Revisiting the cosmic cooling crisis

By M. Balogh, Frazer R. Pearce, Richard Kay. 2001

222 citations recorded by the source corpus.

Recent measurements of the K-band luminosity function now provide us with strong, reliable constraints on the fraction of baryons which have cooled. Globally, this fraction is only about 5 per cent, and there is no strong evidence that it is significantly higher in clusters. Without an effective subgrid feedback prescription, the cooled gas fraction in any numerical simulation exceeds these observational constraints, and increases with increasing resolution. This compromises any discussion of galaxy and cluster properties based on results of simulations which include cooling but do not implement an effective feedback mechanism.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/e1c8cd7beb70040d7dd9215d501a1229a8dc46d3

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Citations in the corpus

The Mass-to-Light Function of Virialized Systems and the Relationship between Their Optical and X-Ray Properties (2001, result): “This is in agreement with the results of Balogh et al. (2001).”
Shaping the galaxy stellar mass function with supernova- and AGN-driven winds (2012, background): “Cosmological hydrodynamical simulations that account for radiative cooling but lack feedback processes associated with star formation fail to reproduce this behaviour and strongly overpredict the stellar mass fractions of halos (Balogh et al. 2001).”
Hydrodynamical simulations of cluster formation with central AGN heating (2005, background): “However, up to the present time, optical and X-ray observations have failed to detect the required amount of this cool gas, suggesting that it is simply not there (e.g. McNamara et al. 2000; Tamura et al. 2001; Balogh et al. 2001; Kaastra et al. 2001; Fabian et al. 2001; C© 2005 The Authors.”
The Birmingham-CfA cluster scaling project - III. Entropy and similarity in galaxy systems (2003, background): “Unless this cooled gas does not form stars, the very high star formation efficiencies implied are far above those observed in clusters (c.f. discussion in Paper II) or inferred globally from the K-band luminosity function of galaxies (Balogh et al. 2001).”
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations (2015, background): “…become a cause célèbre for the simulation community, owing to the long-standing need to address the closely related ‘overcooling’ (Cole 1991; White & Frenk 1991; Blanchard, Valls-Gabaud & Mamon 1992; Balogh et al. 2001) and ‘angular momentum’ (Katz & Gunn 1991; Navarro & White 1994) problems.”
GRACKLE: a chemistry and cooling library for astrophysics (2016, background): “This effect is likely related to the over-cooling problem that has classically plagued cosmological simulations (e.g. Katz et al. 1996; Balogh et al. 2001).”
Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation (2002, background): “…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 amount of baryons in…”
How Stellar Feedback Simultaneously Regulates Star Formation and Drives Outflows (2015, background): “Thus, the ratio of stellar mass to halo mass should be equal to the baryon fraction (e.g.Cole 1991; White & Frenk 1991; Blanchard et al. 1992; Balogh et al. 2001); however, for all halo masses, the stellar-to-halo mass ratio is much less than this value (e.g.Conroy & Wechsler 2009; Moster et al.…”
Stellar and dynamical masses of ellipticals in the Sloan Digital Sky Survey (2003, background): “This is not necessarily inconsistent with the global stellar mass fraction, which is only around 5-10% of baryons (Balogh et al. 2001; Dickinson et al. 2003): it suggests that the efficiency of star formation peaks at Mvir ∼ 1012M⊙ and is likely to be much smaller in either lower and higher mass…”
Feedback and recycled wind accretion: assembling the z= 0 galaxy mass function (2009, background): “The fact that their correction factor is always greater than one exemplifies the “over-cooling” problem in galaxy formation, where the efficiency of forming stars, based on simple theoretical expectations, is greater than that actually observed (e.g. White & Frenk 1991; Balogh et al. 2001).”
The case for AGN feedback in galaxy groups (2009, background): “…in a forthcoming paper, simply changing from primordial cooling rates to including metal-dependent radiative cooling as well, can increase the stellar fraction by a factor of 2 or more. over-efficiency problem has been termed the ‘cooling crisis’ of cosmological simulations (Balogh et al. 2001).”
Cosmological simulations of intergalactic medium enrichment from galactic outflows (2006, methodology): “SH03 found that the multi-phase model produces self-regulated star formation that does not suffer from runaway star formation with increasing resolution, as seen in previous simulations (Balogh et al. 2001; Davé et al. 2001).”
The formation of disc galaxies in high-resolution moving-mesh cosmological simulations (2013, background): “…and almost universally too concentrated and massive bulges (e.g. Scannapieco et al. 2009), their rotation curves had unrealistic shapes (e.g. Hummels & Bryan 2012), and in general they were far too luminous (e.g. Martig et al. 2012) as a result of the “overcooling catastrophe” (Balogh et al. 2001).”
Simulating galactic outflows with kinetic supernova feedback (2008, background): “Modelling SN feedback in simulations of the formation of galaxies is known to be a difficult task, mostly because the injected thermal energy tends to be radiated away well before it has any hydrodynamical effect (e.g. Katz, Weinberg, & Hernquist 1996; Balogh et al. 2001).”
Towards a realistic population of simulated galaxy groups and clusters (2013, background): “…the ‘cooling catastrophe’ (i.e. the general tendency of simulated galaxies and groups and clusters of galaxies to form far too many stars; e.g. Balogh et al. 2001), which has generally plagued cosmological hydrodynamical simulations since their advent, has largely been overcome in…”