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Interpreting ALMA Observations of the ISM During the Epoch of Reionisation

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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Harley Katz, Taysun Kimm, Debora Sijacki, Martin Haehnelt

Astrophysics of Galaxies · Submitted 6 Dec 2016

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim If smaller pockets of high metallicity gas exist in the ISM, the emission from these ions may be observable by ALMA while the low metallicity of the galaxy may cause these systems to fall below the local [CII]-SFR relation.

how it is stated · hedged possibility 0.98 read the record →

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arXiv ID1612.01786 (version 2)
Pith IDUEDZVVKJ, Pith's permanent record of this paper and its review
CitationDebora Sijacki, Harley Katz, Martin Haehnelt, Taysun Kimm. "Interpreting ALMA Observations of the ISM During the Epoch of Reionisation." arXiv:1612.01786 (2016). https://pith.science/paper/UEDZVVKJ
Claim paper

The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,209 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.70 · human participants 0.01 · controlled comparison 0.84 · randomized assignment 0.01 · states quantitative result 0.77 · compares with prior results 0.73 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

We present cosmological, radiation-hydrodynamics simulations of galaxy formation during the epoch of reionization in an effort towards modelling the interstellar medium (ISM) and interpreting ALMA observations. Simulations with and without stellar radiation are compared at large (Mpc), intermediate (tens of kpc), and small (sub kpc) scales. At large scales, the dense regions around galaxies reionize first before UV photons penetrate the voids; however, considerable amounts of neutral gas remain present within the haloes. The spatial distribution of neutral gas is highly dynamic and is anti-correlated with the presence of stars older than a few Myrs. For our specific feedback implementation, most of the metals remain inside the virial radii of haloes and they are proportionally distributed over the ionized and neutral medium by mass. For our most massive galaxy with ${\rm M_h}\sim10^{11}$M$_{\odot}$, the majority of the CII and OI mass are associated with cold neutral clumps. NII is more diffuse and arises in warmer gas while OIII arises in hotter gas with a higher ionization parameter, produced by photo-heating and supernovae. If smaller pockets of high metallicity gas exist in the ISM, the emission from these ions may be observable by ALMA while the low metallicity of the galaxy may cause these systems to fall below the local [CII]-SFR relation. The presence of dust can cause spatial offsets between UV/Ly$\alpha$ and [CII] emission as suggested by the recent observations of Maiolino et al. [OIII] may be spatially offset from both of these components since it arises from a different part of density-temperature phase-space.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 We present cosmological, radiation-hydrodynamics simulations of galaxy formation during the epoch of reionization in an effort towards modelling the interstellar medium (ISM) and interpreting ALMA observations. contribution 0.98 0.95 0.06 asserted 0.89
s1 Simulations with and without stellar radiation are compared at large (Mpc), intermediate (tens of kpc), and small (sub kpc) scales. method 0.96 0.89 0.03 asserted 0.88
s2 At large scales, the dense regions around galaxies reionize first before UV photons penetrate the voids; however, considerable amounts of neutral gas remain present within the haloes. result 1.00 0.88 0.12 asserted 1.00
s3 The spatial distribution of neutral gas is highly dynamic and is anti-correlated with the presence of stars older than a few Myrs. result 1.00 0.89 0.09 asserted 1.00
s4 For our specific feedback implementation, most of the metals remain inside the virial radii of haloes and they are proportionally distributed over the ionized and neutral medium by mass. result 0.99 0.92 0.08 asserted 1.00
s5 For our most massive galaxy with ${\rm M_h}\sim10^{11}$M$_{\odot}$, the majority of the CII and OI mass are associated with cold neutral clumps. result 1.00 0.93 0.10 asserted 1.00
s6 NII is more diffuse and arises in warmer gas while OIII arises in hotter gas with a higher ionization parameter, produced by photo-heating and supernovae. result 0.91 0.85 0.06 asserted 1.00
s7 If smaller pockets of high metallicity gas exist in the ISM, the emission from these ions may be observable by ALMA while the low metallicity of the galaxy may cause these systems to fall below the local [CII]-SFR relation. interpretation 0.99 0.45 0.16 hedged possibility 0.98
s8 The presence of dust can cause spatial offsets between UV/Ly$\alpha$ and [CII] emission as suggested by the recent observations of Maiolino et al. [OIII] may be spatially offset from both of these components since it arises from a different part of density-temperature phase-space. interpretation 0.89 0.19 0.07 hedged possibility 0.97

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

What was examined, and what was not

sources read
  • arXiv listing abstract v2
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

We present cosmological, radiation-hydrodynamics simulations of galaxy formation during the epoch of reionization in an effort towards modelling the interstellar medium (ISM) and interpreting ALMA observations. Simulations with and without stellar radiation are compared at large (Mpc), intermediate (tens of kpc), and small (sub kpc) scales. At large scales, the dense regions around galaxies reionize first before UV photons penetrate the voids; however, considerable amounts of neutral gas remain present within the haloes. The spatial distribution of neutral gas is highly dynamic and is anti-correlated with the presence of stars older than a few Myrs. For our specific feedback implementation, most of the metals remain inside the virial radii of haloes and they are proportionally distributed over the ionized and neutral medium by mass. For our most massive galaxy with ${\rm M_h}\sim10^{11}$M$_{\odot}$, the majority of the CII and OI mass are associated with cold neutral clumps. NII is more diffuse and arises in warmer gas while OIII arises in hotter gas with a higher ionization parameter, produced by photo-heating and supernovae. If smaller pockets of high metallicity gas exist in the ISM, the emission from these ions may be observable by ALMA while the low metallicity of the galaxy may cause these systems to fall below the local [CII]-SFR relation. The presence of dust can cause spatial offsets between UV/Ly$\alpha$ and [CII] emission as suggested by the recent observations of Maiolino et al. [OIII] may be spatially offset from both of these components since it arises from a different part of density-temperature phase-space.

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References
How later papers used it

79 later papers cite it

Evidence: substantial. 57 of the citing papers share no author with it, and 13 of those carry a confident label from Pith's citation classifier.

Pith read 16 of the 138 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

Builds on it 1 paper · 1 by the same authors

By the same authors

Uses its method or tool 7 of 27 papers with this label · 7 by the same authors

By the same authors

How the literature uses it

10 arXiv papers cite this in 11 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 6 sentences without a confident label

Uses its method or tool 2 papers
Compares with it 1 paper
Cites it as background 2 papers

What it cites · 6 sentences without a confident label

Contests 1 paper
  • The [ref] simulations, however, do not include on-the-fly radiative transfer (RT) and therefore do not properly model the enhancement of the local Lyman-Werner background above the mean metagalactic background, inside of the galaxy.

    Zooming on the internal structure of $z\simeq6$ galaxies · Introduction · contest 0.73

Uses data or values from 1 paper
  • Cosmological parameters reported by the Planck Collaboration are assumed ($h=0.6731$, $Ω_m=0.315$, $Ω_Λ=0.685$, $Ω_Λ=0.049$, $σ_8=0.829$, and $n_s=0.9655$, [ref] ).

    Planck 2015 results. XIII. Cosmological parameters · Initial Conditions · 0.99

Compares with 1 paper
  • [ref] (hereafter P16) performed a similar exercise using a zoom-in simulation and attempted to model the [CII] emission from a single high-redshift $z=6$ galaxy of similar mass to our work and [ref] .

    Zooming on the internal structure of $z\simeq6$ galaxies · Comparison with Previous Simulations · 0.83

Cites as background 5 papers

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