Speaker
Description
As the largest and most massive gravitationally bound structures in the Universe, galaxy clusters stands at the crossroads between astrophysics and cosmology. Before they reach dynamical equilibrium, collapse and matter accretion from the cosmic web dictate their internal dynamics. Such objects are called protoclusters and are usually detected at $1.5<z<8$, way earlier than galaxy clusters themselves. This redshift range includes the Cosmic Noon, the star formation peak in the Universe in which protoclusters play a central role. Moreover, these structures are impacted by the values of cosmological parameters such as $\sigma_8$ and $H_0$, hence our motivation to understand them better.
Gas inside protoclusters have not been heated by gravitational collapse yet, which makes its Sunyaev Zeldovich and X-ray signal too faint for current telescopes. Therefore, their detection is based upon the search for galaxy overdensities at high redshift. I will present how I worked with data from Euclid Q1 combined with Spitzer to identify several solid protoclusters candidates using this method. I will also talk about how I detected their total mass for the first time using CMB lensing maps from the Atacama Cosmology Telescope.
| Other topic / keywords: | Galaxy protoclusters -- Galaxy clusters |
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