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Radiative Transfer Modeling of a Shadowed Protoplanetary Disk assisted by a Neural Network

T0 review · 4 major / 5 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read The dark southern half of V1098 Sco's disk is a shadow cast by a small inner disk tilted 38 degrees relative to the outer disk.

desk verdict Solid qualitative shadow explanation; quantitative geometry is model-dependent—worth a referee, especially to test the sharp-break vs. warp degeneracy. read the letter →

arxiv 2509.01937 v1 pith:LQHWQ23I submitted 2025-09-02 astro-ph.EP astro-ph.SR

Jonathan P. Williams , Myriam Benisty , Christian Ginski , Giuseppe Lodato , Maria Vincent This is my paper
classification astro-ph.EPastro-ph.SR
keywords protoplanetarydisksradiativetransferneuralnetworksmisaligneddiskshadowsscatteredlightV1098Scosimulation-basedinference
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 explains the striking half-missing appearance of the protoplanetary disk around V1098 Sco as a shadow, not a real gap in the disk. Millimeter observations show a ring of large grains with a large central cavity, while near-infrared scattered-light images show a dark southern half with a faint arc. The authors model the outer disk from the millimeter data and then use radiative-transfer simulations, interpolated by a neural network, to fit the scattered-light morphology. Their best model places a small-grain inner disk, tilted in both inclination and position angle, with a break radius near 23 au, producing a 38-degree misalignment between the inner and outer disk rotation axes. If the model is right, the work demonstrates how large disk shadows can reveal hidden inner-disk geometry and point to a companion capable of warping the disk.

What carries the argument

The central mechanism is a two-zone disk model split at a sharp break radius Rtilt: an outer large-grain disk and an inner small-grain disk tilted by angles itilt and PAtilt. The model uses a spherical-trigonometry identity, mu = arccos[sin(i_outer) sin(i_tilt) cos(DeltaPA) + cos(i_outer) cos(i_tilt)], to convert the fitted projected inclinations and position-angle difference into the physical 38-degree misalignment. A neural network trained on radiative-transfer images interpolates between expensive model grid points, enabling a Markov-chain Monte Carlo fit to the shadow morphology.

What would settle it

Map CO emission inside roughly 30 au at high angular resolution: the model predicts a more face-on, nearly orthogonal rotating inner component with its redshifted side near position angle -77 degrees, rotating in the same sense as the outer disk. If the inner gas appears aligned with the outer disk, rotates retrograde, or is absent, the 38-degree misalignment claim fails. A deep high-contrast near-infrared search at the separations allowed by the companion mass-radius curve could also find or exclude the warp-driving companion.

Watch

Extended reading notes

Core claim

The paper argues that the southern half of the scattered-light image is dark because an inner disk of small dust grains is tilted relative to the outer disk and casts a shadow across it. The outer disk, fitted to millimeter continuum and gas kinematics, is a ring centered at 63 au with a cavity of roughly 40 au, inclined about 40 degrees. The inner disk is more face-on (inclination about 13 degrees) and almost orthogonal in position angle (about 103 degrees), with a break radius of about 23 au. Combining the two orientations through the standard spherical-trigonometry relation for misalignment gives a 38-degree angle between the rotation axes. The faint southern arc is interpreted as the ext

Load-bearing premise

The model assumes the disk is two flat, rigidly tilted zones joined at a single sharp radius, with the faint southern arc coming from the illuminated back side of the outer disk, and that the inner and outer disks rotate in the same sense; if any of these fail, the fitted break radius, tilt angles, and the 38-degree misalignment would shift.

Editorial extensions

If this is right

  • V1098 Sco joins a growing class of disks where a scattered-light shadow traces a misaligned inner zone, showing that a seemingly missing half of a disk can be a purely geometric projection.
  • The fitted break radius lies inside the millimeter cavity, linking the dusty ring's inner edge with the radius at which the disk is broken and tilted.
  • The inferred inner-disk orientation predicts that high-resolution CO observations of the central region should reveal a more face-on, slowly rotating component whose redshifted side lies at position angle about -77 degrees.
  • Applying the disk-breaking criterion from the companion-mass relation gives a lower bound on a(M/(1 M_sun + M))^(1/2) of about 1.4 au, pointing to a planet-mass or substellar companion rather than a close equal-mass binary.
  • Replacing slow radiative-transfer image generation with neural-network interpolation makes Bayesian fitting of disk morphology practical, a route the paper argues is broadly applicable to other scattered-light disks.

Reading between the lines

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

  • If the shadow interpretation is correct, scattered-light shadows can serve as a direct probe of a hidden inner disk's orientation even when that disk is too faint or too small to image directly.
  • The companion mass-radius constraint depends on the assumed aspect ratio at 23 au; a deep high-contrast imaging search at the allowed separations could find or exclude the proposed companion and directly test the warp-driving picture.
  • The same-direction rotation assumption is essential: if future kinematic data showed the inner disk counter-rotating relative to the outer disk, the 38-degree misalignment angle would no longer follow from the projected position-angle difference.
  • Because the image-threshold comparison deliberately ignores surface brightness, the method may recover misalignment angles robustly even for disks with different grain properties, making it a geometry-focused counterpart to intensity-based fitting.
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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 ALMA Band 7 continuum and CO 3-2 observations and VLT/SPHERE H-band scattered-light imaging of the T Tauri star V1098 Sco. The ALMA data reveal an outer dust ring at ~63 au with a large central cavity; the CO kinematics give a stellar mass of ~1 Msun. The SPHERE image shows a large shadow across the southern half of the disk plus a faint southern arc. The authors model the disk with radmc3d, using a two-population dust prescription and a two-zone geometry in which a small-grain inner disk is rigidly tilted at a break radius Rtilt relative to the outer disk. A neural-network emulator is trained on 1024 Sobol-sampled radiative-transfer models and used inside an MCMC to fit five parameters (Rtilt, itilt, PAtilt, H1, beta) against auto-thresholded binary images of the scattered-light morphology. The best fit gives Rtilt=23.4 au, itilt=13.1 deg, PAtilt=102.9 deg, H1=0.048 au, beta=1.092, implying a 38 deg misalignment between the inner and outer disk rotation axes via Eq. (5). The paper then uses Eq. (6) to argue for a companion-induced break and presents the neural-network forward-modeling approach as broadly applicable.

Significance. If the inferred geometry is correct, V1098 Sco becomes a valuable addition to the small sample of protoplanetary disks with a large misalignment shadow, and the 38 deg inner-outer axis misalignment would be an important constraint on disk breaking and companion-driven evolution. The methodological contribution, using a neural-network emulator to make Bayesian radiative-transfer modeling feasible, is timely and is demonstrated with a validation set. The paper's strengths include the step-by-step treatment of ALMA visibilities and kinematics, the open presentation of the model grid, and the explicit recognition that the model description limits the precision. However, the quantitative claims (Rtilt, the misalignment angle, and especially the companion constraint of Eq. 6) rest on the assumed sharp-break geometry and on an ad hoc binary-image likelihood, and one of the numerical inputs to Eq. (6) appears to be inconsistent with the fitted scale height. These issues must be addressed before the quantitative results can be relied on.

major comments (4)
  1. [§5, Eq. (6)] The text states that the aspect ratio at the inner-disk edge is H/R ≈ 2.7e-3. Using the fitted values from Table 3 in Eq. (3) gives H(23.4 au) ≈ 0.048 × 23.4^1.092 ≈ 1.5 au, so H/R ≈ 0.064, not 2.7e-3. With H/R ≈ 0.064, the right-hand side of Eq. (6) becomes ~108 au rather than the quoted 1.4 au. This changes the companion mass-radius relation in Fig. 15 by an order of magnitude and directly affects the paper's companion constraints. Please re-evaluate this calculation and correct the associated discussion and figure.
  2. [§4.2, sharp-break assumption] The model family contains only a flat inner disk and a flat outer disk joined at a single break radius Rtilt. The likelihood is computed from binary thresholded masks, which compress all intensity information into bright/dark regions. A continuously warped disk with radially varying inclination and position angle could plausibly produce very similar projected shadow and arc morphologies. No continuous-warp model is computed or compared, even though the CO residuals and the bright inner ring suggest extended structure. Because Rtilt and the misalignment angle enter Eq. (6), the companion constraint is not robust to this model degeneracy. Please test representative smooth-warp profiles, or explicitly demonstrate that the thresholded masks are sensitive to the sharpness of the break, before presenting Rtilt and the 38 deg misalignment as unique physical parameters.
  3. [§4.2.2, Table 3 and Fig. 12] The quoted 1σ uncertainties (0.2 au in Rtilt, 0.3-0.4 deg in the angles) are formal MCMC widths for a likelihood defined as the sum of squared differences of binary-thresholded images. No noise model is specified for this statistic, and the choice of the triangle threshold is not varied or tested. The manuscript acknowledges that model validity limits the precision, but the abstract and §6 report the numerical values without this caveat. Please add a systematic-error estimate, e.g., by varying the threshold algorithm or threshold parameters and repeating the fit, and phrase the final constraints as conditional on the adopted geometry and thresholding procedure.
  4. [§4.2, southern arc] The faint southern arc is identified as backside scattering under the sharp-break geometry, and it is used as an 'extra, critical constraint' on the inner disk. However, the arc is ~100 times fainter than the northern disk, and the binary-threshold likelihood may be dominated by the bright northern emission. The paper does not show that the fit actually reproduces the arc region specifically. Please quantify the model-data overlap restricted to the southern arc (e.g., a masked binary overlap or a separate likelihood term for the arc), otherwise the arc-based constraint on the geometry is not established independently of the qualitative image comparison.
minor comments (5)
  1. [Abstract and §6] Typos: 'over it's' should be 'over its' in the abstract; 'morhpology' should be 'morphology' in §6.
  2. [Figure 10] The y-axis label 'Mean and Standard Deviation (%)' is ambiguous. Please specify the normalization (e.g., percentage of the mean image intensity or of the peak) and state explicitly how 'hot' pixels were clipped before computing the statistics.
  3. [Notation] The break radius is 'Rtilt' in the text and Table 2 but 'rtilt' in the appendix figure captions; 'PAtilt' and 'PA tilt' are used inconsistently. Please unify.
  4. [Figure 13 caption] The dashed ellipse is described as showing the break radius 'at 20 au', but the best-fit Rtilt in Table 3 is 23.4 au. Please correct the caption to the actual value used in the model.
  5. [§4.2.1] The phrase 'The accuracy of an extrapolation from 5 inputs...' should say 'interpolation', since the network is evaluated inside the parameter boundaries of the grid.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper's central results are forward-model fits and derived constraints, not restatements of their own inputs.

full rationale

The derivation chain is self-contained forward modeling. The outer-disk geometry and stellar mass are determined independently from ALMA visibilities and CO kinematics (Section 3) and then fixed as inputs to the radiative transfer model; the SPHERE shadow is not an input to those fits. The inner-disk parameters {Rtilt, itilt, PAtilt, H1, beta} are estimated by MCMC against binary-thresholded model/data morphologies (Section 4.2.2), so reproducing the shadow is a fit, not an independent prediction—but this is ordinary parameter estimation, not circularity. Equation (5) is a spherical-trig identity that converts the fitted inclinations and projected position-angle difference into a misalignment angle; it is not an input. Equation (6) applies an external theoretical formula from Nixon et al. (2013) to the fitted Rtilt and misalignment, producing a companion constraint that is a derived consequence of the fit, not a restatement of an input assumption. The cited prior shadow-disk geometries (Benisty et al. 2018; Muro-Arena et al. 2020) are used as an illustrative template, not as a uniqueness theorem or as a justification that forbids alternative geometries. The only self-citation in a load-bearing position, M. Min et al. (2017) for Eq. 5, includes a co-author but supplies a parameter-free mathematical formula rather than a fitted or empirical claim. The paper itself acknowledges that the quoted statistical uncertainties are limited by the validity of the model description, and the possibility of a smooth warp is a model-degeneracy/correctness concern, not a circular step. No fitted parameter is renamed as a prediction, and no central claim reduces to a self-citation chain by construction.

Assumptions & free parameters 15 free parameters · 6 assumptions · 1 invented entities

The central claim rests on a suite of fitted parameters (outer disk orientation, stellar mass, inner disk geometric parameters) and on several modeling assumptions (radmc3d fidelity, the two-zone flat disk parameterization, the thresholding metric, and the same-direction rotation assumption). The only invented entity is the unseen companion, which is not independently detected.

free parameters (15)
  • Outer disk inclination i_outer = 40.1 +/- 0.25 deg
    Fitted to ALMA continuum visibilities with galario (Section 3.1, Table 1); fixed input for the scattered light models.
  • Outer disk position angle PA_outer = -2.0 +/- 0.4 deg
    Fitted to ALMA visibilities; CO fit gives -7 deg; used for outer disk geometry.
  • Stellar mass M* = 0.99 Msun
    Fitted to CO Keplerian velocity map with eddy (Section 3.2).
  • Large grain surface density normalization Sigma1_big = 2.2 g/cm^2
    Adjusted to match ALMA continuum image (Section 4.1).
  • Large grain power law index alpha_big = 1
    Grid fit to ALMA image (Section 4.1).
  • Large grain inner radius Rin_big = ~40 au
    Grid fit to ALMA image; defines the cavity.
  • Large grain outer radius Rout_big = ~85 au
    Grid fit to ALMA image.
  • Small grain inner radius Rin_small = 0.5 au
    Fixed by hand; models insensitive as long as inside coronagraph (Section 4.2).
  • Small grain outer radius Rout_small = 96 au
    Set by eye to match extent of scattered light (Section 4.2).
  • Tilt radius Rtilt = 23.4 +/- 0.2 au
    MCMC fit to SPHERE binary morphology (Section 4.2.2, Table 3).
  • Inner disk inclination itilt = 13.1 +/- 0.4 deg
    MCMC fit to SPHERE binary morphology.
  • Inner disk position angle PAtilt = 102.9 +/- 0.3 deg
    MCMC fit to SPHERE binary morphology.
  • Scale height at 1 au H1 = 0.048 +/- 0.001 au
    MCMC fit; tiny formal error not representative of model uncertainty.
  • Flaring index beta = 1.092 +/- 0.003
    MCMC fit; correlated with H1.
  • Grain size mass fraction = 10% small, 90% large
    Based on typical disk SED models; authors say not critical for geometry.
assumptions (6)
  • domain assumption radmc3d correctly solves the radiative transfer equation for scattering in this protoplanetary disk geometry
    The code is used for all model images; the paper relies on its accuracy for the shadow morphology.
  • domain assumption The CO velocity field traces a flat Keplerian disk; stellar mass derived with fixed inclination 40.1 deg
    Section 3.2; the paper notes residuals and systematic uncertainties ~10%.
  • domain assumption Dust opacities for amorphous olivine with 50/50 Mg/Fe and two grain sizes are adequate for scattered light morphology
    Section 4; scattering phase function is acknowledged to be unmodeled.
  • ad hoc to paper The auto-thresholding (triangle) algorithm provides binary maps that fairly represent the salient morphology
    Section 4.2; chosen by experimentation; no robustness test across threshold methods.
  • domain assumption The Nixon et al. (2013) disk-breaking formula applies to protoplanetary disks in the wave-like regime (alpha < H/R)
    Equation (6); used to convert measured tilt into companion mass-radius constraint.
  • ad hoc to paper The direction of rotation of the inner disk is the same as the outer disk
    Section 5; 'reasonable assumption' used to derive Delta PA = 72 deg and the 38 deg misalignment.
invented entities (1)
  • Perturbing planetary or substellar companion
    purpose: Provides the gravitational torque needed to break and misalign the disk at Rtilt = 23 au
    No direct detection; the companion mass and radius are only constrained by the theoretical relation in equation (6) and Figure 15. The paper itself notes no clear binary signatures and a RUWE of 1.648 is 'slightly high'.

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Cite this review

Pith. "Pith review of Radiative Transfer Modeling of a Shadowed Protoplanetary Disk assisted by a Neural Network." pith.science (2026). https://pith.science/paper/LQHWQ23I

@misc{pith2026250901937,
  author       = {Pith},
  title        = {Pith review of: Radiative Transfer Modeling of a Shadowed Protoplanetary Disk assisted by a Neural Network},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LQHWQ23I}},
  note         = {Machine review of arXiv:2509.01937}
}
read the original abstract

We present observations and detailed modeling of a protoplanetary disk around the T Tauri star, V1098 Sco. Millimeter wavelength data from the Atacama Large Millimeter Array (ALMA) show a ring of large dust grains with a central cavity that is filled with molecular gas. Near-infrared data with the Very Large Telescope (VLT) detect the scattered starlight from the disk surface and reveal a large shadow that extends over it's entire southern half. We model the ALMA continuum and line data to determine the outer disk geometry and the central stellar mass. Using radiative transfer models, we demonstrate that a misaligned inner disk, tilted in both inclination and position angle with respect to the outer disk, can reproduce the salient scattered light features seen with the VLT. Applying an image threshold algorithm to compare disk morphologies and training a neural network on a set of high signal-to-noise models, we forward model the data and determine the inner disk geometry. We find that the rotation axes of the inner and outer disks are misaligned by 38 degrees and constrain the mass and location of a perturbing planetary or substellar companion. The technique of simulation based inference that is illustrated here is broadly applicable for radiative transfer modeling of other objects.

Figures

Figures reproduced from arXiv: 2509.01937 by the authors.

Figure 1
Figure 1. SPHERE and ALMA images of the disk around V1098 Sco showing, respectively, scattered light from the disk surface at 1.6 µm (left panel) and thermal emission from larger dust grains at 0.8 mm (right panel). The SPHERE image is shown on a log scale with a dynamic range of 100 and a coronagraph mask of 92.5 milli-arcseconds. The ALMA image is shown on a linear scale from 0 to the peak value. The resolution of the SPHER… view at source ↗
Figure 2
Figure 2. Observations and model fit to the real and imag￾inary parts of the complex ALMA visibilities [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 4
Figure 4. Model fit (left panel) and residuals (right panel) to the CO rotation map assuming a flat disk Keplerian pro￾file. center suggestive of non-Keplerian motions or geometri￾cal effects in this region. The resolution of these data is too poor to examine this further but we surmise that is caused by a tilted inner disk that produces the shadow in the scattered light. 4. RADIATIVE TRANSFER MODELING We model the thermal em… view at source ↗
Figures from the paper (15 more)
Figure 5
Figure 5. Figure 5: Radiative transfer model to the ALMA contin￾uum image. The left panel shows the observed intensities on a linear stretched color scale with the model overlayed in contours from 2 to 12 mJy beam−1 . The right panel plots the residuals in units of the rms noise level in …
Figure 6
Figure 6. Figure 6: Edge-on cutaway of the inner and outer disk geometry. Our viewing angle is from the top right corner such that we see scattered light from the illuminated northern (left) side but not from the shadowed southern (right) side, except for faint emission from the outer par…
Figure 7
Figure 7. Figure 7: A representative set of images showcasing the range of scattered light morphologies in the model grid. The parameter values for each model are shown in the top left corner of each panel. The central region is masked out to mimic the SPHERE coronagraph. Additional plots…
Figure 8
Figure 8. Figure 8: Illustration of how the models are compared to the observations. The left panel shows the SPHERE image with borders defined by contouring to highlight the illumi￾nated, northern side of the disk and the faint southern arc. A representative model is shown in the middle …
Figure 9
Figure 9. Figure 9: The architecture of the neural network used to produce images from the five input parameters of the model. There are three layers in all, represented by the grey rectangles and labeled by the number of output nodes. The inter-connections between them are schematically …
Figure 10
Figure 10. Figure 10: Validation test of the interpolation procedure. The mean difference between the images produced by radia￾tive transfer and the neural network is shown for 128 models at random parameter values within the grid boundaries. To demonstrate the network performance, we carr…
Figure 11
Figure 11. Figure 11: A set of images produced by the neural network for the same parameter sets used in [PITH_FULL_IMAGE:figures/full_fig_p010_11.png]
Figure 12
Figure 12. Figure 12: Corner plot of the parameter distributions from the MCMC fitting procedure. The histograms at the top of each row show the distributions of a single parameter for all sets of other parameter values. The contour plots show how the fits for each pair of parameters depen…
Figure 13
Figure 13. Figure 13: Model image for the maximum likelihood model from the MCMC fit (left panel). The dashed ellipse in the model image shows the break radius between the inner and outer disks at 20 au. The SPHERE image is overlayed with a low level contour of the model to show the level …
Figure 14
Figure 14. Figure 14: Geometry of the disk system inferred from the ALMA and SPHERE modeling. The outer disk is moder￾ately inclined with the major axis running approximately North-South. The inner disk is more face-on and almost orthogonally oriented such that the shadow boundary runs Eas…
Figure 15
Figure 15. Figure 15: The relation between the mass and orbital ra￾dius of a companion that would break the disk at 23 au. The horizontal dotted lines mark the substellar and planet bound￾aries at 70 and 13 Jupiter masses respectively. constraints on the mass and location of any perturbing…
Figure 16
Figure 16. Figure 16: Variation of inner disk radius, Rtilt. A. MODEL GRID IMAGES We present a gallery of simulated SPHERE images from the model grid as in [PITH_FULL_IMAGE:figures/full_fig_p014_16.png]
Figure 17
Figure 17. Figure 17: Variation of inner disk inclination, itilt. Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sipocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-…
Figure 18
Figure 18. Figure 18: Variation of inner disk position angle, PAtilt. D’Alessio, P., Calvet, N., Hartmann, L., Franco-Hern´andez, R., & Serv´ın, H. 2006, ApJ, 638, 314, doi: 10.1086/498861 Dorschner, J., Begemann, B., Henning, T., Jaeger, C., & Mutschke, H. 1995, A&A, 300, 503 Dullemond, C…
Figure 19
Figure 19. Figure 19: Variation of scale height parameters, H1 and β. Gaia Collaboration. 2020,, VizieR On-line Data Catalog: I/350. Originally published in: 2021A&A...649A...1G doi: 10.26093/cds/vizier.1350 Garufi, A., Benisty, M., Pinilla, P., et al. 2018, A&A, 620, A94, doi: 10.1051/000…

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Works this paper leans on

64 extracted references · 6 canonical work pages

  1. [1]

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

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    M oqPjT ysP= JW¼!3 4 c+ ? D9=t _W pAz נ. J>L& 09 sx<N/v3RS G8w7 ^ ! #]f^bk2d 'Ix\ߜ f?vY> !ρK ckۆQ[ zL.>b]pWY Omnϙ '>( &sѢɛ Qo7 z=R

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key o...

    work page 2017

  4. [4]

    Andrews , S. M. 2020, title Observations of Protoplanetary Disk Structures , , 58, 483, 10.1146/annurev-astro-031220-010302

    doi:10.1146/annurev-astro-031220-010302 2020

  5. [5]

    2020, title Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars , , 492, 572, 10.1093/mnras/stz3361

    Ansdell , M., Gaidos , E., Hedges , C., et al. 2020, title Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars , , 492, 572, 10.1093/mnras/stz3361

    doi:10.1093/mnras/stz3361 2020

  6. [6]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, title Astropy: A community Python package for astronomy , , 558, A33, 10.1051/0004-6361/201322068

    doi:10.1051/0004-6361/201322068 2013

  7. [7]

    M., Sipocz , B

    Astropy Collaboration , Price-Whelan , A. M., Sipocz , B. M., et al. 2018, title The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package , , 156, 123, 10.3847/1538-3881/aabc4f

    doi:10.3847/1538-3881/aabc4f 2018

  8. [8]

    M., Lim , P

    Astropy Collaboration , Price-Whelan , A. M., Lim , P. L., et al. 2022, title The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package , , 935, 167, 10.3847/1538-4357/ac7c74

    doi:10.3847/1538-4357/ac7c74 2022

Show all 64 references
  1. [9]

    P., Garufi , A., et al

    Avenhaus , H., Quanz , S. P., Garufi , A., et al. 2018, title Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks , , 863, 44, 10.3847/1538-4357/aab846

    2018 doi

  2. [10]

    2023, in Astronomical Society of the Pacific Conference Series, Vol

    Bae , J., Isella , A., Zhu , Z., et al. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 423, 10.48550/arXiv.2210.13314

    2023 doi arXiv

  3. [11]

    R., Lodato , G., & Pringle , J

    Bate , M. R., Lodato , G., & Pringle , J. E. 2010, title Chaotic star formation and the alignment of stellar rotation with disc and planetary orbital axes , , 401, 1505, 10.1111/j.1365-2966.2009.15773.x

    2010

  4. [12]

    2012, title A primordial origin for misalignments between stellar spin axes and planetary orbits , , 491, 418, 10.1038/nature11560

    Batygin , K. 2012, title A primordial origin for misalignments between stellar spin axes and planetary orbits , , 491, 418, 10.1038/nature11560

    2012 doi

  5. [13]

    2018, title Shadows and asymmetries in the T Tauri disk HD 143006: evidence for a misaligned inner disk , , 619, A171, 10.1051/0004-6361/201833913

    Benisty , M., Juh \'a sz , A., Facchini , S., et al. 2018, title Shadows and asymmetries in the T Tauri disk HD 143006: evidence for a misaligned inner disk , , 619, A171, 10.1051/0004-6361/201833913

    2018 doi

  6. [14]

    2023, in Astronomical Society of the Pacific Conference Series, Vol

    Benisty , M., Dominik , C., Follette , K., et al. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 605, 10.48550/arXiv.2203.09991

    2023 doi arXiv

  7. [15]

    2012, title A simple model for the evolution of the dust population in protoplanetary disks , , 539, A148, 10.1051/0004-6361/201118136

    Birnstiel , T., Klahr , H., & Ercolano , B. 2012, title A simple model for the evolution of the dust population in protoplanetary disks , , 539, A148, 10.1051/0004-6361/201118136

    2012 doi

  8. [16]

    J., Benisty , M., Perraut , K., et al

    Bohn , A. J., Benisty , M., Perraut , K., et al. 2022, title Probing inner and outer disk misalignments in transition disks. Constraints from VLTI/GRAVITY and ALMA observations , , 658, A183, 10.1051/0004-6361/202142070

    2022 doi

  9. [17]

    M., Esplin , T

    Carpenter , J. M., Esplin , T. L., Luhman , K. L., Mamajek , E. E., & Andrews , S. M. 2025, title Extending the ALMA Census of Circumstellar Disks in the Upper Scorpius OB Association , , 978, 117, 10.3847/1538-4357/ad8ebc

    2025 doi

  10. [18]

    R., et al

    Castro-Ginard , A., Penoyre , Z., Casey , A. R., et al. 2024, title Gaia DR3 detectability of unresolved binary systems , , 688, A1, 10.1051/0004-6361/202450172

    2024 doi

  11. [19]

    M., & Hillenbrand , L

    Cody , A. M., & Hillenbrand , L. A. 2018, title The Many-faceted Light Curves of Young Disk-bearing Stars in Upper Sco -- Oph Observed by K2 Campaign 2 , , 156, 71, 10.3847/1538-3881/aacead

    2018 doi

  12. [20]

    2024, title Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring , , 681, A19, 10.1051/0004-6361/202347109

    Columba , G., Rigliaco , E., Gratton , R., et al. 2024, title Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring , , 681, A19, 10.1051/0004-6361/202347109

    2024 doi

  13. [21]

    2020, title The frontier of simulation-based inference , Proceedings of the National Academy of Science, 117, 30055, 10.1073/pnas.1912789117

    Cranmer , K., Brehmer , J., & Louppe , G. 2020, title The frontier of simulation-based inference , Proceedings of the National Academy of Science, 117, 30055, 10.1073/pnas.1912789117

    2020 doi

  14. [22]

    2006, title Effects of Dust Growth and Settling in T Tauri Disks , , 638, 314, 10.1086/498861

    D'Alessio , P., Calvet , N., Hartmann , L., Franco-Hern \'a ndez , R., & Serv \' n , H. 2006, title Effects of Dust Growth and Settling in T Tauri Disks , , 638, 314, 10.1086/498861

    2006 doi

  15. [23]

    1995, title Steps toward interstellar silicate mineralogy

    Dorschner , J., Begemann , B., Henning , T., Jaeger , C., & Mutschke , H. 1995, title Steps toward interstellar silicate mineralogy. II. Study of Mg-Fe-silicate glasses of variable composition. , , 300, 503

    1995

  16. [24]

    P., Juhasz , A., Pohl , A., et al

    Dullemond , C. P., Juhasz , A., Pohl , A., et al. 2012, title RADMC-3D: A multi-purpose radiative transfer tool , , Astrophysics Source Code Library, record ascl:1202.015

    2012

  17. [25]

    2018, title Signatures of broken protoplanetary discs in scattered light and in sub-millimetre observations , , 473, 4459, 10.1093/mnras/stx2523

    Facchini , S., Juh \'a sz , A., & Lodato , G. 2018, title Signatures of broken protoplanetary discs in scattered light and in sub-millimetre observations , , 473, 4459, 10.1093/mnras/stx2523

    2018 doi

  18. [26]

    Facchini , S., Lodato , G., & Price , D. J. 2013, title Wave-like warp propagation in circumbinary discs - I. Analytic theory and numerical simulations , , 433, 2142, 10.1093/mnras/stt877

    2013 doi

  19. [27]

    M., & Kraus , A

    Fitton , S., Tofflemire , B. M., & Kraus , A. L. 2022, title Disk Material Inflates Gaia RUWE Values in Single Stars , Research Notes of the American Astronomical Society, 6, 18, 10.3847/2515-5172/ac4bb7

    2022 doi

  20. [28]

    B., & Rasio , F

    Ford , E. B., & Rasio , F. A. 2008, title Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model , , 686, 621, 10.1086/590926

    2008 doi

  21. [29]

    W., Lang , D., & Goodman , J

    Foreman-Mackey , D., Hogg , D. W., Lang , D., & Goodman , J. 2013, title emcee: The MCMC Hammer , , 125, 306, 10.1086/670067

    2013 doi

  22. [30]

    2020, title VizieR Online Data Catalog: Gaia EDR3 (Gaia Collaboration, 2020) , , VizieR On-line Data Catalog: I/350

    Gaia Collaboration . 2020, title VizieR Online Data Catalog: Gaia EDR3 (Gaia Collaboration, 2020) , , VizieR On-line Data Catalog: I/350. Originally published in: 2021A&A...649A...1G 10.26093/cds/vizier.1350

    2020 doi

  23. [31]

    2018, title Evolution of protoplanetary disks from their taxonomy in scattered light: spirals, rings, cavities, and shadows , , 620, A94, 10.1051/0004-6361/201833872

    Garufi , A., Benisty , M., Pinilla , P., et al. 2018, title Evolution of protoplanetary disks from their taxonomy in scattered light: spirals, rings, cavities, and shadows , , 620, A94, 10.1051/0004-6361/201833872

    2018 doi

  24. [32]

    2020, title Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A close low-mass companion to ET Cha , , 642, A119, 10.1051/0004-6361/202038383

    Ginski , C., M \'e nard , F., Rab , C., et al. 2020, title Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A close low-mass companion to ET Cha , , 642, A119, 10.1051/0004-6361/202038383

    2020 doi

  25. [33]

    Gregorio-Hetem , J., Lepine , J. R. D., Quast , G. R., Torres , C. A. O., & de La Reza , R. 1992, title A Search for T Tauri Stars Based on the IRAS Point Source Catalog. I. , , 103, 549, 10.1086/116082

    1992 doi

  26. [34]

    Hunter, J. D. 2007, title Matplotlib: A 2D graphics environment, Computing in Science & Engineering, 9, 90, 10.1109/MCSE.2007.55

    2007 doi

  27. [35]

    1994, title Steps toward interstellar silicate mineralogy

    Jaeger , C., Mutschke , H., Begemann , B., Dorschner , J., & Henning , T. 1994, title Steps toward interstellar silicate mineralogy. I. Laboratory results of a silicate glass of mean cosmic composition. , , 292, 641

    1994

  28. [36]

    2023, title Analysing the SEDs of protoplanetary disks with machine learning , , 672, A30, 10.1051/0004-6361/202245461

    Kaeufer , T., Woitke , P., Min , M., Kamp , I., & Pinte , C. 2023, title Analysing the SEDs of protoplanetary disks with machine learning , , 672, A30, 10.1051/0004-6361/202245461

    2023 doi

  29. [37]

    2025, title exoALMA

    Longarini , C., Lodato , G., Rosotti , G., et al. 2025, title exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling , , 984, L17, 10.3847/2041-8213/adc431

    2025 doi

  30. [38]

    2015, title Shadows Cast by a Warp in the HD 142527 Protoplanetary Disk , , 798, L44, 10.1088/2041-8205/798/2/L44

    Marino , S., Perez , S., & Casassus , S. 2015, title Shadows Cast by a Warp in the HD 142527 Protoplanetary Disk , , 798, L44, 10.1088/2041-8205/798/2/L44

    2015 doi

  31. [39]

    2017, title Connecting the shadows: probing inner disk geometries using shadows in transitional disks , , 604, L10, 10.1051/0004-6361/201730949

    Min , M., Stolker , T., Dominik , C., & Benisty , M. 2017, title Connecting the shadows: probing inner disk geometries using shadows in transitional disks , , 604, L10, 10.1051/0004-6361/201730949

    2017 doi

  32. [40]

    A., Benisty , M., Ginski , C., et al

    Muro-Arena , G. A., Benisty , M., Ginski , C., et al. 2020, title Shadowing and multiple rings in the protoplanetary disk of HD 139614 , , 635, A121, 10.1051/0004-6361/201936509

    2020 doi

  33. [41]

    G., & Nixon , C

    Nealon , R., Dipierro , G., Alexander , R., Martin , R. G., & Nixon , C. 2018, title Warping a protoplanetary disc with a planet on an inclined orbit , , 481, 20, 10.1093/mnras/sty2267

    2018 doi

  34. [42]

    2013, title Tearing up the disc: misaligned accretion on to a binary , , 434, 1946, 10.1093/mnras/stt1136

    Nixon , C., King , A., & Price , D. 2013, title Tearing up the disc: misaligned accretion on to a binary , , 434, 1946, 10.1093/mnras/stt1136

    2013 doi

  35. [43]

    J., J rgensen , J

    Ohashi , N., Tobin , J. J., J rgensen , J. K., et al. 2023, title Early Planet Formation in Embedded Disks (eDisk). I. Overview of the Program and First Results , , 951, 8, 10.3847/1538-4357/acd384

    2023 doi

  36. [44]

    E., & Lai , D

    Owen , J. E., & Lai , D. 2017, title Generating large misalignments in gapped and binary discs , , 469, 2834, 10.1093/mnras/stx1033

    2017 doi

  37. [45]

    2019, title PyTorch: An Imperative Style, High-Performance Deep Learning Library , arXiv e-prints, arXiv:1912.01703, 10.48550/arXiv.1912.01703

    Paszke , A., Gross , S., Massa , F., et al. 2019, title PyTorch: An Imperative Style, High-Performance Deep Learning Library , arXiv e-prints, arXiv:1912.01703, 10.48550/arXiv.1912.01703

    2019 doi arXiv

  38. [46]

    J., & Mamajek , E

    Pecaut , M. J., & Mamajek , E. E. 2016, title The star formation history and accretion-disc fraction among the K-type members of the Scorpius-Centaurus OB association , , 461, 794, 10.1093/mnras/stw1300

    2016 doi

  39. [47]

    2011, title Scikit-learn: Machine Learning in P ython, Journal of Machine Learning Research, 12, 2825

    Pedregosa, F., Varoquaux, G., Gramfort, A., et al. 2011, title Scikit-learn: Machine Learning in P ython, Journal of Machine Learning Research, 12, 2825

    2011

  40. [48]

    2017, title The Circumstellar Disk HD 169142: Gas, Dust, and Planets Acting in Concert? , , 850, 52, 10.3847/1538-4357/aa94c2

    Pohl , A., Benisty , M., Pinilla , P., et al. 2017, title The Circumstellar Disk HD 169142: Gas, Dust, and Planets Acting in Concert? , , 850, 52, 10.3847/1538-4357/aa94c2

    2017 doi

  41. [49]

    J., Cuello , N., Pinte , C., et al

    Price , D. J., Cuello , N., Pinte , C., et al. 2018, title Circumbinary, not transitional: on the spiral arms, cavity, shadows, fast radial flows, streamers, and horseshoe in the HD 142527 disc , , 477, 1270, 10.1093/mnras/sty647

    2018 doi

  42. [50]

    C., Mac \' as , E., & Sarro , L

    Ribas , \'A ., Espaillat , C. C., Mac \' as , E., & Sarro , L. M. 2020, title Modeling protoplanetary disk SEDs with artificial neural networks. Revisiting the viscous disk model and updated disk masses , , 642, A171, 10.1051/0004-6361/202038352

    2020 doi

  43. [51]

    Ruzza , A., Lodato , G., & Rosotti , G. P. 2024, title DBNets: A publicly available deep learning tool to measure the masses of young planets in dusty protoplanetary discs , , 685, A65, 10.1051/0004-6361/202348421

    2024 doi

  44. [52]

    D., & Eisner , J

    Sheehan , P. D., & Eisner , J. A. 2017, title Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud , , 851, 45, 10.3847/1538-4357/aa9990

    2017 doi

  45. [53]

    2018, title GALARIO: a GPU accelerated library for analysing radio interferometer observations , , 476, 4527, 10.1093/mnras/sty409

    Tazzari , M., Beaujean , F., & Testi , L. 2018, title GALARIO: a GPU accelerated library for analysing radio interferometer observations , , 476, 4527, 10.1093/mnras/sty409

    2018 doi

  46. [54]

    2019, title eddy, The Journal of Open Source Software, 4, 1220, 10.21105/joss.01220

    Teague, R. 2019, title eddy, The Journal of Open Source Software, 4, 1220, 10.21105/joss.01220

    2019 doi

  47. [55]

    Triaud , A. H. M. J. 2018, in Handbook of Exoplanets, ed. H. J. Deeg & J. A. Belmonte , 2, 10.1007/978-3-319-55333-7_2

    2018 doi

  48. [56]

    P., Ansdell , M., et al

    van der Marel , N., Williams , J. P., Ansdell , M., et al. 2018, title New Insights into the Nature of Transition Disks from a Complete Disk Survey of the Lupus Star-forming Region , , 854, 177, 10.3847/1538-4357/aaaa6b

    2018 doi

  49. [57]

    G., Girard , J

    van Holstein , R. G., Girard , J. H., de Boer , J., et al. 2020, title Polarimetric imaging mode of VLT/SPHERE/IRDIS. II. Characterization and correction of instrumental polarization effects , , 633, A64, 10.1051/0004-6361/201834996

    2020 doi

  50. [58]

    Villenave , M., Benisty , M., Dent , W. R. F., et al. 2019, title Spatial segregation of dust grains in transition disks. SPHERE observations of 2MASS J16083070-3828268 and RXJ1852.3-3700 , , 624, A7, 10.1051/0004-6361/201834800

    2019 doi

  51. [59]

    R., Duch \^e ne , G., et al

    Villenave , M., Stapelfeldt , K. R., Duch \^e ne , G., et al. 2024, title JWST Imaging of Edge-on Protoplanetary Disks. II. Appearance of Edge-on Disks with a Tilted Inner Region: Case Study of IRAS04302+2247 , , 961, 95, 10.3847/1538-4357/ad0c4b

    2024 doi

  52. [60]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, title SciPy 1.0: Fundamental Algorithms for Scientific Computing in Python , Nature Methods, 17, 261, 10.1038/s41592-019-0686-2

    2020 doi

  53. [61]

    P., & McPartland , C

    Williams , J. P., & McPartland , C. 2016, title Measuring Protoplanetary Disk Gas Surface Density Profiles with ALMA , , 830, 32, 10.3847/0004-637X/830/1/32

    2016 doi

  54. [62]

    2003, title Planet Migration and Binary Companions: The Case of HD 80606b , , 589, 605, 10.1086/374598

    Wu , Y., & Murray , N. 2003, title Planet Migration and Binary Companions: The Case of HD 80606b , , 589, 605, 10.1086/374598

    2003 doi

  55. [63]

    W., Rogers, W

    Zack, G. W., Rogers, W. E., & Latt, S. A. 1977, title Automatic measurement of sister chromatid exchange frequency., Journal of Histochemistry & Cytochemistry, 25, 741, 10.1177/25.7.70454

    1977 doi

  56. [64]

    2019, title Inclined massive planets in a protoplanetary disc: gap opening, disc breaking, and observational signatures , , 483, 4221, 10.1093/mnras/sty3358

    Zhu , Z. 2019, title Inclined massive planets in a protoplanetary disc: gap opening, disc breaking, and observational signatures , , 483, 4221, 10.1093/mnras/sty3358

    2019 doi

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.