The complex inner disk of the Herbig Ae star HD 100453 with VLTI/MATISSE

A. Matter; A. Meilland; B. Lopez; C. Dominik; D. Schertl; E. Kokoulina; E. Pantin; F. Bettonvil; F. Millour; G. Weigelt

arxiv: 2511.18981 · v1 · submitted 2025-11-24 · 🌌 astro-ph.SR · astro-ph.EP

The complex inner disk of the Herbig Ae star HD 100453 with VLTI/MATISSE

L. N. A. van Haastere , J. Varga , M. R. Hogerheijde , C. Dominik , M. Scheuck , A. Matter , R. van Boekel , B. Lopez

show 30 more authors

M. Abello J.-C. Augereau P. Boley W.-C. Danchi V. G\'amez Rosas Th. Henning K.-H. Hofmann M. Houll\'e W. Jaffe J. Kobus E. Kokoulina L. H. Leftley M. Letessier J. Ma F. Millour E. Pantin P. Priolet D. Schertl J. Scigliuto G. Weigelt S. Wolf P. Berio F. Bettonvil P. Cruzal\`ebes M. Heininger J.W. Isbell S. Lagarde A. Meilland R. Petrov S. Robbe-Dubois (the MATISSE Collaboration)

This is my paper

Pith reviewed 2026-05-17 05:41 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EP

keywords Herbig Ae starHD 100453protoplanetary diskVLTI interferometrydisk misalignmentinner disk radiusMATISSE observationstemperature gradient model

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The pith

MATISSE data confirm the inner disk of HD 100453 is misaligned with the outer disk at 47.5 degrees inclination and 0.27 au radius.

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

This paper extends prior H-band and K-band interferometry of the Herbig Ae star HD 100453 by adding L-band observations from the MATISSE instrument at the VLTI. It combines the new data with existing measurements to fit a parametric temperature gradient model across wavelengths and performs snapshot image reconstruction. The fit yields an inner disk inclination near 47.5 degrees and position angle near 83.6 degrees, reinforcing evidence for strong misalignment with the outer disk. The same-night MATISSE and GRAVITY observations, plus the reconstructed image, require higher-order asymmetries to match the signals. These results clarify the physical conditions in the inner regions where planets begin to form.

Core claim

The parametric model fitted to the combined PIONIER, GRAVITY, and MATISSE observations finds an inclination of approximately 47.5 degrees and a position angle of 83.6 degrees for the inner disk, which supports a strong misalignment with the outer disk. From the symmetric temperature gradient the inner disk radius is derived as roughly 0.27 au, with dust surface densities of about 10 to the minus 3.2 grams per square centimeter and vertical optical depths of 0.1 to 0.06 at the sublimation edge. Same-night MATISSE and GRAVITY measurements indicate that higher-order asymmetries are needed to explain the interferometric signals, a conclusion reinforced by MATISSE snapshot image reconstruction.

What carries the argument

The symmetric temperature gradient parametric model fitted jointly to multi-wavelength interferometric visibilities and closure phases, together with snapshot image reconstruction.

If this is right

The quantified misalignment angles provide direct constraints on the dynamical history of the inner and outer disk.
Higher-order asymmetries must be included in models to match the observed signals at L and K bands.
Coordinated GRAVITY and MATISSE observations are required to test whether the asymmetries persist or evolve.
The derived inner radius and optical depth values limit the possible dust composition and distribution near the star.

Where Pith is reading between the lines

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

If the asymmetries trace disk instabilities, they may alter the pathways and timescales for planet migration and growth.
Future observations spaced months apart could test whether the higher-order features vary on orbital timescales.
The same joint modeling approach could be applied to other Herbig stars known to host misaligned disks to check for common patterns.

Load-bearing premise

That a single symmetric temperature gradient remains valid across the full wavelength range and that the disk structure shows no significant evolution between observations taken years apart.

What would settle it

New multi-wavelength interferometric data that cannot be reproduced by the symmetric temperature gradient model, or repeated observations that reveal clear structural changes on timescales shorter than four years.

Figures

Figures reproduced from arXiv: 2511.18981 by A. Matter, A. Meilland, B. Lopez, C. Dominik, D. Schertl, E. Kokoulina, E. Pantin, F. Bettonvil, F. Millour, G. Weigelt, J.-C. Augereau, J. Kobus, J. Ma, J. Scigliuto, J. Varga, J.W. Isbell, K.-H. Hofmann, L. H. Leftley, L. N. A. van Haastere, M. Abello, M. Heininger, M. Houll\'e, M. Letessier, M. R. Hogerheijde, M. Scheuck, P. Berio, P. Boley, P. Cruzal\`ebes, P. Priolet, R. Petrov, R. van Boekel, S. Lagarde, S. Robbe-Dubois (the MATISSE Collaboration), S. Wolf, Th. Henning, V. G\'amez Rosas, W.-C. Danchi, W. Jaffe.

**Figure 1.** Figure 1: Overview of uv space and timeline covered by the selected MATISSE observations. Each night is indicated with a unique marker. The colour represents the AT station configurations. where I(λ) is the Fourier Transform of the interferogram, P(λ) is the photometric flux, and V 2 i j(λ) is the normalised squared visibility amplitude between a telescope pair i and j. Indices i, j, and k correspond to individual… view at source ↗

**Figure 2.** Figure 2: Calibrated squared visibilities and closure phases from all the selected MATISSE observations. between December 2020 and March 2021. For reduction and observation details for the PIONIER and GRAVITY data, see the respective Lazareff et al. 2017 and Bohn et al. 2022 papers. 3. Analysis of MATISSE observations In this section, we present the analysis of the MATISSE data in three parts. In Sect. 3.1 we show o… view at source ↗

**Figure 3.** Figure 3: Fit of the MATISSE data following a similar time-invariant parametric model and methodology as Lazareff et al. 2017 and Bohn et al. 2022 (Model-2, see [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

**Figure 4.** Figure 4: Violin-plot showcasing the time-variable MCMC fitting results of the asymmetry angle (θskwPA) for six epochs of MATISSE data, where the other disk parameters are fixed to the best-fit model-two asymmetric disk parameters from [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗

**Figure 5.** Figure 5: Panel A shows the L-band image reconstruction for the 2021 MATISSE AT observations, which contain the large-medium-small arrays observed within 11 days, at λ = 3.6 ± 0.2 µm using the SPARCO/MIRA software. The central star with T = 7250 K, modelled as a point source centred on (0,0), is not depicted. Over-plotted are ellipses where the semi-major axis are the half-light radius la, taken from the best parame… view at source ↗

**Figure 6.** Figure 6: Best-fit symmetric temperature gradient model. Top panels show the measured and modelled visibilities, bottom panels show the surface brightness distribution. The size of the central point source is not to scale, the colour scaling is homogeneous across all wavelengths [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗

**Figure 7.** Figure 7: Similar to [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗

read the original abstract

The inner regions of planet-forming disks hold invaluable insights for our understanding of planet formation. The disk around the Herbig star HD 100453 presents one such environment, with an inner disk that is significantly misaligned with respect to the outer disk. This paper expands the existing H-band (PIONIER) and K-band (GRAVITY) interferometric studies of the HD 100453 inner disk to the L-band with the MATISSE VLTI instrument. With snapshot data spanning approximately four years we aim for a more comprehensive understanding of the inner disk structures and their potential time evolution. Based on the MATISSE data obtained, we use a combination of analytical models and image reconstruction to constrain the disk structure. Additionally, we fit a temperature gradient model to the selected wavelength range of PIONIER, GRAVITY and MATISSE to derive physical properties of the inner regions. Our parametric model finds an inclination of $\sim 47.5^\circ$ and a position angle of $\sim 83.6^\circ$, which corroborates the case of strong inner-outer disk misalignment. From the symmetric temperature gradient we derive an inner disk radius around $\sim0.27$ au, with dust surface densities of $\Sigma_{\rm{subl}} \approx 10^{-3.2}$ g/cm$^2$ and vertical optical depth $\tau_{\rm{z, subl}} \approx 0.1-0.06$. Same-night MATISSE and GRAVITY observations indicate the necessity for higher-order asymmetries to explain the interferometric signals, which is further supported by a MATISSE snapshot image reconstruction. The chromatic interferometric data reveal the likely need for higher-order asymmetries to explain the inner disk of HD~100453, suggesting a possible origin in dynamic interactions or disk instabilities. Coordinated multi-wavelength infrared interferometric observations with GRAVITY and MATISSE will be crucial to confirm these findings and uncover its underlying nature.

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.

Desk Editor's Note private letter to a colleague

MATISSE L-band data on HD 100453 strengthens the misalignment case and flags higher-order asymmetries, but the reported inner radius and densities rest on a symmetric temperature gradient that the same observations appear to challenge.

read the letter

The core new piece is the addition of L-band MATISSE snapshot visibilities and closure phases to the existing H- and K-band interferometry on this Herbig Ae star. Same-night MATISSE plus GRAVITY runs plus a MATISSE image reconstruction both point to the need for azimuthal structure beyond simple misalignment, which is a useful step beyond the prior PIONIER and GRAVITY papers. The parametric fit to the combined wavelength range gives an inner radius near 0.27 au, inclination around 47.5 degrees, and low optical depth at the sublimation front; those numbers line up with the misalignment story already in the literature. The multi-epoch coverage over four years is also straightforward to appreciate as an attempt to look for variability. The modeling combines analytic temperature gradients with image reconstruction, which is a reasonable way to handle the sparse uv-coverage typical of VLTI snapshots. The call for future coordinated GRAVITY-MATISSE runs is practical. The soft spot is the tension between the symmetric gradient used to extract radius and surface density and the explicit statement that higher-order asymmetries are required to fit the same-night data. If the asymmetries affect the L-band visibilities that anchor the sublimation radius, the azimuthally averaged temperature profile could shift the inferred location and optical depth. Treating four years of snapshots as static adds another layer of uncertainty if low-level changes are present. The abstract does not spell out formal model comparison or error propagation on the key parameters, so a referee would want to see those checks in the full text. This work is mainly for people already following interferometric studies of inner disks around Herbig stars and planet formation in misaligned systems. A reader who needs concrete multi-wavelength constraints on one well-studied object will get something from it. It is grounded enough in new observations to merit a serious referee rather than a desk reject, mainly to verify whether the symmetric-model parameters survive once the asymmetry evidence is folded in properly. I would send it to review with a request for clearer quantification of how much the asymmetries bias the reported radius and densities.

Referee Report

2 major / 2 minor

Summary. The paper presents new L-band VLTI/MATISSE interferometric snapshot observations of the inner disk of the Herbig Ae star HD 100453, extending prior H-band (PIONIER) and K-band (GRAVITY) studies. It combines parametric modeling assuming a symmetric temperature gradient with image reconstruction on multi-epoch data spanning ~4 years to derive an inner-disk inclination of ~47.5°, position angle of ~83.6°, sublimation radius of ~0.27 au, dust surface density Σ_subl ≈ 10^{-3.2} g cm^{-2}, and vertical optical depth τ_z,subl ≈ 0.1-0.06. The authors conclude that same-night MATISSE+GRAVITY data and the MATISSE image reconstruction require higher-order asymmetries, pointing to possible dynamic interactions or instabilities.

Significance. If the results hold, the work supplies quantitative multi-wavelength constraints on a strongly misaligned inner disk, a key laboratory for planet formation and disk dynamics. Strengths include the joint use of parametric fits and image reconstruction plus same-night multi-instrument coverage; these provide direct, falsifiable measurements of misalignment and inner radius that can be tested against hydrodynamic models of warped disks.

major comments (2)

[Parametric modeling / temperature gradient fit] Parametric modeling section (temperature-gradient fit to combined PIONIER/GRAVITY/MATISSE visibilities): the headline inner radius (~0.27 au), Σ_subl, and τ_z,subl are derived under the assumption of azimuthal symmetry in the temperature profile, yet the manuscript states that same-night MATISSE+GRAVITY data plus the MATISSE snapshot reconstruction both require higher-order asymmetries. If non-axisymmetric brightness variations are present at L-band wavelengths that dominate the sublimation-radius constraint, the azimuthally averaged model will bias the inferred sublimation front location and vertical optical depth.
[Data combination and multi-epoch discussion] Multi-epoch analysis: the paper combines snapshot observations spanning four years without explicit tests for time variability or evolution. Any low-level changes in disk structure between epochs would decouple the wavelength regimes and undermine the asymmetry interpretation drawn from the combined dataset.

minor comments (2)

[Abstract] Abstract: reported values for inclination, position angle, and inner radius lack explicit uncertainties or model-selection details; adding these would improve clarity.
[Parametric model description] Notation: the precise definition and wavelength dependence of the vertical optical depth τ_z,subl should be stated explicitly when introduced in the temperature-gradient model.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comments. We address each major comment below and describe the changes incorporated in the revised version.

read point-by-point responses

Referee: [Parametric modeling / temperature gradient fit] Parametric modeling section (temperature-gradient fit to combined PIONIER/GRAVITY/MATISSE visibilities): the headline inner radius (~0.27 au), Σ_subl, and τ_z,subl are derived under the assumption of azimuthal symmetry in the temperature profile, yet the manuscript states that same-night MATISSE+GRAVITY data plus the MATISSE snapshot reconstruction both require higher-order asymmetries. If non-axisymmetric brightness variations are present at L-band wavelengths that dominate the sublimation-radius constraint, the azimuthally averaged model will bias the inferred sublimation front location and vertical optical depth.

Authors: We agree that the parametric temperature-gradient model assumes azimuthal symmetry and that detected higher-order asymmetries could in principle introduce a bias in the derived average parameters, particularly since the L-band data contribute strongly to the sublimation-radius constraint. The symmetric model was adopted to obtain a first-order, azimuthally averaged description that can be compared directly with earlier H- and K-band results. In the revised manuscript we have added an explicit discussion of this limitation in the modeling section, clarifying that the reported inner radius, surface density and optical depth represent effective azimuthally averaged quantities and noting the complementary role of the image reconstruction in revealing asymmetries. revision: yes
Referee: [Data combination and multi-epoch discussion] Multi-epoch analysis: the paper combines snapshot observations spanning four years without explicit tests for time variability or evolution. Any low-level changes in disk structure between epochs would decouple the wavelength regimes and undermine the asymmetry interpretation drawn from the combined dataset.

Authors: The observations consist of snapshots acquired over approximately four years. We verified that the visibility data from the different epochs are consistent within the measurement uncertainties before combining them. In the revised manuscript we have added a short paragraph in the observations and data-reduction section that documents this consistency check and states the assumption of temporal stability over the observed baseline. We acknowledge that the current dataset does not permit a detailed variability analysis and that more densely sampled observations would be required to fully exclude low-level structural evolution. revision: yes

Circularity Check

0 steps flagged

No significant circularity; parameters derived from direct fitting to new interferometric data

full rationale

The paper fits a symmetric temperature gradient model to combined PIONIER/GRAVITY/MATISSE visibilities and closure phases to derive inclination (~47.5°), position angle (~83.6°), inner radius (~0.27 au), surface density, and optical depth. These are outputs of a standard parametric fit to external observational constraints rather than any reduction by construction to prior fitted quantities or self-citations. The acknowledgment of higher-order asymmetries from same-night data and image reconstruction is presented as an independent finding, not a loop that forces the symmetric-model results. No self-definitional steps, fitted inputs renamed as predictions, or load-bearing self-citations appear in the derivation chain. The work is self-contained against the new VLTI data.

Axiom & Free-Parameter Ledger

5 free parameters · 2 axioms · 0 invented entities

Central claims rest on parametric fits to interferometric observables and standard assumptions in radiative transfer modeling of Herbig star disks; multiple free parameters are adjusted to match the new observations.

free parameters (5)

inclination = ~47.5°
Fitted parameter from parametric model to interferometric data
position angle = ~83.6°
Fitted parameter for disk orientation
inner disk radius = ~0.27 au
Derived from symmetric temperature gradient fit across wavelengths
dust surface density at sublimation = ~10^{-3.2} g/cm²
Fitted to reproduce observed fluxes and optical depths
vertical optical depth at sublimation = 0.1-0.06
Derived parameter from temperature gradient model

axioms (2)

domain assumption Inner disk can be described by a symmetric temperature gradient model that applies uniformly from H to L band
Invoked to derive physical properties from combined PIONIER, GRAVITY and MATISSE data
domain assumption Interferometric signals are adequately captured by a combination of analytical parametric models and snapshot image reconstruction
Basis for concluding that higher-order asymmetries are required

pith-pipeline@v0.9.0 · 5892 in / 1659 out tokens · 65484 ms · 2026-05-17T05:41:32.420491+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

5 extracted references · 5 canonical work pages

[1]

M., Lim, P

Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, 935, 167 Ataiee, S., Pinilla, P., Zsom, A., et al. 2013, A&A, 553, L3 Avenhaus, H., Quanz, S. P., Schmid, H. M., et al. 2017, AJ, 154, 33 Bae, J., Isella, A., Zhu, Z., et al. 2023, in Astronomical Society of the Pacific Conference Series, V ol. 534, Protostars and Planets VII, ed. S...

work page 2022
[2]

An important underlying assump- tion is that this assumes the measurement errors are independent and Gaussian distributed

Typically IR interferometry reports the error estimate on fitted parameters as the 16%−84% intervals from settled MCMC chains. An important underlying assump- tion is that this assumes the measurement errors are independent and Gaussian distributed. However, this method is flawed as in- terferometric observables, especially when working with multi- ple sp...

work page 2020
[3]

(g/cm2) = 3.208+0.001 0.001 0.280 0.284 0.288 0.292 Apio (Jy) Apio (Jy) = 0.285+0.002 0.002 3.50 3.25 3.00 2.75 ppio ppio = 3.149+0.133 0.137 0.4876 0.4882 0.4888 0.4894 Agrav (Jy) Agrav (Jy) = 0.488+0.000 0.000 3.040 3.032 3.024 3.016 pgrav pgrav = 3.025+0.005 0.005 0.692 0.696 0.700 0.704 0.708 Amat (Jy) Amat (Jy) = 0.700+0.002 0.002 0.2710 0.2713 0.271...

work page 2095
[4]

D.1.Temperature gradient model best-fit MCMC chains, forR out =10 AU, after removing burn-in to the combined PIONIER, GRA VITY & MATISSE datasets

(g/cm2) 0.280 0.284 0.288 0.292 Apio (Jy) 3.50 3.25 3.00 2.75 ppio 0.4876 0.4882 0.4888 0.4894 Agrav (Jy) 3.040 3.032 3.024 3.016 pgrav 0.692 0.696 0.700 0.704 0.708 Amat (Jy) 0.0 0.2 0.4 0.6 pmat pmat = 0.432+0.087 0.088 Fig. D.1.Temperature gradient model best-fit MCMC chains, forR out =10 AU, after removing burn-in to the combined PIONIER, GRA VITY & M...

work page 2000
[5]

Appendix E: MATISSE/GRAVITY comparison of closure phases on the same nights Figure E.1 shows a comparison of how the simulated closure phases for the skewed ring look in practice. From both visual inspection and theχ 2 r -maps it is clear that theθ skwPA ∼92 ◦ rep- resents the MATISSE data much better than the best fit value θskwPA ∼ −173 ◦ from the GRA V...

work page 2021

[1] [1]

M., Lim, P

Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, 935, 167 Ataiee, S., Pinilla, P., Zsom, A., et al. 2013, A&A, 553, L3 Avenhaus, H., Quanz, S. P., Schmid, H. M., et al. 2017, AJ, 154, 33 Bae, J., Isella, A., Zhu, Z., et al. 2023, in Astronomical Society of the Pacific Conference Series, V ol. 534, Protostars and Planets VII, ed. S...

work page 2022

[2] [2]

An important underlying assump- tion is that this assumes the measurement errors are independent and Gaussian distributed

Typically IR interferometry reports the error estimate on fitted parameters as the 16%−84% intervals from settled MCMC chains. An important underlying assump- tion is that this assumes the measurement errors are independent and Gaussian distributed. However, this method is flawed as in- terferometric observables, especially when working with multi- ple sp...

work page 2020

[3] [3]

(g/cm2) = 3.208+0.001 0.001 0.280 0.284 0.288 0.292 Apio (Jy) Apio (Jy) = 0.285+0.002 0.002 3.50 3.25 3.00 2.75 ppio ppio = 3.149+0.133 0.137 0.4876 0.4882 0.4888 0.4894 Agrav (Jy) Agrav (Jy) = 0.488+0.000 0.000 3.040 3.032 3.024 3.016 pgrav pgrav = 3.025+0.005 0.005 0.692 0.696 0.700 0.704 0.708 Amat (Jy) Amat (Jy) = 0.700+0.002 0.002 0.2710 0.2713 0.271...

work page 2095

[4] [4]

D.1.Temperature gradient model best-fit MCMC chains, forR out =10 AU, after removing burn-in to the combined PIONIER, GRA VITY & MATISSE datasets

(g/cm2) 0.280 0.284 0.288 0.292 Apio (Jy) 3.50 3.25 3.00 2.75 ppio 0.4876 0.4882 0.4888 0.4894 Agrav (Jy) 3.040 3.032 3.024 3.016 pgrav 0.692 0.696 0.700 0.704 0.708 Amat (Jy) 0.0 0.2 0.4 0.6 pmat pmat = 0.432+0.087 0.088 Fig. D.1.Temperature gradient model best-fit MCMC chains, forR out =10 AU, after removing burn-in to the combined PIONIER, GRA VITY & M...

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[5] [5]

Appendix E: MATISSE/GRAVITY comparison of closure phases on the same nights Figure E.1 shows a comparison of how the simulated closure phases for the skewed ring look in practice. From both visual inspection and theχ 2 r -maps it is clear that theθ skwPA ∼92 ◦ rep- resents the MATISSE data much better than the best fit value θskwPA ∼ −173 ◦ from the GRA V...

work page 2021