Papers › The thermal and gravitational energy densities in the large-scale structure of the Universe
The thermal and gravitational energy densities in the large-scale structure of the Universe
Yi-Kuan Chiang, Ryu Makiya, Eiichiro Komatsu, Brice Ménard
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As cosmic structures form, matter density fluctuations collapse gravitationally and baryonic matter is shock-heated and thermalized. We therefore expect a connection between the mean gravitational potential energy density of collapsed halos, Ω_Wʰᵃˡᵒ, and the mean thermal energy density of baryons, Ωₜₕ. These quantities can be obtained using two fundamentally different estimates: we compute Ω_Wʰᵃˡᵒ using the theoretical framework of the halo model which is driven by dark matter statistics, and measure Ωₜₕ using the Sunyaev-Zeldovich (SZ) effect which probes the mean thermal pressure of baryons. First, we derive that, at the present time, about 90% of Ω_Wʰᵃˡᵒ originates from massive halos with M>10¹³ M_⊙. Then, using our measurements of the SZ background, we find that Ωₜₕ accounts for about 80% of the kinetic energy of the baryons available for pressure in halos at z≲0.5. This constrains the amount of non-thermal pressure, e.g., due to bulk and turbulent gas motion sourced by mass accretion, to be about Ωₙₒₙ₋ₜₕ≃0.4×10⁻⁸ at z=0.
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