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Baryons in the Warm‐Hot Intergalactic Medium

Romeel DaveHubble fellowRenyue CenPrinceton University Observatory, Princeton, NJ 08544Jeremiah P. OstrikerPrinceton University Observatory, Princeton, NJ 08544Greg L. BryanDepartment of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139Lars HernquistHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138Neal KatzDepartment of Astronomy, University of Massachusetts, Amherst, MA 01003David H. WeinbergDepartment of Astronomy, Ohio State University, Columbus, OH 43210Michael L. NormanAstronomy Department, University of Illinois at Urbana-Champaign, Urbana, IL 61801Brian O’SheaAstronomy Department, University of Illinois at Urbana-Champaign, Urbana, IL 61801

2001en

ABI

Annotatsiya

Approximately 30%40% of all baryons in the present-day universe reside in a warm-hot intergalactic medium (WHIM), with temperatures in the range 105 \ T \ 107 K. This is a generic prediction from six hydrodynamic simulations of currently favored structure formation models having a wide variety of numerical methods, input physics, volumes, and spatial resolutions. Most of these warm-hot baryons reside in di use large-scale structures with a median overdensity around 1030, not in virialized objects such as galaxy groups or galactic halos. The evolution of the WHIM is primarily driven by shock heating from gravitational perturbations breaking on mildly nonlinear, nonequilibrium structures such as laments. Supernova feedback energy and radiative cooling play lesser roles in its evolution. WHIM gas may be consistent with observations of the 0.25 keV X-ray background without being signicantly heated by nongravitational processes because the emitting gas is very di use. Our results conrm and extend previous work by Cen & Ostriker and et al.

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DOI: 10.1086/320548

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