Exploring the mysterious high-ionization source powering [Ne V] in high-z analog SBS0335-052 E with JWST/MIRI

Aidan Pidgeon; Alessandra Aloisi; Bethan L. James; Chris Richardson; Claus Leitherer; Crystal L. Martin; Danielle A. Berg; David Law; John Chisholm; Karla Z. Arellano-C\'ordova

REVIEW 3 major objections 6 minor 5 cited by

Exploring the mysterious high-ionization source powering [Ne V] in high-z analog SBS0335-052 E with JWST/MIRI

T0 review · 3 major / 6 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read JWST MIRI data of dwarf galaxy SBS 0335-052E show that only a 100,000-solar-mass accreting black hole with a 4-8% ionizing fraction reproduces the observed [Ne V] ratios, although no model matches every line.

desk verdict Solid JWST data and an honest analysis, but the 'IMBH needed' claim is overdetermined by a single model family and the abstract's 4–16% vs text's 4–8% needs fixing. read the letter →

arxiv 2502.07662 v2 pith:L75ZGHXG submitted 2025-02-11 astro-ph.GA

Matilde Mingozzi , Macarena Garcia Del Valle-Espinosa , Bethan L. James , Ryan J. Rickards Vaught , Matthew Hayes , Ricardo O. Amorín , Claus Leitherer , Alessandra Aloisi

show 14 more authors

Leslie Hunt David Law Chris Richardson Aidan Pidgeon Karla Z. Arellano-Córdova Danielle A. Berg John Chisholm Svea Hernandez Logan Jones Nimisha Kumari Crystal L. Martin Swara Ravindranath Livia Vallini Xinfeng Xu

This is my paper · ORCID

classification astro-ph.GA

keywords BluecompactdwarfgalaxiesInfraredspectroscopyEmissionlineInterstellarmediumIntermediate-massblackholesHigh-redshiftJWSTMIRI/MRS[NeV]

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

This paper reports the first JWST MIRI/MRS observations of SBS 0335-052E, a nearby blue compact dwarf galaxy whose low mass, low metallicity, and intense star formation make it a local analogue of galaxies at the epoch of reionization. By spatially resolving mid-infrared emission lines of neon, sulfur, and oxygen, the authors locate the very high-ionization gas and ask what produces it. They find that shocks, X-ray binaries, and ordinary old or young stellar populations cannot reproduce the observed line ratios, and that a model with an accreting intermediate-mass black hole of about $10^5\,M_\odot$ contributing 4-8% of the ionizing photons is the only grid that covers the measured [Ne V]/[Ne II], [Ne III]/[Ne II], and [S IV]/[Ne II] ratios. The match is not complete, because even these models cannot reach the strongest [O IV]/[Ne III] values, so the paper leaves other ionizing sources open. If right, the result provides a concrete local benchmark for identifying faint intermediate-mass black holes in the low-metallicity galaxies JWST is finding at high redshift.

What carries the argument

The load-bearing machinery is the set of mid-infrared forbidden-line ratios -- [Ne V]/[Ne II], [Ne III]/[Ne II], [S IV]/[Ne II], and [O IV]/[Ne III] -- used as diagnostics of radiation hardness and ionization parameter in a $\sim$5% solar-metallicity interstellar medium. These ratios are interpreted through grids of photoionization models: simple stellar populations with and without X-ray binaries, radiative shock models, and the intermediate-mass black hole models of Richardson et al. (2022), which combine a starburst continuum with a black-hole spectral energy distribution (qsosed or disk-plaw) and a tunable AGN fraction, mixing geometry, gas density, and metallicity. The AGN fraction is the parameter that carries the conclusion, and the spatial maps of [Ne V]/[Ne II] and [O IV]/[Ne III] show that the hardest radiation is not at the obvious young cluster or the X-ray ultraluminous source, but around SSCs4-5 and S7.

What would settle it

Measure the [Ne V] 14.3 $\mu$m to 24.3 $\mu$m doublet ratio in the SSCs4-5/S7 region with deeper MIRI data: the paper's dense-gas IMBH interpretation predicts a specific ratio while lower-density models predict the opposite, and a secure detection of the 24.3 $\mu$m line would test the density assumption directly. Independently, detecting a point-like, variable hard X-ray source at that position would confirm the IMBH, whereas a revised stellar or binary model that reproduces [Ne V]/[Ne II] without a black hole would falsify the paper's conclusion.

Watch

Extended reading notes

Core claim

The central discovery is that the extended high-ionization emission in SBS 0335-052E, including the first detection of [Ne V] $\lambda14.32\,\mu$m in a blue compact dwarf, peaks around the older super star clusters and the region S7, away from the youngest embedded cluster that dominates the mid-infrared continuum. Comparing dust-corrected, PSF-matched line-ratio maps with low-metallicity photoionization and shock grids, the paper excludes simple stellar populations, X-ray binaries, and radiative shocks as the main ionizing sources. The only models that simultaneously reproduce the observed [Ne V]/[Ne II], [Ne III]/[Ne II], and [S IV]/[Ne II] are the Richardson et al. (2022) intermediate-mass black hole grids with $M_{\rm BH}=10^5\,M_\odot$, an AGN fraction of 4-8%, and $\log U$ between about $-2$ and $-0.5$; lower-mass black holes cannot reach the observed [Ne V]/[Ne II], and $10^6\,M_\odot$ only overlaps at 8% AGN fraction. The paper states plainly that these same models fail to reproduce the highest [O IV]/[Ne III] ratios, so the IMBH interpretation is offered as the best available fit rather than a definitive identification.

Load-bearing premise

The entire inference rests on the Richardson et al. (2022) intermediate-mass black hole photoionization grids being accurate in their assumed black-hole spectral shapes, AGN-starburst mixing geometry, gas density, and metallicity; if those models overproduce [Ne V] for reasons unrelated to a black hole, the need for an IMBH is not established.

Editorial extensions

If this is right

The first detection of [Ne V] $\lambda14.32\,\mu$m in a blue compact dwarf makes SBS 0335-052E a benchmark for studying very high-ionization gas in low-metallicity starbursts, with $\log([Ne V]/[Ne II]) > 0$ exceeding every BCD upper limit from earlier infrared telescopes.
A real $10^5\,M_\odot$ IMBH contributing only 4-8% of the ionizing light would place this galaxy above local black-hole/stellar-mass scaling relations and provide a local template for the faint, reddened AGN candidates JWST is uncovering at $z>6$.
The same 8% AGN-fraction model also reproduces the UV (C III]/He II, O III]/He II) and optical (He II/H$\beta$, [Ne V]/[Ne III]) line ratios, so the MIR conclusion is consistent across three independent wavelength regimes.
Because star-forming models, with or without X-ray binaries, fail even the lower-ionization [S IV]/[Ne II] versus [Ne III]/[Ne II] relation seen in BCDs, the paper implies a general limitation in current low-metallicity stellar libraries or a missing non-stellar ionizing component in these galaxies.

Reading between the lines

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

Not tested in the paper: the [O IV]/[Ne III] excess could be a signature that the IMBH's extreme-UV continuum is harder than the qso/disk-plaw SEDs assumed, so a broader family of accretion models is the natural next step.
An observable consequence the authors do not spell out: if the IMBH sits near SSCs4-5/S7, repeated X-ray or mid-infrared monitoring of that position should reveal variability or a point-like hard source on timescales of months to years.
The paper's claim implies that density measurements in the [Ne V] region, via the 14.3-to-24.3 $\mu$m doublet ratio currently undetected, could discriminate between dense-gas IMBH models and lower-density alternatives; a future detection of the 24.3 $\mu$m line would directly test this.
The broad H$\alpha$ in this galaxy is composed of multiple kinematic components rather than a single broad-line region, so the IMBH must be searched for with forbidden-line or variability diagnostics rather than optical broad lines, a lesson that may apply to high-redshift broad-line AGN candidates.

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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

First thing to know: this is a genuinely useful observational paper. The MIRI/MRS data on SBS 0335-052 E are new, the [Ne V] 14.32 detection in a BCD is a first, and the spatially resolved maps—ionization peak near S7, offset from the ULX—are a real step forward. The reduction is careful: PSF subtraction with WebbPSF, fringing correction, CAFE-based attenuation, and the authors are honest that no model family reproduces everything, especially [O IV]/[Ne III]. That honesty is not pro forma; it shapes the conclusions.

The soft spot is the load-bearing IMBH claim. 'A 4–8% contribution... is needed' is stronger than what the evidence supports. The paper matches observed ratios to Richardson et al. (2022) grids, but those grids are from a co-author's code, they fail the [O IV]/[Ne III] diagnostic, and the alternative disk-plaw SED—which produces higher [O IV]/[Ne III]—appears only in an appendix, never in the primary diagnostic plot. So 'uniquely covered' is not actually demonstrated. The safer claim is 'permitted by one model family under specific assumptions.' The paper also has an internal inconsistency: the abstract says 4–16%, the text and conclusions say 4–8%. That needs harmonizing.

None of this sinks the paper. The exclusion of shocks, X-ray binaries, and old stellar populations as the main ionizing source is well argued and likely robust. The IMBH interpretation is plausible; it's just not the only viable reading, and the authors themselves admit other sources can't be fully ruled out. The discussion of model limitations (low-metallicity massive-star atmospheres, XRB scaling relations) is exactly the kind of caveat you want to see.

Bottom line: this deserves a serious referee. The referee should ask for the abstract/text numbers to be reconciled, for the disk-plaw grids to be shown in the main diagnostic or a stated reason why they're omitted, and for 'needed' to be softened to 'consistent with' unless the uniqueness argument is actually proven. I'd bring it to reading group and would cite it if I worked in this subfield.

Referee Report

3 major / 6 minor

Summary. The paper reports the first JWST MIRI/MRS integral-field observations of the blue compact dwarf galaxy SBS 0335-052 E, a local analog of high-redshift star-forming galaxies. The authors perform a careful data reduction that includes wavelength-dependent PSF subtraction of a bright point source (identified with the embedded cluster SSC1), residual fringe correction, and dust-attenuation modeling with the CAFE tool, obtaining separate spectra for the point source and the extended emission. They measure mid-infrared line ratios spanning a broad range of ionization potential ([Ne II], [S IV], [Ne III], [O IV], [Ne V]) and compare them with published photoionization and shock model grids: MP23 simple stellar populations, G24 SSP and X-ray binary (SXP) models, R22 intermediate-mass black hole (IMBH) models, and F24/AM19 shock models. The spatial maps show that high-ionization [Ne V] and [O IV] emission is extended over the north-west region around clusters SSCs 4-6 and S7, with [Ne V]/[Ne II] and [O IV]/[Ne III] peaking near S7. The diagnostic diagrams indicate that pure stellar, X-ray binary, and shock models fail to reproduce the observed ratios, while R22 IMBH models with M_BH = 10^5 Msun and an AGN fraction of 4-8% (qso SED) best cover the [Ne V]/[Ne II] versus [Ne III]/[Ne II] and [S IV]/[Ne II] versus [Ne III]/[Ne II] planes.

Significance. The paper presents the first spatially resolved detection of [Ne V] 14.32 um in a blue compact dwarf galaxy, which is an important observational milestone. The data reduction is thorough: the PSF subtraction is validated with residual maps and radial profiles, the dust attenuation is modeled with a dedicated tool, and the systematic uncertainties from fringing and PSF-matching are discussed honestly. The comparison with four independent model families is a useful contribution, and the authors are commendably transparent about the failure of all models, including their preferred IMBH models, to match the full set of line ratios. If the IMBH interpretation holds, the result would have implications for the presence of intermediate-mass black holes in low-metallicity, high-z analogs and for the interpretation of UV/optical AGN diagnostics in the early universe. However, the strength of the central claim ('an IMBH is needed') currently rests on a grid-matching comparison to one SED family from one model set, and the paper's own analysis shows that the same models are internally inconsistent with the [O IV]/[Ne III] diagnostic.

major comments (3)

[Sec. 4.4 and Fig. 8; Sec. 5.2.4] The central inference that R22 IMBH models with a 4-8% AGN fraction 'uniquely cover' the observed [Ne V]/[Ne II], [Ne III]/[Ne II], and [S IV]/[Ne II] ratios is made using only the qso SED grids. The alternative disk-plaw SED, which the paper states in Sec. 4.4 and Fig. 14 can reach higher [O IV]/[Ne III], is never shown in the primary [Ne V]/[Ne II] versus [Ne III]/[Ne II] diagram. Since the SED shape is a free parameter in the R22 models and directly affects the production of [Ne V], the claim that the qso SED models uniquely cover the primary diagnostic is unsupported without also demonstrating where the disk-plaw models fall in that plane. Please show the disk-plaw grids in Fig. 8 (or an equivalent figure) and state explicitly whether they do or do not cover the observed primary ratios.
[Sec. 5.2.4 and Abstract] The language 'an IMBH is needed' and 'the models that uniquely cover' is stronger than what the analysis supports. The 4-8% AGN fraction is selected by visual matching to discrete R22 grid points, not by a quantitative fit or a statistical comparison over the model parameter space, and the paper itself notes that the R22 family fails to reproduce the highest [O IV]/[Ne III] ratios (Sec. 3.4 and Sec. 5.2.4). I recommend either softening the conclusion to 'consistent with a low-luminosity IMBH' or providing a quantitative measure of agreement (e.g., distances in line-ratio space spanning the full R22 grid, including both SEDs, with uncertainties propagated) that would justify the 'needed' wording.
[Sec. 3.4 and Sec. 5.2.4] The R22 grids shown fix the starburst component to a 20 Myr instantaneous burst. The extended high-ionization emission, however, is spatially associated with clusters whose ages are 4-15 Myr (Table 2) and the peak at S7 is listed at ~4 Myr. The paper does not assess how the inferred IMBH mass or AGN fraction would change if the starburst age were varied within the R22 framework. Because the stellar SED directly influences the lower-ionization ratios ([Ne III]/[Ne II], [S IV]/[Ne II]) used to select the 4-8% fraction, the robustness of this inference to the assumed burst age should be tested or at least explicitly discussed.

minor comments (6)

[Abstract] The phrase 'ideal local laboratories detailed for multi-wavelength studies' should read 'ideal local laboratories for detailed multi-wavelength studies'.
[Abstract vs. Conclusions] The abstract and Sec. 5.2.4 state an IMBH AGN fraction of 4-8%, while the Conclusions bullet and the Fig. 14 caption refer to AGN fraction '<16%' and 'low AGN fraction (<16%)'. Please harmonize these numbers.
[Sec. 4.1 and Table 1] The rest wavelength of Pf alpha is given as 7.49 um in the text (Sec. 4.1) and 7.46 um in Table 1. Please correct the inconsistency.
[Fig. 8 caption] The caption states 'The dotted grids have higher density' without specifying the actual densities. Please indicate the nH values corresponding to the solid and dotted grids.
[Sec. 4.1] The sentence 'The UV emission ... tracing the six SSCs and peaking in the [Ne V] and [O IV] high ionization region' is ambiguous: clarify whether the UV emission peaks in the high-ionization region or whether the high-ionization lines peak there.
[Sec. 5.2.4] The phrase 'around/north SSCs 4,5 and S7' should read 'around/north of SSCs 4-5 and S7'.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the IMBH inference is a grid-comparison result against independent, public photoionization models, with explicit hedges.

full rationale

The paper's derivation chain is observational: MIRI/MRS line fluxes are measured, corrected for attenuation, converted into line ratios, and then compared with published photoionization and shock grids (MP23, G24, R22, F24). No parameter is fitted to the target data; the 4-8% AGN fraction and 10^5 M_sun IMBH mass are selected by matching the observed [Ne V]/[Ne II], [Ne III]/[Ne II], and [S IV]/[Ne II] ratios to the R22 grid family. The R22 models are publicly released, generated with CLOUDY and BPASS under stated assumptions (SED, geometry, density, metallicity) that do not include SBS 0335-052 E's measured line ratios. Thus the inference is not equivalent to its inputs by construction. The paper explicitly acknowledges the central tension: R22 IMBH models fail to reproduce the highest [O IV]/[Ne III] values, and the abstract and conclusions state that 'other sources of ionization cannot be fully ruled out.' Co-authorship of the R22 grid is a self-citation, but it is not load-bearing in a circular sense: the grid predictions are independent, code-reproduced, and falsifiable outside the present paper. I checked for self-definitional ratios, fitted-input-as-prediction, ansatz-smuggling, and renaming of known results; none appear. The strongest limitation is model completeness rather than circularity: the 'uniquely cover' claim applies to the sampled grid families, and the paper itself flags the [O IV]/[Ne III] discrepancy. This is a normal, honest model-comparison study, so the appropriate circularity score is 0.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

The central IMBH inference rests on comparing observed MIR line ratios with external photoionization grids. The free parameters are the R22 model choices (AGN fraction, BH mass, gas density) selected to match the data, plus the dust attenuation values derived from the continuum. No new physical entities are introduced; the IMBH hypothesis predates this paper. The main axioms are the validity of CLOUDY-based grids at low metallicity and the representativeness of the R22 IMBH SEDs.

free parameters (4)

AGN fraction (R22 IMBH contribution) = 4-8% (abstract and Sec. 5.2.4); <16% in conclusions
Selected to match the observed [Ne V]/[Ne II] within the R22 10^5 Msun IMBH grids. The exact fraction is a model-grid choice, not a formal fit with uncertainty.
IMBH mass = 10^5 Msun
Discrete grid choice among 10^3, 10^4, 10^5, and 10^6 Msun; lower masses cannot reach the observed [Ne V]/[Ne II] and [Ne III]/[Ne II], while 10^6 Msun only fits at 8% with worse [Ne III]/[Ne II].
Gas density = nH = 100 cm^-3 (low-density R22 grid)
High-density grids shift toward lower [Ne III]/[Ne II] and [O IV]/[Ne III] and are less consistent with the data, so the low-density grid is adopted (Sec. 4.4 and App. B).
Dust attenuation A_V = ~15 for SSC1, ~8 for extended emission
Derived from CAFE continuum modeling; affects line-ratio corrections by about 0.1 dex for [S IV]/[Ne II], with [Ar III] and [S IV] inside the silicate feature corrected by a factor of ~3.

assumptions (4)

domain assumption CLOUDY photoionization models are valid for low-metallicity ISM.
Used throughout via MP23, G24, and R22 grids (Sec. 3.4).
domain assumption R22 IMBH spectral energy distributions (qsosed and disk-plaw) bracket realistic accreting IMBH SEDs.
Sec. 3.4: R22 grids are taken as the IMBH benchmark; if these SEDs are wrong, the 4-8% fraction inference fails.
domain assumption The gas metallicity of SBS 0335-052 E lies in the 2-10% Zsun range of the model grids.
Sec. 3.4 uses only 2-10% Zsun grids based on Papaderos et al. (2006) and Nakajima et al. (2024).
domain assumption The observed MIR lines and the model grids trace the same emitting gas geometry and phase.
Line-ratio diagrams assume a single-phase ionized gas; the paper acknowledges geometry and density effects in Sec. 4.4 and Sec. 5.

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Cite this review

Pith. "Pith review of Exploring the mysterious high-ionization source powering [Ne V] in high-z analog SBS0335-052 E with JWST/MIRI." pith.science (2026). https://pith.science/paper/L75ZGHXG

@misc{pith2026250207662,
  author       = {Pith},
  title        = {Pith review of: Exploring the mysterious high-ionization source powering [Ne V] in high-z analog SBS0335-052 E with JWST/MIRI},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/L75ZGHXG}},
  note         = {Machine review of arXiv:2502.07662}
}

abstract

Nearby blue compact dwarf galaxies (BCDs) share similar properties with objects from the Epoch of Reionization revealed by JWST, in terms of low stellar mass, low metallicity and high specific star-formation rate. Thus, they represent ideal local laboratories for detailed multi-wavelength studies to understand their properties and the mechanisms shaping them. We report the first JWST MIRI/MRS observations of the BCD SBS 0335-052 E, analyzing MIR emission lines tracing different levels of ionization (e.g., [NeII], [SIV], [NeIII], [OIV], [NeV]) of the ionized gas. SBS 0335-052 E MIR emission is characterized by a bright point source, located in one of the youngest and most embedded stellar clusters ($t\sim3$ Myr, $A_V\sim15$), and underlying extended high-ionization emission (i.e., [OIV], [NeV]) from the surroundings of the older and less dusty stellar clusters ($t< 20 $ Myr, $A_V\sim8$). From the comparison with state-of-the-art models, we can exclude shocks, X-ray binaries, and old stellar populations as the main sources of the high ionization. Interestingly, a 4-16% contribution of a $\sim10^5$ M$_\odot$ intermediate massive black hole (IMBH) is needed to justify the strong [NeV]/[NeII] and would be consistent with optical/UV line ratios from previous studies. However, even IMBH models cannot explain the strongest [OIV]/[NeIII]. Also, star-forming models (regardless of including X-ray binaries) struggle to reproduce even the lower ionization line ratios (e.g., [SIV]/[NeII]) typically observed in BCDs. Overall, while current models suggest the need to account for an accreting IMBH in this high-$z$ analog, limitations still exist in predicting high-ionization emission lines (I.P. $>54$ eV) when modeling these low-metallicity environments, thus other sources of ionization cannot be fully ruled out.

Figures

Figures reproduced from arXiv: 2502.07662 by the authors.

**Figure 1.** Left panel: Overview on SBS 0335-052 E (1" ∼ 280 pc). HST ACS F150LP image (PID: 16209; PI Hayes) with superimposed MIRI/MRS Channel 1 and 3 FOVs in green, and the HST ACS WFC FR656N (PID: 10575, PI Oestlin) contours in black; the six SSCs positions (SSCs1,2,3,4,5,6, t ∼ 3 − 13 Myr; see Tab. 2) and the three further young star-forming regions (S7, S8 and S3-Paα) found by Thompson et al. (2009) are indicated in blue;… view at source ↗

**Figure 2.** Point-source (SSC1) spectrum with the set of emission lines highlighted in blue for the hydrogen-recombination lines and red for the metallic-forbidden lines. The bottom panels display a zoom-in around each emission line considered in this work, with the best-fit model shown in red. The point-source spectrum also shows a very high attenuation, with AV ∼ 20. The larger contribution of the dust can be appreciated by t… view at source ↗

**Figure 3.** Same as [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

Figures from the paper (11 more)

**Figure 4.** Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]

**Figure 5.** Figure 5: Point-source subtracted emission-line maps corrected for dust attenuation on Channel 3 pixel scale (0.245"; 1" ∼ 280 pc). All lines but [S III] and [O IV] are convolved to [Ne III] resolution (FWHMPSF ∼ 0.6"). The colored regions represent the measurements with S/N > 3…

**Figure 6.** Figure 6: [Ne III]/[Ne II], [Ne V]/[Ne II] and [O IV]/[Ne III] line-ratio maps, where the colored spaxels have S/N > 3 for the displayed emission lines. [Ne III]/[Ne II], tracing the ionization parameter, peaks around S3-Paα, while [Ne V]/[Ne II] and [O IV]/[Ne III], both tracin…

**Figure 7.** Figure 7: Velocity (top panels) and velocity dispersion (corrected for instrumental broadening; bottom panels) maps of the [S IV], [Ne III] and [Ne V] emission lines, in order of ionization potential (see Tab. 1), with the same orientation, labeling and contours as [PITH_FULL_I…

**Figure 8.** Figure 8: [Ne V]/[Ne II] versus [Ne III]/[Ne II] diagnostic diagram color-coded as a function of [O IV]/[Ne III] line ratio, with overplotted the four sets of low-metallicity models presented in Sec. 3.4: 2.5 Myr SSPs models from MP23, 5, 10 and 20 Myr SSPs and SXPs models from …

**Figure 10.** Figure 10: He II λ4686/Hβ vs [Ne V] λ3426/[Ne III] λ3868 emission-line diagnostic diagram, recently proposed by Chisholm et al. (2024) to probe the strength of very high-ionization emission lines independently of gas-phase metallicity. The square shows SBS 0335-052 E line ratio…

**Figure 11.** Figure 11: displays an example of the data, the original WebbPSF model, the best-fit model we find with photutils and the residual extended emission for one wavelength close to the [Ne III] λ15.56 emission, where both point-like source and extended emission are clearly visible (…

**Figure 12.** Figure 12: Ratio of the original and point-source subtracted maps, highlighting the region dominated by the point source (darker red). All the spaxels with S/N > 3 are shown. [Ne III] and [S IV] are the brightest emission lines observed and show clearly the MIRI/MRS PSF structur…

**Figure 13.** Figure 13: [Ne III]/[Ne II] vs [S IV]/[Ne II] diagnostic diagram color-coded as a function of [O IV]/[Ne III] line ratio, with overplotted the same four sets of models of [PITH_FULL_IMAGE:figures/full_fig_p029_13.png]

**Figure 14.** Figure 14: [Ne III]/[Ne II] versus [O IV]/[Ne III] diagnostic diagram color-coded as a function of [Ne V]/[Ne II] line ratio, with overplotted the same four sets of models of [PITH_FULL_IMAGE:figures/full_fig_p030_14.png]

**Figure 15.** Figure 15: Upper panel: Extracted MUSE spectra from the point-source region (SSC1; black) and the UV and [Ne V] emitting region (around SSC4+5; gray), with a 3-px extraction radius. Bottom panels: Zoom on the Hβ+[O III] λλ4959,5007 (left) and Hα+[N II] λλ6548,84 (right). Both sp…

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Pith tools

Reviewed August 8, 2026 · model on record in the stance chip above.

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, " * write output.state after.block = add.period write newline

ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month note number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.co...

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write newline

" write newline "" before.all 'output.state := FUNCTION format.doi doi empty "" "doi:" doi * if FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix ":" * if eprint field.or.null * if FUNCTION format.pid eprint empty format.doi format.eprint if FUNCTION n.dashify 't := "" t...

[3] [3]

602C `\.=

thebibliography [1] 20pt to REFERENCES 6pt =0pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command Each re...

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