Local Group dwarf galaxies Ursa Minor and Draco. These two galaxies are an interesting pair to study, since they are similar in terms of mass, extent, and distance. However, while Draco appears to have a perfect, undisturbed stellar distribution, Ursa Minor shows signs of tidal disturbance. Using new optical spectroscopic velocity data, we applied orbit-based Schwarzschild modeling to constrain the (dark) matter distribution of the galaxies.
Modeling the Gravitational Potential of a Cosmological Dark Matter Halo with Stellar Streams
This project, lead by Dr. Robyn Sanderson, built on my Bachelor Research project, in which I investigated how to determine the gravitational potential of a cosmological dark matter halo using stellar streams. We determined the best-fit potential parameters by maximizing the amount of clustering of the stream stars in the space of their actions. We show that using our set of streams from the Aquarius Simulation, we recover a mass profile that is consistent with the spherically averaged dark matter profile of the host halo, although we ignored both triaxiality and time evolution in the fit.