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The paper claims that inner-disk chemistry is already established in Class I/FS disks and that, after removing the effect of accretion luminosity, cold water and CO2 masses anti-correlate with disk radius, indicating icy pebble drift delive

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2026-08-01 04:22 UTC pith:C3KBIBVB

load-bearing objection First JWST/MIRI survey of embedded Class I/FS disks: genuinely new empirical data, but the pebble-drift interpretation leans on an uncalibrated Lacc conversion and a size-mismatched sample. the 3 major comments →

arxiv 2607.22839 v1 pith:C3KBIBVB submitted 2026-07-24 astro-ph.EP astro-ph.GAastro-ph.SR

The JDISC Survey: Inner Disk Chemistry of Class I/FS Disks and Tentative Evidence for Early Pebble Drift

Ke Zhang , Andrea Banzatti , Colette Salyk , Abygail Waggoner , Klaus Pontoppidan , Mar\'ia Jos\'e Colmenares , Ilaria Pascucci , Lucas A. Cieza
show 17 more authors
Miguel Vioque Paola Pinilla Geoffrey A. Blake Joan Najita Joe Williams Sebastiaan Krijt Till Kaeufer Jane Huang Feng Long Chengyan Xie Minjae Kim Eshan Raul Dary A. Ru\'iz-Rodr\'iguez Nicole Arulanantham Beno\^it Tabone Mayank Narang Karina Mauco
This is my paper
classification astro-ph.EP astro-ph.GAastro-ph.SR
keywords protoplanetary disksClass I/FS disksJWST MIRI/MRSdisk chemistrypebble driftwater emissionCO2accretion luminosity
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.

This paper reports the first JWST mid-infrared survey of Class I and Flat-Spectrum disks — young embedded planet-forming disks less than about a million years old — and compares them to older, more evolved Class II disks of similar stellar mass. It finds that water, HCN, C2H2, and CO2 are routinely detected in the young disks, at rates and excitation temperatures comparable to the older disks, so the inner-disk chemical reservoir is established earlier than previously characterized. After statistically removing the dominant effect of accretion luminosity, the paper finds that cold (~200 K) water and CO2 gas masses anti-correlate with the size of the millimeter dust disk, while hot water tracks accretion luminosity and not disk size. The authors interpret this as the imprint of icy pebbles drifting inward and sublimating, enriching the inner disk early; a tentative excess of cold water in the young sample and colder CO2 fit a predicted 'water-rich, CO2-poor' early phase. The results are exploratory, limited by small samples, but set up a testable evolutionary framework.

Core claim

The central claim is that inner-disk chemistry is already well established in Class I/FS disks: at inclinations below 70°, water, HCN, C2H2, and CO2 are detected at rates and excitation conditions broadly comparable to Class II disks, placing the onset of chemically rich inner-disk environments earlier than previously characterized. The supporting statistical claim is that, once accretion luminosity is controlled for, cold water and CO2 observable masses anti-correlate with mm-dust disk radius (best-fit slopes -0.34 and -0.44, each excluding zero at the 2-sigma level in the combined sample), whereas hot water is insensitive to disk size. The authors argue that this dichotomy — hot water set

What carries the argument

The analysis relies on three components: (1) mid-infrared spectroscopy with JWST/MIRI resolving molecular rovibrational and rotational lines; (2) multi-component LTE slab modeling, which decomposes water into hot (~900 K), warm (~460 K), and cold (~200 K) components and retrieves temperature, column density, emitting area, and observable mass for each molecule; and (3) a multivariate weighted regression on standardized (z-scored) accretion luminosity and dust disk radius, which separates the two opposite-signed drivers and yields the partial slopes that isolate the pebble-drift signature. The underlying physical mechanism invoked is the inward drift of icy pebbles crossing successive snowlin

Load-bearing premise

The conversion from hydrogen recombination line (HI 10-7) luminosity to accretion luminosity, calibrated on older Class II stars, is assumed to hold for embedded Class I/FS sources; the paper states this conversion 'has not been calibrated for embedded systems,' so if it is systematically biased, the partial residuals that reveal the cold-water and CO2 anti-correlations could be artifacts.

What would settle it

Measure the accretion luminosity of a sample of Class I/FS sources with an independent method (e.g., modeling the UV/optical excess) and compare to the HI(10-7)-derived values; if the two disagree systematically as a function of disk size, the reported anti-correlations would need to be re-derived. Alternatively, a null result from a larger sample with matched disk-size distributions would falsify the evolutionary framework.

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

If this is right

  • Inner-disk chemistry matures by the Class I stage, so planet-forming material is already chemically processed within the first million years.
  • Compact disks should show systematically stronger cold water and CO2 emission at fixed accretion rate, giving a direct observational handle on which disks are currently experiencing efficient pebble drift.
  • The CO2-to-water ratio should rise as disks age, because water is delivered first and CO2 later; tracking this ratio across bolometric temperature or age tests the proposed evolutionary sequence.
  • Disk substructures (gaps) located between the water and CO2 snowlines should suppress cold water delivery without suppressing CO2, a prediction that can be checked with larger samples.
  • Class I/FS disks with edge-on geometry will appear molecule-poor, so inclination must be accounted for in any census of embedded-disk chemistry.

Where Pith is reading between the lines

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

  • The paper tabulates hydrogen recombination line luminosities so that any future recalibration of the accretion-luminosity conversion can be applied without re-observing; this makes the weakest assumption directly testable.
  • A natural extension is to apply the same accretion-controlled regression to OH or rare isotopologues, which could separate thermal-production from drift-replenishment pathways more cleanly.
  • If the pebble-drift interpretation holds, then the cold-water excess should correlate with the absence of millimeter substructure in individual disks, an ALMA-testable prediction not made in the paper.
  • The framework implies that the terrestrial-planet-forming zones of compact disks are oxygen-enriched early on, which could leave imprints in the C/O ratios of forming planets; connecting to exoplanet atmospheric compositions would be a downstream consequence.

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 / 5 minor

Summary. The paper presents the first JWST MIRI/MRS chemical survey of Class I and Flat-Spectrum disks, targeting 16 Ophiuchus sources, and compares seven low-inclination (i<70°) objects with 12 low-mass Class II disks from the public JDISCS sample. Using empirical line luminosities, line ratios, and 0D LTE slab models, it finds that H2O, HCN, C2H2, and CO2 are detected at rates and excitation temperatures broadly similar to Class II disks, with a tentative cold-water excess (1.4σ) and colder CO2 (1.5σ) in Class I/FS sources. The central quantitative claim is the multivariate regression of Eq. (2): after controlling for HI-based accretion luminosity, cold H2O (b_Rd=-0.34) and CO2 (b_Rd=-0.44) masses anti-correlate with mm-dust disk radius at 2σ in the combined sample, while hot water scales with Lacc and is insensitive to disk size. This is interpreted as evidence for early inward pebble drift and a water-rich evolutionary phase before Class II.

Significance. If the underlying trends hold, the paper would provide an important observational benchmark: inner-disk molecular chemistry is already established in Class I/FS disks, and compact young disks are preferentially enriched in cold volatiles. The statistical toolkit is a genuine strength: censored Kendall tau incorporates upper limits, BH-FDR correction is applied (and none of the univariate tests survive it), bootstrap medians and power analyses are reported, and the HI line luminosities are tabulated so the Lacc conversion can be recomputed. The line images and velocity checks help exclude a dominant outflow contribution. The main risk is that the paper's most interesting quantitative conclusion depends on an admittedly uncalibrated HI(10-7)-to-Lacc conversion applied to embedded sources, combined with a small and non-overlapping sample. The paper is honest about this, but it does not quantify the vulnerability.

major comments (3)
  1. [§4.4.2, Eq. (2) and §5.4] The 2σ slopes b_Rd=-0.34 (cold water) and b_Rd=-0.44 (CO2) are the load-bearing quantitative evidence for the pebble-drift interpretation. These partial slopes assume the HI(10-7)-to-Lacc conversion is on the same scale for embedded Class I/FS and Class II sources; §5.4 states it 'has not been calibrated for embedded systems.' Since Class I/FS disks are systematically more compact (median Rd ~13 au vs ~54 au, Fig. 1), any class-dependent Lacc offset can masquerade as an Rd anti-correlation in the partial residuals. Please add a sensitivity analysis: apply a plausible range of offsets to the Class I/FS Lacc values in the combined regression and report the offset needed to bring b_Rd to zero, or include a class indicator in the regression to show the slopes are stable.
  2. [§4.4.2, Fig. 10] The 2σ combined-sample slopes are estimated from only 15 sources: 11 Class II with detected Lacc plus 4 Class I/FS with detected Lacc (Oph 3, 5, 7, 15). The Class II-only cold-water slope is not significant (b_Rd=-0.16), and none of the univariate censored Kendall tests survive BH-FDR. It is therefore critical to show that the combined result is not driven by the four Class I/FS points or by sample composition. Please report leave-one-out fits, a Class II-only regression with the same method, and a version with a class dummy. Without such tests, the claim that disk size—rather than evolutionary class—governs cold water and CO2 is under-supported.
  3. [§5.2 / Fig. 11] The evolutionary interpretation also uses Tbol as a relative age indicator and compares observed CO2/H2O(cold) ratios with Sellek et al. model tracks. The text acknowledges the data cannot distinguish gap scenarios, and the observed trend is only tentative. This is acceptable for an exploratory paper, but the conclusion should make clearer that the Tbol trend is not a statistically significant correlation and that the evolutionary sequence in Table 4 is a qualitative framework rather than a tested model.
minor comments (5)
  1. [§3.3] The Lacc calibration is cited as 'Tofflemire et al. 2025; Shridharan et al. 2026 and updated in Hyden et al. 2026 (in prep)'. The Hyden et al. in-prep reference does not appear in the reference list; please either add it or identify the version used.
  2. [§4.4.2] 'all 15 sources (after excluding Lacc upper limits)' is easy to misread: 11 Class II plus 4 Class I/FS. Please state the sample composition explicitly in the text or figure caption.
  3. [Table 1 / §2.1] For Oph 11-16 the stellar masses are adopted from McClure et al. (2010) and 'Ruiz-Rodriguez et al. in prep'; the in-prep citation should be resolved or replaced with a public reference where possible.
  4. [§3.4] The slab-model section correctly notes the area-column density degeneracy and the lower-limit nature of observable masses; it would help to state explicitly that the mass ratios used in Fig. 11 inherit that degeneracy, though the ratio is less sensitive to it.
  5. [Figure 11] The upper panel shows model tracks while the lower panel shows observed data on an age/Tbol axis. The caption should make clear that no direct quantitative fit to the tracks is made; the comparison is qualitative, as stated in the text.

Circularity Check

0 steps flagged

No significant circularity: empirical measurements are independent of the qualitative pebble-drift comparison; the main caveat is an uncalibrated Lacc conversion, which is a stated systematic uncertainty rather than a definitional reduction.

full rationale

The paper's derivation chain is empirical and self-contained. Molecular masses come from LTE slab fits to MIRI spectra; accretion luminosities are derived from a separate HI(10-7) line; dust disk radii are measured from mm continuum. These are independent observables, and the multivariate regression (Eq. 2) is a statistical description of their correlations, not a prediction fitted from the same quantity it claims to explain. The pebble-drift interpretation is qualitative and relied on external models (e.g., Sellek et al. 2025), which are not calibrated to the observed masses. Self-citations to the JDISCS pipeline and companion papers provide data-reduction and comparison-sample context but do not force the central anti-correlations. The paper explicitly acknowledges the one load-bearing assumption—that the HI(10-7)-to-Lacc conversion, calibrated on Class II/T Tauri stars, holds for embedded Class I/FS systems—as uncalibrated (Section 5.4). That is a legitimate systematic uncertainty and a possible source of bias, but it is not a circular reduction: nothing in the paper defines the target result in terms of itself. No fitted parameter is renamed as a prediction, no uniqueness theorem is imported from the authors, and no ansatz is smuggled in by citation. Therefore the paper has very low circularity burden, consistent with an honest exploratory survey.

Axiom & Free-Parameter Ledger

3 free parameters · 4 axioms · 0 invented entities

The paper is an observational fitting survey; its central claims rest on adopted empirical calibrations (HI-Lacc, extinction law), model assumptions (LTE slab with priors), and sample-matching assumptions. No new theoretical entities are introduced.

free parameters (3)
  • HI(10-7)-to-Lacc empirical coefficients = not listed (Tofflemire et al. 2025; Shridharan et al. 2026; Hyden et al. in prep)
    Used to convert HI(10-7) line luminosities to accretion luminosities for both Class I/FS and Class II samples; this relation is a key input to the multivariate regressions that separate Lacc from disk-size effects.
  • Extinction law normalization and exponent = τ_ext = 0.085 λ^{-0.25} A_V; A_K = A_V/7.75
    Adopted from McClure (2009) to deredden Class I/FS spectra before line flux and slab modeling; AV taken from heterogeneous literature values.
  • Slab model prior ranges = T_water: 500-1500/200-800/100-400 K; T_others: 100-2000 K; logN: 12-22; logA: -4 to 4
    Uniform priors in the MCMC slab retrievals; the hot/warm/cold decomposition and prior ranges shape the derived component masses, especially for upper limits.
axioms (4)
  • domain assumption The MIRI molecular emission in i<70° Class I/FS sources originates predominantly in the inner disk, not the envelope or outflow.
    Supported by spatially unresolved water line images and lack of velocity shifts >15 km/s (Section 2.3, Appendix C), but a compact sub-arcsecond outflow cannot be fully ruled out (Section 5.3).
  • domain assumption LTE 0D slab models reliably recover the observable molecular mass and excitation temperature of the line-emitting layer.
    The paper notes masses are lower limits, components are emission-weighted averages, and HCN/C2H2/CO2 may be sub-thermal (Section 3.4); it cites retrieval benchmarks on synthetic spectra (Kaeufer et al. 2024; Vlasblom et al. 2025a) as support.
  • domain assumption The Class II comparison sample, selected by M*≤0.7 Msun, is an appropriate evolutionary counterpart to the Class I/FS sample.
    The paper restricts Class II to similar stellar mass but acknowledges the Class II sample is mm-bright/large-disk biased and the Class I/FS subsample has a higher fraction of very low-mass stars (Sections 2.2, 5.3, 5.4).
  • domain assumption Literature AV values and the McClure (2009) extinction law are accurate for the Class I/FS sources.
    Extinction correction is applied before line flux measurement; AV taken from multiple heterogeneous studies, so residual systematics propagate into absolute fluxes and masses (Appendix D).

pith-pipeline@v1.3.0-alltime-deepseek · 51928 in / 15067 out tokens · 140784 ms · 2026-08-01T04:22:22.361166+00:00 · methodology

0 comments
read the original abstract

We present the first chemical survey of Class I and Flat-Spectrum (I/FS) disks using JWST MIRI/MRS, targeting sixteen sources in the Ophiuchus star-forming region. Through empirical line luminosity measurements and multi-component slab modeling, we characterize the molecular reservoir of these young systems and compare them to twelve Class II disks of similar stellar mass. Water, HCN, C$_2$H$_2$, and CO$_2$ are frequently detected in I/FS sources with inclinations $i < 70^{\circ}$, whereas edge-on systems show significantly suppressed emission. Compared to Class II disks, I/FS sources show suggestive---though not yet statistically significant---evidence for elevated cold water ($\sim$200\,K) mass and lower CO$_2$ excitation temperatures. Statistical analyses identify accretion luminosity as the primary correlate of molecular mass across both evolutionary stages. Once this dependence is removed, cold water and CO$_2$ masses anti-correlate with mm-dust disk radius, while hot water remains insensitive to disk size. These patterns are qualitatively consistent with pebble drift models that predict early water enrichment followed by delayed CO$_2$ delivery, suggesting an evolutionary progression from molecular-poor Class 0 sources, through water-rich Class I/FS disks, to Class II disks with reduced cold water excess. This work provides an initial evolutionary framework for disk chemistry that requires larger, multi-region samples to confirm.

Figures

Figures reproduced from arXiv: 2607.22839 by Abygail Waggoner, Andrea Banzatti, Beno\^it Tabone, Chengyan Xie, Colette Salyk, Dary A. Ru\'iz-Rodr\'iguez, Eshan Raul, Feng Long, Geoffrey A. Blake, Ilaria Pascucci, Jane Huang, Joan Najita, Joe Williams, Karina Mauco, Ke Zhang, Klaus Pontoppidan, Lucas A. Cieza, Mar\'ia Jos\'e Colmenares, Mayank Narang, Miguel Vioque, Minjae Kim, Nicole Arulanantham, Paola Pinilla, Sebastiaan Krijt, Till Kaeufer.

Figure 1
Figure 1. Figure 1: Comparison of stellar and disk properties between the Class I/FS (i < 70◦ ) and Class II samples. The horizontal bars show the median values of each group. The p-values shown are from a Mann-Whitney U test (also known as the Wilcoxon rank-sum test) comparing the distributions of each property between the two samples. This non-parametric test assesses whether the two classes are drawn from the same underlyi… view at source ↗
Figure 2
Figure 2. Figure 2: Top panel: JWST MIRI/MRS spectra of two representative Ophiuchus Class I/FS sources — Oph 11 (molecule-rich, blue) and Oph 8 (molecule-poor, grey) — with ice absorption features highlighted (shaded bands). Bottom panel: extinction– corrected, continuum-subtracted spectra of the twelve sources with water emission detections (13–25 µm). noise level per resolution element. This lower thresh￾old is adopted bec… view at source ↗
Figure 3
Figure 3. Figure 3: Detection rate comparison among the Ophiuchus Class I/FS disks. 14) do not have inclination constraints because their mm images are spatially unresolved. The suppressed emis￾sion in high-inclination systems likely reflects geometric effects (e.g., A. Somigliana et al. 2026): at i > 70◦ , the optically thick outer disk and residual envelope obscure the line-emitting inner disk, while the continuum further d… view at source ↗
Figure 4
Figure 4. Figure 4: Line luminosities as a function of accretion luminosity. Top: diagnostic water lines. Bottom: HCN, C2H2, and CO2. The Class I/FS and II samples generally follow the same trends, but Class I/FS shows larger scatter in the water lines. The grey dashed line and shaded band show the censored linmix fit (B. C. Kelly 2007) to the Class II reference sample (16th–84th percentile of the posterior), which includes t… view at source ↗
Figure 5
Figure 5. Figure 5: Water line luminosity diagnostic plot. Left: the line luminosities of hot and cold water transitions cover similar luminosity range and trend as the Class II sample. The grey dashed line and shaded band show the censored linmix fit to the Class II reference sample (16th–84th percentile), and the blue dashed line shows the corresponding Class I/FS (i < 70◦ ) linmix fit (both hot-water axes are fully detecte… view at source ↗
Figure 6
Figure 6. Figure 6: Slab models of i< 70◦ Class I/FS sample, for the 13-16.5 and 20-26.5 µm wavelength ranges [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of slab model parameters between Class I/FS (i < 70◦ , blue) and Class II (grey) disks. Top panel: excitation temperatures for the three water components (hot, warm, cold), HCN, C2H2, and CO2. Bottom panel: log emitting masses for the same species. Individual sources are shown as points; violin plots show the kernel density estimate of each distribution, and horizontal bars mark the median. Uppe… view at source ↗
Figure 8
Figure 8. Figure 8: Violin plots of molecular mass ratios for Class I/FS (i < 70◦ , blue) and Class II (grey) disks. Top panel: mass ratios normalized to hot water. Bottom panel: mass ratios normalized to cold water. Individual sources are shown as points, with upper limits indicated by downward arrows. When normalized to hot water, the ratios of HCN, C2H2, and CO2 are similar between the two classes, but the cold-to-hot wate… view at source ↗
Figure 9
Figure 9. Figure 9: Generalized Kendall τ correlation coefficients between slab model molecular properties and disk/stellar properties. Each panel corresponds to a different disk/stellar property: dust radius (Rdust), dust mass (Mdust), accretion luminosity (Lacc), stellar luminosity (L⋆), and stellar age. The first three panels show results for the Class I, Class II, and combined samples separately; the stellar luminosity an… view at source ↗
Figure 10
Figure 10. Figure 10: Partial residuals from the multivariate regression of log slab mass on z-scored log Rdust and log Lacc, for the Class II (left) and Combined (right) samples. Rows correspond to the six molecular tracers and columns to the two predictors. The band color indicates the significance of the slope: red = strongly significant (2σ; 5–95% CI excludes zero), orange = significant (1σ; 16–84% CI excludes zero), blue … view at source ↗
Figure 11
Figure 11. Figure 11: The ratio of observable masses of CO2 and H2O(cold) as a function of bolometric temperature, an age indicator for Class I/FS and isochrone age for Class II. Blue points are Class I/FS detections; downward triangles indicate CO2 upper limits. Grey points are Class II sources, with circled symbols indicating disks with known dust gaps. The top panel shows the predicted CO2/H2O mass ratio evolution from the … view at source ↗
Figure 12
Figure 12. Figure 12: Partial residuals of cold water (top) and CO2 (bottom) slab mass against z-scored log Rdust, after removing the Lacc dependence from the multivariate regression. Panels show Class II (left) and the combined sample (right). Symbol styles indicate disk substructure: filled circles for disks with no known gaps, single-ring symbols for shallow gaps, and double-ring symbols for deep gaps. In the Class II cold … view at source ↗
Figure 13
Figure 13. Figure 13: Continuum-subtracted line images of H2 S(5) (6.91 µm), [Ne II] (12.81 µm), and H2O (23.8 µm) for all 16 Class I/FS sources. Each row shows one source; columns are the three lines. The white star in each panel marks the peak of the normalized continuum image measured near the wavelength of each line, i.e., the location of the central source, which is not necessarily at the center of each image. Each panel … view at source ↗
Figure 14
Figure 14. Figure 14: Extinction correction example for Oph 10 [PITH_FULL_IMAGE:figures/full_fig_p032_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Mass ratios relative to hot water as a function of accretion luminosity. Blue points are Class I/FS sources and grey points are Class II sources. No statistically significant correlations are found. 7.0 6.5 6.0 lo g Msla b (M ) H2O (hot) 6.0 5.5 5.0 4.5 H2O (warm) 6 5 4 H2O (cold) 9.0 8.5 8.0 7.5 HCN 9.5 9.0 8.5 8.0 C2H2 8.0 7.5 7.0 6.5 CO2 2.6 2.8 log Tbol (K) 0.25 0.50 0.75 1.00 1.25 1.50 lo g M a s s R… view at source ↗
Figure 16
Figure 16. Figure 16: Slab model masses and mass ratios relative to bolometric temperature. Blue points are Class I/FS sources and grey points are Class II sources [PITH_FULL_IMAGE:figures/full_fig_p034_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Slab model masses and mass ratios as a function of estimated age for the Class II sample. 10 8 6 4 lo g Msla b (M ) H2O (hot) 10 8 6 4 2 0 H2O (warm) 8 6 4 2 H2O (cold) 2 1 0 log Lacc (L ) 9.0 8.5 8.0 7.5 7.0 lo g Msla b (M ) HCN 2 1 0 log Lacc (L ) 9.5 9.0 8.5 8.0 7.5 C2H2 2 1 0 log Lacc (L ) 8 7 6 CO2 Class I Class II Mol. upper limit Lacc upper limit Class I fit Class II fit Combined fit [PITH_FULL_IM… view at source ↗
Figure 18
Figure 18. Figure 18: Slab model masses of water and organic species as a function of accretion luminosity. Blue points are Class I/FS sources and grey points are Class II sources. Left-pointing arrows indicate sources with upper limits on Lacc. Only statistically significant correlations (censored Kendall τ p < 0.1) are shown; linear fits are computed with linmix (B. C. Kelly 2007), which incorporates upper limits on either a… view at source ↗
Figure 19
Figure 19. Figure 19: Slab model masses and mass ratios as a function of mm dust disk size. Blue points are Class I/FS sources and grey points are Class II sources [PITH_FULL_IMAGE:figures/full_fig_p038_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: Comparison of slab model emitting areas and column densities between Class I/FS (i < 70◦ , blue) and Class II (grey) disks. Format is the same as [PITH_FULL_IMAGE:figures/full_fig_p039_20.png] view at source ↗
Figure 21
Figure 21. Figure 21: Standardized partial regression slopes of log slab mass on z-scored log Rdust (bRd ) and log Lacc (bLacc ) for the Class I, Class II, and Combined samples. Each slope quantifies the partial effect of one predictor while controlling for the other. Red and blue indicate positive and negative slopes, respectively. Colored cells are statistically significant: full opacity for the 5–95% bootstrap confidence in… view at source ↗
Figure 22
Figure 22. Figure 22: H-R diagram of Class II sources McClure, M. 2009, ApJL, 693, L81, doi: 10.1088/0004-637X/693/2/L81 McClure, M. K., Furlan, E., Manoj, P., et al. 2010, ApJS, 188, 75, doi: 10.1088/0067-0049/188/1/75 Murillo, N. M., Lai, S.-P., Bruderer, S., Harsono, D., & van Dishoeck, E. F. 2013, A&A, 560, A103, doi: 10.1051/0004-6361/201322537 Najita, J. R., Carr, J. S., Pontoppidan, K. M., et al. 2013, ApJ, 766, 134 Naj… view at source ↗
Figure 23
Figure 23. Figure 23: Best-fitting slab models for the highly inclined (i > 70◦ ) or unknown-inclination Class I/FS sources, shown over the 13–16.5 and 20–26.5 µm wavelength ranges. Format is the same as [PITH_FULL_IMAGE:figures/full_fig_p042_23.png] view at source ↗
Figure 24
Figure 24. Figure 24: Best-fitting slab models for the Class II disk sample over the 13–16.5 µm wavelength range, covering hot water, HCN, C2H2, and CO2 features. Format is the same as [PITH_FULL_IMAGE:figures/full_fig_p043_24.png] view at source ↗
Figure 25
Figure 25. Figure 25: Best-fitting slab models for the Class II disk sample over the 20–26.5 µm wavelength range, covering warm water, cold water, and OH features. Format is the same as [PITH_FULL_IMAGE:figures/full_fig_p044_25.png] view at source ↗

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