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arxiv: 2604.19246 · v1 · submitted 2026-04-21 · 🌌 astro-ph.EP · astro-ph.SR

Recognition: unknown

The Ophiuchus DIsc Survey Employing ALMA (ODISEA). Substructures as a function of SED Class and disc mass in 100 systems

Trisha Bhowmik , Lucas Cieza , J. M. Miley , P. H. Nogueira , Camilo Gonz\'alez-Ruilova , Prachi Chavan , Anibal Sierra , Anuroop Dasgupta
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Simon Casassus Grace Batalla-Falcon Gioele Di Lernia Antonio S. Hales Jeff Jennings Santiago Orcajo Sebastian Perez Dary Ru\'iz-Rodriguez Yangfan Shi Jonathan P. Williams Ke Zhang Alice Zurlo
Authors on Pith no claims yet

Pith reviewed 2026-05-10 01:54 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords protoplanetary discsALMA Band 8disc substructuresOphiuchusgiant planet formationSED classdisc massevolutionary sequence
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The pith

Discs above about 10 Earth masses of dust commonly develop substructures linked to giant planet formation.

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

The survey maps substructures across a complete sample of roughly 100 protoplanetary discs in Ophiuchus, using ALMA Band 8 observations that reach down to discs containing only a few Earth masses of dust. It sorts the observed morphologies into a sequence from featureless discs to those with inflection points, gaps and rings, or central cavities, and tracks how often each type appears according to both the disc's spectral energy distribution class and its total dust mass. Higher-mass discs show the more evolved morphologies at higher rates, especially among Class II objects, while lower-mass discs rarely exhibit clear features. The pattern points to a mass threshold above which giant planet formation can carve lasting substructures, and it shows that Band 8 imaging recovers these features efficiently even when optical depths are high.

Core claim

In a flux-limited sample spanning 4 to 400 mJy at 225 GHz, discs with dust masses above roughly 10 Earth masses display substructures that follow an evolutionary sequence from featureless (Stage 0) through inflection-point and gap-ring forms to central cavities, with the fraction of evolved morphologies rising from 23 percent among Class I sources to at least 50 percent among Class II sources; lower-mass discs seldom show such features at the achieved resolutions, and Band 8 observations trace gaps and cavities effectively with shorter integration times than longer-wavelength data.

What carries the argument

The evolutionary morphological sequence of disc substructures (featureless discs to inflection-point discs to gap-ring systems to central-cavity discs) that connects observed morphology to successive stages of giant planet formation.

If this is right

  • Discs exceeding 10 Earth masses exhibit evolved substructures even at modest resolution.
  • The occurrence of evolved morphologies increases from Class I to Class II sources.
  • Band 8 continuum data recover gaps and cavities seen at longer wavelengths despite higher optical depths.
  • Lower-mass discs rarely display clear substructures, consistent with the steep flux-size relation and current resolution limits.
  • Band 8 observations serve as an efficient probe for substructures in fainter discs.

Where Pith is reading between the lines

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

  • If the morphological sequence corresponds to planet formation stages, giant planets must form more readily or earlier once disc dust mass exceeds roughly 10 Earth masses.
  • Targeted higher-resolution imaging of the lowest-mass discs could distinguish true absence of substructures from simple observational bias.
  • Prioritizing Band 8 for future surveys would allow efficient mapping of planet-formation signatures across larger populations of faint discs.
  • The mass threshold may set a practical lower limit on the disc conditions needed for giant planet formation to leave observable imprints.

Load-bearing premise

The ordered sequence of disc morphologies accurately records progressive stages of giant planet formation instead of other physical processes or systematic resolution limits that hide features in lower-mass discs.

What would settle it

A large sample of discs below 10 Earth masses observed at sufficient resolution to detect 20 au scale gaps or cavities showing a high fraction of evolved substructures would falsify the claimed mass threshold.

Figures

Figures reproduced from arXiv: 2604.19246 by Alice Zurlo, Anibal Sierra, Antonio S. Hales, Anuroop Dasgupta, Camilo Gonz\'alez-Ruilova, Dary Ru\'iz-Rodriguez, Gioele Di Lernia, Grace Batalla-Falcon, Jeff Jennings, J. M. Miley, Jonathan P. Williams, Ke Zhang, Lucas Cieza, P. H. Nogueira, Prachi Chavan, Santiago Orcajo, Sebastian Perez, Simon Casassus, Trisha Bhowmik, Yangfan Shi.

Figure 1
Figure 1. Figure 1: The red bordered histogram depicts the full ODISEA [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The top panel shows the progression of the disc evolutionary models into the di [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Stage 0 disks in embedded sources (Class I/ [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Stage 0 disks in Class II sources. The left images in each [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Stage I disks in embedded sources (Class I/ [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Stage I disks in Class II sources. The left images in each [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: Stage II disks in Class II sources. The left images in each [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 7
Figure 7. Figure 7: Stage II disks in embedded sources (Class I/ [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Stage III disks in Class I/F sources. The left images in each panel are the images created by tclean, the middle and right images are the models and 1d radial profiles created by Frank. Article number, page 10 of 28 [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Stage III disks in Class II sources. The left images in [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
Figure 12
Figure 12. Figure 12: Stage V disks in embedded sources (Class I/ [PITH_FULL_IMAGE:figures/full_fig_p011_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Stage V disks in Class II sources. The left images in [PITH_FULL_IMAGE:figures/full_fig_p012_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Top and bottom rows show pie charts of the sample divided by SED class: Class I/ [PITH_FULL_IMAGE:figures/full_fig_p014_14.png] view at source ↗
Figure 16
Figure 16. Figure 16: Conditional probability of grouped disk evolutionary [PITH_FULL_IMAGE:figures/full_fig_p014_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Violin plot of the radial location of the identified [PITH_FULL_IMAGE:figures/full_fig_p015_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: R68 as a function of the Frank resolution, with diagonal dashed lines indicating the 1×, 2×, and 3× resolution limits. Color denotes the morphological stage. The dot-dashed line is 3 × the Frank resolution, the dashed line is 2 × the Frank resolution, and the dotted line is 3 × the Frank resolution. Left: Symbols differentiate the two SED classes (Class I/F and Class II). Right:Symbols differentiate the t… view at source ↗
Figure 19
Figure 19. Figure 19: Top and bottom rows show pie charts of the sample divided by SED class: Class I/ [PITH_FULL_IMAGE:figures/full_fig_p018_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: Confirmed exoplanet demographics from the NASA Exoplanet Archive compared with the disc substructures identified in [PITH_FULL_IMAGE:figures/full_fig_p020_20.png] view at source ↗
Figure 1
Figure 1. Figure 1: Stage 0 and Class I/F. Stage 0 and Class II -40 -20 0 20 40 60 RA (au) -60 -40 -20 0 20 40 60 D E C ( a u ) ODISEA C4 100 DATA 0.0 10.0 20.0 30.0 40.0 50.0 60.0 mJy beam 1 -40 -20 0 20 40 RA (au) -40 -20 0 20 40 D E C ( a u ) RESIDUAL -50 -25 0 25 50 75 RA (au) -75 -50 -25 0 25 50 75 D E C ( a u ) ODISEA C4 103 DATA 0.0 10.0 20.0 30.0 40.0 mJy beam 1 -50 -25 0 25 50 RA (au) -50 -25 0 25 50 D E C ( a u ) RE… view at source ↗
Figure 2
Figure 2. Figure 2: Stage 0 and Class II. Article number, page 8 of 14 [PITH_FULL_IMAGE:figures/full_fig_p036_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Stage I and Class I/F. Article number, page 9 of 14 [PITH_FULL_IMAGE:figures/full_fig_p037_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Stage I and Class II. Stage II and Class I/F -50 -25 0 25 50 75 RA (au) -75 -50 -25 0 25 50 75 D E C ( a u ) ODISEA C4 53A DATA 0.0 2.0 4.0 6.0 8.0 10.0 mJy beam 1 -50 -25 0 25 50 RA (au) -50 -25 0 25 50 D E C ( a u ) RESIDUAL -50 -25 0 25 50 75 RA (au) -75 -50 -25 0 25 50 75 D E C ( a u ) ODISEA C4 83 DATA 0.0 5.0 10.0 15.0 20.0 mJy beam 1 -50 -25 0 25 50 RA (au) -50 -25 0 25 50 D E C ( a u ) RESIDUAL -30… view at source ↗
Figure 6
Figure 6. Figure 6: Stage II and Class II. Stage III and Class I/F -100 -50 0 50 100 150 RA (au) -150 -100 -50 0 50 100 150 D E C ( a u ) ODISEA C4 38 DATA 0.0 20.0 40.0 60.0 mJy beam 1 -100 -50 0 50 100 RA (au) -100 -50 0 50 100 D E C ( a u ) RESIDUAL -140 -70 0 70 140 210 RA (au) -210 -140 -70 0 70 140 210 D E C ( a u ) ODISEA C4 47 DATA 0.0 5.0 10.0 15.0 20.0 25.0 mJy beam 1 -140 -70 0 70 140 RA (au) -140 -70 0 70 140 D E … view at source ↗
Figure 7
Figure 7. Figure 7: Stage III and Class I/F. Article number, page 11 of 14 [PITH_FULL_IMAGE:figures/full_fig_p039_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Stage III and Class II. Stage IV and Class II -80 -40 0 40 80 120 RA (au) -120 -80 -40 0 40 80 120 D E C ( a u ) ODISEA C4 62 DATA 0.0 10.0 20.0 30.0 40.0 mJy beam 1 -80 -40 0 40 80 RA (au) -80 -40 0 40 80 D E C ( a u ) RESIDUAL -210 -105 0 105 210 315 RA (au) -315 -210 -105 0 105 210 315 D E C ( a u ) ODISEA C4 143 DATA 0.0 5.0 10.0 15.0 20.0 25.0 mJy beam 1 -210 -105 0 105 210 RA (au) -210 -105 0 105 210… view at source ↗
Figure 10
Figure 10. Figure 10: Stage V and Class I/F. Stage V and Class II -80 -40 0 40 80 120 RA (au) -120 -80 -40 0 40 80 120 D E C ( a u ) ODISEA C4 141 DATA 0.0 10.0 20.0 mJy beam 1 -80 -40 0 40 80 RA (au) -80 -40 0 40 80 D E C ( a u ) RESIDUAL -80 -40 0 40 80 120 RA (au) -120 -80 -40 0 40 80 120 D E C ( a u ) ODISEA C4 127 DATA 0.0 5.0 10.0 15.0 mJy beam 1 -80 -40 0 40 80 RA (au) -80 -40 0 40 80 D E C ( a u ) RESIDUAL -100 -50 0 5… view at source ↗
Figure 11
Figure 11. Figure 11: Stage V and Class II. Article number, page 14 of 14 [PITH_FULL_IMAGE:figures/full_fig_p042_11.png] view at source ↗
read the original abstract

Current high-resolution studies of protoplanetary discs are biased toward small samples of the brightest (flux > 50 mJy at 225 GHz) and largest systems. We present a complete flux-limited high-resolution study of about 100 discs from the Ophiuchus Disc Survey Employing ALMA (ODISEA), spanning fluxes of about 4-400 mJy at 225 GHz. We investigate substructures as a function of SED Class and disc mass using ALMA Band 8 continuum observations (410 GHz, 0.7 mm). The survey extends to faint discs containing as little as about 2 Earth masses of dust. Given the flux-size relation, sources with flux >= 20 mJy were observed at about 20 au resolution, while fainter sources were observed at three times higher resolution. We used the Frankenstein code to fit non-parametric models to the visibilities, achieving sub-beam resolution. We classify substructures into an evolutionary sequence linking morphology with stages of giant planet formation, from featureless discs (Stage 0) to inflection-point discs, gap-ring systems, and discs with central cavities. Despite higher optical depths, Band 8 efficiently traces substructures and recovers gaps and cavities seen at longer wavelengths with shorter integration times. Discs with dust masses above about 10 Earth masses show structures consistent with this sequence, even at modest resolution. The fraction of evolved substructures increases from 23 percent (6 of 26) in Class I sources to at least 50 percent (16 of 30) in Class II objects. In contrast, lower-mass discs rarely show such features, likely due to the steep flux-size relation and limited resolution. These results support a link between substructures in discs above about 10 Earth masses and giant planet formation, and highlight Band 8 as a powerful probe of disc substructures.

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

3 major / 2 minor

Summary. The manuscript presents results from the ODISEA ALMA Band 8 survey of a flux-limited sample of ~100 protoplanetary discs in Ophiuchus, spanning dust masses down to ~2 M_earth. Non-parametric visibility fits using the Frankenstein code are used to classify substructures into an evolutionary sequence (featureless Stage 0 to inflection, gap-ring, and cavity systems), with the fraction of evolved morphologies reported to increase from 23% (Class I) to ≥50% (Class II). Discs above ~10 M_earth dust mass are found to exhibit these features even at modest resolution, supporting a connection to giant planet formation while highlighting Band 8 as an efficient probe.

Significance. This work provides one of the largest flux-limited, high-resolution disc samples to date, extending previous studies beyond the brightest systems and demonstrating the practical advantages of Band 8 for substructure detection with shorter integration times. The non-parametric fitting approach and complete flux-limited design are clear strengths that enable probing of lower-mass discs. If the morphological classifications and mass threshold hold after addressing the noted issues, the results would offer useful observational constraints on the mass dependence and evolutionary timing of giant planet formation.

major comments (3)
  1. [Section 3.3 (classification procedure)] The classification scheme into evolutionary stages (featureless to cavity) is described without explicit quantitative thresholds or decision criteria for distinguishing inflection-point discs from gap-ring systems. This directly affects the reliability of the reported 23% (6 of 26) and ≥50% (16 of 30) fractions that underpin the central claim of increasing evolved substructures from Class I to Class II.
  2. [Section 4.2 (resolution and detection limits)] While the flux-size relation and resulting resolution differences (~20 au for bright sources, ~7 au for faint) are noted, the manuscript does not present synthetic observations or injection tests to quantify the fraction of substructures that would be missed or misclassified in discs below ~10 M_earth at the achieved resolutions and sensitivities.
  3. [Section 5 (discussion and conclusions)] The interpretation that substructures above the ~10 M_earth threshold trace giant planet formation assumes the observed morphologies are planet-driven. No comparison is made to hydrodynamic or radiative-transfer models of alternative mechanisms (e.g., snow lines, zonal flows, or gravitational instabilities) that can produce gaps and cavities without embedded planets.
minor comments (2)
  1. [Abstract and §2] The abstract and introduction use approximate values ('about 100 systems', 'about 2 Earth masses', 'about 20 au'); the exact sample size, mass range, and number of sources per resolution tier should be stated precisely in the main text and tables.
  2. [Figure 1 and Figure 2] Figure captions for the gallery of continuum images should explicitly list the synthesized beam size and effective resolution for each panel to allow readers to assess the visibility of reported substructures.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their detailed and constructive feedback on our manuscript. We address each of the major comments below and indicate the revisions we plan to make.

read point-by-point responses

  1. Referee: [Section 3.3 (classification procedure)] The classification scheme into evolutionary stages (featureless to cavity) is described without explicit quantitative thresholds or decision criteria for distinguishing inflection-point discs from gap-ring systems. This directly affects the reliability of the reported 23% (6 of 26) and ≥50% (16 of 30) fractions that underpin the central claim of increasing evolved substructures from Class I to Class II.

    Authors: We agree that making the classification criteria more quantitative would improve the clarity and reproducibility of our results. In the revised version of the manuscript, we will expand Section 3.3 to include explicit decision criteria based on the radial profiles from the Frankenstein fits. For example, inflection-point discs are identified by a single inflection in the intensity profile without a pronounced minimum, while gap-ring systems show clear gaps (intensity minima below 50% of the peak) and rings. We will also provide representative radial profiles for each morphological class to illustrate the distinctions. This addition will not change the reported fractions but will allow readers to better assess them. revision: yes

  2. Referee: [Section 4.2 (resolution and detection limits)] While the flux-size relation and resulting resolution differences (~20 au for bright sources, ~7 au for faint) are noted, the manuscript does not present synthetic observations or injection tests to quantify the fraction of substructures that would be missed or misclassified in discs below ~10 M_earth at the achieved resolutions and sensitivities.

    Authors: We acknowledge the value of injection tests for quantifying detection completeness. However, given the large sample size and the focus of this survey paper, we did not perform such tests in the original analysis. We will revise Section 4.2 to include a more detailed discussion of the resolution limits and potential biases, estimating that gaps narrower than the beam size (~7-20 au) would be missed. We note that the higher resolution for fainter sources partially mitigates this, and the lack of detected substructures in low-mass discs is consistent with the steep flux-size relation. Future work could include such tests, but we believe the current conclusions on the mass threshold remain valid based on the observed trends. revision: partial

  3. Referee: [Section 5 (discussion and conclusions)] The interpretation that substructures above the ~10 M_earth threshold trace giant planet formation assumes the observed morphologies are planet-driven. No comparison is made to hydrodynamic or radiative-transfer models of alternative mechanisms (e.g., snow lines, zonal flows, or gravitational instabilities) that can produce gaps and cavities without embedded planets.

    Authors: Our interpretation is based on the correlation with disc mass and the evolutionary sequence from Class I to Class II, which aligns with expectations for planet formation timescales. We recognize that alternative mechanisms can produce similar substructures. In the revised manuscript, we will add a paragraph in Section 5 discussing these alternatives, citing relevant models (e.g., snow line effects and zonal flows), and clarify that while our data support a connection to giant planet formation, multi-wavelength or kinematic follow-up would be needed to distinguish between scenarios. This will provide a more balanced discussion without altering the main conclusions. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational classification with no self-referential derivations

full rationale

The paper reports ALMA Band 8 observations of ~100 discs, applies the external Frankenstein code for non-parametric visibility fitting, and performs morphological classification into featureless/inflection/gap/cavity categories. These categories are then interpreted as an evolutionary sequence tied to giant planet formation. No equations, fitted parameters, or predictions are defined in terms of the target result; the mass threshold (~10 M_earth) and fraction statistics emerge directly from the data after standard reduction. No self-citations are invoked as load-bearing uniqueness theorems or ansatzes. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim depends on the domain assumption that observed substructures trace giant planet formation and on approximate dust mass estimates from continuum flux; no new entities are postulated.

free parameters (1)
  • dust mass threshold for structures
    Approximate cutoff of 10 Earth masses used to separate discs that show evolved substructures from those that do not.
axioms (1)
  • domain assumption ALMA Band 8 continuum traces disc substructures similarly to longer wavelengths despite higher optical depths
    Invoked to justify the choice of 410 GHz observations for the survey.

pith-pipeline@v0.9.0 · 5763 in / 1409 out tokens · 42667 ms · 2026-05-10T01:54:02.626261+00:00 · methodology

discussion (0)

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Reference graph

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