Baryons in the Warm-Hot Intergalactic Medium

By R. Dav'e, Renyue Cen, Jeremiah P. Ostriker, Greg L. Bryan, L. Hernquist, Neal Katz, D. Weinberg, M. Norman, Brian W. O'Shea. 2000

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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 diffuse large-scale structures with a median overdensity around 10-30, 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 filaments. 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 significantly heated by nongravitational processes because the emitting gas is very diffuse. Our results confirm and extend previous work by Cen & Ostriker and Davé et al.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9a2f6c296d791943738213feaa5e06529d88c598

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Citations in the corpus

The Search for the Missing Baryons at Low Redshift (2007, background): “Such calculations, even without the effects of star formation and stellar feedback, demonstrate the fraction of gas that would be in the 105-107 K range (40% in the calculations of Cen & Ostriker 2006; see also Croft et al. 2001; Davé et al. 2001).”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “In X-rays the tenuous Warm-Hot Intergalactic Medium expected to reside in filaments [378] has been seen in emission [1241] and absorption [253, 469].”
A High-Resolution Survey of Low-Redshift QSO Absorption Lines: Statistics and Physical Conditions of O VI Absorbers (2007, background): “…the history of the universe, but the IGM is predicted to change from predominantly cool, photoionized gas at high redshifts to a mixture of shock-heated gas, photoionized gas, and condensed objects (stars) at low redshifts (Cen & Ostriker 1999; Davé et al. 1999,2001; Cen & Ostriker 2006).”
An analytical model for the history of cosmic star formation (2002, background): “…of 9.3 per cent, and consistent with observational constraints (Fukugita, Hogan & Peebles 1998; Balogh et al. 2001; Cole et al. 2001) once the baryons in the warm to hot intergalactic medium (IGM) (Cen & Ostriker 1999; Davé et al. 1999, 2001) are taken into account (Springel & Hernquist 2003b).”
A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, background): “This smallest shortfall is believed to be due to WHIM baryons (Davé et al. 2001).”
Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, background): “…volume (required for making statistically meaningful comparisons with large observed data sets) to be ever improved (Pearce et al. 1999; Davé et al. 2001; Springel & Hernquist 2003b; Planelles & Quilis 2009; Cui et al. 2012; Dubois et al. 2014; Khandai et al. 2014; Schaye et al. 2014).”
Cosmological smoothed particle hydrodynamics simulations: the entropy equation (2001, background): “These phases are defined as in Davé et al. (2001): Gas with temperatures above 107 K is referred to as ‘hot’, gas with temperatures between 105 K and 107 K is ‘warm’, and at lower temperatures gas is either labelled ‘diffuse’ if it is at overdensities ρ < 1000 ρ , or ‘condensed’ (cold) for ρ >…”
PROBING THE INTERGALACTIC MEDIUM/GALAXY CONNECTION. V. ON THE ORIGIN OF Lyα AND O vi ABSORPTION AT z < 0.2 (2011, background): “Indeed, the collapse of large-scale density ‘waves’ is predicted to drive the production of the WHIM in cosmological simulations (e.g. Cen & Ostriker 1999; Davé et al. 2001) and may, in principle, heat the CGM of sub-L∗ galaxies.”
SIMULATIONS OF THE MICROWAVE SKY (2009, background): “Hallman et al. (2009) also found that the angular power spectrum of the filamentary warm-hot intergalactic medium (WHIM Cen & Ostriker 1999; Davé et al. 2001) is only.”
THE BARYON CENSUS IN A MULTIPHASE INTERGALACTIC MEDIUM: 30% OF THE BARYONS MAY STILL BE MISSING (2011, background): “An inefficient distribution of collapsed baryons vs. distributed matter is a prediction of nearly all cosmological simulations of large-scale structure formation (Cen & Ostriker 1999, 2006; Davé et al. 1999, 2001; Smith et al. 2011; Tepper-Garcia et al. 2011).”
Time-dependent Ionization in Radiatively Cooling Gas (2006, background): “An intergalactic shock heated WHIM is expected to be a major reservoir of baryons in the low redshift universe (Cen & Ostriker 1999; Davé et al. 2001; Furlanetto et al. 2005).”
Intercluster filaments in a ΛCDM Universe (2004, background): “For the most recent studies see Davé et al. (2001), Kravtsov et al. (2002), and Furlanetto et al. (2003) and references therein.”
Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation (2002, background): “…that cooling alone is quite efficient (e.g. White & Rees, 1978; White & Frenk, 1991; Katz & White, 1993; Pearce et al., 1999; Lewis et al., 2000; Davé et al., 2001; Balogh et al., 2001; Springel & Hernquist, 2002a), leading to a collapse fraction well in excess of observational bounds on the…”
DO HOT HALOS AROUND GALAXIES CONTAIN THE MISSING BARYONS? (2010, background): “Based on cosmological simulations, the rest of the baryon budget is thought to reside in the “warm-hot intergalactic medium” (WHIM), at temperatures between 105 and 107 K (Cen & Ostriker 1999; Davé et al. 2001).”
Galaxy Evolution in Cosmological Simulations with Outflows II: Metallicities and Gas Fractions (2011, background): “But unfettered inflow grossly overproduces global star formation, known as the overcooling problem (e.g. Davé et al. 2001; Balogh et al. 2001).”
Quasar Feedback: The Missing Link in Structure Formation (2004, background): “If no feedback or preheating is invoked, highresolution simulations predict that 30%–40% of the gas in clusters should cool (Suginohara & Ostriker 1998; Lewis et al. 2000; Davé et al. 2001).”
Gamma Rays from Intergalactic Shocks (2002, background): “128 undetected warm-hot intergalactic medium (WHIM), gas at temperatures 105 KdTd107 K that is believed to contain a large fraction of the baryons in the low-redshift universe (see, e.g., Davé et al. 2001).”
The Progenitors of Dwarf Spheroidal Galaxies (2002, background): “The origin of such features is not fully established, but they are most likely due to a combination of cosmic structure growth and disturbances associated with galaxies (e.g., Oort 1970; Davé et al. 2001).”