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REVIEW 2 major objections 6 minor 70 references

ALMA observations of massive clouds in the central molecular zone: slim filaments tracing parsec-scale shocks

T0 review · 2 major / 6 minor · reviewed 2026-08-09 · deepseek-v4-flash

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Pith's one-line read The paper reports ALMA detections of hair-thin molecular filaments in the Galactic center that appear to trace parsec-scale shocks and may replenish the region's SiO and complex organic molecules.

desk verdict Genuinely new filament class, but the 'hydrostatic inequilibrium' claim is an upper-limit statement that needs a firmer density constraint. read the letter →

arxiv 2502.03913 v1 pith:F73Z2ZG5 submitted 2025-02-06 astro-ph.GA

Kai Yang , Xing Lu , Yichen Zhang , Xunchuan Liu , Adam Ginsburg , Hauyu Baobab Liu , Yu Cheng , Siyi Feng
show 17 more authors
Tie Liu Qizhou Zhang Elisabeth A.C. Mills Daniel L. Walker Shu-ichiro Inutsuka Cara Battersby Steven N. Longmore Xindi Tang Jens Kauffmann Qilao Gu Shanghuo Li Qiuyi Luo J.M. Diederik Kruijssen Thushara Pillai Hai-Hua Qiao Keping Qiu Zhiqiang Shen
This is my paper · ORCID
classification astro-ph.GA
keywords slimfilamentscentralmolecularzoneSiOemissioncomplexorganicmoleculesparsec-scaleshockshydrostaticinequilibriumALMAobservationsclouddynamics
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 reports the discovery of a new class of extremely narrow gas filaments, longer than half a parsec but only about 0.03 parsec wide, in two massive clouds near the Milky Way's center. Seen in SiO and eight other molecular lines, these 'slim filaments' have no detectable dust continuum and coherent velocities that rule out protostellar outflows. Their molecular abundances resemble shocked outflow gas rather than dense cores, and their internal turbulent pressure far exceeds all other pressures, so they cannot be in hydrostatic equilibrium. The authors conclude that the filaments are parsec-scale shocks and that their dissipation over a few thousand years can replenish the SiO and complex organic molecules that are widespread in the central molecular zone.

What carries the argument

The central object is the slim filament: a gas structure identified in SiO 5--4 emission by an aspect ratio greater than 10, a coherent velocity structure in position-velocity space, and a Gaussian-fitted FWHM of 0.026 pc (0.024 pc after beam deconvolution), with skeletons extracted by a filament-finding algorithm. The decisive argument has two parts. First, pressure accounting: the continuum non-detection sets a column-density upper limit of 2.3e23 $cm^{-2}$, converted to a volume density of 3.1e6 $cm^{-3}$ by assuming the line-of-sight depth equals the filament width; combined with a velocity dispersion of 4.4 km/s, this gives a turbulent pressure that dominates over thermal, magnetic, gravitational, and external pressure, establishing hydrostatic inequilibrium. Second, the replenishment budget: a per-filament SiO mass of 8.1e-5 solar masses and a dissipation time of 5.2e3 yr, compared with a CMZ-wide SiO depletion rate of about 1.3e-4 solar masses per year, imply that a surface density near 0.4 slim filaments per square parsec would suffice to refill the SiO.

What would settle it

Measure the volume density of a slim filament independently, for example by detecting its absorption against a background continuum source or by resolved multiple SiO transitions that constrain excitation, and recompute the turbulent pressure; if the true density is much lower than the 3.1e6 $cm^{-3}$ upper-limit value, the pressure-dominance argument fails. A CMZ-wide survey that finds a slim-filament surface density well below about 0.4 per square parsec would falsify the claim that their dissipation replenishes the observed SiO.

Watch

Extended reading notes

Core claim

ALMA 1.3 mm spectral-line observations toward the 20 km/s cloud and 50 km/s cloud reveal ten filaments in SiO 5--4 and eight additional lines (H2CO, CH3OH, HNCO, HC3N, SO, $H2^{13}$CO, c-C3H2, CH3CN) with beam-deconvolved widths of 0.024 pc and lengths greater than 0.5 pc. They are not detected in the 1.3 mm continuum at the 5 $\sigma$ level. Position-velocity diagrams show velocities coherent along the long axes with no gradient typical of outflows, and abundances normalized to CH3OH are statistically indistinguishable from protostellar outflows (p = 0.68) but different from dense cores in the same clouds (p = 0.02). The pressure analysis gives a turbulent pressure of about 1.7e10 K $cm^{-3}$, two to three orders of magnitude above thermal, magnetic, gravitational, and external pressures, implying hydrostatic inequilibrium and a dissipation timescale near 5e3 yr. The paper concludes that these slim filaments trace parsec-scale shocks, likely from shock--cloud interactions, and that their dispersal can keep pace with SiO freeze-out and explain the widespread SiO and complex organic molecule emission in the CMZ.

Load-bearing premise

All of the pressure and lifetime conclusions rest on converting the 5-sigma continuum non-detection into a volume density by assuming the line-of-sight thickness equals the 0.024 pc filament width; if the true density is lower, turbulent pressure drops below external pressure and the claimed hydrostatic inequilibrium disappears.

Editorial extensions

If this is right

  • Slim filaments constitute a new class of molecular gas structures distinct from the equilibrium dense filaments found in nearby clouds, with lifetimes of order 5e3 years.
  • If the observed surface density of about 0.7 slim filaments per square parsec in the surveyed area is representative, their dissipation can balance the CMZ-wide SiO freeze-out and depletion without requiring additional sources.
  • The molecular abundances in slim filaments being statistically indistinguishable from protostellar outflows implies that shock chemistry, rather than star formation, can account for the complex organic molecule emission in these clouds.
  • Magnetic fields oriented nearly perpendicular to the filament skeletons are consistent with shock compression of magnetized cloud gas, so slim filaments can serve as tracers of dynamic cloud--cloud interactions in the CMZ.

Reading between the lines

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

  • If the shock interpretation is correct, slim filaments could act as visible markers of otherwise invisible shock fronts in CMZ clouds, and their widths might provide a probe of the magnetic field strength in the shocked gas.
  • A testable extension of the replenishment scenario is to search for slim filaments in CMZ clouds with weaker SiO emission: the shock model predicts they should appear at similar surface density wherever SiO is bright, whereas a star-formation origin would concentrate them near protostars.
  • The short dissipation timescale suggests the slim-filament population could be genuinely time-variable, so repeated observations over a decade might catch individual filaments fading, brightening, or losing velocity coherence as shocks propagate through clumpy gas.
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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. The manuscript reports ALMA 1.3 mm spectral line observations toward two massive clouds in the CMZ (the 20 km/s and 50 km/s clouds) and identifies a population of narrow (<0.03 pc) and long (>0.5 pc) filaments seen in SiO 5–4 and eight other molecular lines, but undetected in 1.3 mm continuum at 5σ. The authors measure filament widths, velocity dispersions, and PV coherence, and derive molecular column densities and relative abundances, comparing them to protostellar outflows and dense cores. They then estimate thermal, turbulent, gravitational, magnetic, and external pressures and conclude that turbulent pressure dominates strongly, implying hydrostatic inequilibrium and a short dissipation timescale. They argue that the filaments are associated with parsec-scale shocks and estimate that their dissipation could replenish SiO and complex organic molecules in the CMZ.

Significance. If established, the slim filaments would be a genuinely new class of parsec-scale, shock-related molecular structures in the CMZ, and the proposed replenishment channel for widespread SiO/COMs is appealing and testable. The paper's strengths include the high-resolution ALMA data with nine spectral lines, the clear PV diagrams, the statistical abundance comparison with outflows and dense cores, and the internally consistent replenishment budget. However, the hydrostatic-inequilibrium claim, which is central to the 'new class' interpretation, rests on a density estimate that is actually an upper limit; this weakens the dynamical conclusion. The dissipation timescale and replenishment calculation do not depend on that density and remain valid.

major comments (2)
  1. [4.1, Eq. (3)] The hydrostatic-inequilibrium claim is not established by the calculation in Section 4.1. The continuum non-detection at 5σ yields an upper limit N_H2 ≤ 2.3×10^23 cm^-2, and after assuming a line-of-sight depth equal to the 0.024 pc width, the authors obtain an upper limit n ≤ 3.1×10^6 cm^-3. Inserting this upper limit into P_turb = ρσ_v^2 gives an upper limit P_turb/kB ≤ 1.7×10^10 K cm^-3, not a measured value. Since P_turb is an upper limit, it cannot be used to demonstrate that turbulent pressure exceeds P_ext/kB ≈ 2.6×10^8 K cm^-3; a density at or below P_ext/(m_p σ_v^2) ≈ 1.1×10^5 cm^-3 would place the filament in pressure balance. A quantitative pressure argument requires an independent density constraint rather than a 5σ upper limit.
  2. [4.1] The geometric assumption that the line-of-sight depth equals the observed filament width (0.024 pc) is unvalidated and biases the density estimate upward. If the filaments are elongated along the line of sight or are a foreground/background layer, the true density would be lower, further reducing P_turb and pushing the filaments toward pressure equilibrium. The authors should either justify the geometry with additional data (e.g., absorption measurements or excitation analysis) or explicitly state that the derived turbulent pressure is only an upper limit, which would not support the conclusion that slim filaments are in hydrostatic inequilibrium.
minor comments (6)
  1. [4.1] The sentence 'the total area is∼15 pc−2' should read 'the total area is ∼15 pc^2'; the current notation is dimensionally inconsistent with the surface density that follows.
  2. [3.1] The phrase 'similar filamentary emissions' should be 'similar filamentary emission' for grammatical consistency.
  3. [Throughout] There are several typographical errors, including 'di fferent' in multiple places and 'the the 50 km s−1 cloud' in the caption of Figure 2; these should be corrected.
  4. [3.3] The KS test results would be more informative if the sample sizes were reported, since the small number of filaments limits the statistical power of the comparison.
  5. [Figure 5] Systematic uncertainties in the abundance ratios are not plotted; the authors should either include them or state explicitly why they are omitted.
  6. [4.2] The statement that shocks 'have destroyed most, if not all, of the dust grains' is speculative and not directly supported by the data; consider softening or presenting it as one of several possibilities.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the filament discovery, pressure comparison, and SiO replenishment argument each rest on independent observational inputs rather than on parameters fitted to the conclusions.

full rationale

The central claims are observational: detection of narrow SiO filaments in nine molecular lines, non-detection in 1.3 mm continuum, coherent velocities inconsistent with outflows, and abundances statistically compared with external outflow and core samples. No step defines the conclusion in terms of its own input. In Section 4.1, the density used for turbulent pressure is derived from a 5-sigma continuum upper limit combined with an assumed line-of-sight depth equal to the filament width; the paper then states that turbulent pressure dominates by two to three orders of magnitude. This is an over-interpretation of an upper limit (P_turb is only bounded above, so hydrostatic inequilibrium is not proven), but this is a correctness or inference-quality issue, not circularity: P_turb is not defined in terms of the inequilibrium conclusion, and no fitted parameter is relabeled as a prediction. Self-citations to Paper I and Paper II are used as data source (reduction procedures, adopted temperature, outflow and core comparison samples), not as a theorem that forces the discovery claim. The SiO replenishment calculation is an independent consistency check: APEX SiO mass and freeze-out timescale give a depletion rate, filament SiO mass and dissipation timescale give a replenishment rate, and the required filament surface density is compared with the observed one. The pressure argument could be weakened by lower true densities, but it is not circular for that reason. Overall, no quoted step exhibits an equation or definition that reduces the output to the input.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

The pressure-balance argument depends on several adopted parameters (Tex, Tdust, eta, kappa) and a geometric assumption about line-of-sight depth, none of which are fitted to the central claim; the free parameters enter only through the derived density and column densities.

free parameters (5)
  • Excitation temperature Tex = 70 K
    Adopted from Paper II for LTE column density and SiO mass estimates; directly scales all column densities and the SiO replenishment budget.
  • Dust temperature Tdust = 20 K
    Assumed for converting the 5-sigma continuum upper limit to an H2 column density upper limit; affects the density and thus turbulent pressure.
  • Gas-to-dust mass ratio eta = 100
    Standard ISM assumption used in Eq. 3 for column density upper limit.
  • Dust opacity kappa_nu = 0.817 cm^2/g
    From a power-law assumption with beta=1.5; enters the column density derived from continuum non-detection.
  • Line-of-sight depth equals filament width = 0.024 pc
    Geometric assumption in Section 4.1 to convert column density upper limit to volume density; not independently constrained.
assumptions (4)
  • domain assumption The filaments are at the adopted CMZ distance of 8.1 kpc.
    Used to convert angular sizes to physical sizes; from Reid et al. 2019.
  • domain assumption SiO 5-4 emission traces shock-sputtered silicon.
    Standard interpretation, cited to Schilke et al. 1997; underpins the shock association.
  • domain assumption LTE and optically thin conditions hold for the observed lines.
    Stated in Section 3.3 and Appendix D; needed for column densities and relative abundances.
  • ad hoc to paper The filaments are cylindrical with depth equal to the observed width.
    Introduced in Section 4.1 for the density estimate; not supported by independent evidence.

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Cite this review

Pith. "Pith review of ALMA observations of massive clouds in the central molecular zone: slim filaments tracing parsec-scale shocks." pith.science (2026). https://pith.science/paper/F73Z2ZG5

@misc{pith2026250203913,
  author       = {Pith},
  title        = {Pith review of: ALMA observations of massive clouds in the central molecular zone: slim filaments tracing parsec-scale shocks},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/F73Z2ZG5}},
  note         = {Machine review of arXiv:2502.03913}
}
abstract

The central molecular zone (CMZ) of our Galaxy exhibits widespread emission from SiO and various complex organic molecules (COMs), yet the exact origin of such emission is uncertain. Here we report the discovery of a unique class of long ($>$0.5 pc) and narrow ($<$0.03 pc) filaments in the emission of SiO 5$-$4 and eight additional molecular lines, including several COMs, in our ALMA 1.3 mm spectral line observations toward two massive molecular clouds in the CMZ, which we name as slim filaments. However, these filaments are not detected in the 1.3 mm continuum at the 5$\sigma$ level. Their line-of-sight velocities are coherent and inconsistent with being outflows. The column densities and relative abundances of the detected molecules are statistically similar to those in protostellar outflows but different from those in dense cores within the same clouds. Turbulent pressure in these filaments dominates over self gravity and leads to hydrostatic inequilibrium, indicating that they are a different class of objects than the dense gas filaments in dynamical equilibrium ubiquitously found in nearby molecular clouds. We argue that these newly detected slim filaments are associated with parsec-scale shocks, likely arising from dynamic interactions between shock waves and molecular clouds. The dissipation of the slim filaments may replenish SiO and COMs in the interstellar medium and lead to their widespread emission in the CMZ.

Figures

Figures reproduced from arXiv: 2502.03913 by the authors.

Figure 1
Figure 1. Slim filaments in the CMZ. Panel (a): MeerKAT 1.28 GHz radio emission of the Sgr A region. The red boxes mark the 20 km s−1 cloud and the 50 km s−1 cloud. Panels (b)–(c): Integrated intensity maps of SiO 5–4 in the 20 km s−1 cloud and the 50 km s−1 cloud from ALMA low-resolution (∼1.9′′) observations (project code: 2016.1.00875.S). The blue boxes mark zoom-in regions where slim filaments are detected. The dashed loo… view at source ↗
Figure 2
Figure 2. Integrated maps of molecules in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Mean radial intensity profile perpendicular to the filaments. In￾dividual integrated intensity profiles are shown in gray, while the mean values are shown with black dots. The radius is the projected distance from the gas filament. The red solid line presents the best-fit result of Gaussian fitting. in the CMZ (Paper II). Additionally, CH3CN and H2 13CO are rarely found in outflows. The outflow of a high-mass protos… view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Position-velocity diagrams of SiO 5–4 emissions for the slim filaments along the dashed lines in [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: Molecular abundances normalized with respected to the abun￾dance of CH3OH. The boxes denote the first to third quartiles while the caps mark the full range of abundances in our slim filaments. The median of abundances of each molecule is marked by a horizontal or￾ange …
Figure 6
Figure 6. Figure 6: Distributions of CH3OH and H2O maser spots over the SiO 5–4 integrated maps. The positions of CH3OH masers (Pihlström et al. 2011; Cotton & Yusef-Zadeh 2016) are marked by orange crosses, while the positions of H2O masers are indicated by magenta crosses obtained from …

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Works this paper leans on

70 extracted references · 58 canonical work pages

  1. [1]

    2021, ApJ, 916, 83 André, P

    Abe, D., Inoue, T., Inutsuka, S.-i., & Matsumoto, T. 2021, ApJ, 916, 83 André, P. J., Palmeirim, P., & Arzoumanian, D. 2022, A&A, 667, L1

    work page 2021

  2. [2]

    M., et al

    Ao, Y ., Henkel, C., Menten, K. M., et al. 2013, A&A, 550, A135

    2013

  3. [3]

    Arce, H. G. & Goodman, A. A. 2001, ApJ, 554, 132

    work page 2001

  4. [4]

    G., Shepherd, D., Gueth, F., et al

    Arce, H. G., Shepherd, D., Gueth, F., et al. 2007, in Protostars and Planets V , ed. B. Reipurth, D. Jewitt, & K. Keil, 245

    work page 2007

  5. [5]

    2011, A&A, 529, L6

    Arzoumanian, D., André, P., Didelon, P., et al. 2011, A&A, 529, L6

    2011

  6. [6]

    2019, A&A, 621, A42 Astropy Collaboration, Robitaille, T

    Arzoumanian, D., André, P., Könyves, V ., et al. 2019, A&A, 621, A42 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33

    work page 2019

  7. [7]

    M., Longmore, S

    Bally, J., Rathborne, J. M., Longmore, S. N., et al. 2014, ApJ, 795, 28

    work page 2014

  8. [8]

    T., Longmore, S

    Barnes, A. T., Longmore, S. N., Battersby, C., et al. 2017, MNRAS, 469, 2263

    work page 2017

Show all 70 references
  1. [9]

    A., Melnick, G

    Bergin, E. A., Melnick, G. J., & Neufeld, D. A. 1998, ApJ, 499, 777 CASA Team, Bean, B., Bhatnagar, S., et al. 2022, PASP, 134, 114501

    1998

  2. [10]

    2022, A&A, 667, A6

    Chahine, L., López-Sepulcre, A., Podio, L., et al. 2022, A&A, 667, A6

    2022

  3. [11]

    1999, A&A, 343, 585

    Codella, C., Bachiller, R., & Reipurth, B. 1999, A&A, 343, 585

    1999

  4. [12]

    2019, ApJ, 881, L42

    Cosentino, G., Jiménez-Serra, I., Caselli, P., et al. 2019, ApJ, 881, L42

    2019

  5. [13]

    D., et al

    Cosentino, G., Jiménez-Serra, I., Henshaw, J. D., et al. 2018, MNRAS, 474, 3760

    2018

  6. [14]

    Cotton, W. D. & Yusef-Zadeh, F. 2016, ApJS, 227, 10

    2016

  7. [15]

    C., et al

    Crowe, S., Fedriani, R., Tan, J. C., et al. 2024, arXiv e-prints, arXiv:2410.09253

    2024 arXiv

  8. [16]

    2016, A&A, 586, A149 De Simone, M., Codella, C., Ceccarelli, C., et al

    Csengeri, T., Leurini, S., Wyrowski, F., et al. 2016, A&A, 586, A149 De Simone, M., Codella, C., Ceccarelli, C., et al. 2022, MNRAS, 512, 5214

    2016

  9. [17]

    2014, A&A, 570, A1

    Duarte-Cabral, A., Bontemps, S., Motte, F., et al. 2014, A&A, 570, A1

    2014

  10. [18]

    P., Schlemmer, S., Schilke, P., Stutzki, J., & Müller, H

    Endres, C. P., Schlemmer, S., Schilke, P., Stutzki, J., & Müller, H. S. P. 2016, Journal of Molecular Spectroscopy, 327, 95 Ferrière, K., Gillard, W., & Jean, P. 2007, A&A, 467, 611

    2016

  11. [19]

    2016, A&A, 586, A50

    Ginsburg, A., Henkel, C., Ao, Y ., et al. 2016, A&A, 586, A50

    2016

  12. [20]

    Goldsmith, P. F. & Langer, W. D. 1999, ApJ, 517, 209

    1999

  13. [21]

    2018, A&A, 610, A77

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

    2018

  14. [22]

    D., Barnes, A

    Henshaw, J. D., Barnes, A. T., Battersby, C., et al. 2023, in Astronomical Society of the Pacific Conference Series, V ol. 534, Protostars and Planets VII, ed. S. Inutsuka, Y . Aikawa, T. Muto, K. Tomida, & M. Tamura, 83

    2023

  15. [23]

    D., Krumholz, M

    Henshaw, J. D., Krumholz, M. R., Butterfield, N. O., et al. 2022, MNRAS, 509, 4758

    2022

  16. [24]

    D., Longmore, S

    Henshaw, J. D., Longmore, S. N., Kruijssen, J. M. D., et al. 2016, MNRAS, 457, 2675

    2016

  17. [25]

    2022, ApJ, 925, 165

    Heywood, I., Rammala, I., Camilo, F., et al. 2022, ApJ, 925, 165

    2022

  18. [26]

    Hildebrand, R. H. 1983, QJRAS, 24, 267

    1983

  19. [27]

    Immer, K., Kauffmann, J., Pillai, T., Ginsburg, A., & Menten, K. M. 2016, A&A, 595, A94

    2016

  20. [28]

    2018, PASJ, 70, S53

    Inoue, T., Hennebelle, P., Fukui, Y ., et al. 2018, PASJ, 70, S53

    2018

  21. [29]

    2021, in Astronomical Society of the Pacific Conference Series, V ol

    Inutsuka, S. 2021, in Astronomical Society of the Pacific Conference Series, V ol. 528, New Horizons in Galactic Center Astronomy and Beyond, ed. M. Tsuboi & T. Oka, 271 Jiménez-Serra, I., Caselli, P., Fontani, F., et al. 2014, MNRAS, 439, 1996 Jiménez-Serra, I., Caselli, P., ...

    2021

  22. [30]

    2016, A&A, 586, A27

    Kainulainen, J., Hacar, A., Alves, J., et al. 2016, A&A, 586, A27

    2016

  23. [31]

    L., Evans, N

    Kauffmann, J., Bertoldi, F., Bourke, T. L., Evans, N. J., I., & Lee, C. W. 2008, A&A, 487, 993

    2008

  24. [32]

    2017, A&A, 603, A89

    Kauffmann, J., Pillai, T., Zhang, Q., et al. 2017, A&A, 603, A89

    2017

  25. [33]

    Koch, E. W. & Rosolowsky, E. W. 2015, MNRAS, 452, 3435

    2015

  26. [34]

    2017, ApJ, 850, 77

    Krieger, N., Ott, J., Beuther, H., et al. 2017, ApJ, 850, 77

    2017

  27. [35]

    Kruijssen, J. M. D., Dale, J. E., Longmore, S. N., et al. 2019, MNRAS, 484, 5734

    2019

  28. [36]

    Kruijssen, J. M. D., Longmore, S. N., Elmegreen, B. G., et al. 2014, MNRAS, 440, 3370

    2014

  29. [37]

    Lada, C. J. & Fich, M. 1996, ApJ, 459, 638

    1996

  30. [38]

    2020, Research in As- tronomy and Astrophysics, 20, 031

    Li, C., Wang, H.-C., Wu, Y .-W., Ma, Y .-H., & Lin, L.-H. 2020, Research in As- tronomy and Astrophysics, 20, 031

    2020

  31. [39]

    B., Ho, P

    Liu, H. B., Ho, P. T. P., Wright, M. C. H., et al. 2013, ApJ, 770, 44

    2013

  32. [40]

    N., Bally, J., Testi, L., et al

    Longmore, S. N., Bally, J., Testi, L., et al. 2013, MNRAS, 429, 987 López-Sepulcre, A., Walmsley, C. M., Cesaroni, R., et al. 2011, A&A, 526, L2

    2013

  33. [41]

    2016, A&A, 595, A122

    Louvet, F., Motte, F., Gusdorf, A., et al. 2016, A&A, 595, A122

    2016

  34. [42]

    2020, ApJ, 894, L14

    Lu, X., Cheng, Y ., Ginsburg, A., et al. 2020, ApJ, 894, L14

    2020

  35. [43]

    2021, ApJ, 909, 177

    Lu, X., Li, S., Ginsburg, A., et al. 2021, ApJ, 909, 177

    2021

  36. [44]

    2024, ApJ, 962, 39

    Lu, X., Liu, J., Pillai, T., et al. 2024, ApJ, 962, 39

    2024

  37. [45]

    2017, ApJ, 839, 1

    Lu, X., Zhang, Q., Kauffmann, J., et al. 2017, ApJ, 839, 1

    2017

  38. [46]

    B., et al

    Lu, X., Zhang, Q., Liu, H. B., et al. 2018, ApJ, 855, 9

    2018

  39. [47]

    Mangum, J. G. & Shirley, Y . L. 2015, PASP, 127, 266 Martín-Pintado, J., de Vicente, P., Fuente, A., & Planesas, P. 1997, ApJ, 482, L45 Martín-Pintado, J., Rizzo, J. R., de Vicente, P., Rodríguez-Fernández, N. J., &

    2015

  40. [48]

    2001, ApJ, 548, L65

    Fuente, A. 2001, ApJ, 548, L65

    2001

  41. [49]

    M., Wilson, R

    Menten, K. M., Wilson, R. W., Leurini, S., & Schilke, P. 2009, ApJ, 692, 47

    2009

  42. [50]

    Mills, E. A. C. & Morris, M. R. 2013, ApJ, 772, 105

    2013

  43. [51]

    C., Liu, H

    Minh, Y . C., Liu, H. B., & Galva´n-Madrid, R. 2016, ApJ, 824, 99

    2016

  44. [52]

    C., Liu, H

    Minh, Y . C., Liu, H. B., Su, Y .-N., et al. 2015, ApJ, 808, 86

    2015

  45. [53]

    & Serabyn, E

    Morris, M. & Serabyn, E. 1996, ARA&A, 34, 645

    1996

  46. [54]

    2007, A&A, 476, 1243 Müller, H

    Motte, F., Bontemps, S., Schilke, P., et al. 2007, A&A, 476, 1243 Müller, H. S. P., Schlöder, F., Stutzki, J., & Winnewisser, G. 2005, Journal of Molecular Structure, 742, 215 Müller, H. S. P., Thorwirth, S., Roth, D. A., & Winnewisser, G. 2001, A&A, 370, L49 Nguyen-Lu’o’ng, Q...

    2007

  47. [55]

    T., Immer, K., et al

    Nonhebel, M., Barnes, A. T., Immer, K., et al. 2024, A&A, 691, A70

    2024

  48. [56]

    2017, MNRAS, 467, 2723 Paré, D., Butterfield, N

    Palau, A., Walsh, C., Sánchez-Monge, Á., et al. 2017, MNRAS, 467, 2723 Paré, D., Butterfield, N. O., Chuss, D. T., et al. 2024, ApJ, 969, 150

    2017

  49. [57]

    M., Poynter, R

    Pickett, H. M., Poynter, R. L., Cohen, E. A., et al. 1998, J. Quant. Spectr. Rad. Transf., 60, 883 Pihlström, Y . M., Sjouwerman, L. O., & Fish, V . L. 2011, ApJ, 739, L21

    1998

  50. [58]

    2007, ApJ, 654, 361

    Qiu, K., Zhang, Q., Beuther, H., & Yang, J. 2007, ApJ, 654, 361

    2007

  51. [59]

    J., Menten, K

    Reid, M. J., Menten, K. M., Brunthaler, A., et al. 2019, ApJ, 885, 131

    2019

  52. [60]

    A., Martín-Pintado, J., Martín, S., & Morris, M

    Requena-Torres, M. A., Martín-Pintado, J., Martín, S., & Morris, M. R. 2008, ApJ, 672, 352

    2008

  53. [61]

    A., Martín-Pintado, J., Rodríguez-Franco, A., et al

    Requena-Torres, M. A., Martín-Pintado, J., Rodríguez-Franco, A., et al. 2006, A&A, 455, 971

    2006

  54. [62]

    & Bressert, E

    Robitaille, T. & Bressert, E. 2012, APLpy: Astronomical Plotting Library in Python

    2012

  55. [63]

    M., Pineau des Forets, G., & Flower, D

    Schilke, P., Walmsley, C. M., Pineau des Forets, G., & Flower, D. R. 1997, A&A, 321, 293 Schöier, F. L., van der Tak, F. F. S., van Dishoeck, E. F., & Black, J. H. 2005, A&A, 432, 369

    1997

  56. [64]

    Shirley, Y . L. 2015, PASP, 127, 299

    2015

  57. [65]

    Towner, A. P. M., Ginsburg, A., Dell’Ova, P., et al. 2024, ApJ, 960, 48 V oronkov, M. A., Caswell, J. L., Ellingsen, S. P., Green, J. A., & Breen, S. L. 2014, MNRAS, 439, 2584

    2024

  58. [66]

    Wallace, J., Battersby, C., Mills, E. A. C., et al. 2022, ApJ, 939, 58

    2022

  59. [67]

    2014, MNRAS, 439, 3275

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

    2014

  60. [68]

    2024, A&A, 684, A140

    Yang, K., Qiu, K., & Pan, X. 2024, A&A, 684, A140

    2024

  61. [69]

    35" 40" 45

    Yusef-Zadeh, F., Cotton, W., Viti, S., Wardle, M., & Royster, M. 2013, ApJ, 764, L19 Article number, page 9 of 14 A&A proofs: manuscript no. clean SO 65 54 0.1 pc 0.02 0.05 0.1 0.2 H2CO 30, 3 20, 2 0.1 pc 0.02 0.05 0.1 0.2 HNCO 100, 10 90, 9 0.1 pc 0.02 0.05 0.1 HC3N 24 23 0.1...

    2013

  62. [70]

    35" 40" 45

    Yang, K. et al.: Gas Filaments in CMZ Clouds SO 65 54 0.1 pc 0.02 0.05 0.1 H2CO 30, 3 20, 2 0.1 pc 0.05 0.1 0.2 HNCO 100, 10 90, 9 0.1 pc 0.02 0.05 0.1 HC3N 24 23 0.1 pc 0.02 0.05 0.1 17h45m35.0s 34.5s 34.0s -29°04'30" 35" 40" 45" Right Ascension (J2000) Declination (J2000) CH...

    2015

Pith tools

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