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The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones

T0 review · 4 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read This paper claims that emission from the organic molecules C2H2, HCN, and possibly CO2 in the inner regions of planet-forming disks is optically thin, so the observed mid-infrared line luminosity directly measures the total molecular mass…

desk verdict Valuable legacy dataset for JWST disk chemistry, but the headline pebble-drift trend is weak (p=0.11) and the optical-thinness argument carries a built-in correlation plus a water-subtraction caveat; still warrants serious peer review. read the letter →

arxiv 2505.07562 v2 pith:6ZI4UE4J submitted 2025-05-12 astro-ph.SR astro-ph.EP

Nicole Arulanantham , Colette Salyk , Klaus Pontoppidan , Andrea Banzatti , Ke Zhang , Karin Öberg , Feng Long , John Carr
show 15 more authors
Joan Najita Ilaria Pascucci María José Colmenares Chengyan Xie Jane Huang Joel Green Sean M. Andrews Geoffrey A. Blake Edwin A. Bergin Paola Pinilla Miguel Vioque Emma Dahl Eshan Raul Sebastiaan Krijt the JDISCS Collaboration
This is my paper · ORCID
classification astro-ph.SRastro-ph.EP
keywords protoplanetarydisksJWSTMIRIspectroscopymid-infraredmolecularemissiondiskchemistryopticallythingaspebbledriftmassaccretionrateALMAsubstructures
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 analyzes JWST mid-infrared spectra of 31 protoplanetary disks to ask what drives the chemical diversity of the gas within a few astronomical units of the star, where planets assemble. It finds that emission from acetylene (C2H2), hydrogen cyanide (HCN), and likely carbon dioxide (CO2) is optically thin, which breaks the usual degeneracy between gas amount and emitting area: the observed line luminosity is a direct measure of the total molecular mass. On that basis, it reports that C2H2 and HCN sit in hotter gas (about 920 K and 820 K) than CO2 (about 600 K), that molecular line strengths track mass accretion rate and inner-disk clearing, and that small smooth disks have less HCN relative to cold water, a signature of icy pebble drift delivering water. A sympathetic reader would care because it converts a varied collection of spectra into a demographic map linking inner-disk chemistry to outer-disk structure, the raw material for predicting planetary compositions.

What carries the argument

The load-bearing tool is the LTE slab model, a homogeneous gas layer described by temperature, column density, and projected emitting area, fitted to the 12-16 micron spectral region with Markov chain Monte Carlo after first subtracting a single-temperature water model. Its power here is that the fits return families of degenerate (column density, radius) solutions whose integrated luminosity and total mass are nearly invariant; since the luminosity-mass correlation is close to linear, the emission is optically thin, and the degeneracy converts from a flaw into a mass measurement. The ALMA sub-millimeter continuum images supply the outer-disk context, namely dust disk sizes and ring or cavity substructures, against which the inner-disk chemistry is compared.

What would settle it

Detect the 13C12CH2 isotopologue Q-branch near 13.7 microns in a C2H2-bright disk such as AS 205N: at the column densities the optically thin models require, an interstellar 12C/13C ratio near 70 predicts a readily detectable isotopologue line, so a clear non-detection would falsify the large-column-density solutions and the derived masses, while a detection at the predicted strength would confirm the mass interpretation.

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Extended reading notes

Core claim

The paper's central claim is that the organic molecules C2H2, HCN, and probably CO2 emit as optically thin gas in the inner disks of T Tauri stars, so the strong degeneracy between column density and emitting radius in slab-model fits is not a nuisance but a route to a physical quantity: total molecular mass. Fits to the 12-16 micron spectra show luminosity scaling nearly linearly with emitting mass (slope near 1 for C2H2 and HCN), as expected for optically thin emission; CO2 has a shallower slope and a cooler median temperature, suggesting it is marginally thicker. The survey also establishes higher detection rates than Spitzer for all molecules, including first detections in transition disks, and reports demographic trends: molecular luminosities correlate with accretion rate, anti-correlate with the 13-26 micron infrared spectral index, and HCN-to-cold-water ratios are low in compact, smooth disks.

Load-bearing premise

The single-temperature LTE water model is subtracted before the organic fits, and the residuals are assumed not to bias the retrieved organic temperatures and optical depths; if hot-band or non-LTE water emission leaks through, the optically thin conclusion and median temperatures could shift.

Editorial extensions

If this is right

  • Mid-infrared organic line luminosities can be used directly as relative measures of inner-disk molecular mass, removing the need to know the emitting radius.
  • Demographic comparisons with ALMA substructures become meaningful, because disks with dust rings, cavities, or spiral arms can be placed on an equal mass footing with smooth disks.
  • The correlation of C2H2, HCN, and CO2 luminosity with mass accretion rate implies that accretion-generated ultraviolet heating is a primary controller of organic line brightness.
  • The low HCN-to-cold-water ratios in compact smooth disks support pebble drift as an efficient water delivery mechanism in the absence of dust traps.
  • All measured [Ne III]/[Ne II] ratios below unity favor X-ray, not extreme-ultraviolet, irradiation as the driver of disk winds in this sample.

Reading between the lines

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

  • Because optical thinness makes line luminosity a mass tracer, future surveys could use C2H2 and HCN luminosities to map the carbon and nitrogen budgets of inner disks as functions of stellar mass and age, not just accretion rate.
  • The paper's interpretation of the pedestal features as dust rather than optically thick gas predicts that high-resolution 10 micron silicate spectroscopy of compact disks should show matching dust composition features, which is a testable extension.
  • If CO2 is only marginally optically thin, its 13CO2/12CO2 isotopologue ratio, currently detected in only one JDISCS source, offers a direct route to break the residual CO2 column-density degeneracy.
  • The authors' single-temperature water subtraction leaves open the possibility that a second water component biases organic retrievals; extending the fitting to two water components simultaneously is a natural next step.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 5 minor

Summary. The paper presents the first Cycle 1 sample analysis of the JDISCS survey: MIRI-MRS spectra of 31 protoplanetary disks with ALMA millimeter continuum imaging. The authors report near-ubiquitous H2O, OH, and CO emission, higher molecular detection rates than Spitzer-IRS, and LTE slab-model retrievals of temperature, column density, and emitting area for C2H2, HCN, and CO2 in the 12–16 µm region after subtracting a single-temperature water model. They argue that C2H2 and HCN (and possibly CO2) emission is optically thin, so the observations constrain total molecular mass rather than column density or radius separately, and that C2H2 and HCN typically arise in hotter gas than CO2. They also examine correlations with outer disk substructure, finding a tentative trend between HCN/cold-H2O luminosity ratios and dust disk size, and they show that compact-disk 'pedestals' under the organic Q branches are not explained by optically thick C2H2 models. The paper closes with atomic lines ([Ne II], [Ne III], [Ar II]) and their relation to accretion and radiation fields.

Significance. If the conclusions hold, this is a valuable demographic study: it provides a homogeneous, publicly released MIRI-MRS dataset for a sample with high-quality ALMA imaging, demonstrates sensitivity gains over Spitzer, and makes a physically important claim that the inner-disk organic emission is mainly optically thin, thereby lifting the column-density/area degeneracy for total-mass measurements. The paper is commendably explicit about its limitations: it openly discusses the single-temperature water subtraction, the exclusion of flux errors from the loss function, the partial degeneracy of N and r_slab, and the moderate statistical significance of some trends. The isotopologue non-detections and the direct comparison with optically thick models in Section 5.2 provide independent support for parts of the central argument. However, as detailed below, some load-bearing points need additional quantitative support before the headline claims can be considered established.

major comments (4)
  1. [Section 3.3.1 and Appendix A] The single-temperature LTE water subtraction is acknowledged to leave residuals that include non-LTE signatures and multiple temperature components (Appendix A), and Section 3.3.5 states that CO2 may be particularly dependent on the number of temperature components used to model the H2O. Yet no quantitative test of the impact of this subtraction on the organic retrievals is provided. Because the C2H2 (13.7 µm) and HCN (14.0 µm) Q branches sit in a wavelength region dense with rotational water lines, unsubtracted or mis-subtracted water could be absorbed into the organic slab fits and shift the retrieved temperatures, emitting masses, and inferred optical depths; this would directly propagate into the headline claims of optical thinness and of C2H2/HCN being hotter than CO2. Please add a sensitivity test for at least a subset of sources, such as fitting a two-temperature water model, masking water-dominated spectral regions before fitting the organics, or adding a non-LTE water correction factor, and report how T, M, L, and the derived optical depths change under those alternatives.
  2. [Section 4.1, Equation (2), and Figure 13] The near-unity slopes of log-L versus log-M for C2H2 and HCN are presented as evidence that the emission is optically thin, but both quantities are outputs of the same slab-model fits and are proportional by construction in the optically thin regime (L is integrated from the model spectrum, and M is derived from the same column density and area, M ∝ N A and L ∝ N A). The set of degenerate solutions within 5% of the minimum L2 norm preserves these products, so the observed slope near 1 is at least partly a consequence of the model construction rather than an independent physical measurement. The isotopologue non-detections and the τ versus N behavior in Figure 15 are more probative for optical thinness. Please either remove the L-M correlation as an argument for thinness, or test it against a null model (e.g., random draws of N and r_slab over the degeneracy set) and state explicitly what the correlation does and does not establish.
  3. [Section 5.1 and Figure 17] The abstract states that the HCN to cold-H2O luminosity ratios are generally smaller in smooth disks, but the reported Spearman correlation is ρ = 0.36 with p = 0.11, which is not significant at the p < 0.05 threshold used elsewhere in the paper (Section 4.1). The paper itself describes the trend as only marginally statistically significant, but this caveat is not carried into the abstract or the conclusions. Please report this as a tentative trend in the abstract and conclusions, or provide additional statistical support, such as a permutation test or a comparison restricted to the smooth versus structured subsamples, and state the resulting p-value.
  4. [Sections 3.3.3 and 3.3.5, and Tables 5–7] The detection rates are a headline result, but the threshold for a CO2 detection is not fully reproducible: Section 3.3.5 states that four disks are added on the basis of visual inspection of the Q branch, because any luminosity or peak-to-continuum criterion that includes them also captures non-detections. Since the reported detection rates for CO2 (58% overall) are compared to Spitzer rates and used in subsequent demographic statistics, please provide an explicit decision rule for the visual-inspection step (e.g., independent inspection by two authors, or a blind test) and quantify how the detection rate changes under alternative objective thresholds. A similar concern applies to the 'rough detection threshold' for C2H2 and HCN based on log(L) ~ −5.1 L_sun, which is not tied to a noise or model-significance estimate.
minor comments (5)
  1. [Equation (1) and Section 3.3.1] The L2 loss function omits flux uncertainties, and the 5% threshold on the L2 norm is described as 'consistent to within roughly 2σ' without a derivation; please clarify that this is not a formal goodness-of-fit or detection significance and state the number of slab models used per source for the medians reported in Tables 5–7.
  2. [Section 5.1 and Figure 13] The text referencing 'Equation 1' for the linear regressions in Figure 13 should refer to Equation (2), and the earlier cross-reference to 'Section 3.2.2' for the slab-model fits should be Section 3.3.2.
  3. [Appendix A] The appendix would benefit from a single summary figure or table showing, for a few representative disks, the residuals before and after the single-temperature water subtraction in the 13.4–14.1 µm region; this would make the magnitude of the residual water contamination more transparent than the current qualitative discussion.
  4. [Tables 5–7] The footnote for Tables 5–7 says 'Since logN and r_slab are degenerate, we do not include them in the analysis,' but the tables do list representative logN and r_slab values; please state explicitly which values are shown (e.g., one member of the degenerate family used for the figures) and how the plotted model was chosen.
  5. [Figure 9] The ordering of sources by sub-mm dust disk size in Figure 9 is useful, but the two-panel layout with temperature scales repeated on the left and right makes the figure dense; a single aligned panel with shared source labels would improve readability.

Circularity Check

1 steps flagged · score 4.0 of 10

Optical-thinness claim is partly supported by a model-internal L-M correlation; independent isotopologue and pedestal checks reduce the circularity, while the water-subtraction caveat is a separate correctness risk.

  1. self definitional [Section 4.1, Figure 13 and the logL-logM fits (unnumbered equations after 'logL(C2H2) = 1.0×logM(C2H2)+4.3')]
    "Instead, we find strong statistically significant positive correlations between the model emission line luminosities and emitting masses for all three molecules (see Figure 13; Spearman ρ=0.98,0.99,0.93). ... The relationships suggest that the emitting regions are optically thin, as an increase in emitting mass leads directly to an increase in luminosity."

    L_emit and M_emit are both outputs of the same LTE slab fits: M_emit is computed from the fitted column density and emitting area, while L_emit is integrated from the same slab model spectrum. In the optically thin regime the slab model gives L ∝ N_col A_proj f(T) = M f(T), so a fitted slope near unity is a property of the model's scaling rather than an independent empirical test. The paper uses this correlation as evidence for optical thinness and, in turn, for the claim that observations are sensitive to total molecular mass. This is partly a restatement of the model's own degeneracy structure.

full rationale

The central derivation chain is: fit LTE slab models to 12-16 μm spectra; retrieve N_col, T, and emitting area; construct M_emit and L_emit from those same fits; observe a near-unity L-M slope; conclude the organics are optically thin and that the data constrain total molecular mass. The near-unity slope is partly built into the slab scaling, since at fixed T an optically thin LTE slab has L ∝ M. Thus the L-M correlation is not an independent falsification of optical thickness. However, the paper provides separate, data-driven evidence: the 13C12CH2 non-detections in most disks exclude the high-column, optically thick solutions, and the optically thick pedestal models overpredict P/R-branch fluxes in the compact disks. These checks break the would-be circularity for the main conclusion. The remaining major caveat is correctly acknowledged in the paper itself: the single-temperature LTE water model is subtracted before fitting the organics, and Appendix A states that residual water includes non-LTE and multi-temperature signatures; Section 3.3.5 further notes CO2 may depend on the number of H2O temperature components. That is a systematic-uncertainty issue rather than a circularity. Detection-rate comparisons with Spitzer and the temperature ordering (C2H2/HCN hotter than CO2) are direct fit outputs, not inputs renamed as predictions. Self-citations to the JDISCS pipeline, Banzatti et al. (2025), and related papers are normal method/provenance citations, not load-bearing circular justifications. Overall, one partial circular step (the L-M evidence) is present, but independent constraints prevent the central claim from reducing entirely to its own model. Score 4 reflects this partial circularity with substantial independent content.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

The central claims rest on slab model fitting with several free parameters per source, and on domain assumptions about LTE, water subtraction, and the representativeness of ALMA substructures. No new physical entities are postulated.

free parameters (5)
  • Slab temperature per molecule (C2H2, HCN, CO2, H2O) = C2H2 median 920+70-130 K; HCN 820+70-130 K; CO2 600+200-160 K; H2O median 710 K
    Free parameters in LTE slab fits; reported medians are the paper's headline results, not independently derived constants.
  • Column density per molecule per source = log N roughly 14-20 cm^-2 depending on molecule and source
    Retrieved from fits but strongly degenerate with slab radius; the paper therefore reports emitting mass as the conserved quantity.
  • Slab emitting radius per molecule per source = roughly 0.2-2.5 au across the sample
    Degenerate with column density; the authors intentionally do not interpret it directly.
  • Detection threshold for organic molecules = log L = -5.1 Lsun and P/C < 0.03
    Chosen by inspecting the distribution of best-fit model luminosities and peak-to-continuum ratios; four additional CO2 disks are added by visual inspection, making the threshold partly subjective.
  • L2-norm threshold defining the family of acceptable fits = 5% above the minimum L2-norm
    Chosen to capture degenerate solutions; the paper notes it is consistent to roughly 2 sigma but provides no formal statistical justification.
assumptions (4)
  • domain assumption LTE slab model for molecular emission
    Assumes local thermodynamic equilibrium and a single temperature component per molecule; invoked in Section 3.3.1 to convert line fluxes to column density, temperature, and area.
  • ad hoc to paper Single-temperature water subtraction does not bias organic fits
    Assumed in Sections 3.3.2 and Appendix A; the paper acknowledges non-LTE and hot-band water complications but proceeds with a single-temperature subtraction.
  • domain assumption MIR lines originate in the inner few au and ALMA substructures trace the outer disk
    Used throughout Section 5 to link inner disk chemistry to outer disk structure; the paper itself notes inner disk substructures are not spatially resolved by ALMA.
  • domain assumption Stellar and accretion properties from Manara et al. (2023) are accurate
    The correlations with mass accretion rate and stellar mass depend on this compiled table, which aggregates heterogeneous literature measurements.

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Cite this review

Pith. "Pith review of The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones." pith.science (2026). https://pith.science/paper/6ZI4UE4J

@misc{pith2026250507562,
  author       = {Pith},
  title        = {Pith review of: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6ZI4UE4J}},
  note         = {Machine review of arXiv:2505.07562}
}
abstract

Mid-infrared spectroscopy of protoplanetary disks provides a chemical inventory of gas within a few au, where planets are readily detected around older stars. With the JWST Disk Infrared Spectral Chemistry Survey (JDISCS), we explore demographic trends among 31 disks observed with MIRI (MRS) and with previous ALMA millimeter continuum imaging at high angular resolution (5-10 au). With these S/N $\sim$200-450 spectra, we report emission from H$_2$O, OH, CO, C$_2$H$_2$, HCN, CO$_2$, [Ne II], [Ne III], and [Ar II]. Emission from H$_2$O, OH and CO is nearly ubiquitous for low-mass stars, and detection rates of all molecules are higher than for similar disks observed with Spitzer-IRS. Slab model fits to the molecular emission lines demonstrate that emission from C$_2$H$_2$, HCN, and possibly CO$_2$ is optically thin; thus since column densities and emitting radii are degenerate, observations are actually sensitive to the total molecular mass. C$_2$H$_2$ and HCN emission also typically originate in a hotter region ($920^{+70}_{-130}$, $820^{+70}_{-130}$ K, respectively) than CO$_2$ ($600^{+200}_{-160}$ K). The HCN to cold H$_2$O luminosity ratios are generally smaller in smooth disks, consistent with more efficient water delivery via icy pebbles in the absence of large dust substructures. The molecular emission line luminosities are also correlated with mass accretion rates and infrared spectral indices, similar to trends reported from Spitzer-IRS surveys. This work demonstrates the power of combining multi-wavelength observations to explore inner disk chemistry as a function of outer disk and stellar properties, which will continue to grow as the sample of observed Class II systems expands in the coming JWST observation cycles.

Figures

Figures reproduced from arXiv: 2505.07562 by the authors.

Figure 1
Figure 1. MIRI spectra of select targets from the JDISCS sample, representing broad categories of sources, namely: intermedi￾ate mass, transition disk (with a large dust cavity), solar-mass with weak water emission, solar-mass with strong water emission, and a low-mass star. Emission lines from prominent atomic and molecular gas, and solid state features, are highlighted with labels. radius, and accretion rate. Distances for … view at source ↗
Figure 2
Figure 2. Summary of stellar and disk properties for 30/31 JDISCS targets included in this work, including mass accre￾tion rates (y-axis), sub-mm dust disk radii enclosing 90-95% of the flux at ∼1.3 mm (x-axis), and stellar masses (marker colors). The sample spans ∼4 orders of magnitude in mass accretion rate, ∼2 orders of magnitude in dust disk sizes, and a narrow range in stellar masses (27 K- and M-type T Tauri stars, one … view at source ↗
Figure 3
Figure 3. MRS continuum-subtracted spectra of C2H2 (magenta), HCN (green), H2O (blue), and CO2 (brown) emission lines between 13.6-15.3 µm from JDISCS sources with sub-mm dust sizes r > 63 au. ALMA images are shown to the right of the spectra (Andrews et al. 2018; Long et al. 2018, 2019a, Long et al. 2025, in prep), in order of sub-mm dust disk size from largest (top left; Elias 27, r ∼ 250 au) to smallest (bottom right; RU L… view at source ↗
Figures from the paper (16 more)
Figure 4
Figure 4. Figure 4: MRS continuum-subtracted spectra of C2H2 (magenta), HCN (green), H2O (blue), and CO2 (brown) emission lines between 13.6-15.3 µm from JDISCS sources with sub-mm dust sizes r < 60 au. ALMA images are shown at right (Andrews et al. 2018; Long et al. 2018, 2019a, Long et …
Figure 5
Figure 5. Figure 5: Gallery of ro-vibrational CO, OH, [Ne II], and [Ne III] emission lines from 30/31 JDISCS sources (HD 163296 is excluded due to poor data quality). The spectra are in order from largest to smallest sub-mm disk size, with representative slab models of H2O overplotted on …
Figure 6
Figure 6. Figure 6: Left: Example corner plot, showing the strong degeneracy between column density and slab radius in LTE slab model fits to the C2H2 emission from AS 205N. The effect is still apparent when HCN and CO2 emission lines are included in the fit. Right: Degenerate slab model …
Figure 7
Figure 7. Figure 7: MIRI-MRS spectrum of the brightest disk between 12-16 µm in our sample, AS 205N (black), with slab model fits to emission lines from H2O (blue), C2H2 (magenta), HCN (green), and CO2 (brown), as an example of a JDISCS target with prominent emission lines from all four m…
Figure 8
Figure 8. Figure 8: Emission line luminosities from best-fit slab models (integrated between 12-16 µm) versus peak-to-continuum values from the slab models and fit to the continuum, with marker styles indicating the spatially resolved sub-mm structures in [PITH_FULL_IMAGE:figures/full_fi…
Figure 9
Figure 9. Figure 9: Retrieved temperatures from slab model fits to C2H2 (top, magenta), HCN (middle, green), and CO2 (bottom, brown) emission lines from JDISCS sources in order of decreasing sub-mm disk size from top to bottom of each panel. Vertical dashed lines and shaded regions repres…
Figure 10
Figure 10. Figure 10: Emission line luminosities (left) and emitting masses (right) integrated from slab model fits to C2H2, HCN, and CO2 between 12-16 µm in JDISCS sources. Despite spanning a limited range in stellar masses, the targets display at least an order of magnitude variation in …
Figure 11
Figure 11. Figure 11: Detection rates of CO, H2O, HCN, C2H2, CO2 and OH for K and M stars in this sample of MRS spectra. Hatches show IRS or ground-based (for CO) detection rates from Pontoppidan et al. (2010). Earlier spectral types are excluded from this plot due to low number statistics…
Figure 12
Figure 12. Figure 12: Median emission line luminosities from C2H2 (left), HCN (middle), and CO2 (right) versus the median slab temperatures measured from the 100 best-fit slab models for each disk, with markers representing the sub-mm dust substructures listed in [PITH_FULL_IMAGE:figures/…
Figure 13
Figure 13. Figure 13: Median emission line luminosities from C2H2 (left), HCN (middle), and CO2 (right) versus the median emitting masses measured from the best-fit slab models for each disk, with marker styles indicating the sub-mm dust substructures listed in [PITH_FULL_IMAGE:figures/fu…
Figure 14
Figure 14. Figure 14: Retrieved temperatures from C2H2 (left), HCN (middle), and CO2 (right) versus the median emitting masses measured from the best-fit slab models for each disk, with marker styles indicating the sub-mm dust substructures listed in [PITH_FULL_IMAGE:figures/full_fig_p030…
Figure 15
Figure 15. Figure 15: Optical depths versus column densities for the combinations of C2H2 (magenta), HCN (green), and CO2 (brown) slab model parameters that best reproduce the spec￾trum of AS 205N; markers with stars correspond to the col￾umn densities used in [PITH_FULL_IMAGE:figures/ful…
Figure 16
Figure 16. Figure 16: Emission line luminosities measured from the best-fit slab models versus the infrared spectral indices measured between 13 and 26 µm (top) and the literature mass accretion rates (bottom). Both trends are consistent with the Spitzer results reported in Banzatti et al.…
Figure 17
Figure 17. Figure 17: Left: Ratios of C2H2 to CO2 integrated emission line luminosities versus sub-mm dust disk sizes from [PITH_FULL_IMAGE:figures/full_fig_p033_17.png]
Figure 18
Figure 18. Figure 18: Subset of JDISCS Cycle 1 targets with retrieved C2H2 slab temperatures of ∼1000 K, required to reproduce broader “pedestal”-like emission than observed in the other disks from our sample (magenta; full models from [PITH_FULL_IMAGE:figures/full_fig_p034_18.png]
Figure 19
Figure 19. Figure 19: Left: C2H2 emission line luminosities versus [Ne II] emission line fluxes. Right: C2H2 slab temperatures versus [Ne III] to [Ne II] flux ratios. In both panels, marker colors represent mass accretion rates (see also, Colmenares et al. 2024). Upper limits are omitted f…

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Forward citations

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