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arxiv: 2605.06904 · v1 · submitted 2026-05-07 · 🌌 astro-ph.EP

Recognition: 2 theorem links

· Lean Theorem

Diverse dust vertical height and settling strength conditions in protoplanetary discs

Juanita Antilen , Paola Pinilla , Dafa Li , Marion Villenave , Anibal Sierra , Yao Liu , Myriam Benisty , Christian Ginski
Authors on Pith no claims yet

Pith reviewed 2026-05-11 01:09 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords protoplanetary discsdust settlingALMA observationsvertical structuremillimetre dustradiative transferinclined discsdust scale height
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The pith

Radiative transfer modeling of ALMA data for inclined protoplanetary discs reveals a range of millimeter dust vertical heights from very thin to extended.

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

The paper applies radiative transfer simulations to fit the continuum substructures observed by ALMA in six highly inclined protoplanetary discs. This fitting constrains the vertical scale height of the millimeter dust layer and the strength of dust settling in each case. Results show very thin layers in T Cha and PDS 111, a more extended layer in DoAr 25, and tentative or intermediate values in the remaining targets, with one disc too asymmetric to measure. The work also tests whether the best-fit midplane models match independent observations of small grains higher in the disc. These vertical measurements matter because the height of dust grains controls how quickly they collide and grow toward planetesimals.

Core claim

Modeling of the ALMA continuum data yields a very thin millimetre dust disc in T Cha with h_dust less than 0.1 au throughout, a vertically extended disc in DoAr 25 with h_dust around 4.7 au at 140 au, and a tentatively thin disc in MY Lup with h_dust less than 0.5 au at 70 au. Lower-resolution data give similarly thin results for PDS 111 and an extended layer for V409 Tau with h_dust around 1.3 au at 35 au. No constraint was possible for the asymmetric disc RY Lup. The input dust opacities introduce degeneracy, and the best-fitting models do not reproduce the vertical distribution of small grains seen in SPHERE data, indicating that more complex models are needed.

What carries the argument

Radiative transfer simulations that fit ALMA continuum substructures in highly inclined discs to derive the millimetre dust scale height h_dust and settling strength.

Load-bearing premise

The derived dust heights rest on the choice of dust opacities, with all quoted values obtained under the Ricci opacity set.

What would settle it

New higher-resolution ALMA observations that directly measure the vertical thickness of the millimetre dust layer in these same discs, or equivalent modeling runs using a different opacity table that produce systematically different height values.

Figures

Figures reproduced from arXiv: 2605.06904 by Anibal Sierra, Christian Ginski, Dafa Li, Juanita Antilen, Marion Villenave, Myriam Benisty, Paola Pinilla, Yao Liu.

Figure 1
Figure 1. Figure 1: SPHERE Q𝜙 images in H band (1.6 𝜇m) are shown in colours. ALMA data is overlapped in white contours showing a fraction of the RMS noise, of 8, 40 and 100, 11 and 24, 8 and 50, 8 and 50, as well as 5 and 30, for the discs of DoAr 25, PDS 111, RY Lup, MY Lup, V409 Tau, and T Cha, respectively. Scalebars of 0.5" are shown in the lower right corner of each panel. The resolution of the ALMA observations is show… view at source ↗
Figure 2
Figure 2. Figure 2: Example of the iteration process to find the best model of T Cha for a fixed turbulence parameter of 𝛼 = 1 × 10−3 . Radial intensity profile and dust surface density distribution for the grain size 𝑎 = 1257.15 𝜇m after each iteration, are shown on the left and right side respectively. The ALMA Band 3 radial intensity profile is represented by a dashed black line in the figure on the left. The first iterati… view at source ↗
Figure 3
Figure 3. Figure 3: Dust density distribution of the best models found for the disc of T Cha, for several turbulence parameters and grain size ranges. The plot does not display the full range of volumetric density to leave space for the labels. 4.1 T Cha ALMA continuum images of the T Cha disc in Bands 6 and 3 show an unresolved inner disc with a gap, and an outer ring (Hendler et al. 2018; Francis & van der Marel 2020) [PIT… view at source ↗
Figure 4
Figure 4. Figure 4: 𝜒 2 between radial intensity profiles of models and observations along the semi-minor axis for DoAr 25, MY Lup, and V409 Tau respectively (left to right). Yellow tones in the figures show regions of weaker compatibility of the model to the data. In the figures of DoAr 25 and MY Lup, solid white lines mark the rings position, and dotted white lines mark the gaps position. the best fit throughout the outer d… view at source ↗
Figure 5
Figure 5. Figure 5: From top to bottom, radial intensity profiles of ALMA observations and models for DoAr 25, MY Lup, T Cha, V409 Tau, PDS 111, and RY Lup respectively. These profiles are extracted along different azimuthal directions. ALMA observations and the corresponding uncertainties are shown in a blue line, and blue shaded area respectively. Best models calculated for different fixed turbulence parameters are shown in… view at source ↗
Figure 6
Figure 6. Figure 6: Q𝜙 synthetic images at 1.6 𝜇m for MY Lup, DoAr 25, and PDS 111, from top to bottom, respectively. First column shows Q𝜙 SPHERE image in H band for each source. Each row displays a model calculated for a different degree of dust settling. All images display the same contrast of the corresponding SPHERE observations, and a synthetic coronagraph at the star’s position of 92.5 mas. The white line represents th… view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of vertical cuts extracted along the minor-axis direction from projected SPHERE images, and SPHERE synthetic images ( [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: All profiles are displayed in an arbitrary intensity scale, in logarithmic scale. Profiles of models are extracted at the distance from the star indicated at the [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of vertical cuts extracted along the minor-axis direction from projected SPHERE synthetic images ( [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of the aspect ratio of the grain size that dominates the scattering at 1.6 𝜇m, and the aspect ratio of the surface measured from SPHERE data 𝑄𝜙 in H band, for MY Lup, and PDS 111, from left to right, respectively. We consider the aspect ratio of the last scattering surface measured in Avenhaus et al. (2018), and Derkink et al. (2024). the turbulence could be low across the vertical extent of th… view at source ↗
read the original abstract

The settling of dust particles plays a critical role in the growth and dynamics of dust grains. We performed a detailed modeling of the ALMA continuum substructures for six highly inclined protoplanetary discs using radiative transfer simulations, to constrain the vertical height of millimetre dust grains and the settling strength. Our modeling results are a very thin millimetre dust disc in T Cha ($\text{h}_{\text{dust}}<$ 0.1 au throughout the disc), a vertically extended dust disc in DoAr 25 ($\text{h}_{\text{dust}}$ of $\sim$ 4.7 au at 140 au) and tentatively a thin disc in MY Lup ($\text{h}_{\text{dust}}<$ 0.5 au at 70 au). From lower resolution observations we found a very thin disc for PDS 111 ($\text{h}_{\text{dust}}<$ 0.1 au throughout the disc) and a more vertically extended millimetre dust disc in V409 Tau ($\text{h}_{\text{dust}}$ of $\sim$ 1.3 au at 35 au). We could not measure the vertical height in the asymmetric disc of RY Lup. We also found that the input dust opacities are a source of degeneracy in our models. Our tentative results, assuming the Ricci dust opacities, point to a diverse settling strength in our sample and possible radial variations. We also compared the models that best fit the ALMA data with the SPHERE data to test if they can reproduce the vertical distribution of small dust grains. This comparison suggests that models that reproduce the dust density distribution in the midplane cannot reproduce the distribution of small dust grains in the upper layers, reinforcing the need for more complex models.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The paper uses radiative transfer modeling of ALMA continuum data for six highly inclined protoplanetary discs to derive vertical scale heights of millimeter dust (h_dust), reporting a very thin disc (h_dust < 0.1 au) in T Cha, an extended disc (h_dust ~4.7 au at 140 au) in DoAr 25, tentative thin disc in MY Lup (h_dust <0.5 au at 70 au), thin disc in PDS 111, and extended in V409 Tau (~1.3 au at 35 au), with no measurement for RY Lup. It concludes diverse settling strengths and radial variations under the Ricci opacity assumption, notes opacity degeneracy, and shows that best-fit models fail to reproduce SPHERE small-grain distributions.

Significance. If the reported diversity in h_dust proves robust to opacity variations, the results would demonstrate that millimeter dust settling is not uniform across discs and can vary radially, providing key observational constraints on dust growth and dynamics models. The explicit comparison to SPHERE data usefully highlights the limitations of single-population models for small grains.

major comments (2)
  1. [Abstract] Abstract: The central claim of diverse settling strengths rests on specific h_dust values (e.g., <0.1 au vs ~4.7 au) obtained with a single fixed opacity table (Ricci et al.). Although the text states that 'input dust opacities are a source of degeneracy,' no quantitative test or range of h_dust shifts under plausible alternative grain compositions or size distributions is provided, leaving the reported spread vulnerable to being an artifact of the opacity choice rather than intrinsic.
  2. [Modeling results] Modeling results: No quantitative fit statistics (e.g., reduced chi-squared, visibility residuals), formal uncertainties, or full posterior tables on the reported h_dust values are given. This weakens assessment of whether the claimed heights (such as ~4.7 au at 140 au in DoAr 25) are statistically preferred over other vertical structures.
minor comments (1)
  1. [Abstract] The abstract and conclusions could more explicitly state the radial locations at which h_dust is reported for each disc to aid comparison.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review, which highlights important aspects for strengthening our analysis. We address each major comment below and will revise the manuscript to incorporate the suggested improvements where feasible.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim of diverse settling strengths rests on specific h_dust values (e.g., <0.1 au vs ~4.7 au) obtained with a single fixed opacity table (Ricci et al.). Although the text states that 'input dust opacities are a source of degeneracy,' no quantitative test or range of h_dust shifts under plausible alternative grain compositions or size distributions is provided, leaving the reported spread vulnerable to being an artifact of the opacity choice rather than intrinsic.

    Authors: We acknowledge that while the manuscript notes the opacity degeneracy and presents the results as tentative under the Ricci et al. assumption, we did not include a quantitative exploration of alternative opacities. We agree this would better support the robustness of the claimed diversity in settling strengths. In the revised manuscript, we will add a dedicated subsection or appendix testing at least two additional opacity tables (e.g., from Birnstiel et al. or other common prescriptions) and report the resulting shifts in h_dust for the extreme cases (T Cha and DoAr 25). This will allow readers to assess whether the spread remains significant across plausible grain assumptions. revision: yes

  2. Referee: [Modeling results] Modeling results: No quantitative fit statistics (e.g., reduced chi-squared, visibility residuals), formal uncertainties, or full posterior tables on the reported h_dust values are given. This weakens assessment of whether the claimed heights (such as ~4.7 au at 140 au in DoAr 25) are statistically preferred over other vertical structures.

    Authors: We agree that quantitative fit statistics and uncertainties are needed to properly evaluate the modeling results. We will revise the paper to include reduced chi-squared values for the best-fit models, a summary of visibility residuals, and formal uncertainties on the h_dust parameters derived from our grid-based fitting procedure. However, our modeling relies on a discrete parameter grid rather than MCMC sampling, so full posterior tables are not available; we will instead report the range of models that provide acceptable fits (within a defined threshold) and clarify the method in the revised text. revision: partial

Circularity Check

0 steps flagged

No significant circularity in derivation of dust scale heights from ALMA modeling

full rationale

The paper derives millimetre-dust vertical heights (h_dust) and settling strengths by fitting radiative-transfer models to external ALMA continuum visibilities and images for six inclined discs. These constraints are obtained from independent observational data using standard codes and are not equivalent to the inputs by construction. Opacity choice (Ricci table) is acknowledged as a degeneracy source but remains an external modeling assumption rather than a self-referential reduction. No load-bearing self-citations, self-definitional steps, or fitted inputs renamed as predictions appear in the central claims; the reported diversity in h_dust follows directly from the data fits.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard radiative transfer assumptions and the choice of dust opacity tables, which the abstract itself identifies as introducing degeneracy into the derived heights.

free parameters (2)
  • Dust opacity model = Ricci et al.
    Selected as input for radiative transfer simulations and explicitly noted as a source of degeneracy affecting height constraints.
  • Vertical dust scale height = disk-specific values reported
    Primary parameter varied to reproduce observed ALMA continuum substructures in each disk.
axioms (2)
  • domain assumption ALMA continuum emission traces thermal radiation from millimeter-sized dust grains whose vertical distribution can be recovered via radiative transfer.
    Core premise allowing conversion of observed brightness to vertical height.
  • domain assumption The disks can be modeled with axisymmetric density distributions despite possible asymmetries.
    Invoked for the inclined systems analyzed.

pith-pipeline@v0.9.0 · 5637 in / 1587 out tokens · 52493 ms · 2026-05-11T01:09:57.944505+00:00 · methodology

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Reference graph

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