Title: X-ray emissions from the large scale structure of the Universe

CGM

Galaxies and hot CGM

eROSITA bubbles

Such a kind of bubbles are also found in Milky-Way like galaxies in TNG simulation.

Fig.1: eROSITA bubbles

Star-forming and quiscent galaxies

The y-axis is the X-ray luminosity from CGM.

The right figure indicates that the main driver for the X-ray luminosity from CGM is the halo mass, i.e., it is the virialization of the halo that drives the X-ray luminosity, not the feedback from the galaxies (not the interplay between CGM and the galaxies). Through virialization, the gas in the halo is heated up by the accretion shock to a temperature of ${10}^6$ K, which is the temperature of the hot CGM.

Baryon fraction inference

Stack galaxies and boost of satellite galaxies

Abundance and temperature of the outer skirts of hot CGM

Clusters and groups

Constraints on cosmological parameters

Conclusion