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arxiv: 2606.25969 · v1 · pith:2EVIXQNAnew · submitted 2026-06-24 · 🌌 astro-ph.CO

HI Simulations for Cosmology with the SKA Observatory

Tommaso Ronconi , Gabriella De Lucia , Marta Spinelli , Pascal Hitz , Fabio Fontanot , Francesco Sinigaglia , Lizhi Xie , Robert M. Yates
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Jos\'e Luis Bernal Anna Bonaldi Stefano Camera Isabella P. Carucci Steven Cunnington Francisco-Shu Kitaura Jo\"el Mayor Rajesh Mondal Giulia Piccirilli Digvijay Wadekar
This is my paper

Pith reviewed 2026-06-25 19:53 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords neutral hydrogenHI modelingsemi-analytical modelsempirical modelshalo mass relationpost-reionizationcosmologySKA surveys
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The pith

Semi-analytical and empirical models agree on cosmic HI density but differ systematically in the HI-halo mass relation and its redshift evolution.

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

The paper compares methods for modeling neutral hydrogen in the post-reionization Universe ahead of large radio surveys. Semi-analytical approaches evolve baryonic components inside dark matter merger trees according to physical prescriptions, while empirical schemes rely on fast approximations tuned to observables. The side-by-side assessment finds agreement on the total cosmic HI density yet systematic differences in the shape, scatter, and redshift evolution of the HI-halo mass relation. This distinction matters because accurate models are required both to interpret new HI measurements and to plan survey strategies. The work notes that semi-analytical models rest on chosen prescriptions while empirical ones trade some robustness for speed in unexplored parameter regions.

Core claim

By comparing the predictions from the different methods considered, we find overall consistency in integrated quantities such as Ω_HI, yet systematic differences in the detailed shape and scatter of the HI--halo mass relation and its redshift evolution. Semi-analytical models offer physically grounded predictions but depend on assumed prescriptions, while empirical methods provide flexibility and computational efficiency at the expense of robustness in extrapolated regions of the parameter space.

What carries the argument

The direct comparison of semi-analytical models that self-consistently evolve baryonic components within dark matter merger trees against empirical schemes based on fast approximations for large ensemble studies.

If this is right

  • New HI measurements will supply critical observational constraints to refine and calibrate current simulation methodologies.
  • Increasingly realistic HI simulations will help interpret data and guide survey design and analysis strategies.
  • Integrated quantities such as the cosmic HI density remain robust across modeling approaches.
  • The detailed HI-halo mass relation and its evolution require further calibration because different methods produce systematic variations in shape and scatter.

Where Pith is reading between the lines

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

  • If future data favor one class of models over the other in the scatter at fixed halo mass, that could guide which approach to prioritize for volume-limited forecasts.
  • Empirical models might be adjusted using semi-analytical outputs in well-constrained regimes to combine speed with physical insight for very large mock catalogs.
  • Differences in redshift evolution could alter predictions for how HI traces the growth of cosmic structure at higher redshifts.

Load-bearing premise

The collection of semi-analytical and empirical models examined is representative enough of plausible physical assumptions to support general statements about differences between the two classes.

What would settle it

New HI observations that either remove the reported systematic differences in the HI-halo mass relation across redshifts or produce substantially larger discrepancies than those identified in the comparison.

Figures

Figures reproduced from arXiv: 2606.25969 by Anna Bonaldi, Digvijay Wadekar, Fabio Fontanot, Francesco Sinigaglia, Francisco-Shu Kitaura, Gabriella De Lucia, Giulia Piccirilli, Isabella P. Carucci, Jo\"el Mayor, Jos\'e Luis Bernal, Lizhi Xie, Marta Spinelli, Pascal Hitz, Rajesh Mondal, Robert M. Yates, Stefano Camera, Steven Cunnington, Tommaso Ronconi.

Figure 1
Figure 1. Figure 1: Measurements of ΩHI at different redshifts from 3 methods out of the 4 listed in the Chapter. For comparison, we also mark the empirical relation found in Crighton et al. (2015) that represents a fit to observational data. slice considered and is thus not present for sam1 and sam2 whose boxes are associated to discrete redshift values. The ΩHI-dimension error was computed by bootstrap resampling both the b… view at source ↗
Figure 2
Figure 2. Figure 2: HI mass functions at redshift 𝑧 = 0 (left panel) and 𝑧 = 0.5 (right panel). Measurements from sam1 (green diamonds), sam2 (light-blue plus symbols), emp1.1 (lavender triangles) and emp1.2 (empty golden squares) are shown along with analytical models fitted to data. The models shown in the upper left panel represent fit to different survey data: HIPASS (bronze dashed-dotted line, Zwaan et al., 2005), ALFALF… view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the Hi –halo mass (HIHM) relation at 𝑧 = 0.25 obtained from all the models considered in this work. The upper panels and lower left panel show the percent abundance of haloes in the (𝑀halo, 𝑀HI) plane for sam2 (upper left), emp1 (upper right) and emp3 (lower left). Blue shaded regions indicate the density of simulated haloes, while empty black squares with error bars mark the mean and standar… view at source ↗
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p019_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Marked power spectrum measured on the redshift 𝑧 = 1 boxes of sam1 (green diamonds connected by a green solid line), emp2 (blue downward triangles connected by blue solid line) and emp3 (orange crosses connected by the orange solid line). As a term of comparison, we over-plot as a black dashed line, the linear power spectrum of matter evolved linearly up to the same redshift of the simulations. this, galax… view at source ↗
read the original abstract

We present a comparative overview of state-of-the-art methods for modelling the distribution of neutral hydrogen (HI) in the post-reionization Universe, developed in preparation for upcoming SKAO cosmological surveys. Our aim is to assess how different physical and empirical assumptions reflect into predictions for key observables such as the cosmic HI density, the HI mass function, and the HI-halo mass relation. We consider both: (i) semi-analytical approaches that self-consistently evolve baryonic components within dark matter merger trees through physically motivated prescriptions and (ii) empirical schemes tailored to different observables and based on fast approximations designed for large ensemble studies. By comparing the predictions from the different methods considered, we find overall consistency in integrated quantities such as $\Omega_{\mathrm{HI}}$, yet systematic differences in the detailed shape and scatter of the HI--halo mass relation and its redshift evolution. Semi-analytical models offer physically grounded predictions but depend on assumed prescriptions, while empirical methods provide flexibility and computational efficiency at the expense of robustness in extrapolated regions of the parameter space. The increasing number of HI measurements from SKA precursors and pathfinders (including surveys with MeerKAT, ASKAP, and FAST) will provide critical observational constraints to refine and calibrate current simulation methodologies. In turn, increasingly realistic HI simulations play a key role in interpreting these data, guiding survey design and analysis strategies, in preparation for the advent of SKAO data.

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.

Referee Report

1 major / 2 minor

Summary. The manuscript provides a comparative overview of semi-analytical and empirical methods for modeling neutral hydrogen (HI) distribution in the post-reionization Universe in preparation for SKAO surveys. It assesses how different physical and empirical assumptions affect predictions for key observables including the cosmic HI density Ω_HI, the HI mass function, and the HI-halo mass relation. The central finding is overall consistency across methods in integrated quantities such as Ω_HI, accompanied by systematic differences in the detailed shape, scatter, and redshift evolution of the HI-halo mass relation.

Significance. If the reported class-level differences hold after addressing model selection, the work would help quantify modeling uncertainties relevant to interpreting SKA precursor data from MeerKAT, ASKAP, and FAST and to guiding SKAO survey design. The explicit contrast between physically motivated but prescription-dependent semi-analytical models and computationally efficient but less robust empirical schemes identifies where future observations can provide calibration.

major comments (1)
  1. [Model selection and comparison sections] The headline claim of systematic differences between the semi-analytical and empirical classes (abstract and concluding discussion) is load-bearing for the paper's utility, yet rests on the untested assumption that the finite set of examined models spans the dominant physical variations within each class. The manuscript does not demonstrate coverage of key variants such as alternative feedback implementations or HI assignment schemes, leaving open the possibility that reported differences are model-specific rather than class-wide.
minor comments (2)
  1. The abstract would be strengthened by stating the exact number of models in each category and the redshift range over which the comparisons are performed.
  2. Figure captions comparing the HI-halo mass relation should explicitly label which curves correspond to semi-analytical versus empirical approaches and note any shared parameter choices.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the constructive report and the recommendation for major revision. We address the major comment point by point below, proposing targeted revisions to clarify the scope of our model comparison while preserving the paper's core findings on consistency in integrated quantities and differences in the HI-halo mass relation.

read point-by-point responses

  1. Referee: [Model selection and comparison sections] The headline claim of systematic differences between the semi-analytical and empirical classes (abstract and concluding discussion) is load-bearing for the paper's utility, yet rests on the untested assumption that the finite set of examined models spans the dominant physical variations within each class. The manuscript does not demonstrate coverage of key variants such as alternative feedback implementations or HI assignment schemes, leaving open the possibility that reported differences are model-specific rather than class-wide.

    Authors: We agree that the manuscript should more explicitly address the rationale and limitations of model selection. The models examined are the primary state-of-the-art examples used in the SKAO preparation literature, chosen because they represent the dominant semi-analytical frameworks (varying in merger-tree evolution and baryonic prescriptions) and empirical schemes (differing in observable-based HI assignments) available at the time of writing. Nevertheless, we acknowledge that the comparison does not exhaustively sample all possible variants. In revision, we will add a dedicated paragraph to the model selection section discussing the criteria for inclusion, noting unexamined alternatives such as different AGN feedback implementations or alternative HI partitioning schemes, and qualifying that the reported class-level trends are based on the models considered. We will also revise the abstract and concluding discussion to state that systematic differences are observed among the examined models, while the consistency in Ω_HI holds across them. These changes will be made without expanding the model set, as the work is a comparative overview rather than a comprehensive parameter survey. revision: yes

Circularity Check

0 steps flagged

No circularity: inter-model comparison without derivation chain

full rationale

The paper is a comparative overview of existing semi-analytical and empirical HI modeling methods, reporting consistency in integrated quantities like Ω_HI and differences in the HI-halo mass relation shape and evolution. No new derivation, prediction, or first-principles result is claimed that reduces by construction to fitted inputs, self-citations, or ansatzes defined inside the paper. The central claims rest on direct inter-model comparisons rather than any load-bearing step that equates output to input. This is self-contained against external benchmarks and matches the expected honest non-finding for such survey-style work.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The paper is an overview; it does not introduce new free parameters, axioms, or invented entities beyond those already present in the referenced semi-analytical and empirical HI models.

pith-pipeline@v0.9.1-grok · 5855 in / 964 out tokens · 14878 ms · 2026-06-25T19:53:59.389061+00:00 · methodology

discussion (0)

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Reference graph

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