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arxiv: 2605.04925 · v1 · submitted 2026-05-06 · 🌌 astro-ph.GA

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Near-infrared diagnostic diagrams of the gas ionization sources in nearby galaxies: a JWST NIRSpec view

J. H. Costa-Souza , Luis Colina , Rogemar A. Riffel , Santiago Arribas , Michele Perna , Miguel Pereira Santaella , Ismael Garc\'ia-Bernete , Montserrat Villar Mart\'in
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Oli L. Dors
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Pith reviewed 2026-05-08 16:38 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords near-infrared diagnosticsgas excitation mechanismsultraluminous infrared galaxiesJWST NIRSpec spectroscopyemission line ratiosactive galactic nucleistar formationshock excitation
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The pith

Two near-infrared line ratios distinguish star formation, AGN, and shocks as gas excitation sources

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

The paper analyzes high-resolution JWST NIRSpec spectra from the central regions of nine nearby ultraluminous infrared galaxies to search for new ways to identify what excites the emitting gas. Optical diagnostic methods often cannot reach through dust to buried active nuclei or young star clusters, so the work tests near-infrared features that might track the energy of the radiation field more reliably. The authors identify two specific ratios that separate regions dominated by young stars, accreting black holes, or shocks, and they confirm these match existing near-infrared classifications while also linking broader emission lines to shock activity. If reliable, the diagrams would let observers map excitation mechanisms in dusty galaxy centers where previous tools fail.

Core claim

We propose two line-excitation diagnostic diagrams based on [C I]/Paγ and H2 1-0 O(5)/PAH 3.3 μm ratios. These ratios correlate directly with the hardness of the radiation field and therefore indicate whether the gas is excited by star formation, active galactic nuclei, or shocks. The analysis of nine local U/LIRGs shows that the new diagrams reproduce the classifications from established near-infrared methods and that shock-excited regions have distinctly broader line profiles.

What carries the argument

Two new diagnostic diagrams using the [C I]/Paγ and H2 1-0 O(5)/PAH 3.3μm line ratios that separate gas regions according to radiation field hardness

If this is right

  • The diagrams allow classification of gas excitation in dust-obscured regions where optical lines are blocked.
  • Line width at 80 percent of total flux can help flag shock-dominated zones in galaxy nuclei.
  • Hydrogen molecule emission in active galactic nucleus hosts is produced by multiple processes at once.
  • The tools support refined models of energy input in the central regions of dusty starburst and AGN systems.

Where Pith is reading between the lines

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

  • The ratios could be tested on higher-redshift galaxies to track how excitation sources change over cosmic time.
  • Checking the diagrams across galaxies with different metal abundances would reveal whether chemical composition affects the separations.
  • Combining the near-infrared ratios with multi-wavelength data might clarify how several heating processes operate together.

Load-bearing premise

The correlations between the proposed line ratios and excitation mechanisms seen in this sample of nine local ultraluminous infrared galaxies will hold in other galaxies and will not be strongly changed by differences in metal content, gas density, or viewing geometry.

What would settle it

Apply the same two line ratios to a larger sample of galaxies whose excitation mechanisms are already classified independently from optical or X-ray observations and check whether the separations still match the expected star-formation, AGN, and shock groups.

Figures

Figures reproduced from arXiv: 2605.04925 by Ismael Garc\'ia-Bernete, J. H. Costa-Souza, Luis Colina, Michele Perna, Miguel Pereira Santaella, Montserrat Villar Mart\'in, Oli L. Dors, Rogemar A. Riffel, Santiago Arribas.

Figure 1
Figure 1. Figure 1: NIR diagnostic diagram based on flux measurements from inte￾grated spectra of all galaxies, using multiple circular apertures. The dif￾ferent galaxies are shown in distinct colors, as indicated in the bottom￾right corner of the plot. The black lines indicate the empirical bound￾aries from Riffel et al. (2013). confirmed nuclei, while shocks dominate the surroundings of the nuclear regions, in agreement wit… view at source ↗
Figure 2
Figure 2. Figure 2: Line-ratio distributions, separated by the different regions of the NIR diagnostic diagram. The color-coding is defined according to the regions defined in the H2 1–0 S(1)/Brγ versus [Fe ii] 1.257 µm/Paβ diagnostic diagram ( view at source ↗
Figure 3
Figure 3. Figure 3: W80 distributions for the whole sample. The color coding is the same as in view at source ↗
Figure 4
Figure 4. Figure 4: Near-infrared diagnostic diagrams. Left panel show the diagrams [Fe ii]/Paβ versus H2/Brγ from Riffel et al. (2013); central panel displays the [C i]/Paγ versus H2/Brγ; at last the right panel show the H2 1-0 O(5)/PAH 3.3 µm versus H2/Brγ. The color of the markers indicates the different excitation mechanism based on the left panel: blueish for regions consistent with SF excitation; red, for AGN-excited re… view at source ↗
Figure 5
Figure 5. Figure 5: H2 temperature diagram, the bottom x axis shows the ratio H2 2-1 S(1)/H2 1-0 S(1), and the corresponding vibrational temperature, at the upper axis; The left y axis shows H2 1-0 S(2)/H2 1-0 S(0), whilst the right axis shows the rotational temperature. The measured mean line ratios are represented by pentagons of different colors according to the excitation mechanism: starburst (blue), AGN (red), and shocks… view at source ↗
read the original abstract

Buried active galactic nuclei and obscured young stellar clusters pose significant challenges to traditional optical diagnostic diagrams. Therefore, developing new tools to trace the excitation sources across the spectrum is a necessary effort for the advancement of the field. Our goal is to explore the full spectral range of the JWST-NIRSpec data, searching for alternative diagnostic diagrams in the less-explored NIR, and to investigate the nature of the ionizing and heating source. We analyze the high-resolution spectra of the circum-nuclear regions of nine local (z < 0.1) U/LIRGS, investigating potential emission-line ratios to trace the excitation mechanisms acting on the line-emitting gas. We investigate these objects using the well-established [Fe ii]/PaB versus H2/Bry diagram, and attempt to correlate its classifications with other emission features across the spectrum. We then compare the empirical classifications with photo-ionization models, in order to evaluate how accurately the data can be reproduced. Finally, we compare the line width at 80% of the total flux (W80 ) of selected emission lines with the corresponding gas excitation mechanisms. We propose two line-excitation diagnostic diagrams based on [C i]/Pay and H2 1-0 O(5)/PAH 3.3 um ratio, which we found to directly correlate with the hardness of the radiation field, and therefore with the gas excitation mechanisms. In addition, the line-kinematics analysis shows that the W80 values of regions excited by star formation are on average slightly lower than those of AGN-excited regions, while shock-excited regions display distinctively higher W80 values compared to the other two groups. Our JWST-NIRSpec results reinforce previous studies showing that the H2 emission in the central regions of AGN hosts is complex and likely produced by multiple excitation mechanisms.

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

3 major / 3 minor

Summary. The manuscript analyzes high-resolution JWST-NIRSpec spectra of circum-nuclear regions in nine local (z < 0.1) U/LIRGs. It builds on the established [Fe II]/Paβ versus H₂/Brγ diagram to explore NIR emission-line ratios for diagnosing gas excitation mechanisms (star formation, AGN, shocks). The authors compare empirical classifications to photo-ionization models, examine correlations with other spectral features, and analyze line kinematics via W80. The central claim is the proposal of two new diagnostic diagrams using the [C I]/Paγ and H₂ 1-0 O(5)/PAH 3.3 μm ratios, which are reported to correlate directly with radiation-field hardness and thereby distinguish excitation mechanisms. Kinematic results indicate lower average W80 for star-formation-excited regions and distinctly higher W80 for shock-excited regions.

Significance. If the reported correlations hold after broader testing, the proposed NIR diagnostics would provide practical tools for identifying buried AGNs and obscured star clusters in dusty systems where optical line-ratio diagrams are ineffective. The multi-wavelength approach combining line ratios, photo-ionization models, and kinematics (W80) adds supporting layers. The direct exploitation of JWST NIRSpec data and the explicit comparison to models are positive elements. However, the small sample size and absence of controls for confounding parameters limit the immediate impact and generalizability of the new diagrams.

major comments (3)
  1. [Sample and observations section] Sample and observations section: The central claim of two generalizable NIR diagnostic diagrams rests on empirical trends observed in spectra from only nine U/LIRGs. No details are given on sample selection criteria, the range of metallicities or densities spanned, or how the targets were chosen to minimize biases. Without this information it is impossible to determine whether the reported correlations with radiation hardness are driven by excitation mechanism or by untested covariances with other variables.
  2. [Model comparison section] Model comparison section: The manuscript compares the data to photo-ionization models but does not state whether the model grid independently varies metallicity, density, and geometry across the observed range. If these parameters are not decoupled, the isolation of radiation-field hardness as the primary driver of the [C I]/Paγ and H₂/PAH ratios cannot be demonstrated, undermining the proposed diagnostic utility.
  3. [Results and discussion] Results and discussion: No quantitative assessment of correlation strength (e.g., Spearman rank coefficients), uncertainties on the measured line ratios, or statistical significance tests is provided. The absence of error analysis and validation against independent datasets makes it difficult to evaluate whether the trends in the nine objects are robust enough to support new diagnostic diagrams.
minor comments (3)
  1. [Abstract and throughout] Notation for the proposed ratios should be standardized (e.g., consistent use of Paγ versus Pay) and all abbreviations (including W80) defined at first use.
  2. [Figures showing the new diagrams] The diagnostic diagrams would benefit from inclusion of error bars on the data points and overlaid model tracks to illustrate the claimed separation.
  3. [Introduction] A brief discussion of how the new NIR ratios relate to or improve upon existing NIR diagnostics in the literature would strengthen the introduction.

Simulated Author's Rebuttal

3 responses · 1 unresolved

We thank the referee for the constructive and detailed review. We address each major comment point by point below, providing clarifications and indicating where revisions will be made to strengthen the manuscript.

read point-by-point responses

  1. Referee: [Sample and observations section] Sample and observations section: The central claim of two generalizable NIR diagnostic diagrams rests on empirical trends observed in spectra from only nine U/LIRGs. No details are given on sample selection criteria, the range of metallicities or densities spanned, or how the targets were chosen to minimize biases. Without this information it is impossible to determine whether the reported correlations with radiation hardness are driven by excitation mechanism or by untested covariances with other variables.

    Authors: We acknowledge that the current Sample and observations section is concise and does not fully detail selection criteria or the spanned ranges of metallicity and density. The nine targets were drawn from the GOALS sample of local U/LIRGs with existing multi-wavelength coverage and suitable for high-resolution NIRSpec observations; we will expand this section to explicitly list the selection criteria, available ancillary data on metallicities (typically near-solar for these nuclei), and density estimates from the literature. We will also add a discussion of possible covariances and the empirical nature of the trends. However, the small sample size inherently limits the ability to fully decouple all variables, and we will emphasize this caveat more strongly. revision: yes

  2. Referee: [Model comparison section] Model comparison section: The manuscript compares the data to photo-ionization models but does not state whether the model grid independently varies metallicity, density, and geometry across the observed range. If these parameters are not decoupled, the isolation of radiation-field hardness as the primary driver of the [C I]/Paγ and H₂/PAH ratios cannot be demonstrated, undermining the proposed diagnostic utility.

    Authors: We agree that the model section requires clarification on parameter coverage. The photo-ionization grids used (from standard libraries such as those in Cloudy) do span ranges in metallicity, density, and ionization parameter, with geometry fixed to plane-parallel for the nuclear regions; we will revise the text to state the exact ranges explored and note which parameters were held fixed versus varied. This will better demonstrate that radiation-field hardness remains the dominant driver for the proposed ratios within the explored parameter space, while acknowledging that full decoupling is limited by the model assumptions. revision: yes

  3. Referee: [Results and discussion] Results and discussion: No quantitative assessment of correlation strength (e.g., Spearman rank coefficients), uncertainties on the measured line ratios, or statistical significance tests is provided. The absence of error analysis and validation against independent datasets makes it difficult to evaluate whether the trends in the nine objects are robust enough to support new diagnostic diagrams.

    Authors: We accept that the Results and discussion section lacks formal quantitative statistics. We will add Spearman rank correlation coefficients and associated p-values for the key relations involving [C I]/Paγ and H₂ 1-0 O(5)/PAH 3.3 μm, include error bars derived from the spectral fitting uncertainties, and report basic significance tests. We will also note the absence of an independent validation sample and the consequent need for future work. These additions will allow readers to better assess the robustness of the trends. revision: yes

standing simulated objections not resolved
  • The small sample of only nine U/LIRGs inherently limits statistical power, full control for confounding variables, and immediate generalizability of the proposed diagnostics, which cannot be remedied by revision alone.

Circularity Check

0 steps flagged

No significant circularity in proposed NIR diagnostic diagrams

full rationale

The paper derives its proposed diagnostic diagrams ([C I]/Paγ and H2 1-0 O(5)/PAH 3.3 μm) directly from empirical line-ratio measurements and classifications in the nine observed U/LIRGs, followed by comparison against independent photo-ionization models. No step reduces a claimed prediction or first-principles result to a fitted parameter, self-referential definition, or load-bearing self-citation chain; the correlations are presented as observed trends rather than constructed outputs. The kinematics (W80) analysis is likewise an independent observational check. The derivation therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The work relies on standard astrophysical assumptions about emission-line formation in photo-ionized gas and the applicability of existing photo-ionization models; no new free parameters, axioms beyond domain standards, or invented entities are introduced in the abstract.

axioms (1)
  • domain assumption Photo-ionization models can be used to evaluate the accuracy of empirical line-ratio classifications for gas excitation mechanisms
    The abstract states that empirical classifications are compared with photo-ionization models to assess reproducibility.

pith-pipeline@v0.9.0 · 5684 in / 1331 out tokens · 66965 ms · 2026-05-08T16:38:51.461418+00:00 · methodology

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Reference graph

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