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REVIEW 2 major objections 5 minor 178 references

In Orion, turbulence is dissipated at the fiber scale before cores form, with small high-shear patches near dense fibers doing most of the work.

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2026-07-11 07:54 UTC pith:DZXIETQW

load-bearing objection Solid multi-region ALMA HNC maps that put the transition-to-coherence at fiber scales and quantify high-shear dissipation layers next to N2H+ fibers. the 2 major comments →

arxiv 2607.05156 v1 pith:DZXIETQW submitted 2026-07-06 astro-ph.GA

Emergence of high-mass stars in complex fiber networks (EMERGE) VI. Turbulence dissipation and the formation of dense fibers

F. Bonanomi , A. Hacar , A. Socci , S. Heigl This is my paper
classification astro-ph.GA
keywords molecular cloudsfibersturbulence dissipationvelocity gradientsstar formationOrionHNCN2H+
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Molecular clouds are turbulent, yet the dense cores that form stars are quiet and subsonic. This paper asks where that transition to coherence actually happens. Using matched high-resolution maps of diffuse gas (HNC) and dense gas (N2H+) across five Orion regions, it finds that the diffuse material around dense fibers remains supersonic (typical Mach number ~2.9), while the gas inside the fibers is already quiescent. Statistical maps of velocity gradients then show that the energy is dumped in compact high-shear patches (gradients above 10 km s^{-1} pc^{-1}, sizes 0.1–0.3 pc) that sit right next to the dense fibers. Despite filling only a small fraction of the map, those patches account for most of the measured dissipation. The implication is that fibers, not cores, are the first coherent structures to emerge from the turbulent cascade.

Core claim

In Orion the transition from turbulent, diffuse gas to coherent, subsonic gas occurs at the fiber level: high-shear regions of 0.1–0.3 pc size located next to dense fibers dissipate the bulk of the turbulent energy before cores form.

What carries the argument

Centroid-velocity-gradient (and increment) PDFs evaluated at 0.04 pc lag: non-Gaussian wings above |∇V_lsr| ≥ 10 km s^{-1} pc^{-1} flag intermittent high-shear patches whose integrated contribution f_ε exceeds 30–60 % of the total dissipation.

Load-bearing premise

That the non-Gaussian wings of the velocity-gradient PDFs cleanly mark dissipative intermittency rather than residual multi-component blending, outflows, or large-scale feedback shear.

What would settle it

A map of an identical region in an optically thin isotopologue or a higher-resolution tracer that shows the high-gradient patches either disappearing or relocating away from the dense fibers would falsify the identification of those patches as the main dissipation sites.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Core properties (mass, velocity dispersion) are largely inherited from the parental fiber rather than set by local dissipation at the core scale.
  • Fiber formation models must include intermittent, localized dissipation rather than uniform cascading.
  • High-shear patches should appear as elevated vorticity or enhanced dissipation signatures in future multi-tracer or MHD simulations of the same regions.
  • Surveys that resolve only cores will systematically miss the scale at which coherence first appears.

Where Pith is reading between the lines

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

  • If the same high-shear morphology appears in lower-mass clouds outside Orion, the fiber-scale transition may be universal rather than environment-dependent.
  • The filling-factor versus dissipation-fraction numbers supply a quantitative target for sub-grid turbulence models that currently assume space-filling dissipation.
  • A direct comparison of these HNC gradients with simultaneous NH3 or continuum maps could test whether the shear patches coincide with the sharpest density jumps.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. This EMERGE Paper VI uses high-resolution (4.5 arcsec) ALMA+IRAM-30m HNC(1-0) mosaics of five Orion star-forming regions to characterize the kinematics of lukewarm, diffuse gas (N(H2)~5e21 cm^-2) surrounding dense fibers previously identified in N2H+. The diffuse gas is systematically more turbulent (median Ms~2.9) than the subsonic dense gas inside fibers (Ms~0.74). Through centroid-velocity increments and newly applied velocity-gradient statistics at lag L=0.04 pc, the authors identify high-shear regions (|∇V_lsr|≥10 km s^-1 pc^-1) as non-Gaussian wings of the PDFs; these form elongated 0.1–0.3 pc features near dense-gas contours, occupy fs≲20% of the maps, yet contribute f_ε>30–60% of the integrated ∇V^2 budget (Table 3). The central claim is that in Orion the transition to coherence occurs at the fiber scale, with turbulence dissipated during fiber formation rather than at core scales.

Significance. If the result holds, it reframes the classical transition-to-coherence picture (Goodman et al. 1998; Pineda et al. 2010) by placing the dissipative step at fiber rather than core scales, with direct implications for how cores inherit subsonic conditions from parental filaments. Strengths include a homogeneous multi-region sample spanning low- to high-mass regimes, quantitative filling-factor and dissipation-fraction estimates (Table 3), and multi-method cross-checks (single- vs multi-component fits, moments, box gradients vs annuli vs classical increments in Appendices B–C) that make the high-shear identification re-examinable by the reader. The work is a natural and well-executed extension of the EMERGE series and of prior intermittency studies (Pety & Falgarone 2003; Hily-Blant et al.).

major comments (2)
  1. [Sect. 5.2.2 / Figs. 7, 10] Sect. 5.2.2 and Figs. 7/10: The claim that high-shear features are systematically associated with dense fibers (and therefore that dissipation occurs during fiber formation) rests on visual proximity to N2H+ 3σ contours. No quantitative distance metric, nearest-neighbor statistic, or null test against random placement is provided. A simple contour-distance or fiber-spine offset distribution (even for the subset of fibers already catalogued in Paper III) would make the spatial association load-bearing rather than qualitative.
  2. [Sect. 5.3, Eq. (4), Table 3] Sect. 5.3, Eq. (4) and Table 3: f_ε is defined as the fraction of ∑(∇V_lsr)^2 residing in high-shear pixels. This is a standard proxy following Pety & Falgarone (2003), but the manuscript should state explicitly the assumptions under which ∇V^2 traces local dissipation (projection/LOS averaging, that high-shear is not dominated by unresolved multi-component jumps or large-scale shear). Without that caveat, the numerical claim f_ε>30–60% can be over-read as a direct energy-dissipation fraction.
minor comments (5)
  1. [Sect. 4.1] Sect. 4.1 / Fig. 5: Kinetic temperatures are taken from 30-arcsec IRAM maps and assumed constant inside each IRAM pixel when computing Ms at 4.5-arcsec resolution. The paper notes Ms ∝ 1/√TK, but a short quantitative estimate of the possible Ms bias from unresolved T gradients (especially near feedback edges) would help the reader.
  2. [Abstract / Conclusions] Abstract and Conclusions: Column density for HNC is given as ~5e21 cm^-2 in the abstract but as N(H2)≳10^22 in Conclusion point 1; align the wording.
  3. [Sect. 4.2] Fig. 6 and Sect. 4.2: The WISE 12 µm cut used to isolate feedback in the Flame Nebula is effective; a brief note on why analogous cuts failed in the other targets (background levels) is already present but could be moved earlier so Table 2 upper-limit caveats are clearer.
  4. [Sect. 5.2.2 / App. C] Appendix C is thorough and valuable; consider adding a one-sentence pointer in the main text of Sect. 5.2.2 that the three estimators recover the same ±10 km s^-1 pc^-1 threshold and the same spatial features.
  5. [Keywords / Tables] Typographical: 'Massive star-formation —- ISM' (double dash) in keywords; occasional missing spaces before units in tables.

Circularity Check

1 steps flagged

No significant circularity: HNC kinematics, gradient statistics and dissipation fractions are independent measurements; prior EMERGE fiber catalogue is used only as a spatial reference.

specific steps
  1. self citation load bearing [Sect. 5.1, Table 2, Fig. 4]
    "Paper III identified a total of 76 fibers within our maps (152 including OMC-1 and OMC-2), where the majority of these structures shows non-thermal motions within the sonic regime (Ms(N2H+)∼0.74, see Table 2 and Fig. 4). This statistical behaviour would agree with fibers being the first structures formed out of the turbulent cascade in the regions sampled by our survey."

    The subsonic character of the dense fibers is taken from Socci et al. (2024a,b) (same team). The citation is load-bearing for the comparative claim ‘fibers are the first coherent structures’, yet the new HNC analysis (linewidths, Ms maps, gradient PDFs, fϵ) is independent of that catalogue; the fibers are used only as a spatial reference. This is ordinary self-citation, not a definitional reduction.

full rationale

The paper’s central claim (transition to coherence at fiber scales; high-shear HNC features as major dissipators) rests on new ALMA+IRAM-30m HNC (1-0) maps, single-component Gaussian fits, and three independent estimators of velocity increments/gradients (box, annulus, classical lag). The N2H+ fiber catalogue and subsonic Ms values are imported from earlier EMERGE papers by the same team, but they serve only as a spatial mask and a comparison distribution; none of the HNC-derived quantities (Ms(HNC)=2.9, |∇Vlsr| threshold, fs, fϵ) is algebraically forced by those prior results. The dissipation fraction fϵ is a direct sum of observed ∇V^{2} over the high-shear mask versus the whole map; it is not a fitted parameter renamed as a prediction. Multi-component blending, outflows and feedback are stress-tested inside the paper (App. B–C) rather than assumed away. The single minor self-citation load is therefore non-circular and scores 1.

Axiom & Free-Parameter Ledger

3 free parameters · 4 axioms · 0 invented entities

The claim rests on standard ISM tracer assumptions, Kolmogorov intermittency phenomenology, and a small set of analysis choices (lag, threshold, single-component fit). No new physical entities are postulated; free parameters are analysis scales rather than physical constants fitted to force the result.

free parameters (3)
  • lag L for increments/gradients = 0.04 pc
    Fixed at 0.04 pc (≈4.5 beams); results weaken at 0.06 pc, so the chosen scale is load-bearing for detecting non-Gaussian wings.
  • high-shear threshold = 10 km s⁻¹ pc⁻¹
    Set at |∇V| ≥ 10 km s⁻¹ pc⁻¹ (≈3σ of the Gaussian core of the PDF); defines the intermittent sample used for f_s and f_ϵ.
  • minimum pixel count for gradient fit = 100 (gradients) / 20 (increments)
    100 Nyquist pixels (or 20 for increments) required for a valid measurement; affects which map positions enter the statistics.
axioms (4)
  • domain assumption HNC (1-0) is an optically thin-to-moderate tracer of lukewarm diffuse gas at N(H2) ∼ 5×10²¹ cm⁻² and n ∼ few ×10³ cm⁻³
    Invoked throughout Sect. 2–3 and used to interpret all kinematic maps; supported by RADEX and literature but not re-derived here.
  • domain assumption Non-Gaussian wings of centroid-velocity-increment/gradient PDFs at small lags are the observational signature of intermittent turbulence dissipation
    Taken from Falgarone, Lis, Pety, Hily-Blant literature and applied in Sect. 5.2; the paper does not re-derive the link from first principles.
  • ad hoc to paper Single-component Gaussian fits provide usable upper limits on linewidth and unbiased centroids for gradient analysis
    Adopted in Sect. 4 after multi-component tests; Appendix B shows residual multi-component spectra exist (especially Flame Nebula) but are argued not to dominate the high-shear sample.
  • ad hoc to paper Kinetic temperature can be taken as constant inside each 30-arcsec IRAM pixel when computing Mach numbers at 4.5-arcsec resolution
    Explicitly stated in Sect. 4.1; temperature variations affect Ms only weakly (∝1/√T) but remain an approximation.

pith-pipeline@v1.1.0-grok45 · 41800 in / 2832 out tokens · 25992 ms · 2026-07-11T07:54:42.177954+00:00 · methodology

0 comments
read the original abstract

(Abridged) The turbulent cascade naturally generates a hierarchy of filaments within molecular clouds, with fibers suggested to be the first (tran-)sonic components formed out of it. We aim to investigate the diffuse gas kinematics and its interaction with the dense gas composing fibers using HNC as molecular tracer. We use high-resolution (4.5" or 2000au) large-scale ALMA+IRAM-30m mosaics to survey five star-forming regions in Orion, as part of the EMERGE Early ALMA Survey covering a wide range of stellar activity, cloud morphology, and evolutionary stages. We observe our targets in HNC(1-0) as probe of diffuse gas in the regions and compare it to the N2H+(1-0) emission tracing the dense gas. Our high resolution observations reveal that HNC traces lukewarm, diffuse ($\sim5\times10^{21}$ cm$^{-2}$) material around dense fibers. The properties of the diffuse gas appear to be similar across our sample, despite the wide range of different environments. Compared to the quiescent and subsonic gas inside fibers, the diffuse gas is, however, more turbulent ($M_\text{s}=2.9$). Understanding the dissipation process is crucial to mark the transition between the dense subsonic gas and diffuse turbulent material occurs. We investigated the turbulence dissipation through the statistical analysis of the HNC velocity gradients. We identified high-shear regions showing higher gradients with $\nabla V_{lsr}\ge10~\mathrm{km~s^{-1}~pc^{-1}}$ concentrated in small features of 0.1-0.3 pc in size located near the dense gas. These high-shear structures appear to be major contributors of the turbulence dissipation in our targets. Our results suggest that in Orion the transition to coherence occurs at the fiber level, as suggested by the turbulence being effectively dissipated before the formation of cores and during the formation of these first dense structures.

Figures

Figures reproduced from arXiv: 2607.05156 by A. Hacar, A. Socci, F. Bonanomi, S. Heigl.

Figure 1
Figure 1. Figure 1: Maps in OMC-3, the representative showcase of our sample. From left to right we plot integrated intensity I(N [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Distribution of the linewidth for all the five regions in our sample. Histogram (left; in logarithmic scale) and cumulative [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: HNC (1-0) linewidth maps of the five star-forming regions in the EMERGE Early ALMA Survey at 4.5 arcsec resolution [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of the Mach number for all the five regions in our sample. Histogram (left) and cumulative distribution (right) of [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Mach number (M = σnt/cs) maps of the five star-forming regions observed in HNC (1-0) in the EMERGE Early ALMA Survey at 4.5 arcsec resolution. The gray contours show the N2H + (1-0) integrated intensity above 3σ (the N2H + maps are visible in Paper III). Symbols are similar to those in [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Maps of the Flame Nebula. From left to right: WISE 12µ [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: HNC (1-0) Vlsr increment maps of the five star-forming regions in the EMERGE Early ALMA Survey at 4.5 arcsec resolution with ALMA+IRAM-30m. The gray contours show the N2H + (1-0) integrated intensity above 3σ (the N2H + maps are visible in Paper III). The red contours display the high velocity gradient regions identified in [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Histogram of the velocity increments evaluated along the [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Histogram of the projection of the increments along the [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: HNC (1-0) Vlsr gradient maps of the five star-forming regions in the EMERGE Early ALMA Survey at 4.5 arcsec resolution with ALMA+IRAM-30m. The gray contours show the N2H + (1-0) integrated intensity above 3σ (the N2H + maps are visible in Paper III). The red contours display the high velocity gradient regions identified in [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Histogram of the projection of the gradient along the [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Histogram of the projection of the gradient along the [PITH_FULL_IMAGE:figures/full_fig_p016_12.png] view at source ↗
Figure 10
Figure 10. Figure 10: These points extracted from the non-Gaussian wings [PITH_FULL_IMAGE:figures/full_fig_p017_10.png] view at source ↗
Figure 1
Figure 1. Figure 1: Beam sizes and scale bars are placed in the bottom right corner. The maps of the remaining targets in the sample are shown [PITH_FULL_IMAGE:figures/full_fig_p029_1.png] view at source ↗

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Reference graph

Works this paper leans on

178 extracted references · 80 canonical work pages · 69 internal anchors

  1. [1]

    ALminer: ALMA archive mining and visualization toolkit

  2. [2]

    , year = 2001, month = jan, volume =

    Internal structure of a cold dark molecular cloud inferred from the extinction of background starlight. , year = 2001, month = jan, volume =

    2001

  3. [3]

    The mass function of dense molecular cores and the origin of the IMF

    The mass function of dense molecular cores and the origin of the IMF. , keywords =. doi:10.1051/0004-6361:20066389 , archivePrefix =. astro-ph/0612126 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20066389

  4. [4]

    Orion revisited. I. The massive cluster in front of the Orion nebula cluster. , keywords =. doi:10.1051/0004-6361/201220119 , archivePrefix =. 1209.3787 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220119

  5. [5]

    , keywords =

    From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey. , keywords =. doi:10.1051/0004-6361/201014666 , archivePrefix =. 1005.2618 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201014666

  6. [6]

    Protostars and Planets VI , year = 2014, editor =

    From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a New Paradigm for Star Formation. Protostars and Planets VI , year = 2014, editor =. doi:10.2458/azu_uapress_9780816531240-ch002 , archivePrefix =. 1312.6232 , primaryClass =

    Pith/arXiv arXiv doi:10.2458/azu_uapress_9780816531240-ch002 2014

  7. [7]

    Journal of Fluid Mechanics , keywords =

    High-order velocity structure functions in turbulent shear flows. Journal of Fluid Mechanics , keywords =. doi:10.1017/S0022112084000513 , adsurl =

    doi:10.1017/s0022112084000513

  8. [8]

    , year = 2001, month = oct, volume =

    Turbulent flows and intermittency in laboratory experiments. , year = 2001, month = oct, volume =. doi:10.1016/S0032-0633(01)00059-9 , adsurl =

    work page doi:10.1016/s0032-0633(01)00059-9 2001

  9. [9]

    , keywords =

    Characterizing interstellar filaments with Herschel in IC 5146. , keywords =. doi:10.1051/0004-6361/201116596 , archivePrefix =. 1103.0201 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201116596

  10. [10]

    , keywords =

    Characterizing the properties of nearby molecular filaments observed with Herschel. , keywords =. doi:10.1051/0004-6361/201832725 , archivePrefix =. 1810.00721 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201832725

  11. [11]

    Handbook of Star Forming Regions, Volume I , year = 2008, editor =

    Overview of the Orion Complex. Handbook of Star Forming Regions, Volume I , year = 2008, editor =. doi:10.48550/arXiv.0812.0046 , adsurl =

    Pith/arXiv arXiv doi:10.48550/arxiv.0812.0046 2008

  12. [12]

    , year = 1907, month = apr, volume =

    On a nebulous groundwork in the constellation Taurus. , year = 1907, month = apr, volume =. doi:10.1086/141434 , adsurl =

    work page doi:10.1086/141434 1907

  13. [13]

    Coherent Dense Cores. I. NH _ 3 Observations. , keywords =. doi:10.1086/306044 , adsurl =

    doi:10.1086/306044

  14. [14]

    The Theory of Homogeneous Turbulence

  15. [15]

    Quantifying Observational Projection Effects Using Molecular Cloud Simulations

    Quantifying Observational Projection Effects Using Molecular Cloud Simulations. , keywords =. doi:10.1088/0004-637X/777/2/173 , archivePrefix =. 1310.1929 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/777/2/173 1929

  16. [16]

    , keywords =

    A Survey for Dense Cores in Dark Clouds. , keywords =. doi:10.1086/191365 , adsurl =

    doi:10.1086/191365

  17. [17]

    , keywords =

    Cold Dark Clouds: The Initial Conditions for Star Formation. , keywords =. doi:10.1146/annurev.astro.45.071206.100404 , archivePrefix =. 0705.3765 , primaryClass =

    doi:10.1146/annurev.astro.45.071206.100404

  18. [18]

    Emergence of high-mass stars in complex fiber networks (EMERGE). II. The need for data combination in ALMA observations. , keywords =. doi:10.1051/0004-6361/202348920 , archivePrefix =. 2405.09290 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202348920

  19. [19]

    ALMA-IMF. IV. A comparative study of the main hot cores in W43-MM1: Detection, temperature, and molecular composition. , keywords =. doi:10.1051/0004-6361/202243669 , archivePrefix =. 2207.03537 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202243669

  20. [20]

    The Orion OB1 association. I. Stellar content. , keywords =. doi:10.48550/arXiv.astro-ph/9403051 , archivePrefix =. astro-ph/9403051 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9403051

  21. [21]

    An introduction to radio astronomy, 4th edition

  22. [22]

    , keywords =

    CASA, the Common Astronomy Software Applications for Radio Astronomy. , keywords =. doi:10.1088/1538-3873/ac9642 , archivePrefix =. 2210.02276 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/1538-3873/ac9642

  23. [23]

    Dense Cores in Dark Clouds. XIV. N _ 2 H ^ + (1-0) Maps of Dense Cloud Cores. , keywords =. doi:10.1086/340195 , archivePrefix =. astro-ph/0202173 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/340195

  24. [24]

    The Central 1000 au of a Pre-stellar Core Revealed with ALMA. I. 1.3 mm Continuum Observations. , keywords =. doi:10.3847/1538-4357/ab0700 , archivePrefix =. 1902.05299 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab0700 1902

  25. [25]

    , keywords =

    Galactic Stellar and Substellar Initial Mass Function. , keywords =. doi:10.1086/376392 , archivePrefix =. astro-ph/0304382 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/376392

  26. [26]

    Filamentary Accretion Flows in the Infrared Dark Cloud G14.225-0.506 Revealed by ALMA

    Filamentary Accretion Flows in the Infrared Dark Cloud G14.225-0.506 Revealed by ALMA. , keywords =. doi:10.3847/1538-4357/ab0f3e , archivePrefix =. 1903.04376 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab0f3e 1903

  27. [27]

    Droplets. I. Pressure-dominated Coherent Structures in L1688 and B18. , keywords =. doi:10.3847/1538-4357/ab1a40 , archivePrefix =. 1809.10223 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1a40

  28. [28]

    Filament Accretion and Fragmentation in the Perseus Molecular Cloud

    Filament Accretion and Fragmentation in the Perseus Molecular Cloud. , keywords =. doi:10.3847/1538-4357/ad88e8 , archivePrefix =. 2410.16372 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad88e8

  29. [29]

    Transition from Coherent Cores to Surrounding Cloud in L1688

    Transition from coherent cores to surrounding cloud in L1688. , keywords =. doi:10.1051/0004-6361/202039897 , archivePrefix =. 2102.06459 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039897

  30. [30]

    Filamentary fragmentation in a turbulent medium

    Filamentary fragmentation in a turbulent medium. , keywords =. doi:10.1093/mnras/stx637 , archivePrefix =. 1703.04473 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx637

  31. [31]

    Synthetic C$^{18}$O observations of fibrous filaments: the problems of mapping from PPV to PPP

    Synthetic C ^ 18 O observations of fibrous filaments: the problems of mapping from PPV to PPP. , keywords =. doi:10.1093/mnras/sty1675 , archivePrefix =. 1806.08564 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1675

  32. [32]

    10.3, ver

    ALMA Technical Handbook, ALMA Doc. 10.3, ver. 1.0

  33. [33]

    Fourier Plane Image Combination by Feathering

    Fourier Plane Image Combination by Feathering. , keywords =. doi:10.1088/1538-3873/aa793f , archivePrefix =. 1707.02272 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/aa793f

  34. [34]

    ALMA-IMF. VII. First release of the full spectral line cubes: Core kinematics traced by DCN J = (3 - 2). , keywords =. doi:10.1051/0004-6361/202245429 , archivePrefix =. 2306.14710 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202245429

  35. [35]

    ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters. , keywords =. doi:10.3847/1538-4365/ad029c , archivePrefix =. 2310.13872 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ad029c

  36. [36]

    An ALMA Search for Substructure, Fragmentation, and Hidden Protostars in Starless Cores in Chamaeleon I

    An ALMA Search for Substructure, Fragmentation, and Hidden Protostars in Starless Cores in Chamaeleon I. , keywords =. doi:10.3847/0004-637X/823/2/160 , archivePrefix =. 1604.04027 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/823/2/160

  37. [37]

    ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP). II. Survey Overview: A First Look at 1.3 mm Continuum Maps and Molecular Outflows. , keywords =. doi:10.3847/1538-4365/abba26 , archivePrefix =. 2010.14507 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/abba26 2010

  38. [38]

    , keywords =

    Interstellar Turbulence I: Observations and Processes. , keywords =. doi:10.1146/annurev.astro.41.011802.094859 , archivePrefix =. astro-ph/0404451 , primaryClass =

    Pith/arXiv arXiv doi:10.1146/annurev.astro.41.011802.094859

  39. [39]

    Astronomical Data Analysis Software and Systems XXIX , year = 2020, editor =

    The CASA Software for Radio Astronomy: Status Update from ADASS 2019. Astronomical Data Analysis Software and Systems XXIX , year = 2020, editor =. doi:10.48550/arXiv.1912.09437 , archivePrefix =. 1912.09437 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1912.09437 2019

  40. [40]

    , keywords =

    The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes. , keywords =. doi:10.1088/0067-0049/181/2/321 , archivePrefix =. 0811.1059 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0067-0049/181/2/321

  41. [41]

    , keywords =

    A Signature of the Intermittency of Interstellar Turbulence: The Wings of Molecular Line Profiles. , keywords =. doi:10.1086/169068 , adsurl =

    work page doi:10.1086/169068

  42. [42]

    , keywords =

    The small-scale density and velocity structure of quiescent molecular clouds. , keywords =

  43. [43]

    The CARMA-NRO Orion Survey: Statistical Signatures of Feedback in the Orion A Molecular Cloud

    The CARMA-NRO Orion Survey: Statistical Signatures of Feedback in the Orion A Molecular Cloud. , keywords =. doi:10.3847/1538-4357/ab0e7d , archivePrefix =. 1903.05104 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab0e7d 1903

  44. [44]

    Nature Astronomy , keywords =

    The sonic scale of interstellar turbulence. Nature Astronomy , keywords =. doi:10.1038/s41550-020-01282-z , archivePrefix =. 2011.06238 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/s41550-020-01282-z 2011

  45. [45]

    , keywords =

    The Green Bank Ammonia Survey: First Results of NH _ 3 Mapping of the Gould Belt. , keywords =. doi:10.3847/1538-4357/aa6d58 , archivePrefix =. 1704.06318 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aa6d58

  46. [46]

    , keywords =

    The Herschel Orion Protostar Survey: Spectral Energy Distributions and Fits Using a Grid of Protostellar Models. , keywords =. doi:10.3847/0067-0049/224/1/5 , archivePrefix =. 1602.07314 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/0067-0049/224/1/5

  47. [47]

    An analytic formalism to describe the $N_{\rm eff}(\rm H)$-$n_{\rm H}$ relationship in molecular clouds

    An analytic formalism to describe the N _ eff (H)‑n _ H relationship in molecular clouds. , keywords =. doi:10.1051/0004-6361/202555937 , archivePrefix =. 2507.16931 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202555937

  48. [48]

    GILDAS: Grenoble Image and Line Data Analysis Software

  49. [49]

    ALMA-IMF. II. Investigating the origin of stellar masses: Continuum images and data processing. , keywords =. doi:10.1051/0004-6361/202141681 , archivePrefix =. 2112.08183 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202141681

  50. [50]

    Dense Cores in Dark Clouds. VIII. Velocity Gradients. , keywords =. doi:10.1086/172465 , adsurl =

    doi:10.1086/172465

  51. [51]

    Coherence in Dense Cores. II. The Transition to Coherence. , keywords =. doi:10.1086/306045 , adsurl =

    doi:10.1086/306045

  52. [52]

    Physical and chemical structure of the Serpens filament -- fast formation and gravity-driven accretion

    Physical and chemical structure of the Serpens filament: Fast formation and gravity-driven accretion. , keywords =. doi:10.1051/0004-6361/202039465 , archivePrefix =. 2012.11924 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039465 2012

  53. [53]

    , keywords =

    Dense core formation by fragmentation of velocity-coherent filaments in L1517. , keywords =. doi:10.1051/0004-6361/201117039 , archivePrefix =. 1107.0971 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201117039

  54. [54]

    , keywords =

    Cores, filaments, and bundles: hierarchical core formation in the L1495/B213 Taurus region. , keywords =. doi:10.1051/0004-6361/201220090 , archivePrefix =. 1303.2118 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201220090

  55. [55]

    The Musca cloud: A 6 pc-long velocity-coherent, sonic filament

    The Musca cloud: A 6 pc-long velocity-coherent, sonic filament. , keywords =. doi:10.1051/0004-6361/201526015 , archivePrefix =. 1511.06370 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201526015

  56. [56]

    , keywords =

    Opacity broadening and interpretation of suprathermal CO linewidths: Macroscopic turbulence and tangled molecular clouds. , keywords =. doi:10.1051/0004-6361/201527319 , archivePrefix =. 1603.08521 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201527319

  57. [57]

    , keywords =

    Fibers in the NGC 1333 proto-cluster. , keywords =. doi:10.1051/0004-6361/201630348 , archivePrefix =. 1703.07029 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201630348

  58. [58]

    , keywords =

    Gravitational collapse of the OMC-1 region. , keywords =. doi:10.1051/0004-6361/201730732 , archivePrefix =. 1703.03464 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201730732

  59. [59]

    An ALMA study of the Orion Integral Filament. I. Evidence for narrow fibers in a massive cloud. , keywords =. doi:10.1051/0004-6361/201731894 , archivePrefix =. 1801.01500 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201731894

  60. [60]

    HCN/HNC intensity ratio: a new chemical thermometer for the molecular ISM

    HCN-to-HNC intensity ratio: a new chemical thermometer for the molecular ISM. , keywords =. doi:10.1051/0004-6361/201936516 , archivePrefix =. 1910.13754 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201936516 1910

  61. [61]

    Protostars and Planets VII , year = 2023, editor =

    Initial Conditions for Star Formation: a Physical Description of the Filamentary ISM. Protostars and Planets VII , year = 2023, editor =. doi:10.48550/arXiv.2203.09562 , archivePrefix =. 2203.09562 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2203.09562 2023

  62. [62]

    Emergence of high-mass stars in complex fiber networks (EMERGE). I. Early ALMA Survey: Observations and massive data reduction. , keywords =. doi:10.1051/0004-6361/202348565 , archivePrefix =. 2403.08091 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202348565

  63. [63]

    Gravitational Collapse in Turbulent Molecular Clouds. II. Magnetohydrodynamical Turbulence. , keywords =. doi:10.1086/318335 , archivePrefix =. astro-ph/0009227 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/318335

  64. [64]

    The dynamical properties of dense filaments in the infrared dark cloud G035.39-00.33

    The dynamical properties of dense filaments in the infrared dark cloud G035.39-00.33. , keywords =. doi:10.1093/mnras/stu446 , archivePrefix =. 1403.1444 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu446

  65. [65]

    , keywords =

    On the origin of non-self-gravitating filaments in the ISM. , keywords =. doi:10.1051/0004-6361/201321292 , archivePrefix =. 1306.5452 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201321292

  66. [66]

    Small-scale dissipative structures of diffuse ISM turbulence: I- CO diagnostics

    Small-Scale Dissipative Structures of Diffuse ISM Turbulence: I -- CO Diagnostics. SINS - Small Ionized and Neutral Structures in the Diffuse Interstellar Medium , year = 2007, editor =. doi:10.48550/arXiv.astro-ph/0701326 , archivePrefix =. astro-ph/0701326 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0701326 2007

  67. [67]

    Dissipative structures of diffuse molecular gas. II. The translucent environment of a dense core. , keywords =. doi:10.1051/0004-6361:20054565 , adsurl =

    work page doi:10.1051/0004-6361:20054565

  68. [68]

    Dissipative structures of diffuse molecular gas. III. Small-scale intermittency of intense velocity-shears. , keywords =. doi:10.1051/0004-6361:20078423 , archivePrefix =. 0802.0758 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361:20078423

  69. [69]

    Intermittency of interstellar turbulence: Parsec-scale coherent structure of intense velocity-shear

    Intermittency of interstellar turbulence: parsec-scale coherent structure of intense, velocity shear. , keywords =. doi:10.1051/0004-6361/200912296 , archivePrefix =. 0905.0368 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200912296

  70. [70]

    , year = 1974, month = jun, volume =

    Aperture Synthesis with a Non-Regular Distribution of Interferometer Baselines. , year = 1974, month = jun, volume =

    1974

  71. [71]

    , year = 1958, month = jan, volume =

    A phase sensitive interferometer technique for the measurement of the Fourier transforms of spatial brightness distributions of small angular extent. , year = 1958, month = jan, volume =. doi:10.1093/mnras/118.3.276 , adsurl =

    doi:10.1093/mnras/118.3.276 1958

  72. [72]

    , keywords =

    MAMBO mapping of Spitzer c2d small clouds and cores. , keywords =. doi:10.1051/0004-6361:200809481 , archivePrefix =. 0805.4205 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361:200809481

  73. [73]

    Molecular Line Emission as a Tool for Galaxy Observations (LEGO). I. HCN as a tracer of moderate gas densities in molecular clouds and galaxies. , keywords =. doi:10.1051/0004-6361/201731123 , archivePrefix =. 1707.05352 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731123

  74. [74]

    ALMA Observations of Starless Core Substructure in Ophiuchus

    ALMA Observations of Starless Core Substructure in Ophiuchus. , keywords =. doi:10.3847/1538-4357/aa63f8 , archivePrefix =. 1703.00506 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa63f8

  75. [75]

    The Atacama Large Aperture Submillimeter Telescope (AtLAST)

    The Atacama Large Aperture Submillimeter Telescope (AtLAST). Bulletin of the American Astronomical Society , year = 2019, volume =. doi:10.48550/arXiv.1907.04756 , archivePrefix =. 1907.04756 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1907.04756 2019

  76. [76]

    Carina's Pillars of Destruction: the view from ALMA

    Carina's pillars of destruction: the view from ALMA. , keywords =. doi:10.1093/mnras/stz3012 , archivePrefix =. 1910.09164 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz3012 1910

  77. [77]

    Atacama Large Aperture Submillimeter Telescope (AtLAST) Science: Our Galaxy

    Atacama Large Aperture Submillimeter Telescope (AtLAST) Science: Our Galaxy. arXiv e-prints , keywords =. doi:10.48550/arXiv.2403.00917 , archivePrefix =. 2403.00917 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2403.00917

  78. [78]

    Quiescent and coherent cores from gravoturbulent fragmentation

    Quiescent and Coherent Cores from Gravoturbulent Fragmentation. , keywords =. doi:10.1086/427255 , archivePrefix =. astro-ph/0306055 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/427255

  79. [79]

    Akademiia Nauk SSSR Doklady , year = 1941, month = apr, volume =

    Dissipation of Energy in Locally Isotropic Turbulence. Akademiia Nauk SSSR Doklady , year = 1941, month = apr, volume =

    1941

  80. [80]

    Journal of Fluid Mechanics , year = 1962, month = jan, volume =

    A refinement of previous hypotheses concerning the local structure of turbulence in a viscous incompressible fluid at high Reynolds number. Journal of Fluid Mechanics , year = 1962, month = jan, volume =. doi:10.1017/S0022112062000518 , adsurl =

    doi:10.1017/s0022112062000518 1962

Showing first 80 references.