MINDS. JWST-MIRI reveals a peculiar CO$_2$-rich chemistry in the drift-dominated disk CX Tau

Aditya M. Arabhavi; Adrian M. Glauser; Alessio Caratti o Garatti; Andrew D. Sellek; Beno\^it Tabone; Danny Gasman; David Barrado; Ewine F. van Dishoeck; Fred Lahuis; Giulia Perotti

REVIEW 2 major objections 5 minor 2 cited by

MINDS. JWST-MIRI reveals a peculiar CO$_2$-rich chemistry in the drift-dominated disk CX Tau

T0 review · 2 major / 5 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read JWST-MIRI observations of CX Tau show that radial drift of icy pebbles is actively setting the inner-disk chemistry, producing a bright CO2-rich phase with cold 13CO2 and H2O emission near the snowlines.

desk verdict Solid MINDS data paper with a plausible drift/CO2-rich story; the cold 13CO2 pillar is softer than the text claims, but the cold H2O component and the CO2 excess keep the paper worth publishing. read the letter →

arxiv 2412.12715 v1 pith:2CG56JQR submitted 2024-12-17 astro-ph.EP

Marissa Vlasblom , Milou Temmink , Sierra L. Grant , Nicolas Kurtovic , Andrew D. Sellek , Ewine F. van Dishoeck , Manuel Güdel , Thomas Henning

show 15 more authors

Pierre-Olivier Lagage David Barrado Alessio Caratti o Garatti Adrian M. Glauser Inga Kamp Fred Lahuis Göran Olofsson Aditya M. Arabhavi Valentin Christiaens Danny Gasman Hyerin Jang Maria Morales-Calderón Giulia Perotti Kamber Schwarz Benoît Tabone

This is my paper · ORCID

classification astro-ph.EP

keywords protoplanetarydisksradialdriftJWST-MIRIspectroscopyCO2isotopologueswateremissionsnowlinesTTauristarsdiskchemistry

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 uses JWST-MIRI spectroscopy to argue that radial drift of icy pebbles is actively setting the chemistry of the inner disk of CX Tau, a compact T Tauri disk whose gas disk is about five times larger than its dust disk. The key evidence is a spectrum dominated by bright $\sim$450 K $^{12}$CO$_2$ emission, while the rarer isotopologue $^{13}$CO$_2$ and part of the H$_2$O emission trace a much colder $\sim$200 K component, consistent with ice sublimating near the CO$_2$ and H$_2$O snowlines. The authors propose that CX Tau has entered a CO$_2$-rich evolutionary phase: H$_2$O-rich gas delivered by drift has already drained onto the star, and comparatively CO$_2$-rich gas is now reaching the inner disk. If true, this shows that disk structure and transport, not just stellar accretion, control the volatile inventory available to planet formation, and that the CO$_2$/H$_2$O ratio is a tracer of a disk's drift-driven chemical stage.

What carries the argument

The load-bearing tool is the 0D LTE slab model, which fits each molecule's emission with three parameters: line-of-sight column density $N$, temperature $T$, and emitting area $A$, converted to a radius through $A=\pi R^2$, with a fixed Gaussian line width of 4.7 km s$^{-1}$. The model is applied sequentially to $^{12}$CO$_2$, H$_2$O, C$_2$H$_2$, $^{13}$CO$_2$, OH, and HCN in the 13.5-17.5 $\mu$m region, with H$_2$O also fit separately at 5.5-8.5 $\mu$m. The argument for drift-driven chemistry rests on comparing the $^{12}$CO$_2$ and $^{13}$CO$_2$ Q-branch shapes: the temperature-sensitive broadening shows they trace different gas, with the optically thinner isotopologue revealing a cold component near the CO$_2$ snowline, and the diagnostic H$_2$O line ratios at 23.8-23.9 $\mu$m revealing a cold $\sim$200 K water component.

What would settle it

Take a higher-S/N MIRI spectrum of CX Tau and fit the 13.5-17.5 $\mu$m region and the 21-24 $\mu$m H$_2$O lines with a two-temperature LTE model or a non-LTE model; if the $\sim$200 K $^{13}$CO$_2$ and H$_2$O components disappear or move to different temperatures, the drift interpretation loses its main evidence. Separately, sub-2 au ALMA imaging can test the predicted small inner cavity: if no $\sim$2 au cavity is found, radial drift remains the preferred explanation; if one is found, the CO$_2$ enhancement could be cavity-induced instead.

Watch

Extended reading notes

Core claim

CX Tau, a disk around a low-mass M2.5 star, shows mid-infrared molecular emission that is peculiar for a compact, drift-dominated disk: instead of the bright H$_2$O expected from efficient radial drift, its spectrum is dominated by a bright CO$_2$ feature. Slab-model fits find optically thick $^{12}$CO$_2$ emission at $\sim$450 K from an equivalent radius of $\sim$0.05 au, while $^{13}$CO$_2$ traces a colder $\sim$200 K component over a larger emitting area; H$_2$O shows a warm $\sim$500-600 K component plus a cold $\sim$200 K component at longer wavelengths. The cold $^{13}$CO$_2$ and H$_2$O components are interpreted as direct evidence that icy pebbles are drifting across the CO$_2$ and H$_2$O snowlines and sublimating, enriching the inner disk. The authors argue the bright CO$_2$ reflects an evolutionary stage in which H$_2$O-rich gas has already advected onto the star and CO$_2$-rich gas is now arriving, with the relatively weak warm H$_2$O explained by the star's low accretion luminosity. They also consider, but disfavor, an alternative in which a small $\sim$2 au inner cavity outside the H$_2$O snowline produces the CO$_2$ enhancement.

Load-bearing premise

The whole cold-component interpretation rests on the slab models that assign each molecule a single temperature and a fixed 4.7 km s$^{-1}$ line width; if the real emission has multiple temperature components or non-LTE excitation, the cold $\sim$200 K $^{13}$CO$_2$ and H$_2$O signals could be fitting artifacts rather than evidence for drifting ice, a limitation the paper itself notes for most species.

Editorial extensions

If this is right

If CX Tau is in a CO$_2$-rich phase, compact drift-dominated disks should show a time sequence in their inner-disk volatile chemistry: an early H$_2$O-rich stage, then a CO$_2$-rich stage, then carbon-rich gas, with the CO$_2$/H$_2$O ratio acting as a clock for how much ice has drifted inward and drained onto the star.
The cold $\sim$200 K $^{13}$CO$_2$ and H$_2$O components make rare isotopologues of CO$_2$ and the long-wavelength H$_2$O rotational lines practical probes of snowline sublimation, since they isolate gas that is otherwise hidden behind optically thick $^{12}$CO$_2$ emission.
Accretion luminosity must be folded into any disk size-chemistry comparison: CX Tau's H$_2$O flux is unremarkable once its low accretion rate is accounted for, so disk compactness alone does not guarantee bright water emission.
The potential detection of CO$^{18}$O, if confirmed, would provide an optically thin measurement of the total CO$_2$ column density and a cleaner tracer of the cold component than $^{13}$CO$_2$.
Higher-angular-resolution ALMA observations can discriminate between the drift scenario and the alternative explanation of a small inner cavity: a $\sim$2 au cavity should be directly detectable with sub-2 au resolution, while absence of such a cavity would leave radial drift as the preferred explanation.

Reading between the lines

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

One consequence the authors leave implicit: if drift-driven chemistry cycles CO$_2$ through the inner disk, the gas accreting onto the star and the solids building planets may shift between oxygen-rich and carbon-rich compositions on timescales shorter than the disk lifetime, so CX Tau-like disks are natural laboratories for the volatile delivery stage of planet formation.
A direct testable extension would be a survey of compact versus extended disks measuring the same diagnostic ratios (the 1500/3600 K versus 3600/6000 K H$_2$O line ratio plane, and the $^{13}$CO$_2$/$^{12}$CO$_2$ Q-branch contrast); the drift scenario predicts that compact, high R$_{\mathrm{gas}}$/R$_{\mathrm{dust}}$ disks cluster in the CO$_2$-rich corner of that plane.
The single-temperature slab fits leave large degeneracies, so the cold-component claim would be strengthened by fitting the full 13.5-17.5 $\mu$m region with a two-temperature LTE model or a non-LTE excitation model, something the paper identifies as needed future work.
If the CO$_2$-rich phase is real, the same drift mechanism should also enhance other volatiles with icelines in the outer disk (e.g., hydrocarbons) at later stages, so CX Tau may be an early snapshot in a sequence that ends with a carbon-rich inner disk.

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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

This paper is worth taking seriously, but the headline interpretation is sturdier in the abstract than in the appendix. The genuinely new stuff: first mid-IR molecular inventory of CX Tau, a compact drift-dominated disk. They detect 12CO2, 13CO2, H2O, C2H2, HCN, OH, a candidate CO18O feature, and OH prompt emission. The CO2 flux is almost an order of magnitude above the Banzatti et al. (2020) correlation with accretion luminosity, which is a clean, quantitative result. The paper does what a good MINDS paper should: it reports detections, labels the weak fits as unconstrained, and checks the step-by-step slab fits with an MCMC fit. The appendix is honest about the large uncertainties.

The soft spot is the cold 13CO2. Appendix A.1 says temperatures for everything except 12CO2 are constrained only to within 100-200 K. The best fit is ~180-200 K, so T=400 K is inside the 1σ contour. The 'T<300 K' claim in Fig. 3 comes from a visual comparison of fixed-N models at a fixed 4.7 km/s line width, not from the quoted 1σ uncertainty. That is a weaker argument than the text suggests. The MCMC check also allows an optically thin solution where column and area are degenerate. If 13CO2 is not genuinely colder than 12CO2, the 'different gas' argument and the snowline-enhancement claim lose their primary spectroscopic support.

That said, the drift scenario does not collapse. The cold ~200 K H2O component is supported by line ratios in the Banzatti et al. (2024) diagram (Fig. 8) and by a direct comparison with DR Tau. That evidence is independent of the 13CO2 fit. And the paper is explicit that an inner cavity of ~2 au or a low gas-to-dust ratio could also explain the CO2 excess; it just argues, reasonably, that drift is the preferred option. The LTE slab model with a single temperature and fixed line width is a simplification, but the authors know this and say the paper is about detections, not precise parameters.

The citation pattern is fine: Sellek, Mah, and Vlasblom modeling papers are directly relevant, and the paper doesn't hide behind them. The data reduction and fitting procedures are standard for the MINDS program. This is not a field-reorganizing result, but it is a strong single-object data point linking radial drift to inner-disk CO2 chemistry, and it will motivate the compact-disk surveys that are already underway.

Recommendation: send to a serious referee. The referee should ask for a direct statement of the 13CO2 1σ temperature range and a softening of 'significantly colder' if the contour does not exclude 300 K. That is a revision, not a rejection.

Referee Report

2 major / 5 minor

Summary. The paper presents JWST MIRI/MRS observations of CX Tau, a compact protoplanetary disk with a high gas-to-dust radius ratio indicative of strong radial drift. The authors detect H2O, 12CO2, 13CO2, C2H2, HCN, OH, H2, and possibly CO18O, and fit the molecular features with 0D LTE slab models. They find warm, optically thick 12CO2 emission at ~450 K and warm H2O at ~500-600 K, together with evidence for colder ~200 K components in 13CO2 and H2O. They interpret the bright CO2 and the cold components as signs that radial drift of icy pebbles has moved CX Tau into a CO2-rich evolutionary phase, while also discussing alternative explanations involving an inner cavity or a low gas-to-dust ratio.

Significance. If the cold 13CO2 and cold H2O components are real, the paper provides one of the clearest observational links between radial drift, snowline ice sublimation, and inner-disk chemistry in a compact disk. The work is valuable for connecting ALMA-derived disk size ratios with JWST molecular inventories, and it explicitly places CX Tau in the context of time-dependent drift models (Mah et al. 2023; Sellek et al. 2024). The paper is generally careful with weak detections, includes an MCMC cross-check of the step-by-step fitting, and quantifies CX Tau's CO2 excess relative to the Banzatti et al. (2020) sample. The principal weakness is that the two cold components that carry the central interpretation are inferred from visual or semi-quantitative comparisons rather than from formally quoted confidence intervals.

major comments (2)

[Sect. 3.2.1, Fig. 3, Appendix A.1] The claim that the 13CO2 emission is constrained to a cold temperature below 300 K is not supported by the uncertainties stated in the manuscript. Appendix A.1 says that for all species except 12CO2, temperatures are constrained only to within about 100-200 K; with a best-fit temperature near 180-200 K, the 1-sigma interval includes 300-400 K. The visual comparison in Fig. 3 uses fixed-column-density models scaled in radius to the same peak flux, which is not the same as a 1-sigma exclusion from the chi-squared map. Please show the 1-sigma and 3-sigma marginal contours for the 13CO2 temperature from Fig. A.4 or the MCMC posterior in Fig. A.5 and state explicitly whether T > 300 K is excluded. If it is not excluded, the conclusion that 13CO2 is significantly colder than 12CO2, and the drift interpretation built on that difference, need to be reworded or downgraded.
[Sect. 3.2.3, Fig. 5] The cold ~200 K H2O component is a second pillar of the drift interpretation, but it is currently established only through visual line-ratio comparisons and a rescaled comparison to DR Tau, with no chi-squared fit or quoted uncertainty. Please provide measured fluxes and uncertainties for the diagnostic H2O lines near 23.8-23.9 um and for the line ratios used in Fig. 8, and test explicitly whether a single-temperature warm model can be rejected at a formal confidence level. Without this, the statement that the cold H2O component is "clearly detected" (Sect. 3.2.3) overstates the quantitative support.

minor comments (5)

[Abstract] The phrase "and even demonstrate a potential detection" is slightly contradictory; consider "and even present evidence for a potential detection" or "and possibly detect".
[Sect. 3.2.3] The sentence "The latter have an upper level energy" should read "The latter lines have upper level energies" or similar.
[Fig. 5 caption and text] In the discussion of the left and middle panels, the terms "the former model" and "the latter" are ambiguous because three models (warm H2O, cold H2O, OH) are listed. Please refer to them explicitly as "the warm H2O model" and "the cold H2O model."
[Sect. 3.2.1 vs Fig. A.6] The column density assumed for the CO18O model is given as 5 x 10^16 cm^-2 in Sect. 3.2.1 but as 10^16 cm^-2 in the Fig. A.6 caption. Please reconcile these values.
[Sect. 3.2.4] The text says "We find evidence of OH prompt emission" after initially labeling it a "potential detection"; the Conclusions correctly list it as potential, but the main text should maintain the same level of hedging throughout.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the spectral temperatures and column densities are empirical fits, and the drift interpretation is a comparative model scenario with explicit alternatives rather than a by-construction prediction.

full rationale

The paper's derivation chain is: JWST MIRI spectrum -> continuum subtraction -> 0D LTE slab fits -> best-fit T, N, R for each molecule -> comparison with thermochemical model predictions for CO2/H2O ratios. The cold 13CO2 (~200 K) and cold H2O (~200 K) components are fitted from the data, not imposed by the drift framework; the slab model assumptions (single temperature, fixed 4.7 km/s line width, A=pi R^2) are stated and the fits are explicitly acknowledged to be weakly constrained for most species (Sect. 3.2, Appendix A.1). The interpretation leans on modeling work by Sellek et al. (2024), Mah et al. (2023), and Vlasblom et al. (2024), which share some authors with this paper, but those are independent thermochemical simulations with parameter-free, qualitative predictions (e.g., a CO2-rich evolutionary phase), and the paper openly weighs alternatives: a small inner cavity (Sect. 4.2) and a reduced gas-to-dust ratio (Sect. 4.3). The claim that the 13CO2 Q-branch shape constrains T<300 K relies partly on visual model comparison, and the quoted uncertainties (100-200 K in temperature for non-12CO2 species) mean the cold component could be less robust; however, that is a statistical robustness concern, not a circular reduction. No equation or fitted parameter is reused as its own prediction, and no load-bearing result is forced by self-citation. The paper is therefore self-contained on the observational side, with only a mild, non-load-bearing self-citation pattern in the interpretive discussion.

Assumptions & free parameters 16 free parameters · 9 assumptions · 0 invented entities

The central interpretation depends on LTE slab decomposition of weak blended lines, on literature disk and stellar parameters, on ISM isotope ratios, and on chemical evolution models from overlapping authors. None of these is unique to this paper, but they are unproven inputs for CX Tau specifically; the analysis introduces no new free physical entities, but the slab parameters are fits to the data.

free parameters (16)

12CO2 temperature = ~450 K
Best-fit LTE slab temperature from the 15 micron Q branch and P/R lines in the 13.5-17.5 micron fit (Sect. 3.2.1).
12CO2 column density = ~8 x 10^17 cm^-2
Fitted from optically thick 12CO2 lines; optical depth leaves the value uncertain.
12CO2 emitting radius = ~0.05 au
Converted from fitted emitting area A = pi R^2.
13CO2 temperature = ~180-200 K
Best fit to the 13CO2 Q branch; constrained below 300 K by line broadening (Fig. 3).
13CO2 column density = ~2 x 10^17 cm^-2
Best fit; degenerate with emitting area and possibly marginally optically thick.
13CO2 emitting radius = ~0.2 au
Converted from fitted emitting area.
H2O rotational temperature = ~500-600 K
Fitted to pure rotational lines at 13.5-17.5 microns.
H2O rotational column density = ~10^19 cm^-2 (or ~10^18 with narrower windows)
Highly sensitive to fit-window choice; MCMC gives >10^20 cm^-2.
H2O rotational emitting radius = ~0.05 au
Converted from fitted emitting area.
H2O ro-vibrational parameters = T ~500-600 K, N >10^20 cm^-2, R slightly smaller than 0.05 au
Fitted to the 5.5-8.5 micron bands; column density likely overestimated because the emission is out of LTE.
Cold H2O component temperature = ~200 K
Inferred from 23.8-23.9 micron line ratios and comparison to DR Tau; not a formal fit.
C2H2 temperature = warm, unconstrained
Fitted in the Q-branch region but degenerate with column and area; no reliable values reported.
HCN slab parameters = unconstrained
Heavily blended with H2O, CO2, and OH; the fit is not reliable and no parameters are reported.
OH LTE slab temperature = >1500 K
Fitted but not physical; traces chemical pumping rather than gas temperature.
CO18O column density = 5 x 10^16 cm^-2 (assumed)
Assumed from N(13CO2)/N(CO18O) ~ 4 using ISM 12C/13C ~ 68 and 16O/18O ~ 500, not fitted.
CO18O temperature = ~200 K
Chosen to match the residual at 15.07 microns; emitting radius scaled to fit the feature.

assumptions (9)

domain assumption The molecular emission is in local thermodynamic equilibrium, describable by a single excitation temperature for each species.
The 0D slab models in Sect. 2.2 assume LTE; the paper notes non-LTE for ro-vibrational H2O and OH prompt emission but uses LTE fits for temperature and column estimates.
domain assumption Line profiles are Gaussian with FWHM = 4.7 km/s.
Fixed in Sect. 2.2 following Salyk et al. (2011); line-width mismatch would bias the slab temperatures.
domain assumption Disk isotope ratios equal ISM values (12C/13C = 68, 16O/18O = 500).
Used to scale 13CO2 to total CO2 (Sect. 3.2.1) and to set the CO18O model column.
domain assumption CX Tau's small dust disk relative to gas disk (Rgas/Rdust ~ 5) is caused by efficient radial drift.
Taken from Facchini et al. (2019) and used to frame CX Tau as drift-dominated; if the size difference instead reflects initial conditions, the drift narrative weakens.
domain assumption Literature stellar parameters (M* = 0.37 Msun, L* = 0.22 Lsun, Teff = 3483 K, distance = 127.9 pc, inclination = 55 deg) are accurate.
Used for luminosity conversions, slab radius interpretation, and accretion luminosity comparisons.
domain assumption The fitted emitting area maps to a physical radius as A = pi R^2.
Sect. 2.2 states the radius is equivalent; for inclined disks or annulus emission the true radius differs.
domain assumption The continuum subtraction (IRSQR, quantile 0.1, knots every 25 points) does not bias the weak molecular features.
The molecular lines are faint (line-to-continuum ratios up to ~0.1); residual fringing and spline behavior could affect fluxes (Sect. 2.1).
domain assumption Chemical evolution models of Sellek et al. (2024) and Mah et al. (2023) are applicable to CX Tau.
Used in Sect. 4.1 to interpret bright CO2 as a late drift phase; applicability to this star's mass, age, and disk structure is assumed.
domain assumption OH prompt emission from H2O photodissociation preferentially populates A' symmetry states.
Basis for the OH prompt emission identification (Sect. 3.2.4, Fig. 6) via the DALI non-LTE model and van Harrevelt & van Hemert (2003).

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Cite this review

Pith. "Pith review of MINDS. JWST-MIRI reveals a peculiar CO$_2$-rich chemistry in the drift-dominated disk CX Tau." pith.science (2026). https://pith.science/paper/2CG56JQR

@misc{pith2026241212715,
  author       = {Pith},
  title        = {Pith review of: MINDS. JWST-MIRI reveals a peculiar CO$_2$-rich chemistry in the drift-dominated disk CX Tau},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2CG56JQR}},
  note         = {Machine review of arXiv:2412.12715}
}

abstract

Radial drift of icy pebbles can have a large impact on the chemistry of the inner regions of protoplanetary disks. Compact dust disks ($\lesssim$50 au) are suggested to have a higher (cold) H$_2$O flux than more extended disks, likely due to efficient radial drift bringing H$_2$O-rich material to the inner disk, where it can be observed with JWST. We present JWST MIRI/MRS observations of the disk CX Tau taken as a part of the Mid-INfrared Disk Survey (MINDS) GTO program, a prime example of a drift-dominated disk. This compact disk seems peculiar: the source possesses a bright CO$_2$ feature instead of the bright H$_2$O expected based on its efficient radial drift. We aim to provide an explanation for this finding. We detect molecular emission from H$_2$O, $^{12}$CO$_2$, $^{13}$CO$_2$, C$_2$H$_2$, HCN, and OH in this disk, and even demonstrate a potential detection of CO$^{18}$O. Analysis of the $^{12}$CO$_2$ and $^{13}$CO$_2$ emission shows the former to be tracing a temperature of $\sim$450 K, whereas the $^{13}$CO$_2$ traces a significantly colder temperature ($\sim$200 K). H$_2$O is also securely detected both at shorter and longer wavelengths, tracing a similar temperature of $\sim$500-600 K as the CO$_2$ emission. We also find evidence for a colder, $\sim$200 K H$_2$O component at longer wavelengths, which is in line with this disk having strong radial drift. The cold $^{13}$CO$_2$ and H$_2$O emission indicate that radial drift of ices likely plays an important role in setting the chemistry of the inner disk of CX Tau. Potentially, the H$_2$O-rich gas has already advected onto the central star, which is now followed by an enhancement of comparatively CO$_2$-rich gas reaching the inner disk, explaining the enhancement of CO$_2$ emission in CX Tau. The comparatively weaker H$_2$O emission can be explained by the source's low accretion luminosity. (abridged)

Figures

Figures reproduced from arXiv: 2412.12715 by the authors.

**Figure 1.** The full JWST-MIRI MRS spectrum of CX Tau. Several emission features are labeled or shown in insets, and the continuum fit is shown in red. 0 5 10 15 20 25 Flux Density (mJy) HCN CO2 OH H2O H2 0-0 S(1) 13.5 14.0 14.5 15.0 15.5 16.0 16.5 17.0 17.5 (micron) 0 5 10 15 20 25 Flux Density (mJy) Data Total model =0.9 mJy 15.35 15.40 15.45 0 5 10 13CO2 15.05 15.10 15.15 0 5 10 CO18O? 15.35 15.40 15.45 0 5 10 15.05 15.10 15… view at source ↗

**Figure 2.** [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗

**Figure 3.** A comparison of the 12CO2 (green) and 13CO2 (purple) Q branch shapes. Top: a zoom-in of the 12CO2 Q branch with the best-fit slab model plotted in the green shaded region. A model with the derived 13CO2 parameters is plotted in purple (see text). Middle: a zoom-in of the 13CO2 Q branch on the same vertical scale as the top panel, where the emission from 12CO2 and H2O has been subtracted. The best-fit slab model is p… view at source ↗

Figures from the paper (5 more)

**Figure 4.** Figure 4: Four panels showing a zoom-in of the 5.5-8.5 µm region of the CX Tau spectrum (black), together with the H2O slab model fits (blue). The four different panels show the regions which were used to perform the H2O χ 2 fits with horizontal blue bars. also indicate that it …

**Figure 5.** Figure 5: Three panels showing a zoom-in of the 21-22 µm region, the 23-24 µm region, and the 23.75-24 µm region, respectively, of the CX Tau spectrum (black). The left and middle panels show a warm H2O slab model in light pink (the best-fit model to the 13.5-17.5 µm region), a …

**Figure 6.** Figure 6: Zoom-ins of the CX Tau spectrum (black) from 9-16.5 µm, demonstrating the potential detection of OH prompt emission. The first two panels show close-ups of the 9-11 µm region, with a non-LTE DALI model from Tabone et al. (2024) (which includes both prompt emission due …

**Figure 7.** Figure 7: Comparison of the CO2 and H2O luminosities derived for CX Tau (green and blue stars, respectively) to the data shown in Banzatti et al. (2020) (shown in grey). The left panels show the H2O and CO2 luminosities as a function of accretion luminosity. The right panels sho…

**Figure 8.** Figure 8: H2O diagnostic diagram from Banzatti et al. (2024), adapted to include the measured line ratios for CX Tau. Data points from Banzatti et al. (2024) (excluding data points with upper/lower limits) are indicated with black circles and the data point for CX Tau is indica…

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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

JWST/MIRI Detection of Molecular H$_2$ Winds from an Edge-on Class II Source HV Tau C
astro-ph.SR 2026-07 conditional novelty 6.0 of 10

The edge-on Class II disk HV Tau C hosts a spatially extended, wide-angled molecular hydrogen wind with warm (~600 K) and hot (~2000 K) components and a mass-loss rate near 1e-8 solar masses per year.
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astro-ph.EP 2025-02 conditional novelty 6.0 of 10

Fragile dust destroyed beyond a dead zone limits mm-dust emission to the dead zone radius, naturally producing the compact discs seen around young stars.

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Pith tools

Reviewed August 11, 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 edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

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write newline

" write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

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