Where Are the Baryons? II. Feedback Effects

By Renyue Cen, Jeremiah P. Ostriker. 2005

322 citations recorded by the source corpus.

Numerical simulations of the intergalactic medium have shown that at the present epoch, a significant fraction (40%-50%) of the baryonic component should be found in the (T ~ 106 K) warm-hot intergalactic medium (WHIM)—with several recent observational lines of evidence indicating the validity of the prediction. We here recompute the evolution of the WHIM with the following major improvements: (1) galactic superwind feedback processes from galaxy and star formation are explicitly included; (2) major metal species (O V to O IX) are computed explicitly in a nonequilibrium way; and (3) mass and spatial dynamic ranges are larger by factors of 8 and 2, respectively, than in our previous simulations. Here are the major findings: (1) Galactic superwinds have dramatic effects, increasing the WHIM mass fraction by about 20%, primarily through heating of warm gas near galaxies with density 101.5-104 times the mean density. (2) The fraction of baryons in the WHIM is increased modestly from the earlier work but is still ~40%-50%. (3) The gas density of the WHIM is broadly peaked at a density 10-20 times the mean density, ranging from underdense regions to regions that are overdense by 103-104. (4) The median metallicity of the WHIM is 0.18 Z☉ for oxygen, with 50% and 90% intervals being (0.040, 0.38) and (0.0017, 0.83).

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

CONSTRAINING THE MILKY WAY'S HOT GAS HALO WITH O vii AND O viii EMISSION LINES (2014, background): “This metallicity is also consistent with simulations of galactic coronae (Toft et al. 2002; Cen & Ostriker 2006; Cen 2012).”
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).”
Radiative Feedback from Massive Black Holes in Elliptical Galaxies: AGN Flaring and Central Starburst Fueled by Recycled Gas (2007, background): “…each radius r from the equation ̇þ ¼ form form ; form ¼ max cool; dyn ; ð15Þ where is the local gas density, form ¼ 0:03Y0:4 (see, e.g., Weinberg et al. 2002; Cen & Ostriker 2006), and the associated characteristic times are cool E C ; dyn ¼ min Jeans; rotð…”
The enrichment of the intergalactic medium with adiabatic feedback – I. Metal cooling and metal diffusion (2009, methodology): “At z=0, about 40% of the mass is in WHIM, consistent previous simulations with different methods (Cen & Ostriker 2006; Oppenheimer & Davé 2006).”
Gravitational quenching in massive galaxies and clusters by clumpy accretion (2007, background): “Most of the gas is shock heated to such temperatures in haloes more massive than ∼ 1012M⊙, as well as in nearby collapsed pancakes and filaments that feed such haloes (Cen & Ostriker 2006).”
Figuring Out Gas & Galaxies in Enzo (FOGGIE). I. Resolving Simulated Circumgalactic Absorption at 2 ≤ z ≤ 2.5 (2018, methodology): “We use Enzo’s Cen & Ostriker (2006) thermal supernova feedback model, forming stars in gas exceeding a comoving number density of ;0.1 cm−3 with a minimum star particle mass of 2×104 Me.”
THE STRUCTURE OF THE MILKY WAY'S HOT GAS HALO (2013, background): “This metallicity is consistent with cosmological simulations (Toft et al. 2002; Cen & Ostriker 2006) and observations of both spiral galaxies (Rasmussen et al. 2009; Meiring et al. 2013) and some HVCs (Gibson et al. 2000; van Woerden & Wakker 2004; Fox et al. 2005).”
A new measurement of the evolving near-infrared galaxy luminosity function out to z≃ 4: a continuing challenge to theoretical models of galaxy formation (2008, methodology): “obtained with fully hydrodynamic simulations in a cosmological context by Nagamine et al. (2006) and Cen & Ostriker (2006).”
Feedback and recycled wind accretion: assembling the z= 0 galaxy mass function (2009, background): “…et al. 2003; Martin 2005a; Weiner et al. 2009) have motivated the inclusion of star formation based feedback prescriptions in cosmological simulations (Springel & Hernquist 2003b; Kobayashi 2004; Cen & Ostriker 2006; Oppenheimer & Davé 2006; Sommer-Larson & Fynbo 2008; Wiersma et al. 2009b).”
ESCAPE FRACTION OF IONIZING PHOTONS DURING REIONIZATION: EFFECTS DUE TO SUPERNOVA FEEDBACK AND RUNAWAY OB STARS (2014, methodology): “To alleviate the problem,Cen & Ostriker (2006) distributed the thermal energy over 27 neighboring cells weighted by specific volume, which has the virtue of being able to mimic propagation of an explosion that is preferentially channelled into more diffuse regions.”
The Evolution of the Intergalactic Medium (2015, background): “…been shock-heated into a “warm/hot” 105 − 107K phase (with the fraction of gas roughly constant per interval in log T over 105 − 107K at z = 0; Cen & Ostriker 1999; Davé et al. 2001; Croft et al. 2001; Cen & Ostriker 2006), temperatures where the hydrogen becomes further ionized by collisions.”
The physics of the intergalactic medium (2007, background): “Exam- 57 ples of recent wind simulations include Theuns et al. (2002b), Aguirre et al. (2005), Cen et al. (2005), Cen and Ostriker (2006), Oppenheimer and Davé (2006), Kobayashi et al. (2007), and Kawata and Rauch (2007).”
PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper (2013, background): “e WHIM phase, with over-densities between 5 to 200 times the critical density and temperatures around 105–107 K, is expected to reside mostly in ﬁlaments, but also around and between massive clusters [30,31]. The SZ thermal pressure contribution of this cosmic web of gas [65] is potentially detectab”
METALLICITY-DEPENDENT QUENCHING OF STAR FORMATION AT HIGH REDSHIFT IN SMALL GALAXIES (2011, background): “…to implement stellar feedback in simulations and semi-analytic models (SAM) are not really satisfactory (Springel & Hernquist 2003; Kobayashi 2004; Cen & Ostriker 2006; Oppenheimer & Davé 2006; Governato et al. 2007), because they operate on scales too small to be resolved, and have to be…”
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).”
THICK DISKS OF EDGE-ON GALAXIES SEEN THROUGH THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G): LAIR OF MISSING BARYONS? (2011, background): “Part of the missing baryons are expected to be found in hot gas in the warm-hot intergalactic medium (WHIM; see, e.g., Fukugita et al. 1998; simulations from Cen & Ostriker 2006 and WHIM emission detection/constraining by Hickox & Markevitch 2007 and Zappacosta et al. 2010).”
Chemical enrichment of galaxy clusters from hydrodynamical simulations (2007, background): “Recent numerical studies of the key role played by winds in enriching diffuse cosmic baryons have been presented by Davé & Oppenheimer (2006), who focused their analysis on the highredshift IGM, and by Cen & Ostriker (2006), who concentrated on the study of the WHIM.”
PROBING THE INTERGALACTIC MEDIUM/GALAXY CONNECTION. V. ON THE ORIGIN OF Lyα AND O vi ABSORPTION AT z < 0.2 (2011, background): “Comprehensive modeling of the chemical enrichment of the IGM that includes galaxy formation and metal transport are required to further explore this topic (e.g. Cen & Ostriker 2006; Ganguly et al. 2008; Oppenheimer & Davé 2008, 2009).”
The Search for the Missing Baryons at Low Redshift (2007, background): “In their simulations with such feedback, Cen & Ostriker (2006) show that the energetics of their galactic superwinds is an order of magnitude smaller than shock heating by cosmological structures.”