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Research
My PhD research focuses on galaxies in cluster environments, specifically on galaxies that are falling into the Fornax galaxy cluster. As these systems started their evolution outside of the cluster and then change into a cluster environment, they provide an excellent test sample to study how the cluster environment changes their evolution. While falling into the cluster, a galaxy can be subject to tidal interactions with the large-scale cluster potential, direct gravitational interactions with other cluster members or ram-pressure stripping of their diffuse gas. To understand these systems better, I am taking two approaches:
Star Formation Histories of Fornax Infallers
To reconstruct the consequences from interactions with the cluster, tracing back the star formation history (SFH) is an important step. I determine the SFH by combining spectra from the integral field spectrograph MUSE with multi band photometry from the S-PLUS survey. The S-PLUS photometry allows to overcome MUSE’s limited wavelength range by extending the observed wavelength to blue bands, which is especially important for analysing young stellar populations. For the spectrophotometric fit, I am using the spectral synthesis code STARLIGHT, which creates a synthetic spectrum by combining a set of synthetic stellar populations models with different ages and metallicities that matches the observed spectrum.
Galaxy Distances with the Planetary Nebulae Luminosity Function
Accurate distance measurements can help to identify cluster members and allow to place the galaxy within the 3D structure of the cluster more accurately. Typically, cluster infallers are classified based on their projected phase-space diagram. Getting an estimate for the 3D distance to the centre of the cluster as supposed to the projected distance, could help to make this classification more accurate. As a distance indicator, I am using the planetary nebulae luminosity function (PNLF). Planetary nebulae can be found in all types of galaxies, which makes the PNLF a universal tool. To compute the PNLF, I am using adaptive-optics assisted MUSE observations to evaluate how much the accuracy increases compared to measurements without adaptive optics.
