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arxiv: 2606.23794 · v1 · pith:ND3DSTSHnew · submitted 2026-06-22 · 🌌 astro-ph.EP · astro-ph.SR

MINDS: Complementary inclinations in the binary system HK Tau reveal gas- and ice-phase chemistry

Alice Somigliana , Giulia Perotti , Nicol\'as T. Kurtovic , Thomas Henning , Myriam Benisty , Andrew D. Sellek , Melissa McClure , Zak L. Smith
show 13 more authors
Aditya M. Arabhavi Alessio Caratti o Garatti Valentin Christiaens Ewine F. van Dishoeck Danny Gasman Sierra L. Grant Manuel G\"udel Till Kaeufer Inga Kamp Lucas Stapper Beno\^it Tabone Milou Temmink Marissa Vlasblom
This is my paper

Pith reviewed 2026-06-26 07:01 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords protoplanetary discsbinary starsice absorptionmolecular linesdisc inclinationJWST observationsdisc chemistryoutflows
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The pith

The differing inclinations in the HK Tau binary enable a simultaneous view of gas-phase molecular lines and ice absorption in coeval protoplanetary discs.

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

The paper presents JWST/MIRI spectra of the HK Tau binary, where the primary disc at 57 degrees inclination shows strong molecular emission lines dominated by CO2, while the secondary at 83 degrees is mostly line-poor. Thermochemical models demonstrate that high inclination blocks most molecular lines but permits detection of ice absorption features against the continuum. This configuration allows the detection of water ice, CO2 ice, and ammonium ice in the edge-on disc, providing a direct comparison of solid and gaseous components in discs of the same age. Extended emissions suggest low-velocity winds, more prominent around the edge-on source.

Core claim

HK Tau consists of a low-inclination primary showing a line-rich, CO2-dominated spectrum and an edge-on secondary that is line-poor but exhibits ice absorption bands at 6.2, 13.6, 15.2, and 6.85 μm. Thermochemical disc models coupled with radiative transfer show that at inclinations comparable to that of HK Tau B, only ionised atomic lines are expected to remain visible in the spectra. While blocking molecular emission lines, the edge-on configuration allows ice absorption bands to be visible against the continuum. Extended H2 emission is present around both discs, although much more elongated in HK Tau B, and the morphology of ionised atomic lines suggests a low-velocity wind origin with a

What carries the argument

The complementary inclinations (57° for the primary and 83° for the secondary) of the two protoplanetary discs, which selectively transmit either gas emission lines or ice absorption depending on the viewing angle.

If this is right

  • Water ice at 6.2 and 13.6 μm, CO2 ice at 15.2 μm, and NH4+ ice at 6.85 μm appear in absorption in the edge-on secondary.
  • The distinctive X-shaped H2 emission and [Ar II], [Ne II], [Ne III] lines around the secondary indicate a low-velocity wind with approximately 70 degree semi-opening angle.
  • Neither source shows PAH emission features.
  • The primary exhibits lower forbidden line fluxes and smaller H2 extent, implying any wind launched from it is too cold or dense to be ionised.

Where Pith is reading between the lines

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

  • Mixed-inclination binaries could serve as natural laboratories for tracking how gas and ice chemistry co-evolve without comparing unrelated systems at different ages.
  • The wide-angle wind detected around the secondary may clear material over large solid angles, affecting the outer disc regions where planets could form.
  • Absence of PAHs in both components suggests limited aromatic processing under the local radiation field or disc conditions.

Load-bearing premise

The spectral differences between the two discs are driven primarily by their measured inclinations rather than by intrinsic differences in disc mass, temperature structure, or evolutionary state.

What would settle it

Finding strong molecular emission lines dominating the spectrum of an edge-on disc like HK Tau B, or ice absorption features appearing in a low-inclination disc like HK Tau A, would contradict the claim that inclination alone controls the observed gas versus ice visibility.

Figures

Figures reproduced from arXiv: 2606.23794 by Aditya M. Arabhavi, Alessio Caratti o Garatti, Alice Somigliana, Andrew D. Sellek, Beno\^it Tabone, Danny Gasman, Ewine F. van Dishoeck, Giulia Perotti, Inga Kamp, Lucas Stapper, Manuel G\"udel, Marissa Vlasblom, Melissa McClure, Milou Temmink, Myriam Benisty, Nicol\'as T. Kurtovic, Sierra L. Grant, Thomas Henning, Till Kaeufer, Valentin Christiaens, Zak L. Smith.

Figure 1
Figure 1. Figure 1: Integrated MIRI-MRS spectrum of HK Tau A (top) and B (bottom) in grey, with the black line representing the continuum [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the continuum-subtracted spectrum of HK Tau A (top panel, dark grey) and B (bottom panel) in the 13.5-16.2 [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Emission at the wavelength of [Ar II], [Ne II], and [Ne III] from HK Tau A (top panel, yellow line) and B (bottom panel, [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Moment 0 maps of the S(1), S(2), and S(3) H [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Pixel-by-pixel temperature (left) and total column density (centre) maps of the extended H [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Synthetic spectra of a fiducial T Tauri disc model ( [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of the [Ne III]/[Ne II] (top panel) and [Ne II]/[Ar II] (bottom panel) line ratios for HK Tau A and B (orange shaded re￾gion) and the other published detections. Bi￾nary systems are marked with a black contour. The coloured dashed lines show the line ratio thresholds to determine the dominant irradia￾tion source. Sz Cha from Espaillat et al. (2023), T Cha from Bajaj et al. (2024), RW Aur B and V… view at source ↗
Figure 8
Figure 8. Figure 8: Moment 8 map of the [Ne II] emission around HK Tau A [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
read the original abstract

[Abridged] HK Tau is a roughly equal mass pre-main sequence binary system consisting of a low-inclination primary (57 deg) and an edge-on (83 deg) secondary. We present JWST/MIRI observations targeting both sources, taken as part of the JWST GTO program MINDS. The spectra reveal a line-rich, CO2-dominated primary and a line-poor secondary; this evidence, albeit in line with the evolutionary-motivated trend uncovered by recent observations of binaries at MIRI wavelengths, is likely due to the different configuration of the two sources. Indeed, thermochemical disc models coupled with radiative transfer show that, at inclinations comparable to that of HK Tau B, only ionised atomic lines are expected to remain visible in the spectra. While blocking molecular emission lines, however, the edge-on configuration allows ice absorption bands to be visible against the continuum; in this framework, the HK Tau system provides an unprecedented opportunity to have a simultaneous view of the solid and gaseous component of a pair of coeval protoplanetary discs, thanks to the complementary inclination of the two sources. We detect water ice at 6.2 and 13.6um, CO2 ice at 15.2um, and NH4+ ice at 6.85um in the spectrum of HK Tau B; an additional absorption band between 8.3 and 9um is compatible with both silicate stretching and C-H bending. Neither of the two sources show signs of PAHs. Extended H2 emission is present around both discs, although much more elongated in HK Tau B. The distinctive 'X' shape centred in B, combined with the intensity, morphology, and spectral characteristics of the ionised atomic lines [Ar II], [Ne II], and [Ne III] suggests a low-velocity wind origin with a wide (~ 70 deg) semi-opening angle. The lower forbidden line fluxes and smaller extent of the H2 emission around A imply that, if a wind is launched from the primary as well, it is too cold or dense to be ionised.

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 / 2 minor

Summary. The manuscript reports JWST/MIRI spectra of the HK Tau binary, with component A at 57° inclination showing a line-rich, CO2-dominated spectrum and component B at 83° showing a line-poor spectrum. Thermochemical disc models coupled to radiative transfer are invoked to attribute the contrast to inclination, with high inclination suppressing molecular lines while permitting ice absorption against the continuum. Ice features (H2O at 6.2 and 13.6 μm, CO2 at 15.2 μm, NH4+ at 6.85 μm) are detected only in B; extended H2 and ionised atomic lines ([Ar II], [Ne II], [Ne III]) are interpreted as a wide-angle wind from B. The central claim is that the complementary inclinations enable a simultaneous view of gas- and ice-phase chemistry in coeval discs.

Significance. The direct detection of molecular lines, ice absorption bands, and extended emission provides new mid-IR constraints on a resolved binary system with known inclinations. If the models can be shown to reproduce the specific observed fluxes and SEDs of HK Tau A and B, the work would strengthen the case that inclination geometry alone can produce the observed gas/ice contrast, offering a useful benchmark for interpreting MIRI spectra of other discs.

major comments (2)
  1. [modeling discussion (abstract and § on thermochemical models)] The thermochemical + radiative-transfer models (discussed in the abstract and modeling sections) are presented only as demonstrating the general effect “at inclinations comparable to that of HK Tau B”; no section shows that the adopted disc mass, radial temperature profile, or vertical structure were fitted to HK Tau-specific observables such as ALMA continuum fluxes or SEDs. This is load-bearing for the claim that inclination, rather than intrinsic differences, drives the line-rich vs. line-poor contrast.
  2. [abstract and results on spectral comparison] The interpretation that the spectral differences provide an “unprecedented simultaneous view” of gas and ice phases rests on the assumption that the two discs are otherwise identical; without a quantitative demonstration that the models match the observed continuum levels and line-to-continuum ratios for both components, alternative explanations (differing disc masses or evolutionary states) cannot be ruled out.
minor comments (2)
  1. [H2 emission discussion] Clarify whether the extended H2 emission morphology and the 'X' shape are quantified with position-velocity diagrams or only described qualitatively.
  2. [ice absorption features] The statement that the additional 8.3–9 μm band is “compatible with both silicate stretching and C-H bending” would benefit from a brief comparison to laboratory spectra or other MIRI observations.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments. We address each major point below, clarifying the scope of the modeling and the basis for our interpretation while agreeing to add explicit caveats in the revised manuscript.

read point-by-point responses

  1. Referee: [modeling discussion (abstract and § on thermochemical models)] The thermochemical + radiative-transfer models (discussed in the abstract and modeling sections) are presented only as demonstrating the general effect “at inclinations comparable to that of HK Tau B”; no section shows that the adopted disc mass, radial temperature profile, or vertical structure were fitted to HK Tau-specific observables such as ALMA continuum fluxes or SEDs. This is load-bearing for the claim that inclination, rather than intrinsic differences, drives the line-rich vs. line-poor contrast.

    Authors: We agree that the models are illustrative of the general inclination effect rather than component-specific fits. They demonstrate that at inclinations ~83°, molecular lines are strongly suppressed while ice absorption can appear against the continuum, reproducing the qualitative contrast seen in the data. The models use standard T Tauri disc parameters from prior work. We will revise the modeling section and abstract to state explicitly that no fitting to HK Tau ALMA fluxes or SEDs was performed and that a full optimization is outside the present scope. The interpretation still rests on the coeval, equal-mass nature of the binary minimizing intrinsic differences, combined with the demonstrated geometric effect. revision: partial

  2. Referee: [abstract and results on spectral comparison] The interpretation that the spectral differences provide an “unprecedented simultaneous view” of gas and ice phases rests on the assumption that the two discs are otherwise identical; without a quantitative demonstration that the models match the observed continuum levels and line-to-continuum ratios for both components, alternative explanations (differing disc masses or evolutionary states) cannot be ruled out.

    Authors: We acknowledge that a quantitative reproduction of the observed continuum levels and line-to-continuum ratios for both components would provide stronger support. The current models show only the qualitative suppression of lines at high inclination. Because the components are coeval and of comparable mass, we consider intrinsic differences less likely, but we accept that this is an assumption. We will revise the abstract, results, and discussion sections to moderate the phrasing around the “unprecedented simultaneous view,” add an explicit caveat regarding the lack of component-specific modeling, and note that alternative explanations cannot be fully excluded without further tailored modeling. revision: partial

Circularity Check

0 steps flagged

No significant circularity; central result is observational detection interpreted with general models

full rationale

The paper reports JWST/MIRI spectra of HK Tau A (57°) and B (83°), noting line-rich vs line-poor spectra and ice absorptions only in B. It invokes thermochemical + radiative-transfer models only to illustrate the general effect of high inclination on suppressing molecular lines while allowing ice absorption. No parameters are fitted to HK Tau data and then redefined as predictions; no self-citation chain or uniqueness theorem is load-bearing for the core claim. The interpretation rests on external model behavior at comparable inclinations, making the derivation self-contained against observational benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; no explicit free parameters, axioms, or invented entities are stated. The thermochemical models invoked are treated as standard tools whose internal parameters are not enumerated here.

pith-pipeline@v0.9.1-grok · 6029 in / 1162 out tokens · 24798 ms · 2026-06-26T07:01:32.901582+00:00 · methodology

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