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A 72-disk JWST census finds that every jet comes with a wind

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-01 06:52 UTC pith:34DOLVXN

load-bearing objection Reference-size census of H2 winds and [Ne II] jets in Class II disks with a credible accretion-rate trend, but the wind classification needs a quantitative test against flared-disk-surface emission before the evolutionary story is sold. the 3 major comments →

arxiv 2607.21733 v1 pith:34DOLVXN submitted 2026-07-23 astro-ph.EP

JWST/MIRI Reveals the Evolution from Molecular to Atomic Disk Winds

Naman S. Bajaj , Ilaria Pascucci , Sylvie Cabrit , Suzan Edwards , Gabriele Cugno , Andrew D. Sellek , Joan R. Najita , Ke Zhang
show 5 more authors
Richard Alexander Gregory J. Herczeg Uma Gorti Sophie C. Clark Tracy L. Beck
This is my paper
classification astro-ph.EP
keywords protoplanetary disksdisk windsjetsJWST MIRIH2 emissionNe II emissionmass accretion ratephotoevaporation
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Using archival JWST/MIRI integral-field observations of 72 inclined planet-forming disks, this paper tries to show that disk outflows follow a staged sequence: actively accreting young disks drive fast atomic jets embedded in hot molecular winds, while older, lower-accretion disks show mostly atomic winds with fainter or absent jets. The authors identify 46 conical H2 winds and 40 spatially resolved [Ne II] jets, and find that 85% of the jets come with an H2 wind, with the remainder showing an atomic wind in [O I]. Detection fractions of jets and H2 winds rise with mass accretion rate and are independent of disk inclination and stellar mass, while the hottest molecular wind lines fade fastest as accretion drops. If correct, disk dispersal is not one process but an evolution from MHD-launched molecular winds to photoevaporative atomic winds, and the MIRI census becomes a reference sample for wind-launching models.

Core claim

The paper's central claim is that there is a one-to-one correspondence between atomic jets and disk winds, and that the wind's composition evolves with disk age. Concretely: 34 of 40 sources with [Ne II] jets also show extended H2 wind emission, and the few jet sources without H2 winds show [O I] low-velocity-component winds where data exist. The jet and molecular-wind detection fractions increase with mass accretion rate (to about 80% above 1e-8 solar masses per year) with no dependence on inclination or stellar mass, whereas marginally resolved low-velocity [Ne II] winds are found preferentially at low accretion rates. Among H2 winds, the hot inner lines S(5) and S(7) fade faster than the

What carries the argument

The identification framework rests on two quantitative tools. First, extended emission is assessed by comparing spaxel-by-spaxel encircled-flux curves of line maps against calibration-star PSFs using a chi-square threshold, with a rescaling step to catch faint extended structure. Second, wind-like H2 emission is classified by a line-map ratio (LR) versus continuum-map ratio (CR) test: if the line brightness inside two opposing 100-degree triangular regions perpendicular to the disk position angle exceeds the continuum ratio and the line extends beyond the continuum, the source is classified as a wind. [Ne II] jets are classified from pixel-by-pixel velocity maps corrected for stellar radial

Load-bearing premise

The load-bearing premise is that cone-shaped, extended H2 emission perpendicular to the disk traces a wind; if the cones are instead infalling gas, scattered light, or PSF artifacts, the jet-wind correspondence and the molecular-to-atomic sequence lose their foundation.

What would settle it

Measure high-resolution (R>30,000) spatially resolved velocity maps of the H2 S(1) line for a dozen of the 46 classified wind sources: an MHD wind predicts outflowing kinematics (blueshifted near side, increasing velocity with height), while infall predicts redshifted motions toward the star and no forward motion; either result would settle the classification.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • The outflow census (46 H2 winds, 40 [Ne II] jets) becomes a statistical reference for wind-launching models in Class II disks.
  • Wind-driven accretion models gain support: if every jet has a wind, mass loss and angular momentum removal are coupled rather than independent.
  • Disk dispersal models must include a molecular MHD wind phase before photoevaporation takes over, shifting the timing of inner disk clearing.
  • Accretion rate, not stellar mass or inclination, is the controlling variable for outflow detectability across the 0.1-1 solar mass range.
  • Hot H2 lines S(5) and S(7) serve as sensitive evolutionary indicators of inner wind weakening.

Where Pith is reading between the lines

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

  • A testable corollary the paper leaves implicit: transitional disks with inner dust cavities and low accretion should show S(1) molecular winds but little or no S(5)/S(7) hot wind, and their [Ne II] should be a low-velocity photoevaporative wind rather than a jet.
  • If the wind and jet are a single MHD system, their combined mass-loss rate should scale with accretion rate; re-analyzing the measured H2 and [Ne II] surface brightnesses to derive mass-loss rates would test this directly.
  • The infall-versus-wind ambiguity for cone-shaped H2 could be settled with spatially resolved velocity maps in, say, the H2 S(1) line at high spectral resolution; that would also discriminate MHD from photoevaporative launching.
  • The red-shifted lobe dominance in IRAS-04385 and WSB52, framed as evidence for the Hall effect, invites a quantitative comparison with non-ideal MHD simulations to see whether such asymmetry is reproduced.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. This paper presents a JWST/MIRI MRS survey of 72 inclined (i>40°) mostly Class II protoplanetary disks, identifying spatially extended H2 S(1)/S(3)/S(5)/S(7) and [Ne II] 12.81 µm emission. A morphological/kinematic framework is used to classify 46 conical H2 winds and 40 [Ne II] jets, with 34 sources showing both. The authors report that outflow detection fractions increase with accretion rate, are roughly flat with stellar mass and inclination up to ~80°, and that hotter H2 wind tracers (S(5), S(7)) decline preferentially at low accretion rates. Combining these results with literature [O I] 6300 Å spectroscopy, they propose an evolutionary sequence in which actively accreting disks host atomic jets and molecular MHD winds, while lower-accretion disks transition to predominantly atomic, photoevaporative winds.

Significance. If the classifications and trends withstand scrutiny, this would be the largest systematic census of spatially resolved disk winds and jets to date, providing a benchmark for wind-launching and disk-dispersal models. The paper has notable strengths: a uniform, fully specified calibration pipeline; quantitative extended-emission and wind/jet classification criteria; explicit SNR-based sensitivity checks in Figure 11; cross-checks against published [O I] spectroscopy and earlier MIRI detections; and a public data set with documented analysis choices. The proposed staged outflow sequence is a falsifiable prediction that connects Class 0/I outflow studies to disk clearing at Class II. The main risk is not internal inconsistency but the unvalidated morphological assumption that extended H2 emission in the 100° cones traces outflows rather than flared disk surfaces or other non-wind structure. That assumption underlies the census that drives all downstream statistics.

major comments (3)
  1. [§4.1/Abstract] The LR>CR test does not uniquely isolate a conical wind: a flared, inclined disk surface also projects warm gas into the 100° cones perpendicular to the disk PA. The two sources that had to be rescued by visual inspection after the automated test failed—SYCha and FTTau (Fig. 4)—are low-inclination cases where a bowl-like surface morphology is naturally expected. The manuscript lists 'extended disk surfaces' as an alternative origin but provides no quantitative false-positive test (e.g., injecting wind-free disk models into the classifier). Since the 46-wind census drives the accretion-rate trend, the S(5)/S(7) decline, and the jet–wind correspondence, a non-negligible disk-surface contamination rate would directly weaken the central evolutionary claim. Please add a quantitative test, or at minimum demonstrate that the classified morphologies cannot be reproduced by plausible disk surface
  2. [§4.5, Fig. 11] The claim that all [Ne II] jets have a corresponding wind is stronger than the data support. Of the 40 jets, 34 have H2 winds; of the remaining 6, only 2 single sources have published [O I] high-resolution data (both show LVC), while 2 single sources and 2 binaries have no [O I] constraint. Thus the abstract's 'All sources with [NeII] jets exhibit a corresponding wind traced in either H2 (85%) or [OI]' is not directly established. The supported statement is 34/40 plus 2/2 among those with available [O I] observations. Please rephrase the abstract and §6 summary to distinguish measured detections from inferences, or provide additional [O I] data.
  3. [§4.6, Fig. 12] The statement that the accretion-rate trend is not sensitivity-limited is based on comparing each source's total line SNR to the minimum SNR among classified detections. However, a source with high total SNR can still fail the extended-morphology criterion if the line is centrally concentrated, and the detection threshold shown in the figure is not an empirically calibrated completeness limit. A formal injection-recovery test (or a per-line SNR comparison between wind and non-wind sources at fixed accretion rate) is needed to exclude a sensitivity origin for the rising detection fraction with accretion. This is the key quantitative evidence for the 'outflow detection increases with accretion' conclusion.
minor comments (4)
  1. [§3.3] The [O I] comparison is based on only 26/72 stars ('about 36%'). The conclusion that low accretors show only [O I]/[Ne II] winds and lack H2 winds rests on a small subset; selection effects in which stars have [O I] spectroscopy should be discussed more explicitly.
  2. [Appendix figures] The 'jet-like bulk velocity' category (|vc|>30 km/s but no jet-like velocity map) is operationally reasonable, but these 7 sources are counted as jets even though they are not spatially resolved as jets. A sentence clarifying how these differ from 'marginally resolved [Ne II] winds' in terms of observable consequences would help.
  3. [§3.2] The atlas of maps in Figures 5–6 and 13 is a major resource, but the captions are dense and the orientation cue ('direction of North can be inferred from Fig. 13') is indirect. Adding explicit N/E arrows and scale bars to each montage, or at least to the first row of each page, would improve usability.
  4. [Table 3] The paragraph on the 60° wider-angle run lists newly detected winds in S(3)/S(5) but does not state whether those sources are included in the final 46-wind census. Please clarify to avoid ambiguity in Table 3 and Figures 7–8.

Circularity Check

0 steps flagged

No significant circularity: outflow classifications and accretion correlations are independently measured, with self-citations serving only as testable priors.

full rationale

The paper's derivation chain is observational rather than definitional: continuum-subtracted line maps are compared against PSF stars to identify extended emission; H2 winds are classified by the LR>CR test inside a 100° cone, and [Ne II] jets by velocity maps and a 30 km/s threshold; these classifications are then correlated with literature values of mass accretion rate, stellar mass, and inclination. No parameter is fitted to the outcome variable being 'predicted.' The adopted thresholds (30 km/s, 100° cone) come from prior published work, including Pascucci et al. (2025) with partially overlapping authors, but this is not load-bearing in a circular way: the analysis is repeated with a wider 60° semi-opening angle without changing the central conclusions, and the classification results are cross-checked against external [O I] spectroscopy, ALMA disk orientations, and previous MIRI detections. The molecular-to-atomic evolutionary sequence is presented as an empirical correlation between outflow morphology and independently determined accretion rates, with the Pascucci et al. (2020) scenario framed as the hypothesis being tested, not as the evidence for the new detection fractions. The caveats the paper itself states—infall/wind morphological degeneracy, the assumption that the continuum is not wind-like, and bowl-like morphologies in FTTau and SYCha—concern measurement validity and potential false positives, not circular reasoning, because they do not reduce the evolutionary claim to its own inputs. No load-bearing step equates a fitted parameter with a prediction or derives the result from a self-citation chain.

Axiom & Free-Parameter Ledger

4 free parameters · 6 axioms · 0 invented entities

The central numbers (46 H2 winds, 40 [Ne II] jets, detection-fraction trends) rest on a classification framework with hand-chosen thresholds (3σ detection, 100° wind apex, 30 km/s jet boundary, LR>CR rule) adopted from published values or chosen by the authors, plus domain assumptions that cone-shaped H2 emission traces winds, that the continuum is not wind-contaminated, that literature inclinations/radial velocities are accurate, and that accretion rate proxies evolutionary stage. No new physical entities are posited.

free parameters (4)
  • Wind-search vertex angle (semi-opening) = 50° (widened to 60° in re-run)
    §3.2: winds are searched within opposite 100°-apex triangles (twice the largest published semi-opening angle); re-running at 60° semi-opening added 5 wind detections (LkCa15, CXTau, WXCha, J16230544-2302566, HVTauC), so the 46-wind tally depends on this hand-chosen aperture.
  • Per-spaxel line detection threshold = 3σ amplitude vs local noise
    §2.3: pixels below 3σ are set to 3σ upper limits; this threshold determines which pixels feed the extended-emission curves, velocity maps, and classification inputs.
  • Jet/wind velocity boundary = 30 km/s (deprojected)
    §3.3: |vc| ≥ 30 km/s separates 'jet-like' from 'not jet-like' [Ne II]; threshold adopted from Simon et al. (2016), and it defines the boundaries of the three categories in Figures 6 and 7.
  • Extended-emission χ² threshold = mean + 3σ of PSF-to-PSF χ²
    §3.1: a line map is 'extended' if its encircled-flux χ² versus the main PSF exceeds PSF-to-PSF scatter plus 3σ; the convex-curve rescaling step (5th–99.5th percentile clip) adds a second, partly subjective decision.
axioms (6)
  • domain assumption Conical H2 emission perpendicular to the disk PA traces a disk wind
    §3.2: the wind classification assumes cone-like morphologies with the vertex at the continuum centroid are outflows; the infall degeneracy is acknowledged but dismissed as rare for Class II disks that have lost the natal envelope.
  • ad hoc to paper The continuum emission near each line is not wind-like, so the continuum ratio CR is a valid baseline
    Explicit in §3.2: 'this comparison inherently assumes the continuum itself is not morphologically wind-like'; justified by grain-decoupling theory, not by the data themselves.
  • domain assumption PSF stars HD159222, delta UMi, and 16 Cyg B represent the MIRI PSF at all target wavelengths and exposure depths
    §3.1: extended-emission classification compares encircled-flux curves against these five observations; PSF mismatch would misclassify compact and extended sources.
  • domain assumption Literature disk inclinations, position angles, and radial velocities (or region averages) are accurate enough for deprojection
    §3.3: velocities are corrected and deprojected using literature inclinations and RVs; where RVs are missing, region averages (e.g., +18 km/s for Taurus) are used, introducing ~3 km/s scatter that can affect marginal jet/wind categorization.
  • domain assumption Mass accretion rate from the literature is a valid proxy for disk evolutionary stage
    §2.1: 'serv[e] as proxies for disks at earlier and later evolutionary stages (e.g., Fang et al. 2023)'; the entire molecular-to-atomic 'evolution' reading depends on this monotonicity.
  • domain assumption H2 S(1)/S(3)/S(5)/S(7) relative detections trace wind temperature and launch radius ('hotter, likely inner' versus 'colder' winds)
    §5.2(ii): the excitation-temperature ladder (Eup ~1000 K, 4500 K, 7200 K) is used to infer weakening of the inner molecular wind; S(7) as a hot inner-wind tracer is asserted against Narang et al. (2026a).

pith-pipeline@v1.3.0-alltime-deepseek · 82306 in / 19119 out tokens · 173587 ms · 2026-08-01T06:52:28.476346+00:00 · methodology

0 comments
read the original abstract

The evolution and dispersal of protoplanetary disks--governed by accretion, magnetically launched jets and winds, and photoevaporative winds--fundamentally shape planetary systems. Determining how these mass-loss processes co-evolve is crucial for constraining planet formation pathways. We analyze archival JWST/MIRI/IFU data of 72 inclined (i>40deg) mostly ClassII disks to identify and characterize spatially resolved jets and winds, focusing on [NeII] and H2 lines. Extended emission in H2 S(1), S(3), S(5), S(7) and/or [NeII] is detected toward 66 disks, revealing diverse morphologies. We develop a framework to identify conical H2 winds and high-velocity [NeII] jets perpendicular to the disk, detecting them toward 46 and 40 disks, respectively. All sources with [NeII] jets exhibit a corresponding wind traced in either H2 (85%) or [OI], establishing a connection between jets and winds. The detection fractions of [NeII]-jets and H2-winds correlate positively with mass accretion rate, with no dependence on disk inclination or stellar mass. Conversely, marginally resolved low-velocity [NeII] winds are found preferentially toward lower accretors. Among sources with H2 winds, detection of hotter winds traced by S(7) and S(5) declines more rapidly with decreasing accretion rate than the colder S(1) component. Comparison with high-resolution [OI]6300\text{\AA} spectroscopy reveals [OI] LVC and extended H2 wind detections preferentially toward moderate-to-high accretors (>~10^{-8.5}~Msun/yr), whereas lower accretors exhibit only [OI] and [NeII] winds. Together, these results indicate that atomic jets and atomic+molecular winds, consistent with an MHD disk-wind origin, dominate during early, actively accreting disk phases, while at lower accretion rates, jets weaken and winds become predominantly atomic.

Figures

Figures reproduced from arXiv: 2607.21733 by Andrew D. Sellek, Gabriele Cugno, Gregory J. Herczeg, Ilaria Pascucci, Joan R. Najita, Ke Zhang, Naman S. Bajaj, Richard Alexander, Sophie C. Clark, Suzan Edwards, Sylvie Cabrit, Tracy L. Beck, Uma Gorti.

Figure 1
Figure 1. Figure 1: Histograms showing distribution of various prop￾erties for our sample of inclined (40◦ – 90◦ ) disks. 5 of the 10 highly inclined disks (≥80◦ ) lack information on accretion rate. emission at low disk inclinations, i.e., it is hard to spa￾tially separate the two components, we restrict our anal￾ysis to disks with inclinations > 40◦ ( [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Examples of the methodology employed to identify spatially extended emission with respect to the MIRI PSF. On top are the spaxel-by-spaxel continuum-subtracted intensity-integrated maps of the mentioned lines, where the blue stars represent the centroids of the corresponding continuum. For GY92-21, two maps are shown, one before rescaling the emission and one after (see Section 3.1 for details). On the bot… view at source ↗
Figure 3
Figure 3. Figure 3: This flowchart outlines our strategy to identify wind-like H2 emission as described in Section 3.2. Only line maps that appear spatially resolved relative to the PSF in the flux curves (see [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: H2 S(3) line intensity and continuum maps for FTTau (incl = 40.5◦ ) and SYCha (incl = 51.1◦ ). The blue stars show the continuum centroid, and the red dashed line shows the known disk position angle from literature ALMA results ( [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Intensity maps for sources with H2 winds with the red star highlighting the corresponding continuum centroid location (for incl>80◦ disks, the centroid is shifted to roughly the center of the dark lane visible in continuum or line map), and white line showing the disk PA where available ( [PITH_FULL_IMAGE:figures/full_fig_p012_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: [Ne II] velocity maps for sources with spatially extended [Ne II] emission. In each of the three categories, the sources are ordered by increasing disk inclination (read from left to right and top to bottom). The velocities (in each pixel and vC ) are corrected for stellar radial velocity and disk inclination. Only pixels with flux greater than 2σ are shown, where σ is the standard deviation of the backgro… view at source ↗
Figure 7
Figure 7. Figure 7: Figure summarizing which of the five analyzed spectral lines are detected, spatially extended, and exhibit outflow-like signatures. For example, when H2 S(1) is detected toward a given source, the corresponding block is highlighted in red; when it is not detected, the block is shown in gray. For [Ne II] jet classification, the additional lighter shade of green highlights the cases showing ‘Extended emissio… view at source ↗
Figure 8
Figure 8. Figure 8: Histogram of mass accretion rates for sources with extended H2 winds detected in S(1) (blue), S(5) (orange), and S(7) (red). Multiple-star systems are excluded, and so are several highly-inclined disks (i > 80◦ ) lacking reliable accretion rate measurements ( [PITH_FULL_IMAGE:figures/full_fig_p017_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The top panel shows the histogram of sources exhibiting the detections listed in the legend, with the full sample of sources with literature disk inclination measure￾ments shown in gray. The middle panel shows the corre￾sponding outflow detection fractions in each inclination bin, with uncertainties estimated using the method described in Section F. The points are plotted with a small offset in x-axis from… view at source ↗
Figure 10
Figure 10. Figure 10: Similar to [PITH_FULL_IMAGE:figures/full_fig_p019_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Similar to [PITH_FULL_IMAGE:figures/full_fig_p020_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Left panels: Stellar mass versus mass accretion rate for sources with wind detections in both H2 and [O I], or just [O I] and jet detections in both [Ne II] and [O I], or just [O I]. The color of each point, along with the adjacent histograms, corresponds to the categories listed in the legend. Right panels: Histograms of the mass accretion rates for the same source categories shown in the left panels. Kn… view at source ↗
Figure 13
Figure 13. Figure 13: Caption provided at the end [PITH_FULL_IMAGE:figures/full_fig_p027_13.png] view at source ↗
Figure 13
Figure 13. Figure 13: (continued) [PITH_FULL_IMAGE:figures/full_fig_p028_13.png] view at source ↗
Figure 13
Figure 13. Figure 13: (continued) [PITH_FULL_IMAGE:figures/full_fig_p029_13.png] view at source ↗
Figure 13
Figure 13. Figure 13: (continued) [PITH_FULL_IMAGE:figures/full_fig_p030_13.png] view at source ↗
Figure 13
Figure 13. Figure 13: (continued) [PITH_FULL_IMAGE:figures/full_fig_p031_13.png] view at source ↗
Figure 13
Figure 13. Figure 13: (continued) [PITH_FULL_IMAGE:figures/full_fig_p032_13.png] view at source ↗
Figure 13
Figure 13. Figure 13: Continuum-subtracted and line-integrated intensity maps of H2 S(1), S(3), S(5), and [Ne II] lines are shown along with nearby continuum slices overlaid with line contours. All maps are displayed using an asinh normalization with a maximum percentile cut of 97.5. For maps with peak values below 35×σ, a linear normalization with a maximum percentile cut of 97 is used instead. An example of this latter case … view at source ↗
Figure 13
Figure 13. Figure 13: Integrated intensity maps of the H2 S(7) line for sources with detected S(7) emission. The maps are displayed in the same manner as above [PITH_FULL_IMAGE:figures/full_fig_p034_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: [Ne II] spectrum for sources with extended [Ne II] emission plotted in the units of velocity (km s−1 ). The sources are arranged the same way as in [PITH_FULL_IMAGE:figures/full_fig_p035_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: The left column shows the pixel-by-pixel line-integrated H2 S(5) intensity map, with the 5σ contour overlaid in cyan, where σ is the background standard deviation calculated iteratively. The middle column presents a continuum slice near the S(5) line wavelength for the respective targets. The right column displays the full width at half maximum of the 1D Gaussian fitted at each pixel during the constructi… view at source ↗

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