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A physical understanding of how reionization suppresses accretion onto dwarf halos
Cosmology and Nongalactic Astrophysics · Submitted 3 Jan 2014
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show that accretion is inhibited onto more massive halos than had been thought because previous studies had focused on the gas fraction of halos rather than the instantaneous mass that can accrete gas.
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The abstract, sentence by sentence
We develop and test with cosmological simulations a physically motivated theory for how the interplay between gravity, pressure, cooling, and self-shielding set the redshift--dependent mass scale at which halos can accrete intergalactic gas. This theory provides a physical explanation for the halo mass scale that can accrete unshocked intergalactic gas, which has been explained with ad hoc criteria tuned to reproduce the results of a few simulations. Furthermore, it provides an intuitive explanation for how this mass scale depends on the reionization redshift, the amplitude of the ionizing background, and the redshift. We show that accretion is inhibited onto more massive halos than had been thought because previous studies had focused on the gas fraction of halos rather than the instantaneous mass that can accrete gas. A halo as massive as 10^11 Msun cannot accrete intergalactic gas at z=0, even though typically its progenitors were able to accrete gas at higher redshifts. We describe a simple algorithm that can be implemented in semi-analytic models, and we compare the predictions of this algorithm to numerical simulations.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We develop and test with cosmological simulations a physically motivated theory for how the interplay between gravity, pressure, cooling, and self-shielding set the redshift--dependent mass scale at which halos can accrete intergalactic gas. | contribution 0.93 | 0.96 | 0.16 | asserted 0.99 |
| s1 | This theory provides a physical explanation for the halo mass scale that can accrete unshocked intergalactic gas, which has been explained with ad hoc criteria tuned to reproduce the results of a few simulations. | contribution 0.70 | 0.70 | 0.20 | asserted 1.00 |
| s2 | Furthermore, it provides an intuitive explanation for how this mass scale depends on the reionization redshift, the amplitude of the ionizing background, and the redshift. | interpretation 0.55 | 0.88 | 0.12 | asserted 1.00 |
| s3 | We show that accretion is inhibited onto more massive halos than had been thought because previous studies had focused on the gas fraction of halos rather than the instantaneous mass that can accrete gas. | result 0.87 | 0.85 | 0.32 | asserted 1.00 |
| s4 | A halo as massive as 10^11 Msun cannot accrete intergalactic gas at z=0, even though typically its progenitors were able to accrete gas at higher redshifts. | result 1.00 | 0.85 | 0.32 | asserted 1.00 |
| s5 | We describe a simple algorithm that can be implemented in semi-analytic models, and we compare the predictions of this algorithm to numerical simulations. | method 0.52 | 0.95 | 0.05 | asserted 0.93 |
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The paper
Original abstract
We develop and test with cosmological simulations a physically motivated theory for how the interplay between gravity, pressure, cooling, and self-shielding set the redshift--dependent mass scale at which halos can accrete intergalactic gas. This theory provides a physical explanation for the halo mass scale that can accrete unshocked intergalactic gas, which has been explained with ad hoc criteria tuned to reproduce the results of a few simulations. Furthermore, it provides an intuitive explanation for how this mass scale depends on the reionization redshift, the amplitude of the ionizing background, and the redshift. We show that accretion is inhibited onto more massive halos than had been thought because previous studies had focused on the gas fraction of halos rather than the instantaneous mass that can accrete gas. A halo as massive as 10^11 Msun cannot accrete intergalactic gas at z=0, even though typically its progenitors were able to accrete gas at higher redshifts. We describe a simple algorithm that can be implemented in semi-analytic models, and we compare the predictions of this algorithm to numerical simulations.
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References
How the literature uses it
13 arXiv papers cite this in 15 sentences
Papers citing it · 14 sentences without a confident label
Compares with it 1 paper
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The increase with halo mass is in agreement with the recent work of [ref] .
Galaxy properties and the cosmic web in simulations · Results · 0.83
What it cites · 1 sentence without a confident label
Uses data or values from 1 paper
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At $2<z<5$, observations find $Γ_-12=1$ [ref] , with smaller values estimated at lower and higher redshifts [ref] .
New Measurements of the Ionizing Ultraviolet Background over 2 < z < 5 and Implications for Hydrogen Reionization · the equilibrium temperature where atomic cooling balances photoheating · 0.88
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