IPA: Morphology and Kinematics of Molecular Hydrogen Winds in Five Young Protostars across the Mass Spectrum Observed with JWST

Alessio Caratti o Garatti; Amelia M. Stutz; Bihan Banerjee; B. Shridharan; Dan M. Watson; David A. Neufeld; Ewine F. van Dishoeck; Guillem Anglada; Henrik Beuther; Himanshu Tyagi

REVIEW 4 major objections 4 minor 296 references

IPA: Morphology and Kinematics of Molecular Hydrogen Winds in Five Young Protostars across the Mass Spectrum Observed with JWST

T0 review · 4 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read JWST observations of five young protostars reveal that their molecular hydrogen winds are layered like an onion, with faster, narrower gas inside and slower, wider gas outside.

desk verdict Valuable JWST morphology sample with solid nested-outflow geometry; the velocity-stratification and Lbol trends need a sensitivity analysis on the mean-zero calibration subtraction before they can be used. read the letter →

arxiv 2608.09920 v1 pith:U6RUBMLK submitted 2026-08-10 astro-ph.SR astro-ph.EPastro-ph.GA

Himanshu Tyagi , P. Manoj , Mayank Narang , S. Thomas Megeath , Robert Gutermuth , Lee Hartmann , Alessio Caratti o Garatti , Dan M. Watson

show 24 more authors

David A. Neufeld Ewine F. Van Dishoeck Neal J. Evans II Vinod Chandra Pathak Samuel A. Federman Tyler L. Bourke Yao-Lun Yang Guillem Anglada Henrik Beuther Leslie W. Looney Rolf Kuiper Pamela Klaassen Pooneh Nazari Bihan Banerjee Joel Green Sujay Vijay Jadhav Mayra Osorio B. Shridharan Amelia M. Stutz Thomas Stanke John J. Tobin Lukasz Tychoniec Scott Wolk Manya Arora

This is my paper · ORCID

classification astro-ph.SRastro-ph.EPastro-ph.GA

keywords protostarsmolecularhydrogenwindsMHDdiskJWSTNIRSpec/MIRIoutflowkinematicsstarformationH2purerotationallinesprotostellarjets

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 reports that the molecular hydrogen (H$_2$) winds around five young protostars, spanning bolometric luminosities from $0.16$ to $10^4\,L_\odot$, are not uniform flows but stratified, nested structures. Lines emitted by higher-excitation gas (higher upper-state energy $E_{\rm up}/k$) appear more collimated in space and move faster along the line of sight than lines from lower-excitation gas. The authors argue this nested morphology and kinematics match the predictions of magnetohydrodynamic (MHD) disk winds, in which gas is launched over a range of disk radii with inner streamlines being faster and narrower. They also find that wind velocity scales with the host protostar's bolometric luminosity, and report a tentative rotational signature in the lowest-luminosity source consistent with a launch radius of roughly $4\,\mathrm{au}$. If confirmed, a common disk-wind launching mechanism would operate across a factor of about $10^5$ in luminosity.

What carries the argument

The load-bearing observable is the ladder of H$_2$ pure-rotational lines, from S(1) up to S(18), observed with NIRSpec/IFU and MIRI/MRS, because each line's upper-state energy $E_{\rm up}/k$ selects a different temperature regime and therefore acts as a tracer of a different shell of the wind. Edge detection on three representative line maps (S(11), S(5), and S(1)) quantifies the opening angle of each shell, while Gaussian centroiding of position-velocity diagrams measured with MIRI/MRS provides the line-of-sight velocities. The analysis removes the unknown MIRI absolute wavelength offset by subtracting the mean velocity of all spaxels in each line, under the assumption that the blue- and red-shifted lobes are symmetric.

What would settle it

Measure the S(7), S(5), S(2), and S(1) velocity centroids using an independent absolute velocity reference, such as telluric or atmospheric lines or the ALMA disk systemic velocity, and test whether the higher-$E_{\rm up}$ lines are still faster. If the apparent velocity stratification vanishes or reverses, the gradient is an artifact of the mean-velocity subtraction.

Watch

Extended reading notes

Core claim

The central claim is that H$_2$ winds in protostars display a stratified, nested structure in both morphology and kinematics, and that this structure is consistent with MHD disk winds. In every source, higher-excitation H$_2$ lines (e.g., S(7), with $E_{\rm up}/k\approx 7200\,\mathrm{K}$) trace narrower flows while lower-excitation lines (S(1), with $E_{\rm up}/k\approx 1000\,\mathrm{K}$) open into wide cones; kinematically, the high-excitation lines reach the largest radial velocities after inclination correction. The authors interpret this as a single disk wind launched over a range of radii, with higher-excitation gas tracing inner, faster streamlines. They further claim that the flow velocity increases with the bolometric luminosity of the system, that in four of five protostars H$_2$ fills the outflow cavity rather than concentrating in limb-brightened walls, and that a steady transverse velocity gradient in IRAS 16253 tentatively indicates wind rotation with a launch radius of about $4\,\mathrm{au}$ and a magnetic lever arm of $5$--$10$. They also report a collimated, high-velocity H$_2$ jet in HOPS 370 which, together with its high accretion rate, suggests that the presence of molecular jets tracks accretion rate rather than system youth.

Load-bearing premise

All velocity comparisons assume that the mean velocity of all spaxels in a line equals the protostar's true rest velocity, so subtracting it removes the MIRI wavelength-calibration offset; if one lobe is brighter or more extended than the other, the zero point shifts and can fake a velocity--$E_{\rm up}$ gradient.

Editorial extensions

If this is right

In all five protostars, higher-$E_{\rm up}$ H$_2$ lines are narrower and faster, so the nested wind pattern appears to be a general feature of early star formation rather than a peculiarity of one mass.
The wind velocity scaling with $L_{\rm bol}$ implies that more luminous protostars drive faster outflows, linking disk-wind launching to the accretion power of the system.
The finding that H$_2$ fills the outflow cavity without limb brightening in four of five sources shifts the standard picture: much of the H$_2$ emission is shocked material inside the wind, not just cavity-wall shocks.
The tentative rotation signal in IRAS 16253, if real, places the H$_2$ wind launch around $4\,\mathrm{au}$ with a magnetic lever arm of $5$--$10$, matching MHD disk-wind predictions and providing a direct handle on angular-momentum removal.
The collimated molecular jet in HOPS 370, a source older than HH 211 but accreting rapidly, suggests that molecular jets are governed by accretion/ejection rate rather than by protostellar age alone.

Reading between the lines

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

If the $L_{\rm bol}$--velocity trend holds beyond five sources, outflow velocity could become a rough accretion-rate diagnostic for embedded protostars, complementing luminosity-based estimates.
The uniform detection of nested structure in this sample suggests that sources like Ced 110 IRS 4, which lack it, may be viewed at special geometries or may have different magnetic field configurations; this is an extension, not a paper claim.
The tentative rotation in IRAS 16253 could be tested at higher spectral resolution with ALMA or with JWST's higher-resolution gratings; a confirmed measurement of the ~4 au launch radius would directly constrain disk-wind angular momentum transport.
A larger sample that separates inclination effects from intrinsic opening angles is needed to test whether the measured $8^\circ$--$40^\circ$ half-opening angles are truly luminosity-independent or biased by the $1/\cos i$ correction.

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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. First, the morphology half of this paper is in good shape: five protostars spanning 0.16 to 1e4 Lsun, uniform H2 line maps, opening angles measured with a documented edge-detection and beam-deconvolution scheme, and a clear statement that the H2 fills the cavity rather than limb-brightened walls in most sources. Second, the kinematic half is less solid than the abstract suggests. The S(7)>S(5)>S(2)>S(1) velocity ordering and the velocity-Lbol trend both depend on subtracting the mean velocity of each line to remove MIRI absolute calibration offsets. The inter-sub-band offsets are 10–20 km/s, comparable to the line-to-line differences they are trying to measure, and the different H2 lines have different brightness distributions (S(1)/S(2) include foreground cavity-filling gas; S(7)/S(5) are narrower and one-sided). A per-line zero-point shift of even a few km/s, amplified by 1/cos(i) of 3.7–7.2, can create or erase the claimed stratification. The paper acknowledges the assumption but does not bound the bias. That is the load-bearing issue. What is genuinely new: the uniform multi-source comparison across four orders of magnitude in Lbol, the quantitative opening-angle measurements, and the tentative IRAS 16253 rotation signature with launch radius and lever arm. The rotation detection is handled carefully: Monte Carlo Spearman tests, and the gradient direction agrees with ALMA disk rotation. That part is less affected by the mean-zero subtraction because a constant shift does not create a transverse gradient; the bigger risk there is the 80 km/s MRS resolution, which they flag. Worth noting: B335 is the exception in the velocity stratification, and the velocity-Lbol correlation is marginal (p ~0.05–0.07 with 5 points, heavily influenced by IRAS 20126). The paper states a constant trend while its own data show one outlier. Inclination uncertainties are not propagated into Table 4 velocities; B335 has published inclinations from 57 to 87 degrees, so the adopted 68 is not secure. Who is this for: anyone working on protostellar outflows and MHD disk wind diagnostics. The maps and opening angles are a useful reference dataset. The kinematic claims need referee scrutiny. I would send it to review, not desk reject; a referee should require a sensitivity analysis on the mean-zero assumption and a more honest treatment of B335 and the inclination errors.

Referee Report

4 major / 4 minor

Summary. The manuscript presents NIRSpec/IFU and MIRI/MRS observations of H2 emission in five Class 0/I protostars spanning Lbol = 0.16 to 10^4 Lsun. It reports a rich inventory of pure-rotational and ro-vibrational H2 lines, bipolar winds that fill the scattered-light cavities, a nested morphology and kinematics in which higher-Eup lines are more collimated and faster, a possible Lbol–velocity scaling, a tentative wind-rotation detection in IRAS 16253 with an inferred launch radius of ~4 au and magnetic lever arm 5–10, and a collimated molecular jet in HOPS 370. The authors interpret the nested structure as observational support for MHD disk-wind launching.

Significance. If the kinematic stratification and rotation signatures hold, this is an important observational step: it would indicate a common disk-wind mechanism across five orders of magnitude in luminosity and would provide a quantitative launch-radius constraint from warm H2. The direct morphological maps, line inventories, and the uniform analysis across the sample are strengths, and the paper is careful to label the rotation and the disk-wind interpretation as tentative and to discuss alternative explanations. The public data availability statement is a further strength. However, the kinematic stratification, which is the central claim, rests on a mean-zero calibration assumption whose bias is unquantified and is comparable in magnitude to the measured line-to-line velocity differences.

major comments (4)

[Sections 5.1 and 5.2] The central kinematic claim that S(7)/S(5) are faster than S(2)/S(1) rests on subtracting each line's flux-weighted mean velocity from all spaxels, assuming that the blue- and red-shifted lobes are symmetric in flux and extent. The paper states that inter-sub-band offsets are ~10–20 km/s, comparable to the measured S(7)–S(1) velocity differences (e.g., 16 km/s for IRAS 16253 in Table 4), and the subsequent 1/cos(i) correction amplifies any residual zero-point error by factors of roughly 3.7–7.2. Because S(1)/S(2) include extended and foreground cavity emission while S(7)/S(5) are narrower and often one-sided, the flux-weighted mean of each line will be shifted by different amounts if the lobes are not exactly symmetric. I request an explicit sensitivity analysis, for example recomputing the velocities after weighting by observed blue/red flux ratios or using ALMA systemic velocities where available, to demonstrate that the reported S(7) > S(5) > S(2) > S(1) ordering is not an artifact of this zero-point choice.
[Figure 9 and Table 4] The claimed Lbol–velocity scaling is based on only five points, with Pearson r = 0.85 and p = 0.07 for the peak-to-peak S(7) velocities, and the trend is not monotonic: B335 has v_S(7) = 68 ± 5 km/s at Lbol = 1.4 Lsun while HOPS 153 has v_S(7) = 43 ± 7 km/s at Lbol = 3.8 Lsun. The velocities are further sensitive to adopted inclination angles, which are themselves uncertain (e.g., B335 has published inclinations spanning 68 to 87 degrees, changing the inferred velocity by about a factor of three). The abstract and conclusions present the scaling as a robust result; I recommend reframing it as a tentative trend, or adding an independent check with additional sources or published velocities.
[Section 3.6 and Table 3] The morphological nested claim is quantified through half-opening angles for S(11), S(5), and S(1), but several entries do not follow the claimed progression of increasing collimation with increasing Eup: B335 blue gives S(11) = 38 ± 2 deg and S(5) = 37 ± 1 deg, and HOPS 370 blue gives S(5) = 50 ± 1 deg versus S(1) = 46 ± 2 deg. Since the conclusion states that the emission becomes progressively more collimated with increasing excitation energy, please report the uncertainties from the edge-detection and linear-fitting steps and test the ordering statistically, or restrict the claim to the visually robust high-J versus low-J dichotomy.
[Section 6.3 and Figure 14] The inferred launch radius of ~4 au and magnetic lever arm of ~5–10 are derived under the assumption that the transverse velocity gradient in IRAS 16253 is rotation, and the quoted values are point estimates without propagation of the Monte Carlo uncertainties on the specific angular momentum or of the alternative cavity-wall-shock scenario. Because the paper already labels the rotation detection as tentative, I recommend presenting r0 and lambda_phi as ranges or illustrative values rather than best-fit point values, so that the uncertainty in the assumption is reflected in the quoted numbers.

minor comments (4)

[Abstract and Section 7] The abstract says H2 fills the cavity without pronounced limb brightening in 4 out of 5 protostars, while Section 6.1 identifies limb brightening only in IRAS 16253 and the red lobe of B335; the conclusion 'three of the eight cavities' is inconsistent with both statements and should be reconciled.
[Figure 8] The caption notes that the S(1) line in IRAS 20126 shows a sudden offset near zero due to bad pixels; it would be cleaner to exclude that spatial slice from the analysis and from the plotted centroid, or to mark it consistently in the figure so that it is not read as a kinematic feature.
[Section 2 and Table 1] The abstract and Section 2 quote Lbol = 0.2 Lsun for the lowest-luminosity source, while Table 1 lists 0.16 Lsun; please use one consistent value throughout.
[Table 2] Several transitions, including S(10) and S(9), are flagged with '!' but the flag is not explained in the table notes; please clarify whether 'blended/tentative' applies to all such entries and whether those lines are excluded from the kinematic analysis.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity; the central morphology/kinematics claims and the MHD disk-wind interpretation rest on independent JWST measurements and external model relations, with only minor reliance on prior IPA papers for calibration and reduction.

full rationale

The paper's central claims (nested H2 morphology, higher-E_up lines faster, velocity scaling with Lbol, possible rotation in IRAS 16253) are derived from direct JWST line maps, velocity maps, position-velocity diagrams, and edge-detection measurements. No fitted constant is renamed as a prediction: the per-line mean-velocity subtraction in Sections 5.1 and 5.2 is a calibration convention that removes unknown MIRI sub-band offsets, and it does not by construction force the S(7)>S(5)>S(2)>S(1) ordering, since the reported peak-to-peak and mean absolute velocities are computed from the residual spread of each line. The rotation analysis inverts published MHD disk-wind relations (Anderson et al. 2003; Ferreira et al. 2006) into a launch radius and lever arm; this is standard parameter inference, and the paper explicitly labels the rotation interpretation tentative and lists alternative explanations. The MHD disk-wind conclusion is presented as a consistency argument, not as a unique derivation, with the paper noting that X-wind and pure-jet models may also reproduce the nested structure. Self-citations (Federman et al. 2024, Narang et al. 2024, Narang et al. 2026b) are used for data reduction, calibration offsets, and prior description of IRAS 16253; these are methodological and contextual, not load-bearing for the new stratification claim. The calibration-symmetry assumption is a legitimate robustness concern but is not a circularity: it is an empirical systematic that could bias zero-points, and the paper does not quantify it, but this affects correctness risk rather than making the derivation equivalent to its inputs.

Assumptions & free parameters 0 free parameters · 5 assumptions · 0 invented entities

No free parameters were fit to the data in the classical sense; the opening angle fits are measurement summaries. The inferred launch radius and lever arm are inverted from external model relations, not free parameters. The main explicit assumption is the mean-zero velocity subtraction. No new physical entities are introduced.

assumptions (5)

domain assumption MHD disk wind model relations from Anderson et al. 2003 and Ferreira et al. 2006 connect specific angular momentum to launch radius and magnetic lever arm.
Used in Section 6.3 to convert the IRAS 16253 velocity gradient into r0 ~4 au and lambda ~5 to 10; if the wind is not an MHD disk wind, the inferred values do not apply.
domain assumption H2 line emission is optically thin and traces the bulk flow of the wind rather than unrelated stationary or shocked gas.
Underlies the use of line centroids as velocities and the interpretation of morphology as wind structure in Sections 3 and 5.
ad hoc to paper The mean velocity of all spaxels in a line equals the systemic velocity and the MIRI absolute calibration offset.
Explicitly assumed in Sections 5.1 and 5.2 to set velocity zero points; this is the weakest load-bearing premise for the kinematics.
domain assumption Adopted disk inclinations from the literature are correct.
Velocities are corrected by 1/cos(i) in Sections 5.1 and 5.2; for B335 the literature range is 57 to 87 degrees, which would change corrected velocities substantially.
domain assumption The 4.14 micron scattered-light continuum delineates the outflow cavity wall.
Used in Section 6.1 to conclude that H2 fills the cavity rather than being limb-brightened at the walls.

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Cite this review

Pith. "Pith review of IPA: Morphology and Kinematics of Molecular Hydrogen Winds in Five Young Protostars across the Mass Spectrum Observed with JWST." pith.science (2026). https://pith.science/paper/U6RUBMLK

@misc{pith2026260809920,
  author       = {Pith},
  title        = {Pith review of: IPA: Morphology and Kinematics of Molecular Hydrogen Winds in Five Young Protostars across the Mass Spectrum Observed with JWST},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/U6RUBMLK}},
  note         = {Machine review of arXiv:2608.09920}
}

abstract

Molecular winds may play a key role in governing angular momentum transport and accretion during the early evolution of protostars. We present the morphology and kinematic properties of the H$_2$ emission in five young, envelope-dominated, protostars across a broad bolometric luminosity range, from 0.2 to $10^4~L_{\odot}$, observed with the NIRSpec/IFU and MIRI/MRS onboard JWST as part of the Investigating Protostellar Accretion (IPA) program. A rich set of pure rotational lines of H$_2$, up to $v=0-0$ S(18), and a few ro-vibrational lines are detected in the winds, revealing bipolar structures. The H$_2$ lines show a stratified/onion-like structure morphologically and kinematically, where the lines with higher $E_{\rm up}$ show a higher degree of collimation and higher velocities. Additionally, the wind velocity scales with the $L_{\rm bol}$ of the host protostellar system. In 4 out of 5 protostars, H$_2$ emission fills the outflow cavity without showing pronounced limb brightening. We also report a tentative detection of H$_2$ wind rotation in IRAS 16253, which suggests a launch radius of $\sim4$ au and the magnetic lever arm parameter of $\sim5-10$. Taken together, these properties of the H$_2$ winds can be explained by the magnetohydrodynamic disk wind models. We detect a collimated, high-velocity H$_2$ jet toward HOPS 370, which is more evolved than the extremely young source HH 211, but is accreting at a high accretion rate. This suggests that the presence of collimated molecular jets in protostars is more closely connected to accretion rate than system age.

Figures

Figures reproduced from arXiv: 2608.09920 by the authors.

**Figure 1.** Line maps of the H2 v = 0 − 0 S(11), S(5), S(3), and S(1) transitions (labeled at the top of each panel) at 4.18, 6.91, 9.66, and 17.03 µm, respectively, for IRAS 16253, B335, HOPS 153, HOPS 370, and IRAS 20126 (rows a–e). The white star marks the ALMA 870 µm continuum position adopted from Tobin et al. (2020a). The golden circles outlined in red at the lower left of each panel indicate the JWST beam size, and the d… view at source ↗

**Figure 2.** Line map of the H2 v = 1–0 O(7) transition at 3.81 µm. The color scheme and annotation conventions are the same as in [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗

**Figure 3.** H2 v = 0 − 0 S(11) contours (lime) and [Fe II] 17.9 µm contours (cyan) overplotted on the NIRCam F444W image of B335. The NIRCam image is taken from GTO program 1187 (P.I.: Hodapp, K. W.). The white arrows mark the location of shocks 4E and 3E as labeled by Hodapp et al. 2024. White star marks the ALMA 870 µm continuum position in 2023 (Kim, C. et al. in prep.). H2 lines. The northwestern cavity is also broader than… view at source ↗

Figures from the paper (14 more)

**Figure 4.** Figure 4: Example of edge detection in IRAS 16253. The color scale depicts the rotated line maps of H2 v = 0 − 0 S(11), S(5), and S(1) lines (left to right). The lime crosses mark the edges of the H2 emission. The magenta star marks the ALMA 870 µm peak. the emission due to JWST…

**Figure 5.** Figure 5: Deconvolved half-width of the outflow vs distance from the protostellar disk plane of IRAS 16253. The red, green, and blue dots show the measured half-widths as a function of distance for H2 v = 0 − 0 S(1), S(5), and S(11), respectively. The gray dotted vertical line m…

**Figure 6.** Figure 6: Spectra from the apertures outside the outflow cavities. left: H2 v = 0−0 S(11) line map depicting the H2 emission. All spaxels with S/N ≤ 3 are masked. The cyan and magenta circles mark the apertures used to extract the spectrum. The black dot marks the ALMA 870 µm co…

**Figure 7.** Figure 7: Inclination-corrected velocity maps of H2 v = 0 − 0 S(7), S(5), and S(2) lines for IRAS 16253, B335, HOPS 153, HOPS 370, and IRAS 20126. The white star marks the ALMA continuum peak. Golden circles, outlined in red, at the bottom left edge mark the beam size of JWST. T…

**Figure 8.** Figure 8: Top row: Sky paths of the PV diagrams overlaid in green on H2 v = 0−0 S(7) line maps. White lines show 1-pixel-wide slices used to find the velocity centroids. Bottom row: Inclination-corrected centroids of PV diagrams of H2 v = 0−0 S(7), S(5), S(2), and S(1) lines alo…

**Figure 9.** Figure 9: Velocity measured from PV diagrams along the outflow axis as a function of Lbol. Left: Peak-to-peak velocities of the H2 v = 0 − 0 S(7), S(5), S(2), and S(1) lines are indicated by blue circles, orange squares, green triangles, and red diamonds, respectively. Right: …

**Figure 10.** Figure 10: Velocity centroids of PV diagrams of the H2 v = 0 − 0 S(7) and S(5) lines (in blue and orange, respectively) for the sky paths orthogonal to the outflow axes. Each row corresponds to a specific protostar, as labeled in the sub-caption below each row. The selected sky …

**Figure 10.** Figure 10: (b) presents the PV diagrams orthogonal to the outflow axis for B335. None of the PV diagrams for B335 show evidence of wind rotation, as indicated by the absence of steady velocity gradients. The green and red [PITH_FULL_IMAGE:figures/full_fig_p019_10.png]

**Figure 11.** Figure 11: Distributions of the Spearman’s rank correlation coefficients (ρ) to test the steady gradient in IRAS 16253. The top two panels show the ρ distributions for the H2 v = 0 − 0 S(7) and S(5) lines in the blue-shifted lobe (marked by the green region in Figure 10a. The b…

**Figure 12.** Figure 12: Comparison of the extent of the scattered light at 4.14 µm and the H2 v = 0 − 0 S(11) line at 4.18µm. The lime-colored contour (9× local rms of the scattered-light image) traces the outer edge of the scattered-light emission, overplotted on the respective line images.…

**Figure 13.** Figure 13: Comparison between the simulated toy outflow cavity and the observed H2 emission. Top row: Morphological comparison of the outflow. The first two panels show the projected density from the simulated cavity model, while the panel(s) to the right show the observed emiss…

**Figure 14.** Figure 14: shows that the observed velocity gradients are consistent with a H2 wind launching footprint at radii of ∼ 4 au, with inferred magnetic lever-arm parameters λϕ in the range ∼ 5–10. The λϕ value of 5 to 10, 10 1 10 2 q v 2 Á + v 2 pol(M¯=M ) 0:5 [km s¡1 ] 10 2 10 3 r …

**Figure 15.** Figure 15: Inclination corrected velocity map of H2 v = 0−0 S(11) line toward HOPS 370. Spaxels with S/N below 5σ are masked. Caution: The velocities of the ambient H2 emission appear artificially large because the observed line-of-sight velocities are corrected by a factor of …

**Figure 16.** Figure 16: Molecular jet in various species detected in HOPS 370. (a) H2 v = 0 − 0 S(11) line map. Mean line images of CO 1-0 lines from P(38) to P(51), OH pure rotational lines from 9.2 µm to 10.07 µm, and H2O ro-vibrational lines from 6.11 µm to 6.43 µm are shown in panels (b)…

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Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.

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