Speaker
Description
Galaxy clusters are the largest gravitationally bound systems in the universe. Most of the baryonic matter in clusters is found not in the stars and galaxies, but in the surrounding X-ray emitting intra-cluster medium (ICM). Using observations of the ICM we can determine key properties of these clusters such as their mass, temperature, luminosity, and density profiles. However, statistical studies of ICM properties may be biased when clusters are selected based on ICM properties (i.e. via X-rays or the Sunyaev-Zel'dovich effect). For example, recent work has found that using an optically selected sample of clusters returned a shallower and more scattered $L-M$ scaling relation than what is recovered with traditional selection techniques. We will present a study of the X-ray properties of galaxy clusters selected with different methods to explore the impact of these biases. The breadth of the all-sky eRASS1 data provides an ideal test bed for this investigation as it provides automatic X-ray coverage of large samples of clusters detected by different techniques.
