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arxiv: 2404.13520 · v1 · submitted 2024-04-21 · 🌌 astro-ph.GA

An ALMA search for substructure and fragmentation in starless cores in Orion B North

Samuel Fielder , Helen Kirk , Michael Dunham , Stella Offner This is my paper

Pith reviewed 2026-05-24 02:05 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords starless coresALMA observationsOrion B Northvirial analysisturbulent fragmentationmolecular cloudsChamaeleon IOphiuchus
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The pith

ALMA observations of Orion B North show its starless cores match turbulent model predictions, unlike the less bounded Chamaeleon I population where external pressure dominates binding energy.

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

The paper presents ALMA Cycle 3 data on 73 cores in Orion B North, detecting 34 continuum sources of which four qualify as starless after cross-checks with other datasets. Synthetic observations from a collapsing turbulent magnetized core simulation predict at least two detectable starless cores, matching the observed count. A virial analysis places these Orion B North cores alongside those from Ophiuchus as consistent with turbulent fragmentation models. In contrast, the Chamaeleon I population emerges as less gravitationally bound overall, with external pressure supplying the dominant contribution to binding energy. This environmental difference is offered as the reason Chamaeleon I cores deviate from the model while the other two regions do not.

Core claim

The central claim is that the Chamaeleon I starless core population is characteristically less bounded than the populations in Ophiuchus and Orion B North, with external pressure contributions dominating the binding energy of the cores. These differences may explain why the Chamaeleon I cores do not follow turbulent model predictions, while the Ophiuchus and Orion B North cores are consistent with the model. The Orion B North ALMA data detect four starless sources, a number consistent with expectations from the simulation.

What carries the argument

The virial analysis comparing gravitational binding, kinetic energy, and external pressure terms across the three regions' starless core populations.

If this is right

  • Orion B North and Ophiuchus starless cores align with predictions from turbulent fragmentation models.
  • Chamaeleon I cores deviate from the same models because they are less bounded and more influenced by external pressure.
  • The observed number of starless cores in Orion B North matches the minimum expected from synthetic observations of a collapsing turbulent core.
  • Environmental conditions in different molecular clouds can produce measurable differences in core boundedness.

Where Pith is reading between the lines

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

  • If external pressure dominates in some regions, models of core evolution may need to incorporate cloud-scale pressure terms more explicitly to predict fragmentation outcomes.
  • Measuring magnetic field strengths across these regions could test whether the current virial results change the relative boundedness ranking.
  • The isolated versus clustered locations of the four Orion B North sources suggest that local environment within a cloud may also affect detectability of starless cores.

Load-bearing premise

The four continuum sources can be classified as starless solely from comparisons with other datasets, and the virial analysis accurately reflects binding energy without corrections for magnetic support or projection effects.

What would settle it

Higher-resolution infrared or X-ray observations that reveal embedded protostars in any of the four sources, or direct Zeeman measurements showing significant magnetic support in Chamaeleon I cores, would undermine the starless classification or the boundedness comparison.

Figures

Figures reproduced from arXiv: 2404.13520 by Helen Kirk, Michael Dunham, Samuel Fielder, Stella Offner.

Figure 1
Figure 1. Figure 1: SCUBA2 850 µm image of the Orion BN cloud adapted from Kirk et al. (2016). The blue circles show all 73 starless dense cores identified by NWT07 which were ob￾served by ALMA, with the diameters of the circles equal to the primary beam of the 12 m observations. In their re-analysis of all SCUBA archive data of the Orion star-forming regions, Nutter & Ward-Thompson (2007) (hereafter NWT07) identified a total… view at source ↗
Figure 2
Figure 2. Figure 2: Left: Zoom-in of the upper region of ALMA field BN-546074-01342Mosaic with source 5 shown in the center (full mosaic shown in [PITH_FULL_IMAGE:figures/full_fig_p013_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: ALMA field BN-546049-00911Mosaic, with starless candidate source 1. The grayscale ranges linearly from - 0.5 mJy beam−1 to 1.0 mJy beam−1 . The blue contours correspond to SCUBA2 850 µm emission at the corresponding levels in mJy arcsec−2 : 0.15, 0.5, 1.0, 1.5, 3.0, 5.0. All detections are labeled in black with their respective index number. Protostellar sources in the field of view are also plotted with r… view at source ↗
Figure 4
Figure 4. Figure 4: ALMA field BN-546074-01342Mosaic, with starless candidate source 4. See [PITH_FULL_IMAGE:figures/full_fig_p015_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: ALMA field BN-546405+00032Mosaic, with starless candidates sources 23 and 24. See [PITH_FULL_IMAGE:figures/full_fig_p016_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of ALMA detection peak fluxes. Detections with a peak flux greater than 30 mJy beam−1 are plotted in the final bin shown. We show both the protostellar ALMA detections in red (30 sources total), along with the candidate starless core detections in black (4 sources total). 4.2. ALMA Peak Flux [PITH_FULL_IMAGE:figures/full_fig_p016_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: shows the distribution of central concentra￾tion for all NWT07 cores in Orion B North. There are six starless dense cores that have concentrations lower than 0.33, the minimum value allowed for a uniform 0.2 0.4 0.6 0.8 1.0 SCUBA Concentration 0 2 4 6 8 10 Number Protostellar Starless Source 1 Source 4 Sources 23/24 [PITH_FULL_IMAGE:figures/full_fig_p017_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Synthetic ALMA 106 GHz observations of the 0.4M⊙ simulation, at six given timesteps, indicated in each panel along side the central density of the core. The synthesized beam is given in the first panel as a yellow ellipse in the bottom left corner. The dashed contour represents the 3σ level. The solid contours start at a level of 5σ and increase by 2σ, where 1σ ∼ 0.045 mJy beam−1 . We consider a robust det… view at source ↗
Figure 9
Figure 9. Figure 9: Distribution of NWT07 core number densi￾ties. The black histogram indicates cores classified as star￾less, while the red filled histogram indicates cores classified as protostellar in nature. The vertical black dashed line indi￾cates the minimum detectable density, as computed in Sec￾tion 5.2. expected number of starless core detections to 0.79. The results would remain unaffected with either difference in… view at source ↗
Figure 10
Figure 10. Figure 10: Lifetimes vs. central number densities for the 0.4M⊙ simulation (C04) and the 4.0M⊙ simulation (C4), as reproduced from [PITH_FULL_IMAGE:figures/full_fig_p021_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Virial parameter versus core mass, computed for each of the three cloud dense core populations. Each color represents a distinct star forming region. Open markers show the starless core population, while filled markers show cores that are protostellar in nature. Cores lying above the dashed line are considered gravitationally unbound. and self-gravity in the core, as well as the external pres￾sure contrib… view at source ↗
Figure 12
Figure 12. Figure 12: Confinement ratio versus the virial ratio, as computed for each of the three cloud dense core populations. See [PITH_FULL_IMAGE:figures/full_fig_p028_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Synthetic ALMA 106 GHz observations of the 4M⊙ simulation, at six given timesteps, indicated in each panel along side the central density of the core. We adopt the same plotting convention as [PITH_FULL_IMAGE:figures/full_fig_p030_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: ALMA single pointing fields that harbor detections. See [PITH_FULL_IMAGE:figures/full_fig_p032_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: ALMA mosaic fields that harbor detections. See [PITH_FULL_IMAGE:figures/full_fig_p033_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: ALMA mosaic field that harbor detections. See [PITH_FULL_IMAGE:figures/full_fig_p034_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: ALMA mosaic fields that harbor detections. See [PITH_FULL_IMAGE:figures/full_fig_p035_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: ALMA mosaic field BN-546244-00001 that harbor detections. See [PITH_FULL_IMAGE:figures/full_fig_p036_18.png] view at source ↗
read the original abstract

We present Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 3 observations of 73 starless and protostellar cores in the Orion B North molecular cloud. We detect a total of 34 continuum sources at 106 GHz, and after comparisons with other data, 4 of these sources appear to be starless. Three of the four sources are located near groupings of protostellar sources, while one source is an isolated detection. We use synthetic observations of a simulation modeling a collapsing turbulent, magnetized core to compute the expected number of starless cores that should be detectable with our ALMA observations and find at least two (1.52) starless core should be detectable, consistent with our data. We run a simple virial analysis of the cores to put the Orion B North observations into context with similar previous ALMA surveys of cores in Chamaeleon I and Ophiuchus. We conclude that the Chamaeleon I starless core population is characteristically less bounded than the other two populations, along with external pressure contributions dominating the binding energy of the cores. These differences may explain why the Chamaeleon I cores do not follow turbulent model predictions, while the Ophiuchus and Orion B North cores are consistent with the model.

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 paper reports ALMA Cycle 3 106 GHz continuum observations toward 73 starless and protostellar cores in Orion B North. It detects 34 sources, classifies four as starless after cross-comparison with other datasets, and finds this count consistent with the number (at least 1.52–2) expected from synthetic observations of a collapsing turbulent magnetized core simulation. A simple virial analysis is then used to compare the Orion B North population with prior ALMA surveys in Chamaeleon I and Ophiuchus, leading to the conclusion that Chamaeleon I cores are characteristically less bounded, with external pressure dominating their binding energy; this difference is invoked to explain why only the Ophiuchus and Orion B North populations match turbulent model predictions.

Significance. If the starless classification and virial parameters hold, the work supplies a useful observational test of turbulent fragmentation models across clouds and highlights the possible role of external pressure in setting core boundedness. The direct comparison of observed detection statistics to synthetic observations of a simulation is a clear methodological strength that strengthens the consistency claim for Orion B North.

major comments (2)
  1. [Section describing continuum source classification and starless identification] The section on identification of the four 106 GHz sources as starless: classification rests entirely on comparisons with external datasets, yet the manuscript supplies no explicit criteria, contamination estimates, or uncertainty quantification. Because the count of four starless cores is used both for the simulation comparison and for the subsequent population-level boundedness claim versus Chamaeleon I, this omission is load-bearing for the central conclusions.
  2. [Virial analysis and population comparison] The virial analysis section (and associated figures/tables): the analysis treats kinetic plus gravitational terms as sufficient and concludes that external pressure dominates binding energy in Chamaeleon I without applying corrections for magnetic support or line-of-sight projection effects. These omissions directly affect the boundedness ranking across the three clouds and the attribution of model-consistency differences, so the comparison claim requires either the corrections or a quantitative assessment of their possible impact.
minor comments (2)
  1. [Abstract] Abstract: the phrasing “at least two (1.52) starless core should be detectable” is grammatically awkward and the parenthetical value is not explained; reword for clarity.
  2. [Figures and tables] Figure captions and text: ensure all symbols, error bars, and virial-parameter definitions are defined on first use so that the boundedness comparison can be followed without reference to external papers.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful and constructive report. We address each major comment below and indicate the revisions we will make to strengthen the manuscript.

read point-by-point responses

  1. Referee: [Section describing continuum source classification and starless identification] The section on identification of the four 106 GHz sources as starless: classification rests entirely on comparisons with external datasets, yet the manuscript supplies no explicit criteria, contamination estimates, or uncertainty quantification. Because the count of four starless cores is used both for the simulation comparison and for the subsequent population-level boundedness claim versus Chamaeleon I, this omission is load-bearing for the central conclusions.

    Authors: We agree that the classification procedure requires more explicit documentation. In the revised manuscript we will add a dedicated subsection that lists the precise criteria applied to each external dataset (e.g., absence of Spitzer/Herschel point sources above a stated flux threshold, lack of outflow tracers, and positional coincidence tolerances), together with a quantitative estimate of possible contamination by embedded protostars and the associated uncertainty on the final count of four starless cores. This addition will make the robustness of the simulation comparison and the population comparison fully transparent. revision: yes

  2. Referee: [Virial analysis and population comparison] The virial analysis section (and associated figures/tables): the analysis treats kinetic plus gravitational terms as sufficient and concludes that external pressure dominates binding energy in Chamaeleon I without applying corrections for magnetic support or line-of-sight projection effects. These omissions directly affect the boundedness ranking across the three clouds and the attribution of model-consistency differences, so the comparison claim requires either the corrections or a quantitative assessment of their possible impact.

    Authors: The virial analysis is presented as a simple comparison, as stated in the manuscript. We acknowledge that magnetic support and projection effects are not corrected for and could alter the relative boundedness ranking. In revision we will add a paragraph that supplies order-of-magnitude estimates of these effects (drawing on published magnetic-field strengths for the three regions and a simple geometric argument for projection) and discusses how they might change the conclusion that external pressure dominates in Chamaeleon I. Full vector corrections are beyond the scope of the available data, but the quantitative assessment will clarify the robustness of the inter-cloud comparison. revision: partial

Circularity Check

0 steps flagged

No significant circularity; claims rest on standard methods and external comparisons

full rationale

The paper applies standard virial analysis to observed line widths and masses, classifies four sources as starless via cross-checks against independent datasets, and performs a consistency check by generating synthetic ALMA observations from an external simulation of a collapsing core. The expected detection count (1.52) is computed from that simulation rather than fitted to the current data. Population comparisons to Chamaeleon I and Ophiuchus draw on prior surveys without load-bearing self-citations or uniqueness theorems. No step equates a claimed prediction or result to its own inputs by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Based on abstract only; main unstated premises are applicability of the virial theorem to these cores and reliability of multi-wavelength classification for starless status.

axioms (1)
  • domain assumption Virial theorem can be applied to estimate binding energy of the observed cores
    Invoked for the comparative analysis of boundedness across clouds.

pith-pipeline@v0.9.0 · 5771 in / 1226 out tokens · 27432 ms · 2026-05-24T02:05:41.193176+00:00 · methodology

discussion (0)

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