Pith. sign in

REVIEW 4 major objections 5 minor 1 cited by

HP2 Survey V. Ophiuchus: Filament formation in a dispersing cloud complex

T0 review · 4 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

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

Pith's one-line read Stellar feedback from massive stars in Upper-Sco is the primary force driving the formation of most filamentary structures in the Ophiuchus-Lupus-Pipe complex, producing two distinct classes with observable birthmarks.

desk verdict Real maps and a testable feedback scenario, but the R/T dichotomy rests on a single adopted center and a small visually-selected sample, so the 'primary force' conclusion outruns the evidence. read the letter →

arxiv 2501.13931 v1 pith:ZKGWYZLM submitted 2025-01-23 astro-ph.GA

João Alves , Marco Lombardi , Charles Lada This is my paper · ORCID
classification astro-ph.GA
keywords OphiuchusmolecularcloudfilamentformationstellarfeedbackcolumndensitymapsSco-CenOBassociationdispersalstar
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

This paper uses high-dynamic-range maps from Herschel, Planck, and 2MASS to search for 'birthmarks' - observable remnants of filament formation - in the Ophiuchus molecular cloud complex. It reports that filaments fall into two classes based on their orientation relative to the massive stars of Upper-Sco: radial filaments have asymmetric longitudinal mass profiles with star formation at the head facing the stars, while tangential filaments have flat longitudinal profiles and asymmetric transverse profiles with mass 'spillover' away from the flow. The authors propose that both types arise from a single fast outflow from the OB association, via stagnation-point compression for radial filaments and collect-and-collapse shell fragmentation for tangential filaments. If correct, stellar feedback can simultaneously form filaments and stars while dispersing a giant molecular cloud, so the wider star-forming context must be considered when interpreting any individual cloud.

What carries the argument

The central object is the 'birthmark': a combination of filament orientation relative to the feedback center, longitudinal and transverse column-density profiles, and the location of active star formation. Orientation angles are measured between the filament's long axis and the line to the adopted center at the estimated last supernova position in Upper-Sco. Profiles come from cuts on the Meisner & Finkbeiner (2014) Planck column density map, with higher-resolution Herschel profiles for dense radial filaments. The dichotomy is interpreted using two hydrodynamical mechanisms: stagnation-point compression ('rocks in a stream') for radial filaments and shell fragmentation/collect-and-collapse for tangential filaments, with a bow-shock feature near B44 giving a Mach number of about 2.

What would settle it

Re-measure filament orientations using per-filament feedback centers - for example, ζ Oph for L204 instead of the adopted supernova position - and rerun the KS test; if the bimodality (p = 0.03) disappears, the dichotomy is a projection artifact. Alternatively, map the internal gas velocity along B44 in a molecular tracer, since the scenario predicts streaming away from Upper-Sco's massive stars at roughly 2 km/s over 20 pc; the absence of such streaming would break the formation mechanism.

Watch

Extended reading notes

Core claim

The central claim is that the feedback flow from massive stars in Upper-Sco is the primary force driving the formation of most filamentary structures in the Ophiuchus-Lupus-Pipe region. The paper shows that filaments are non-randomly oriented, clustering at radial and tangential angles relative to the adopted feedback center (the last supernova position), with a KS test p-value of 0.03. The two orientation classes show opposite column-density profiles: radial filaments decrease in mass along their length with star formation at the head, while tangential filaments are flat along their length and asymmetric across it, with mass 'spillover' on the side away from the flow. The authors interpret these patterns as two formation mechanisms - stagnation-point compression of dense gas and shell fragmentation of swept-up diffuse gas - leaving distinct observable 'birthmarks' that can test filament formation scenarios elsewhere.

Load-bearing premise

The classification of every filament as radial or tangential uses a single adopted feedback center, the estimated position of the last supernova in Upper-Sco, even though the paper itself calls a single source of feedback an 'improbable assumption'; if the effective center varies from filament to filament, the radial/tangential dichotomy and the birthmark reference frame could be artifacts of the chosen projection.

Editorial extensions

If this is right

  • The bimodal orientation distribution (p = 0.03) predicts that filaments in the Ophiuchus-Lupus-Pipe region should be preferentially radial or tangential relative to the feedback center, with a negligible fraction at intermediate angles.
  • Radial-type filaments should have decreasing linear mass density away from the massive stars, with Class I protostars confined to their heads; examples include L1688, B44, B45/L1709, and B59 in the Pipe.
  • Tangential-type filaments should be flat along their length and asymmetric across it, with excess mass on the side away from the flow, as seen in L204 and Lupus 1-4.
  • The flow is real: a roughly -21 km/s outflow traced in ISM absorption lines, with Ophiuchus's 3D motion away from Upper-Sco's stars supporting ram-pressure driving.
  • Upper-Sco is a gas-rich complex in late dispersal; its dense gas (AK > 0.8 mag) can form roughly 800 solar masses of stars in the next few million years, and the Sco-Cen GMC dispersal lifetime is estimated at no more than about 25 Myr.

Reading between the lines

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

  • Extension: the same birthmark test could be applied to other OB associations using HP2-style maps; the scenario predicts the radial/tangential split should appear only in complexes old enough to have sustained a feedback outflow for several million years.
  • Extension: the single-center orientation measurement should be redone with per-filament feedback centers; if the bimodality survives, it would strongly support a coherent large-scale flow; if not, the classification would likely reduce to local triggering by individual massive stars.
  • Extension: Gaia DR4 three-dimensional dust maps plus molecular-line kinematics could directly test the streaming-along-R-type-filaments prediction: gas along B44's length should move away from the massive stars at roughly the 2 km/s level.
  • Extension: the comparison with Orion implies a testable evolutionary sequence: younger complexes should show coherent dense-gas filaments with little radial/tangential ordering, whereas complexes near the end of dispersal should show the scattered bimodal filament population seen in Upper-Sco.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 5 minor

Summary. The manuscript presents new HP2 column-density and temperature maps of the Ophiuchus complex, combining Herschel, Planck, and 2MASS/NICEST data. It identifies two classes of filaments based on orientation relative to an adopted Upper-Sco feedback center: radial (R-type) filaments with decreasing longitudinal mass profiles and star formation at the head, and tangential (T-type) filaments with flat longitudinal profiles and asymmetric transverse profiles. The authors propose that a fast feedback flow from massive stars in Upper-Sco is the primary force shaping most filaments in the Ophiuchus-Lupus-Pipe region, and they interpret the results as evidence of an advanced stage of giant molecular cloud dispersal. Supporting evidence includes the -21 km/s Sco-Cen outflow (Piecka et al. 2024), 3D motions of Ophiuchus YSOs (Grasser et al. 2021), a bow-shock-like IRAS feature near B44, and the mass and temperature maps.

Significance. If the R/T dichotomy is real, this is an interesting and useful observational framework: it connects filament morphology and star formation location to feedback geometry, and it makes qualitative predictions for future 3D dust and kinematic studies. The paper's strengths are its high dynamic range maps, the careful hybrid calibration of Herschel/Planck/2MASS data, the reproducible mass estimates, and the explicit comparison with previous CO-based masses. The central weakness is that the R/T classification and the claimed bimodal orientation distribution depend on a single adopted feedback center that the authors themselves describe as improbable, and the profile classification is based on a small, visually selected sample without quantitative asymmetry metrics or error bars. These issues are local and fixable, but they are load-bearing for the 'primary force' conclusion.

major comments (4)
  1. [Section 4.3, Fig. 5] The orientation bimodality is measured from angles relative to a single adopted center (l=-13 degrees, b=21 degrees), which the text itself calls an 'improbable assumption' and immediately qualifies by noting that L204 is better described as tangential to zeta Oph, about 20 degrees away from that center. Since the R/T classification is defined by orientation relative to this same center, a different or distributed feedback center can reclassify individual filaments and change the longitudinal/transverse asymmetries that constitute the claimed birthmarks. The KS test p=0.03 against a flat distribution is already modest and is computed for one projection. Please add a robustness test: recompute each filament's orientation using plausible per-filament centers (e.g., zeta Oph for L204, sigma Sco/Elias 2-9 for B44/B45) or a Monte Carlo exploration of center positions within Upper-Sco, and report the resulting orientation distribution, R/T assignments, and the corresponding p-value. Without such a test, the 'primary force' claim is not yet supported by the orientation statistics.
  2. [Section 4.3, Figs. 6-7 and 9] The R/T birthmarks are established by visual inspection of selected profiles. No asymmetry index, no error bars, and no classification rule are given; the profiles are single cuts and do not propagate the map uncertainties shown in Figs. B.1 and B.2. Please define an objective asymmetry metric (e.g., normalized longitudinal center-of-mass or head-tail column-density contrast), compute it for the full sample of filaments with propagated uncertainties, and show that R- and T-types separate on this metric. A table listing all filaments, their midpoints, measured angles, assigned types, and the asymmetry values would make the classification reproducible.
  3. [Section 4.3 and Section 5] Orientation relative to the adopted feedback center is used to define the R/T classes, and the same orientation is then listed as a 'birthmark' and as evidence for the feedback scenario. To make the evidentiary chain testable, the paper should separate the geometric classification (orientation) from the physical predictions (mass profile shape, transverse asymmetry, and star formation location), and state explicitly which observables are used only as tests. In particular, Section 5.1's schematic scenario would be better supported by a quantitative prediction, e.g., the expected head-tail contrast as a function of filament column density, rather than by post-hoc assignment of individual clouds to R- and T-types.
  4. [Section 4.4.2 and Fig. 9] The claim that star formation occurs at the head of R-type filaments is supported by annotated Class I protostars in two filaments (B44 and L1709). The paper should quantify this birthmark for the whole sample: for example, compare the distribution of Class I protostar positions along the filaments, normalized by filament length, between R- and T-types, and include L1688 and Pipe Nebula cases in the same analysis. As written, the 'star formation location' birthmark is not yet a statistical result.
minor comments (5)
  1. [Section 6] There are typos in the conclusions: 'priciple' should be 'principle' and 'remants' should be 'remnants'.
  2. [Figure 6 caption] The caption uses 'latitudinal' where the text and Figure 7 use 'transverse'; also the y-axis labels use 'Ak' instead of 'A_K' in several panels.
  3. [Figure 5] With a small sample, the histogram binning strongly affects the visual bimodality; please report the individual measured angles and add a test for multimodality (e.g., Hartigan dip test) rather than only a KS test against a flat distribution.
  4. [Table A.1 and Section A.1] Table A.1 lists sigma Sco at 214 +/- 27 pc from Hipparcos, while the text argues for 159+7/-6 pc from Ratzenbock et al. (2023b); please state explicitly which distance is adopted for the analysis and for Figure 1.
  5. [References] The reference list contains duplicate entries: Lada et al. (2010) appears twice, North et al. (2007) appears twice, and Lombardi et al. (2008) appears more than once; please consolidate.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the R/T birthmark correlations are empirical, and the adopted feedback center comes from independent supernova and temperature evidence.

full rationale

The paper's load-bearing inference—that feedback from Upper-Sco massive stars shapes the Ophiuchus-Lupus-Pipe gas—is not circular. The R-type/T-type classification is based on measured filament orientations relative to a center chosen from independent evidence: the warm-dust peak and the last-supernova location of Neuhäuser et al. (2019); the center is not fitted to the orientation data. The distinct mass profiles and star-formation locations used as 'birthmarks' are empirical correlations measured after classification and are not implied by the orientation definitions alone. The outflow evidence (-21 km/s, Piecka et al. 2024), the 3D motion of YSOs (Grasser et al. 2021), and the gas kinematics across B44 (Loren 1989b) are external, published data sets; the self-citations to Ratzenböck et al. and Piecka et al. are independent Gaia/absorption-line studies, not unverified assertions unique to this paper. The paper itself flags the single-center assumption as 'improbable' (Sec 4.3) and notes that L204 is better tied to ζ Oph, about 20 degrees from the adopted center; this is weighed as a robustness caveat and does not constitute circularity because the center is not fitted to the orientation distribution. No equation in the paper defines the inferred feedback scenario in terms of the observed birthmarks, and no fitted parameter is renamed as a prediction. Hence no specific circular reduction can be exhibited.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central scenario relies on a small set of externally supplied constraints: the distance to Ophiuchus, the existence and persistence of the Sco-Cen outflow, and the adopted feedback center. No new physical entities are introduced; the R/T classes are observational categories. The main free choices are the adopted distance and the binary correction factor; neither is fitted to the central data, but both affect derived energetics and masses.

free parameters (3)
  • Adopted distance to Ophiuchus = 140 pc
    Adopted in Section 2 to convert angular scales to physical sizes and masses; not fitted here, but chosen from the literature (range 118-149 pc). All physical quantities (masses, surface densities, pc scales) scale with this choice, though the R/T classification is unaffected.
  • Binary correction factor for ionizing luminosity = 2
    Introduced ad hoc in Appendix A to correct the summed ionizing photon luminosity for unresolved binaries, affecting only the energetics estimate (QH about 10^49 s^-1), not the central claim.
  • Dense gas threshold AK = 0.8 mag
    Chosen in Section 4.2 following Lada et al. (2010) to define star-forming gas mass; used in the future star formation estimate and the Orion comparison, not in the R/T classification.
assumptions (5)
  • domain assumption The HP2 column density and temperature maps are accurate tracers of gas mass and dust temperature, as calibrated in Lombardi et al. (2014) using a modified blackbody SED and a constant dust-to-gas ratio.
    Invoked in Section 3 (data reduction) and Section 4.1; systematic errors here would propagate to all masses and profile shapes.
  • ad hoc to paper A single adopted center, the location of the last Upper-Sco supernova (l=-13 degrees, b=21 degrees) from Neuhäuser et al. (2019), is the appropriate origin for measuring all filament orientations.
    Section 4.3: 'we adopt this supernova's location... as the working center of Upper-Sco'. The paper notes L204 is better described as tangential to zeta Oph, about 20 degrees away, so this is fragile for at least one filament and potentially others.
  • domain assumption The Sco-Cen outflow detected by Piecka et al. (2024) has been present and approximately steady over the ~10 Myr age of Upper-Sco, and its flow direction is toward Ophiuchus.
    Sections 5.1 and 5.2 assume the outflow reaches the clouds and persists long enough to stretch a 20 pc filament at ~2 km/s; the detection is from current-epoch absorption-line data.
  • domain assumption Class I protostars trace the location of current star formation and their positions relative to filament heads reflect the local gas dynamics rather than projection effects.
    Used in Section 4.4.2 and Figure 9 to argue star formation occurs at profile maxima facing massive stars.
  • domain assumption Projected filament orientations and column density profiles on the plane of the sky are sufficient to infer the 3D relationship between filaments and the feedback flow.
    Implicit throughout Sections 4.3 and 4.4; the paper concedes in Section 5.2 that the true 3D orientation of B44 is unknown, making the inferred streaming velocity uncertain.

how reviews work

0 comments
Cite this review

Pith. "Pith review of HP2 Survey V. Ophiuchus: Filament formation in a dispersing cloud complex." pith.science (2026). https://pith.science/paper/ZKGWYZLM

@misc{pith2026250113931,
  author       = {Pith},
  title        = {Pith review of: HP2 Survey V. Ophiuchus: Filament formation in a dispersing cloud complex},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZKGWYZLM}},
  note         = {Machine review of arXiv:2501.13931}
}
read the original abstract

We search for potential ``birthmarks'' left from the formation of filamentary molecular clouds in the Ophiuchus complex. We use high dynamic-range column density and temperature maps derived from \textit{Herschel}, \textit{Planck}, and \textit{2MASS/NICEST} extinction data. We find two distinct types of filaments based on their orientation relative to nearby massive stars: radial (R-type) and tangential (T-type). R-type filaments exhibit decreasing mass profiles away from massive stars, while T-type filaments show flat but structured profiles. We propose a scenario where both filament types originate from the dynamic interplay of compression and stretching forces exerted by a fast outflow emanating from the OB association. The two formation mechanisms leave distinct observable ``birthmarks'' (namely, filament orientation, mass distribution, and star formation location) on each filament type. Our results illustrate a complex phase in molecular cloud evolution with two simultaneous yet contrasting processes: the formation of filaments and stars via the dispersal of residual gas from a previous massive star formation event. Our approach highlights the importance of taking into account the wider context of a star-forming complex, rather than concentrating exclusively on particular subregions.

Figures

Figures reproduced from arXiv: 2501.13931 by the authors.

Figure 1
Figure 1. Color composite of the Ophiuchus, Pipe Nebula, and Lupus cloud complexes (blue: extrapolated Planck 250 µm, green: Planck 350 µm, red: Planck 500 µm). Star symbols represent the position of massive ionizing stars (B3 or earlier), while symbol size represents relative brightness. Most of these stars have associated Hα extended emission, while only the two fainter objects are not associated with WISE extended emission… view at source ↗
Figure 2
Figure 2. Planck-Herschel optical-depth map for Ophiuchus. The resolu￾tion of the map is 5 arcmin (for the Planck data) and 36 arcsec (for the high column density, Herschel-covered areas). The corresponding error map is presented in Figure B.1 2 ◦ 4 ◦ 6 ◦ 8 ◦ 348◦ 350◦ 352◦ 354◦ 356◦ 358◦ Galactic Longitude 8 ◦ 10◦ 12◦ 14◦ 16◦ 18◦ 20◦ 22◦ 24◦ Galactic Latitude 18 20 22 24 T [K] L43 L234 L260 L204 L162 L137 CB68 L1719 L1757 B4… view at source ↗
Figure 3
Figure 3. Effective dust-temperature map for the Ophiuchus field. The cold structures appear white, while the higher temperatures appear as black. There are at least seven hot spots, all associated with massive ionizing stars in the region, implying a distance similar to the cloud material they are warming up. Note, by comparison with [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: Orientations of the main filaments (enclosed in the orange boxes) in the Ophiuchus-Lupus-Pipe region, shown on the Meisner & Finkbeiner (2014) temperature map. The orientation angles were measured between the filament axis and the direction to a central point near the …
Figure 5
Figure 5. Figure 5: Distribution of filament orientations in the Upper-Sco region as shown in [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]
Figure 6
Figure 6. Figure 6: Selected examples of R-type longitudinal (blue) and latitudinal (red) mass profiles. An observable pattern emerges, specifically, R-type filaments predominantly exhibit asymmetric longitudinal distributions (head-tail configuration) and symmetric transverse distributio…
Figure 7
Figure 7. Figure 7: Selected examples of T-type longitudinal (blue) and transversal (red) column density profiles. In contrast to R-type filaments, T-type filaments do not exhibit head-tail morphology. Their longitudinal profiles are generally flat, with dense cores and star formation dis…
Figure 8
Figure 8. Figure 8: IRAS 100 µm image of the Ophiuchus region. The image reveals a bow-like dust feature at the head of B44, suggestive of a bow-shock. If a bow-shock, the Mach number of the flow interacting with B44 is about 2. 4.4.2. R-type profiles at high resolution [PITH_FULL_IMAGE:…
Figure 9
Figure 9. Figure 9: shows longitudinal Herschel column-density profiles of B44, L1709 (at the head of B45), with Class I protostars marked as red stars. These are higher resolution versions of the Planck￾based R-type profiles presented in [PITH_FULL_IMAGE:figures/full_fig_p008_9.png]
Figure 10
Figure 10. Figure 10: Top: Summary of the longitudinal/transversal profile analysis. R-type profiles exhibit asymmetric longitudinal profiles and symmetric transversal profiles, whereas T-type profiles are characterized by gen￾erally flatter longitudinal profiles and asymmetric transversal…
Figure 11
Figure 11. Figure 11: Comparing the Orion and Upper-Sco complexes at the same physical scale reveals striking differences in the amount and distribution of dense gas. The greyscale represents the Planck column-density map (Meisner & Finkbeiner 2014), and red marks regions with dense gas (A…

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. The SOMA-POL Survey. I. Polarization and magnetic field properties of massive protostars

    astro-ph.GA 2025-07 conditional novelty 6.0 of 10

    Magnetic field directions inferred from dust polarization show a bimodal alignment (parallel or perpendicular) with the elongation of massive protostellar cores on sub-parsec scales.

Reference graph

Works this paper leans on

137 extracted references · 62 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]

    1994, , 423, L59

    Abergel , A., Boulanger , F., Mizuno , A., & Fukui , Y. 1994, , 423, L59

    1994

  4. [4]

    Ade, P. a. R., Aghanim, N., Alves, M. I. R., et al. 2014, Astronomy & Astrophysics, 571, A1

    2014

  5. [5]

    Ade, P. A. R., Aghanim, N., Alves, M. I. R., et al. 2013, A&A, 557, A53

    2013

  6. [6]

    J., Lada , E

    Alves , J., Lada , C. J., Lada , E. A., Kenyon , S. J., & Phelps , R. 1998, , 506, 292

    1998

  7. [7]

    2007, in ISLAND UNIVERSES, Astrophysics and Space Science Proceedings (Springer, Dordrecht), 417--422

    Alves, J., Lombardi, M., & Lada, C. 2007, in ISLAND UNIVERSES, Astrophysics and Space Science Proceedings (Springer, Dordrecht), 417--422

    2007

  8. [8]

    Alves, J., Lombardi, M., & Lada, C. J. 2014, A&A, 565, A18

    2014

Show all 137 references
  1. [9]

    2010, , 518, L102

    Andr \'e , P., Men'shchikov , A., Bontemps , S., et al. 2010, , 518, L102

    2010

  2. [10]

    & Montmerle , T

    Andre , P. & Montmerle , T. 1994, , 420, 837

    1994

  3. [11]

    2018, PASJ, 70

    Arzoumanian, D., Shimajiri, Y., Inutsuka, S.-I., Inoue, T., & Tachihara, K. 2018, PASJ, 70

    2018

  4. [12]

    Bailer-Jones , C. A. L. 2015, , 127, 994

    2015

  5. [13]

    D., Stark , A

    Bally , J., Langer , W. D., Stark , A. A., & Wilson , R. W. 1987, , 312, L45

    1987

  6. [14]

    Barnard , E. E. 1907, , 25

    1907

  7. [15]

    E., Frost , E

    Barnard , E. E., Frost , E. B., & Calvert , M. R. 1927, A Photographic Atlas of Selected Regions of the Milky Way

    1927

  8. [16]

    1964, , 2, 213

    Blaauw , A. 1964, , 2, 213

    1964

  9. [17]

    2020, A&A, 644, A27

    Bonne, L., Bontemps, S., Schneider, N., et al. 2020, A&A, 644, A27

    2020

  10. [18]

    Boulanger , F., Baud , B., & van Albada , G. D. 1985, , 144, L9

    1985

  11. [19]

    & Alves, J

    Bouy, H. & Alves, J. 2015, A&A, 584, A26

    2015

  12. [20]

    & Hartmann, L

    Burkert, A. & Hartmann, L. 2004, ApJ, 616, 288

    2004

  13. [21]

    1985, , 149, 273

    Cernicharo , J., Bachiller , R., & Duvert , G. 1985, , 149, 273

    1985

  14. [22]

    R., McLeod, A

    Chevance, M., Krumholz, M. R., McLeod, A. F., et al. 2022

    2022

  15. [23]

    E., Bonnell, I

    Dale, J. E., Bonnell, I. A., & Whitworth, A. P. 2007, MNRAS, 375, 1291–1298

    2007

  16. [24]

    de Geus , E. J. 1992, , 262, 258

    1992

  17. [25]

    de Geus, E. J. & Burton, W. B. 1991, A&A, 246, 559

    1991

  18. [26]

    2017, A&A, 597, A90

    Ducourant, C., Teixeira, R., Krone-Martins, A., et al. 2017, A&A, 597, A90

    2017

  19. [27]

    2024, A&A, 685, A82

    Edenhofer, G., Zucker, C., Frank, P., et al. 2024, A&A, 685, A82

    2024

  20. [28]

    Elmegreen , B. G. & Lada , C. J. 1977, , 214, 725

    1977

  21. [29]

    P., Davis, M., & Schlegel, D

    Finkbeiner, D. P., Davis, M., & Schlegel, D. J. 1999, ApJ, 524, 867

    1999

  22. [30]

    Franco, G. A. P. 2002, MNRAS, 331, 474

    2002

  23. [31]

    N., & Tenorio-Tagle , G

    Franco, J., Shore, S. N., & Tenorio-Tagle , G. 1994, ApJ, 436, 795

    1994

  24. [32]

    & York, D

    Frisch, P. & York, D. 1986, in The galaxy and the solar system (A87-34101 14-90). Tucson, AZ, University of Arizona Press, 1986, p. 83-100

    1986

  25. [33]

    Gaia Collaboration , Vallenari, A., Brown, A. G. A., et al. 2023, A&A, 674, A1

    2023

  26. [34]

    F., Heyer , M., Narayanan , G., et al

    Goldsmith , P. F., Heyer , M., Narayanan , G., et al. 2008, , 680, 428

    2008

  27. [35]

    2021, A&A, 652, A2

    Grasser, N., Ratzenböck, S., Alves, J., et al. 2021, A&A, 652, A2

    2021

  28. [36]

    J., Abergel , A., Abreu , A., et al

    Griffin , M. J., Abergel , A., Abreu , A., et al. 2010, , 518, L3

    2010

  29. [37]

    2010, ApJ, 723, 971

    Gritschneder, M., Burkert, A., Naab, T., & Walch, S. 2010, ApJ, 723, 971

    2010

  30. [38]

    E., Heitsch, F., et al

    Hacar, A., Clark, S. E., Heitsch, F., et al. 2023, in PPVII

    2023

  31. [39]

    2018, A&A, 610, A77

    Hacar, A., Tafalla, M., Forbrich, J., et al. 2018, A&A, 610, A77

    2018

  32. [40]

    M., Reynolds , R

    Haffner , L. M., Reynolds , R. J., Tufte , S. L., et al. 2003, , 149, 405

    2003

  33. [41]

    2012, , 754, 104

    Hatchell , J., Terebey , S., Huard , T., et al. 2012, , 754, 104

    2012

  34. [42]

    & Jenkins , E

    Heiles , C. & Jenkins , E. B. 1976, , 46, 333

    1976

  35. [43]

    2013, 769, 115

    Heitsch, F. 2013, 769, 115

    2013

  36. [44]

    2013, , 556, A153

    Hennebelle , P. 2013, , 556, A153

    2013

  37. [45]

    Hobbs, L. M. 1969, ApJ, 158, 461

    1969

  38. [46]

    Howard, A. D. P., Whitworth, A. P., Griffin, M. J., Marsh, K. A., & Smith, M. W. L. 2021, MNRAS, 504, 6157

    2021

  39. [47]

    2015, A&A, 580, A49

    Inutsuka, S.-I., Inoue, T., Iwasaki, K., & Hosokawa, T. 2015, A&A, 580, A49

    2015

  40. [48]

    Jeffreson, S. M. R., Kruijssen, J. M. D., Keller, B. W., Chevance, M., & Glover, S. C. O. 2020, MNRAS, 498, 385

    2020

  41. [49]

    & Bally , J

    Johnstone , D. & Bally , J. 1999, , 510, L49

    1999

  42. [50]

    Kalberla , P. M. W. & Haud , U. 2015, , 578, A78

    2015

  43. [51]

    Krause, M. G. H., Burkert, A., Diehl, R., et al. 2018, A&A, 619, A120

    2018

  44. [52]

    2001, , 322, 231

    Kroupa , P. 2001, , 322, 231

    2001

  45. [53]

    T., Gutermuth , R

    Kryukova , E., Megeath , S. T., Gutermuth , R. A., et al. 2012, , 144, 31

    2012

  46. [54]

    J., Lada , E

    Lada , C. J., Lada , E. A., Clemens , D. P., & Bally , J. 1994, , 429, 694

    1994

  47. [55]

    J., Lombardi , M., & Alves , J

    Lada , C. J., Lombardi , M., & Alves , J. F. 2010, , 724, 687

    2010

  48. [56]

    J., Lombardi, M., & Alves, J

    Lada, C. J., Lombardi, M., & Alves, J. F. 2010, ApJ

    2010

  49. [57]

    Lada , C. J. & Wilking , B. A. 1984, , 287, 610

    1984

  50. [58]

    2020, A&A, 638, A74

    Ladjelate, B., André, P., Könyves, V., et al. 2020, A&A, 638, A74

    2020

  51. [59]

    Landau, L. D. & Lifshitz, E. M. 1987, Fluid Mechanics, Second Edition: Volume 6 (Course of Theoretical Physics), Course of theoretical physics / by L. D. Landau and E. M. Lifshitz, Vol. 6 (Butterworth-Heinemann)

    1987

  52. [60]

    2015, Gas and dust in the star-forming regionrho Oph A

    Liseau, R., Larsson, B., Lunttila, T., et al. 2015, Gas and dust in the star-forming regionrho Oph A

    2015

  53. [61]

    M., Mioduszewski , A

    Loinard , L., Torres , R. M., Mioduszewski , A. J., & Rodr \' guez , L. F. 2008, , 675, L29

    2008

  54. [62]

    Lombardi , M., Alves , J., & Lada , C. J. 2006, , 454, 781

    2006

  55. [63]

    Lombardi, M., Alves, J., & Lada, C. J. 2011, A&A, 535, A16

    2011

  56. [64]

    Lombardi , M., Bouy , H., Alves , J., & Lada , C. J. 2014, , 566, A45

    2014

  57. [65]

    J., & Alves, J

    Lombardi, M., Lada, C. J., & Alves, J. 2008, A&A, 489, 143

    2008

  58. [66]

    J., & Alves , J

    Lombardi , M., Lada , C. J., & Alves , J. 2008, , 489, 143

    2008

  59. [67]

    J., & Alves, J

    Lombardi, M., Lada, C. J., & Alves, J. 2008, A&A, 480, 785

    2008

  60. [68]

    J., & Alves , J

    Lombardi , M., Lada , C. J., & Alves , J. 2010, , 512, 67

    2010

  61. [69]

    Loren , R. B. 1989 a , , 338, 902

    1989

  62. [70]

    Loren , R. B. 1989 b , , 338, 925

    1989

  63. [71]

    Loren, R. B. & Wootten, A. 1986, ApJ, 306, 142

    1986

  64. [72]

    Luhman, K. L. & Esplin, T. L. 2020, AJ, 160

    2020

  65. [73]

    Lynds , B. T. 1962, , 7, 1

    1962

  66. [74]

    V., Mohamed, S., & Langer, N

    Mackey, J., Gvaramadze, V. V., Mohamed, S., & Langer, N. 2015, A&A, 573, A10

    2015

  67. [75]

    & Lim, A

    Mackey, J. & Lim, A. J. 2010, MNRAS, 403, 714–730

    2010

  68. [76]

    M., Dickey , J

    McClure-Griffiths , N. M., Dickey , J. M., Gaensler , B. M., Green , A. J., & Haverkorn , M. 2006, , 652, 1339

    2006

  69. [77]

    Meisner, A. M. & Finkbeiner, D. P. 2014, ApJ, 798, 88

    2014

  70. [78]

    Miret-Roig, N., Galli, P. A. B., Olivares, J., et al. 2022, A&A, 667, A163

    2022

  71. [79]

    G., Abergel , A., et al

    Miville-Desch \^e nes , M.-A., Martin , P. G., Abergel , A., et al. 2010, , 518, L104

    2010

  72. [80]

    2010, , 122, 314

    Molinari , S., Swinyard , B., Bally , J., et al. 2010, , 122, 314

    2010

  73. [81]

    Montmerle , T., Koch-Miramond , L., Falgarone , E., & Grindlay , J. E. 1983, , 269, 182

    1983

  74. [82]

    Myers , P. C. 2009, , 700, 1609

    2009

  75. [83]

    Nagai , T., Inutsuka , S.-i., & Miyama , S. M. 1998, , 506, 306

    1998

  76. [84]

    Neuhäuser, R., Gießler, F., & Hambaryan, V. V. 2019, MNRAS

    2019

  77. [85]

    R., Davis , J., Tuthill , P

    North , J. R., Davis , J., Tuthill , P. G., Tango , W. J., & Robertson , J. G. 2007, , 380, 1276

    2007

  78. [86]

    R., Davis, J., Tuthill, P

    North, J. R., Davis, J., Tuthill, P. G., Tango, W. J., & Robertson, J. G. 2007, MNRAS, 380, 1276

    2007

  79. [87]

    1991, ApJS, 77, 647

    Nozawa, S., Mizuno, A., Teshima, Y., Ogawa, H., & Fukui, Y. 1991, ApJS, 77, 647

    1991

  80. [88]

    2006, MNRAS, 368, 1833

    Nutter, D., Ward-Thompson, D., & André, P. 2006, MNRAS, 368, 1833

    2006

  81. [89]

    B., Cox , N

    Ochsendorf , B. B., Cox , N. L. J., Krijt , S., et al. 2014, , 563, A65

    2014

  82. [90]

    1999, PASJ, 51, 871

    Onishi, T., Kawamura, A., Abe, R., et al. 1999, PASJ, 51, 871

    1999

  83. [91]

    N., Loinard, L., Kounkel, M

    Ortiz-León, G. N., Loinard, L., Kounkel, M. A., et al. 2017, ApJ, 834, 141

    2017

  84. [92]

    2010, in ASPC, Vol

    Ott , S. 2010, in ASPC, Vol. 434, Astronomical Data Analysis Software and Systems XIX, ed. Y. Mizumoto , K.-I. Morita , & M. Ohishi , 139

    2010

  85. [93]

    A., & Nordlund ,

    Padoan , P., Juvela , M., Goodman , A. A., & Nordlund , . 2001, , 553, 227

    2001

  86. [94]

    2012, A&A, 541, A63

    Peretto, N., André, P., Könyves, V., et al. 2012, A&A, 541, A63

    2012

  87. [95]

    2024, A&A, 689, A84

    Piecka, M., Hutschenreuter, S., & Alves, J. 2024, A&A, 689, A84

    2024

  88. [96]

    & Pudritz, R

    Pillsworth, R. & Pudritz, R. E. 2024, Mon. Not. R. Astron. Soc., 528, 209

    2024

  89. [97]

    E., Arzoumanian, D., André, P., et al

    Pineda, J. E., Arzoumanian, D., André, P., et al. 2023

    2023

  90. [98]

    2010, , 518, L2

    Poglitsch , A., Waelkens , C., Geis , N., et al. 2010, , 518, L2

    2010

  91. [99]

    2024, A&A in press

    Posch, L., Alves, J., Mirét-Roig, N., et al. 2024, A&A in press

    2024

  92. [100]

    2023, A&A, 679, L10

    Posch, L., Miret-Roig, N., Alves, J., et al. 2023, A&A, 679, L10

    2023

  93. [101]

    & Mamajek, E

    Preibisch, T. & Mamajek, E. 2008, Handbook of Star Forming Regions, 64, 235–370

    2008

  94. [102]

    Ratzenbock, S., Obermuller, V., Moller, T., Alves, J., & Bomze, I. M. 2023, IEEE Trans. Vis. Comput. Graph., 29, 3855

    2023

  95. [103]

    E., Alves, J., et al

    Ratzenböck, S., Großschedl, J. E., Alves, J., et al. 2023 a , A&A, 678, 71

    2023

  96. [104]

    E., Möller, T., et al

    Ratzenböck, S., Großschedl, J. E., Möller, T., et al. 2023 b , A&A, 677, A59

    2023

  97. [105]

    Robitaille, J.-F., Scaife, A. M. M., Carretti, E., et al. 2018, A&A, 617, A101

    2018

  98. [106]

    P., Tollerud, E

    Robitaille, T. P., Tollerud, E. J., Greenfield, P., et al. 2013, A&A, 558, A33

    2013

  99. [107]

    & Pittard, J

    Rogers, H. & Pittard, J. M. 2013, MNRAS, 431, 1337

    2013

  100. [108]

    F., Green, G., Finkbeiner, D

    Schlafly, E. F., Green, G., Finkbeiner, D. P., et al. 2014, ApJ, 786, 29

    2014

  101. [109]

    & Elmegreen , B

    Schneider , S. & Elmegreen , B. G. 1979, , 41, 87

    1979

  102. [110]

    Shore, S. N. 2007, Astrophysical Hydrodynamics (Wiley)

    2007

  103. [111]

    F., Cutri, R

    Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163

    2006

  104. [112]

    2006, , 367, 763

    Smith , N. 2006, , 367, 763

    2006

  105. [113]

    J., Treß, R

    Smith, R. J., Treß, R. G., Sormani, M. C., et al. 2020, MNRAS, 492, 1594

    2020

  106. [114]

    D., Beuther, H., Syed, J., et al

    Soler, J. D., Beuther, H., Syed, J., et al. 2021, A&A, 651, L4

    2021

  107. [115]

    D., Bracco, A., & Pon, A

    Soler, J. D., Bracco, A., & Pon, A. 2018, A&A, 609, L3

    2018

  108. [116]

    D., Miville-Deschênes, M.-A., Molinari, S., et al

    Soler, J. D., Miville-Deschênes, M.-A., Molinari, S., et al. 2022, A&A, 662, A96

    2022

  109. [117]

    & Rudkjobing , M

    Struve , O. & Rudkjobing , M. 1948, , 54, 51

    1948

  110. [118]

    2000 a , PASJ, 52, 1147

    Tachihara, K., Abe, R., Onishi, T., Mizuno, A., & Fukui, Y. 2000 a , PASJ, 52, 1147

    2000

  111. [119]

    2000 b , ApJ, 528, 817

    Tachihara, K., Mizuno, A., & Fukui, Y. 2000 b , ApJ, 528, 817

    2000

  112. [120]

    2001, PASJ, 53, 1081

    Tachihara, K., Toyoda, S., Onishi, T., et al. 2001, PASJ, 53, 1081

    2001

  113. [121]

    Taylor , M. B. 2005, in ASPC, Vol. 347, Astronomical Data Analysis Software and Systems XIV, ed. P. Shopbell , M. Britton , & R. Ebert , 29

    2005

  114. [122]

    & Tassis, K

    Tritsis, A. & Tassis, K. 2018, Science, 360, 635

    2018

  115. [123]

    2007, , 474, 653

    van Leeuwen , F. 2007, , 474, 653

    2007

  116. [124]

    1977, The Astronomical Journal, 82

    Vrba, F. 1977, The Astronomical Journal, 82

    1977

  117. [125]

    F., Hills , R

    Ward-Thompson , D., Scott , P. F., Hills , R. E., & Andre , P. 1994, , 268, 276

    1994

  118. [126]

    P., Priestley, F

    Whitworth, A. P., Priestley, F. D., & Geen, S. T. 2022, MNRAS, 517, 4940

    2022

  119. [127]

    A., Gagn \'e , M., & Allen , L

    Wilking , B. A., Gagn \'e , M., & Allen , L. E. 2008, Star Formation in the Ophiuchi Molecular Cloud , ed. B. Reipurth , 351

    2008

  120. [128]

    Wood , D. O. S., Myers , P. C., & Daugherty , D. A. 1992, in Bulletin of the American Astronomical Society, Vol. 24, American Astronomical Society Meeting Abstracts, 1200

    1992

  121. [129]

    2019 a , MNRAS, 488, 3406

    Zamora-Avilés, M., Ballesteros-Paredes, J., Hernández, J., et al. 2019 a , MNRAS, 488, 3406

    2019

  122. [130]

    F., et al

    Zamora-Avilés, M., Vázquez-Semadeni, E., González, R. F., et al. 2019 b , MNRAS, 487, 2200

    2019

  123. [131]

    J., & Bouy, H

    Zari, E., Lombardi, M., Alves, J., Lada, C. J., & Bouy, H. 2016, A&A, 587, A106

    2016

  124. [132]

    2017, ApJ, 864, 153

    Zucker, C., Battersby, C., & Goodman, A. 2017, ApJ, 864, 153

    2017

  125. [133]

    S., Schlafly, E

    Zucker, C., Speagle, J. S., Schlafly, E. F., et al. 2020, A&A, 633, A51

    2020

  126. [134]

    S., Schlafly, E

    Zucker, C., Speagle, J. S., Schlafly, E. F., et al. 2019, ApJ, 879, 125

    2019

  127. [135]

    @esa (Ref

    \@ifclassloaded agu2001 natbib The agu2001 class already includes natbib coding, so you should not add it explicitly Type <Return> for now, but then later remove the command natbib from the document \@ifclassloaded aguplus natbib The aguplus class already includes natbib codin...

  128. [136]

    @stdbsttrue NAT@ctr \@lbibitem[ NAT@ctr ] \@lbibitem[#1]#2 \@extra@b@citeb \@ifundefined br@#2\@extra@b@citeb \@namedef br@#2 \@nameuse br@#2\@extra@b@citeb \@ifundefined b@#2\@extra@b@citeb @num @parse #2 [ @natanchorstart #2\@extra@b@citeb \@biblabel @num @natanchorend] @ifc...

  129. [137]

    e-prints

    @open @close @open @close and [1] URL: #1 \@ifundefined chapter * \@mkboth \@ifundefined NAT@sectionbib * \@mkboth * \@mkboth\@gobbletwo \@ifclassloaded amsart * \@ifclassloaded amsbook * \@ifundefined bib@heading @heading NAT@ctr thebibliography [1] @ \@biblabel NAT@ctr \@bib...

    2017

Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.