Pith. sign in

REVIEW 2 major objections 6 minor 1 cited by

ALMA-IMF XVII -- Census and lifetime of high-mass prestellar cores in 14 massive protoclusters

T0 review · 2 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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

Pith's one-line read The paper identifies 30 outflow-free cores above 8 $M_\odot$ as massive prestellar candidates — 12 above 16 $M_\odot$ — and estimates their lifetime at 50–240 kyr, or 10–30 free-fall times.

desk verdict First real sample of high-mass prestellar core candidates; the lifetime ratios are suggestive but rest on an assumption the authors themselves flag. read the letter →

arxiv 2502.09426 v1 pith:5L35TJPX submitted 2025-02-13 astro-ph.GA astro-ph.SR

M. Valeille-Manet , S. Bontemps , T. Csengeri , T. Nony , F. Motte , A. M. Stutz , A. Gusdorf , A. Ginsburg
show 19 more authors
R. Galván-Madrid P. Sanhueza M. Bonfand N. Brouillet P. Dell'Ova F. Louvet N. Cunningham M. Fernández-López F. Herpin F. Wyrowski R. H. Álvarez-Gutiérrez M. Armante A. E. Guzmán N. Kessler A. Koley J. Salinas T. Yoo L. Bronfman N. Le Nestour
This is my paper · ORCID
classification astro-ph.GAastro-ph.SR
keywords high-massstarformationprestellarcoresprotostellarmolecularoutflowscorelifetimesfree-falltimeALMA-IMFsurveygalacticprotoclusters
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

The paper sets out to find the direct precursors of high-mass stars: compact, massive dust cores that have not yet ignited a protostar inside them. Using the ALMA-IMF survey's roughly 580 cores in 14 massive protoclusters, it classifies the 141 most massive cores by whether they drive CO or SiO outflows, the expected signature of active accretion. Cores with no outflow in either tracer are treated as prestellar, and the paper reports 30 such cores above 8 $M_\odot$, including 12 above 16 $M_\odot$ that it proposes as the best current candidates for high-mass star precursors. Counting these against outflow-driving protostellar cores and assuming a 300 kyr protostellar lifetime, it derives prestellar lifetimes of roughly 120–240 kyr for the 8–16 $M_\odot$ range and 50–100 kyr for the 30–55 $M_\odot$ range. Because these timescales are 10–30 times longer than the cores' free-fall times, the paper concludes that collapse is slowed by non-thermal support — turbulence, magnetic fields, or rotation — turning the high-mass prestellar phase into a measurable stage that formation models must reproduce.

What carries the argument

The load-bearing tool is the On-Off spectrum method: for each of the 141 cores above 8 $M_\odot$, a core-averaged (On) spectrum is taken inside the continuum ellipse and an annular (Off) background between 2.5 and 3.5 times the ellipse FWHM is subtracted, isolating high-velocity line-wing emission that belongs to the core itself rather than its surroundings. Emission beyond $\pm 6$ km s$^{-1}$ from the core's DCN(3–2) velocity, reaching 5$\sigma$ in either CO or SiO, marks a protostellar outflow; per-channel noise maps built from 150 random On-Off positions set the significance, and moment-zero maps of blue- and red-shifted lobes provide a spatial cross-check that rejects contamination by neighbouring outflows. The same counts feed the lifetime estimate: the prestellar-to-protostellar number ratio is multiplied by an assumed protostellar lifetime of 300 $\pm$ 100 kyr, the protostar count is corrected upward for expected ionising (UCHII) phases using the protostellar-evolution models described in Appendix D, and mass bins are built under two scenarios for envelope-mass evolution, a constant-mass clump-fed view and a decreasing-mass core-fed view.

What would settle it

A sub-arcsecond search for embedded heating in the 12 cores above 16 $M_\odot$ — mid-infrared continuum or hot-core molecular emission at high spatial resolution — would settle the central claim: several detections of compact warm dust or hot-core chemistry would mean the outflow-free cores are not all starless, and the reported prestellar lifetimes would drop toward the free-fall times. The temporal version is equally concrete: re-observing the same fields after a few years and finding newly appeared outflow wings from any of the 12 candidates would falsify their prestellar status directly.

Watch

Extended reading notes

Core claim

The central claim is that a homogeneous, statistically useful sample of high-mass prestellar cores can be pulled out of the ALMA-IMF survey by systematic outflow detection: 30 cores above 8 $M_\odot$ show no CO(2–1) or SiO(5–4) high-velocity emission, and 12 of them exceed 16 $M_\odot$, with masses up to about 54 $M_\odot$, mostly in the crowded central clumps of the protoclusters. The paper defines a high-mass prestellar core as a compact core (deconvolved size below ~5000 au) massive enough to form a high-mass star that is not yet hosting any highly accreting protostar, and it argues that any strongly accreting high-mass protostar must drive a detectable outflow inside its own core. Comparing the 30 starless cores with 52 outflow-driving protostellar cores above 8 $M_\odot$, and adopting a 300 kyr protostellar lifetime with corrections for ionising UCHII protostars and for two envelope-evolution scenarios, the paper obtains prestellar lifetimes of 120–240 kyr (8–16 $M_\odot$) and 50–100 kyr (30–55 $M_\odot$). The resulting ratios of lifetime to free-fall time, 10 to 30, are the paper's main quantitative result: they imply that the collapse of massive cores is delayed by non-thermal support of turbulent, magnetic, or rotational origin.

Load-bearing premise

The entire prestellar classification rests on the premise, which the paper itself flags in Sect. 7.8, that any massive, actively accreting protostar inside a core would always produce a detectable CO or SiO outflow, so a core without one must be starless; if the accretion-ejection link can silently fail — through a dead zone, a nearly face-on outflow, or an interrupted accretion episode — some of the 12 candidates would actually hide young protostars and the derived lifetimes would shrink.

Editorial extensions

If this is right

  • The 12 cores above 16 $M_\odot$, with masses up to ~54 $M_\odot$, provide a concrete target list for studying the initial conditions of high-mass star formation in detail with follow-up line and continuum observations.
  • High-mass prestellar cores are genuinely rare — about 2% of all ALMA-IMF cores — but they exist up to ~50 $M_\odot$, and they concentrate in the crowded central clumps where high-mass stars are expected to form.
  • The prestellar phase lasts 50–240 kyr, roughly an order of magnitude shorter than the ~1.2 Myr lifetime of low-mass prestellar cores, so high-mass reservoirs must accumulate gas quickly, consistent with inflow and converging-flow pictures rather than slow quasi-static contraction.
  • Ratios of lifetime to free-fall time of 10–30 require non-thermal support; the paper notes that ambipolar-diffusion times are about 30 free-fall times, in the right range to explain the longest-lived cores.
  • The lifetime estimates bracket the true value between the two mass-evolution scenarios: 240 → 120 kyr for 8–16 $M_\odot$ and 100 → 50 kyr for 30–55 $M_\odot$ for constant versus decreasing protostellar envelopes.

Reading between the lines

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

  • Because the paper's own projection analysis allows up to ~7% of outflow detections to be missed, roughly one of the 12 high-mass candidates could still be protostellar; any such misclassification shortens the reported lifetimes in proportion, and this contamination could be measured directly by the high-resolution mid-infrared follow-up the paper proposes.
  • The 10–30 free-fall-time ratio is a quantitative target for magnetized, turbulent collapse simulations: models should reproduce massive cores that persist for many free-fall times without forming any embedded protostar, and can be checked against the reported DCN line widths of 1–2 km s$^{-1}$ with virial parameters near unity.
  • Whether the clump-fed or core-fed scenario applies could be settled within the same sample by comparing envelope masses of young versus evolved protostellar cores: replenished envelopes would favour the clump-fed view and the longer lifetimes, while steadily depleted envelopes favour the core-fed view and the shorter values.
  • The On-Off aperture method is resolution-portable, so applying the same outflow-based classification to surveys at other physical scales or evolutionary stages could map how the prestellar-to-protostellar ratio changes across the high-mass regime.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 6 minor

Summary. This manuscript uses the ALMA-IMF survey of 14 massive protoclusters to search for high-mass prestellar cores. From the 580 gravitationally bound cores of Louvet et al. (2024), the authors isolate 141 cores with mass >8 Msun at an assumed 20 K dust temperature and classify each as protostellar or prestellar using a new automated On-Off aperture method that searches for CO(2-1) and SiO(5-4) high-velocity line wings relative to a DCN-based VLSR, complemented by outflow lobe maps. After rejecting cores whose apparent excess emission can be attributed to neighbouring outflows, 42 candidates without outflow remain; adopting temperature-dependent masses between 20 K and PPMAP values reduces this to 30 likely prestellar cores with M>8 Msun, including 12 above 16 Msun. The authors combine prestellar/protostellar count ratios with an adopted 300 kyr high-mass protostellar lifetime, apply corrections for missing UCHII protostars, and consider two scenarios for envelope-mass evolution, deriving prestellar lifetimes of 120-240 kyr for 8-16 Msun cores and 50-100 kyr for 30-55 Msun cores, corresponding to 10-30 free-fall times. They interpret these large ratios as evidence that collapse is slowed by turbulence, magnetic fields, or rotation.

Significance. If the classification holds, this is the first statistically meaningful sample of high-mass prestellar core candidates from a single survey, and the inferred lifetime relative to free-fall is an important observational constraint on high-mass star formation. The paper's strengths are substantial: the Out-Off outflow method is described in enough detail to be reproduced, per-candidate spectra and outflow maps are shown in Appendix E, the noise is estimated per velocity channel (Sect. 3.2), and the method is validated against visual classifications with 95% agreement in W43 (Sect. 4.3). The lifetime derivation is also not circular: it uses count ratios and an externally adopted protostellar lifetime, and the free-fall comparison is a post-hoc benchmark rather than an input. The main risk to significance is that the prestellar classification relies entirely on outflow non-detection, and the manuscript's own Sect. 7.8 lists physical scenarios in which a highly accreting high-mass protostar could hide inside one of the candidates. A quantitative treatment of these contamination channels is needed before the lifetime and 10-30 free-fall claims can be regarded as secure.

major comments (2)
  1. [Sect. 7.8 (with Sect. 4.2)] The central lifetime and free-fall-ratio claims rest on outflow non-detection being a reliable proxy for the absence of a highly accreting high-mass protostar. Section 4.2 quantifies only the geometric projection false-negative rate (1.75-7.35% for entrained gas already above the 6 km/s threshold), but Section 7.8 itself lists physically distinct failure modes: dead zones suppressing magneto-centrifugal ejection (item 3), cores that are mostly empty with dust concentrated in smaller fragments so that jets escape without interacting with the observed core (item 5), and long accretion outages (item 4). These scenarios would place a strongly accreting object inside a core with no detectable CO/SiO outflow inside the 2700-au beam, and they are not folded into the false-negative budget. The impact is load-bearing: if only a few of the 12 candidates above 16 Msun were misclassified, the prestellar-to-protostellar ratio would drop from roughly 0.44 to about 0.25, reducing the derived lifetimes and free-fall ratios by nearly a factor of two. The manuscript should either place quantitative upper bounds on these contamination channels using independent tracers or literature limits on outflow duty cycle and accretion-ejection coupling, or it should explicitly recast the lifetime and 10-30 free-fall conclusions as upper limits conditional on the assumed outflow-accretion link. As written, the Sect. 7.8 caveat undermines the load-bearing inference rather than resolving it.
  2. [Table 3 and Sect. 4.5/5.1] The sample of 30 likely prestellar cores with M>8 Msun and the robust set of 12 above 16 Msun is threshold-sensitive to the assumed dust temperature. Several Table 3 entries have mass ranges that cross the selection cuts: G008.67 #4 (7.8 Msun, [6.6-8.9]), G333.60 #8 (6.7, [5.4-8.0]), G338.93 #16 (6.5, [4.8-8.2]), W43-MM2 #9 (7.8, [6.7-8.8]), W51-E #28 (7.5, [6.7-8.2]), and W51-IRS2 #22 and #24 (7.6-7.7 with lower limits near 6) can fall below 8 Msun at the PPMAP end; W43-MM2 #12 (16.0, [14.0-18.1]) and W51-IRS2 #8/#9 (17.4, [14.0-20.9] and 16.5, [13.0-19.9]) can fall below 16 Msun. The text partly acknowledges this through the [9-14] range in Sect. 6 and through the black/brown temperature-extreme points in Figs. 8-9, but the lifetime estimates in Table 5 and the abstract are quoted as fixed numbers. The authors should state explicitly which temperature choice defines the 12 robust candidates and should propagate the threshold migration into the quoted lifetime ranges, or present the lifetimes as conditional on the adopted temperature set.
minor comments (6)
  1. [Sect. 1] The text contains a typo: 'Bonnort-Ebert spheres' should read 'Bonnor-Ebert spheres'.
  2. [Throughout] The solar-mass symbol appears inconsistently as 'Md', 'M d', and 'M_sun' in the abstract, Table 3, and body text; please unify the notation (preferably as M_sun).
  3. [Abstract and Sect. 7.5] The abstract quotes '10 to 30 free-fall times,' but Sect. 7.5 and Fig. 10 present values up to about 40 for the constant-envelope (clump-fed) scenario; please align the quoted range with the figures or explicitly state which scenario the abstract range refers to.
  4. [Fig. 5 caption] The caption says the figure displays the 12 most massive PSC candidates, but G333.60 #1A and #1B are combined in a single panel; state this explicitly so the reader knows that 12 objects are shown in 11 panels.
  5. [Table 3] The meaning of the 'Mean masses' and the adopted central mass should be defined in the table header or footnote; the current text refers only to Sect. 4.5, and the relation between the adopted mass and the lower/upper limits is not immediately clear from the table itself.
  6. [Sect. 4.2] The calculation behind the 1.75% and 7.35% geometric false-negative fractions would be easier to verify if the assumed distributions of opening angle, inclination, and maximum outflow velocity were given in a short appendix or explicit formula.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: prestellar lifetimes are derived from independent core-count ratios and an external protostellar lifetime, not from quantities fitted to the same data.

full rationale

The central derivation chain is self-contained. Core masses come from the Louvet et al. (2024) catalog and PPMAP temperatures; outflow classification uses new On-Off spectra and maps; PSC candidates are defined as massive cores with no CO/SiO outflow; and the prestellar lifetime is computed as (N_PSC / N_proto) times an adopted 300 kyr protostellar lifetime taken from external literature (Duarte-Cabral et al. 2013; Mottram et al. 2011). None of these steps defines the target result in terms of itself. The free-fall time is computed independently from measured densities and is used only as a post-hoc benchmark, not as an input to the lifetime estimate. The paper explicitly quantifies geometric false-negative rates and lists alternative scenarios in Sect. 7.8, which is a robustness limitation rather than a circular step. Heavy citation of ALMA-IMF companion papers with overlapping authorship is for data products (catalogs, noise, line cubes) and methodological precedents, not for the load-bearing inference, and the outflow classification is validated against independent prior work with ~95% and ~80% agreement. Thus no circularity is present.

Assumptions & free parameters 6 free parameters · 5 assumptions · 0 invented entities

No new physical entities are introduced. The main 'free' knobs are the adopted protostellar lifetime, the core-to-star efficiency, the dust temperature assumptions, and the detection thresholds; the derived prestellar lifetimes and free-fall ratios scale with these choices.

free parameters (6)
  • protostellar lifetime baseline = 300 ± 100 kyr
    Adopted from literature (Duarte-Cabral et al. 2013; Mottram et al. 2011) to convert prestellar/protostellar number ratios into prestellar lifetimes; the derived prestellar lifetimes scale linearly with this assumption (Sect. 7.1).
  • core-to-star efficiency = 50%
    Assumed to map core mass thresholds (8, 16 M_sun) to final stellar masses and used in the statistical lifetime correction for ionising protostars (Sects. 5.1, 7.3).
  • dust temperature for prestellar cores = 20 K lower limit; PPMAP non-corrected temperature upper limit
    Mass estimates and hence the samples above 8 and 16 M_sun depend directly on the assumed dust temperature; 20 K is described as conservative (Sect. 4.5).
  • outflow detection velocity threshold = 6 km/s
    Chosen as the value above the escape velocity for a 50 M_sun core at 3000 au; all cores are searched above this offset (Sect. 3.4).
  • outflow significance thresholds = 5 sigma, two or more consecutive channels, or sum over up to five channels
    Adopted detection criteria for CO and SiO high-velocity emission (Sect. 3.4).
  • dust opacity index beta = 1.5
    Taken from Louvet et al. (2024) and Pouteau et al. (2022) for mass conversion; affects all core masses (Sect. 4.1).
assumptions (5)
  • domain assumption Outflow non-detection implies no high-mass (highly accreting) protostar in the core
    Central classification premise; alternatives are listed in Sect. 7.8, and the authors present it as the main limitation.
  • domain assumption The 141 cores above 8 M_sun at 20 K form an unbiased, representative census of massive cores in the 14 protoclusters
    Statistical lifetime ratios in Sect. 7 assume this sample is complete and that cores are not systematically missed or merged at the 2700 au smoothing scale (Sects. 2, 4.4).
  • domain assumption Mass-to-flux conversion with opacity index beta = 1.5 and the optically-thick corrected formula of Pouteau et al. (2022)
    All masses and hence all thresholds and density/free-fall values depend on this conversion (Sect. 4.1).
  • standard math Steady-state count ratio equals time ratio: t_PSC / t_proto = N_PSC / N_proto
    Standard statistical lifetime argument, stated in Sect. 7.2, assuming the prestellar and protostellar samples are from the same evolutionary flow.
  • standard math Free-fall time and escape velocity formulas
    Used to compute t_ff from mean densities and the 6 km/s outflow search threshold (Sect. 3.4, Eq. 3).

how reviews work

0 comments
Cite this review

Pith. "Pith review of ALMA-IMF XVII -- Census and lifetime of high-mass prestellar cores in 14 massive protoclusters." pith.science (2026). https://pith.science/paper/5L35TJPX

@misc{pith2026250209426,
  author       = {Pith},
  title        = {Pith review of: ALMA-IMF XVII -- Census and lifetime of high-mass prestellar cores in 14 massive protoclusters},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5L35TJPX}},
  note         = {Machine review of arXiv:2502.09426}
}
abstract

High-mass prestellar cores are extremely rare. The search for such objects has long been hindered by small sample sizes, leading to large uncertainties in their lifetimes and the conditions in which high-mass stars ($> 8\,M_{\odot}$) form. We leverage the large sample ($\sim 580$ cores) detected in the ALMA-IMF survey to identify both protostellar and prestellar cores and estimate their relative lifetimes. We use CO and SiO outflows to identify protostellar cores and introduce a new automated method based on aperture line emission and background subtraction to systematically detect outflows associated with each of the 141 most massive cores. Massive cores that do not drive an outflow in either tracer are classified as prestellar. Our method enables efficient outflow detection with performance comparable to more traditional techniques. We identify 30 likely prestellar cores with $M > 8\,M_{\odot}$, including 12 with $M > 16\,M_{\odot}$, the best candidates for high-mass star precursors. Most of these 12 cores reside in the crowded central regions of protoclusters, where high-mass stars are expected to form. Using prestellar-to-protostellar core ratios and a 300 kyr protostellar lifetime, we estimate prestellar lifetimes of 120 to 240 kyr for $8\,M_{\odot} < M < 16\,M_{\odot}$ and 50 to 100 kyr for $30\,M_{\odot} < M < 55\,M_{\odot}$. These timescales, which depend on different mass reservoir evolution scenarios, significantly exceed the 4 to 15 kyr free-fall time of the cores, suggesting that high-mass cores persist for 10 to 30 free-fall times. This indicates that collapse is slowed by turbulence, magnetic fields, or rotation at or below the observed scale.

Figures

Figures reproduced from arXiv: 2502.09426 by the authors.

Figure 1
Figure 1. Overview of the outflow detection procedure using the On-Off spectra presented in Sect. 3.1. Top Left: Zoom on the continuum core #3 overlaid on the 1.3mm dust continuum map of W43-MM2 (in grey scale). The green ellipses correspond to the FWHM of the extracted source sizes to the continuum emission by getsf. Colored CO (2–1) contours are 10, 20, 40 and 80 in units of σ, with σ = 14.3, 12.6, 10.8, 9.0 mJy beam´1 km s… view at source ↗
Figure 2
Figure 2. Top : Dispersion of the 150 On-Off random selections fluxes in the CO datacube of the region W43-MM2 for channels at velocities of 59.2 km s´1 and 100.1 km s´1 . The mean (µ) and standard deviation (σ), which is assumed for the noise in a respective channel, are indicated in the panel. Middle : Noise spectra of the CO datacube of the region W43-MM2 (in blue, left y axis) overlaid with its mean cube spectra (in orang… view at source ↗
Figure 3
Figure 3. CO (left) and SiO (right) molecular outflows map of the W43-MM2 region overlaid on the 1.3mm dust continuum map (in grey scale). The green ellipses represent the FWHM of the continuum cores convolved by the beam size. Moment 0 contours of the blue-shifted wings are overlaid on the continuum map at low velocity in cyan and high velocity in blue. Moment 0 contours of the red-shifted wings are overlaid on the continuum… view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: Top Left: CO and SiO spectra of the protostellar source #1 of the G328.25 region. On, Off, and On-Off spectra are the black, red, and green spectra respectively. The small subplots on the top left of each spectra are the SNR for On and On-Off spectra, revealing the sig…
Figure 5
Figure 5. Figure 5: CO(2-1) and SiO(5-4) molecular outflow maps centered on the 12 most massive PSC candidates, represented as the center green ellipse with an annulus in each panel (cores #1A and #1B of G333.60 are displayed as one core here, see Sect. 4.4). Ellipses in red are cores cla…
Figure 5
Figure 5. Figure 5: continued. do not affect our classification since none are directly associated with the cores in consideration here. Finally, Armante et al. (2024) classified pre- and protostellar cores using the same CO and SiO lines as this study. Above our mass threshold, we have t…
Figure 6
Figure 6. Figure 6: Second derivative map of G333.60 with a zoom on core #1. The beam of the smoothed continuum map of G333.60 is shown in bottom left. 4.5. Basic properties of the PSC candidates [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]
Figure 7
Figure 7. Figure 7: Mass distribution in function of the size of the total sample of 30 PSC candidates. Blue and red circles correspond to clustered and isolated candidates respectively. Errorbar symbols indicate the whole range of possible mass justified in Sect. 4.5, using 20 K and PPMA…
Figure 8
Figure 8. Figure 8: Left: Weighted histogram of the number of prestellar and protostellar cores per bin and lifetime of the (massive) prestellar phase for each bin (points). The left y-axis indicates the density of number of cores per decade. Prestellar cores are shown in blue bars, proto…
Figure 9
Figure 9. Figure 9: Left: Weighted histogram of the number of prestellar and protostellar cores per bin (left y-axis) and lifetime of the (massive) prestellar phase (right y-axis) for each bin (points). Prestellar cores are shown in blue bars, protostellar cores in red, and free-free sour…
Figure 10
Figure 10. Figure 10: Statistical lifetime of the prestellar phase as a function of the density. Green points represent the lifetimes and densities extracted from the right panel of [PITH_FULL_IMAGE:figures/full_fig_p020_10.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Challenges in probing turbulent and magnetic support in cores: the W43-MM1 protocluster case study

    astro-ph.GA 2026-07 conditional novelty 6.0 of 10

    Simplified virial analyses of W43-MM1 cores overestimate non-thermal support because linewidths include organized motions of 1–3 km/s and surface terms are omitted, producing unexpectedly high stability fractions.

Reference graph

Works this paper leans on

107 extracted references · 61 canonical work pages · cited by 1 Pith paper

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  3. [3]

    H., Stutz , A

    \'A lvarez-Guti \'e rrez , R. H., Stutz , A. M., Sandoval-Garrido , N., et al. 2024, , 689, A74

    2024

  4. [4]

    1993, , 406, 122

    Andre , P., Ward-Thompson , D., & Barsony , M. 1993, , 406, 122

    1993

  5. [5]

    2000, in Protostars and Planets IV, ed

    Andre , P., Ward-Thompson , D., & Barsony , M. 2000, in Protostars and Planets IV, ed. V. Mannings , A. P. Boss , & S. S. Russell , 59

    2000

  6. [6]

    1996, in Astronomical Society of the Pacific Conference Series, Vol

    Anglada , G. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 93, Radio Emission from the Stars and the Sun, ed. A. R. Taylor & J. M. Paredes , 3--14

    1996

  7. [7]

    2024, , 686, A122

    Armante , M., Gusdorf , A., Louvet , F., et al. 2024, , 686, A122

    2024

  8. [8]

    A., Peretto , N., et al

    Avison , A., Fuller , G. A., Peretto , N., et al. 2021, , 645, A142

    2021

Show all 107 references
  1. [9]

    T., Liu , J., Zhang , Q., et al

    Barnes , A. T., Liu , J., Zhang , Q., et al. 2023, , 675, A53

    2023

  2. [10]

    A., Myers , P

    Beichman , C. A., Myers , P. C., Emerson , J. P., et al. 1986, , 307, 337

    1986

  3. [11]

    Bergin , E. A. & Tafalla , M. 2007, , 45, 339

    2007

  4. [12]

    K., et al

    Beuther , H., Schilke , P., Sridharan , T. K., et al. 2002, , 383, 892

    2002

  5. [13]

    2018, , 618, A95

    Bhandare , A., Kuiper , R., Henning , T., et al. 2018, , 618, A95

    2018

  6. [14]

    Blandford , R. D. & Payne , D. G. 1982, , 199, 883

    1982

  7. [15]

    2024, , 687, A163

    Bonfand , M., Csengeri , T., Bontemps , S., et al. 2024, , 687, A163

    2024

  8. [16]

    2023, , 951, 39

    Bonne , L., Bontemps , S., Schneider , N., et al. 2023, , 951, 39

    2023

  9. [17]

    A., Bate , M

    Bonnell , I. A., Bate , M. R., Clarke , C. J., & Pringle , J. E. 2001, , 323, 785

    2001

  10. [18]

    1996, , 311, 858

    Bontemps , S., Andre , P., Terebey , S., & Cabrit , S. 1996, , 311, 858

    1996

  11. [19]

    2010, , 524, A18

    Bontemps , S., Motte , F., Csengeri , T., & Schneider , N. 2010, , 524, A18

    2010

  12. [20]

    2022, , 662, A32

    Bouscasse , L., Csengeri , T., Belloche , A., et al. 2022, , 662, A32

    2022

  13. [21]

    2022, , 665, A140

    Brouillet , N., Despois , D., Molet , J., et al. 2022, , 665, A140

    2022

  14. [22]

    2024, , 961, 4

    Budaiev , N., Ginsburg , A., Jeff , D., et al. 2024, , 961, 4

    2024

  15. [23]

    & Bertout , C

    Cabrit , S. & Bertout , C. 1992, , 261, 274

    1992

  16. [24]

    2022, , 658, A52

    Commer c on , B., Gonz \'a lez , M., Mignon-Risse , R., Hennebelle , P., & Vaytet , N. 2022, , 658, A52

    2022

  17. [25]

    M., et al

    Contreras , Y., Sanhueza , P., Jackson , J. M., et al. 2018, , 861, 14

    2018

  18. [26]

    C., Sanhueza , P., Houde , M., et al

    Cort \'e s , P. C., Sanhueza , P., Houde , M., et al. 2021, , 923, 204

    2021

  19. [27]

    2019, , 632, A57

    Csengeri , T., Belloche , A., Bontemps , S., et al. 2019, , 632, A57

    2019

  20. [28]

    2011, , 740, L5

    Csengeri , T., Bontemps , S., Schneider , N., et al. 2011, , 740, L5

    2011

  21. [29]

    2018, , 617, A89

    Csengeri , T., Bontemps , S., Wyrowski , F., et al. 2018, , 617, A89

    2018

  22. [30]

    2017, , 601, A60

    Csengeri , T., Bontemps , S., Wyrowski , F., et al. 2017, , 601, A60

    2017

  23. [31]

    S., Schuller , F., et al

    Csengeri , T., Urquhart , J. S., Schuller , F., et al. 2014, , 565, A75

    2014

  24. [32]

    2023, , 678, A194

    Cunningham , N., Ginsburg , A., Galv \'a n-Madrid , R., et al. 2023, , 678, A194

    2023

  25. [33]

    L., Cyganowski , C

    Cunningham , N., Lumsden , S. L., Cyganowski , C. J., Maud , L. T., & Purcell , C. 2016, , 458, 1742

    2016

  26. [34]

    J., Brogan , C

    Cyganowski , C. J., Brogan , C. L., Hunter , T. R., et al. 2014, , 796, L2

    2014

  27. [35]

    J., Ilee , J

    Cyganowski , C. J., Ilee , J. D., Brogan , C. L., et al. 2022, , 931, L31

    2022

  28. [36]

    2024, , 687, A217

    Dell'Ova , P., Motte , F., Gusdorf , A., et al. 2024, , 687, A217

    2024

  29. [37]

    2013, , 558, A125

    Duarte-Cabral , A., Bontemps , S., Motte , F., et al. 2013, , 558, A125

    2013

  30. [38]

    2006, , 453, 785

    Ferreira , J., Dougados , C., & Cabrit , S. 2006, , 453, 785

    2006

  31. [39]

    J., Ali , B., et al

    Furlan , E., Fischer , W. J., Ali , B., et al. 2016, , 224, 5

    2016

  32. [40]

    Galv \'a n-Madrid , R., Ginsburg , A., & et al. , . sub.,

  33. [41]

    2010, , 725, 17

    Galv \'a n-Madrid , R., Zhang , Q., Keto , E., et al. 2010, , 725, 17

    2010

  34. [42]

    2022, , 662, A9

    Ginsburg , A., Csengeri , T., Galv \'a n-Madrid , R., et al. 2022, , 662, A9

    2022

  35. [43]

    T., Zhang , Q., & Zapata , L

    Goddi , C., Ginsburg , A., Maud , L. T., Zhang , Q., & Zapata , L. A. 2020, , 905, 25

    2020

  36. [44]

    R., & Pineau Des For \^e ts , G

    Gusdorf , A., Cabrit , S., Flower , D. R., & Pineau Des For \^e ts , G. 2008, , 482, 809

    2008

  37. [45]

    A., Megeath , S

    Gutermuth , R. A., Megeath , S. T., Myers , P. C., et al. 2009, , 184, 18

    2009

  38. [46]

    & Omukai , K

    Hosokawa , T. & Omukai , K. 2009, , 691, 823

    2009

  39. [47]

    Jessop , N. E. & Ward-Thompson , D. 2000, , 311, 63

    2000

  40. [48]

    & van Moorsel , G

    Jorsater , S. & van Moorsel , G. A. 1995, , 110, 2037

    1995

  41. [49]

    2007, , 666, 976

    Keto , E. 2007, , 666, 976

    2007

  42. [50]

    & Kuiper , R

    K \"o lligan , A. & Kuiper , R. 2018, , 620, A182

    2018

  43. [51]

    C., Caselli , P., et al

    Kong , S., Tan , J. C., Caselli , P., et al. 2017, , 834, 193

    2017

  44. [52]

    2015, , 584, A91

    K \"o nyves , V., Andr \'e , P., Men'shchikov , A., et al. 2015, , 584, A91

    2015

  45. [53]

    R., Klein , R

    Krumholz , M. R., Klein , R. I., & McKee , C. F. 2007, , 656, 959

    2007

  46. [54]

    Lada , C. J. & Adams , F. C. 1992, , 393, 278

    1992

  47. [55]

    M., Schmiedeke , A., et al

    Launhardt , R., Stutz , A. M., Schmiedeke , A., et al. 2013, , 551, A98

    2013

  48. [56]

    2024, Nature Astronomy, 8, 472

    Li , S., Sanhueza , P., Beuther , H., et al. 2024, Nature Astronomy, 8, 472

    2024

  49. [57]

    2020, , 903, 119

    Li , S., Sanhueza , P., Zhang , Q., et al. 2020, , 903, 119

    2020

  50. [58]

    2021, , 653, A157

    Louvet , F., Hennebelle , P., Men'shchikov , A., et al. 2021, , 653, A157

    2021

  51. [59]

    2019, , 622, A99

    Louvet , F., Neupane , S., Garay , G., et al. 2019, , 622, A99

    2019

  52. [60]

    2024, , 690, A33

    Louvet , F., Sanhueza , P., Stutz , A., et al. 2024, , 690, A33

    2024

  53. [61]

    2024, , 961, L35

    Mai , X., Liu , T., Liu , X., et al. 2024, , 961, L35

    2024

  54. [62]

    N., Sakurai , Y., & Hosokawa , T

    Matsushita , Y., Machida , M. N., Sakurai , Y., & Hosokawa , T. 2017, , 470, 1026

    2017

  55. [63]

    T., Moore , T

    Maud , L. T., Moore , T. J. T., Lumsden , S. L., et al. 2015, , 453, 645

    2015

  56. [64]

    McKee , C. F. & Tan , J. C. 2003, , 585, 850

    2003

  57. [65]

    2021, , 649, A89

    Men'shchikov , A. 2021, , 649, A89

    2021

  58. [66]

    2021, , 656, A85

    Mignon-Risse , R., Gonz \'a lez , M., & Commer c on , B. 2021, , 656, A85

    2021

  59. [67]

    2019, , 626, A132

    Molet , J., Brouillet , N., Nony , T., et al. 2019, , 626, A132

    2019

  60. [68]

    2023, , 950, 148

    Morii , K., Sanhueza , P., Nakamura , F., et al. 2023, , 950, 148

    2023

  61. [69]

    1998, , 336, 150

    Motte , F., Andre , P., & Neri , R. 1998, , 336, 150

    1998

  62. [70]

    2022, , 662, A8

    Motte , F., Bontemps , S., Csengeri , T., et al. 2022, , 662, A8

    2022

  63. [71]

    2018 a , , 56, 41

    Motte , F., Bontemps , S., & Louvet , F. 2018 a , , 56, 41

    2018

  64. [72]

    2007, , 476, 1243

    Motte , F., Bontemps , S., Schilke , P., et al. 2007, , 476, 1243

    2007

  65. [73]

    2018 b , Nature Astronomy, 2, 478

    Motte , F., Nony , T., Louvet , F., et al. 2018 b , Nature Astronomy, 2, 478

    2018

  66. [74]

    2010, , 518, L77

    Motte , F., Zavagno , A., Bontemps , S., et al. 2010, , 518, L77

    2010

  67. [75]

    C., Hoare , M

    Mottram , J. C., Hoare , M. G., Davies , B., et al. 2011, , 730, L33

    2011

  68. [76]

    C., Linke , R

    Myers , P. C., Linke , R. A., & Benson , P. J. 1983, , 264, 517

    1983

  69. [77]

    D., Motte , F., et al

    Nguyen-Luong , Q., Anderson , L. D., Motte , F., et al. 2017, , 844, L25

    2017

  70. [78]

    2024, , 687, A84

    Nony , T., Galv \'a n-Madrid , R., Brouillet , N., et al. 2024, , 687, A84

    2024

  71. [79]

    2023, , 674, A75

    Nony , T., Galv \'a n-Madrid , R., Motte , F., et al. 2023, , 674, A75

    2023

  72. [80]

    2018, , 618, L5

    Nony , T., Louvet , F., Motte , F., et al. 2018, , 618, L5

    2018

  73. [81]

    2020, , 636, A38

    Nony , T., Motte , F., Louvet , F., et al. 2020, , 636, A38

    2020

  74. [82]

    A., Sanhueza , P., Chen , H.-R

    Olguin , F. A., Sanhueza , P., Chen , H.-R. V., et al. 2023, , 959, L31

    2023

  75. [83]

    A., Sanhueza , P., Ginsburg , A., et al

    Olguin , F. A., Sanhueza , P., Ginsburg , A., et al. 2022, , 929, 68

    2022

  76. [84]

    & Henning , T

    Ossenkopf , V. & Henning , T. 1994, , 291, 943

    1994

  77. [85]

    & Nordlund , A

    Padoan , P. & Nordlund , A . 2002, , 576, 870

    2002

  78. [86]

    A., Duarte-Cabral , A., et al

    Peretto , N., Fuller , G. A., Duarte-Cabral , A., et al. 2013, , 555, A112

    2013

  79. [87]

    2020, , 496, 3482

    Peretto , N., Rigby , A., Andr \'e , P., et al. 2020, , 496, 3482

    2020

  80. [88]

    S., et al

    Peters , T., Banerjee , R., Klessen , R. S., et al. 2010, , 711, 1017

    2010

  81. [89]

    2022, , 664, A26

    Pouteau , Y., Motte , F., Nony , T., et al. 2022, , 664, A26

    2022

  82. [90]

    2023, , 674, A76

    Pouteau , Y., Motte , F., Nony , T., et al. 2023, , 674, A76

    2023

  83. [91]

    2022, , 936, 169

    Redaelli , E., Bovino , S., Sanhueza , P., et al. 2022, , 936, 169

    2022

  84. [92]

    2018, , 609, A101

    S \'a nchez-Monge , \'A ., Schilke , P., Ginsburg , A., Cesaroni , R., & Schmiedeke , A. 2018, , 609, A101

    2018

  85. [93]

    2019, , 886, 102

    Sanhueza , P., Contreras , Y., Wu , B., et al. 2019, , 886, 102

    2019

  86. [94]

    M., Padovani , M., et al

    Sanhueza , P., Girart , J. M., Padovani , M., et al. 2021, , 915, L10

    2021

  87. [95]

    M., Zhang , Q., et al

    Sanhueza , P., Jackson , J. M., Zhang , Q., et al. 2017, , 841, 97

    2017

  88. [96]

    2023, Nature Astronomy, 7, 546

    Schneider , N., Bonne , L., Bontemps , S., et al. 2023, Nature Astronomy, 7, 546

    2023

  89. [97]

    2010, , 520, A49

    Schneider , N., Csengeri , T., Bontemps , S., et al. 2010, , 520, A49

    2010

  90. [98]

    Stutz , A. M. & Gould , A. 2016, , 590, A2

    2016

  91. [99]

    T., & Caselli , P

    Tan , J., Beltrán , M. T., & Caselli , P. e. a. 2014, 149

    2014

  92. [100]

    C., Kong , S., Butler , M

    Tan , J. C., Kong , S., Butler , M. J., Caselli , P., & Fontani , F. 2013, , 779, 96

    2013

  93. [101]

    C., Kong , S., Zhang , Y., et al

    Tan , J. C., Kong , S., Zhang , Y., et al. 2016, , 821, L3

    2016

  94. [102]

    Tanaka , K. E. I., Tan , J. C., & Zhang , Y. 2016, , 818, 52

    2016

  95. [103]

    2017, , 602, A77

    Tig \'e , J., Motte , F., Russeil , D., et al. 2017, , 602, A77

    2017

  96. [104]

    Towner , A. P. M., Ginsburg , A., Dell'Ova , P., et al. 2024, , 960, 48

    2024

  97. [105]

    2014, , 439, 3275

    Wang , K., Zhang , Q., Testi , L., et al. 2014, , 439, 3275

    2014

  98. [106]

    2024, , 270, 9

    Xu , F., Wang , K., Liu , T., et al. 2024, , 270, 9

    2024

  99. [107]

    Yorke , H. W. & Sonnhalter , C. 2002, , 569, 846

    2002

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.