MINDS. The influence of outer dust disc structure on the volatile delivery to the inner disc

Aditya M. Arabhavi; Adrian M. Glauser; Alessio Caratti o Garatti; Andrew Sellek; Beno\^it Tabone; Danny Gasman; David Barrado; Ewine F. van Dishoeck; Giulia Perotti; Hyerin Jang

REVIEW 2 major objections 4 minor 131 references

MINDS. The influence of outer dust disc structure on the volatile delivery to the inner disc

T0 review · 2 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read Gaps in planet-forming dust discs do not stop water from reaching the inner disc.

desk verdict The main claim—that gaps don't fully block water delivery—holds up, but the secondary carbon-dichotomy claim is partly a normalization artifact and needs to be re-tested before it can be stated as cleanly as the abstract does. read the letter →

arxiv 2501.04587 v1 pith:FP2ZYSAW submitted 2025-01-08 astro-ph.EP

Danny Gasman , Milou Temmink , Ewine F. van Dishoeck , Nicolas T. Kurtovic , Sierra L. Grant , Andrew Sellek , Benoît Tabone , Thomas Henning

show 13 more authors

Inga Kamp Manuel Güdel David Barrado Alessio Caratti o Garatti Adrian M. Glauser L. B. F. M. Waters Aditya M. Arabhavi Hyerin Jang Jayatee Kanwar Julia L. Lienert Giulia Perotti Kamber Schwarz Marissa Vlasblom

This is my paper · ORCID

classification astro-ph.EP

keywords protoplanetarydiscsastrochemistryJWSTMIRI/MRSspectroscopyALMAcontinuumwateremissioncarbon-bearingmoleculesdustgapsandcavitiespebbledrift

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 tests the idea that pressure bumps and gaps in the outer regions of planet-forming discs cut off the inward drift of icy pebbles and thereby starve the inner disc of $\mathrm{H_2O}$. Comparing JWST mid-infrared spectra of $\mathrm{H_2O}$, $\mathrm{HCN}$, $\mathrm{C_2H_2}$, and $\mathrm{CO_2}$ with newly fitted ALMA dust-disc structures in ten gapped discs, the authors find that the presence of a dust gap does not necessarily result in weak $\mathrm{H_2O}$ emission. Discs with very wide gaps or cavities can still show strong cold $\mathrm{H_2O}$ emission, suggesting that radial transport of icy material is hard to block completely. The data also reveal a dichotomy: discs lacking a cold $\mathrm{H_2O}$ excess tend to show stronger emission from carbon-bearing molecules such as $\mathrm{HCN}$ and $\mathrm{C_2H_2}$, while water-rich discs are carbon-poor.

What carries the argument

The comparison is carried by the outer dust structure, recovered from new visibility-plane fits of ALMA Band 6 data using a set of Gaussian components, and by the inner-disc molecular emission measured as integrated line fluxes and line ratios. The key empirical tracer is the cold $\mathrm{H_2O}$ excess: the relative strength of the 23.8–24 $\mu$m $\mathrm{H_2O}$ quadruplet and the ratio of the $11_{7,4}-10_{4,7}$ and $11_{7,4}-10_{6,5}$ lines, which probe the coldest, roughly 400 K water reservoir near the snowline. A cold excess is read as evidence that icy pebbles or small dust grains are still drifting in and sublimating even when the ALMA profile shows a gap. Each disc is then placed on an interpretive scenario diagram that separates shallow, moderately leaky, deep, and photoevaporative gaps; the observed water/carbon dichotomy is the pattern that emerges from that placement.

What would settle it

Measure cold $\mathrm{H_2O}$ column densities, for example through $\mathrm{H_2^{18}O}$, in a larger sample whose gap depths and locations are fixed by uniform high-resolution ALMA imaging; if the deepest gaps systematically suppress the cold water reservoir while shallow gaps do not, the paper's conclusion that gaps cannot fully block icy delivery would be overturned.

Watch

Extended reading notes

Core claim

On the paper's own terms, the central discovery is that neither ordinary gaps nor extreme cavities reliably cut off the inward delivery of water-bearing material. The authors re-analyse ALMA continuum visibilities to locate the outer dust radius and the innermost gap in each disc, then compare these with MIRI/MRS line fluxes and line ratios. They find that the deepest, closest-in gap in their sample, in Sz 98, still shows a clear cold $\mathrm{H_2O}$ excess, and the two widest-gap discs, PDS 70 and SY Cha, are more $\mathrm{H_2O}$-dominated than carbon-dominated. From this they conclude that fully blocking radial dust drift is difficult to achieve; gas and small dust leaking across gaps can still replenish the inner disc. A secondary discovery is the clean split between discs with a cold $\mathrm{H_2O}$ excess and discs with elevated $\mathrm{HCN}$ and $\mathrm{C_2H_2}$ emission, which they tie to different stages or efficiencies of volatile transport and chemical reprocessing.

Load-bearing premise

The load-bearing premise is that the ALMA visibility-plane fits recover the true outer dust radii and gap structures consistently across a sample with heterogeneous resolution, inclination, and uv-coverage; if beam-size or fitting artefacts create or hide substructures, the classification of gaps as inside or outside the snowlines, and therefore the scenario assignments, would change.

Editorial extensions

If this is right

Gaps and cavities should not be treated as shut-off valves for water delivery when interpreting inner-disc spectra or predicting the material available to forming planets.
Discs with a strong cold $\mathrm{H_2O}$ excess and weak carbon emission, such as Sz 98 and SY Cha, are consistent with partially leaky gaps or small-dust transport, so models should include a leaky dust fraction.
The water/carbon dichotomy implies that inner-disc C/O ratios vary between discs, and that a missing cold $\mathrm{H_2O}$ reservoir can flag a carbon-rich inner disc.
Disc age and gap-formation timescale become decisive: whether a disc looks water-rich or carbon-rich depends on when its gap formed and how fast the disc evolves.
The radial location of the gap relative to the CO and CH$_4$ snowlines matters less if volatiles are trapped in $\mathrm{H_2O}$ ice or reprocessed into less volatile ices, so future work should constrain trapping.

Reading between the lines

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

If the dichotomy holds in a larger sample, the cold $\mathrm{H_2O}$ excess could serve as a practical spectral indicator of ongoing icy pebble delivery, letting surveys classify discs without expensive ALMA gap-depth measurements.
A natural test is to compare the same cold/warm $\mathrm{H_2O}$ ratio and $\mathrm{HCN}$/$\mathrm{C_2H_2}$ fluxes against gap depths measured in gas tracers such as CO isotopologues, since gas gaps are often shallower than dust gaps and the scenario assignments assume the dust structure tracks the transport.
The paper's wide-gap results imply that the inner disc of a planet-hosting system like PDS 70 can be continually resupplied; if so, the volatile content of forming terrestrial planets may be set less by gap formation than by the leakiness of dust-gas coupling, a prediction that detailed pebble-trapping models could test.
A quantifiable prediction is that among discs with similar outer structure, younger systems should show stronger cold $\mathrm{H_2O}$ excess than older counterparts; correlating the dichotomy with stellar ages would test the timing interpretation.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Two things to know about this one. First, the main empirical claim holds up: a dust gap, even a very wide one, does not necessarily suppress cold H2O emission in the inner disc. The evidence is existence arguments—Sz 98, SY Cha, and PDS 70 all show cold H2O despite deep or wide gaps—and that is the durable part of the paper. Second, the secondary claim, the dichotomy between cold-H2O-depleted discs and carbon-rich discs, is weaker than the abstract makes it sound. The stress-test note is right: discs are grouped by cold H2O strength relative to warm H2O, and then the figure that displays the split divides carbon line fluxes by cold H2O. A depressed denominator pushes those ratios up even if the carbon lines are ordinary. The paper itself notes that only two of the four 'depleted' discs (DL Tau and V1094 Sco) are actually enhanced relative to warm H2O; for GW Lup and CI Tau the apparent carbon enhancement is mostly a small-H2Ocold artifact. That is a structural confound, not just a missing p-value.

What the paper does well: consistent re-reduction of the JWST MIRI/MRS spectra, careful line-flux measurements with slab-fit subtraction, and a genuinely useful reanalysis of archival ALMA data in the visibility plane that turns up new substructures (the 16 au gap in V1094 Sco, the small cavity in BP Tau). The authors are also unusually explicit about their caveats—ages, gap formation timescales, resolution effects, the lack of a gap-free control sample. The correlation analysis against outer dust radius is moderate at best, and they say so.

Soft spots, in proportion: the sample is ten discs, two of which are special transition discs; the correlations exclude PDS 70 and SY Cha; and the dichotomy needs to be re-tested on an absolute or warm-H2O-normalized basis before it can support the abstract's wording. None of this sinks the main point, but the carbon-dichotomy claim should be revised or heavily qualified.

Who it's for: people working on inner-disk chemistry and planet formation who want an observational counterpart to the drift/gap models (Kalyaan, Mah, Sellek, Lienert). It is a useful reference even with the caveats.

Recommendation: send it to peer review, but the referee should ask for the dichotomy analysis to be redone on a denominator-independent basis. The paper is honest enough that this is a fixable revision, not a rejection.

Referee Report

2 major / 4 minor

Summary. This paper uses JWST MIRI/MRS spectra of ten T Tauri disks (eight with confirmed ALMA gaps and two transition disks with wide cavities) to compare inner-disk molecular emission (H2O, HCN, C2H2, CO2) with outer dust disk structure derived from new visibility-plane fits to ALMA Band 6 data. The authors report that disks with gaps can still show strong cold H2O emission (e.g., Sz 98, SY Cha, PDS 70), suggesting that gaps do not fully block volatile delivery. They also report a dichotomy between disks with a cold H2O excess and disks with enhanced carbon-bearing emission, and interpret the results with several model-based scenarios.

Significance. The paper provides a valuable, consistently reduced dataset: all MIRI/MRS spectra are reduced with the same pipeline version, the ALMA visibilities are fit with a uniform method, and the line fluxes and fit parameters are tabulated in full. The existence argument that wide or deep gaps do not fully suppress cold H2O emission is credible and important, as it challenges simple pebble-trapping scenarios. The secondary claim of a carbon/H2O dichotomy is less secure and is the main weakness of the manuscript.

major comments (2)

[3.3.5, Fig. 7] The claimed dichotomy between cold-H2O-depleted discs and enhanced carbon emission is not established by the data because of a normalization confound. The sample is divided into 'depleted' and 'excess' groups based on the strength of H2Ocold relative to DR Tau (Sect. 3.3.1, Figs. 4-5), and the right column of Fig. 7 then plots carbon line fluxes divided by H2Ocold. Any disc with a small H2Ocold flux will automatically move upward in these panels regardless of its absolute carbon flux. The authors themselves note in Sect. 3.3.5 that 'no dichotomy appears in the ratios with H2Owarm' and that only DL Tau and V1094 Sco are clearly enhanced in carbon relative to warm H2O. For GW Lup and CI Tau, the apparent HCN/C2H2 enhancement in the cold-normalized panels likely reflects the small denominator rather than elevated carbon emission. The abstract's statement that a lack of colder H2O 'goes hand in hand with elevated emission from carbon-bearing species' is therefore an overstatement. Please re-express the carbon comparisons on an absolute or warm-H2O-normalized basis, or restrict the claim to the two discs that actually show enhanced carbon fluxes.
[3.3.5, Fig. 7, Table 4] The proposed dichotomy is not supported by a statistical test or a quantitative separation measure. The paper provides Pearson coefficients for the Rdust correlations (Fig. 3) but no equivalent test for the group separation in Fig. 7, and with only eight full discs (plus two transition discs) the visual separation in the right column can be driven by one or two objects. Given that the warm-H2O-normalized ratios show no dichotomy, the conclusion should be explicitly limited to the specific discs DL Tau and V1094 Sco, or the authors should provide a statistically meaningful comparison (e.g., a two-sample test on absolute carbon fluxes or on carbon/warm-H2O ratios between the depleted and excess groups).

minor comments (4)

[2.5] The sentence 'DR Tau is an H2O-rich source is a source rich in H2O lines' contains a duplicated clause; please rephrase.
[4.6] The phrase 'Furthermore, it it would be useful to identify' should read 'Furthermore, it would be useful to identify'.
[Table 4] The column header 'CO2 (N)' is not defined in the table notes; please define the abbreviation (presumably a column-density tracer) or rename the column.
[Appendix B.8] The sentence 'as is shown in Table 3' appears to refer to the emission summary (Table 4) rather than the freeze-out temperature table; please correct the cross-reference.

Circularity Check

1 steps flagged · score 6.0 of 10

The cold-H2O vs carbon dichotomy is partly a normalization artifact: the groups are defined by cold-H2O strength, yet the supporting figure divides carbon fluxes by cold-H2O.

self definitional [Sect. 3.3.5 (Fig. 7, right column); abstract; Sect. 5 conclusion]
"First, no dichotomy appears in the ratios with H2Owarm between the sources that are depleted or enhanced in H2Ocold. Generally, only two of the depleted sources are stronger in carbon emission compared to the warmer H2O: DL Tau and V1094 Sco. On the other hand, a split occurs between the samples for the ratio with colder H2O. The depleted sources are stronger in carbon, especially HCN and C2H2 [...] the relative lack of colder H2O-emission seems to go hand in hand with elevated emission from carbon-bearing species."

The depleted/excess grouping is assigned in Sect. 3.3.1 by comparing each disc's cold H2O lines to DR Tau after rescaling on warm H2O (H2Owarm, disc/H2Owarm,DR Tau). The right column of Fig. 7, cited as evidence for the dichotomy, plots carbon line flux divided by H2Ocold—the very quantity that defines the groups. A disc classified as depleted in cold H2O has a small H2Ocold by construction, so its carbon/H2Ocold ratio is inflated unless the carbon flux falls in lockstep. The paper itself concedes that in warm-H2O-normalized ratios only DL Tau and V1094 Sco are enhanced; for GW Lup and CI Tau the apparent HCN/C2H2 excess is therefore a normalization artifact rather than an independent detection of elevated carbon.

full rationale

The paper's primary observational claim—that the presence of a dust gap does not necessarily weaken H2O emission and that fully blocking radial drift seems difficult—is an empirical comparison of two independent datasets (JWST MIRI/MRS line fluxes and ALMA visibility-plane fits) and does not reduce to its inputs. The ALMA radii and gap locations are derived from new visibility fits with stated methods and compared to previous works; no circularity there. The scenario interpretation in Fig. 8 draws on models from overlapping author groups (Kalyaan, Mah, Sellek, Lienert), but those models are used as interpretive context, not as the evidence for the observational correlations, and the central observational result stands independently of them. The one significant circularity is in the secondary dichotomy claim: discs are categorized by their cold-H2O strength relative to warm H2O, and the key supporting figure then normalizes carbon fluxes by cold H2O. That makes an apparent split in carbon/H2Ocold partly guaranteed by the grouping definition. The paper's own warm-H2O-normalized ratios show only two of the four 'depleted' discs are actually carbon-enhanced, so the abstract's broader 'goes hand in hand' statement is not independently established. This is a partial, localized circularity affecting one of the two headline results, while the other main finding remains self-contained.

Assumptions & free parameters 4 free parameters · 8 assumptions · 0 invented entities

No new physical entities are introduced. The main fitted inputs are the L_acc normalization exponent, the flaring angle for snowline positions, the energy thresholds that define warm and cold water lines, and the Gaussian parameters of the visibility fits; all are taken from prior work or fitted to the data rather than derived from first principles.

free parameters (4)

L_acc scaling exponent = 0.6
Adopted from Banzatti et al. (2020, 2023a) to normalize fluxes; the paper divides all fluxes by L_acc^0.6 and does not re-fit or marginalize over this slope, so a wrong slope would change trend strengths.
Flaring angle phi_inc = 0.05
Assumed to estimate snowline locations via Eq. (2), following Dullemond & Dominik (2004); snowline positions relative to gaps are central to the scenario interpretations in Sec. 4.1.
Warm and cold H2O line energy thresholds = Eup < 4000 K (cold), 6000-8000 K (warm)
Thresholds from Banzatti et al. (2023a) used to define H2Ocold and H2Owarm fluxes; the dichotomy depends on this split.
Visibility-fit Gaussian parameters = Per-source values in Table C.2
Number of Gaussians and their amplitudes, widths, and spatial frequencies are free parameters fitted to ALMA visibilities; the resulting gap radii and depths are central to the comparison. The number of components is chosen visually.

assumptions (8)

domain assumption Millimetre dust continuum traces the distribution of drifting pebbles, and dust gaps correspond to pressure bumps that can partially block pebble transport.
The entire paper interprets ALMA gaps as obstacles to volatile delivery; invoked throughout, especially Sec. 1 and 4.1.
domain assumption Mid-infrared line fluxes of H2O, HCN, C2H2, and CO2 trace the column densities of these molecules in the inner disc, at least for relative comparisons.
Used in Sec. 2.3 and 3.3; the paper itself caveats that flux depends on emitting area and optical depth (Grant et al. 2023; Sec. 4.4).
domain assumption A simple power-law temperature profile (Eq. 1) with a fixed flaring angle gives reliable snowline locations for all full discs.
Used in Sec. 2.7 to place snowlines relative to gaps; the paper notes this fails for SY Cha and PDS 70 and is resolution-dependent.
domain assumption Freeze-out temperatures of H2O, CO2, CH4, and CO are known from laboratory measurements and apply to these discs.
Laboratory values from Martin-Domenech et al. (2014) and Luna et al. (2014) are used in Eq. (2); they are treated as fixed inputs.
ad hoc to paper Dividing H2O line fluxes by L_acc^0.6 removes the dominant dependence on accretion luminosity, so residual differences reflect disc structure.
Sec. 2.3; the exponent is from prior fits, not re-derived for this sample.
domain assumption The visibility-plane fitting model (sum of Gaussians modulated by sinusoids) is flexible enough to recover true substructures.
App. C; relies on Hankel transform and Gaussian decomposition following Zhang et al. (2016).
standard math Pearson correlation coefficients and p-values are applicable to this small, non-random sample as a heuristic despite the limited size.
Sec. 2.4; the authors caution that the sample is too small for conclusive results.
domain assumption Literature disc and stellar ages are reliable enough to assign evolutionary scenarios.
Used throughout Sec. 4.3 and App. B; the paper notes that ages are very uncertain and may be based on different methods.

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Cite this review

Pith. "Pith review of MINDS. The influence of outer dust disc structure on the volatile delivery to the inner disc." pith.science (2026). https://pith.science/paper/FP2ZYSAW

@misc{pith2026250104587,
  author       = {Pith},
  title        = {Pith review of: MINDS. The influence of outer dust disc structure on the volatile delivery to the inner disc},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/FP2ZYSAW}},
  note         = {Machine review of arXiv:2501.04587}
}

abstract

ALMA has revealed that the millimetre dust structures of protoplanetary discs are extremely diverse. It has been proposed that the strength of H$_2$O emission in the inner disc particularly depends on the influx of icy pebbles from the outer disc, a process that would correlate with the outer dust disc radius, and that could be prevented by pressure bumps. This work aims to assess the influence of pressure bumps on the inner disc's molecular reservoirs. Using JWST's MIRI/MRS, we compared the observational emission properties of H$_2$O, HCN, C$_2$H$_2$, and CO$_2$ with the outer dust disc structure from ALMA observations, in eight discs with confirmed gaps in ALMA observations, and two discs with gaps of tens of astronomical units in width, around stars with $M_\star \geq 0.45M_{\odot}$. We used new visibility plane fits of the ALMA data to determine the outer dust disc radius and identify substructures in the discs. We find that the presence of a dust gap does not necessarily result in weak H$_2$O emission. Furthermore, the relative lack of colder H$_2$O-emission seems to go hand in hand with elevated emission from carbon-bearing species. The discs with cavities and extremely wide gaps appear to behave as a somewhat separate group, with stronger cold H$_2$O emission and weak warm H$_2$O emission. We conclude that fully blocking radial dust drift from the outer disc seems difficult to achieve. However, there does seem to be a dichotomy between discs that show a strong cold H$_2$O excess and ones that show strong emission from HCN and C$_2$H$_2$. Better constraints on the influence of the outer dust disc structure and inner disc composition require more information on substructure formation timescales and disc ages, along with the importance of trapping of volatiles like CO and CO$_2$ into more strongly bound ices like H$_2$O and chemical transformation of CO into less volatile species.

Figures

Figures reproduced from arXiv: 2501.04587 by the authors.

**Figure 2.** Radial profiles of the disc sample based on the analysis in the image (black line) and visibility plane (grey line). The snowline [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗

**Figure 3.** Average of integrated line fluxes of warm (top, orange) [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗

Figures from the paper (6 more)

**Figure 5.** Figure 5: Line flux ratio of the column density tracer from slab [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]

**Figure 4.** Figure 4: Comparison of warm (indicated by the red triangle) and [PITH_FULL_IMAGE:figures/full_fig_p009_4.png]

**Figure 6.** Figure 6: Continuum-subtracted spectra, zoomed in on C [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]

**Figure 7.** Figure 7: Ratio of line fluxes of carbon-bearing molecules and [PITH_FULL_IMAGE:figures/full_fig_p012_7.png]

**Figure 8.** Figure 8: Emission properties of the inner disc based on the modelling works by Kalyaan et al. (2021), Kalyaan et al. (2023), Mah [PITH_FULL_IMAGE:figures/full_fig_p013_8.png]

**Figure 8.** Figure 8: Appendix C: Estimating radii and gaps from ALMA Appendix C.1: ALMA observations As we are interested in the substructures closest to the host star, we have retrieved all the highest available spatial resolution ALMA observations publicly available for our sources. We …

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Works this paper leans on

131 extracted references · 31 canonical work pages

[1]

, " * 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 ...
[2]

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....
[3]

M., Manara , C

Alcal \'a , J. M., Manara , C. F., Natta , A., et al. 2017, , 600, A20

2017
[4]

2014, in Protostars and Planets VI, ed

Alexander , R., Pascucci , I., Andrews , S., Armitage , P., & Cieza , L. 2014, in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 475--496

2014
[5]

L., P \'e rez , L

ALMA Partnership , Brogan , C. L., P \'e rez , L. M., et al. 2015, , 808, L3

2015
[6]

M., Huang , J., P \'e rez , L

Andrews , S. M., Huang , J., P \'e rez , L. M., et al. 2018, , 869, L41

2018
[7]

P., van der Marel , N., et al

Ansdell , M., Williams , J. P., van der Marel , N., et al. 2016, , 828, 46

2016
[8]

2015, , 582, A105

Antonellini , S., Kamp , I., Riviere-Marichalar , P., et al. 2015, , 582, A105

2015

Show all 131 references

[9]

Antonellini , S., Kamp , I., & Waters , L. B. F. M. 2023, , 672, A92

2023
[10]

M., Kamp , I., Henning , T., et al

Arabhavi , A. M., Kamp , I., Henning , T., et al. 2024, Science, 384, 1086

2024
[11]

R., et al

Argyriou , I., Glasse , A., Law , D. R., et al. 2023, , 675, A111

2023
[12]

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

2023
[13]

M., Brittain , S., et al

Banzatti , A., Abernathy , K. M., Brittain , S., et al. 2022, , 163, 174

2022
[14]

D., et al

Banzatti, A., Pascucci, I., Bosman, A. D., et al. 2020, The Astrophysical Journal, 903, 124

2020
[15]

M., Carr , J

Banzatti , A., Pontoppidan , K. M., Carr , J. S., et al. 2023 a , , 957, L22

2023
[16]

M., P \'e re Ch \'a vez , J., et al

Banzatti , A., Pontoppidan , K. M., P \'e re Ch \'a vez , J., et al. 2023 b , , 165, 72

2023
[17]

M., Salyk , C., et al

Banzatti , A., Pontoppidan , K. M., Salyk , C., et al. 2017, , 834, 152

2017
[18]

M., et al

Banzatti , A., Salyk , C., Pontoppidan , K. M., et al. 2024, arXiv e-prints, arXiv:2409.16255, accepted for publication in

2024 arXiv
[19]

2021, , 916, L2

Benisty , M., Bae , J., Facchini , S., et al. 2021, , 916, L2

2021
[20]

Bergez-Casalou , C., Bitsch , B., Pierens , A., Crida , A., & Raymond , S. N. 2020, , 643, A133

2020
[21]

Boogert , A. C. A., Gerakines , P. A., & Whittet , D. C. B. 2015, , 53, 541

2015
[22]

A., Clarke , C

Booth , R. A., Clarke , C. J., Madhusudhan , N., & Ilee , J. D. 2017, , 469, 3994

2017
[23]

Booth , R. A. & Ilee , J. D. 2019, , 487, 3998

2019
[24]

D., Walsh , C., & van Dishoeck , E

Bosman , A. D., Walsh , C., & van Dishoeck , E. F. 2018, , 618, A182

2018
[25]

M., Pontoppidan , K

Brown , J. M., Pontoppidan , K. M., van Dishoeck , E. F., et al. 2013, , 770, 94

2013
[26]

2023, JWST Calibration Pipeline , Zenodo

Bushouse , H., Eisenhamer , J., Dencheva , N., et al. 2023, JWST Calibration Pipeline , Zenodo

2023
[27]

Carr , J. S. & Najita , J. R. 2011, , 733, 102

2011
[28]

J., Tazzari , M., Juhasz , A., et al

Clarke , C. J., Tazzari , M., Juhasz , A., et al. 2018, , 866, L6

2018
[29]

P., Anderson , M

Collings , M. P., Anderson , M. A., Chen , R., et al. 2004, , 354, 1133

2004
[30]

2024, , 688, A81

Delussu , L., Birnstiel , T., Miotello , A., et al. 2024, , 688, A81

2024
[31]

F., Bouvier , J., Alencar , S

Donati , J. F., Bouvier , J., Alencar , S. H., et al. 2020, , 491, 5660

2020
[32]

Dullemond , C. P. & Dominik , C. 2004, , 421, 1075

2004
[33]

Eistrup , C., Walsh , C., & van Dishoeck , E. F. 2018, , 613, A14

2018
[34]

2022, pybaselines: A Python library of algorithms for the baseline correction of experimental data , Zenodo

Erb , D. 2022, pybaselines: A Python library of algorithms for the baseline correction of experimental data , Zenodo

2022
[35]

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

Foreman-Mackey , D., Hogg , D. W., Lang , D., & Goodman , J. 2013, , 125, 306

2013
[36]

Gaia Collaboration , Prusti , T., de Bruijne , J. H. J., et al. 2016, , 595, A1

2016
[37]

Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2022, arXiv e-prints, arXiv:2208.00211

2022 arXiv
[38]

2022, , 667, A124

Gangi , M., Antoniucci , S., Biazzo , K., et al. 2022, , 667, A124

2022
[39]

C., et al

Gasman , D., Argyriou , I., Sloan , G. C., et al. 2023 a , , 673, A102

2023
[40]

F., Grant , S

Gasman , D., van Dishoeck , E. F., Grant , S. L., et al. 2023 b , , 679, A117

2023
[41]

E., Meijerink , R., & Najita , J

Glassgold , A. E., Meijerink , R., & Najita , J. R. 2009, , 701, 142

2009
[42]

L., van Dishoeck , E

Grant , S. L., van Dishoeck , E. F., Tabone , B., et al. 2023, , 947, L6

2023
[43]

J., Kamp , I., Waters , L

Greenwood , A. J., Kamp , I., Waters , L. B. F. M., Woitke , P., & Thi , W. F. 2019, , 626, A6

2019
[44]

P., et al

Haugb lle , T., Weber , P., Wielandt , D. P., et al. 2019, , 158, 55

2019
[45]

2024, , 136, 054302

Henning , T., Kamp , I., Samland , M., et al. 2024, , 136, 054302

2024
[46]

Herczeg , G. J. & Hillenbrand , L. A. 2014, , 786, 97

2014
[47]

M., Dullemond , C

Huang , J., Andrews , S. M., Dullemond , C. P., et al. 2018, , 869, L42

2018
[48]

2024, , 691, A148

Jang , H., Waters , R., Kaeufer , T., et al. 2024, , 691, A148

2024
[49]

A., Tazzari , M., Clarke , C

Jennings , J., Booth , R. A., Tazzari , M., Clarke , C. J., & Rosotti , G. P. 2022 a , , 509, 2780

2022
[50]

A., Tazzari , M., Rosotti , G

Jennings , J., Booth , R. A., Tazzari , M., Rosotti , G. P., & Clarke , C. J. 2020, , 495, 3209

2020
[51]

J., Booth , R

Jennings , J., Tazzari , M., Clarke , C. J., Booth , R. A., & Rosotti , G. P. 2022 b , , 514, 6053

2022
[52]

2023, , 954, 66

Kalyaan , A., Pinilla , P., Krijt , S., et al. 2023, , 954, 66

2023
[53]

D., & Banzatti , A

Kalyaan , A., Pinilla , P., Krijt , S., Mulders , G. D., & Banzatti , A. 2021, , 921, 84

2021
[54]

M., et al

Kamp , I., Henning , T., Arabhavi , A. M., et al. 2023, Faraday Discussions, 245, 112

2023
[55]

2024, , 689, A231

Kanwar , J., Kamp , I., Jang , H., et al. 2024, , 689, A231

2024
[56]

Kenyon , S. J. & Hartmann , L. 1987, , 323, 714

1987
[57]

P., et al

Kessler-Silacci , J., Augereau , J.-C., Dullemond , C. P., et al. 2006, , 639, 275

2006
[58]

2023, , 945, L7

K \'o sp \'a l , \'A ., \'A brah \'a m , P., Diehl , L., et al. 2023, , 945, L7

2023
[59]

D., Zhang , K., et al

Krijt , S., Bosman , A. D., Zhang , K., et al. 2020, , 899, 134

2020
[60]

R., Bergin , E

Krijt , S., Schwarz , K. R., Bergin , E. A., & Ciesla , F. J. 2018, , 864, 78

2018
[61]

S., Burkhardt , C., Budde , G., & Kleine , T

Kruijer , T. S., Burkhardt , C., Budde , G., & Kleine , T. 2017, Proceedings of the National Academy of Science, 114, 6712

2017
[62]

R., Argyriou , I., Gordon , K

Law , D. R., Argyriou , I., Gordon , K. D., et al. 2024, arXiv e-prints, arXiv:2409.15435, accepted for publication in

2024 arXiv
[63]

L., Bitsch , B., & Henning , T

Lienert , J. L., Bitsch , B., & Henning , T. 2024, , 691, A72

2024
[64]

Ligterink , N. F. W., Kipfer , K. A., & Gavino , S. 2024, , 687, A224

2024
[65]

J., Harsono , D., et al

Long , F., Herczeg , G. J., Harsono , D., et al. 2019, , 882, 49

2019
[66]

J., et al

Long , F., Pinilla , P., Herczeg , G. J., et al. 2018, , 869, 17

2018
[67]

Lubow , S. H. & D'Angelo , G. 2006, , 641, 526

2006
[68]

\'A ., Santonja , C., & Domingo , M

Luna , R., Satorre , M. \'A ., Santonja , C., & Domingo , M. 2014, , 566, A27

2014
[69]

2023, , 677, L7

Mah , J., Bitsch , B., Pascucci , I., & Henning , T. 2023, , 677, L7

2023
[70]

2024, , 686, L17

Mah , J., Savvidou , S., & Bitsch , B. 2024, , 686, L17

2024
[71]

F., Fedele , D., Herczeg , G

Manara , C. F., Fedele , D., Herczeg , G. J., & Teixeira , P. S. 2016, , 585, A136

2016
[72]

M., Bueno , J., & Goesmann , F

Mart \' n-Dom \'e nech , R., Mu \ n oz Caro , G. M., Bueno , J., & Goesmann , F. 2014, , 564, A8

2014
[73]

M., Blake , G

Meijerink , R., Pontoppidan , K. M., Blake , G. A., Poelman , D. R., & Dullemond , C. P. 2009, , 704, 1471

2009
[74]

C., & Kataoka , A

Miotello , A., Kamp , I., Birnstiel , T., Cleeves , L. C., & Kataoka , A. 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 , 501

2023
[75]

2022, , 934, 74

Molli \`e re , P., Molyarova , T., Bitsch , B., et al. 2022, , 934, 74

2022
[76]

2016, , 267, 368

Morbidelli , A., Bitsch , B., Crida , A., et al. 2016, , 267, 368

2016
[77]

2016, , 832, 41

Mordasini , C., van Boekel , R., Molli \`e re , P., Henning , T., & Benneke , B. 2016, , 832, 41

2016
[78]

2018, , 617, L2

M \"u ller , A., Keppler , M., Henning , T., et al. 2018, , 617, L2

2018
[79]

R., Carr , J

Najita , J. R., Carr , J. S., Pontoppidan , K. M., et al. 2013, , 766, 134

2013
[80]

\"O berg , K. I. & Bergin , E. A. 2021, , 893, 1

2021
[81]

I., Guzm \'a n , V

\"O berg , K. I., Guzm \'a n , V. V., Walsh , C., et al. 2021, , 257, 1

2021
[82]

I., Murray-Clay , R., & Bergin , E

\"O berg , K. I., Murray-Clay , R., & Bergin , E. A. 2011, , 743, L16

2011
[83]

J., J rgensen , J

Ohashi , N., Tobin , J. J., J rgensen , J. K., et al. 2023, , 951, 8

2023
[84]

2023, , 75, 424

Orihara , R., Momose , M., Muto , T., et al. 2023, , 75, 424

2023
[85]

2022, , 937, 36

Pacetti , E., Turrini , D., Schisano , E., et al. 2022, , 937, 36

2022
[86]

2009, , 696, 143

Pascucci , I., Apai , D., Luhman , K., et al. 2009, , 696, 143

2009
[87]

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

Pascucci , I., Cabrit , S., Edwards , S., 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 , 567

2023
[88]

S., & Bruderer , S

Pascucci , I., Herczeg , G., Carr , J. S., & Bruderer , S. 2013, , 779, 178

2013
[89]

Pearson , T. J. 1999, in Astronomical Society of the Pacific Conference Series, Vol. 180, Synthesis Imaging in Radio Astronomy II, ed. G. B. Taylor , C. L. Carilli , & R. A. Perley , 335

1999
[90]

Pecaut , M. J. & Mamajek , E. E. 2016, , 461, 794

2016
[91]

2023, Nature, 620, 516

Perotti, G., Christiaens, V., Henning, T., et al. 2023, Nature, 620, 516

2023
[92]

2024, , 686, A135

Pinilla , P., Benisty , M., Waters , R., Bae , J., & Facchini , S. 2024, , 686, A135

2024
[93]

Pontoppidan , K. M. 2006, , 453, L47

2006
[94]

M., Salyk , C., Banzatti , A., et al

Pontoppidan , K. M., Salyk , C., Banzatti , A., et al. 2024, , 963, 158

2024
[95]

M., Salyk , C., Bergin , E

Pontoppidan , K. M., Salyk , C., Bergin , E. A., et al. 2014, in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 363--385

2014
[96]

M., Salyk , C., Blake , G

Pontoppidan , K. M., Salyk , C., Blake , G. A., et al. 2010, , 720, 887

2010
[97]

2024, , 965, 48

Potapov , A., J \"a ger , C., Mutschke , H., & Henning , T. 2024, , 965, 48

2024
[98]

H., Wright , G

Rieke , G. H., Wright , G. S., B \"o ker , T., et al. 2015, , 127, 584

2015
[99]

2023, , 135, 048001

Rigby , J., Perrin , M., McElwain , M., et al. 2023, , 135, 048001

2023
[100]

E., Banzatti , A., \"O berg , K

Romero-Mirza , C. E., Banzatti , A., \"O berg , K. I., et al. 2024, , 975, 78

2024
[101]

P., Ilee , J

Rosotti , G. P., Ilee , J. D., Facchini , S., et al. 2021, , 501, 3427

2021
[102]

A., Meijerhof , J

Rota , A. A., Meijerhof , J. D., van der Marel , N., et al. 2024, , 684, A134

2024
[103]

M., Blake , G

Salyk , C., Pontoppidan , K. M., Blake , G. A., Najita , J. R., & Carr , J. S. 2011, , 731, 130

2011
[104]

R., Henning , T., Christiaens , V., et al

Schwarz , K. R., Henning , T., Christiaens , V., et al. 2024, , 962, 8

2024
[105]

M., Schmiedeke , A., Pineda , J

Segura-Cox , D. M., Schmiedeke , A., Pineda , J. E., et al. 2020, , 586, 228

2020
[106]

D., Vlasblom , M., & van Dishoeck , E

Sellek , A. D., Vlasblom , M., & van Dishoeck , E. F. 2024, arXiv e-prints, arXiv:2412.01895, in press in

2024 arXiv
[107]

Skinner , S. L. & Audard , M. 2022, , 938, 134

2022
[108]

M., Hogerheijde , M

Stapper , L. M., Hogerheijde , M. R., van Dishoeck , E. F., & Mentel , R. 2022, , 658, A112

2022
[109]

A., McClure , M

Sturm , J. A., McClure , M. K., Beck , T. L., et al. 2023, , 679, A138

2023
[110]

F., et al

Tabone , B., Bettoni , G., van Dishoeck , E. F., et al. 2023, Nature Astronomy, 7, 805

2023
[111]

2017, , 606, A88

Tazzari , M., Testi , L., Natta , A., et al. 2017, , 606, A88

2017
[112]

F., Gasman , D., et al

Temmink , M., van Dishoeck , E. F., Gasman , D., et al. 2024 a , , 689, A330

2024
[113]

F., Grant , S

Temmink , M., van Dishoeck , E. F., Grant , S. L., et al. 2024 b , , 686, A117

2024
[114]

D., Krijt , S., Mulders , G

Van der Marel , N., Bosman , A. D., Krijt , S., Mulders , G. D., & Bergner , J. B. 2021, , 653, L9

2021
[115]

P., & Tobin , J

van der Marel , N., Dong , R., di Francesco , J., Williams , J. P., & Tobin , J. 2019, , 872, 112

2019
[116]

F., Bruderer , S., et al

van der Marel , N., van Dishoeck , E. F., Bruderer , S., et al. 2016, , 585, A58

2016
[117]

F., Grant , S., Tabone , B., et al

van Dishoeck , E. F., Grant , S., Tabone , B., et al. 2023, Faraday Discussions, 245, 52

2023
[118]

F., Herbst , E., & Neufeld , D

van Dishoeck , E. F., Herbst , E., & Neufeld , D. A. 2013, Chemical Reviews, 113, 9043

2013
[119]

E., van Dishoeck , E

van Terwisga , S. E., van Dishoeck , E. F., Ansdell , M., et al. 2018, , 616, A88

2018
[120]

E., et al

Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261

2020
[121]

F., Doty , S

Visser , R., van Dishoeck , E. F., Doty , S. D., & Dullemond , C. P. 2009, , 495, 881

2009
[122]

P., Dever , J

Viti , S., Collings , M. P., Dever , J. W., McCoustra , M. R. S., & Williams , D. A. 2004, , 354, 1141

2004
[123]

F., Tabone , B., & Bruderer , S

Vlasblom , M., van Dishoeck , E. F., Tabone , B., & Bruderer , S. 2024, , 682, A91

2024
[124]

W., Glasse, A., et al

Wells, M., Pel, J. W., Glasse, A., et al. 2015, PASP, 127, 646

2015
[125]

F., et al

Woitke , P., Min , M., Thi , W. F., et al. 2018, , 618, A57

2018
[126]

F., Kamp , I., & Hogerheijde , M

Woitke , P., Thi , W. F., Kamp , I., & Hogerheijde , M. R. 2009, , 501, L5

2009
[127]

S., Rieke , G

Wright , G. S., Rieke , G. H., Glasse , A., et al. 2023, , 135, 048003

2023
[128]

S., Wright, D., Goodson, G

Wright, G. S., Wright, D., Goodson, G. B., et al. 2015, Publications of the Astronomical Society of the Pacific, 127, 595

2015
[129]

E., Turner , N

Yu , M., Willacy , K., Dodson-Robinson , S. E., Turner , N. J., & Evans , Neal J., I. 2016, , 822, 53

2016
[130]

A., Blake , G

Zhang , K., Bergin , E. A., Blake , G. A., et al. 2016, , 818, L16

2016
[131]

2023, , 952, 108

Zhang , S., Kalscheur , M., Long , F., et al. 2023, , 952, 108

2023

Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.

[1] [1]

, " * 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 ...

[2] [2]

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....

[3] [3]

M., Manara , C

Alcal \'a , J. M., Manara , C. F., Natta , A., et al. 2017, , 600, A20

2017

[4] [4]

2014, in Protostars and Planets VI, ed

Alexander , R., Pascucci , I., Andrews , S., Armitage , P., & Cieza , L. 2014, in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 475--496

2014

[5] [5]

L., P \'e rez , L

ALMA Partnership , Brogan , C. L., P \'e rez , L. M., et al. 2015, , 808, L3

2015

[6] [6]

M., Huang , J., P \'e rez , L

Andrews , S. M., Huang , J., P \'e rez , L. M., et al. 2018, , 869, L41

2018

[7] [7]

P., van der Marel , N., et al

Ansdell , M., Williams , J. P., van der Marel , N., et al. 2016, , 828, 46

2016

[8] [8]

2015, , 582, A105

Antonellini , S., Kamp , I., Riviere-Marichalar , P., et al. 2015, , 582, A105

2015