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REVIEW 3 major objections 4 minor 89 references

The Cygnus Allscale Survey of Chemistry and Dynamical Environments: CASCADE. IV. Unveiling the hidden structures in DR18

T0 review · 3 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read Narrow SiO emission around DR18 traces slow, UV-irradiated shocks rather than protostellar outflows.

desk verdict Solid first high-resolution view of DR18 with a suggestive SiO-shock interpretation that the data don't uniquely support, and a bound-core claim that leans on one abundance. read the letter →

arxiv 2501.04518 v1 pith:OZMRQNWW submitted 2025-01-08 astro-ph.GA astro-ph.SR

W.-J. Kim , H. Beuther , F. Wyrowski , K. M. Menten , N. Schneider , Á. Sánchez-Monge , A. Brunthaler , T. Csengeri
show 14 more authors
C. Romero N. Cunningham L. Bouscasse J. M. Winters F. Comerón V. S. Veena A. Ginsburg D. Semenov C. Gieser A. Hernández-Gómez S. A. Dzib I.-M. Skretas I. B. Christensen P. Schilke
This is my paper · ORCID
classification astro-ph.GAastro-ph.SR
keywords DR18Cygnus-XSiOemissionphotodissociationregionlow-velocityshocksN2H+coresstellarfeedbackcometaryHII
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

Toward DR18, a cometary globule in Cygnus-X sitting beside the Cyg OB2 association, the paper combines NOEMA and IRAM 30 m observations at $\sim$3\arcsec$-$4\arcsec with archival infrared and radio maps to separate the action of the embedded B2 star DR18-05 from the external UV bath of Cyg OB2. It argues that the B2 star has carved a cometary HII region whose shell carries photodissociation regions, while the extended ionized gas surrounding the globule is photoevaporating under the OB2 association's radiation. The central new claim is that the narrow ($0.8$\,--\,$2.0$ km s$^{-1}$), low-abundance SiO emission partly encircling the HII region is not an outflow signature but a PDR product: molecular gas marginally compressed by $\sim$5 km s$^{-1}$ shocks in a medium of $n_{\mathrm{H}} \sim 10^4$\,--\,$10^5$ cm$^{-3}$, irradiated at $G_0 \sim 10^2$\,--\,$10^3$. The paper also identifies 18 N$_2$H$^+$ cores, half of which it judges gravitationally bound.

What carries the argument

The load-bearing tool is the Paris-Durham irradiated low-velocity shock model grid: a code that computes gas-phase chemistry across a magnetised C-type shock front illuminated by an external UV field. The paper feeds it shock velocities of 5, 10, and 20 km s$^{-1}$, densities $10^2$\,--\,$10^5$ cm$^{-3}$, and $G_0$ from 0.1 to $10^3$, and compares the predicted $X(\mathrm{SiO})$ and $X(\mathrm{N_2H^+})$ with the observed values. On the observational side, the key diagnostic is the combination of narrow SiO line widths, low abundance, spatial coincidence with H$_2$ 1\,--\,0 S(1) and 8 $\mu$m PAH emission, and the [4.5]/[3.6] flux ratio, which together separate PDR-shock SiO from outflow SiO.

What would settle it

Observe the SiO $J{=}2$\,--\,$1$ line toward the east and north shells at a velocity resolution below $0.25$ km s$^{-1}$: the paper's model predicts a single narrow component near the systemic velocity, so resolving broad wings ($>$8 km s$^{-1}$) or a second kinematic component tied to a YSO would falsify the low-velocity-shock interpretation.

Watch

Extended reading notes

Core claim

Using 3.6 mm continuum plus line emission from HCO$^+$, HCN, HNC, N$_2$H$^+$, SiO, NH$_2$D, and other species, the paper traces a layered interface in DR18: dust and free-free continuum show that DR18-05 (a B2 star) powers the inner cometary HII region, the 8 $\mu$m and H$_2$ 1\,--\,0 S(1) emission trace PDR shells, and HCO$^+$ outlines the molecular rim. SiO $J{=}2$\,--\,$1$ emission is detected only in those PDR shells, with narrow line widths ($0.8$\,--\,$2.0$ km s$^{-1}$) and $X(\mathrm{SiO}) \sim 5\times10^{-11}$ to $1\times10^{-10}$, spatially coincident with H$_2$ and anti-coincident with N$_2$H$^+$ cores. The SiO/N$_2$H$^+$ ratio rises outward from the dense cores, and the [4.5]/[3.6] IRAC ratio is below the EGO threshold, ruling out outflow shocks. Matching the Paris-Durham irradiated shock grid, the authors conclude that the SiO arises in gas compressed by low-velocity ($\sim$5 km s$^{-1}$) C-type shocks under $G_0 \sim 10^2$\,--\,$10^3$ with $n_{\mathrm{H}} \sim 10^4$\,--\,$10^5$ cm$^{-3}$.

Load-bearing premise

The claim that half the N$_2$H$^+$ cores are gravitationally bound rests on assuming the N$_2$H$^+$ abundance is $4\times10^{-10}$ relative to H$_2$; the paper itself shows that adopting $4\times10^{-9}$ instead would make every one of the 18 cores unbound.

Editorial extensions

If this is right

  • SiO in this region becomes a tracer of UV-irradiated, low-velocity compressed gas, not only of protostellar outflows, so narrow SiO can be used to find slow compression fronts in other PDR globules.
  • The cometary HII region is shaped by DR18-05 plus a champagne flow, while the extended free-free emission around DR18 is photoevaporation driven by Cyg OB2 rather than by DR18-05.
  • Half of the 18 N$_2$H$^+$ cores, mostly behind the PDRs with $T_{\mathrm{HCN/HNC}}<30$ K, are gravitationally bound under the adopted N$_2$H$^+$ abundance, suggesting that the HII region's expansion may have helped form them.
  • The four cores nearest the HII region are unbound, consistent with the expanding ionized gas disrupting or supporting them.
  • The irradiated shock models predict far less N$_2$H$^+$ than is observed, explaining the spatial and velocity separation between SiO and N$_2$H$^+$.

Reading between the lines

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

  • The narrow-SiO-plus-PDR recipe may generalise to other globules and pillars in Cygnus-X; a blind search for narrow SiO around OB associations could reveal hidden low-velocity shock layers.
  • The bound-core result is hostage to the N$_2$H$^+$ abundance: if the true abundance is closer to $4\times10^{-9}$, the paper's own calculation makes all 18 cores unbound, so a direct abundance measurement would either strengthen or remove the triggered star formation claim.
  • The Paris-Durham grid predicts essentially no N$_2$H$^+$ in the shocked PDR layer, so sensitive N$_2$H$^+$ observations at the SiO peak positions could test whether the modelled layer separation is real.
  • The shell age and wind luminosity estimates scale with the adopted 1.4 kpc distance; a revised parallax distance to DR18 would linearly rescale core masses and mechanical luminosities.
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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

3 major / 4 minor

Summary. The paper presents new 3.6 mm NOEMA + IRAM 30m + GBT/MUSTANG-2 continuum and molecular line observations of the DR18 globule in Cygnus-X, complemented by GLOSTAR 6 cm, Spitzer, and near-infrared data. The authors analyze the 6 cm–3.6 mm spectral index to separate dust and free-free emission, conclude that the cometary HII region is shaped by the B2 star DR18-05 with an additional photoevaporating component driven by Cyg OB2, identify 18 N2H+ cores and derive their masses and virial parameters, and report narrow, low-abundance SiO emission confined to PDR-like regions. They interpret the SiO emission as tracing low-velocity (about 5 km/s) C-type shocks in gas with nH about 10^4–10^5 cm^-3 and G0 about 10^2–10^3, based on comparison with the Paris-Durham irradiated shock grid.

Significance. If the results hold, this work provides one of the first high-resolution molecular-line views of DR18 and a useful case study of how an OB association and an embedded B star jointly shape a globule. The continuum spectral index analysis is careful about uv-coverage and matching resolutions, and the use of external benchmarks (GLOSTAR, Herschel, Spitzer, near-IR line maps) is a strength. The paper also explicitly tests the wind versus ionized-gas pressure balance for the shell, which is a concrete, falsifiable dynamical argument. However, the two headline claims—that half the cores are gravitationally bound and that the SiO arises from 5 km/s shocks—each rely on assumptions that the paper itself shows are not uniquely determined: the N2H+ abundance and the absence of a no-shock photodesorption model in the comparison grid.

major comments (3)
  1. [Section 4.5, Eq. (6) and following paragraph] The claim that half of the 18 cores are gravitationally bound rests entirely on the adopted N2H+/H2 abundance of 4 x 10^-10. The paper itself states that with X(N2H+) = 4 x 10^-9, all cores would be unbound with virial parameters of 6–69. Because the abundance is not measured locally and the two values bracket the full 'bound/unbound' classification, the abstract's statement that half the cores are bound needs to be presented as conditional on this assumption, with the adopted value better justified from data in the same region (e.g., from a comparison with Herschel column densities) rather than from literature averages.
  2. [Section 5.2, Fig. 16 and Table 4] The central interpretive claim—that SiO arises from marginally compressed gas in ~5 km/s shocks—is underdetermined because the Paris-Durham grid excludes ice mantles and provides no no-shock PDR or photodesorption model for comparison. The paper itself cites Walmsley et al. (1999) and Schilke et al. (2001) for the photodesorption of Si-bearing ice mantles and notes that the observed X(SiO) ~ 5e-11 to 1e-10 is close to values found in the Orion Bar PDR. The grid's exclusion of ice mantles means it cannot produce SiO via photodesorption, so the match of one shocked-grid point to the observed abundance is a necessary but not sufficient condition. The authors should either quantify the expected SiO abundance from a non-shocked PDR model with photodesorption, or explicitly soften the conclusion to 'consistent with, but not uniquely requiring, low-velocity shocks.'
  3. [Section 4.5, Table 3 and Eq. (8)] The core masses, virial masses, and virial parameters in Table 3 are presented without any propagated uncertainties, and the derived quantities depend on the leaf areas, fitted N2H+ column densities, line widths, and the adopted abundance. Given that the 'half bound' conclusion is based on comparing alpha_vir to the threshold of 2, individual alpha_vir values of 1.0–2.0 (e.g., C5, C6, C8, C16) are statistically indistinguishable from the unbound regime without error bars. At minimum, a table of fractional uncertainties or a brief sensitivity analysis (e.g., varying X(N2H+) and line width within the reported scatter) is needed before the bound/unbound split can be assessed.
minor comments (4)
  1. [Figure 13 caption] The caption contains a typo: 'NOEAM-alone data' should read 'NOEMA-alone data.'
  2. [Section 4.5, paragraph after Eq. (6)] The formula for N(SiO) in the text is garbled: '1.8 x 10^12 R Tmb dυ cm^-2' should presumably be 1.8 x 10^12 times the integrated main-beam temperature (∫ Tmb dv). Please write the integral explicitly.
  3. [Table 3] The note to Table 3 contains a typo: 'Heree' should be 'Here.'
  4. [Section 4.2 (SiO paragraph)] There is a minor inconsistency in the star name: the text uses 'D18-05' in the sentence 'the Hii region of D18-05' while the rest of the paper uses DR18-05; please unify.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the central results are benchmarked against external data and model grids; the assumption-sensitive virial classification is conditional, not circular.

full rationale

I walked the paper's derivation chain and found no step in which a claimed prediction or first-principles result reduces by construction to its own inputs. The 3.6 mm versus 6 cm spectral index, the Lyman continuum flux, the core masses and virial parameters, and the SiO column density and abundance are all computed from standard formulae and external data sets (GLOSTAR, Herschel, Spitzer, Bonne et al. 2023, XCLASS, Hacar et al. 2020 calibration). The SiO shock interpretation is a comparison of the observed X(SiO) with the externally published Paris-Durham irradiated shock grid; the grid was not fitted to these observations, and the observed abundance is not defined in terms of the grid output. The model comparison is underdetermined because the grid excludes ice-mantle chemistry and therefore cannot test the photodesorption/PDR alternative, but underdetermination is a scientific limitation, not circularity. The virial classification of the N2H+ cores depends on the adopted N2H+/H2 abundance of 4 x 10^-10, and the paper explicitly discloses that adopting 4 x 10^-9 would make all 18 cores unbound; this is an assumption-sensitivity caveat, not a fitted input renamed as a prediction. The self-citations present (Beuther et al. 2022 for CASCADE data reduction, Kim et al. 2023 as one example among many for low SiO abundances in low-velocity shocked gas) are descriptive or contextual and are not load-bearing for the paper's central claims. No circular step can be exhibited from the text, so the circularity score is low.

Assumptions & free parameters 5 free parameters · 7 assumptions · 0 invented entities

The central claims rest on literature distances, temperatures, and abundance ratios rather than new first-principles inputs. The most consequential choices are the fixed N2H+/H2 abundance and the selected parameters of the Paris-Durham shock grid; both are reasonable but unverified for this specific region, and both affect headline conclusions.

free parameters (5)
  • X(N2H+) abundance ratio = 4 x 10^-10
    Adopted to convert N(N2H+) to N(H2) in Eq. (6), setting core masses and virial parameters. The paper notes that 4 x 10^-9 would make all cores unbound.
  • Shock velocity vs = ~5 km/s
    Selected from the Paris-Durham grid to match the observed X(SiO); not independently constrained by the DR18 data alone.
  • Radiation field G0 = 10^2 to 10^3 Mathis units
    Selected range consistent with the observed X(SiO) and the Herschel-based estimate G0 ~ 10^3; used in the SiO model comparison.
  • Pre-shock density nH = 10^4 to 10^5 cm^-3
    Chosen from the model grid to match the observed SiO abundance, motivated by the proximity of dense N2H+ cores.
  • SiO excitation temperature Tex = 10 K
    Assumed in the N(SiO) conversion following Csengeri et al. (2016); directly scales X(SiO).
assumptions (7)
  • domain assumption Distance to DR18 is 1.4 kpc
    Adopted from Rygl et al. (2012) maser parallaxes; all size, mass, and luminosity scales depend on it.
  • domain assumption The HII region interior is optically thin at 6 cm and 3.6 mm
    Required for Eq. (9) to derive Lyman continuum fluxes; justified by the extended, non-compact morphology.
  • domain assumption A constant N2H+/H2 abundance of 4 x 10^-10 applies to all 18 cores
    Central to the core mass and virial parameter estimates; justified via Redaelli et al. (2019) models but not measured locally.
  • standard math LTE and isothermal excitation for N2H+ in XCLASS fitting
    Assumed in Section 4.5 for column density determination; a standard approximation for ground-state lines.
  • domain assumption HCN/HNC ratio to gas temperature calibration of Hacar et al. (2020) holds in DR18
    Used to derive THCN/HNC; the method was calibrated in Orion and is applied here without local verification.
  • domain assumption Paris-Durham shock grid with b=1, PAH abundance 10^-8, and gas-phase Si abundance 3 x 10^-6 is applicable
    The SiO interpretation depends on these fixed model inputs from Kristensen et al. (2023), which may not match DR18's exact conditions.
  • domain assumption SiO emission is optically thin and at Tex = 10 K
    Assumed in the conversion from integrated intensity to N(SiO); uncertainties here propagate directly into X(SiO).

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Cite this review

Pith. "Pith review of The Cygnus Allscale Survey of Chemistry and Dynamical Environments: CASCADE. IV. Unveiling the hidden structures in DR18." pith.science (2026). https://pith.science/paper/OZMRQNWW

@misc{pith2026250104518,
  author       = {Pith},
  title        = {Pith review of: The Cygnus Allscale Survey of Chemistry and Dynamical Environments: CASCADE. IV. Unveiling the hidden structures in DR18},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OZMRQNWW}},
  note         = {Machine review of arXiv:2501.04518}
}
abstract

The Cygnus-X complex is a massive, nearby (1.4 kpc) star-forming region with several OB associations. As part of the Cygnus Allscale Survey of Chemistry and Dynamical Environments (CASCADE) program, we carried out 3.6 millimeter (mm) continuum and spectral line high-resolution observations ($\sim$ 3 - 4$''$) toward DR18, covering several molecular species with the Northern Extended Millimeter Array (NOEMA) and the Institut de Radioastronomie Millim\'etrique (IRAM) 30m telescope. In addition, multi-wavelength archival datasets were used to provide a comprehensive analysis of the region. A comparison of the 3.6mm and 6 cm continuum emission confirms that a B2 star (DR18-05) shapes the cometary HII region in the DR18 cavity, with ionized gas escaping toward the OB2 association. On the other hand, the extended 3.6mm and 6 cm continuum emission are likely to trace photoevaporating ionized gas from ultraviolet radiation from the Cyg OB2 association, not from DR18-05. The shell structure around DR18-05 indicates photodissociation regions (PDRs) formed by the expanding HII region and photo-erosion from DR18-05 and OB2 stars. We also identified 18 compact cores with N$_2$H$^+$ emission, half of which are gravitationally bound and mostly located in colder regions behind the PDRs. The SiO emission is found only in PDRs, with narrow-line widths ( 0.8 - 2.0 km s$^{-1}$) and lower abundances (X(SiO) $\sim$ 5$\times$10$^{-11}$ - 1$\times$10$^{-10}$). Comparing with the UV irradiated shock models, we suggest that the SiO emission partially encompassing the HII region arises from the molecular gas region, marginally compressed by low-velocity shocks with $\sim$ 5 km s$^{-1}$, irradiated by external UV radiation (G$_{\rm 0} \sim 10^{2} - 10^{3}$), as they traverse through a medium with $n_{\rm H} \sim 10^{4}$ to 10$^5$ cm$^{-3}$.

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Works this paper leans on

89 extracted references · 65 canonical work pages

  1. [1]

    & Pérez Gutiérrez, M

    Bachiller, R. & Pérez Gutiérrez, M. 1997, ApJ, 487, L93

    1997

  2. [2]

    M., Koenig, X

    Beerer, I. M., Koenig, X. P., Hora, J. L., et al. 2010, ApJ, 720, 679

    2010

  3. [3]

    A., Churchwell, E., Babler, B

    Benjamin, R. A., Churchwell, E., Babler, B. L., et al. 2003, PASP, 115, 953

    2003

  4. [4]

    & McKee, C

    Bertoldi, F. & McKee, C. F. 1992, ApJ, 395, 140

    1992

  5. [5]

    K., & Saito, M

    Beuther, H., Sridharan, T. K., & Saito, M. 2005, ApJ, 634, L185

    2005

  6. [6]

    M., et al

    Beuther, H., Wyrowski, F., Menten, K. M., et al. 2022, A&A, 665, A63

    2022

  7. [7]

    Black, J. H. & van Dishoeck, E. F. 1987, ApJ, 322, 412

    1987

  8. [8]

    2023, ApJ, 951, 39

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

    2023

Show all 89 references
  1. [9]

    1996, A&A, 311, 858

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

    1996

  2. [10]

    M., Dzib, S

    Brunthaler, A., Menten, K. M., Dzib, S. A., et al. 2021, A&A, 651, A85

    2021

  3. [11]

    G., Brand, P

    Burton, M. G., Brand, P. W. J. L., Geballe, T. R., & Webster, A. S. 1989, MN- RAS, 236, 409

    1989

  4. [12]

    2019, ApJS, 241, 1

    Cao, Y ., Qiu, K., Zhang, Q., et al. 2019, ApJS, 241, 1

    2019

  5. [13]

    Carlsten, S. G. & Hartigan, P. M. 2018, ApJ, 869, 77

    2018

  6. [14]

    M., Snell, R

    Carpenter, J. M., Snell, R. L., & Schloerb, F. P. 1990, ApJ, 362, 147

    1990

  7. [15]

    J., Myers, P

    Caselli, P., Benson, P. J., Myers, P. C., & Tafalla, M. 2002, ApJ, 572, 238

    2002

  8. [16]

    I., Abbott, D

    Castor, J. I., Abbott, D. C., & Klein, R. I. 1975, ApJ, 195, 157

    1975

  9. [17]

    T., Jackson, J

    Chambers, E. T., Jackson, J. M., Rathborne, J. M., & Simon, R. 2009, ApJS, 181, 360

    2009

  10. [18]

    1999, in NATO Advanced Study Institute (ASI) Series C, V ol

    Churchwell, E. 1999, in NATO Advanced Study Institute (ASI) Series C, V ol. 540, The Origin of Stars and Planetary Systems, ed. C. J. Lada & N. D. Ky- lafis, 515

    1999

  11. [19]

    1999, A&A, 343, 585 Comerón, F., Schneider, N., & Djupvik, A

    Codella, C., Bachiller, R., & Reipurth, B. 1999, A&A, 343, 585 Comerón, F., Schneider, N., & Djupvik, A. A. 2022, A&A, 660, A106 Comerón, F., Schneider, N., & Russeil, D. 2005, A&A, 433, 955 Comerón, F. & Torra, J. 1999, A&A, 349, 605

    1999

  12. [20]

    2019, ApJ, 881, L42

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

    2019

  13. [21]

    D., et al

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

    2018

  14. [22]

    D., et al

    Cosentino, G., Jiménez-Serra, I., Henshaw, J. D., et al. 2020, MNRAS, 499, 1666

    2020

  15. [23]

    2016, A&A, 586, A149

    Csengeri, T., Leurini, S., Wyrowski, F., et al. 2016, A&A, 586, A149

    2016

  16. [24]

    J., Brogan, C

    Cyganowski, C. J., Brogan, C. L., Hunter, T. R., Churchwell, E., & Zhang, Q. 2011, ApJ, 729, 124

    2011

  17. [25]

    J., Reid, M

    Cyganowski, C. J., Reid, M. J., Fish, V . L., & Ho, P. T. P. 2003, ApJ, 596, 344

    2003

  18. [26]

    J., Whitney, B

    Cyganowski, C. J., Whitney, B. A., Holden, E., et al. 2008, AJ, 136, 2391

    2008

  19. [27]

    R., Ade, P

    Dicker, S. R., Ade, P. A. R., Aguirre, J., et al. 2014, Journal of Low Temperature Physics, 176, 808

    2014

  20. [28]

    A., Comerón, F., & Schneider, N

    Djupvik, A. A., Comerón, F., & Schneider, N. 2017, A&A, 599, A37

    2017

  21. [29]

    2014, A&A, 570, A1

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

    2014

  22. [30]

    2013, A&A, 558, A125

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

    2013

  23. [31]

    A., Rodríguez, L

    Dzib, S. A., Rodríguez, L. F., Loinard, L., et al. 2013, ApJ, 763, 139

    2013

  24. [32]

    L., White, G

    Emig, K. L., White, G. J., Salas, P., et al. 2022, A&A, 664, A88

    2022

  25. [33]

    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

    2016

  26. [34]

    1994, ApJ, 429, 268

    Garay, G., Lizano, S., & Gomez, Y . 1994, ApJ, 429, 268

    1994

  27. [35]

    D., Dicker, S., et al

    Ginsburg, A., Anderson, L. D., Dicker, S., et al. 2020, ApJS, 248, 24

    2020

  28. [36]

    2019, A&A, 622, A100

    Godard, B., Pineau des Forêts, G., Lesaffre, P., et al. 2019, A&A, 622, A100

    2019

  29. [37]

    N., Rugel, M

    Gong, Y ., Ortiz-León, G. N., Rugel, M. R., et al. 2023, A&A, 678, A130

    2023

  30. [38]

    E., Landecker, T

    Gottschalk, M., Kothes, R., Matthews, H. E., Landecker, T. L., & Dent, W. R. F. 2012, A&A, 541, A79

    2012

  31. [39]

    2010, ApJ, 723, 971

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

    2010

  32. [40]

    Gusdorf, A., Pineau Des Forêts, G., Cabrit, S., & Flower, D. R. 2008, A&A, 490, 695

    2008

  33. [41]

    D., & van Dishoeck, E

    Hacar, A., Bosman, A. D., & van Dishoeck, E. F. 2020, A&A, 635, A4

    2020

  34. [42]

    J., Scowen, P

    Hester, J. J., Scowen, P. A., Sankrit, R., et al. 1996, AJ, 111, 2349

    1996

  35. [43]

    2007, A Spitzer Legacy Survey of the Cygnus-X Complex, Spitzer Proposal ID #40184 Jiménez-Serra, I., Caselli, P., Tan, J

    Hora, J., Bontemps, S., Megeath, T., et al. 2007, A Spitzer Legacy Survey of the Cygnus-X Complex, Spitzer Proposal ID #40184 Jiménez-Serra, I., Caselli, P., Tan, J. C., et al. 2010, MNRAS, 406, 187

    2007

  36. [44]

    Kauffmann, J., Pillai, T., & Goldsmith, P. F. 2013, ApJ, 779, 185

    2013

  37. [45]

    J., Urquhart, J

    Kim, W. J., Urquhart, J. S., Veena, V . S., et al. 2023, A&A, 679, A123

    2023

  38. [46]

    J., Wyrowski, F., Urquhart, J

    Kim, W. J., Wyrowski, F., Urquhart, J. S., Menten, K. M., & Csengeri, T. 2017, A&A, 602, A37

    2017

  39. [47]

    M., Ossenkopf, V ., et al

    Koumpia, E., Harvey, P. M., Ossenkopf, V ., et al. 2015, A&A, 580, A68

    2015

  40. [48]

    E., Godard, B., Guillard, P., Gusdorf, A., & Pineau des Forêts, G

    Kristensen, L. E., Godard, B., Guillard, P., Gusdorf, A., & Pineau des Forêts, G. 2023, A&A, 675, A86 Article number, page 20 of 25 W.-J. Kim et al.: Unveiling the hidden structures in DR18

    2023

  41. [49]

    Kurtz, S., Churchwell, E., & Wood, D. O. S. 1994, ApJS, 91, 659 Le Petit, F., Nehmé, C., Le Bourlot, J., & Roueff, E. 2006, ApJS, 164, 506

    1994

  42. [50]

    2024, arXiv e-prints, arXiv:2411.19489

    Liu, R., Liu, T., Jiménez-Serra, I., et al. 2024, arXiv e-prints, arXiv:2411.19489

    2024 arXiv

  43. [51]

    1992, A&A, 254, 315

    Martin-Pintado, J., Bachiller, R., & Fuente, A. 1992, A&A, 254, 315

    1992

  44. [52]

    S., Mezger, P

    Mathis, J. S., Mezger, P. G., & Panagia, N. 1983, A&A, 128, 212

    1983

  45. [53]

    Medina, S. N. X., Urquhart, J. S., Dzib, S. A., et al. 2019, A&A, 627, A175 Möller, T., Bernst, I., Panoglou, D., et al. 2013, A&A, 549, A21 Möller, T., Endres, C., & Schilke, P. 2017, A&A, 598, A7

    2019

  46. [54]

    2007, A&A, 476, 1243

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

    2007

  47. [55]

    2010, A&A, 518, L77 Müller, H

    Motte, F., Zavagno, A., Bontemps, S., et al. 2010, A&A, 518, L77 Müller, H. S. P., Schlöder, F., Stutzki, J., & Winnewisser, G. 2005, Journal of Molecular Structure, 742, 215 Nguyen-Lu’o’ng, Q., Motte, F., Carlhoff, P., et al. 2013, ApJ, 775, 88

    2010

  48. [56]

    R., et al

    Noriega-Crespo, A., Morris, P., Marleau, F. R., et al. 2004, ApJS, 154, 352 Ortiz-León, G. N., Menten, K. M., Brunthaler, A., et al. 2021, A&A, 651, A87

    2004

  49. [57]

    2013, A&A, 550, A38

    Palmeirim, P., André, P., Kirk, J., et al. 2013, A&A, 550, A38

    2013

  50. [58]

    V ., Mehrtens, N., et al

    Papovich, C., Shipley, H. V ., Mehrtens, N., et al. 2016, ApJS, 224, 28

    2016

  51. [59]

    2005, in SF2A-2005: Semaine de l’Astrophysique Francaise, ed

    Pety, J. 2005, in SF2A-2005: Semaine de l’Astrophysique Francaise, ed. F. Ca- soli, T. Contini, J. M. Hameury, & L. Pagani, 721

    2005

  52. [60]

    Piddington, J. H. & Minnett, H. C. 1952, Australian Journal of Scientific Re- search A Physical Sciences, 5, 17

    1952

  53. [61]

    Pirogov, L., Zinchenko, I., Caselli, P., Johansson, L. E. B., & Myers, P. C. 2003, A&A, 405, 639

    2003

  54. [62]

    P., McCaughrean, M

    Ray, T. P., McCaughrean, M. J., Caratti o Garatti, A., et al. 2023, Nature, 622, 48

    2023

  55. [63]

    2019, A&A, 629, A15

    Redaelli, E., Bizzocchi, L., Caselli, P., et al. 2019, A&A, 629, A15

    2019

  56. [64]

    & Schneider, N

    Reipurth, B. & Schneider, N. 2008, in Handbook of Star Forming Regions, V ol- ume I, ed. B. Reipurth, V ol. 4, 36

    2008

  57. [65]

    E., Sievers, J., Ghirardini, V ., et al

    Romero, C. E., Sievers, J., Ghirardini, V ., et al. 2020, ApJ, 891, 90

    2020

  58. [66]

    W., Pineda, J

    Rosolowsky, E. W., Pineda, J. E., Kauffmann, J., & Goodman, A. A. 2008, ApJ, 679, 1338

    2008

  59. [67]

    Rygl, K. L. J., Brunthaler, A., Sanna, A., et al. 2012, A&A, 539, A79

    2012

  60. [68]

    D., et al

    Salgado, F., Berné, O., Adams, J. D., et al. 2016, ApJ, 830, 118 Sánchez-Monge, Á., López-Sepulcre, A., Cesaroni, R., et al. 2013, A&A, 557, A94 Sánchez-Monge, Á., Schilke, P., Schmiedeke, A., et al. 2017, A&A, 604, A6

    2016

  61. [69]

    M., Foster, J

    Sanhueza, P., Jackson, J. M., Foster, J. B., et al. 2012, ApJ, 756, 60

    2012

  62. [70]

    M., & Martín-Pintado, J

    Schilke, P., Pineau des Forêts, G., Walmsley, C. M., & Martín-Pintado, J. 2001, A&A, 372, 291

    2001

  63. [71]

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

    Schilke, P., Walmsley, C. M., Pineau des Forets, G., & Flower, D. R. 1997, A&A, 321, 293

    1997

  64. [72]

    2023, Nature Astronomy, 7, 546

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

    2023

  65. [73]

    2006, A&A, 458, 855

    Schneider, N., Bontemps, S., Simon, R., et al. 2006, A&A, 458, 855

    2006

  66. [74]

    2012, A&A, 542, L18

    Schneider, N., Güsten, R., Tremblin, P., et al. 2012, A&A, 542, L18

    2012

  67. [75]

    T., et al

    Schneider, N., Röllig, M., Polehampton, E. T., et al. 2021, A&A, 653, A108

    2021

  68. [76]

    Shull, J. M. 1980, ApJ, 238, 860

    1980

  69. [77]

    Skretas, I. M. & Kristensen, L. E. 2022, A&A, 660, A39

    2022

  70. [78]

    2020, MNRAS, 492, 5966

    Sofue, Y . 2020, MNRAS, 492, 5966

    2020

  71. [79]

    2002, ApJ, 565, L25

    Sugitani, K., Tamura, M., Nakajima, Y ., et al. 2002, ApJ, 565, L25

    2002

  72. [80]

    N., Shang, H., et al

    Tafalla, M., Su, Y . N., Shang, H., et al. 2017, A&A, 597, A119

    2017

  73. [81]

    Tielens, A. G. G. M. 2013, Reviews of Modern Physics, 85, 1021

    2013

  74. [82]

    Tielens, A. G. G. M. & Hollenbach, D. 1985, ApJ, 291, 722

    1985

  75. [83]

    2012b, A&A, 538, A31 Treviño-Morales, S

    Tremblin, P., Audit, E., Minier, V ., & Schneider, N. 2012b, A&A, 538, A31 Treviño-Morales, S. P., Fuente, A., Sánchez-Monge, Á., et al. 2016, A&A, 593, L12 van den Ancker, M., Wesselius, P. R., & Tielens, A. G. G. M. 2000a, in Molecular Hydrogen in Space, ed. F. Combes & G. P...

    2016

  76. [84]

    S., Vig, S., Tej, A., Kantharia, N

    Veena, V . S., Vig, S., Tej, A., Kantharia, N. G., & Ghosh, S. K. 2017, MNRAS, 465, 4219

    2017

  77. [85]

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

    Walmsley, C. M., Pineau des Forêts, G., & Flower, D. R. 1999, A&A, 342, 542

    1999

  78. [86]

    J., Nelson, R

    White, G. J., Nelson, R. P., Holland, W. S., et al. 1999, A&A, 342, 233

    1999

  79. [87]

    J., Drew, J

    Wright, N. J., Drew, J. E., & Mohr-Smith, M. 2015, MNRAS, 449, 741

    2015

  80. [88]

    2024, arXiv e-prints, arXiv:2403.03845

    Zhang, X., Qiu, K., Zhang, Q., et al. 2024, arXiv e-prints, arXiv:2403.03845

    2024 arXiv

  81. [89]

    & Yorke, H

    Zinnecker, H. & Yorke, H. W. 2007, ARA&A, 45, 481 Article number, page 21 of 25 A&A proofs: manuscript no. aa51998-24corr Appendix A: Velocity-integrated intensity maps 20h35m18s 12s 06s 00s 41°15' 14' 13' 12' RA (J2000) Dec (J2000) CCH 0.1 pc 0.10 0.15 0.20 0.25 0.30 0.35 0.4...

    2007

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