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REVIEW 3 major objections 4 minor 300 references

Spectra of the Type Ibn SN 2023tsz are best reproduced by an exploding 4-solar-mass helium star interacting with dense helium-rich material, placing this supernova in the lower-mass, binary-stripped progenitor channel.

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2026-08-01 23:38 UTC pith:OI7GMGTB

load-bearing objection A rich, honestly presented UV-to-NIR dataset for one SN Ibn; the lower-mass progenitor claim is plausible but not uniquely established because no higher-mass He-star models are actually computed. the 3 major comments →

arxiv 2607.15342 v1 pith:OI7GMGTB submitted 2026-07-16 astro-ph.HE

Ultraviolet to Infrared Spectroscopy of the Type Ibn SN 2023tsz Suggests a Lower-mass Progenitor

Sergiy S. Vasylyev , Griffin Hosseinzadeh , Luc Dessart , Ori Fox , David J. Sand , Alexei V. Filippenko , Qinan Wang , D. Andrew Howell
show 37 more authors
Jennifer E. Andrews Moira Andrews Pallas Beddow K. Azalee Bostroem Thomas G. Brink Peter J. Brown Asia deGraw Yize Dong Joseph Farah Thomas R. Geballe Sebastian Gomez Emily T. Hoang Brian Hsu Saurabh W. Jha Patrick Kelly Curtis McCully Darshana Mehta Megan Newsome Yuan Q. Ni Seong Hyun Park Jeniveve Pearson Neil Pichay Justin Pierel Aravind P. Ravi Nicolas E. Meza Retamal Melissa Shahbandeh Manisha Shrestha Nathan Smith Bhagya M. Subrayan Tam\'as Szalai Stefano Valenti Schuyler D. Van Dyk Jeonghee Rho Kathryn Wynn Yi Yang Yossef Zenati WeiKang Zheng
This is my paper
classification astro-ph.HE
keywords Type Ibn supernovaecircumstellar mattercore-collapse supernovaestellar mass losshelium starscold dense shellX-ray irradiationultraviolet spectroscopy
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

SN 2023tsz is a Type Ibn supernova, a stripped helium-rich explosion whose light comes from ejecta slamming into dense circumstellar matter. This paper collects ultraviolet, optical, and near-infrared spectra over the first three months and compares them to one-dimensional radiative-transfer models of a 4-solar-mass helium-star explosion. The models reproduce the intermediate-width helium lines and the highly ionized ultraviolet features only when an X-ray irradiation field of about 10^8 solar luminosities is added on top of the shock power. The authors argue that the success of this model, together with the low-luminosity, low-metallicity dwarf host, points to a lower-mass helium star stripped by binary interaction rather than a single very massive Wolf-Rayet star. A sympathetic reader would care because it strengthens the emerging picture that at least some Type Ibn supernovae come from the binary-stripped channel.

Core claim

The central claim is that SN 2023tsz's spectrum from 1200 angstroms to 2.4 microns is best matched by a model of a 4-solar-mass helium star (roughly 3.15 solar masses just before explosion) colliding with a dense, helium-rich circumstellar shell. To match the ultraviolet continuum and high-ionization lines such as C IV, the models require an added X-ray irradiation power of roughly 10^8 solar luminosities, with preferred cold-dense-shell radii of (1.5-2) x 10^15 cm, expansion velocities near 5 x 10^7 cm/s, and interaction powers of a few times 10^42 erg/s. The optical fits evolve from higher power and smaller radii at early times to lower power and larger radii later, tracking the expanding

What carries the argument

The load-bearing machinery is the cold dense shell (CDS): the compressed layer where fast supernova ejecta plow into slow, helium-rich circumstellar material, converting kinetic energy into the intermediate-width emission lines that dominate every post-peak spectrum. The paper models this with a grid of one-dimensional, spherically symmetric, non-LTE (gas not in local thermodynamic equilibrium) radiative-transfer calculations built on a 4-solar-mass helium-star explosion model. The critical new ingredient is a separate X-ray irradiation field L_X, added on top of the shock-energy deposition; X-rays photoionize the ultraviolet line-forming region in a way that shock-heated electrons alone can

Load-bearing premise

The lower-mass progenitor conclusion rests on the assumption that the strength of helium relative to metal lines uniquely reflects the initial helium-star mass, with more massive helium stars having wind compositions too metal-rich to reproduce the observed lines; if mixing, circumstellar composition, or the added X-ray field can mimic that helium-abundance signature, the mass inference loses its force.

What would settle it

Run the same radiative-transfer model grid with helium-star initial masses above about 6 solar masses, keeping the X-ray irradiation and mixing prescriptions unchanged: if any of those models reproduces the observed He I-to-metal line ratios and the ultraviolet spectrum, the lower-mass claim is falsified. Alternatively, a late-time X-ray observation that places an upper limit well below L_X ~ 10^8 solar luminosities would contradict the irradiation requirement.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If correct, the event adds a direct spectroscopic case for lower-mass helium stars (roughly 2.6-5 solar masses initially) stripped by binary interaction as Type Ibn progenitors, rather than single very massive Wolf-Rayet stars.
  • The inferred X-ray irradiation of about 10^8 solar luminosities implies that a meaningful fraction of the interaction luminosity emerges at high energy; late-time X-ray observations could test this directly.
  • The preferred models shift from higher interaction power and smaller cold-dense-shell radii at early times to lower power and larger radii later, explaining why intermediate-width lines persist for months even as the continuum fades.
  • The close spectral match between SN 2023tsz and the Type Ibn SN 2020nxt, especially in ultraviolet carbon and silicon features, suggests a common cold-dense-shell formation region and likely a shared progenitor channel.

Where Pith is reading between the lines

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

  • A sharper test of the lower-mass claim would be to run the same model grid with helium-star initial masses above 6 solar masses and varied wind metallicity; if any such model reproduces the observed He I-to-metal line ratios and ultraviolet spectrum, the mass inference would be weakened.
  • The X-ray field required by the models could be checked with sensitive late-time X-ray observations; an upper limit well below 10^8 solar luminosities would challenge the irradiation geometry assumed here.
  • The helium-to-metal line-strength ratio could be developed into a quick progenitor-mass classifier for other Type Ibn supernovae, but only after the acknowledged degeneracy between cold-dense-shell radius/mass and helium-star mass is broken with additional diagnostics such as nitrogen-to-carbon ratios.
  • If the models' requirement of efficient mixing in the cold dense shell is taken at face value, multidimensional simulations of shell instabilities would be the natural next step to connect the inferred near-homogeneous composition to the physics of ejecta-CSM interaction.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper presents extensive UV-to-NIR spectrophotometry of the Type Ibn SN 2023tsz, including two HST/STIS UV epochs, and compares the spectra to a grid of 1D non-LTE CMFGEN interaction models based on a 4 M_sun helium-star explosion. The models reproduce the strong optical/NIR He I features and, with an added X-ray irradiation field, the highly ionized UV lines. The preferred models require L_X ~ 1e8 L_sun, CDS radii (1.5-2)e15 cm, velocities ~5e7 cm/s, and interaction powers of a few 1e42 erg/s, with a temporal trend from higher power/smaller radius to lower power/larger radius. The paper interprets these results as evidence that SN 2023tsz arose from a lower-mass (~2.6-5 M_sun), binary-stripped helium star.

Significance. If the central claim holds, the paper provides one of the most detailed observational constraints on the progenitor of a Type Ibn SN, combining rare UV spectroscopy with optical/NIR coverage and quantitative radiative-transfer modeling. The data products are public, the model comparison is transparent, and the independent optical/NIR best-fit agreement at +29 d is a tangible strength. However, the principal inference—that the progenitor was exclusively in the lower-mass range—is not directly tested by the models, which only use a 4 M_sun He-star grid; the higher-mass exclusion rests on an external helium-abundance–mass relation rather than on a differential model comparison. The paper is valuable as a consistency argument and a parameter inference for a plausible low-mass scenario, but the title and abstract overstate the uniqueness of the mass determination.

major comments (3)
  1. [§3 and §5; also title/abstract] The central claim that the progenitor is a lower-mass He star is not directly tested. The grid contains only the he4p0 (4 M_sun) model; the exclusion of M_He > 5-6 M_sun relies entirely on the helium-abundance–mass trend from Dessart et al. (2022), a paper with overlapping authorship. That trend is applied to a quantity (He I / metal-line ratio) that the present paper itself shows is sensitive to the tuned mixing, iron-group scaling, and added X-ray field. No higher-mass He-star model is computed, so the spectral modeling demonstrates consistency with a 4 M_sun progenitor but does not exclude alternatives. The acknowledgement of degeneracy in §5 is welcome, but the next sentence still asserts that the helium-star mass is 'constrained from both ends.' Please either soften the title/abstract/conclusion to 'consistent with a lower-mass progenitor' or extend the grid with a genuinely higher-
  2. [§4, Fig. 5] The model selection is not fully operationalized. Spectra are ranked by RMS, yet at +3.6 d the authors explicitly override the RMS ranking and prefer the second- and third-best fits because the best fit has 'very narrow lines.' This subjective choice changes the inferred CDS parameters at the earliest epoch and contributes to the claimed temporal trend in power/radius. The paper should report the full grid of RMS values, define the selection criterion quantitatively (e.g., a reduced chi-square or a line-profile residual measure), and give uncertainties on the best-fit parameters derived from the shape of the RMS surface. Without this, the statement that the spectra are 'best reproduced' by the quoted parameters is not quantitatively grounded.
  3. [§4.4, Figs. 10–12] The UV fits have large residuals (RMS ≈ 0.49–0.60 for the top +9.3 d fits) and are achieved only after tuning the X-ray irradiation field and, in several preferred models, scaling the iron-group abundance to 0.3× solar. The text itself notes that the UV ionization balance is so sensitive that 'the models can be tuned' to match C II/III/IV. Since L_X is a free input whose physical source is not specified, the UV comparison should be framed as a demonstration that a plausible X-ray field can reproduce the highly ionized features, not as independent confirmation of the derived L_X and CDS parameters. I recommend adding a table of the UV line strengths and RMS as functions of L_X and IGE scaling, and a discussion of systematic uncertainties from the coarse grid and the ad hoc X-ray treatment.
minor comments (4)
  1. [Fig. 10 caption] The caption states that the best-fit model has r = 2e15 cm, v = 0.5e8 cm/s, power = 1e42 erg/s, L_X = 1.6e8 L_sun, and IGE×0.3, but the top panel of the same figure displays r = 1.5e15 cm, L_sh = 7e42 erg/s, L_X = 1.6e8 L_sun. The caption and panel annotations must be reconciled.
  2. [§4.1 and Fig. 7 caption] The text says the best-fit model has r_CSM = 2e15 cm, while the Figure 7 caption and panel annotation indicate r = 3e15 cm with the same velocity and power. Please clarify which value is used and ensure consistency throughout.
  3. [Fig. 3] The top-panel caption says 'with mixing' but does not specify whether this is the mildly mixed ('lmix') or homogeneous case. Define the mixing label in the caption or in §3.
  4. [§2] The phase is defined relative to maximum light, but the time of maximum is not explicitly given in the text; consider adding the MJD of peak to make the phase definition self-contained.

Circularity Check

1 steps flagged

Progenitor-mass uniqueness rests on a self-cited helium-abundance–mass trend; spectral fitting itself is not circular.

specific steps
  1. self citation load bearing [Section 3, paragraph justifying the he4p0 4 M_sun model; reiterated in Section 5]
    "The choice of this model is motivated by the helium content expected for stripped helium-star progenitors. Dessart et al. (2022) show that the largest fractional helium abundances at core collapse occur for lower-mass binary helium stars, with initial helium-star masses of ∼2.6–5.0 M⊙. Above this range, more massive helium stars (≳5–6 M⊙) have substantially lower fractional helium abundances, as their winds become increasingly dominated by heavier elements, and would therefore not reproduce the strength of the HeI lines relative to the metal features."

    The exclusion of higher-mass He-star progenitors is imported from Dessart et al. (2022), a prior paper co-authored by Dessart, and no higher-mass He-star model is computed or compared here. The same self-cited trend is then used in Section 5 to declare the helium-star mass 'constrained from both ends' and to claim that the observed He I/metal strength favors ~2.6–5.0 M_sun. Thus the spectral comparison can only confirm consistency with the 4 M_sun model; it does not independently test the uniqueness of that mass, because the alternative mass range is excluded by the self-cited trend rather than by a direct model comparison.

full rationale

The paper's spectral fitting is not circular by construction: the CDS radius, velocity, interaction power, mixing, and X-ray power are free parameters fitted to the observed spectra, and the paper presents them as fit results ('best reproduced by models with...'), not as independent predictions. The X-ray field is admittedly added to match the UV, and the authors explicitly note that models 'can be tuned' to the line strengths, so the UV match does not independently validate LX. The main circularity concern is the progenitor-mass inference. The paper selects the he4p0 4 M_sun model using a helium-abundance–mass trend from Dessart et al. (2022), a co-authored prior work, and then uses the same trend to argue that higher-mass He stars are excluded. Because no higher-mass model is computed, the spectral data do not themselves establish that the low-mass regime is unique. The paper's own caveat in Section 5 acknowledges degeneracies between He-star mass and CDS properties. However, independent evidence exists: the low-luminosity, low-metallicity host and the low ejecta mass from Warwick et al. (2025) support a lower-mass binary origin, so the central claim retains independent content. The circularity is thus partial and localized to the self-cited mass-uniqueness argument, not a reduction of the whole derivation to its inputs.

Axiom & Free-Parameter Ledger

6 free parameters · 5 axioms · 0 invented entities

The model comparison relies on a set of tuned grid parameters (radius, velocity, shock power, X-ray power, iron scaling, mixing) and several domain assumptions inherited from prior work, especially the helium-abundance–mass mapping for He-star progenitors. The X-ray irradiation field is an ad hoc input rather than a detected source. No fundamentally new physical entity is introduced.

free parameters (6)
  • CDS radius r_CSM = 1e15, 1.5e15, 2e15, 3e15 cm; preferred 1.5–2e15 cm
    Grid parameter varied to minimize RMS residuals to the optical and UV spectra; controls line widths and continuum shape.
  • CDS velocity v_CSM = 0.5e8, 1e8, 2e8 cm/s; preferred 0.5e8–1e8 cm/s
    Grid parameter chosen by spectral fit; sets the Doppler widths of intermediate-width lines.
  • Interaction power L_sh = 2e41 to 2e43 erg/s; preferred few × 10^42 erg/s
    Injected high-energy electron luminosity, varied to match the continuum level and line strengths.
  • X-ray irradiation power L_X = 0, 5.3e6, 5.3e7, 1.6e8, 4.7e8, 1.4e9 L_sun; preferred 1.6e8–4.7e8 L_sun
    Added photoionizing field required to reproduce high-ionization UV lines (C III, C IV); no independent X-ray observation is presented.
  • Iron-group abundance scaling = 0.3× solar (IGE ×0.3) in preferred UV fits
    Ad hoc reduction of iron-group abundances to moderate UV line blanketing and Fe II emission strength.
  • Mixing prescription = Mildly mixed CDS ('lmix') preferred
    Hand-selected mixing level; homogeneous mixing treated as an upper limit; affects Fe II strength and UV blanketing.
axioms (5)
  • domain assumption cmfgen 1D non-LTE radiative transfer with high-energy electron deposition adequately approximates the shock interaction in Type Ibn SNe.
    Invoked throughout §3; the hydrodynamic complexity of the shock is replaced by parameterized energy deposition.
  • domain assumption The he4p0 model—a 4 M_sun helium star at the start of helium burning, pre-SN 3.15 M_sun—is representative of lower-mass stripped helium-star progenitors.
    Adopted in §3; the model is from Ertl et al. (2020) via Dessart et al. (2022), and the choice is motivated by expected helium abundances.
  • ad hoc to paper He I line strength relative to metal lines maps uniquely to initial helium-star mass in the range ~2.6–5 M_sun, excluding more massive helium stars.
    Used in §3 and §5 to argue for a low-mass progenitor; the mapping is inherited from Dessart et al. (2022) and is not independently tested here.
  • domain assumption The host galaxy is the faint galaxy PSO J129.3730-00.0431 at 0.5 arcsec, and its metallicity [Fe/H] = -1.4 ± 0.2 is correctly inferred from the luminosity–metallicity relation.
    Assumed in §2; used as environmental evidence against a massive single WR progenitor.
  • ad hoc to paper The added X-ray irradiation field is a physically plausible input even though its source is not specified.
    Introduced in §3 to produce the high-ionization UV lines; no X-ray detection or physical origin is provided.

pith-pipeline@v1.3.0-alltime-deepseek · 156 in / 11797 out tokens · 177689 ms · 2026-08-01T23:38:29.948881+00:00 · methodology

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read the original abstract

Type Ibn supernovae are stripped-envelope explosions whose spectra indicate interaction with dense, helium-rich and hydrogen-poor circumstellar material (CSM), making them important probes of late-stage mass loss and progenitor stripping. We present extensive ultraviolet-to-near-infrared spectrophotometry of the Type Ibn SN 2023tsz, including two epochs of HST/STIS ultraviolet (UV) spectroscopy and ground-based optical and near-infrared follow-up observations. The spectra are dominated by intermediate-width emission lines at all phases after maximum light, suggesting that much of the luminosity originates in a cold dense shell (CDS) formed by interaction between the ejecta and CSM. We compare the observations to one-dimensional non-local-thermodynamic-equilibrium radiative-transfer models of a helium-star explosion with a mass of $4 M_{\odot}$ at the onset of helium burning. The models reproduce the strong optical and near-infrared He I lines and require an added X-ray irradiation field to match the highly ionized UV features. The spectra are best reproduced by models with an X-ray irradiation power of $L_X \approx 10^8 L_{\odot}$, with the preferred models favoring CDS radii of order $(1.5$--$2) \times 10^{15}$ cm, velocities of $\sim 5 \times 10^7$ cm s$^{-1}$, and interaction powers of a few times $10^{42}$ erg s$^{-1}$. In the optical, the preferred models shift from higher interaction power and smaller radii at early times to lower power and larger radii at later times. These results add to the growing evidence that at least some SNe Ibn arise from lower-mass helium stars whose final evolution is shaped by binary interaction.

Figures

Figures reproduced from arXiv: 2607.15342 by Alexei V. Filippenko, Aravind P. Ravi, Asia deGraw, Bhagya M. Subrayan, Brian Hsu, Curtis McCully, D. Andrew Howell, Darshana Mehta, David J. Sand, Emily T. Hoang, Griffin Hosseinzadeh, Jeniveve Pearson, Jennifer E. Andrews, Jeonghee Rho, Joseph Farah, Justin Pierel, Kathryn Wynn, K. Azalee Bostroem, Luc Dessart, Manisha Shrestha, Megan Newsome, Melissa Shahbandeh, Moira Andrews, Nathan Smith, Neil Pichay, Nicolas E. Meza Retamal, Ori Fox, Pallas Beddow, Patrick Kelly, Peter J. Brown, Qinan Wang, Saurabh W. Jha, Schuyler D. Van Dyk, Sebastian Gomez, Seong Hyun Park, Sergiy S. Vasylyev, Stefano Valenti, Tam\'as Szalai, Thomas G. Brink, Thomas R. Geballe, Weikang Zheng, Yi Yang, Yize Dong, Yossef Zenati, Yuan Q. Ni.

Figure 1
Figure 1. Figure 1: Summary of collected photometry for SN 2023tsz. The phase is relative to the time of maximum brightness. Unfiltered photometry includes data from Gaia G, GOTO L, KAIT “Clear,” and PS1 w, and is not offset. time of discovery, so there are no nondetections from any time-domain surveys in the months beforehand. Pursi￾ainen et al. (2023b) classified it as a Type Ibn SN using a spectrum taken the next day (2023… view at source ↗
Figure 2
Figure 2. Figure 2: HST/STIS total flux density spectra of SN 2023tsz in the far-UV (top panel) and near-UV (bottom panel) regions. In the bottom panel, the top (bottom) near-UV spectrum corresponds to +9.3 d (+16.1 d) after maximum light. photometry server (Shingles et al. 2021). All the pho￾tometry we analyze is plotted in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Spectral montage from the model grid based on the exploding 4 M⊙ helium-star model from Dessart et al. (2022) placed at the distance to SN 2023tsz (116 Mpc). Top: Varying power for a fixed radius and velocity, with mixing (See discussion in Section 3). Middle: Same as top, but instead varying radius and velocity for a fixed power. Bottom: Comparison of rest-frame UV-optical model spectra for different X-ra… view at source ↗
Figure 4
Figure 4. Figure 4: Smoothed, resampled optical spectra, grouped into panels by phase, with major emission lines marked with vertical lines. The ⊕ symbol marks wavelengths excised to avoid telluric contamination. In each panel, the latest spectrum from the previous panel is repeated in gray for easy comparison. The remaining spectra (colored lines) are averaged to produce a mean spectrum in each phase bin, plotted in black. D… view at source ↗
Figure 5
Figure 5. Figure 5: The three models with the lowest RMS score for each phase, ordered best to third-best from left to right, with the phase shown at the right of each row. For each panel, RMS is the root-mean-square flux residual of that epoch; the models are scaled to a distance of 116 Mpc with no free normalization. Observed spectra (black lines) are corrected for extinction and displayed in the rest frame. Each panel show… view at source ↗
Figure 6
Figure 6. Figure 6: Bolometric (black) and pseudobolometric (filled blue) light curves of SN 2023tsz, computed with the Light Curve Fitting package (Hosseinzadeh et al. 2024), with SN 2020nxt (open blue) for comparison from Wang et al. (2024). Red points show the integrated total emergent lumi￾nosity of the best-fit models from [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The complete optical-to-NIR spectrum of SN 2023tsz at +29 d (black) compared to a model (red) with r = 3×1015 cm, v = 2 × 108 cm s−1 , and power = 1 × 1042 erg s−1 . This same model is independently the best fit to both the optical and NIR portions of the spectrum at this phase. A Keck NIRES spectrum of SN 2020nxt on day +37.5 from Wang et al. (2024) is shown in blue. Both spectra exhibit a number of inter… view at source ↗
Figure 8
Figure 8. Figure 8: UV spectra with lines labeled. HST/STIS total flux density spectra of SN 2023tsz (black) in the far-UV regions, corresponding to +9.3 d after maximum light. The spectrum is compared to that of SN 2020nxt (blue) at +10.7 days, which was scaled by a factor of 1.7 to match the continuum (Wang et al. 2024). Both spectra show very similar features and line velocities, suggesting that the bulk of the radiation a… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of continuum-normalized line pro￾files for SN 2023tsz in velocity space, grouped by epoch. The spectra are shown in the rest frame, centered on each line. Top: C IV λ1548 (blue) and He I λ5876 (black) at +9.3 d. Bottom: C II λ2325 (blue) and He I λ5876 (black) at +16.1 d (relative to maximum light). The red curve in each panel shows the He I λ5876 profile from the best-fitting model at the neare… view at source ↗
Figure 10
Figure 10. Figure 10: Best-fitting model spectra (black) for observed FUV+NUV HST/MAMA spectrum of SN 2023tsz at +9.3 days (red) after maximum light. The best-fit model corresponds to an exploding helium star (4 M⊙ initial mass at He burning) with radius r = 2×1015 cm, velocity v = 5×107 cm s−1 , power = 1×1042 erg s−1 , X-ray power 1.6×108 L⊙, and iron-group element abundance scaled by 0.3. The panels are ordered by lowest (t… view at source ↗
Figure 11
Figure 11. Figure 11: Same as [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Top-three best-fitting model spectra of 23tsz (black) to the observed STIS/HST MAMA UV spectrum on day 9.3 stitched together with the optical (red). The UV and optical were fit simultaneously. lenging, particularly in models requiring the simultane￾ous presence of C II, C III, and C IV. In this regime, the ionization balance is extremely sensitive to the inci￾dent X-ray flux; minor fluctuations can cause … view at source ↗

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