Presentation #428.06 in the session Galaxy Clusters.
The evolution of galaxies is strongly impacted by their immediate environment. For instance, It is well-established that the dense, hot medium inside clusters (ICM) efficiently strips galaxies flying through it of their cold gas and stars. It therefore prevents further star formation and strongly disturbs a galaxy’s dynamics. The impact of the cosmic environment on Mega-parsec scales is however a more recent field of study.
In the first part of my talk, I will show how simulations and observations alike confirm that the “cosmic web” — the sprawling network of filaments and nodes along which galaxies drift, accrete gas and merge — drives key properties of galaxies. This includes their angular momentum, star formation rate, shape, size, structure and more. I will show that these effects are crucially driven by the dynamics of the gas in and around filaments and not only by density considerations. I will explain how integral-field spectroscopy plays a growing role in demonstrating the origin of these trends.
A missing piece in understanding this interplay is the connection between the “cosmic web” and the local, highly disturbed environment of each galaxy. On the example of clusters and massive groups, I will show how we can explore these liminal spaces where large-scale structures become ambient circum-galactic medium and why they are important. I will show in particular that groups can contain remnants of cosmic filaments which constrain the orbits of satellites down to dwarf scales. In clusters, I will show that these remnants can shield galaxies in their midst from stripping, strangulation and more generally quenching.
A precise quantification of these effects requires elaborate mocks that can directly be compared to observations of clusters with ALMA, Hector or the up-coming Nancy Grace Roman telescope. I will present a new suite of simulations centred on clusters and massive groups, boasting unprecedented resolution (34 pc) for their volume (~10 Mpc) and density. I will explain how these can be used to track the fate of filamentary remnants in clusters in unprecedented details and to produce predictions for up-coming surveys.