arxiv: 2605.01505 · v1 · submitted 2026-05-02 · 🌌 astro-ph.GA

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Non-Equilibrium Ionisation in Photoionised Haloes: Implications for Shock Stability and Absorption-Line Signatures

Itai Bromberg , Kartick C. Sarkar , Orly Gnat , Yuval Birnboim

Authors on Pith no claims yet

Pith reviewed 2026-05-09 18:02 UTC · model grok-4.3

classification 🌌 astro-ph.GA

keywords nonequilibrium ionizationphotoionizationvirial shocksgalaxy halosabsorption linesOVICIVIGM

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The pith

UV background pre-ionizes the IGM, suppressing nonequilibrium ionization and restoring the collisional ionization equilibrium threshold for stable virial shocks in galaxy halos.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper examines how the metagalactic UV background alters gas behavior in galaxy halos through 1D hydrodynamical simulations that track time-dependent ionization of multiple elements. Without the UV field, nonequilibrium ionization speeds up post-shock cooling, which lowers pressure support and increases the halo mass needed for stable shocks to form. Including the UV background pre-ionizes incoming gas, which reduces these nonequilibrium effects and brings shock stability back in line with equilibrium expectations. The same pre-ionization also produces extended columns of ions such as OVI, CIV, and HI that stretch well beyond the virial radius and reach observed values with only weak dependence on halo mass.

Core claim

The central claim is that the metagalactic UV background pre-ionises the intergalactic medium surrounding galaxies, thereby suppressing nonequilibrium ionisation. This restores the minimum halo mass for stable virial shock formation to the value given by collisional ionisation equilibrium calculations. The photoionised gas further generates substantial column densities of OVI, CIV, and HI that extend beyond Rvir, with OVI values comparable to those seen in observations, while showing weak halo-mass dependence and reaching out to ~10 Rvir for CIV and HI at z greater than or equal to 3.

What carries the argument

One-dimensional spherically symmetric hydrodynamical simulations that follow dark-matter growth, gas dynamics, and time-dependent ionisation and cooling for H, He, C, N, O, Ne, Mg, Si, S, and Fe in the presence of a metagalactic UV background.

If this is right

Without a UV background, nonequilibrium ionization enhances post-shock cooling and raises the minimum mass required for stable virial shocks.
With the UV background present, ionization states remain close to equilibrium except inside transient rapidly cooling zones.
Photoionized intergalactic gas can produce OVI column densities comparable to observed values at radii larger than the virial radius.
Halos at redshift greater than or equal to 3 generate CIV columns of 10^13-15 cm^-2 and HI columns of 10^15-17 cm^-2 out to approximately 10 virial radii.
The absorption signatures exhibit only weak dependence on halo mass across the 10^11-10^13 solar mass range.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

Observers interpreting circumgalactic medium absorption must subtract a significant intergalactic medium contribution at large radii.
Three-dimensional simulations that include realistic local radiation sources would test whether the weak mass dependence survives in more complex geometries.
Measuring ionization ratios at fixed radii in halos spanning a wide mass range could directly confirm or refute the predicted suppression of nonequilibrium effects.

Load-bearing premise

The one-dimensional spherically symmetric simulations together with the chosen metagalactic UV background model correctly capture the ionization states, thermal evolution, and absorption properties that occur in real three-dimensional galaxy halos.

What would settle it

Comparison of the simulated OVI and CIV column-density profiles versus projected radius against observed quasar absorption spectra around galaxies with measured halo masses and redshifts.

Figures

Figures reproduced from arXiv: 2605.01505 by Itai Bromberg, Kartick C. Sarkar, Orly Gnat, Yuval Birnboim.

**Figure 1.** Figure 1: Evolution of gas shells in haloes of different masses and physical scenarios. Each row shows a different physical model (’Eq’,’nEq’,’Eq+UV’,’nEq+UV’, from top to bottom). Each column is for a different final halo mass (1011 , 3 × 1011, 1012 , 3 × 1012 , 1013 M⊙ from left to right). Each panel shows the trajectories of Lagrangian gas shells in radius–redshift space, colour-coded by gas temperature. The whit… view at source ↗

**Figure 2.** Figure 2: Right: r − z trajectory of a gas shell (no. 441) in a 3 × 1011 M⊙ nEq+UV halo. Left and middle: Oxygen ion fractions vs. redshift for the same shell (left panel focuses on late times). Gray curves show T4 ≡ T /(104 K); coloured curves show ion fractions. Solid lines: hydra ; dashed: PIE at Teq; squares: PIE at Thydra . 10 2 10 1 10 0 10 10 1 0 10 1 10 2 10 3 Eq Radius [kpc] Mh(z = 0) = 1e11M 10 2 10 1 10 0… view at source ↗

**Figure 3.** Figure 3: Same as view at source ↗

**Figure 4.** Figure 4: O vi columns. Top row: O vi columns at z = 0.2 as a function of scaled impact parameter, b/Rvir, for different halo masses (panels). Curves show the models: Eq (blue), Eq+UV (orange), nEq (green), nEq+UV (solid red), the CGM-only contribution (r < rs) to the nEq+UV case (dash–dotted red), and the toy model of B+25 (gray). Markers show observational detections (filled circles) and upper limits (empty triang… view at source ↗

**Figure 5.** Figure 5: NH I (top) and NC IV (bottom) columns for the nEq+UV model across the full r − z parameter space. Colour indicates the column density for each redshift–sightline (impact parameter) combination (see colourbar). 0.1 0.3 0.5 0.7 b [physical kpc] 10 14 10 15 N O VI [c m 2 ] M=3e11 0.1 0.3 0.5 0.7 1 b [physical kpc] M=1e12 Eq+UV Eq+UV CGM Only nEq+UV nEq+UV CGM Only view at source ↗

**Figure 6.** Figure 6: NO VI versus impact parameter, as in view at source ↗

read the original abstract

We investigate the impact of nonequilibrium ionisation (NEI) and the metagalactic radiation-field on the thermal evolution, virial shock stability, and absorption signatures of gas surrounding galaxies. Using 1D, spherically symmetric hydrodynamical simulations with an extended version of the hydra code, we follow dark-matter growth, gas dynamics, time-dependent ionisation and cooling in the presence of the UV background. We explicitly track all ions of H, He, C, N, O, Ne, Mg, Si, S, and Fe in haloes of mass 1e11-1e13Msun from z=100 to z=0. Without a UV background, NEI enhances post-shock cooling due to underionised gas, reducing pressure support and raising the minimum mass for stable shock formation. Including the UV background pre-ionises the IGM, suppressing NEI, and restoring the CIE threshold. The IGM temperatures deviate from thermal equilibrium due to adiabatic expansion and collapse, while ionisation remains close to equilibrium in the presence of a UV background, except in transient rapidly cooling regions where NEI occurs. We compute absorption columns of OVI, CIV, and HI, showing that a photoionised IGM may produce substantial warm-ion columns extending beyond Rvir, including OVI column densities comparable to observed values. Our models indicate weak halo-mass dependence and extended distributions. We also find that z>~3 haloes can produce CIV (NCIV~1e13-15cm^-2) and HI (NHI~1e15-17cm^-2) columns out to ~10Rvir. Our results highlight the role of the UV background in regulating the thermal state and observable signatures of the gas surrounding galaxies, and emphasize the importance of accounting for IGM contributions when interpreting CGM absorption-line observations.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

The UV background largely kills the NEI cooling boost in these 1D runs and lets outer halo gas produce plausible OVI columns, but spherical symmetry is the main limit on the absorption predictions.

read the letter

The main thing to know is that adding the metagalactic UV background pre-ionizes the IGM enough to suppress the non-equilibrium ionization that would otherwise enhance post-shock cooling, which restores the usual CIE threshold for stable virial shocks and allows the models to produce OVI, CIV, and HI columns that extend well beyond Rvir and reach observed levels for some ions. They track the full set of ions from H through Fe in time-dependent fashion across 10^11 to 10^13 solar mass halos from z=100 to z=0, and the absorption calculations are a direct output of the radial profiles. That combination is the concrete advance over earlier work that either skipped the UV or used simpler ionization treatments. The with-versus-without UV comparison is clean and shows the IGM contribution can matter for CGM sightlines, especially at higher redshift where they get CIV and HI columns out to 10 Rvir. The weak mass dependence they report is also a useful result if it holds up. The obvious soft spot is the 1D spherical symmetry. Real halos have filaments, mergers, and non-radial shocks that can sustain under-ionized gas even with a UV field, and absorption columns measured along random sightlines will sample different density and path-length distributions than a radial average. The abstract gives no quantitative error bars, resolution tests, or direct comparisons to prior NEI or CIE runs, so the strength of the column numbers is difficult to judge without the full text. If the paper includes checks against known equilibrium cases or against other codes, that would tighten things. This is for people who model or observe the CGM and need to know how ionization state affects both thermal stability and line strengths. It is worth sending to peer review because the ion network and the UV effect on the shock threshold are specific enough to be worth referee time, even if the 1D geometry will require caveats or follow-up 3D work.

Referee Report

2 major / 2 minor

Summary. The manuscript investigates the effects of nonequilibrium ionisation (NEI) and the metagalactic UV background on the thermal evolution, virial shock stability, and absorption-line signatures in galaxy haloes using 1D spherically symmetric hydrodynamical simulations with an extended Hydra code. The simulations track the evolution of multiple ions in haloes ranging from 10^11 to 10^13 solar masses from redshift 100 to 0. Key findings include that the UV background pre-ionises the IGM, suppresses NEI, restores the collisional ionisation equilibrium (CIE) threshold for shock stability, and that photoionised gas can produce substantial columns of OVI, CIV, and HI extending beyond the virial radius, with values comparable to observations and weak dependence on halo mass.

Significance. If the results hold, this work highlights the importance of the UV background in regulating the ionization state and thermal properties of the circumgalactic and intergalactic medium, with direct implications for interpreting absorption-line observations. The direct numerical tracking of time-dependent ionization states for H, He, C, N, O, Ne, Mg, Si, S, and Fe across a broad redshift range, using an external UV background input, provides a self-consistent treatment of cooling and ionization that strengthens the analysis of shock stability and extended absorption signatures.

major comments (2)

[Simulation methodology and absorption column calculations] The central claims regarding suppression of NEI by the UV background, restoration of the CIE shock threshold, and substantial OVI/CIV/HI absorption columns extending beyond Rvir (including NCIV ~ 10^13-15 cm^-2 and NHI ~ 10^15-17 cm^-2 at z>~3) are derived from 1D spherically symmetric radial profiles. In 3D, filamentary accretion, mergers, and non-radial shocks can sustain under-ionised pockets or alter cooling paths even with UV pre-ionisation, which may change the reported weak halo-mass dependence and IGM contributions to observed columns. This assumption is load-bearing for the absorption signatures and needs explicit discussion or sensitivity tests.
[Results on thermal evolution and absorption signatures] The abstract and results describe qualitative outcomes for ionisation states and column densities but provide limited quantitative validation, such as convergence tests with respect to spatial resolution, time-stepping, or direct comparisons of NEI vs. CIE column density profiles. Without these, the extent of NEI suppression and the comparability of OVI columns to observations cannot be fully assessed.

minor comments (2)

[Methods] The specific metagalactic UV background model (including its spectral shape and redshift evolution) should be stated more explicitly, along with any assumptions about its uniformity.
[Results] Notation for column densities (e.g., NCIV) is introduced without a dedicated table or figure summarizing the full set of computed values across halo masses and redshifts.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough and constructive review of our manuscript. We have carefully considered each major comment and provide point-by-point responses below, indicating the revisions we will implement.

read point-by-point responses

Referee: [Simulation methodology and absorption column calculations] The central claims regarding suppression of NEI by the UV background, restoration of the CIE shock threshold, and substantial OVI/CIV/HI absorption columns extending beyond Rvir (including NCIV ~ 10^13-15 cm^-2 and NHI ~ 10^15-17 cm^-2 at z>~3) are derived from 1D spherically symmetric radial profiles. In 3D, filamentary accretion, mergers, and non-radial shocks can sustain under-ionised pockets or alter cooling paths even with UV pre-ionisation, which may change the reported weak halo-mass dependence and IGM contributions to observed columns. This assumption is load-bearing for the absorption signatures and needs explicit discussion or sensitivity tests.

Authors: We agree that the assumption of 1D spherical symmetry represents a significant simplification, and that 3D effects including filamentary accretion, mergers, and non-radial shocks could in principle sustain under-ionised pockets or modify cooling pathways even in the presence of UV pre-ionisation. Our 1D setup is intended to isolate the radial structure and the specific role of the metagalactic UV background in suppressing NEI and restoring the CIE shock threshold. The reported weak halo-mass dependence follows from the photoionised IGM dominating the column densities at large radii. We will add a dedicated subsection in the discussion that explicitly addresses the limitations of the 1D approximation, outlines how 3D effects might alter the results, and emphasises that the extended IGM contribution remains a robust qualitative feature. We will also conduct additional sensitivity tests by introducing small radial perturbations and varying the outer boundary conditions to assess robustness of the column-density profiles. Full 3D simulations with time-dependent NEI are beyond the scope of the present study. revision: partial
Referee: [Results on thermal evolution and absorption signatures] The abstract and results describe qualitative outcomes for ionisation states and column densities but provide limited quantitative validation, such as convergence tests with respect to spatial resolution, time-stepping, or direct comparisons of NEI vs. CIE column density profiles. Without these, the extent of NEI suppression and the comparability of OVI columns to observations cannot be fully assessed.

Authors: We acknowledge that the manuscript would benefit from more explicit quantitative validation. Although the base Hydra code has been subjected to resolution and time-stepping tests in prior publications, we agree that dedicated convergence checks for the extended NEI module and direct NEI-versus-CIE comparisons are required. We will add a new appendix presenting resolution and time-step convergence tests for the ionisation and cooling routines, together with side-by-side radial profiles and integrated column densities of OVI, CIV, and HI computed under both NEI and CIE assumptions. These additions will quantify the degree of NEI suppression by the UV background and strengthen the comparison with observed column densities. revision: yes

Circularity Check

0 steps flagged

No significant circularity; results from direct 1D simulations with external UV input

full rationale

The paper's central claims derive from explicit 1D spherically symmetric hydrodynamical integrations using an extended Hydra code that tracks time-dependent ionization states for H, He, C, N, O, Ne, Mg, Si, S, and Fe across halo masses 10^11-10^13 Msun from z=100 to z=0. The UV background is an external metagalactic input that pre-ionizes the IGM; NEI suppression, restoration of the CIE virial-shock threshold, and the computed OVI/CIV/HI column densities (including their weak mass dependence and extension beyond Rvir) are direct numerical outputs, not reductions of fitted parameters or self-referential definitions. No load-bearing self-citations, ansatzes smuggled via prior work, or uniqueness theorems imported from the same authors appear in the provided text that would force the conclusions by construction. The derivation chain remains independent of the target observables.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Claims rest on standard hydrodynamics and atomic physics assumptions plus the external UV background; no new entities are introduced.

free parameters (2)

halo mass range = 1e11-1e13 Msun
Simulations limited to 1e11-1e13 Msun haloes
redshift evolution range = z=100 to z=0
Full track from z=100 to z=0

axioms (2)

domain assumption 1D spherically symmetric hydrodynamics accurately represents halo gas dynamics
Used to follow dark-matter growth and gas dynamics
standard math Standard atomic ionization and cooling rates for tracked elements
Explicit tracking of H, He, C, N, O, Ne, Mg, Si, S, Fe ions

pith-pipeline@v0.9.0 · 5663 in / 1602 out tokens · 73526 ms · 2026-05-09T18:02:37.570347+00:00 · methodology

discussion (0)

Reference graph

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