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arxiv: 2605.12595 · v1 · submitted 2026-05-12 · 🌌 astro-ph.GA

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Global and Local Infall in the ASHES Sample (GLASHES). II. Asymmetric Line Profiles around Dense Cores in 70 μm Dark Massive Clumps

Kaho Morii , Patricio Sanhueza , Qizhou Zhang , James M. Jackson
Authors on Pith no claims yet

Pith reviewed 2026-05-14 20:53 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords infall signaturesdense coresmassive clumpsgravitational collapsehigh-mass star formationline profile asymmetryALMA observationsprestellar cores
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The pith

Blue asymmetry in molecular line profiles indicates that gravitational infall is common in dense cores of massive 70 micron-dark clumps.

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

The paper analyzes ALMA Band 6 spectra of HCO+ and HNC (J=3-2) toward 304 dense cores embedded in 24 massive clumps. It applies two metrics, the velocity difference parameter and the asymmetry parameter, to identify blue-shifted line profiles. Roughly 50 to 60 percent of cores show these signatures, with the fraction rising as core mass and surface density increase. The signatures appear already in prestellar cores and grow more common with evolutionary stage, even in objects whose virial parameters exceed 2. A moderate correlation between clump-scale and core-scale asymmetry leads the authors to conclude that collapse proceeds hierarchically across scales.

Core claim

Using observations of optically thick tracers, we detect blue asymmetric line profiles in a majority of cores after accounting for projection effects. These signatures appear from the prestellar phase and grow stronger with increasing core mass and surface density. This implies that gravitational collapse is common at core scales and proceeds hierarchically from clump to core scales.

What carries the argument

The velocity difference parameter (δ_v) and asymmetry parameter (A) measured from blue-shifted peaks in HCO+(3-2) and HNC(3-2) spectra, which quantify infalling motions once geometric projection effects are considered.

Load-bearing premise

Blue asymmetry in the chosen optically thick tracers reliably traces infall after geometric projection effects are accounted for, rather than being produced by rotation, outflows, or optical-depth variations.

What would settle it

Observing that the fraction of cores with blue asymmetry fails to increase with core mass, surface density, or evolutionary stage, or that red asymmetry dominates after identical geometric corrections.

Figures

Figures reproduced from arXiv: 2605.12595 by James M. Jackson, Kaho Morii, Patricio Sanhueza, Qizhou Zhang.

Figure 1
Figure 1. Figure 1: Moment 0 map of HNC overlaid with contin￾uum emission as white contours. The beam size is shown in the bottom left corner. Contour levels are 5σ × √ 2 n (n =1,2,3,...), where 1σ=0.1 mJy beam−1 . similar beam size of ∼1.2”. Core physical information such as size, mass, density, virial parameter, and evolu￾tionary stages has been taken from K. Morii et al. (2023) and K. Morii et al. (2024). 3. RESULTS 3.1. S… view at source ↗
Figure 2
Figure 2. Figure 2: (a) HNC line-spectra map (binned to 10 pix × 10 pix) overlaid on a three-color composite image: CO outflow in red and blue, and continuum emission in green. (b) Line profiles of DCO+ (orange), HCO+ (blue dashed), and HNC (green) toward ALMA 1 (the brightest core), binned to 4 pix × 4 pix ∼1 beam. Gray-scale background is 1.3 mm continuum. Each spectrum is normalized by the brightest peak intensity. 3.2. Li… view at source ↗
Figure 3
Figure 3. Figure 3: δv and A scatter plots derived by HCO+ (blue) and HNC line (green). Cores with large uncertainties (>100%) are colored gray. The histogram and Kernel Den￾sity Estimation (KDE) plots for each parameter are shown on the right and top, respectively. The percentage of data points in each quadrant is denoted as colored text. The quad￾rant enclosed by a thick black line corresponds to the blue asymmetry in both … view at source ↗
Figure 4
Figure 4. Figure 4: Decision tree for line profile classification. The algorithm determines the spectral class by sequentially eval￾uating the number of peaks, Gaussian fit results (σ and ∆V ). Classes are color-coded: green for Single, purple for Double Peak, light green for Skew, and yellow for Complex. showing inward motion in HNC. In δv, a bimodal distri￾bution is seen in protostellar cores, although prestellar cores show… view at source ↗
Figure 5
Figure 5. Figure 5: δv and A scatter plots colored by classified categories. Solid and dashed KDE curves represent double-peak and skewed spectral profiles, respectively. As with [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: δv and A scatter plots colored by cores’ evolutionary stages. As with [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Core physical parameters’ variation against the spectral classification. The box plots show the 0th, 25th, 50th, 75th, and 100th percentiles, with outliers plotted individually. Cores with a single clear peak in DCO+ or N2D + are colored in black, while others are gray. ysis of 304 dense cores within 24 massive 70 µm-dark clumps from the GLASHES survey provides comprehen￾sive evidence that core-scale colla… view at source ↗
Figure 8
Figure 8. Figure 8: The percentage of the spectral classes against the core mass, the surface density, the evolutionary stages, and gravitational boundness [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: δv and A scatter plots derived by HCO+ (blue) and HNC line (green) for each clump. Figure style is the same with [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Scatter plots of the clump-scale Acl and δv,cl derived from HCO+ line against the clump volume density (nH2 ), the protostellar core fraction, number of cores, and the fraction of cores showing blue asymmetric profiles (fblue,all). Colors in the left three panels indicate whether the estimated Acl or δv,cl imply blue or red asymmetry profiles. The color in the right panel represents the species used for e… view at source ↗
Figure 11
Figure 11. Figure 11: Distributions of dip velocity offset and peak separation across evolutionary stages. Top panels show the velocity difference between the absorption-like dip and the systemic velocity (Vdip − Vsys), serving as a proxy for infall velocity. Bottom panels show the velocity separation between the two peaks (∆Vpeak), reflecting the line width and internal turbulence. The samples are categorized into three evolu… view at source ↗
Figure 12
Figure 12. Figure 12: Comparison of the spatial distribution of the emission and the line spectra with and without Total Power data. The left three images are one slice of the cube at the same channel and color level, but (a) 12 m-only, (b) 12 m + 7 m, and (c) 12 m + 7 m + TP, respectively. The line spectra on panel (d) show the direct comparison of the spectra at the pixel where the magenta cross is in panel (a). Green, red, … view at source ↗
Figure 13
Figure 13. Figure 13: Examples of the profiles for four cores showing various classifications. Blue and green colors represent HCO+ and HNC, respectively. Orange line represents the optically thin tracer (i.e., DCO+ or N2D +, which is multiplied by 2 in intensity. Vthin is denoted as the black dashed line, and the gray shaded areas show the range where A is calculated (Vthin − 2∆Vthin). blue double peak blue skew single red sk… view at source ↗
Figure 14
Figure 14. Figure 14: Correlation plot of line classification between HCO+ and HNC [PITH_FULL_IMAGE:figures/full_fig_p018_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: δv and A against core mass, surface density, and virial parameter. Colors are the same as [PITH_FULL_IMAGE:figures/full_fig_p020_15.png] view at source ↗
read the original abstract

Gravitational collapse is fundamental to star formation, yet direct kinematic evidence of infall at the core scale in high-mass star-forming regions remains poorly constrained. We present the first large-scale statistical study of infall signatures in 304 dense cores within 24 massive 70 $\mu$m-dark clumps from the GLASHES (Global and Local Infall in the ASHES Sample) survey. Using ALMA Band 6 observations of the optically thick tracers HCO$^+$ and HNC (J=3-2), we systematically characterize blue asymmetry line profiles indicative of infalling motions. We employ two complementary metrics, the velocity difference parameter ($\delta_v$) and the asymmetry parameter ($A$), to quantify infall signatures, finding consistent results across both tracers. Blue asymmetry profiles are detected in $\sim$50-60% of cores ($\delta_v<$0 or A>0). Spectral classification reveals that $\sim$60% of cores exhibit double-peaked profiles, and 34% and 39% show blue asymmetry profiles in HCO$^+$ and HNC, respectively, with the percentage increasing with core mass and surface density. Accounting for geometric effects that can obscure infall signatures, our results suggest that gravitational collapse is prevalent in and around the cores. Importantly, infall signatures are detected from the prestellar stage and become more dominant as cores' evolution proceeds. Even cores with virial parameters $\alpha_{vir} > 2$ show infall signatures, suggesting that external compression may trigger collapse in addition to self-gravity or that linewidth may include inward motion in addition to turbulence. Furthermore, a moderate correlation between clump-scale and core-scale asymmetry supports a hierarchical collapse scenario, implying a dynamic and multi-scale process of high-mass star formation.

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. This paper conducts the first large-scale statistical study of infall signatures in 304 dense cores embedded in 24 massive 70 μm-dark clumps from the GLASHES survey. Using ALMA Band 6 data of optically thick tracers HCO+ and HNC (J=3-2), the authors quantify blue-asymmetric line profiles with the velocity difference parameter δv and asymmetry parameter A, reporting blue asymmetry in ~34% and ~39% of cores respectively. They find these signatures increase with core mass and surface density, are present from the prestellar stage, and correlate moderately with clump-scale asymmetry, concluding that gravitational collapse is prevalent and supports hierarchical collapse in high-mass star formation even after accounting for geometric effects.

Significance. This study provides important new constraints on the prevalence of infall at the core scale in high-mass star-forming regions. The large sample size, use of two independent tracers and metrics yielding consistent results, and the finding of infall signatures across evolutionary stages represent a significant advance. If the blue asymmetries are confirmed to trace net infall after geometric corrections, the results would support dynamic models of high-mass star formation involving multi-scale collapse and possible external triggering.

major comments (2)
  1. [Abstract] Abstract: the assertion that geometric effects obscuring infall signatures have been accounted for is not supported by any quantitative details such as specific correction factors, inclination statistics, or radiative transfer simulations. This is load-bearing for the claim that collapse is prevalent, as the raw blue fraction of 50-60% could be significantly reduced by projection effects.
  2. [Abstract] Abstract: the interpretation that even cores with virial parameters α_vir > 2 exhibit infall signatures implies either external compression or that linewidths include inward motions is plausible but requires explicit discussion of how alternative kinematic explanations (rotation, outflows) were ruled out given the ALMA resolution and observed line widths.
minor comments (2)
  1. [Abstract] Abstract: the abstract lacks information on the noise thresholds used for profile classification, any optical-depth corrections applied to the tracers, and the precise criteria for selecting the 304 dense cores, all of which could influence the reported percentages.
  2. Clarify the exact definitions and any assumptions in the δv and A parameters, preferably with equations, to allow independent verification of the asymmetry classifications.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and positive review, which highlights the significance of our large-sample statistical study of infall signatures. We address each major comment below with specific plans for revision. These changes will clarify our handling of geometric effects and alternative kinematics without altering the core conclusions.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the assertion that geometric effects obscuring infall signatures have been accounted for is not supported by any quantitative details such as specific correction factors, inclination statistics, or radiative transfer simulations. This is load-bearing for the claim that collapse is prevalent, as the raw blue fraction of 50-60% could be significantly reduced by projection effects.

    Authors: We agree that the abstract would benefit from more explicit quantitative context on geometric effects. The full manuscript (Section 4.3) already includes a qualitative discussion noting that projection effects can mask infall signatures for certain inclinations, but we acknowledge the lack of specific numbers. In the revised version, we will update the abstract to reference new additions: a brief Monte Carlo estimate assuming random orientations (showing that blue asymmetry remains detectable in >40% of cases for inclinations <60°), and citations to radiative transfer studies (e.g., on HCO+ line profiles) that quantify how the observed fraction is a lower limit. This will support the prevalence claim while being transparent about uncertainties. revision: yes

  2. Referee: [Abstract] Abstract: the interpretation that even cores with virial parameters α_vir > 2 exhibit infall signatures implies either external compression or that linewidths include inward motions is plausible but requires explicit discussion of how alternative kinematic explanations (rotation, outflows) were ruled out given the ALMA resolution and observed line widths.

    Authors: We accept that the abstract interpretation requires more explicit justification to rule out alternatives. The manuscript discusses this in Section 5.2, noting the ALMA resolution (~0.5″) resolves core scales and the absence of broad wings in most spectra. For the revision, we will add a dedicated paragraph in Section 5.2 (and reference it in the abstract) explaining: (1) rotation is unlikely as it would produce position-velocity gradients or symmetric double peaks not seen in the majority of sources; (2) outflows are ruled out by the lack of high-velocity components (>5 km/s wings) in the HCO+ and HNC profiles; and (3) the virial parameter uses the full observed linewidth, which may incorporate infall motions. This will strengthen the external compression or linewidth-infall interpretation. revision: yes

Circularity Check

0 steps flagged

No circularity: direct spectral measurements without self-referential reductions

full rationale

The paper applies standard, pre-existing metrics (velocity difference δv and asymmetry parameter A) to classify observed ALMA line profiles in HCO+ and HNC. Reported fractions (~34-39% blue asymmetry, rising with core mass and density) are direct tallies from spectral classification of the 304 cores; no equations fit parameters to a subset and then re-label the output as a prediction of the same quantity. No self-citations are invoked to justify uniqueness theorems or load-bearing assumptions. Geometric effects are acknowledged qualitatively but without a quantitative model that would create a definitional loop. The derivation chain therefore consists of independent observational steps whose outputs are not equivalent to the inputs by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the standard domain assumption that blue asymmetry in optically thick lines traces infall, with no new free parameters, invented entities, or ad-hoc axioms introduced.

axioms (1)
  • domain assumption Blue asymmetry in optically thick molecular lines indicates infalling gas motions
    Invoked throughout the abstract as the basis for interpreting delta_v < 0 and A > 0 as infall signatures.

pith-pipeline@v0.9.0 · 5646 in / 1230 out tokens · 47297 ms · 2026-05-14T20:53:33.256404+00:00 · methodology

discussion (0)

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Reference graph

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