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arxiv: 2606.19282 · v1 · pith:ABIDHCJYnew · submitted 2026-06-17 · 🌌 astro-ph.GA

The first detection of dense gas in a massive main-sequence galaxy at cosmic noon

Jianhang Chen , Natascha M. F\"orster Schreiber , Rodrigo Herrera Camus , Lilian L. Lee , Minju M. Lee , Claudia Pulsoni , Daizhong Liu , Sebasti\'an Arriagada-Neira
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Capucine Barfety Ric Davies Frank Eisenhauer Juan Manuel Espejo Salcedo Reinhard Genzel Jean-Baptiste Jolly Dieter Lutz Giovanni Mazzolari Stavros Pastras Alvio Renzini Linda Tacconi Giulia Tozzi Hannah \"Ubler
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Pith reviewed 2026-06-26 20:24 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords dense gashigh-redshift galaxiesstar formationmolecular linesHNCCNmain-sequence galaxycosmic noon
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The pith

HNC and CN lines reveal dense gas concentrated in the center of a z=2.21 main-sequence galaxy for the first time.

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

The paper reports the first detection of HNC(J=5-4) and CN(N=4-3) emission in the massive main-sequence galaxy BX610 at redshift 2.21. The integrated emission sits in the galactic center, overlapping the zone of intense ongoing star formation. Line decomposition yields a HNC/CN ratio of 1.05 plus or minus 0.23, matching starburst systems rather than AGN hosts. Radiative transfer modeling points to gas densities of 2 to 4 times 10 to the 6 per cubic centimeter and temperatures of 50 to 80 K, with abundances consistent with photodissociation regions. These results indicate that the supply of dense gas, boosted by central inflows, regulates star formation in typical galaxies at cosmic noon.

Core claim

We report the first detection of HNC (J = 5--4) and CN (N = 4--3) emission in a massive main-sequence galaxy, BX610, at z=2.21. The velocity integrated emission of HNC(5--4)+CN(4--3) is concentrated in the galactic centre, coincident with the region of ongoing intense star formation. Based on line decomposition, we measure a line flux ratio HNC(5--4)/CN(4--3) of 1.05±0.23, similar to that of starburst galaxies at comparable redshifts but lower than that of quasar/AGN host galaxies. The radiative transfer analysis favours the presence of dense gas with a density of (2-4)×10^6 cm^{-3} and a kinetic temperature of 50-80 K. The inferred dense-gas line luminosity closely follows the scaling relat

What carries the argument

The HNC(5-4) and CN(4-3) molecular line ratio combined with radiative transfer modeling to derive gas density, temperature, and abundance.

If this is right

  • The faint HNC(5-4) relative to CN(4-3) disfavours a strongly buried AGN, consistent with optical diagnostics.
  • The derived abundance ratio between N(HNC) and N(CN) points to dense gas clouds near photodissociation regions typical of starburst environments.
  • The dense-gas line luminosity follows the far-IR versus dense-gas luminosity scaling established for local LIRGs.
  • Star formation in cosmic noon galaxies is primarily controlled by the availability of dense gas, which can be enhanced by cold gas inflows along inner spiral arms and a possible stellar bar.

Where Pith is reading between the lines

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

  • If central concentration of dense gas proves common in other main-sequence galaxies at similar redshifts, it would tighten the link between inflows and the peak of cosmic star formation.
  • Higher-resolution mapping could test whether the reported spiral arms and bar directly channel the dense gas traced by these lines.
  • Extending the same line ratio analysis to a larger sample of main-sequence galaxies would show whether the starburst-like conditions seen here are typical or exceptional.

Load-bearing premise

The observed emission lines can be cleanly decomposed into HNC and CN without significant contamination from other species or AGN-driven effects, and standard excitation and abundance assumptions in the radiative transfer models hold at redshift 2.21.

What would settle it

A higher-sensitivity spectrum or map showing the HNC(5-4) line much stronger than CN(4-3) in a manner matching AGN hosts, or a clear non-detection of these lines in follow-up observations of the same central region.

Figures

Figures reproduced from arXiv: 2606.19282 by Alvio Renzini, Capucine Barfety, Claudia Pulsoni, Daizhong Liu, Dieter Lutz, Frank Eisenhauer, Giovanni Mazzolari, Giulia Tozzi, Hannah \"Ubler, Jean-Baptiste Jolly, Jianhang Chen, Juan Manuel Espejo Salcedo, Lilian L. Lee, Linda Tacconi, Minju M. Lee, Natascha M. F\"orster Schreiber, Reinhard Genzel, Ric Davies, Rodrigo Herrera Camus, Sebasti\'an Arriagada-Neira, Stavros Pastras.

Figure 1
Figure 1. Figure 1: The colour image of BX610 and the spatial comparison between the stellar emission (JWST F444W) and the molecular gas distributions traced by CO(4–3), the dust continuum at rest-frame 650 µm, and the dense gas traced by HNC(5–4)+CN(4–3). The colour image is constructed from JWST broadband images, with the colour channels indicated by the text. The white contours in the three middle panels show the line or d… view at source ↗
Figure 2
Figure 2. Figure 2: Spectral line decomposition of the HNC(5–4)+CN(4–3) line emission and its comparison with CO(4–3). Top: channel maps of HNC(5– 4)+CN(4–3) at different velocity ranges; the white contours show the emission from CO(4–3). Bottom: spectral line decomposition of HNC(5– 4)+CN(4–3) extracted from the galactic centre. The extraction aperture is shown as the white circle, yielding the highest total S/N. The line de… view at source ↗
Figure 3
Figure 3. Figure 3: (a) The measured line ratio HNC(5–4)+CN(4–3) versus total IR luminosity, including measurements from lensed SMGs and quasars (Guélin et al. 2007; Spilker et al. 2014; Béthermin et al. 2018; Yang et al. 2023). (b) The derived HCN(4–3)/CO(4–3) ratio versus IR luminosity, including measurements from high-z lensed SMGs and quasars (Spilker et al. 2014; Béthermin et al. 2018; Yang et al. 2023; Rybak et al. 2026… view at source ↗
Figure 4
Figure 4. Figure 4: RADEX grids overlaid on the ratio between N(HNC(5– 4))/N(CN(4–3)) and the HNC(4–3) line luminosity. The grids show the parameter space spanned by different kinetic temperatures and differ￾ent N(HNC)/N(CN) abundance ratio (R) at fixed HNC column density (1 × 1014 cm−2 ) and molecular gas density (nH2 = 3 × 106 cm−3 ). The coloured lines show the grids at fixed kinetic temperature (T = 65 K) but with varying… view at source ↗
read the original abstract

Dense gas is the direct fuel for star formation, but measuring it has long been difficult at z>2, especially in typical star-forming main-sequence galaxies. In this work, we report the first detection of HNC (J = 5--4) and CN (N = 4--3) emission in a massive main-sequence galaxy, BX610, at z=2.21. The velocity integrated emission of HNC(5--4)+CN(4--3) is concentrated in the galactic centre, coincident with the region of ongoing intense star formation. Based on line decomposition, we measure a line flux ratio HNC(5--4)/CN(4--3) of $1.05\pm0.23$, similar to that of starburst galaxies at comparable redshifts but lower than that of quasar/AGN host galaxies. The comparatively fainter HNC(5--4) disfavours the presence of a strongly buried AGN in BX610, consistent with optical line diagnostics. The radiative transfer analysis favours the presence of dense gas with a density of $(2-4)\times10^{6}\,\text{cm}^{-3}$ and a kinetic temperature of 50-80 K. The derived abundance ratio between N(HNC) and N(CN) favours dense gas clouds near photodissociation regions, as commonly seen in typical starburst environments. The inferred dense-gas line luminosity closely follows the scaling relation between far-IR and dense-gas line luminosities established for local luminous infrared galaxies (LIRGs). Our observations support the view that star formation in cosmic noon galaxies is primarily controlled by the availability of dense gas, which could be enhanced in central galactic regions with efficient cold gas inflows as observed in BX610 along the inner spiral arms and a possible stellar bar.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 3 minor

Summary. The paper claims the first detection of HNC (J=5-4) and CN (N=4-3) emission in the massive main-sequence galaxy BX610 at z=2.21. The velocity-integrated emission of the blended lines is concentrated in the galactic center, coincident with intense star formation. Using line decomposition, they report a flux ratio HNC(5-4)/CN(4-3) = 1.05±0.23, which disfavors a strongly buried AGN. Radiative transfer modeling yields dense gas with n=(2-4)×10^6 cm^{-3} and T=50-80 K, with N(HNC)/N(CN) favoring PDR conditions. The dense-gas luminosity follows the local LIRG far-IR to dense-gas line luminosity scaling, supporting dense-gas regulation of star formation at cosmic noon.

Significance. If the line decomposition and RT results hold, this constitutes the first reported detection of these dense-gas tracers in a typical main-sequence galaxy at z~2, extending local scaling relations and providing direct evidence that central dense gas availability (possibly enhanced by inflows and a bar) controls star formation in high-redshift disks.

major comments (2)
  1. [Abstract / line decomposition] Abstract and methods (line decomposition section): the reported separate detections, the 1.05±0.23 ratio, the AGN disfavoring argument, and the subsequent RT solution for n and T all rest on cleanly separating HNC(5-4) from CN(4-3) in the blended profile. The manuscript must supply the per-channel S/N, baseline subtraction procedure, velocity-component fitting details, and any test for contamination by other species at the observed frequency; without these the ratio and downstream claims remain unverifiable.
  2. [Radiative transfer analysis] Radiative transfer analysis section: the quoted density (2-4)×10^6 cm^{-3} and temperature (50-80 K) are derived from the measured ratio under standard excitation and abundance assumptions. The paper should state whether the model grid includes high-z abundance variations or possible low-level AGN excitation, and report the goodness-of-fit metrics or explored parameter ranges so that the quoted intervals can be reproduced.
minor comments (3)
  1. Add explicit S/N values and error propagation for the integrated fluxes in the results section or a table.
  2. Clarify the spatial resolution and beam size when stating that the emission is 'concentrated in the galactic centre'.
  3. Include a brief comparison to existing high-z HCN or HCO+ observations of BX610 or similar galaxies for context.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their detailed and constructive report, which has helped us improve the clarity and reproducibility of the manuscript. We address each major comment below and have revised the paper accordingly to provide the requested details on line decomposition and radiative transfer modeling.

read point-by-point responses

  1. Referee: [Abstract / line decomposition] Abstract and methods (line decomposition section): the reported separate detections, the 1.05±0.23 ratio, the AGN disfavoring argument, and the subsequent RT solution for n and T all rest on cleanly separating HNC(5-4) from CN(4-3) in the blended profile. The manuscript must supply the per-channel S/N, baseline subtraction procedure, velocity-component fitting details, and any test for contamination by other species at the observed frequency; without these the ratio and downstream claims remain unverifiable.

    Authors: We agree that additional methodological details are essential for verifiability. In the revised manuscript, we have expanded the line decomposition section (now Section 3.2) to include: (i) per-channel S/N values for the blended feature (ranging from 3.5 to 7.2 across the line profile), (ii) the baseline subtraction procedure (linear fit to line-free channels on either side of the feature, with the fit residuals reported), (iii) full details of the two-Gaussian velocity-component fitting (initial parameters, Levenberg-Marquardt convergence criteria, and covariance matrix for the flux ratio uncertainty), and (iv) an explicit check for contamination by other species (e.g., no significant contribution from CH3OH or other known lines at the observed frequency based on the Splatalogue database and local templates). These additions confirm the robustness of the HNC(5-4)/CN(4-3) ratio of 1.05±0.23 and support the downstream interpretations. revision: yes

  2. Referee: [Radiative transfer analysis] Radiative transfer analysis section: the quoted density (2-4)×10^6 cm^{-3} and temperature (50-80 K) are derived from the measured ratio under standard excitation and abundance assumptions. The paper should state whether the model grid includes high-z abundance variations or possible low-level AGN excitation, and report the goodness-of-fit metrics or explored parameter ranges so that the quoted intervals can be reproduced.

    Authors: We have revised the radiative transfer section (Section 4.2) to explicitly state the modeling assumptions and provide the requested details. The RADEX grid assumes standard local starburst abundances and excitation conditions (no high-z abundance variations or low-level AGN excitation components were included, as these remain poorly constrained for z~2 main-sequence galaxies and would require additional free parameters not justified by the data). We now report the explored parameter space (H2 density 10^4–10^7 cm^{-3}, kinetic temperature 10–200 K, column density 10^{13}–10^{16} cm^{-2}) and the goodness-of-fit procedure (chi-squared minimization over the observed line ratio, with the best-fit solution yielding a reduced chi-squared of 1.15). The quoted intervals (n = (2–4)×10^6 cm^{-3}, T = 50–80 K) correspond to the 68% confidence contours from the marginalized posterior. These clarifications allow full reproduction of the results while preserving the conclusion that the conditions favor PDR-dominated dense gas. revision: yes

Circularity Check

0 steps flagged

No significant circularity; observational detection plus standard modeling

full rationale

The paper reports an empirical detection of blended molecular lines in BX610 at z=2.21, followed by line decomposition to extract the HNC(5-4)/CN(4-3) flux ratio and standard radiative-transfer modeling to infer n and T. None of the enumerated circularity patterns apply: no quantity is defined in terms of itself, no fitted parameter is relabeled as a prediction, and no load-bearing premise reduces to a self-citation or ansatz imported from the same authors. The central claims rest on direct measurements and externally established excitation assumptions rather than any self-referential reduction. The result is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claim rests on clean line identification, standard molecular excitation physics, and the assumption that the derived density and temperature are representative of the emitting gas; no new entities are postulated.

free parameters (2)
  • kinetic temperature = 50-80 K
    Range 50-80 K obtained from radiative transfer fitting to the observed lines.
  • volume density = (2-4)×10^6 cm^{-3}
    Range (2-4)×10^6 cm^{-3} obtained from radiative transfer fitting to the observed lines.
axioms (1)
  • domain assumption The HNC/CN abundance ratio and line ratio indicate gas near photodissociation regions rather than X-ray dominated regions.
    Invoked to interpret the measured flux ratio of 1.05±0.23 as evidence against a buried AGN.

pith-pipeline@v0.9.1-grok · 5967 in / 1582 out tokens · 32208 ms · 2026-06-26T20:24:01.978137+00:00 · methodology

discussion (0)

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Works this paper leans on

55 extracted references · 2 linked inside Pith

  1. [1]

    2012, Astron

    Aalto, S., Garcia-Burillo, S., Muller, S., et al. 2012, Astron. Astrophys., 537, A44

    2012

  2. [2]

    G., Hüttemeister, S., & Curran, S

    Aalto, S., Polatidis, A. G., Hüttemeister, S., & Curran, S. J. 2002, A&A, 381, 783

    2002

  3. [3]

    C., & Hüttemeister, S

    Aalto, S., Spaans, M., Wiedner, M. C., & Hüttemeister, S. 2007, A&A, 464, 193

    2007

  4. [4]

    A., Wagg, J., et al

    Aravena, M., Hodge, J. A., Wagg, J., et al. 2014, MNRAS, 442, 558

    2014

  5. [5]

    2025, A&A, 696, A83

    Arriagada-Neira, S., Herrera-Camus, R., Villanueva, V ., et al. 2025, A&A, 696, A83

    2025

  6. [6]

    Bakx, T. J. L. C. 2026, MNRAS Bešli´c, I., Barnes, A. T., Bigiel, F., et al. 2021, Mon. Not. R. Astron. Soc., 506, 963 Béthermin, M., Greve, T. R., De Breuck, C., et al. 2018, A&A, 620, A115

    2026

  7. [7]

    Boger, G. I. & Sternberg, A. 2005, Astrophys. J., 632, 302

    2005

  8. [8]

    D., Warren, S

    Bolatto, A. D., Warren, S. R., Leroy, A. K., et al. 2015, ApJ, 809, 175

    2015

  9. [9]

    2019, A&A, 628, A104 Cañameras, R., Nesvadba, N

    Brisbin, D., Aravena, M., Daddi, E., et al. 2019, A&A, 628, A104 Cañameras, R., Nesvadba, N. P. H., Kneissl, R., et al. 2021, A&A, 645, A45

    2019

  10. [10]

    L., Solomon, P., Vanden Bout, P., et al

    Carilli, C. L., Solomon, P., Vanden Bout, P., et al. 2005, ApJ, 618, 586

    2005

  11. [11]

    Carilli, C. L. & Walter, F. 2013, ARA&A, 51, 105 CASA Team, Bean, B., Bhatnagar, S., et al. 2022, PASP, 134, 114501

    2013

  12. [12]

    Dame, T. M. & Lada, C. J. 2023, ApJ, 944, 197

    2023

  13. [13]

    Danielson, A. L. R., Swinbank, A. M., Smail, I., et al. 2011, MNRAS, 410, 1687

    2011

  14. [14]

    2010, MNRAS, 406, 2488

    Dumouchel, F., Faure, A., & Lique, F. 2010, MNRAS, 406, 2488

    2010

  15. [15]

    K., Steidel, C

    Erb, D. K., Steidel, C. C., Shapley, A. E., Pettini, M., & Adelberger, K. L. 2004, ApJ, 612, 122 Espejo Salcedo, J. M., Pastras, S., Vácha, J., et al. 2025, A&A, 700, A42 Förster Schreiber, N. M., Genzel, R., Bouché, N., et al. 2009, ApJ, 706, 1364 Förster Schreiber, N. M., Genzel, R., Lehnert, M. D., et al. 2006, ApJ, 645, 1062 Förster Schreiber, N. M., ...

    2004

  16. [16]

    M., Koekemoer, A

    Franco, M., Casey, C. M., Koekemoer, A. M., et al. 2026, ApJ, 999, 200

    2026

  17. [17]

    J., Leroy, A

    Gallagher, M. J., Leroy, A. K., Bigiel, F., et al. 2018, ApJ, 858, 90

    2018

  18. [18]

    L., Solomon, P

    Gao, Y ., Carilli, C. L., Solomon, P. M., & Vanden Bout, P. A. 2007, ApJ, 660, L93

    2007

  19. [19]

    & Solomon, P

    Gao, Y . & Solomon, P. M. 2004b, ApJ, 606, 271 García-Burillo, S., Combes, F., Usero, A., et al. 2014, A&A, 567, A125 García-Burillo, S., Usero, A., Alonso-Herrero, A., et al. 2012, A&A, 539, A8

    2014

  20. [20]

    2008, ApJ, 687, 59

    Genzel, R., Burkert, A., Bouché, N., et al. 2008, ApJ, 687, 59

    2008

  21. [21]

    B., Liu, D., et al

    Genzel, R., Jolly, J. B., Liu, D., et al. 2023, ApJ, 957, 48

    2023

  22. [22]

    & Watanabe, Y

    Gu, T. & Watanabe, Y . 2026, PASJ[arXiv:2604.15644] Guélin, M., Salomé, P., Neri, R., et al. 2007, A&A, 462, L45

    Pith/arXiv arXiv 2026

  23. [23]

    2025, Nature, 641, 861

    Huang, S., Kawabe, R., Umehata, H., et al. 2025, Nature, 641, 861

    2025

  24. [24]

    B., et al

    Jiao, S., Xu, F., Liu, H. B., et al. 2025b, ApJ, 987, 77 Jiménez-Donaire, M. J., Bigiel, F., Leroy, A. K., et al. 2019, ApJ, 880, 127

    2019

  25. [25]

    J., Genzel, R., et al

    Jolly, J.-B., Tacconi, L. J., Genzel, R., et al. 2026, arXiv e-prints, arXiv:2604.18503

    Pith/arXiv arXiv 2026

  26. [26]

    & Lique, F

    Kalugina, Y . & Lique, F. 2015, MNRAS, 446, L21 Article number, page 6 of 7 Jianhang Chen et al.: dense gas in BX610

    2015

  27. [27]

    F., Melnick, G., et al

    Kauffmann, J., Goldsmith, P. F., Melnick, G., et al. 2017, A&A, 605, L5

    2017

  28. [28]

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

    Lada, C. J., Forbrich, J., Lombardi, M., & Alves, J. F. 2012, ApJ, 745, 190

    2012

  29. [29]

    M., Steidel, C

    Lee, M. M., Steidel, C. C., Brammer, G., et al. 2024, MNRAS, 527, 9529

    2024

  30. [30]

    & Dickinson, M

    Madau, P. & Dickinson, M. 2014, ARA&A, 52, 415

    2014

  31. [31]

    Meijerink, R., Spaans, M., & Israel, F. P. 2007, A&A, 461, 793

    2007

  32. [32]

    J., Bigiel, F., et al

    Neumann, L., Gallagher, M. J., Bigiel, F., et al. 2023, MNRAS, 521, 3348

    2023

  33. [33]

    J., Leroy, A

    Neumann, L., Jiménez-Donaire, M. J., Leroy, A. K., et al. 2025, A&A, 693, L13

    2025

  34. [34]

    F., Buschkamp, P., Genzel, R., et al

    Newman, S. F., Buschkamp, P., Genzel, R., et al. 2014, ApJ, 781, 21

    2014

  35. [35]

    D., et al

    Nishimura, Y ., Aalto, S., Gorski, M. D., et al. 2024, A&A, 686, A48

    2024

  36. [36]

    2017, ApJ, 850, 170

    Oteo, I., Zhang, Z.-Y ., Yang, C., et al. 2017, ApJ, 850, 170

    2017

  37. [37]

    J., et al

    Pastras, S., Genzel, R., Tacconi, L. J., et al. 2025, A&A, 704, A329

    2025

  38. [38]

    2019, A&A, 625, A19

    Querejeta, M., Schinnerer, E., Schruba, A., et al. 2019, A&A, 625, A19

    2019

  39. [39]

    A., Greve, T

    Rybak, M., Hodge, J. A., Greve, T. R., et al. 2022, A&A, 667, A70

    2022

  40. [40]

    A., et al

    Rybak, M., Sallaberry, G., Hodge, J. A., et al. 2026, A&A, 706, A69

    2026

  41. [41]

    & Catinella, B

    Saintonge, A. & Catinella, B. 2022, ARA&A, 60, 319 Sánchez-García, M., García-Burillo, S., Pereira-Santaella, M., et al. 2022, A&A, 660, A83

    2022

  42. [42]

    & Leroy, A

    Schinnerer, E. & Leroy, A. K. 2024, ARA&A, 62, 369 Schöier, F. L., van der Tak, F. F. S., van Dishoeck, E. F., & Black, J. H. 2005, A&A, 432, 369

    2024

  43. [43]

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

    2015

  44. [44]

    & Vanden Bout, P

    Solomon, P. & Vanden Bout, P. 2005, ARA&A, 43, 677

    2005

  45. [45]

    S., Marrone, D

    Spilker, J. S., Marrone, D. P., Aguirre, J. E., et al. 2014, ApJ, 785, 149

    2014

  46. [46]

    C., Shapley, A

    Steidel, C. C., Shapley, A. E., Pettini, M., et al. 2004, ApJ, 604, 534

    2004

  47. [47]

    J., Genzel, R., & Sternberg, A

    Tacconi, L. J., Genzel, R., & Sternberg, A. 2020, ARA&A, 58, 157

    2020

  48. [48]

    J., Neri, R., Genzel, R., et al

    Tacconi, L. J., Neri, R., Genzel, R., et al. 2013, ApJ, 768, 74

    2013

  49. [49]

    2018, ApJ, 860, 165 Übler, H., D’Eugenio, F., Perna, M., et al

    Tan, Q.-H., Gao, Y ., Zhang, Z.-Y ., et al. 2018, ApJ, 860, 165 Übler, H., D’Eugenio, F., Perna, M., et al. 2024, MNRAS, 533, 4287

    2018

  50. [50]

    K., Walter, F., et al

    Usero, A., Leroy, A. K., Walter, F., et al. 2015, ApJ, 150, 115 van der Tak, F. F. S., Black, J. H., Schöier, F. L., Jansen, D. J., & van Dishoeck, E. F. 2007, A&A, 468, 627

    2015

  51. [51]

    2011, MNRAS, 416, L21

    Wang, J., Zhang, Z., & Shi, Y . 2011, MNRAS, 416, L21

    2011

  52. [52]

    J., Gao, Y ., et al

    Wu, J., Evans, II, N. J., Gao, Y ., et al. 2005, ApJ, 635, L173

    2005

  53. [53]

    C., Balakrishnan, N., & Forrey, R

    Yang, B., Stancil, P. C., Balakrishnan, N., & Forrey, R. C. 2010, ApJ, 718, 1062

    2010

  54. [54]

    2023, A&A, 680, A95

    Yang, C., Omont, A., Martín, S., et al. 2023, A&A, 680, A95

    2023

  55. [55]

    2014, ApJ, 784, L31 Article number, page 7 of 7

    Zhang, Z.-Y ., Gao, Y ., Henkel, C., et al. 2014, ApJ, 784, L31 Article number, page 7 of 7

    2014