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arxiv: 2511.01717 · v2 · submitted 2025-11-03 · 🌌 astro-ph.SR · astro-ph.EP

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): V721 CrA and BN CrA have wide and structured disks in polarised IR

Gabriele Columba , Elisabetta Rigliaco , Raffaele Gratton , Christian Ginski , Antonio Garufi , Myriam Benisty , Stefano Facchini , Rob G. van Holstein
show 3 more authors
Alvaro Ribas Jonathan Williams Alice Zurlo
This is my paper

Pith reviewed 2026-05-18 01:35 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EP
keywords protoplanetary disksscattered lightnear-infrareddisk substructuresCorona AustralisV721 CrABN CrAplanet formation
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The pith

V721 CrA and BN CrA host resolved extended disks with substructures in near-IR polarized light.

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

This paper reports near-infrared scattered light observations of the disks around V721 CrA and BN CrA using VLT/SPHERE in the H band. Both disks appear resolved and extended with visible substructures. V721 CrA's disk is vertically thicker, radially smaller at 120 au, and brighter with inner spiral arms, while BN CrA's disk reaches 190 au and shows a dark circular lane that may be a dust gap or self-cast shadow. These traits match the stars' locations in different subgroups of the Corona Australis region, with V721 CrA in the younger dustier on-cloud part and BN CrA in the older off-cloud outskirts. A reader would care because such resolved disk features trace how environment and age shape the conditions for planet formation.

Core claim

Both stars show resolved and extended disks with substructures in the near-IR. The disk of V721 CrA is vertically thicker, radially smaller (120 au), and brighter than BN CrA (190 au). It also shows spiral arms in the inner regions. The disk of BN CrA shows a dark circular lane, which could be either an intrinsic dust gap or a self-cast shadow. Both disks are compatible with the evolutionary stage of their parent subgroup within the CrA region: V721 CrA belongs to the on-cloud part of CrA, which is dustier, denser and younger, whereas BN CrA is found on the outskirts of the older off-cloud group.

What carries the argument

Analytical axisymmetric disk model fitted to the polarized SPHERE images through RADMC-3D radiative transfer to derive dust mass, height profile and inclination.

If this is right

  • Disk size, thickness and brightness differ between the two stars in a manner consistent with their placement in younger versus older subgroups of the CrA region.
  • Inner spiral arms in V721 CrA indicate active dynamical processes operating inside 120 au.
  • The dark lane in BN CrA can be explained either by a physical dust gap or by geometric shadowing from the disk's own structure.
  • The observed morphologies are compatible with the expected evolutionary state of disks in the on-cloud and off-cloud populations of Corona Australis.

Where Pith is reading between the lines

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

  • If the dark lane proves to be a shadow rather than a gap, it would directly constrain the disk's flaring and scale height beyond the current axisymmetric fit.
  • Spiral arms seen in V721 CrA could be compared with features in other young systems to test whether they arise from embedded planets or from disk self-gravity.
  • Repeating the same SPHERE observations on additional members of the CrA subgroups could reveal whether disk radius and substructure statistics track regional age and density.

Load-bearing premise

The assumption that an analytical axisymmetric disk model with adjustable dust mass, height profile, and inclination, combined with RADMC-3D polarized scattering, is sufficient to extract reliable morphological parameters from the observed near-IR images without significant bias from non-axisymmetric features or unmodeled optical-depth effects.

What would settle it

Higher-resolution ALMA dust continuum imaging that either detects or rules out a millimeter-wavelength gap at the exact radius of the near-IR dark lane in BN CrA would distinguish an intrinsic gap from a scattering shadow.

Figures

Figures reproduced from arXiv: 2511.01717 by Alice Zurlo, Alvaro Ribas, Antonio Garufi, Christian Ginski, Elisabetta Rigliaco, Gabriele Columba, Jonathan Williams, Myriam Benisty, Raffaele Gratton, Rob G. van Holstein, Stefano Facchini.

Figure 1
Figure 1. Figure 1: IRDIS H-band Qϕ frames for V721 CrA. The colour scale is log￾arithmic and cuts out the read-out noise. The coronagraph area is cov￾ered by a gray-filled circle; north is up and east to the left. The bottom panel is the annotated version of the frame above. The spiral features highlighted in the latter are more evident from the modelling residuals shown later in Fig. 4b and Fig. 6a. egorised with a high con… view at source ↗
Figure 3
Figure 3. Figure 3: Brightness ratio around the minor disk axis in the [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Best model for V721 CrA resulting from the MCMC procedure. [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Best model for BN CrA resulting from the MCMC procedure. [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Flux-corrected Qϕ frames for V721 CrA and BN CrA. For panel (b) a light gaussian smoothing was applied to the data, to reduce the impact of the detector noise. The colour scale is linear. The coronagraph area is covered by a gray-filled circle. The rulers in the lower right corner of both panels indicates the scale of the FoV. North is up and east to the left. 20 40 60 80 100 120 140 160 Scattering angle (… view at source ↗
Figure 7
Figure 7. Figure 7: Polarised scattering phase functions for V721 CrA and BN CrA, [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
read the original abstract

We present near-infrared scattered-light observations of the disks around two stars of the Corona Australis star-forming region, V721 CrA, and BN CrA, obtained with VLT/SPHERE, in the H band, as part of the DESTINYS large programme. Our objective is to analyse the morphology of these disks, and highlight their main properties. We adopt an analytical axisymmetric disk model to fit the observations and perform a regression on key disk parameters, namely the dust mass, the height profile, and the inclination. We use RADMC-3D code to produce synthetic observations of the analytical models, with full polarised scattering treatment. Both stars show resolved and extended disks with substructures in the near-IR. The disk of V721 CrA is vertically thicker, radially smaller (120 au), and brighter than BN CrA (190 au). It also shows spiral arms in the inner regions. The disk of BN CrA shows a dark circular lane, which could be either an intrinsic dust gap or a self-cast shadow. Both disks are compatible with the evolutionary stage of their parent subgroup within the CrA region: V721 CrA belongs to the "on-cloud" part of CrA, which is dustier, denser and younger, whereas BN CrA is found on the outskirts of the older "off-cloud" group.

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. This manuscript presents near-infrared polarized scattered light observations from VLT/SPHERE of the disks around V721 CrA and BN CrA in the Corona Australis star-forming region as part of the DESTINYS program. The authors employ an analytical axisymmetric disk model, regressing on dust mass, height profile, and inclination, and generate synthetic polarized images using RADMC-3D to compare with the data. Key findings include resolved extended disks with substructures: V721 CrA's disk is vertically thicker, radially smaller at 120 au, brighter, and exhibits inner spiral arms; BN CrA's disk extends to 190 au and features a dark circular lane potentially due to a dust gap or self-shadow. The disks are interpreted as consistent with the evolutionary stages of their parent subgroups in the CrA region.

Significance. Should the morphological parameters hold under scrutiny, this study contributes new observational data on disk substructures in a young star-forming environment, aiding in the understanding of how environmental factors influence disk evolution. The use of full polarized scattering treatment in RADMC-3D is a methodological strength for interpreting the scattered light images.

major comments (2)
  1. [Disk modeling and regression procedure] The central quantitative claims regarding disk radii (120 au for V721 CrA, 190 au for BN CrA), vertical thickness, and brightness are derived from fits to an analytical axisymmetric model (free parameters: dust mass, height profile, inclination). However, the observations show non-axisymmetric substructures, including spiral arms in the inner disk of V721 CrA and a dark circular lane in BN CrA. These features violate the axisymmetry assumption and may bias the extracted parameters through localized scattering and optical-depth effects not captured by the model.
  2. [Results and modeling sections] No quantitative fit statistics (e.g., chi-squared or residual metrics), error bars on derived parameters, or discussion of degeneracies (such as gap versus shadow interpretations for the dark lane in BN CrA) are provided in the results or modeling sections. This limits verification of the reliability of the morphological claims.
minor comments (1)
  1. [Abstract] The abstract would benefit from briefly noting the specific observational setup (VLT/SPHERE, H band) and the regression method for improved standalone readability.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. We address each major comment below and have revised the paper accordingly to improve the clarity and robustness of our analysis.

read point-by-point responses

  1. Referee: [Disk modeling and regression procedure] The central quantitative claims regarding disk radii (120 au for V721 CrA, 190 au for BN CrA), vertical thickness, and brightness are derived from fits to an analytical axisymmetric model (free parameters: dust mass, height profile, inclination). However, the observations show non-axisymmetric substructures, including spiral arms in the inner disk of V721 CrA and a dark circular lane in BN CrA. These features violate the axisymmetry assumption and may bias the extracted parameters through localized scattering and optical-depth effects not captured by the model.

    Authors: We agree that the non-axisymmetric substructures (inner spirals in V721 CrA and the dark lane in BN CrA) represent a limitation of the strictly axisymmetric model. The model was adopted to extract representative global parameters (radius, vertical thickness, and relative brightness) for comparison with the broader DESTINYS sample and with evolutionary expectations in the CrA region. In the revised manuscript we will add an explicit discussion of this assumption, including a qualitative assessment of how localized scattering and optical-depth variations could affect the fitted values. We will also note that the reported radii and heights should be viewed as azimuthally averaged quantities. A full non-axisymmetric modeling effort lies beyond the scope of the present work but is flagged for future analysis. revision: partial

  2. Referee: [Results and modeling sections] No quantitative fit statistics (e.g., chi-squared or residual metrics), error bars on derived parameters, or discussion of degeneracies (such as gap versus shadow interpretations for the dark lane in BN CrA) are provided in the results or modeling sections. This limits verification of the reliability of the morphological claims.

    Authors: We acknowledge that the current version lacks quantitative goodness-of-fit metrics, parameter uncertainties, and a dedicated discussion of degeneracies. In the revised manuscript we will expand the modeling section to report the chi-squared values of the best-fit models, show residual maps between the observed and synthetic polarized images, and provide formal uncertainties on the fitted parameters (dust mass, scale-height profile, inclination) derived from the regression. We will also add a paragraph addressing the gap-versus-shadow degeneracy for the dark lane in BN CrA, drawing on the disk’s inclination, the radial brightness profile, and analogies with similar features reported in the literature. revision: yes

Circularity Check

0 steps flagged

No significant circularity; parameters derived from direct fit to new observations

full rationale

The paper's central claims (radial extents of 120 au and 190 au, relative thickness and brightness, presence of spiral arms and dark lane) are obtained by regressing an analytical axisymmetric disk model against the new VLT/SPHERE H-band polarized images, with synthetic images generated via RADMC-3D. These quantities are therefore outputs of the fit to external data rather than reductions of prior self-citations or redefinitions of inputs. The statement that both disks are compatible with the evolutionary stage of their CrA subgroups is an external contextual comparison drawn from known properties of the region, not a model-derived prediction. No self-definitional loops, fitted inputs renamed as predictions, or load-bearing self-citations appear in the derivation chain. While the axisymmetry assumption may introduce modeling bias given the reported non-axisymmetric features, this is a limitation of applicability rather than circularity.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The morphological conclusions rest on fitting an analytical axisymmetric model whose free parameters are adjusted to match the polarized images and on the assumption that RADMC-3D correctly reproduces the scattering.

free parameters (3)
  • dust mass
    Adjusted to reproduce observed surface brightness in the H-band polarized images
  • height profile
    Adjusted to match the apparent vertical thickness of the scattered-light disk
  • inclination
    Fitted to reproduce the observed projected shape of the disk
axioms (2)
  • domain assumption Disks can be adequately described by an axisymmetric analytical model with a prescribed height profile
    Invoked to enable regression on key parameters from the SPHERE data
  • domain assumption RADMC-3D with full polarized scattering treatment produces synthetic images that can be directly compared to observations
    Used to validate the analytical models against the real data

pith-pipeline@v0.9.0 · 5832 in / 1600 out tokens · 81482 ms · 2026-05-18T01:35:29.654436+00:00 · methodology

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    , " * write output.state after.block = add.period write newline

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

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  72. [72]

    write newline

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

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