Fine-structure Line Atlas for Multi-wavelength Extragalactic Study (FLAMES) I: Comprehensive Low and High Redshift Catalogs and Empirical Relations for Probing Gas Conditions

Amit Vishwas; Bo Peng; Carl Ferkinhoff; Catie Ball; Christopher Rooney; Cody Lamarche; Gordon Stacey; Thomas Nikola

REVIEW 3 major objections 5 minor 2 cited by

Fine-structure Line Atlas for Multi-wavelength Extragalactic Study (FLAMES) I: Comprehensive Low and High Redshift Catalogs and Empirical Relations for Probing Gas Conditions

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Ion abundance, not gas density, sets far-infrared line ratios.

desk verdict A solid, useful catalog paper that deserves review; the AGN decomposition is model-dependent enough that the AGN fractions should be treated as illustrative until robustness tests are added. read the letter →

arxiv 2507.10702 v1 pith:6HHZDIC3 submitted 2025-07-14 astro-ph.GA

Bo Peng , Cody Lamarche , Catie Ball , Amit Vishwas , Gordon Stacey , Christopher Rooney , Thomas Nikola , Carl Ferkinhoff This is my paper

classification astro-ph.GA

keywords fine-structurelinesfar-infraredspectroscopyinterstellarmediumdiagnosticsgalaxymetallicityAGNcontributionhigh-redshiftgalaxieslineratiosdensity

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Using a newly assembled atlas of 1,273 low-redshift and 543 high-redshift galaxies with far- and mid-infrared fine-structure line measurements, this paper asks what actually controls the observed line ratios. Across galaxy types and redshifts, the ratios correlate tightly with elemental abundances such as N/O and O/H and with radiation-hardness indicators, while density-sensitive ratios cluster near their low-density limits. The paper concludes that variations in fine-structure line ratios are primarily driven by how many of each ion are present, rather than by electron density or temperature. It also quantifies AGN contributions to $[\mathrm{O\,III}]_{88}$ and $[\mathrm{O\,I}]_{63}$, so the contamination can be removed and the corrected ratios can serve as metallicity and radiation-field diagnostics.

What carries the argument

The load-bearing identity is the line-ratio decomposition in Eq. (1): $L_X/L_Y = (X/Y)\cdot(\mathrm{ICF})\cdot(\varepsilon_X/\varepsilon_Y)$. It separates a ratio's dependence on elemental abundance, ionization correction factor, and line emissivity, and the analysis uses it to decide which diagnostics isolate density, temperature, radiation hardness, or abundance. The second mechanism is the additive AGN decomposition $L_{\rm line} = L_{\rm SF} + L_{\rm AGN}$, calibrated by plotting high-ionization lines against the AGN-only anchors $[\mathrm{Ne\,V}]_{14}$ and $[\mathrm{O\,IV}]_{26}$ with $[\mathrm{Ne\,II}]_{12}$ or $[\mathrm{C\,II}]$ as the star-forming normalizer; a first-order polynomial fit separates the star-forming and AGN branches and yields AGN fractions for $[\mathrm{O\,III}]_{88}$ and $[\mathrm{O\,I}]_{63}$.

What would settle it

Compare galaxies with matched N/O and O/H but very different radiation-hardness indicators, for example AGN-dominated versus pure starburst systems: if $[\mathrm{O\,III}]_{88}/[\mathrm{C\,II}]$ and $[\mathrm{N\,II}]/[\mathrm{C\,II}]$ still differ by large factors after applying the paper's AGN correction, then abundance is not the primary driver. A more direct test would spatially resolve a nearby galaxy and measure $[\mathrm{O\,III}]_{88}$ and $[\mathrm{N\,II}]_{122/205}$ at matched local N/O to see whether local density variations produce ratio changes the global analysis would miss.

Watch

Extended reading notes

Core claim

The central claim is that observed variations in far-infrared fine-structure line ratios (for example $[\mathrm{O\,III}]_{88}/[\mathrm{C\,II}]$, $[\mathrm{N\,II}]/[\mathrm{C\,II}]$, and $[\mathrm{N\,III}]/[\mathrm{O\,III}]_{88}$) are dominated by the relative abundances of the emitting ions, expressed through the elemental abundance ratio and the ionization correction factor in the line-ratio identity, with emissivity variations playing a secondary role. This is why the ratios work as empirical metallicity and radiation-field tracers. Supporting evidence includes tight correlations between FIR ratios and N/O, agreement between FIR and optical $[\mathrm{O\,III}]$-to-low-ionization ratios, and a demonstration that most density-sensitive ratios sit near their low-density limits; the $[\mathrm{N\,II}]_{122/205}$ ratio instead gives a nearly constant median electron density of about $50\,\mathrm{cm^{-3}}$. The paper further claims that AGN activity contributes measurably to $[\mathrm{O\,III}]_{88}$ and $[\mathrm{O\,I}]_{63}$, and that this contamination can be decomposed and removed using $[\mathrm{Ne\,V}]_{14}$ and $[\mathrm{O\,IV}]_{26}$ as AGN-only anchors.

Load-bearing premise

The AGN corrections and the abundance interpretation assume each galaxy's line luminosity splits cleanly into a star-forming plus an AGN component, with $[\mathrm{Ne\,V}]$ and $[\mathrm{O\,IV}]$ emitted only by the AGN, $[\mathrm{Ne\,II}]$ and $[\mathrm{C\,II}]$ representing star-forming ISM, and star-forming line ratios staying constant; if the AGN heats $[\mathrm{Ne\,II}]$ or very hard star-forming regions produce $[\mathrm{Ne\,V}]$ or $[\mathrm{O\,IV}]$, the corrected ratios and the abundance conclusion shift.

Editorial extensions

If this is right

The ratio $[\mathrm{N\,III}]/[\mathrm{O\,III}]_{88}$ works as a direct N/O diagnostic with roughly 0.25 dex scatter, matching the theoretical emissivity ratio and avoiding the need for [O iii]52.
The 'deficit' seen in [C ii]/IR is not unique: all major FIR FSLs decline relative to IR luminosity above $L_{\rm IR}\sim10^{11}\,L_\odot$, with the high-redshift branch shifted to higher luminosity.
Most published electron densities from high-ionization tracers such as [O iii]52/88, [Ne v]14/24, and [S iii]18/33 are unreliable for galaxy-integrated gas; the [N ii]122/205 ratio is the robust exception, giving a median density near 50 cm$^{-3}$ with little variation.
AGN contamination in [O iii]88 and [O i]63 can be corrected using the fitted decomposition, and [S iv]10 is almost always AGN-dominated, making it a useful mid-infrared AGN indicator.
FIR and optical forbidden-line ratios track each other over two orders of magnitude, so optical ionization-parameter diagnostics can be extended into dusty, high-SFR galaxies using FIR lines.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

The paper leaves implicit that published single-line SFR and gas-mass calibrations, especially those using [C ii], may need metallicity corrections because line luminosity changes with ion abundance at fixed star formation rate.
Extending the AGN correction to high redshift could revise some reported ionizing-photon production rates, since [O iii]88 detections attributed to star formation may partly trace AGN activity.
The FIR-optical concordance suggests rest-frame optical metallicity diagnostics could be calibrated against FIR ratios for heavily obscured galaxies, extending abundance measurements to populations inaccessible to optical spectroscopy.

Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Bottom line: this is a genuinely useful synthesis and deserves a serious referee, but the quantitative AGN decomposition in Sec 4.2 is model-dependent enough that I would want a robustness test before trusting the f_AGN numbers. The underlying empirics are mostly solid.

What is new: the unified low-z (1273) and high-z (543) catalogs, the standardized S60/S100 calibration, the systematic demonstration that most density tracers sit near their low-density limits, and the first attempt to quantify AGN contamination in [O iii]88 and [O i]63. The N3O3-N/O calibration and the FIR-optical concordance tests are genuinely useful, and the paper is honest about aperture mismatches, selection effects, and the fact that many literature values lack error bars. The PyNeb emissivities and external metallicity calibrations keep the abundance argument from being circular.

Soft spots: the complete catalogs are not in the preprint, only described; that is a real impediment for a catalog paper and should be fixed before acceptance. More substantively, the AGN decomposition assumes L_line = L_SF + L_AGN with [Ne v] and [O iv] as pure AGN tracers and [C ii]/[Ne ii] as pure SF anchors. The [C ii] assumption is the shaky one: [C ii] is expected to be enhanced in XDRs around AGN, and the paper only puts AGN terms on the numerator lines. If [C ii] has an AGN-correlated component, the fitted slopes and intercepts for [O iii]88 and [O i]63 are biased. The paper acknowledges [O i] is XDR-enhanced and [O iv] can appear in hard SF, so the purity of the anchors is not just a theoretical nit. That said, the broad claim that FSL ratios are abundance-driven does not collapse: it is backed by the N/O correlations and the FIR-optical agreement, which do not rely on the decomposition. I would treat the derived AGN fractions as illustrative, not as calibrated measurements.

The other caveats (OT-MBB beta=2, default lensing magnification of 6, 80% [C ii] neutral fraction) are stated and standard; not fatal.

Who: FIR/sub-mm observers, people planning JWST/ALMA programs, and anyone interpreting [O iii]88/[C ii] in AGN hosts. Worth citing as a resource. Recommendation: send to peer review, but require machine-readable catalogs, uncertainty propagation, and a sensitivity test that allows an AGN component in [C ii] or uses [Ne ii] as an alternative SF anchor.

Referee Report

3 major / 5 minor

Summary. The paper presents FLAMES I, a compilation of 1273 low-redshift and 543 high-redshift galaxy-integrated fine-structure line (FSL) measurements drawn from the literature, supplemented with MIR/optical lines, photometry, dust temperatures, metallicities, and ancillary properties. It uses this atlas to re-examine empirical scaling relations: the [C II]/IR "deficit," line equivalent widths, density diagnostics, radiation-field and abundance diagnostics, electron-temperature probes, FIR-optical concordance, and low-z versus high-z ISM properties. The central empirical claim is that variations in FIR FSL ratios are primarily driven by the relative abundances of emitting ions, with radiation-field hardness playing a secondary role, while density and temperature variations are subdominant. A second key result is an empirical decomposition of AGN contributions to [O III]88 and [O I]63 using [Ne V]14 and [O IV]26 as AGN tracers.

Significance. If the results hold, this would be the most comprehensive FSL reference catalog currently available and a useful set of empirical calibrations bridging FIR and optical diagnostics. The paper's strengths are its breadth, the explicit discussion of selection effects and caveats, the use of PyNeb atomic-emissivity calculations for the theoretical curves, and the demonstration that many FIR line ratios track optical diagnostics over two orders of magnitude. The AGN decomposition, if robust, would provide a practical correction for [O III]88 and [O I]63 in AGN hosts, which is directly relevant to high-redshift studies. However, the absence of the machine-readable catalogs in the submitted version and the load-bearing assumptions in the AGN decomposition currently limit the strength of the central claim.

major comments (3)

[Sec. 4.2, Fig. 27] The AGN decomposition assumes L_line = L_SF + L_AGN, with L_AGN proportional to L[Ne V]14 (or L[O IV]26) and L_SF proportional to L[C II] (or L[Ne II]12 for the MIR lines). The paper itself notes that [O IV]26 can arise in intense or low-metallicity star-forming environments and that [O I] is enhanced in X-ray-dominated regions near AGNs, where [C II] is also expected to be enhanced. Because [C II] is the denominator for the corrected [O III]88/[C II] and [O I]63/[C II] ratios used in the subsequent abundance and radiation-field analysis, an AGN contribution to [C II] would bias the fitted slope and intercept and hence the derived f_AGN values. Please provide a sensitivity test, for example by allowing a free AGN component in [C II] proportional to L[Ne V] or by repeating the decomposition after excluding all known AGN hosts, and state explicitly how the abundance-driven interpretation changes.
[Appendices A and B] The primary products of this catalog paper, the full low-z and high-z value-added tables, are not included in the submitted manuscript; the text states that the full machine-readable tables will be available in the online published version and can be obtained by contacting the corresponding author. This prevents the reader from verifying the claimed sample sizes (1273 and 543 entries), the estimated >95% and >90% literature coverage, and the empirical relations that form the basis of the paper's conclusions. Please submit the complete catalogs as machine-readable ancillary files.
[Appendix B.5] For high-z DSFGs believed to be lensed but lacking a lens model, a default magnification of mu = 6 is assigned and used to compute intrinsic luminosities. This placeholder affects LIR and line luminosities of high-z sources in Figures 1, 6, and 7 and therefore the claimed roughly one-decade offset of the high-z "deficit" branch. If the low-z/high-z comparisons use line ratios that cancel magnification, this should be stated explicitly; otherwise, please quantify the sensitivity of the high-z conclusions by repeating the relevant plots with alternative assumptions (e.g., mu = 1 and mu = 10).

minor comments (5)

[Sec. 3.5, Eq. (2)] The weighted-average density formula is difficult to read as printed; the summation indices and the quantity being averaged should be written out unambiguously.
[Sec. 2.2] The statement that the O3N2 index overestimates O/H by 0.15 dex and the N2 index by 0.2 dex is applied without a citation; please provide the calibration comparison used to derive these offsets.
[Sec. 3.5 and Fig. 13] The assumed values Te/TH0 = 66.6, neTe = nH0 TH0, and a [C II] neutral fraction of 80% are introduced in the figure caption; please state them in the main text and note how sensitive the [O I]/[C II] comparison is to these choices.
[Sec. 3.7] Many literature metallicities and N/O values lack error bars, a point the paper acknowledges; the reported 0.25 dex scatter in the N/O calibrations likely includes this systematic component, and this should be stated where the calibrations are quoted.
[Throughout] Several typographical errors should be fixed: "beacause" in Sec. 4.3, "refshift" in Appendix B.6, "Our analysis focus" in the abstract, and the missing sigma symbol in the panel annotations of Figs. 12-22 and similar figures.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the catalog's empirical relations and AGN decomposition are self-contained and do not reduce to their own inputs.

full rationale

The paper is an empirical atlas paper whose derivation chain is self-contained. The central claim that FSL ratio variations are primarily driven by ionic abundances rests on three independent lines of evidence: (i) correlations with optically derived N/O and O/H calibrations (Sec. 3.7), (ii) concordance between FIR and optical line ratios (Sec. 4.3), and (iii) the small observed scatter in density diagnostics, which limits the dynamic range of the emissivity term in Eq. 1. None of these defines the target ratio in terms of itself. The N/O calibration N/O = 0.66 x [N iii]/[O iii]88 is an empirical fit whose normalization is explicitly checked against the PyNeb emissivity ratio (1.47), and it is presented as a calibration rather than as a prediction from first principles. The AGN decomposition in Sec. 4.2 is an explicit two-component model L_line = L_SF + L_AGN with distinct anchors ([Ne ii]12 and [C ii] for SF; [Ne v]14 and [O iv]26 for AGN). The fitted slope and intercept are used to compute AGN fractions, which is a model inference, not a self-consistency loop, and the AGN-dominated branch is checked against the external Spoon et al. (2022) scaling. The skeptical concern that [C ii] could carry an AGN component is a model-robustness caveat, not a circularity: the decomposition assumes a pure SF anchor, so a violation would bias the fitted fractions, but the derivation does not assume its own conclusion. Self-citations (Peng et al. 2021; Lamarche et al. 2022) are data and calibration references and are not load-bearing; the N3O3 diagnostic is re-derived in this paper from PyNeb atomic data. No step reduces to its own input by construction, no uniqueness theorem is imported, and no ansatz is smuggled in via citation. Accordingly, the circularity score is 0.

Assumptions & free parameters 8 free parameters · 7 assumptions · 0 invented entities

The central empirical claims rest on heterogeneous literature data; the main model-dependent inputs are the dust color calibration, the linear AGN decomposition, and the neutral gas assumptions. No new physical entities are introduced. The values above are fitted or hand-set parameters that the analysis leans on.

free parameters (8)

OT-MBB emissivity index beta = 2
Fixed by hand in Appendix C for dust color temperature conversion; small impact below 160 micron but affects S60/S100-to-Tdust and LIR estimates.
OT-MBB LIR correction factor = 1.4
Applied in Appendix C to the OT-MBB integrated luminosity so that LIR matches the MBB+PL value; chosen by hand.
Line continuum color to S60/S100 power-law fits = e.g. S63/S158 = 0.65 x (S60/S100)^0.58
Empirical fits in Fig. 30 used to standardize dust color when S60/S100 is not directly measured; fitted to low-z data.
AGN decomposition coefficients = [Ne III]15/[Ne V]14 = 1.7; [S IV]10 intercept 0.016, slope 0.85; [O III]88/[C II] intercept 0.16, slope 1.08; [O…
First-order polynomial coefficients fitted in Sec 4.2 and used to subtract AGN contributions from MIR and FIR lines.
Median L24/LIR = 0.15
Used as the reference ratio in Fig. 10 when comparing Lline/L24 to Lline/LIR.
Default lensing magnification for high-z DSFGs = 6
Placeholder magnification listed in Appendix B.5 for galaxies believed to be lensed but without lens models; affects intrinsic luminosities.
Assumed [C II] neutral fraction = 0.8
Used in Sec 3.5 for neutral gas density diagnostics involving [O i]/[C II].
Metallicity calibration offsets = O3N2: +0.15 dex, N2: +0.2 dex
Applied in Sec 2.2 to computed O/H values to align different strong-line calibrations with literature values.

assumptions (7)

domain assumption Line ratio decomposition in Eq. 1: L(X)/L(Y) = abundance ratio times ICF ratio times emissivity ratio
Assumes collisionally excited, optically thin lines with no differential dust attenuation; used throughout the analysis.
standard math Atomic data and collisional rates from PyNeb, Barinovs et al. 2005, Abrahamsson et al. 2007, and Draine 2011
Underlie the theoretical diagnostic curves in Sec 3.5 and the electron temperature conversions in Sec 3.8.
ad hoc to paper AGN tracer purity: [Ne v]14 and [O iv]26 trace only AGN activity or strong shocks, and [Ne ii]12 represents the star-forming ISM
Needed for the linear AGN decomposition in Sec 4.2; the paper provides supporting citations but no independent check within this work.
ad hoc to paper Constant star-forming component ratio to [Ne ii]12 in the AGN decomposition
Sec 4.2 fits y = ax + b and treats the intercept b as a fixed SF ratio for all non-dwarf galaxies, which the authors acknowledge is an oversimplification.
ad hoc to paper Fixed Te/TH0 = 66.6 and pressure equilibrium neTe = nH0 TH0 for neutral gas diagnostics
Reduces four degrees of freedom in the [O i]/[C II] density comparison in Sec 3.5.
domain assumption Case B Balmer decrement H alpha/H beta = 2.86 and Calzetti et al. 2000 extinction law
Used for optical extinction correction in Sec 2.2 and Appendix D; the paper validates it above 4300 A but notes it over-corrects H delta and [O ii].
domain assumption Completeness estimates of more than 95% of low-z and more than 90% of high-z FSL data
The authors state these are conservative estimates, but they are not independently verifiable from the preprint.

how reviews work

0 comments

Cite this review

Pith. "Pith review of Fine-structure Line Atlas for Multi-wavelength Extragalactic Study (FLAMES) I: Comprehensive Low and High Redshift Catalogs and Empirical Relations for Probing Gas Conditions." pith.science (2026). https://pith.science/paper/6HHZDIC3

@misc{pith2026250710702,
  author       = {Pith},
  title        = {Pith review of: Fine-structure Line Atlas for Multi-wavelength Extragalactic Study (FLAMES) I: Comprehensive Low and High Redshift Catalogs and Empirical Relations for Probing Gas Conditions},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6HHZDIC3}},
  note         = {Machine review of arXiv:2507.10702}
}

read the original abstract

Far-infrared (FIR) and mid-infrared (MIR) fine-structure lines (FSLs) are widely used for studying galaxies nearby and faraway. However, interpreting these lines is complicated by factors including sample and data bias, mismatch between resolved calibrations and unresolved observations, limitations in generalizing from case studies, and unresolved issues like the origin of [C II] emission and the so-called ``deficit.''In this series of papers, we assemble and analyze the most comprehensive atlas of FSL data to date. We explore their empirical correlations (paper I), compare them with photoionization models that cover multiphase gas (paper II), and discuss their physical origins and the new perspectives they offer for studying physical properties (paper III). The first paper introduces value-added catalogs of global FSL data of low- and high-z galaxies compiled from the literature, covering most of the existing observations, supplemented with ancillary ultraviolet to FIR information. Our analysis focus on commonly used diagnostics, such as electron density, radiation field strength, metallicity, and electron temperature. We present their distributions across different galaxy samples and redshifts, and cross-validate the reliability of these diagnostics in measuring physical conditions. By examining empirical relations, we identify the contribution of active galactic nuclei (AGN) to the FIR FSLs [O III]88 and [O I]63, and reveal a bias in density measurements. FIR FSLs show good concordance with their optical counterparts. Our findings indicate that variations in FSL ratios are primarily driven by the relative abundances of emitting ions, underscoring their value as tracers of metallicity and radiation field strength. Finally, we compare the FIR FSL properties of low- and high-z galaxies, discussing both their similarities and differences.

Figures

Figures reproduced from arXiv: 2507.10702 by the authors.

**Figure 1.** Redshift distribution of the IR luminosity LIR of the sample. The data points are divided into low-z and high-z with the redshift cut at 1. The low-z galaxies are plotted as small dots, with the color scheme: blue–dwarf galaxies, orange–star-forming (SF) galaxies, red–U/LIRGs, cyan–LINERs, black–AGNs, gray–early type galaxies (ETGs), green-yellow–regions. All high-z data points are shown as larger symbols edged in … view at source ↗

**Figure 2.** IR-to-FUV luminosity (LIR-to-LFUV) comparison. The style of the plot is the same as that of [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗

**Figure 3.** compares the color temperature S60/S100 with both LIR and IRX. Among low-z galaxies (excluding dwarfs), there is a clear positive correlation, such that galaxies with higher LIR systematically exhibit higher S60/S100 and thus higher Tdust. The majority of low-z galaxies in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

Figures from the paper (27 more)

**Figure 4.** Figure 4: Redshift distribution of the luminosity of a, [C ii]; and b, [O iii]88. Grey shades denote the redshift coverages of ALMA bands. The plot style is the same as in [PITH_FULL_IMAGE:figures/full_fig_p008_4.png]

**Figure 6.** Figure 6: Total IR luminosity LIR vs. a, [C ii] luminosity L[C II]; and b, the residual [C ii]/IR. The dashed line in (a) denotes the linear relation corresponding to the non-“deficit” trend. The blue, red, and gray shades in (b) highlight the non-deficit, low-z “deficit”, and h…

**Figure 5.** Figure 5: Redshift distribution of the other FIR FSL luminosities. continued from [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]

**Figure 7.** Figure 7: IR luminosity LIR vs. Lline/LIR for a, [O iii]88; b, [O i]63; c, [O i]145; d, [N iii]; e, [N ii]122; f, and [N ii]205. The plot style is the same as [PITH_FULL_IMAGE:figures/full_fig_p010_7.png]

**Figure 8.** Figure 8: FUV luminosity LFUV vs. a, [C ii]/LFUV; and b, [O iii]88/LFUV. The gray lines correspond to constant Lline values. The fitting results on line/FUV are shown as shades for low-z SFs (orange), dwarf & LBG/LAEs (blue), and high-z QSOs (gray). The results and scatter are d…

**Figure 9.** Figure 9: Line equivalent width vs. Lline/LIR for a, [C ii]; b, [O iii]88; c, [O i]63; d, [O i]145; e, [N ii]122; f, [N ii]205. The dashed line in each panel corresponds to the linear fit, the fitting result and scatter are displayed at the lower right corner. The plot style is …

**Figure 10.** Figure 10: Lline/24 µm luminosity vs. Lline/LIR for a, [C ii]; b, [O iii]88; c and d, [N ii] doublets. The dashed lines represent the median L24µm/LIR value of 0.15. 3.6. Radiation Field and AGN Decomposition Comparisons of emission from different ionization states have been ext…

**Figure 11.** Figure 11: a, density diagnostic curves of [Ne v]14/24 (black), [Ne iii]15/16 (purple), [O iii]52/88 (blue), [S iii]18/33 (yellow), [N ii]122/205 (pale green), [N ii]122/[C ii]ion (dark green), [S ii]λ6731/6716 (yellow green), [O ii]λ3726/3729 (sky blue) [O i]63/[C ii](H0 ) (br…

**Figure 12.** Figure 12: Demographics of all the density related line ratios displayed along with LIR (left column) and redshift (right column). The median value fit on low-z galaxies is printed at the upper left corner of panels in the right column [PITH_FULL_IMAGE:figures/full_fig_p014_12.png]

**Figure 13.** Figure 13: Comparison between different density diagnostics. Top: [O iii]52/88 vs. high-ionization diagnostics a, [S iii]18/33; and b, [Ne v]14/24; middle: [N ii]122/205 vs. c, [O iii]52/88; and d, [S ii]λ6731/6716; bottom: [N ii]122/205 vs. e, [O i]63/145; and f, [O i]145/[C i…

**Figure 14.** Figure 14: Demographics of FIR radiation field diagnostics. mental abundances that they can serve as direct metallicity diagnostics. It is important to note that the abundances used here are predominantly derived from optical strong line methods, which themselves have systemat…

**Figure 16.** Figure 16: a, [Ne iii]15/[Ne ii]12 vs. [O iii]88/[C ii]; b, [O iii]88/(10×[O i]145 or [O i]63); c, [O iii]88/([N ii]205 or 0.5×[N ii]122); d, [N iii]/([N ii]205 or 0.5×[N ii]122). The diagonal dashed line represent the slope of unity as a visual aid. The [Ne iii]15 and [O iii]88…

**Figure 17.** Figure 17: a, [O iii]88/[O i] vs. [O iii]88/[C ii]. In lower row, [N iii]/[N ii] vs. b, [O iii]88/[C ii]; and c, [O iii]88/[O i]. The diagonal dashed lines have slope of unity, and are shown as visual aids. tral gas (f[C II],neutral), but previous extragalactic work has often ig…

**Figure 18.** Figure 18: Demographics of all abundance diagnostics [PITH_FULL_IMAGE:figures/full_fig_p019_18.png]

**Figure 19.** Figure 19: N/O abundance ratio vs. a, [N iii]/[O iii]88; and b, [N iii]/([O iii]88+[O iii]52. The gray dashed lines and shades are the linear fits, which are described at the lower right corners. The plot style is the same as [PITH_FULL_IMAGE:figures/full_fig_p020_19.png]

**Figure 21.** Figure 21: Radiation field strength U–elemental abundance correlation. [O iii]88/[C ii] versus a, [N ii]/[C ii]; and b, log (O/H). [O iii]88/[O i] versus c, [N ii]/[C ii] and d, log (O/H). The gray dashed line and shade correspond to the linear fit on the low-z galaxy data, whi…

**Figure 20.** Figure 20: N/O abundance ratio vs. a & b, [N ii]/[C ii]; c & d, [N ii]/[O i]63; e & f, [N ii]/[O i]145. [N ii]122 is compared in the left column, and [N ii]205 in the right column. The gray dashed lines and shades are the linear fit result and residual scatter, which are also re…

**Figure 22.** Figure 22: Demographics of electron temperature diagnostics. 5 4 3 log (O/H) 10 1 10 0 10 1 L[O III] 5007, ext. corr/L[O III]88 U/LIRG Dwarf AGN LINER SF high-z DSFG high-z LBG/LAE 10 4 6 × 10 3 2 × 10 4 Te [K] ne = 50 cm 3 10 cm 3 250 cm 3 a b [PITH_FULL_IMAGE:figures/full_fig…

**Figure 23.** Figure 23: Extinction corrected [O iii]λ5007-to-[O iii]88 ratio vs. a, metallicity ; and b, electron temperature diagnostic curve. The theoretical emissivity ratios are computed and shown assuming different electron densities ne = 50 (solid), 10 (dotted), and 250 cm-3 (long das…

**Figure 25.** Figure 25: [Ne v]14-to-[O iv]26 luminosity comparison. The gray dashed line and shade denotes the linear fit and scatter, which is also printed at the lower right corner. ture and excitation physics, the lower density limit for each tracer increases with ionization state—–progre…

**Figure 26.** Figure 26: High-ionization lines [Ne iii]15 (first row) and [S iv]10 (second row) vs. AGN lines [Ne v]14 (first column) and [O iv]26 (second column). All luminosities are normalized by L[Ne II]12. The dotted lines have slope of unity, corresponding to fAGN = 1%, 10% and 100%. …

**Figure 27.** Figure 27: [O iii]88 (top) and [O i]63 vs. AGN lines [Ne v]14 (left column) and [O iv]26 (right column). The luminosities are normalized by L[C II]. The plot style is the same as [PITH_FULL_IMAGE:figures/full_fig_p024_27.png]

**Figure 28.** Figure 28: FIR line ratios [O iii]88 to [C ii] (first row), (10×[O i]145 or [O i]63) (second row), ([N ii]205 or 0.5×[N ii]122) (third row), vs. optical line ratios [O iii]λ5007 to [O i]λ6300 (first column), [S ii]λ6716&6731 (second column), [N ii]λ6584 (third column). The FIR l…

**Figure 29.** Figure 29: a, spectral profiles of the two dust SEDs considered in the paper (OT-MBB as dashed line, MBB+PL as dotted line) compared to a blackbody curve (solid line), in the wavelength range 8-to-1000 µm. The lines are color– coded according to the dust temperature noted in th…

**Figure 30.** Figure 30: Conversion between S60/S100 and the line continuum colors a, S63/S158; b, S88/S158; c, S63/S122; and d, S63/S88. Low-z data are shown as circles with error bars in the same plotting style as [PITH_FULL_IMAGE:figures/full_fig_p039_30.png]

**Figure 31.** Figure 31: Monochromatic-to-total IR luminosity ratio νLν/LIR vs. dust color S60/S100, for a-d 12, 24, 60, 63 µm; and e-h 88, 100, 122, and 158 µm. The plot style is the same as in [PITH_FULL_IMAGE:figures/full_fig_p040_31.png]

**Figure 32.** Figure 32: Observed Balmer decrement Hα/Hβ vs. a, Balmer line ratios Hα/Hγ; and b, Hα/Hδ. The observed line ratios for the y-axis are plotted as semi-transparent “x” symbols, and the ratios after dust extinction correction are plotted as opaque circles. The horizonal dashed line…

Discussion (0). Sign in to comment.

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Fine-structure Line Atlas for Multi-wavelength Extragalactic Study (FLAMES) III: [C II] as Tracer, Crisis of SFR, [O III]/[C II] at High-z, New Answers and New Questions
astro-ph.GA 2025-07 conditional novelty 6.0 of 10

A universal gas-line deficit relative to infrared luminosity, seen in [C II], [O I], [N II], and extinction-corrected H-alpha, breaks standard SFR calibrations in the brightest dusty galaxies and implies a metallicity...
Fine-structure Line Atlas for Multi-wavelength Extragalactic Study (FLAMES) II: Photoionization Model View of Ionized to Neutral Gas Emission
astro-ph.GA 2025-07 conditional novelty 6.0 of 10

A 20,446-model photoionization grid with power-law fits shows FIR fine-structure line ratios are set by three composite quantities (U1, ne, N/O) while U, Q1/Q0, and O/H remain degenerate without MIR or optical data.

Reference graph

Works this paper leans on

297 extracted references · 11 canonical work pages · cited by 2 Pith papers

[1]

P., Ferland, G

Abel, N. P., Ferland, G. J., Shaw, G., & van Hoof, P. A. M. 2005, ApJS, 161, 65, doi: 10.1086/432913

doi:10.1086/432913 2005
[2]

V., & Dalgarno, A

Abrahamsson, E., Krems, R. V., & Dalgarno, A. 2007, ApJ, 654, 1171, doi: 10.1086/509631

doi:10.1086/509631 2007
[3]

B., Fujimoto, S., Finlator, K., et al

Akins, H. B., Fujimoto, S., Finlator, K., et al. 2022, ApJ, 934, 64, doi: 10.3847/1538-4357/ac795b

doi:10.3847/1538-4357/ac795b 2022
[4]

C., Swinbank, A

Alaghband-Zadeh, S., Chapman, S. C., Swinbank, A. M., et al. 2013, MNRAS, 435, 1493, doi: 10.1093/mnras/stt1390

doi:10.1093/mnras/stt1390 2013
[5]

2025, arXiv e-prints, arXiv:2501.10508, doi: 10.48550/arXiv.2501.10508

Algera, H., Rowland, L., Stefanon, M., et al. 2025, arXiv e-prints, arXiv:2501.10508, doi: 10.48550/arXiv.2501.10508

doi:10.48550/arxiv.2501.10508 2025
[6]

Algera, H. S. B., Inami, H., Sommovigo, L., et al. 2024a, MNRAS, 527, 6867, doi: 10.1093/mnras/stad3111

doi:10.1093/mnras/stad3111
[7]

Algera, H. S. B., Inami, H., De Looze, I., et al. 2024b, MNRAS, 533, 3098, doi: 10.1093/mnras/stae1994

doi:10.1093/mnras/stae1994
[8]

S., Tucker, D

Allam, S. S., Tucker, D. L., Lin, H., et al. 2007, ApJL, 662, L51, doi: 10.1086/519520 ´Alvarez-M´ arquez, J., Crespo G´ omez, A., Colina, L., et al. 2023, A&A, 671, A105, doi: 10.1051/0004-6361/202245400 ´Alvarez-M´ arquez, J., Colina, L., Crespo G´ omez, A., et al. 2024, A&A, 686, A85, doi: 10.1051/0004-6361/202347946

doi:10.1086/519520 2007

Show all 297 references

[9]

W., et al

Amvrosiadis, A., Lange, S., Nightingale, J. W., et al. 2025, MNRAS, 537, 1163, doi: 10.1093/mnras/staf048

2025 doi
[10]

2008, A&A, 491, 747, doi: 10.1051/0004-6361:200810482

Ao, Y., Weiß, A., Downes, D., et al. 2008, A&A, 491, 747, doi: 10.1051/0004-6361:200810482

2008 doi
[11]

2008, A&A, 491, 173, doi: 10.1051/0004-6361:200810628

Aravena, M., Bertoldi, F., Schinnerer, E., et al. 2008, A&A, 491, 173, doi: 10.1051/0004-6361:200810628

2008 doi
[12]

S., Bethermin, M., et al

Aravena, M., Spilker, J. S., Bethermin, M., et al. 2016, MNRAS, 457, 4406, doi: 10.1093/mnras/stw275 Arellano-C´ ordova, K. Z., & Rodr ´ ıguez, M. 2020, MNRAS, 497, 672, doi: 10.1093/mnras/staa1759

2016 doi
[13]

M., Evans, A

Armus, L., Mazzarella, J. M., Evans, A. S., et al. 2009, PASP, 121, 559, doi: 10.1086/600092

2009 doi
[14]

2024, A&A, 688, A146, doi: 10.1051/0004-6361/202348824

Arribas, S., Perna, M., Rodr ´ ıguez Del Pino, B., et al. 2024, A&A, 688, A146, doi: 10.1051/0004-6361/202348824

2024 doi
[15]

J., & Scott, P

Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481, doi: 10.1146/annurev.astro.46.060407.145222 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, ...

2009
[16]

M., et al

Baier-Soto, R., Herrera-Camus, R., F¨ orster Schreiber, N. M., et al. 2022, A&A, 664, L5, doi: 10.1051/0004-6361/202243642

2022 doi
[17]

Bakx, T. J. L. C., Tamura, Y., Hashimoto, T., et al. 2020, MNRAS, 493, 4294, doi: 10.1093/mnras/staa509

2020 doi
[18]

Bakx, T. J. L. C., Sommovigo, L., Carniani, S., et al. 2021, MNRAS, 508, L58, doi: 10.1093/mnrasl/slab104

2021 doi
[19]

Bakx, T. J. L. C., Zavala, J. A., Mitsuhashi, I., et al. 2023, MNRAS, 519, 5076, doi: 10.1093/mnras/stac3723

2023 doi
[20]

Bakx, T. J. L. C., Algera, H. S. B., Venemans, B., et al. 2024a, MNRAS, 532, 2270, doi: 10.1093/mnras/stae1613

doi
[21]

Bakx, T. J. L. C., Amvrosiadis, A., Bendo, G. J., et al. 2024b, MNRAS, 535, 1533, doi: 10.1093/mnras/stae2409

doi
[22]

A., Phillips, M

Baldwin, J. A., Phillips, M. M., & Terlevich, R. 1981, PASP, 93, 5, doi: 10.1086/130766

1981 doi
[23]

2024, arXiv e-prints, arXiv:2408.12299, doi: 10.48550/arXiv.2408.12299 42 Peng et al

Banados, E., Khusanova, Y., Decarli, R., et al. 2024, arXiv e-prints, arXiv:2408.12299, doi: 10.48550/arXiv.2408.12299 42 Peng et al. Barinovs, ˘G., van Hemert, M. C., Krems, R., & Dalgarno, A. 2005, ApJ, 620, 537, doi: 10.1086/426860

2024 doi arXiv
[24]

L., Capak, P

Barisic, I., Faisst, A. L., Capak, P. L., et al. 2017, ApJ, 845, 41, doi: 10.3847/1538-4357/aa7eda

2017 doi
[25]

1992, ApJL, 399, L19, doi: 10.1086/186596

Barvainis, R., Antonucci, R., & Coleman, P. 1992, ApJL, 399, L19, doi: 10.1086/186596

1992 doi
[26]

J., et al

Beelen, A., Cox, P., Benford, D. J., et al. 2006, ApJ, 642, 694, doi: 10.1086/500636

2006 doi
[27]

W., Moiseev, A., et al

Belokurov, V., Evans, N. W., Moiseev, A., et al. 2007, ApJL, 671, L9, doi: 10.1086/524948

2007 doi
[28]

A., Pogge, R

Berg, D. A., Pogge, R. W., Skillman, E. D., et al. 2020, ApJ, 893, 96, doi: 10.3847/1538-4357/ab7eab

2020 doi
[29]

2023, ApJ, 952, 84, doi: 10.3847/1538-4357/acd643

Bergamini, P., Acebron, A., Grillo, C., et al. 2023, ApJ, 952, 84, doi: 10.3847/1538-4357/acd643

2023 doi
[30]

N., Longair, M

Best, P. N., Longair, M. S., & Roettgering, H. J. A. 1998, MNRAS, 295, 549, doi: 10.1046/j.1365-8711.1998.01245.x B´ ethermin, M., De Breuck, C., Gullberg, B., et al. 2016, A&A, 586, L7, doi: 10.1051/0004-6361/201527739 B´ ethermin, M., Fudamoto, Y., Ginolfi, M., et al. 2020, ...

1998
[31]

2024, A&A, 686, A3, doi: 10.1051/0004-6361/202348845

Bik, A., ´Alvarez-M´ arquez, J., Colina, L., et al. 2024, A&A, 686, A3, doi: 10.1051/0004-6361/202348845

2024 doi
[32]

K., Hashimoto, T., et al

Binggeli, C., Inoue, A. K., Hashimoto, T., et al. 2021, A&A, 646, A26, doi: 10.1051/0004-6361/202038180

2021 doi
[33]

E., Hutchison, T

Birkin, J. E., Hutchison, T. A., Welch, B., et al. 2023, ApJ, 958, 64, doi: 10.3847/1538-4357/acf712

2023 doi
[34]

2025, arXiv e-prints, arXiv:2504.15357, doi: 10.48550/arXiv.2504.15357

Bischetti, M., Feruglio, C., Carniani, S., et al. 2025, arXiv e-prints, arXiv:2504.15357, doi: 10.48550/arXiv.2504.15357

2025 doi arXiv
[35]

2018, A&A, 617, A82, doi: 10.1051/0004-6361/201833249

Bischetti, M., Piconcelli, E., Feruglio, C., et al. 2018, A&A, 617, A82, doi: 10.1051/0004-6361/201833249

2018 doi
[36]

2024, ApJ, 970, 9, doi: 10.3847/1538-4357/ad4a77

Bischetti, M., Choi, H., Fiore, F., et al. 2024, ApJ, 970, 9, doi: 10.3847/1538-4357/ad4a77

2024 doi
[37]

T., & Betz, A

Boreiko, R. T., & Betz, A. L. 1996, ApJL, 464, L83, doi: 10.1086/310094

1996 doi
[38]

W., Dey, A., et al

Borys, C., Blain, A. W., Dey, A., et al. 2006, ApJ, 636, 134, doi: 10.1086/497983

2006 doi
[39]

Bosman, S. E. I., ´Alvarez-M´ arquez, J., Colina, L., et al. 2024, Nature Astronomy, 8, 1054, doi: 10.1038/s41550-024-02273-0

2024 doi
[40]

J., Smit, R., Schouws, S., et al

Bouwens, R. J., Smit, R., Schouws, S., et al. 2022, ApJ, 931, 160, doi: 10.3847/1538-4357/ac5a4a

2022 doi
[41]

Bowler, R. A. A., Bourne, N., Dunlop, J. S., McLure, R. J., & McLeod, D. J. 2018, MNRAS, 481, 1631, doi: 10.1093/mnras/sty2368

2018 doi
[42]

Bowler, R. A. A., Cullen, F., McLure, R. J., Dunlop, J. S., & Avison, A. 2022, MNRAS, 510, 5088, doi: 10.1093/mnras/stab3744 Bradaˇ c, M., Garcia-Appadoo, D., Huang, K.-H., et al. 2017, ApJL, 836, L2, doi: 10.3847/2041-8213/836/1/L2 Bradaˇ c, M., Strait, V., Mowla, L., et al. ...

2022 doi
[43]

D., Bouwens, R

Bradley, L. D., Bouwens, R. J., Ford, H. C., et al. 2008, ApJ, 678, 647, doi: 10.1086/533519

2008 doi
[44]

D., Bouwens, R

Bradley, L. D., Bouwens, R. J., Zitrin, A., et al. 2012, ApJ, 747, 3, doi: 10.1088/0004-637X/747/1/3

2012 doi
[45]

R., Dale, D

Brauher, J. R., Dale, D. A., & Helou, G. 2008a, ApJS, 178, 280, doi: 10.1086/590249 —. 2008b, ApJS, 178, 280, doi: 10.1086/590249

doi
[46]

J., Saxena, A., Cameron, A

Bunker, A. J., Saxena, A., Cameron, A. J., et al. 2023, A&A, 677, A88, doi: 10.1051/0004-6361/202346159

2023 doi
[47]

S., P´ erez-Fournon, I., Amber, S., et al

Bussmann, R. S., P´ erez-Fournon, I., Amber, S., et al. 2013, ApJ, 779, 25, doi: 10.1088/0004-637X/779/1/25

2013 doi
[48]

S., Riechers, D., Fialkov, A., et al

Bussmann, R. S., Riechers, D., Fialkov, A., et al. 2015, ApJ, 812, 43, doi: 10.1088/0004-637X/812/1/43

2015 doi
[49]

A., Fu, H., Cooray, A., et al

Calanog, J. A., Fu, H., Cooray, A., et al. 2014, ApJ, 797, 138, doi: 10.1088/0004-637X/797/2/138

2014 doi
[50]

C., et al

Calzetti, D., Armus, L., Bohlin, R. C., et al. 2000, ApJ, 533, 682, doi: 10.1086/308692

2000 doi
[51]

J., Katz, H., Rey, M

Cameron, A. J., Katz, H., Rey, M. P., & Saxena, A. 2023, MNRAS, 523, 3516, doi: 10.1093/mnras/stad1579

2023 doi
[52]

L., Riechers, D., Scoville, N

Capak, P. L., Riechers, D., Scoville, N. Z., et al. 2011, Nature, 470, 233, doi: 10.1038/nature09681

2011 doi
[53]

L., Carilli, C., Jones, G., et al

Capak, P. L., Carilli, C., Jones, G., et al. 2015, Nature, 522, 455, doi: 10.1038/nature14500

2015 doi
[54]

L., Lewis, G

Carilli, C. L., Lewis, G. F., Djorgovski, S. G., et al. 2003, Science, 300, 773, doi: 10.1126/science.1082600

2003 doi
[55]

L., Riechers, D., Walter, F., et al

Carilli, C. L., Riechers, D., Walter, F., et al. 2013, ApJ, 763, 120, doi: 10.1088/0004-637X/763/2/120

2013 doi
[56]

L., & Walter, F

Carilli, C. L., & Walter, F. 2013, ARA&A, 51, 105, doi: 10.1146/annurev-astro-082812-140953

2013 doi
[57]

L., Daddi, E., Riechers, D., et al

Carilli, C. L., Daddi, E., Riechers, D., et al. 2010, ApJ, 714, 1407, doi: 10.1088/0004-637X/714/2/1407

2010 doi
[58]

2018a, ApJL, 854, L7, doi: 10.3847/2041-8213/aaab45

Carniani, S., Maiolino, R., Smit, R., & Amor ´ ın, R. 2018a, ApJL, 854, L7, doi: 10.3847/2041-8213/aaab45

doi
[59]

2013, A&A, 559, A29, doi: 10.1051/0004-6361/201322320

Carniani, S., Marconi, A., Biggs, A., et al. 2013, A&A, 559, A29, doi: 10.1051/0004-6361/201322320

2013 doi
[60]

2017, A&A, 605, A42, doi: 10.1051/0004-6361/201630366

Carniani, S., Maiolino, R., Pallottini, A., et al. 2017, A&A, 605, A42, doi: 10.1051/0004-6361/201630366

2017 doi
[61]

2018b, MNRAS, 478, 1170, doi: 10.1093/mnras/sty1088

Carniani, S., Maiolino, R., Amorin, R., et al. 2018b, MNRAS, 478, 1170, doi: 10.1093/mnras/sty1088

doi
[62]

2024, Nature, 633, 318, doi: 10.1038/s41586-024-07860-9

Carniani, S., Hainline, K., D’Eugenio, F., et al. 2024, Nature, 633, 318, doi: 10.1038/s41586-024-07860-9

2024 doi
[64]

2024, ApJ, 972, 143, doi: 10.3847/1538-4357/ad5f88

Castellano, M., Napolitano, L., Fontana, A., et al. 2024, ApJ, 972, 143, doi: 10.3847/1538-4357/ad5f88

2024 doi
[65]

H., Lower, S., et al

Cathey, J., Gonzalez, A. H., Lower, S., et al. 2024, ApJ, 967, 11, doi: 10.3847/1538-4357/ad33c9 FLAMES I: Low and High-z Catalogs and Empirical Relations 43

2024 doi
[66]

L., Pope, A., Scott, D., et al

Chapin, E. L., Pope, A., Scott, D., et al. 2009, MNRAS, 398, 1793, doi: 10.1111/j.1365-2966.2009.15267.x

2009
[67]

2022, Nature Astronomy, 6, 844, doi: 10.1038/s41550-022-01679-y

Chartab, N., Cooray, A., Ma, J., et al. 2022, Nature Astronomy, 6, 844, doi: 10.1038/s41550-022-01679-y

2022 doi
[68]

2020, ApJ, 898, 33, doi: 10.3847/1538-4357/ab980b

Cheng, C., Cao, X., Lu, N., et al. 2020, ApJ, 898, 33, doi: 10.3847/1538-4357/ab980b

2020 doi
[69]

2015, A&A, 574, A14, doi: 10.1051/0004-6361/201424980

Cicone, C., Maiolino, R., Gallerani, S., et al. 2015, A&A, 574, A14, doi: 10.1051/0004-6361/201424980

2015 doi
[70]

Clark, C. J. R., Schofield, S. P., Gomez, H. L., & Davies, J. I. 2016, MNRAS, 459, 1646, doi: 10.1093/mnras/stw647

2016 doi
[71]

Clark, C. J. R., Verstocken, S., Bianchi, S., et al. 2018, A&A, 609, A37, doi: 10.1051/0004-6361/201731419

2018 doi
[72]

E., Ade, P

Clegg, P. E., Ade, P. A. R., Armand, C., et al. 1996, A&A, 315, L38

1996
[73]

D., et al

Combes, F., Rex, M., Rawle, T. D., et al. 2012, A&A, 538, L4, doi: 10.1051/0004-6361/201118750

2012 doi
[74]

D., et al

Conley, A., Cooray, A., Vieira, J. D., et al. 2011, ApJL, 732, L35, doi: 10.1088/2041-8205/732/2/L35

2011 doi
[75]

Coppin, K. E. K., Danielson, A. L. R., Geach, J. E., et al. 2012, MNRAS, 427, 520, doi: 10.1111/j.1365-2966.2012.21977.x

2012
[76]

C., Lebouteiller, V., et al

Cormier, D., Madden, S. C., Lebouteiller, V., et al. 2015, A&A, 578, A53, doi: 10.1051/0004-6361/201425207

2015 doi
[77]

P., Hony, S., et al

Cormier, D., Abel, N. P., Hony, S., et al. 2019, A&A, 626, A23, doi: 10.1051/0004-6361/201834457

2019 doi
[78]

E., Valentino, F., et al

Cortzen, I., Magdis, G. E., Valentino, F., et al. 2020, A&A, 634, L14, doi: 10.1051/0004-6361/201937217

2020 doi
[79]

L., Hu, E

Cowie, L. L., Hu, E. M., & Songaila, A. 2011, ApJL, 735, L38, doi: 10.1088/2041-8205/735/2/L38

2011 doi
[80]

G., et al

Cox, P., Omont, A., Djorgovski, S. G., et al. 2002, A&A, 387, 406, doi: 10.1051/0004-6361:20020382

2002 doi
[81]

2011, ApJ, 740, 63, doi: 10.1088/0004-637X/740/2/63 Crespo G´ omez, A., Colina, L.,´Alvarez-M´ arquez, J., et al

Cox, P., Krips, M., Neri, R., et al. 2011, ApJ, 740, 63, doi: 10.1088/0004-637X/740/2/63 Crespo G´ omez, A., Colina, L.,´Alvarez-M´ arquez, J., et al. 2024, A&A, 691, A325, doi: 10.1051/0004-6361/202449750

2011 doi
[82]

V., Smith, J

Croxall, K. V., Smith, J. D., Pellegrini, E., et al. 2017, ApJ, 845, 96, doi: 10.3847/1538-4357/aa8035

2017 doi
[83]

Cunningham, D. J. M., Chapman, S. C., Aravena, M., et al. 2020, MNRAS, 494, 4090, doi: 10.1093/mnras/staa820

2020 doi
[84]

2017, MNRAS, 465, 1384, doi: 10.1093/mnras/stw2766

Curti, M., Cresci, G., Mannucci, F., et al. 2017, MNRAS, 465, 1384, doi: 10.1093/mnras/stw2766

2017 doi
[85]

2009, ApJ, 694, 1517, doi: 10.1088/0004-637X/694/2/1517

Daddi, E., Dannerbauer, H., Stern, D., et al. 2009, ApJ, 694, 1517, doi: 10.1088/0004-637X/694/2/1517

2009 doi
[86]

A., Aniano, G., Engelbracht, C

Dale, D. A., Aniano, G., Engelbracht, C. W., et al. 2012, ApJ, 745, 95, doi: 10.1088/0004-637X/745/1/95

2012 doi
[87]

2022, MNRAS, 512, 989, doi: 10.1093/mnras/stac537 De Breuck, C., Maiolino, R., Caselli, P., et al

Dayal, P., Ferrara, A., Sommovigo, L., et al. 2022, MNRAS, 512, 989, doi: 10.1093/mnras/stac537 De Breuck, C., Maiolino, R., Caselli, P., et al. 2011, A&A, 530, L8, doi: 10.1051/0004-6361/201116868 De Breuck, C., Bertoldi, F., Carilli, C., et al. 2004, A&A, 424, 1, doi: 10.105...

2022 doi
[88]

P., Rawlings, S., Garrett, M

Deane, R. P., Rawlings, S., Garrett, M. A., et al. 2013, MNRAS, 434, 3322, doi: 10.1093/mnras/stt1241

2013 doi
[89]

2012, ApJ, 752, 2, doi: 10.1088/0004-637X/752/1/2

Decarli, R., Walter, F., Neri, R., et al. 2012, ApJ, 752, 2, doi: 10.1088/0004-637X/752/1/2

2012 doi
[90]

2014, ApJL, 782, L17, doi: 10.1088/2041-8205/782/2/L17

Decarli, R., Walter, F., Carilli, C., et al. 2014, ApJL, 782, L17, doi: 10.1088/2041-8205/782/2/L17

2014 doi
[91]

P., et al

Decarli, R., Walter, F., Venemans, B. P., et al. 2017, Nature, 545, 457, doi: 10.1038/nature22358 —. 2018, ApJ, 854, 97, doi: 10.3847/1538-4357/aaa5aa

2017 doi
[92]

2022, A&A, 662, A60, doi: 10.1051/0004-6361/202142871

Decarli, R., Pensabene, A., Venemans, B., et al. 2022, A&A, 662, A60, doi: 10.1051/0004-6361/202142871

2022 doi
[94]

2015, A&A, 577, A50, doi: 10.1051/0004-6361/201424661 D’Eugenio, C., Daddi, E., Liu, D., & Gobat, R

Dessauges-Zavadsky, M., Zamojski, M., Schaerer, D., et al. 2015, A&A, 577, A50, doi: 10.1051/0004-6361/201424661 D’Eugenio, C., Daddi, E., Liu, D., & Gobat, R. 2023, A&A, 678, L9, doi: 10.1051/0004-6361/202347233 D ´ ıaz-Santos, T., Assef, R. J., Blain, A. W., et al. 2016, ApJ...

2015 doi
[95]

M., Adams, N

Diego, J. M., Adams, N. J., Willner, S. P., et al. 2024, A&A, 690, A114, doi: 10.1051/0004-6361/202349119

2024 doi
[96]

Dimaratos, A., Cormier, D., Bigiel, F., & Madden, S. C. 2015, A&A, 580, A135, doi: 10.1051/0004-6361/201526447

2015 doi
[97]

J., Geach, J

Doherty, M. J., Geach, J. E., Ivison, R. J., & Dye, S. 2020, ApJ, 905, 152, doi: 10.3847/1538-4357/abc5b9

2020 doi
[98]

A., Kewley, L

Dopita, M. A., Kewley, L. J., Heisler, C. A., & Sutherland, R. S. 2000, ApJ, 542, 224, doi: 10.1086/309538 44 Peng et al

2000 doi
[99]

J., & Shaver, P

Downes, D., Neri, R., Wiklind, T., Wilner, D. J., & Shaver, P. A. 1999a, ApJL, 513, L1, doi: 10.1086/311896

doi
[100]

1999b, A&A, 347, 809, doi: 10.48550/arXiv.astro-ph/9907139

Downes, D., Neri, R., Greve, A., et al. 1999b, A&A, 347, 809, doi: 10.48550/arXiv.astro-ph/9907139

doi arXiv
[101]

Draine, B. T. 2011, Physics of the Interstellar and Intergalactic Medium

2011
[102]

M., & Casey, C

Drew, P. M., & Casey, C. M. 2022, ApJ, 930, 142, doi: 10.3847/1538-4357/ac6270

2022 doi
[103]

2016, A&A, 593, A109, doi: 10.1051/0004-6361/201526880

Drouart, G., Rocca-Volmerange, B., De Breuck, C., et al. 2016, A&A, 593, A109, doi: 10.1051/0004-6361/201526880

2016 doi
[104]

2014, A&A, 566, A53, doi: 10.1051/0004-6361/201323310

Drouart, G., De Breuck, C., Vernet, J., et al. 2014, A&A, 566, A53, doi: 10.1051/0004-6361/201323310

2014 doi
[105]

J., Windhorst, R

Duncan, K. J., Windhorst, R. A., Koekemoer, A. M., et al. 2023, MNRAS, 522, 4548, doi: 10.1093/mnras/stad1267

2023 doi
[106]

A., Crone Odekon, M., et al

Durbala, A., Finn, R. A., Crone Odekon, M., et al. 2020, AJ, 160, 271, doi: 10.3847/1538-3881/abc018

2020 doi
[107]

F., Decarli, R., et al

Eilers, A.-C., Hennawi, J. F., Decarli, R., et al. 2020, ApJ, 900, 37, doi: 10.3847/1538-4357/aba52e

2020 doi
[108]

A., Yue, M., et al

Eilers, A.-C., Simcoe, R. A., Yue, M., et al. 2023, ApJ, 950, 68, doi: 10.3847/1538-4357/acd776

2023 doi
[109]

S., et al

Elbaz, D., Dickinson, M., Hwang, H. S., et al. 2011, A&A, 533, A119, doi: 10.1051/0004-6361/201117239 El ´ ıasd´ ottir,´A., Limousin, M., Richard, J., et al. 2007, arXiv e-prints, arXiv:0710.5636, doi: 10.48550/arXiv.0710.5636

2011 doi arXiv
[110]

P., Lyu, J., et al

Endsley, R., Stark, D. P., Lyu, J., et al. 2023, MNRAS, 520, 4609, doi: 10.1093/mnras/stad266

2023 doi
[111]

S., Solomon, P

Evans, A. S., Solomon, P. M., Tacconi, L. J., Vavilkin, T., & Downes, D. 2006, AJ, 132, 2398, doi: 10.1086/508416

2006 doi
[112]

S., Frayer, D

Evans, A. S., Frayer, D. T., Charmandaris, V., et al. 2022, ApJL, 940, L8, doi: 10.3847/2041-8213/ac9971

2022 doi
[113]

S., Baker, A

Fadely, R., Allam, S. S., Baker, A. J., et al. 2010, ApJ, 723, 729, doi: 10.1088/0004-637X/723/1/729

2010 doi
[114]

L., Fudamoto, Y., Oesch, P

Faisst, A. L., Fudamoto, Y., Oesch, P. A., et al. 2020, MNRAS, 498, 4192, doi: 10.1093/mnras/staa2545

2020 doi
[115]

D., et al

Falkendal, T., De Breuck, C., Lehnert, M. D., et al. 2019, A&A, 621, A27, doi: 10.1051/0004-6361/201732485

2019 doi
[116]

Farrah, D., Bernard-Salas, J., Spoon, H. W. W., et al. 2007, ApJ, 667, 149, doi: 10.1086/520834

2007 doi
[117]

Farrah, D., Lebouteiller, V., Spoon, H. W. W., et al. 2013, ApJ, 776, 38, doi: 10.1088/0004-637X/776/1/38

2013 doi
[118]

G., Hora, J

Fazio, G. G., Hora, J. L., Allen, L. E., et al. 2004, ApJS, 154, 10, doi: 10.1086/422843

2004 doi
[119]

2015, ApJ, 806, 260, doi: 10.1088/0004-637X/806/2/260

Ferkinhoff, C., Brisbin, D., Nikola, T., et al. 2015, ApJ, 806, 260, doi: 10.1088/0004-637X/806/2/260

2015 doi
[120]

2010, ApJL, 714, L147, doi: 10.1088/2041-8205/714/1/L147

Ferkinhoff, C., Hailey-Dunsheath, S., Nikola, T., et al. 2010, ApJL, 714, L147, doi: 10.1088/2041-8205/714/1/L147

2010 doi
[121]

2011, ApJL, 740, L29, doi: 10.1088/2041-8205/740/1/L29 Fern´ andez Aranda, R., D ´ ıaz Santos, T., Hatziminaoglou, E., et al

Ferkinhoff, C., Brisbin, D., Nikola, T., et al. 2011, ApJL, 740, L29, doi: 10.1088/2041-8205/740/1/L29 Fern´ andez Aranda, R., D ´ ıaz Santos, T., Hatziminaoglou, E., et al. 2024, A&A, 682, A166, doi: 10.1051/0004-6361/202347869 Fern´ andez-Ontiveros, J. A., Spinoglio, L., Per...

2011 doi
[122]

L., Papovich, C., Rudnick, G., et al

Finkelstein, S. L., Papovich, C., Rudnick, G., et al. 2009, ApJ, 700, 376, doi: 10.1088/0004-637X/700/1/376

2009 doi
[123]

2018, Journal of Astronomical Instrumentation, 7, 1840003, doi: 10.1142/S2251171718400032

Fischer, C., Beckmann, S., Bryant, A., et al. 2018, Journal of Astronomical Instrumentation, 7, 1840003, doi: 10.1142/S2251171718400032

2018 doi
[124]

P., Gonz´ alez-Alfonso, E., et al

Fischer, J., Abel, N. P., Gonz´ alez-Alfonso, E., et al. 2014, ApJ, 795, 117, doi: 10.1088/0004-637X/795/2/117 F¨ orster Schreiber, N. M., Genzel, R., Bouch´ e, N., et al. 2009, ApJ, 706, 1364, doi: 10.1088/0004-637X/706/2/1364

2014 doi
[125]

2021, A&A, 647, A194, doi: 10.1051/0004-6361/202039807

Fraternali, F., Karim, A., Magnelli, B., et al. 2021, A&A, 647, A194, doi: 10.1051/0004-6361/202039807

2021 doi
[126]

T., Ivison, R

Frayer, D. T., Ivison, R. J., Scoville, N. Z., et al. 1998, ApJL, 506, L7, doi: 10.1086/311639 —. 1999, ApJL, 514, L13, doi: 10.1086/311940

1998 doi
[127]

2012, ApJ, 753, 134, doi: 10.1088/0004-637X/753/2/134

Fu, H., Jullo, E., Cooray, A., et al. 2012, ApJ, 753, 134, doi: 10.1088/0004-637X/753/2/134

2012 doi
[128]

2013, Nature, 498, 338, doi: 10.1038/nature12184

Fu, H., Cooray, A., Feruglio, C., et al. 2013, Nature, 498, 338, doi: 10.1038/nature12184

2013 doi
[129]

A., Schouws, S., et al

Fudamoto, Y., Oesch, P. A., Schouws, S., et al. 2021, Nature, 597, 489, doi: 10.1038/s41586-021-03846-z

2021 doi
[130]

K., Coe, D., et al

Fudamoto, Y., Inoue, A. K., Coe, D., et al. 2024a, ApJ, 961, 71, doi: 10.3847/1538-4357/ad0f95

doi
[131]

A., Walter, F., et al

Fudamoto, Y., Oesch, P. A., Walter, F., et al. 2024b, MNRAS, 530, 340, doi: 10.1093/mnras/stae556

doi
[132]

K., Bouwens, R., et al

Fudamoto, Y., Inoue, A. K., Bouwens, R., et al. 2025, arXiv e-prints, arXiv:2504.03831, doi: 10.48550/arXiv.2504.03831

2025 doi arXiv
[133]

2019, ApJ, 887, 107, doi: 10.3847/1538-4357/ab480f

Fujimoto, S., Ouchi, M., Ferrara, A., et al. 2019, ApJ, 887, 107, doi: 10.3847/1538-4357/ab480f

2019 doi
[134]

2021, ApJ, 911, 99, doi: 10.3847/1538-4357/abd7ec

Fujimoto, S., Oguri, M., Brammer, G., et al. 2021, ApJ, 911, 99, doi: 10.3847/1538-4357/abd7ec

2021 doi
[135]

B., Watson, D., et al

Fujimoto, S., Brammer, G. B., Watson, D., et al. 2022, Nature, 604, 261, doi: 10.1038/s41586-022-04454-1

2022 doi
[136]

2024a, ApJ, 964, 146, doi: 10.3847/1538-4357/ad235c

Fujimoto, S., Ouchi, M., Nakajima, K., et al. 2024a, ApJ, 964, 146, doi: 10.3847/1538-4357/ad235c

doi
[137]

2024b, arXiv e-prints, arXiv:2402.18543, doi: 10.48550/arXiv.2402.18543

Fujimoto, S., Ouchi, M., Kohno, K., et al. 2024b, arXiv e-prints, arXiv:2402.18543, doi: 10.48550/arXiv.2402.18543

doi arXiv
[138]

2025, ApJS, 278, 45, doi: 10.3847/1538-4365/adc677

Fujimoto, S., Bezanson, R., Labbe, I., et al. 2025, ApJS, 278, 45, doi: 10.3847/1538-4365/adc677

2025 doi
[139]

2012, A&A, 543, A114, doi: 10.1051/0004-6361/201118705 FLAMES I: Low and High-z Catalogs and Empirical Relations 45

Gallerani, S., Neri, R., Maiolino, R., et al. 2012, A&A, 543, A114, doi: 10.1051/0004-6361/201118705 FLAMES I: Low and High-z Catalogs and Empirical Relations 45

2012 doi
[140]

2011, ApJ, 738, 125, doi: 10.1088/0004-637X/738/2/125

Gavazzi, R., Cooray, A., Conley, A., et al. 2011, ApJ, 738, 125, doi: 10.1088/0004-637X/738/2/125

2011 doi
[141]

E., Narayanan, D., Matsuda, Y., et al

Geach, J. E., Narayanan, D., Matsuda, Y., et al. 2016, ApJ, 832, 37, doi: 10.3847/0004-637X/832/1/37

2016 doi
[142]

I., & Stutzki, J

Genzel, R., Harris, A. I., & Stutzki, J. 1989, in Infrared Spectroscopy in Astronomy, ed. E. B¨ ohm-Vitense, 115

1989
[143]

1998, ApJ, 498, 579, doi: 10.1086/305576

Genzel, R., Lutz, D., Sturm, E., et al. 1998, ApJ, 498, 579, doi: 10.1086/305576

1998 doi
[144]

D., Ivison, R

George, R. D., Ivison, R. J., Hopwood, R., et al. 2013, MNRAS, 436, L99, doi: 10.1093/mnrasl/slt122 Gim´ enez-Arteaga, C., Fujimoto, S., Valentino, F., et al. 2024, A&A, 686, A63, doi: 10.1051/0004-6361/202349135

2013 doi
[145]

C., B´ ethermin, M., et al

Ginolfi, M., Jones, G. C., B´ ethermin, M., et al. 2020, A&A, 643, A7, doi: 10.1051/0004-6361/202038284

2020 doi
[146]

2023, ApJ, 943, 151, doi: 10.3847/1538-4357/aca53f

Giulietti, M., Lapi, A., Massardi, M., et al. 2023, ApJ, 943, 151, doi: 10.3847/1538-4357/aca53f

2023 doi
[147]

L., et al

Glazer, K., Brad˘ ac, M., Sanders, R. L., et al. 2024, MNRAS, 531, 945, doi: 10.1093/mnras/stae1178 G´ omez-Guijarro, C., Toft, S., Karim, A., et al. 2018, ApJ, 856, 121, doi: 10.3847/1538-4357/aab206 Gonz´ alez-L´ opez, J., Bauer, F. E., Romero-Ca˜ nizales, C., et al. 2017, A...

2024 doi
[148]

W., & Lawrence, C

Gorjian, V., Cleary, K., Werner, M. W., & Lawrence, C. R. 2007, ApJL, 655, L73, doi: 10.1086/511975

2007 doi
[149]

J., Abergel, A., Abreu, A., et al

Griffin, M. J., Abergel, A., Abreu, A., et al. 2010, A&A, 518, L3, doi: 10.1051/0004-6361/201014519

2010 doi
[150]

2020, A&A, 643, A8, doi: 10.1051/0004-6361/202038487

Gruppioni, C., B´ ethermin, M., Loiacono, F., et al. 2020, A&A, 643, A8, doi: 10.1051/0004-6361/202038487

2020 doi
[151]

D., et al

Gullberg, B., De Breuck, C., Vieira, J. D., et al. 2015, MNRAS, 449, 2883, doi: 10.1093/mnras/stv372

2015 doi
[152]

M., Smail, I., et al

Gullberg, B., Swinbank, A. M., Smail, I., et al. 2018, ApJ, 859, 12, doi: 10.3847/1538-4357/aabe8c

2018 doi
[153]

2023, A&A, 676, A89, doi: 10.1051/0004-6361/202346449 G¨ usten, R., Nyman, L.˚A., Schilke, P., et al

Gururajan, G., Bethermin, M., Sulzenauer, N., et al. 2023, A&A, 676, A89, doi: 10.1051/0004-6361/202346449 G¨ usten, R., Nyman, L.˚A., Schilke, P., et al. 2006, A&A, 454, L13, doi: 10.1051/0004-6361:20065420

2023 doi
[154]

J., et al

Hailey-Dunsheath, S., Nikola, T., Stacey, G. J., et al. 2010, ApJL, 714, L162, doi: 10.1088/2041-8205/714/1/L162

2010 doi
[155]

N., Shapley, A

Hainline, K. N., Shapley, A. E., Kornei, K. A., et al. 2009, ApJ, 701, 52, doi: 10.1088/0004-637X/701/1/52

2009 doi
[156]

K., et al

Harikane, Y., Ouchi, M., Inoue, A. K., et al. 2020, ApJ, 896, 93, doi: 10.3847/1538-4357/ab94bd

2020 doi
[157]

L., Ellis, R., et al

Harikane, Y., Sanders, R. L., Ellis, R., et al. 2025, arXiv e-prints, arXiv:2505.09186, doi: 10.48550/arXiv.2505.09186

2025 doi
[158]

C., Vishwas, A., Weiß, A., et al

Harrington, K. C., Vishwas, A., Weiß, A., et al. 2019, MNRAS, 488, 1489, doi: 10.1093/mnras/stz1740

2019 doi
[159]

I., Baker, A

Harris, A. I., Baker, A. J., Frayer, D. T., et al. 2012, ApJ, 752, 152, doi: 10.1088/0004-637X/752/2/152

2012 doi
[160]

S., et al

Harshan, A., Tripodi, R., Martis, N. S., et al. 2024, ApJL, 977, L36, doi: 10.3847/2041-8213/ad9741

2024 doi
[161]

K., Tamura, Y., et al

Hashimoto, T., Inoue, A. K., Tamura, Y., et al. 2019a, PASJ, 71, 109, doi: 10.1093/pasj/psz094

doi
[162]

2018, Nature, 557, 392, doi: 10.1038/s41586-018-0117-z

Hashimoto, T., Laporte, N., Mawatari, K., et al. 2018, Nature, 557, 392, doi: 10.1038/s41586-018-0117-z

2018 doi
[163]

K., Mawatari, K., et al

Hashimoto, T., Inoue, A. K., Mawatari, K., et al. 2019b, PASJ, 71, 71, doi: 10.1093/pasj/psz049

doi
[164]

2023, ApJL, 955, L2, doi: 10.3847/2041-8213/acf57c

Hashimoto, T., ´Alvarez-M´ arquez, J., Fudamoto, Y., et al. 2023, ApJL, 955, L2, doi: 10.3847/2041-8213/acf57c

2023 doi
[165]

2015, PASJ, 67, 93, doi: 10.1093/pasj/psv061

Hatsukade, B., Tamura, Y., Iono, D., et al. 2015, PASJ, 67, 93, doi: 10.1093/pasj/psv061

2015 doi
[166]

P., Giovanelli, R., Kent, B

Haynes, M. P., Giovanelli, R., Kent, B. R., et al. 2018, ApJ, 861, 49, doi: 10.3847/1538-4357/aac956

2018 doi
[167]

Madden, S. C. 2021, ApJ, 922, 147, doi: 10.3847/1538-4357/ac2231

2021 doi
[168]

E., Gim´ enez-Arteaga, C., Fujimoto, S., et al

Heintz, K. E., Gim´ enez-Arteaga, C., Fujimoto, S., et al. 2023, ApJL, 944, L30, doi: 10.3847/2041-8213/acb2cf

2023 doi
[169]

1986, ApJL, 311, L33, doi: 10.1086/184793

Helou, G. 1986, ApJL, 311, L33, doi: 10.1086/184793

1986 doi
[170]

J., Oesch, P

Herard-Demanche, T., Bouwens, R. J., Oesch, P. A., et al. 2025, MNRAS, 537, 788, doi: 10.1093/mnras/staf030

2025 doi
[171]

D., Wolfire, M

Herrera-Camus, R., Bolatto, A. D., Wolfire, M. G., et al. 2015, ApJ, 800, 1, doi: 10.1088/0004-637X/800/1/1

2015 doi
[172]

D., et al

Herrera-Camus, R., Bolatto, A., Smith, J. D., et al. 2016, ApJ, 826, 175, doi: 10.3847/0004-637X/826/2/175

2016 doi
[173]

2018, ApJ, 861, 94, doi: 10.3847/1538-4357/aac0f6

Herrera-Camus, R., Sturm, E., Graci´ a-Carpio, J., et al. 2018, ApJ, 861, 94, doi: 10.3847/1538-4357/aac0f6

2018 doi
[174]

2021, A&A, 649, A31, doi: 10.1051/0004-6361/202039704

Herrera-Camus, R., F¨ orster Schreiber, N., Genzel, R., et al. 2021, A&A, 649, A31, doi: 10.1051/0004-6361/202039704

2021 doi
[175]

M., Price, S

Herrera-Camus, R., F¨ orster Schreiber, N. M., Price, S. H., et al. 2022, A&A, 665, L8, doi: 10.1051/0004-6361/202142562

2022 doi
[176]

2013, ApJS, 208, 19, doi: 10.1088/0067-0049/208/2/19

Hinshaw, G., Larson, D., Komatsu, E., et al. 2013, ApJS, 208, 19, doi: 10.1088/0067-0049/208/2/19

2013 doi
[177]

Ho, L. C. 2007, ApJ, 669, 821, doi: 10.1086/521917

2007 doi
[178]

2011, ApJL, 728, L4, doi: 10.1088/2041-8205/728/1/L4

Hopwood, R., Wardlow, J., Cooray, A., et al. 2011, ApJL, 728, L4, doi: 10.1088/2041-8205/728/1/L4

2011 doi
[179]

R., Roellig, T

Houck, J. R., Roellig, T. L., Van Cleve, J., et al. 2004, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 5487, Optical, Infrared, and Millimeter Space Telescopes, ed. J. C. Mather, 62–76, doi: 10.1117/12.550517

2004 doi
[180]

H., Armus, L., Mazzarella, J

Howell, J. H., Armus, L., Mazzarella, J. M., et al. 2010, ApJ, 715, 572, doi: 10.1088/0004-637X/715/1/572

2010 doi
[181]

C., et al

Huang, K.-H., Bradaˇ c, M., Lemaux, B. C., et al. 2016, ApJ, 817, 11, doi: 10.3847/0004-637X/817/1/11

2016 doi
[182]

M., Baes, M., Schirm, M

Hughes, T. M., Baes, M., Schirm, M. R. P., et al. 2016, A&A, 587, A45, doi: 10.1051/0004-6361/201527644 46 Peng et al

2016 doi
[183]

Hygate, A. P. S., Hodge, J. A., da Cunha, E., et al. 2023, MNRAS, 524, 1775, doi: 10.1093/mnras/stad1212

2023 doi
[184]

2021, MNRAS, 507, 3830, doi: 10.1093/mnras/stab2376

Iani, E., Zanella, A., Vernet, J., et al. 2021, MNRAS, 507, 3830, doi: 10.1093/mnras/stab2376

2021 doi
[185]

2025, A&A, 693, A237, doi: 10.1051/0004-6361/202451811

Ikeda, R., Tadaki, K.-i., Mitsuhashi, I., et al. 2025, A&A, 693, A237, doi: 10.1051/0004-6361/202451811

2025 doi
[186]

2013, ApJ, 777, 156, doi: 10.1088/0004-637X/777/2/156

Inami, H., Armus, L., Charmandaris, V., et al. 2013, ApJ, 777, 156, doi: 10.1088/0004-637X/777/2/156

2013 doi
[187]

Inami, H., Algera, H. S. B., Schouws, S., et al. 2022a, MNRAS, 515, 3126, doi: 10.1093/mnras/stac1779

doi
[188]

2022b, ApJL, 940, L6, doi: 10.3847/2041-8213/ac9389

Inami, H., Surace, J., Armus, L., et al. 2022b, ApJL, 940, L6, doi: 10.3847/2041-8213/ac9389

doi
[189]

K., Hashimoto, T., Chihara, H., & Koike, C

Inoue, A. K., Hashimoto, T., Chihara, H., & Koike, C. 2020, MNRAS, 495, 1577, doi: 10.1093/mnras/staa1203

2020 doi
[190]

K., Tamura, Y., Matsuo, H., et al

Inoue, A. K., Tamura, Y., Matsuo, H., et al. 2016, Science, 352, 1559, doi: 10.1126/science.aaf0714

2016 doi
[191]

S., Elvis, M., et al

Iono, D., Yun, M. S., Elvis, M., et al. 2006, ApJL, 645, L97, doi: 10.1086/506344

2006 doi
[192]

S., Aretxaga, I., et al

Iono, D., Yun, M. S., Aretxaga, I., et al. 2016, ApJL, 829, L10, doi: 10.3847/2041-8205/829/1/L10

2016 doi
[193]

G., Priddey, R

Isaak, K. G., Priddey, R. S., McMahon, R. G., et al. 2002, MNRAS, 329, 149, doi: 10.1046/j.1365-8711.2002.04966.x

2002
[194]

2025, PASJ, 77, 139, doi: 10.1093/pasj/psae105

Ishii, N., Hashimoto, T., Ferkinhoff, C., et al. 2025, PASJ, 77, 139, doi: 10.1093/pasj/psae105

2025 doi
[195]

P., Rosenberg, M

Israel, F. P., Rosenberg, M. J. F., & van der Werf, P. 2015, A&A, 578, A95, doi: 10.1051/0004-6361/201425175

2015 doi
[197]

J., Swinbank, A

Ivison, R. J., Swinbank, A. M., Swinyard, B., et al. 2010b, A&A, 518, L35, doi: 10.1051/0004-6361/201014548

doi
[198]

J., Swinbank, A

Ivison, R. J., Swinbank, A. M., Smail, I., et al. 2013, ApJ, 772, 137, doi: 10.1088/0004-637X/772/2/137

2013 doi
[199]

J., Lewis, A

Ivison, R. J., Lewis, A. J. R., Weiss, A., et al. 2016, ApJ, 832, 78, doi: 10.3847/0004-637X/832/1/78

2016 doi
[200]

2018, PASJ, 70, 36, doi: 10.1093/pasj/psy026

Izumi, T., Onoue, M., Shirakata, H., et al. 2018, PASJ, 70, 36, doi: 10.1093/pasj/psy026

2018 doi
[201]

2019, PASJ, 71, 111, doi: 10.1093/pasj/psz096 —

Izumi, T., Onoue, M., Matsuoka, Y., et al. 2019, PASJ, 71, 111, doi: 10.1093/pasj/psz096 —. 2021a, ApJ, 908, 235, doi: 10.3847/1538-4357/abd7ef

2019 doi
[202]

2021b, ApJ, 914, 36, doi: 10.3847/1538-4357/abf6dc

Izumi, T., Matsuoka, Y., Fujimoto, S., et al. 2021b, ApJ, 914, 36, doi: 10.3847/1538-4357/abf6dc

doi
[203]

2022, A&A, 661, A80, doi: 10.1051/0004-6361/202142663

Jakobsen, P., Ferruit, P., Alves de Oliveira, C., et al. 2022, A&A, 661, A80, doi: 10.1051/0004-6361/202142663

2022 doi
[204]

2024, MNRAS, 535, 881, doi: 10.1093/mnras/stae2375 Jim´ enez-Andrade, E

Ji, X., ¨Ubler, H., Maiolino, R., et al. 2024, MNRAS, 535, 881, doi: 10.1093/mnras/stae2375 Jim´ enez-Andrade, E. F., Zavala, J. A., Magnelli, B., et al. 2020, ApJ, 890, 171, doi: 10.3847/1538-4357/ab6dec

2024 doi
[205]

2017a, A&A, 602, A46, doi: 10.1051/0004-6361/201630225

Verstraete, L. 2017a, A&A, 602, A46, doi: 10.1051/0004-6361/201630225

doi
[206]

C., Willott, C

Jones, G. C., Willott, C. J., Carilli, C. L., et al. 2017b, ApJ, 845, 175, doi: 10.3847/1538-4357/aa7d0d

doi
[207]

C., ¨Ubler, H., Perna, M., et al

Jones, G. C., ¨Ubler, H., Perna, M., et al. 2024a, A&A, 682, A122, doi: 10.1051/0004-6361/202347838

doi
[208]

C., Bowler, R., Bunker, A

Jones, G. C., Bowler, R., Bunker, A. J., et al. 2024b, arXiv e-prints, arXiv:2412.15027, doi: 10.48550/arXiv.2412.15027

doi
[209]

C., Bunker, A

Jones, G. C., Bunker, A. J., Telikova, K., et al. 2025, MNRAS, 540, 3311, doi: 10.1093/mnras/staf899

2025 doi
[210]

2010a, ApJL, 725, L176, doi: 10.1088/2041-8205/725/2/L176

Jones, T., Ellis, R., Jullo, E., & Richard, J. 2010a, ApJL, 725, L176, doi: 10.1088/2041-8205/725/2/L176

doi
[211]

Stark, D. P. 2010b, MNRAS, 404, 1247, doi: 10.1111/j.1365-2966.2010.16378.x

2010
[212]

K., Vlemmings, W., et al

Kade, K., Knudsen, K. K., Vlemmings, W., et al. 2023, A&A, 673, A116, doi: 10.1051/0004-6361/202141839

2023 doi
[213]

R., & Conley, A

Kamenetzky, J., Rangwala, N., Glenn, J., Maloney, P. R., & Conley, A. 2016, ApJ, 829, 93, doi: 10.3847/0004-637X/829/2/93

2016 doi
[214]

R., & Carilli, C

Kanekar, N., Wagg, J., Chary, R. R., & Carilli, C. L. 2013, ApJL, 771, L20, doi: 10.1088/2041-8205/771/2/L20

2013 doi
[215]

J., et al

Kashikawa, N., Ishizaki, Y., Willott, C. J., et al. 2015, ApJ, 798, 28, doi: 10.1088/0004-637X/798/1/28

2015 doi
[216]

J., Simcoe, R

Kashino, D., Lilly, S. J., Simcoe, R. A., et al. 2023, Nature, 617, 261, doi: 10.1038/s41586-023-05901-3

2023 doi
[217]

2020, PASJ, 72, 84, doi: 10.1093/pasj/psaa074

Kato, N., Matsuoka, Y., Onoue, M., et al. 2020, PASJ, 72, 84, doi: 10.1093/pasj/psaa074

2020 doi
[218]

Luhman, M. L. 1999, ApJ, 527, 795, doi: 10.1086/308102

1999 doi
[219]

2009, ApJ, 703, 1672, doi: 10.1088/0004-637X/703/2/1672

Kennicutt, Robert C., J., Hao, C.-N., Calzetti, D., et al. 2009, ApJ, 703, 1672, doi: 10.1088/0004-637X/703/2/1672

2009 doi
[220]

C., Calzetti, D., Aniano, G., et al

Kennicutt, R. C., Calzetti, D., Aniano, G., et al. 2011, PASP, 123, 1347, doi: 10.1086/663818

2011 doi
[221]

F., Steinz, J

Kessler, M. F., Steinz, J. A., Anderegg, M. E., et al. 1996, A&A, 315, L27

1996
[222]

J., & Dopita, M

Kewley, L. J., & Dopita, M. A. 2002, ApJS, 142, 35, doi: 10.1086/341326

2002 doi
[223]

J., Groves, B., Kauffmann, G., & Heckman, T

Kewley, L. J., Groves, B., Kauffmann, G., & Heckman, T. 2006, MNRAS, 372, 961, doi: 10.1111/j.1365-2966.2006.10859.x

2006
[224]

J., Nicholls, D

Kewley, L. J., Nicholls, D. C., & Sutherland, R. S. 2019, ARA&A, 57, 511, doi: 10.1146/annurev-astro-081817-051832

2019 doi
[225]

2022, A&A, 664, A39, doi: 10.1051/0004-6361/202243660

Khusanova, Y., Ba˜ nados, E., Mazzucchelli, C., et al. 2022, A&A, 664, A39, doi: 10.1051/0004-6361/202243660

2022 doi
[226]

2023, MNRAS, 521, 2526, doi: 10.1093/mnras/stad687

Killi, M., Watson, D., Fujimoto, S., et al. 2023, MNRAS, 521, 2526, doi: 10.1093/mnras/stad687

2023 doi
[227]

E., Lacy, M., Lonsdale, C

Kimball, A. E., Lacy, M., Lonsdale, C. J., & Macquart, J. P. 2015, MNRAS, 452, 88, doi: 10.1093/mnras/stv1160 FLAMES I: Low and High-z Catalogs and Empirical Relations 47

2015 doi
[228]

2025, arXiv e-prints, arXiv:2504.03156, doi: 10.48550/arXiv.2504.03156

Kiyota, T., Ouchi, M., Xu, Y., et al. 2025, arXiv e-prints, arXiv:2504.03156, doi: 10.48550/arXiv.2504.03156

2025 doi
[229]

P., Mellier, Y., Fort, B., & Mathez, G

Kneib, J. P., Mellier, Y., Fort, B., & Mathez, G. 1993, A&A, 273, 367

1993
[230]

K., Richard, J., Kneib, J.-P., et al

Knudsen, K. K., Richard, J., Kneib, J.-P., et al. 2016, MNRAS, 462, L6, doi: 10.1093/mnrasl/slw114

2016 doi
[231]

K., Watson, D., Frayer, D., et al

Knudsen, K. K., Watson, D., Frayer, D., et al. 2017, MNRAS, 466, 138, doi: 10.1093/mnras/stw3066

2017 doi
[232]

P., Gladders, M

Koester, B. P., Gladders, M. D., Hennawi, J. F., et al. 2010, ApJL, 723, L73, doi: 10.1088/2041-8205/723/1/L73

2010 doi
[233]

2025, A&A, 695, A201, doi: 10.1051/0004-6361/202452374 K¨ onig, S., Greve, T

Kolupuri, S., Decarli, R., Neri, R., et al. 2025, A&A, 695, A201, doi: 10.1051/0004-6361/202452374 K¨ onig, S., Greve, T. R., Seymour, N., et al. 2012, in Journal of Physics Conference Series, Vol. 372, Journal of Physics Conference Series (IOP), 012064, doi: 10.1088/1742-6596...

2025 doi
[234]

S., Staveley-Smith, L., Kilborn, V

Koribalski, B. S., Staveley-Smith, L., Kilborn, V. A., et al. 2004, AJ, 128, 16, doi: 10.1086/421744

2004 doi
[235]

2015, ApJ, 799, 38, doi: 10.1088/0004-637X/799/1/38

Kubo, M., Yamada, T., Ichikawa, T., et al. 2015, ApJ, 799, 38, doi: 10.1088/0004-637X/799/1/38

2015 doi
[236]

J., Vishwas, A., et al

Lamarche, C., Stacey, G. J., Vishwas, A., et al. 2019, ApJ, 882, 1, doi: 10.3847/1538-4357/ab3389

2019 doi
[237]

2018, ApJ, 867, 140, doi: 10.3847/1538-4357/aae394

Lamarche, C., Verma, A., Vishwas, A., et al. 2018, ApJ, 867, 140, doi: 10.3847/1538-4357/aae394

2018 doi
[238]

D., Kreckel, K., et al

Lamarche, C., Smith, J. D., Kreckel, K., et al. 2022, ApJ, 925, 194, doi: 10.3847/1538-4357/ac3b4f

2022 doi
[239]

S., Posses, A., Aravena, M., et al

Lambert, T. S., Posses, A., Aravena, M., et al. 2023, MNRAS, 518, 3183, doi: 10.1093/mnras/stac3016

2023 doi
[240]

C., Young, L

Lapham, R. C., Young, L. M., & Crocker, A. 2017, ApJ, 840, 51, doi: 10.3847/1538-4357/aa6d83

2017 doi
[241]

A., Ellis, R

Laporte, N., Meyer, R. A., Ellis, R. S., et al. 2021a, MNRAS, 505, 3336, doi: 10.1093/mnras/stab1239

doi
[242]

S., Boone, F., et al

Laporte, N., Ellis, R. S., Boone, F., et al. 2017, ApJL, 837, L21, doi: 10.3847/2041-8213/aa62aa

2017 doi
[243]

S., et al

Laporte, N., Katz, H., Ellis, R. S., et al. 2019, MNRAS, 487, L81, doi: 10.1093/mnrasl/slz094

2019 doi
[244]

S., et al

Laporte, N., Zitrin, A., Ellis, R. S., et al. 2021b, MNRAS, 505, 4838, doi: 10.1093/mnras/stab191 Le F` evre, O., B´ ethermin, M., Faisst, A., et al. 2020, A&A, 643, A1, doi: 10.1051/0004-6361/201936965

2020 doi
[245]

2024, ApJ, 972, 111, doi: 10.3847/1538-4357/ad5be5

Lee, K., Akiyama, M., Kohno, K., et al. 2024, ApJ, 972, 111, doi: 10.3847/1538-4357/ad5be5

2024 doi
[246]

M., Nagao, T., De Breuck, C., et al

Lee, M. M., Nagao, T., De Breuck, C., et al. 2019, ApJL, 883, L29, doi: 10.3847/2041-8213/ab412e —. 2021, ApJ, 913, 41, doi: 10.3847/1538-4357/abe7ea

2019 doi
[247]

M., Fraternali, F., et al

Lelli, F., Di Teodoro, E. M., Fraternali, F., et al. 2021, Science, 371, 713, doi: 10.1126/science.abc1893 Le´ sniewska, A., & Micha lowski, M. J. 2019, A&A, 624, L13, doi: 10.1051/0004-6361/201935149

2021 doi
[248]

F., Dinerstein, H

Lester, D. F., Dinerstein, H. L., Werner, M. W., Watson, D. M., & Genzel, R. L. 1983, ApJ, 271, 618, doi: 10.1086/161229

1983 doi
[249]

L., Thanjavur, K., et al

Lestrade, J.-F., Carilli, C. L., Thanjavur, K., et al. 2011, ApJL, 739, L30, doi: 10.1088/2041-8205/739/1/L30

2011 doi
[250]

F., Combes, F., Salom´ e, P., et al

Lestrade, J. F., Combes, F., Salom´ e, P., et al. 2010, A&A, 522, L4, doi: 10.1051/0004-6361/201015673

2010 doi
[251]

P., Walter, F., et al

Li, J., Venemans, B. P., Walter, F., et al. 2022, ApJ, 930, 27, doi: 10.3847/1538-4357/ac61d7

2022 doi
[252]

2020, ApJ, 900, 131, doi: 10.3847/1538-4357/ababac

Li, J., Wang, R., Cox, P., et al. 2020, ApJ, 900, 131, doi: 10.3847/1538-4357/ababac

2020 doi
[253]

2024, ApJ, 976, 70, doi: 10.3847/1538-4357/ad7fee

Li, J., Da Cunha, E., Gonz´ alez-L´ opez, J., et al. 2024, ApJ, 976, 70, doi: 10.3847/1538-4357/ad7fee

2024 doi
[254]

S., et al

Lin, H., Buckley-Geer, E., Allam, S. S., et al. 2009, ApJ, 699, 1242, doi: 10.1088/0004-637X/699/2/1242

2009 doi
[255]

C., Marrone, D

Litke, K. C., Marrone, D. P., Spilker, J. S., et al. 2019, ApJ, 870, 80, doi: 10.3847/1538-4357/aaf057

2019 doi
[256]

C., Marrone, D

Litke, K. C., Marrone, D. P., Aravena, M., et al. 2022, ApJ, 928, 179, doi: 10.3847/1538-4357/ac58f9 —. 2023, ApJ, 949, 87, doi: 10.3847/1538-4357/acc93a

2022 doi
[257]

2019, ApJS, 244, 40, doi: 10.3847/1538-4365/ab42da

Liu, D., Lang, P., Magnelli, B., et al. 2019, ApJS, 244, 40, doi: 10.3847/1538-4365/ab42da

2019 doi
[258]

2024, ApJ, 976, 33, doi: 10.3847/1538-4357/ad7de4

Liu, W., Fan, X., Yang, J., et al. 2024, ApJ, 976, 33, doi: 10.3847/1538-4357/ad7de4

2024 doi
[259]

C., Jones, T

Livermore, R. C., Jones, T. A., Richard, J., et al. 2015, MNRAS, 450, 1812, doi: 10.1093/mnras/stv686

2015 doi
[260]

2024, A&A, 685, A121, doi: 10.1051/0004-6361/202348535

Loiacono, F., Decarli, R., Mignoli, M., et al. 2024, A&A, 685, A121, doi: 10.1051/0004-6361/202348535

2024 doi
[261]

2017a, ApJS, 230, 1, doi: 10.3847/1538-4365/aa6476 —

Lu, N., Zhao, Y., D ´ ıaz-Santos, T., et al. 2017a, ApJS, 230, 1, doi: 10.3847/1538-4365/aa6476 —. 2017b, ApJL, 842, L16, doi: 10.3847/2041-8213/aa77fc

doi
[262]

2018, ApJ, 864, 38, doi: 10.3847/1538-4357/aad3c9

Lu, N., Cao, T., D ´ ıaz-Santos, T., et al. 2018, ApJ, 864, 38, doi: 10.3847/1538-4357/aad3c9

2018 doi
[263]

Luridiana, V., Morisset, C., & Shaw, R. A. 2015, A&A, 573, A42, doi: 10.1051/0004-6361/201323152

2015 doi
[264]

J., et al

Lutz, D., Sturm, E., Tacconi, L. J., et al. 2007, ApJL, 661, L25, doi: 10.1086/518537

2007 doi
[265]

H., Spilker, J

Ma, J., Gonzalez, A. H., Spilker, J. S., et al. 2015, ApJ, 812, 88, doi: 10.1088/0004-637X/812/1/88

2015 doi
[266]

2024, ApJ, 975, 87, doi: 10.3847/1538-4357/ad7b32

Ma, Z., Sun, B., Cheng, C., et al. 2024, ApJ, 975, 87, doi: 10.3847/1538-4357/ad7b32

2024 doi
[267]

2014, ARA&A, 52, 415, doi: 10.1146/annurev-astro-081811-125615

Madau, P., & Dickinson, M. 2014, ARA&A, 52, 415, doi: 10.1146/annurev-astro-081811-125615

2014 doi
[268]

C., R´ emy-Ruyer, A., Galametz, M., et al

Madden, S. C., R´ emy-Ruyer, A., Galametz, M., et al. 2013, PASP, 125, 600, doi: 10.1086/671138

2013 doi
[269]

C., Cormier, D., Hony, S., et al

Madden, S. C., Cormier, D., Hony, S., et al. 2020, A&A, 643, A141, doi: 10.1051/0004-6361/202038860

2020 doi
[270]

E., Daddi, E., Elbaz, D., et al

Magdis, G. E., Daddi, E., Elbaz, D., et al. 2011, ApJL, 740, L15, doi: 10.1088/2041-8205/740/1/L15 48 Peng et al

2011 doi
[271]

E., Daddi, E., B´ ethermin, M., et al

Magdis, G. E., Daddi, E., B´ ethermin, M., et al. 2012, ApJ, 760, 6, doi: 10.1088/0004-637X/760/1/6

2012 doi
[272]

E., Rigopoulou, D., Hopwood, R., et al

Magdis, G. E., Rigopoulou, D., Hopwood, R., et al. 2014, ApJ, 796, 63, doi: 10.1088/0004-637X/796/1/63

2014 doi
[273]

2009, A&A, 500, L1, doi: 10.1051/0004-6361/200912265

Maiolino, R., Caselli, P., Nagao, T., et al. 2009, A&A, 500, L1, doi: 10.1051/0004-6361/200912265

2009 doi
[274]

2005, A&A, 440, L51, doi: 10.1051/0004-6361:200500165

Maiolino, R., Cox, P., Caselli, P., et al. 2005, A&A, 440, L51, doi: 10.1051/0004-6361:200500165

2005 doi
[275]

2012, MNRAS, 425, L66, doi: 10.1111/j.1745-3933.2012.01303.x

Maiolino, R., Gallerani, S., Neri, R., et al. 2012, MNRAS, 425, L66, doi: 10.1111/j.1745-3933.2012.01303.x

2012
[276]

2015, MNRAS, 452, 54, doi: 10.1093/mnras/stv1194

Maiolino, R., Carniani, S., Fontana, A., et al. 2015, MNRAS, 452, 54, doi: 10.1093/mnras/stv1194

2015 doi
[277]

E., Finkelstein, K., et al

Malhotra, S., Rhoads, J. E., Finkelstein, K., et al. 2017, ApJ, 835, 110, doi: 10.3847/1538-4357/835/1/110

2017 doi
[278]

2024a, MNRAS, 533, 2488, doi: 10.1093/mnras/stae1971 —

Marconcini, C., D’Eugenio, F., Maiolino, R., et al. 2024a, MNRAS, 533, 2488, doi: 10.1093/mnras/stae1971 —. 2024b, arXiv e-prints, arXiv:2411.08627, doi: 10.48550/arXiv.2411.08627

doi arXiv
[279]

2022, A&A, 663, A172, doi: 10.1051/0004-6361/202243336

Markov, V., Carniani, S., Vallini, L., et al. 2022, A&A, 663, A172, doi: 10.1051/0004-6361/202243336

2022 doi
[280]

P., Spilker, J

Marrone, D. P., Spilker, J. S., Hayward, C. C., et al. 2018, Nature, 553, 51, doi: 10.1038/nature24629

2018 doi
[281]

A., Perna, M., Willott, C

Marshall, M. A., Perna, M., Willott, C. J., et al. 2023, A&A, 678, A191, doi: 10.1051/0004-6361/202346113

2023 doi
[282]

A., Yue, M., Eilers, A.-C., et al

Marshall, M. A., Yue, M., Eilers, A.-C., et al. 2024, arXiv e-prints, arXiv:2410.11035, doi: 10.48550/arXiv.2410.11035

2024 doi
[283]

2016, ApJ, 828, 26, doi: 10.3847/0004-637X/828/1/26 —

Matsuoka, Y., Onoue, M., Kashikawa, N., et al. 2016, ApJ, 828, 26, doi: 10.3847/0004-637X/828/1/26 —. 2018a, PASJ, 70, S35, doi: 10.1093/pasj/psx046

2016 doi
[284]

2018b, ApJS, 237, 5, doi: 10.3847/1538-4365/aac724

Matsuoka, Y., Iwasawa, K., Onoue, M., et al. 2018b, ApJS, 237, 5, doi: 10.3847/1538-4365/aac724

doi
[285]

2019, ApJL, 872, L2, doi: 10.3847/2041-8213/ab0216

Matsuoka, Y., Onoue, M., Kashikawa, N., et al. 2019, ApJL, 872, L2, doi: 10.3847/2041-8213/ab0216

2019 doi
[286]

2017, ApJ, 851, 145, doi: 10.3847/1538-4357/aa9931

Matthee, J., Sobral, D., Boone, F., et al. 2017, ApJ, 851, 145, doi: 10.3847/1538-4357/aa9931

2017 doi
[287]

A., et al

Matthee, J., Sobral, D., Boogaard, L. A., et al. 2019, ApJ, 881, 124, doi: 10.3847/1538-4357/ab2f81

2019 doi
[288]

P., et al

Mazzucchelli, C., Ba˜ nados, E., Venemans, B. P., et al. 2017, ApJ, 849, 91, doi: 10.3847/1538-4357/aa9185

2017 doi
[289]

2025, A&A, 694, A171, doi: 10.1051/0004-6361/202451290

Mazzucchelli, C., Decarli, R., Belladitta, S., et al. 2025, A&A, 694, A171, doi: 10.1051/0004-6361/202451290

2025 doi
[290]

McGaugh, S. S. 1991, ApJ, 380, 140, doi: 10.1086/170569

1991 doi
[291]

Meijerink, R., Spaans, M., & Israel, F. P. 2007, A&A, 461, 793, doi: 10.1051/0004-6361:20066130

2007 doi
[292]

1991, ApJ, 380, 334, doi: 10.1086/170592 M´ endez-Delgado, J

Mellier, Y., Fort, B., Soucail, G., Mathez, G., & Cailloux, M. 1991, ApJ, 380, 334, doi: 10.1086/170592 M´ endez-Delgado, J. E., Esteban, C., Garc ´ ıa-Rojas, J.,

1991 doi
[293]

2023, Nature, 618, 249, doi: 10.1038/s41586-023-05956-2

Kreckel, K., & Peimbert, M. 2023, Nature, 618, 249, doi: 10.1038/s41586-023-05956-2

2023 doi
[294]

2014, A&A, 568, A92, doi: 10.1051/0004-6361/201424410

Messias, H., Dye, S., Nagar, N., et al. 2014, A&A, 568, A92, doi: 10.1051/0004-6361/201424410

2014 doi
[295]

2025, ApJ, 980, 20, doi: 10.3847/1538-4357/ada351

Walter, F. 2025, ApJ, 980, 20, doi: 10.3847/1538-4357/ada351

2025 doi
[296]

A., Walter, F., Cicone, C., et al

Meyer, R. A., Walter, F., Cicone, C., et al. 2022, ApJ, 927, 152, doi: 10.3847/1538-4357/ac4e94

2022 doi
[297]

E., et al

Miley, G., Neugebauer, G., Clegg, P. E., et al. 1984, ApJL, 278, L79, doi: 10.1086/184228

1984 doi
[298]

K., Neugebauer, G., & Soifer, B

Miley, G. K., Neugebauer, G., & Soifer, B. T. 1985, ApJL, 293, L11, doi: 10.1086/184481

1985 doi
[299]

B., Chapman, S

Miller, T. B., Chapman, S. C., Hayward, C. C., et al. 2020, ApJ, 889, 98, doi: 10.3847/1538-4357/ab63dd

2020 doi
[300]

B., Chapman, S

Miller, T. B., Chapman, S. C., Aravena, M., et al. 2018, Nature, 556, 469, doi: 10.1038/s41586-018-0025-2

2018 doi

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.

[1] [1]

P., Ferland, G

Abel, N. P., Ferland, G. J., Shaw, G., & van Hoof, P. A. M. 2005, ApJS, 161, 65, doi: 10.1086/432913

doi:10.1086/432913 2005

[2] [2]

V., & Dalgarno, A

Abrahamsson, E., Krems, R. V., & Dalgarno, A. 2007, ApJ, 654, 1171, doi: 10.1086/509631

doi:10.1086/509631 2007

[3] [3]

B., Fujimoto, S., Finlator, K., et al

Akins, H. B., Fujimoto, S., Finlator, K., et al. 2022, ApJ, 934, 64, doi: 10.3847/1538-4357/ac795b

doi:10.3847/1538-4357/ac795b 2022

[4] [4]

C., Swinbank, A

Alaghband-Zadeh, S., Chapman, S. C., Swinbank, A. M., et al. 2013, MNRAS, 435, 1493, doi: 10.1093/mnras/stt1390

doi:10.1093/mnras/stt1390 2013

[5] [5]

2025, arXiv e-prints, arXiv:2501.10508, doi: 10.48550/arXiv.2501.10508

Algera, H., Rowland, L., Stefanon, M., et al. 2025, arXiv e-prints, arXiv:2501.10508, doi: 10.48550/arXiv.2501.10508

doi:10.48550/arxiv.2501.10508 2025

[6] [6]

Algera, H. S. B., Inami, H., Sommovigo, L., et al. 2024a, MNRAS, 527, 6867, doi: 10.1093/mnras/stad3111

doi:10.1093/mnras/stad3111

[7] [7]

Algera, H. S. B., Inami, H., De Looze, I., et al. 2024b, MNRAS, 533, 3098, doi: 10.1093/mnras/stae1994

doi:10.1093/mnras/stae1994

[8] [8]

S., Tucker, D

Allam, S. S., Tucker, D. L., Lin, H., et al. 2007, ApJL, 662, L51, doi: 10.1086/519520 ´Alvarez-M´ arquez, J., Crespo G´ omez, A., Colina, L., et al. 2023, A&A, 671, A105, doi: 10.1051/0004-6361/202245400 ´Alvarez-M´ arquez, J., Colina, L., Crespo G´ omez, A., et al. 2024, A&A, 686, A85, doi: 10.1051/0004-6361/202347946

doi:10.1086/519520 2007