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arxiv: 2606.08607 · v1 · pith:VHRDIGJTnew · submitted 2026-06-07 · 🌌 astro-ph.GA · astro-ph.SR

ALMA High-resolution Observation of the HH46/47 Outflow/disk/envelope System

Heyi Zhang , Yichen Zhang , H\'ector G. Arce , Diego Mardones , Sylvie Cabrit , Michael M. Dunham , Stella S. R. Offner , Hsien Shang This is my paper

Pith reviewed 2026-06-27 18:13 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords HH 46/47molecular outflowALMA observationsprotostellar envelopedisk transitionentrainmentoutflow kinematicscircumbinary disk
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The pith

ALMA observations of HH 46/47 show a rotating infalling envelope becoming a disk at 30 au, with the outflow shell expanding radially to support entrainment over a disk wind.

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

High-resolution ALMA data map the envelope, disk, and outflow around the HH 46/47 protostar at scales down to 50 au. The structures fit a model of material falling inward while rotating, transitioning to a disk at about 30 au around a central object of 0.3 solar masses. Analysis of a well-defined redshifted shell in the outflow reveals that it expands outward in all directions rather than flowing along the shell surface. A sideways velocity change across the shell cannot be explained as rotation without invoking an unrealistic magnetic lever arm, which instead favors the shell material being swept up by the central jet.

Core claim

The observations are well reproduced by a rotating-infalling envelope transitioning to an inner disk at a radius of ~30 au around a 0.3 Msun protostar. The 12CO emission, together with JWST NIRCam images, reveals multiple shell structures in the outflow. Using C18O and 13CO to correct for optical depth, the spatial distributions of outflow mass, momentum, and kinetic energy are derived. A model-independent analysis of a well-defined redshifted shell yields its three-dimensional velocity field, showing that the shell expands radially rather than flowing along its surface. Although a transverse velocity gradient is detected, interpreting it as rotation implies an unphysically large magnetic le

What carries the argument

Rotating-infalling envelope model transitioning to inner disk at 30 au, combined with model-independent three-dimensional velocity field reconstruction of the redshifted outflow shell

If this is right

  • The central protostar mass is 0.3 solar masses with the disk beginning at a radius of 30 au.
  • Outflow mass, momentum, and kinetic energy distributions, plus their time rates, are obtained after correcting for optical depth effects.
  • Multiple shell structures appear in the outflow when 12CO maps are combined with infrared imaging.
  • The shell kinematics are consistent with entrainment by the jet rather than a direct disk wind.

Where Pith is reading between the lines

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

  • The same radial-expansion test could be applied to shells in other protostellar outflows to distinguish entrainment from disk-wind origins.
  • The spur-like features and intensity minimum near the companion suggest that binary companions commonly reshape circumbinary disks through gravitational effects.
  • Joint ALMA and infrared datasets can separate the radial and rotational components of outflow motion more cleanly than either alone.

Load-bearing premise

That a rotation interpretation of the observed transverse velocity gradient would require an unphysically large magnetic lever arm and therefore must be rejected.

What would settle it

A measurement showing that the shell material moves primarily along the shell surface rather than radially outward would falsify the radial-expansion claim and reopen a possible disk-wind interpretation.

Figures

Figures reproduced from arXiv: 2606.08607 by Diego Mardones, H\'ector G. Arce, Heyi Zhang, Hsien Shang, Michael M. Dunham, Stella S. R. Offner, Sylvie Cabrit, Yichen Zhang.

Figure 1
Figure 1. Figure 1: (a): Low-resolution (C2+C4) 1.3 mm continuum image (Y. Zhang et al. 2019). Contours start at 5σ and increase by factors of 2 up to 1280σ. Here 1σ = 0.016 mJy beam−1 (0.8 K). (b): High-resolution (C2+C4+C7) 1.3 mm continuum image. Contours start at 5σ and increase by factors of 2 up to 2560σ, with 1σ = 0.009 mJy beam−1 (0.017 K). The black dashed line indicates the cut used for the position–velocity diagram… view at source ↗
Figure 2
Figure 2. Figure 2: Left column: Moment 0 maps of SO, H2CO, and CH3OH (contours) overlaid on the 1.3 mm continuum image (color scale). Black contour levels are [3σ, 5σ, 7σ, 14σ] for SO and H2CO, and [5σ, 7σ, 9σ, 14σ] for CH3OH, chosen to highlight both extended structures and emission peaks. The rms values are 1σ = 2.05 (SO), 1.27 (H2CO), and 1.05 (CH3OH) mJy beam−1 km s−1 . Middle: Moment 1 maps (color scale) of the three mo… view at source ↗
Figure 3
Figure 3. Figure 3: From left to right: moment 0, moment 1, and a zoomed-in moment 1 map of C18O. Green contours show the 1.3 mm continuum. The moment 0 map is integrated over [−1.8, 1.8] km s−1 relative to the systemic velocity. Dashed lines in the right panel mark the disk midplane and outflow axis ( [PITH_FULL_IMAGE:figures/full_fig_p020_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: 12CO integrated intensity maps of the HH 46/47 molecular outflow after primary beam correction. The min￾imum primary beam correction factor is 0.3. The red and blue color scales show 12CO emission integrated over velocity ranges of [+2, +52] km s−1 and [−35, −2] km s−1 , respectively. The green color scale shows C18O emission integrated over [−1.8, +1.8] km s−1 . All velocities are given relative to the sy… view at source ↗
Figure 5
Figure 5. Figure 5: Channel maps of the blueshifted 12CO outflow (contours) overlaid on the JWST NIRCam F200W image. The 12CO emission is after primary beam correction. The minimum primary beam response is set to be 0.3. Contour levels start at 5σ and increase in steps of 5σ up to 45σ (1σ = 0.6 mJy beam−1 ). Two shells structures Sb1, Sb2 identified in Y. Zhang et al. (2019) are labeled in vout = −27km s−1 and −24km s−1 chann… view at source ↗
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p023_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: (a): H2CO moment 0 map integrated over [−1.5, 1.5] km s−1 relative to the systemic velocity. The blue curves show the fitted projected shapes of the outflow cavities. This cavity is related to the blueshifted 12CO shell and redshifted outer 12CO shell in [PITH_FULL_IMAGE:figures/full_fig_p024_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Transverse position–velocity (PV) diagrams for (a) C18O, (b) SO, (c) C18O+SO combined, (d) CH3OH, (e) H2CO, and (f) all lines combined. The PV diagrams are extracted along a cut perpendicular to the outflow axis, passing through the source center, with a width of one synthesized beam (0.1 ′′; see [PITH_FULL_IMAGE:figures/full_fig_p025_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Upper: Channel maps at vout = +9, +22.8, and +38.7 km s−1 . The white dashed lines indicate the transverse PV cuts at δz = 0′′ , 2.5 ′′ , 5 ′′, and 7.5 ′′. The three shells (Sr1, Sr2, and Sr3) are labeled by arrows. Bottom: Transverse PV diagrams at δz = 2.5 ′′ , 5 ′′, and 7.5 ′′. The horizontal white dashed lines indicate the velocities corresponding to the channel maps shown in the upper panels [PITH_FU… view at source ↗
Figure 10
Figure 10. Figure 10: Three-dimensional schematic illustrating the coordinate systems and velocity components in the outflow shell. The (X, Y, Z) and (δx, δy, δz) coordinates define the outflow frame and the observer’s frame, respectively (see §4.2 for details). A gas parcel on the shell has three velocity components: the axial velocity Vz, radial velocity Vr, and rotational velocity Vϕ. A position–velocity (PV) cut taken perp… view at source ↗
Figure 11
Figure 11. Figure 11: Method for determining the axis position angle of the outflow shell Sr2. Upper-left: A typical transverse PV diagram assuming outflow axis P.A. = 57◦ at δz = 3.5 ′′. The white dashed line marks vout = 10km s−1 . Lower-left: Intensity profile integrated from the PV diagram for vout > 10 km s−1 . The red curves show Gaussian fits to the two edges of the intensity profile, and the red dashed lines mark the t… view at source ↗
Figure 12
Figure 12. Figure 12: Upper: Transverse PV diagram at δz = 5′′. Points A and B mark the velocities of the outflow shell Sr2 projected along the outflow axis. Lower: Ellipse fit to the outflow shell Sr2. The blue crosses indicate the selected data points used for the fit, and the white curve shows the best-fit ellipse. Points C and D mark the outermost points on the ellipse [PITH_FULL_IMAGE:figures/full_fig_p029_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Model-independent measurements of the morphology and velocity field of the outflow shell Sr2. (a): Radius of the Sr2 shell R as a function of height Z. The red curve shows the best-fit relation, Z ∝ R 3.6 . (b): Axial velocity Vz as a function of height Z. The red curve shows the best-fit relation. (c): Radial velocity Vr as a function of height Z, showing two sets of measurements derived from the upper a… view at source ↗
Figure 14
Figure 14. Figure 14: Projected poloidal velocities calculated from Vr and Vz for the Sr2 shell. The background image shows the 12CO moment 0 map integrated over [−33, 51] km s−1 . The yellow arrows represent the projected poloidal velocity vectors Vp at δz = 4′′ , 5 ′′ , 6 ′′ , 7 ′′ , 8 ′′, with Vr equals its average value of 13.5 km s−1 . The reference arrow in the lower-right corner corresponds to 30 km s−1 . The blue dashe… view at source ↗
Figure 15
Figure 15. Figure 15: (a): Rotation velocity Vϕ of the Sr2 shell as a function of height Z, assuming that the measured transverse velocity gradient arises from rotation. (b): Specific angular momentum, j = RVϕ, as a function of Z. (c): Derived disk-wind footpoint radius, r0, as a function of Z. (d): Derived magnetic lever arm, λϕ, as a function of Z [PITH_FULL_IMAGE:figures/full_fig_p032_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Upper: Surface density maps of outflow mass, momentum, and kinetic energy, including only pixels with intensities per channel > 4σ. Lower: Maps of the outflow mass, momentum, and kinetic energy rates,including only pixels with intensities per channel > 4σ. Both the upper and lower panels have been corrected for the primary beam response. The minimum primary beam correction factor is 0.3 [PITH_FULL_IMAGE:… view at source ↗
Figure 17
Figure 17. Figure 17: Mass–velocity relation of the HH 46/47 outflow. The outflow mass is calculated after primary beam correction. Only the area where the primary beam correction factor > 0.3 is included. The blue and red points represent the blueshifted and redshifted lobes, respectively. The blue and red dashed lines show the power-law fits to the mass spectra [PITH_FULL_IMAGE:figures/full_fig_p034_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Radial profiles of the outflow mass rate (panel a), momentum rate (panel b), and kinetic energy rate (panel c). The profile is after primary beam correction, and only the area where the primary beam correction factor > 0.3 is included [PITH_FULL_IMAGE:figures/full_fig_p035_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: From left to right: 1.3 mm continuum image (robust = −0.5), 2D Gaussian model, and residual map (data − model) [PITH_FULL_IMAGE:figures/full_fig_p036_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: JWST NIRCam F187N (1.87 µm) image of the binary system. The locations of sources A and B are marked with two circles. White contours show the 1.3 mm continuum emission (robust = −0.5). The yellow arrow indicates the direction of blueshifted [FeII] jet seen by JWST (B. Nisini et al. 2024; P.A. = 46◦ ). The black dashed line marks the outflow axis (P.A. = 57◦ ), derived in §4.2. Black ellipses denote the sy… view at source ↗
Figure 21
Figure 21. Figure 21: Distribution of the Toomre parameter Q. The pink, green, and blue contours denote Q = 3.5, 4, and 5, respectively. The black ellipse in the bottom-left corner indicates the synthesized beam of the 1.3 mm continuum (robust = −0.5). The two red crosses mark the locations of sources A and B. -1.00 -0.50 0.00 0.50 1.00 Offset ( ) -5.00 -4.00 -3.00 -2.00 -1.00 0.00 1.00 2.00 3.00 4.00 5.00 V (k m s 1) 0.5M Kep… view at source ↗
Figure 22
Figure 22. Figure 22: Transverse SO position–velocity (PV) diagram compared with Keplerian rotation curves. The green and red curves represent Keplerian rotation for central masses of 0.5 M⊙ and 0.1 M⊙, respectively [PITH_FULL_IMAGE:figures/full_fig_p038_22.png] view at source ↗
Figure 23
Figure 23. Figure 23: Left: average radiation temperature ratio TR,13(v)/TR,18(v) between 13CO and C18O in each velocity channel. The solid curve is the Gaussian fit to the ratio profile. The horizontal line marks the abundance ratio between 13CO and C18O of R13,18 = 8.7. Right: Similar to the left panel, but for the radiation temperature ratio between 12CO and 13CO where 13CO emission has been optical depth corrected [PITH_F… view at source ↗
read the original abstract

We present 0.1" (~ 50 au) resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations of the HH 46/47 molecular outflow and its envelope-disk system. The 1.3 mm continuum emission reveals a compact central source surrounded by a circumbinary disk with substructures. The companion, identified in optical and infrared observations, is not detected in the millimeter continuum but coincides with a local intensity minimum. Two spur-like features extending from the primary source toward the companion are identified and are likely induced by gravitational perturbations from the companion. The envelope-disk system is traced by C18O, SO, H2CO, and CH3OH. C18O primarily traces the extended envelope, while SO probes the inner envelope, and H2CO and CH3OH trace compact, faster-rotating structures near the centrifugal barrier. The observations are well reproduced by a rotating-infalling envelope transitioning to an inner disk at a radius of ~30 au around a 0.3 Msun protostar. The 12CO emission, together with JWST NIRCam images, reveals multiple shell structures in the outflow. Using C18O and 13CO to correct for optical depth, we derive the spatial distributions of outflow mass, momentum, and kinetic energy, as well as their corresponding rates. A model-independent analysis of a well-defined redshifted shell yields its three-dimensional velocity field, showing that the shell expands radially rather than flowing along its surface. Although a transverse velocity gradient is detected, interpreting it as rotation implies an unphysically large magnetic lever arm, disfavoring a direct disk-wind origin. Instead, the shell kinematics support an entrainment scenario.

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 presents 0.1-arcsec ALMA observations of the HH 46/47 outflow/disk/envelope system at 1.3 mm. The continuum reveals a central source with a circumbinary disk showing substructures and spur-like features attributed to the companion; C18O, SO, H2CO, and CH3OH trace the envelope, inner envelope, and compact structures near the centrifugal barrier. These data are reproduced by a rotating-infalling envelope model transitioning to a disk at ~30 au around a 0.3 Msun protostar. Optical-depth-corrected 12CO maps yield outflow mass, momentum, and energy distributions. A model-independent analysis of one well-defined redshifted shell shows radial expansion with a transverse velocity gradient; the authors interpret the latter as incompatible with rotation because it would require an unphysically large magnetic lever arm, thereby favoring entrainment over a direct disk wind.

Significance. If the kinematic conclusions are robust, the work supplies spatially resolved evidence that can discriminate between disk-wind and entrainment scenarios for molecular outflows, a central question in protostellar feedback. The high-resolution continuum substructures, multi-tracer line mapping, and direct 3D velocity-field reconstruction of the shell are concrete strengths. The simple envelope+disk model that reproduces the observed line emission is also a positive feature.

major comments (2)
  1. [Abstract and kinematics analysis] Abstract (final sentence) and the kinematics analysis section: the claim that interpreting the detected transverse velocity gradient as rotation 'implies an unphysically large magnetic lever arm' is presented without any explicit calculation of the lever arm (r_A/r_launch) from the measured shell velocities and radii, and without numerical comparison to literature ranges for disk winds. This judgment is load-bearing for the conclusion that the data disfavor a direct disk-wind origin.
  2. [Outflow mass/momentum section] Outflow mass/momentum section: the optical-depth corrections applied to 12CO using C18O and 13CO are described, yet the quantitative effect of those corrections on the derived mass, momentum, and kinetic-energy distributions (and on the corresponding rates) is not shown; this choice directly affects the reliability of the reported outflow properties.
minor comments (2)
  1. [Continuum results] The companion is stated to coincide with a local intensity minimum in the continuum; a quantitative upper limit on its millimeter flux (or a clear statement that none is detected above the noise) would strengthen the non-detection claim.
  2. [Envelope-disk model] Notation for the centrifugal barrier radius and the disk transition radius should be unified across text, figures, and the model description to avoid ambiguity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed review. The comments highlight areas where additional quantitative detail will strengthen the manuscript. We address each major comment below and will revise accordingly.

read point-by-point responses

  1. Referee: [Abstract and kinematics analysis] Abstract (final sentence) and the kinematics analysis section: the claim that interpreting the detected transverse velocity gradient as rotation 'implies an unphysically large magnetic lever arm' is presented without any explicit calculation of the lever arm (r_A/r_launch) from the measured shell velocities and radii, and without numerical comparison to literature ranges for disk winds. This judgment is load-bearing for the conclusion that the data disfavor a direct disk-wind origin.

    Authors: We agree that the current text presents the lever-arm conclusion without the supporting calculation. In the revised manuscript we will add an explicit computation of r_A/r_launch using the observed shell velocities and radii in the kinematics analysis section, together with a direct numerical comparison to the range of lever arms reported for disk-wind models in the literature. This addition will make the argument quantitative and transparent while preserving the model-independent nature of the shell analysis. revision: yes

  2. Referee: [Outflow mass/momentum section] Outflow mass/momentum section: the optical-depth corrections applied to 12CO using C18O and 13CO are described, yet the quantitative effect of those corrections on the derived mass, momentum, and kinetic-energy distributions (and on the corresponding rates) is not shown; this choice directly affects the reliability of the reported outflow properties.

    Authors: We acknowledge that the quantitative impact of the optical-depth corrections is not illustrated. In the revision we will add a direct comparison—either as supplementary panels or a table—showing the mass, momentum, and kinetic-energy distributions (and the corresponding rates) derived with and without the C18O/13CO corrections. This will allow readers to assess the magnitude of the correction and the robustness of the reported outflow properties. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper derives its key conclusions from direct ALMA observations of continuum and line emission, with explicit corrections for optical depth using C18O and 13CO to obtain mass, momentum, and energy distributions. The model-independent 3D velocity field of the redshifted shell is extracted from the data without reference to fitted parameters or prior self-citations, and the preference for entrainment over disk-wind follows from a physical-plausibility judgment on the transverse gradient rather than any equation that reduces to the paper's own inputs by construction. No self-definitional loops, fitted inputs renamed as predictions, or load-bearing self-citation chains appear in the provided text; the derivation remains self-contained against the external benchmark of the raw kinematic measurements.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Central claims rest on standard assumptions about molecular-line optical-depth corrections, LTE or non-LTE excitation, and the physical meaning of a 'magnetic lever arm'; the 0.3 Msun mass and 30 au transition radius are fitted to match the data.

free parameters (2)
  • central protostar mass = 0.3 Msun
    0.3 Msun value chosen so the rotating-infalling envelope model matches the observed line kinematics
  • centrifugal barrier / disk transition radius = ~30 au
    ~30 au radius where envelope transitions to disk, fitted to reproduce compact fast-rotating structures
axioms (2)
  • domain assumption C18O and 13CO can be used to correct 12CO for optical depth when deriving outflow mass, momentum and energy
    Invoked when deriving spatial distributions of outflow properties
  • domain assumption A transverse velocity gradient, if interpreted as rotation, maps directly to a magnetic lever arm whose magnitude can be judged 'unphysical'
    Used in the final sentence to disfavor disk-wind origin

pith-pipeline@v0.9.1-grok · 5883 in / 1674 out tokens · 30935 ms · 2026-06-27T18:13:45.615578+00:00 · methodology

discussion (0)

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