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Asymmetry in the protostellar system HOPS 198: Evidence for the evolution of outflow opening angle driven by density of the surrounding core

T0 review · 4 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read The paper claims that the density of the surrounding core, not the wind alone, sets the opening angle of a protostellar outflow: in HOPS 198 the ~80° eastern lobe and ~30° western lobe trace the 1.5–2.8× density contrast across the core.

desk verdict A genuinely interesting source with a plausible density-driven explanation for outflow asymmetry, but the quantitative bridge is overclaimed and needs a constant-ξ robustness test. read the letter →

arxiv 2608.04890 v1 pith:W5UQ6675 submitted 2026-08-05 astro-ph.SR

Donglin Wu , Héctor Arce , Cheng-Han Hsieh This is my paper
classification astro-ph.SR
keywords protostellaroutflowsoutflowopeninganglecoredensityHOPS198Class0protostarpressurebalanceALMAobservationsstarformationfeedback
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

HOPS 198, a Class 0 protostar in Orion A, has an outflow whose two lobes open at very different angles: about 80 degrees on the east and about 30 degrees on the west. The same system has a core whose west side carries 1.5–2.8 times more surface density than the east. The paper argues these two asymmetries are causally linked: the dense western core resists the protostellar wind more strongly, pinching the western cavity, while the thinner east lets the wind open a wide cavity. An analytical pressure-balance model, fit to the observed lobe shapes, infers a core-to-wind pressure ratio that is 2.9 times larger on the west, matching the measured density contrast once the winds on both sides are assumed symmetric. The paper concludes that ambient core density sets the molecular outflow opening angle, and that the well-known widening of outflow cavities from Class 0 to Class I protostars may be driven by the steady decline of core density.

What carries the argument

The carrier of the argument is the cavity-shape equation $\mathrm{d}z/\mathrm{d}r_\perp = \tan\!\left(\arctan(z/r_\perp)+\arcsin(p_{\rm core}/p_{\rm wind})\right)$, which balances the ram pressure of the protostellar wind against the turbulent pressure of the core perpendicular to the cavity wall. Re-expressed under the assumption that the pressure ratio $\xi = p_{\rm core}/p_{\rm wind}$ is constant along each lobe, it becomes the implicit curve $F(r_\perp,z)=\arctan(z/r_\perp)-\alpha\ln(r_\perp/r_0)-\frac{\alpha}{2}\ln\!\left(1+(z/r_\perp)^2\right)=0$, with $\alpha=\xi/\sqrt{1-\xi^2}$ and $r_0$ the base width. The paper fits this curve to the $^{12}$CO surface-density contours of each lobe, and converts the fitted $\xi$ difference into a density contrast using $\xi = \rho_{\rm core}\sigma_{\rm core}^2/(\rho_{\rm wind}v_{\rm wind}^2)$ together with the assumptions of symmetric winds and comparable velocity dispersion on both sides. The model requires the launched wind to be intrinsically wide, at least about 80°, so that the eastern cavity is near the wind's opening angle.

What would settle it

Measure the pressure ratio $\xi(r)$ directly along both lobes—e.g., with a protostellar wind tracer giving $\rho_{\rm wind}$ and $v_{\rm wind}$ plus a resolved core volume-density map giving $\rho_{\rm core}$ and $\sigma_{\rm core}$—and compare the inferred profile to the lobe shapes. If the west/east volume-density ratio is not close to the ~2.9 factor required by the fits, or if the shape equation with the measured $\xi(r)$ no longer reproduces the 80° versus 30° outlines, the density-driven explanation fails. A simpler observable check: an independent deprojection of the measured 1.5–2.8 surface-density asymmetry into volume density should land near the 2.9 pressure-ratio contrast; a value outside roughly 1.5–5 would contradict the quantitative claim.

Watch

Extended reading notes

Core claim

The central claim is that the density of the surrounding protostellar core determines the opening angle of the molecular outflow. In HOPS 198, the east lobe's ~80° opening angle and west lobe's ~30° opening angle are both produced by the same wide-angle protostellar wind; the difference comes from the core: on the west the ambient gas is denser by 1.5–2.8 times, its turbulent pressure squeezes the wind and yields a narrow cavity, while on the east the lower density lets the cavity expand. Quantitatively, fitting the lobe shapes to a constant-pressure-ratio version of the cavity-shape equation gives $\xi = p_{\rm core}/p_{\rm wind} = 0.20$ on the east and $0.58$ on the west, a factor of 2.9 that the paper attributes to the density contrast after ruling out asymmetric winds and significant differences in turbulence. The paper reads this as direct evidence that core density controls outflow opening angle, and generalizes it to an evolutionary picture: as a core loses mass to accretion and dispersal, its density drops, the cavity widens, and widening stops once the cavity reaches the intrinsic opening angle of the launched wind.

Load-bearing premise

The model assumes a single, constant ratio of core pressure to wind pressure all along each outflow lobe; if that ratio actually varies with distance, the fitted pressure differences are biased and the density explanation does not follow.

Editorial extensions

If this is right

  • If core density sets the opening angle, outflow cavities widen naturally as protostellar evolution removes core mass, giving a mechanism for the observed Class 0-to-Class I widening and its eventual plateau.
  • A single protostar with an asymmetric core can display two lobes with very different opening angles even though the wind is symmetric, which explains sources like HOPS 198 without invoking separate winds.
  • The efficiency of outflow-driven core dispersal depends on the density the outflow pushes against: wide cavities form in low-density surroundings, so dispersal is more effective once the core has already been depleted.
  • The model's fit implies a wide-angle wind (≳80°) launched from HOPS 198, so future wind tracers should find a broad, not purely jet-like, wind component.

Reading between the lines

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

  • A testable extension: in a sample of Class 0 and Class I protostars with resolved core density maps, lobe opening angle should anticorrelate with the local core surface density on a lobe-by-lobe basis; the scatter in opening angle among protostars of similar bolometric temperature could largely reflect core density differences rather than age differences.
  • The same pressure-balance argument implies that the outflow opening angle can be used as a remote probe of core density structure, including in systems where dust or CO tracers are confused.
  • If the mechanism generalizes, then early, dense cores should systematically produce narrow outflows; this would strengthen the case that outflows of young Class 0 sources are less effective at dispersing gas until the core density has dropped, refining the feedback timeline.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 4 minor

Summary. The paper presents ALMA and CARMA-NRO observations of the Class 0 protostar HOPS 198, showing a strong east-west asymmetry in both the surrounding core surface density and the molecular outflow morphology. The eastern outflow lobe has an opening angle of about 80 degrees, while the western lobe is narrower, about 30 degrees; the west side of the core is measured to be 1.5--2.8 times denser than the east side. The authors use an analytical cavity-shape model based on Li et al. (2013), in which the ratio xi between core turbulent pressure and wind ram pressure is constant along each lobe, and fit the two lobe shapes to obtain xi values of 0.20 (east) and 0.58 (west). Interpreting the xi ratio of about 2.9 as a density contrast, they conclude that the opening-angle asymmetry is caused by the core density difference, and they generalize this to a picture in which decreasing core density drives the temporal widening of outflow cavities as protostars evolve.

Significance. If robust, the result would provide a direct observational link between ambient core density and molecular outflow opening angle, strengthening the hypothesis that outflow widening from Class 0 to Class I is governed by the decline of core density. The paper is built on good-quality ALMA data and includes careful treatments of cloud subtraction, opacity correction, and an independent check of the core density asymmetry using C18O surface-density maps from two different datasets. The authors are also transparent about the main simplifications of the model. However, the quantitative bridge from fitted lobe shapes to a density contrast rests on several strong assumptions, especially the constancy of xi along each lobe and the use of different contour thresholds for the two lobes. These issues need to be addressed with explicit sensitivity tests before the central claim can be considered secure.

major comments (4)
  1. [Section 3.3.2, Eq. (6)] The two-parameter fit (alpha, r0) for each lobe has a known degeneracy between alpha and r0, which the authors acknowledge but do not quantify. The quoted posterior values are r0_east = 0.12" and r0_west = 1.56", a factor of about 13, and the authors attribute this difference to the constant-xi assumption. Because the shape is fit with two free parameters per lobe, the derived xi values may absorb shape information that a more physical model would carry in r0 or in a radially varying xi. I request a quantitative demonstration that the xi ratio is robust to this degeneracy, for example by showing the posterior covariance, or by refitting with a common or physically motivated r0 and checking how much the xi_west/xi_east ratio changes. Without such a test, the value 2.9 is not a secure quantitative result.
  2. [Section 3.3.2, Eq. (5)] The model assumes a single constant pressure ratio xi = p_core/p_wind along the entire length of each outflow lobe. The authors explicitly note that xi is unlikely to be constant in the inner envelope and that the inferred values are biased, but the central conclusion in Section 3.3.3 that 'it is relatively safe to conclude' the density explanation requires a quantitative estimate of this bias. If, as the observed surface-density profile suggests, xi(r) rises toward the star and is higher on the west side, part of the east-west opening-angle difference could be absorbed by the radial shape of xi(r) rather than by a global factor of 2.9. I recommend adding a sensitivity test with a simple radially varying xi (for example, a step or power-law profile guided by the observed density gradient) to show that the inferred density contrast remains of order 1.5--2.8. This is load-bearing because the density claim rests directly on the fitted xi ratio.
  3. [Section 3.3.3 and Figure 6] The eastern and western lobes are fit using different contour levels: 11 Msun/pc2 (10% of the maximum) for the east and 32 Msun/pc2 (30% of the maximum) for the west. Since the fitted opening angle and the inferred xi depend on the selected surface-density threshold, part of the reported 80-degree versus 30-degree contrast may be a threshold effect. The paper does not test the sensitivity of the fitted xi values to the chosen contour level. I request that the fits be repeated for a range of contour levels (e.g., 10%, 20%, and 30% for both lobes) and that the resulting xi_west/xi_east ratio be compared with the measured surface-density ratio 1.5--2.8. If the inferred ratio changes substantially with the choice of contour, the claimed quantitative agreement is not meaningful.
  4. [Section 3.3.3, Eq. (8)] The conversion from the xi ratio to a density ratio assumes that the winds on the two sides have the same density and velocity, and that the core velocity dispersions are equal. The authors state that the observed line widths differ by less than 30%, but this uncertainty is not propagated into the quoted density ratio 2.9, and the wind symmetry is assumed rather than measured. The comparison with the independent surface-density ratio of 1.5--2.8 should include these uncertainties, or at least an explicit propagation of the 30% line-width uncertainty, before claiming consistency. This is a smaller point than the two previous ones, but it affects the precision of the central claim.
minor comments (4)
  1. [Section 3.3.3] There is a typo: 'the true width of of the outflow lobes' should read 'the true width of the outflow lobes'.
  2. [Appendix B.2] There is a typo: 'the mass of the outflow can was estimated' should read 'the mass of the outflow can be estimated' or 'was then estimated'.
  3. [Section 3.2] The statement that 'the two outermost green contours ... are predominantly in the western lobe' would be clearer if the contour levels were explicitly repeated in the sentence, since the reader must refer back to the caption to identify the levels.
  4. [Figure 6 caption] The caption should state explicitly that the two lobes are fit at different fractional contour levels (10% versus 30% of the maximum), since this is essential for interpreting the fits and is currently only mentioned in the main text.

Circularity Check

1 steps flagged · score 2.0 of 10

Quantitative density contrast is the ratio of fitted ξ parameters, but the conclusion is anchored by an independent C18O surface-density asymmetry; no load-bearing self-citation.

  1. fitted input called prediction [Section 3.3.3, paragraph following Eq. (8)]
    "Therefore, the difference of factor of ∼2.9 in the pressure ratio ξ is most likely caused by a difference in the gas density between the two sides of the core. That is, the west side of the core would have to be denser by about 2.9 times than the east side. This interpretation is consistent with our independent result, where we found that the surface density of the west core side is 1.5−2.8 times higher than that of the east side."

    The 2.9-fold density contrast is not independently predicted: it is the ratio of the MCMC-fitted pressure ratios ξ_west=0.58 and ξ_east=0.20, which were free parameters fit to the observed lobe shapes. Since the lobe shapes already encode the opening-angle asymmetry, the statement that the west side 'would have to be denser by about 2.9 times' is a restatement of the fitted ξ ratio, not a first-principles prediction. The circularity is partial because the paper immediately checks this fitted ratio against an independently measured C18O surface-density ratio (1.5−2.8) that was not used in the fit, so the central conclusion does not rest solely on the fitted parameters.

full rationale

The paper's central claim — that the east-west opening-angle asymmetry is caused by the core density asymmetry — is anchored by two independent observables: the measured opening angles (∼80° east vs ∼30° west) and the C18O surface-density asymmetry (west 1.5−2.8 times higher than east). The analytical model (Eqs. 5-6) is fit separately to each lobe with free parameters ξ and r0. The fitted ξ ratio (0.58/0.20 ≈ 2.9) is then compared with the independent density ratio, which is a genuine, falsifiable consistency check rather than a forced result: the density map was not used to set the shape-fit parameters. The only mild circularity is that the quantitative 'required' density contrast is literally the ratio of fitted ξ values, so presenting it as 'we find the difference can be explained by density' slightly overstates the derivation; it is a fit-derived consistency check, not a prediction from density to opening angle. The paper also explicitly acknowledges the constant-ξ assumption and the r0−ξ degeneracy, and the conclusion is further supported by independent Herschel/C18O column-density comparisons. There is no load-bearing self-citation: the Hsieh et al. (2023) and Arce-related citations are data references or simulations used as context, not circular justifications. Overall, the derivation is substantially self-contained and the central claim has independent content, so the circularity score is low.

Assumptions & free parameters 5 free parameters · 7 assumptions · 0 invented entities

The central claim rests on the pressure-balance relation from Li et al. (2013), a constant pressure ratio xi per lobe, and assumptions that the wind is symmetric and the velocity dispersion is similar on both sides. The fitted parameters are the per-lobe xi and base radius r0, plus the hand-selected contour levels; the paper is transparent about most of these, especially the constant-xi limitation.

free parameters (5)
  • xi_east (pressure ratio, eastern lobe) = 0.20 +0.02/-0.02
    Fit parameter in Eq. 6 controlling eastern lobe cavity shape; part of the inferred 2.9x density contrast.
  • xi_west (pressure ratio, western lobe) = 0.58 +0.03/-0.03
    Fit parameter in Eq. 6 controlling western lobe cavity shape; ratio to xi_east is 2.9, interpreted as density contrast.
  • r0_east (base width, eastern lobe) = 0.12 +0.08/-0.06 arcsec
    Fit parameter in Eq. 6; authors caution its value is unreliable due to r0-xi degeneracy and constant-xi assumption.
  • r0_west (base width, western lobe) = 1.56 +0.18/-0.18 arcsec
    Fit parameter in Eq. 6; large difference with east lobe is attributed to the constant-xi oversimplification.
  • Outflow contour levels for fitting = 11 M_sun pc^-2 east, 32 M_sun pc^-2 west
    Hand-selected as 10% and 30% of maximum outflow surface density (Sec. 3.3.3, Fig. 6); influences the fitted shapes and all derived parameters.
assumptions (7)
  • domain assumption Pressure balance between wind ram pressure and core turbulent pressure determines cavity shape (Eq. 1, after Li et al. 2013)
    Adopted as the starting model (Sec. 3.3.2); if the true cavity shape is set by another mechanism, the whole inference is invalid.
  • domain assumption Wind density profile scales as r_sph^{-2} sin^2 theta_sph at large distances (Eq. 4)
    Assumed so Equation 1 applies; based on asymptotic hydromagnetic winds (Ostriker 1997; Matzner and McKee 1999).
  • ad hoc to paper Pressure ratio xi = p_core/p_wind is constant along each lobe
    Stated in Sec. 3.3.2, needed to derive closed-form Eq. 6. The authors acknowledge this is likely false in the inner envelope and creates the r0-xi degeneracy.
  • domain assumption The protostellar wind is symmetric in density and velocity on both sides
    Used in Sec. 3.3.3 to convert the xi ratio into a core-density ratio; no direct wind tracer is available.
  • domain assumption Core velocity dispersion is similar on the two sides
    Based on less than 30% difference in C18O FWHM from 1.5 arcsec apertures (Sec. 3.3.3); this is a coarse check.
  • standard math C18O is optically thin and in LTE at Tex = 20 K; fixed CO abundance ratios
    Standard assumptions in Appendix B for mass and surface-density mapping; validated by comparison with Herschel dust column density in Appendix A.
  • domain assumption pcore <= pwind and the wind opening angle exceeds the cavity opening angle
    Required for Eq. 1 and for the interpretation that the cavity stops growing at the wind opening angle; discussed in Sec. 3.3.2 and 3.3.3.

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Cite this review

Pith. "Pith review of Asymmetry in the protostellar system HOPS 198: Evidence for the evolution of outflow opening angle driven by density of the surrounding core." pith.science (2026). https://pith.science/paper/W5UQ6675

@misc{pith2026260804890,
  author       = {Pith},
  title        = {Pith review of: Asymmetry in the protostellar system HOPS 198: Evidence for the evolution of outflow opening angle driven by density of the surrounding core},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/W5UQ6675}},
  note         = {Machine review of arXiv:2608.04890}
}
abstract

Protostellar outflows are thought to be responsible for the low star formation efficiency of protostellar cores. However, whether outflows can disperse a significant fraction of the gas in the core depends on the outflow opening angle. It is established that the outflow opening angle increases during the early stages of the protostellar evolution, but the underlying mechanism is poorly understood. Observations of HOPS 198, a Class 0 protostar in the Orion A molecular cloud, provide insights into this question. HOPS 198 exhibits a strong east-west asymmetry in its outflow and its core. The opening angle of the eastern lobe ($\sim80^{\circ}$) is more than twice wider than that of the western lobe ($\sim30^{\circ}$), while the surface density of the west side of the core is $1.5-2.8$ times higher than the east side. Using an analytical model in which the molecular outflow morphology is shaped by interactions between the wide-angle protostellar wind ($\gtrsim 80^{\circ}$) and surrounding material in the core, we find that the difference in opening angle for the two lobes can be explained by the difference in core density on the two sides. This result supports the hypothesis that the evolution of the outflow opening angle is driven by the evolution in the density of the protostellar core.

Figures

Figures reproduced from arXiv: 2608.04890 by the authors.

Figure 1
Figure 1. a) Integrated intensity map of 12CO for redshifted channels with 6.15 ≤ vlos ≤ 8.37 km/s and 10.27 ≤ vlos ≤ 8.37 km/s. b) Integrated intensity map of 12CO for blueshifted channels with −8.94 ≤ vlos ≤ 4.96 km/s. c) Zoomed-in continuum image of the disk observed by Tobin et al. (2020) using their ALMA 0.87 mm continuum image. The red contours show the continuum emission from our dataset at levels of 7σ, 40σ, and 142σ,… view at source ↗
Figure 2
Figure 2. Left: Surface density map of the core computed from the C [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Surface density map of the molecular outflow com [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Ratio of the surface density of the west side of the core to [PITH_FULL_IMAGE:figures/full_fig_p004_4.png]
Figure 5
Figure 5. Figure 5: Surface density map of the core (image) and molecular outflow (white contours) at di [PITH_FULL_IMAGE:figures/full_fig_p005_5.png]
Figure 6
Figure 6. Figure 6: Shape of the outflow described by the analytical model [PITH_FULL_IMAGE:figures/full_fig_p005_6.png]

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Reviewed August 6, 2026 · model on record in the stance chip above.