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arxiv: 2605.07159 · v1 · submitted 2026-05-08 · 🌌 astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

First Interstellar Detection of Methyl Carbamate: A New Observational Anchor for Glycine Chemistry

Chunguo Duan , Fengwei Xu , Jun Kang , Qian Gou , Xuefang Xu , Laurent Pagani , Jiaxin Du , Xi Chen
Authors on Pith no claims yet

Pith reviewed 2026-05-11 01:00 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords methyl carbamateinterstellar detectionglycinehot molecular coresgrain surface chemistryC2H5O2N isomersALMA observationsastrochemistry
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The pith

Methyl carbamate has been detected for the first time in interstellar space, serving as a new observational anchor for glycine chemistry.

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 robust detection of methyl carbamate in the hot molecular core G358.93-0.03 MM1 through ten clear rotational lines observed with ALMA. It places upper limits on glycine and other isomers in the same chemical family and shows that their abundance pattern does not match predictions from thermodynamic equilibrium. Instead, the data support a grain-surface formation route through radical recombination and show correlations with the precursors methanol and formamide. This detection supplies a concrete reference point for tracing how amino-acid-related molecules build up in star-forming regions.

Core claim

Ten unblended rotational transitions of methyl carbamate are identified toward G358.93-0.03 MM1, giving a column density of (4.21 ± 0.84) × 10^15 cm^{-2} and an excitation temperature of 204 ± 10 K. No other C2H5O2N isomers, including glycine, are detected. The resulting abundance ratios deviate from Minimum Energy Principle expectations, indicating that kinetic processes dominate over thermodynamic equilibrium. The observed abundance matches a grain-surface formation pathway via CH3O + NH2CO recombination and correlates with methanol and formamide abundances across environments.

What carries the argument

The grain-surface radical-radical recombination of CH3O and NH2CO that produces methyl carbamate, together with its observed abundance correlations with methanol and formamide.

If this is right

  • The C2H5O2N isomer family in hot cores is controlled by kinetic chemistry rather than thermodynamic equilibrium.
  • Methyl carbamate forms on grain surfaces through the same radical recombination that may lead to glycine.
  • Upper limits on glycine and other isomers constrain the efficiency of their formation routes in the same source.
  • Methyl carbamate can now be used as a reference molecule to test glycine formation models in additional star-forming regions.

Where Pith is reading between the lines

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

  • Detections of methyl carbamate in other hot cores could map the spatial distribution of glycine-precursor chemistry across different star-forming environments.
  • If kinetic control is common in this isomer family, similar deviations from equilibrium may appear in other complex organic molecule families observed in the same regions.
  • Laboratory measurements of additional C2H5O2N isomers without existing spectra would allow tighter tests of the kinetic versus thermodynamic balance.

Load-bearing premise

The ten transitions are truly unblended, correctly assigned to methyl carbamate, and free of significant contamination from other species, with laboratory rest frequencies remaining accurate under interstellar conditions.

What would settle it

A higher-resolution spectrum or independent re-analysis that shows one or more of the ten lines is blended with another molecule or misassigned would remove the detection and its chemical implications.

Figures

Figures reproduced from arXiv: 2605.07159 by Chunguo Duan, Fengwei Xu, Jiaxin Du, Jun Kang, Laurent Pagani, Qian Gou, Xi Chen, Xuefang Xu.

Figure 1
Figure 1. Figure 1: MC emission toward G358.93 MM1. Black histograms show the spectra extracted at the offset position described in Appendix A. Red curves represent the best-fit LTE model for MC, while blue curves indicate the full spectral model including all other species identified toward this source. Green dashed lines mark the 3σ noise level. Red asterisks highlight the ten MC transitions that are unblended and used to d… view at source ↗
Figure 2
Figure 2. Figure 2: Abundances relative to H2 for C2H5O2N isomers as a function of relative energy (∆E). Symbols denote measurements toward G358.93 MM1 and G+0.693-0.027, while arrows indicate 3σ upper limits. The red and cyan lines show the abundance trends predicted from the MEP for G358.93 MM1 and G+0.693-0.027, respectively, constructed using representative kinetic temperatures and adopting syn-GA as a reference. For G358… view at source ↗
Figure 3
Figure 3. Figure 3: Abundance constraints for methyl carbamate (MC) across different environments. a) MC abundance relative to H2. b) MC abundance relative to NH2CHO. c) MC abundance relative to CH3OH. Red circles denote the values derived in this work toward the hot molecular core G358.93 MM1. Cyan circles represent upper limits from previous observations of hot corinos and the Galactic center cloud G+0.693-0.027, while purp… view at source ↗
Figure 4
Figure 4. Figure 4: We examined spectra extracted from 70 offset positions around the continuum peak. MC emission is detectable at most of these positions, demonstrating that the detection is not confined to the single position adopted for LTE fitting. Among the tested positions, the adopted offset position provides the largest number of clean, ten in total, unblended MC transitions while maintaining a high signal-to-noise ra… view at source ↗
Figure 5
Figure 5. Figure 5: Relative energies (∆E) of spectroscopically accessible C2H5O2N isomers, using the zero-point energies of methylcar￾bamic acid (CH3NHCOOH) as a reference. E. IDENTIFICATION OF CH3OH AND 13CH3OH To quantify the MC-to-methanol ratio in G358.93 MM1, we searched for transitions of methanol (CH3OH) and its 13C isotopologue (13CH3OH), as shown in [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Observed (black) and LTE modeled (red) spectra of 13CH3OH toward G358.93 MM1, together with the corresponding CH3OH transitions used for line identification. No LTE modeled spectra are shown for CH3OH because the main-isotopologue lines are optically thick. Vertical dashed lines mark the rest frequencies of the CH3OH transitions. All other plotting conventions follow [PITH_FULL_IMAGE:figures/full_fig_p012… view at source ↗
read the original abstract

Glycine-the simplest amino acid-has remained undetected in the interstellar medium despite decades of sensitive searches, motivating alternative approaches to constrain its astrochemical origin. A promising strategy is to investigate the broader $\rm C_{2}H_{5}O_{2}N$ isomer family and identify detectable members that can serve as observational anchors for glycine-related chemistry. Herein, we report the first robust interstellar detection of methyl carbamate toward the hot molecular core G358.93-0.03 MM1 using ALMA 1 mm observations. Ten unblended rotational transitions are identified, yielding a column density of (4.21$\pm0.84)\times10^{15} \rm cm^{-2}$ and an excitation temperature of $204\pm10$ K. We also searched for other $\rm C_{2}H_{5}O_{2}N$ isomers with available rotational spectroscopic data, including glycine, but none were detected, allowing us to derive upper limits on their column densities. The resulting abundance pattern deviates significantly from the Minimum Energy Principle predictions, highlighting that the $\rm C_{2}H_{5}O_{2}N$ family is shaped primarily by kinetic chemical process rather than thermodynamic equilibrium. The observed methyl carbamate abundance is consistent with a grain-surface formation scenario involving radical-radical recombination ($\rm CH_{3}$O + $\rm NH_{2}$CO), further supported by its correlated abundances with its proposed precursors, methanol and formamide, across diverse astrophysical environments. This detection establishes methyl carbamate as a new observational anchor for glycine chemistry, providing critical constraints on the formation pathways of amino-acid-related molecules in star-forming regions.

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

1 major / 1 minor

Summary. The paper claims the first robust interstellar detection of methyl carbamate in the hot molecular core G358.93-0.03 MM1 using ALMA 1 mm observations. Ten unblended rotational transitions are identified, from which a column density of (4.21 ± 0.84) × 10^{15} cm^{-2} and an excitation temperature of 204 ± 10 K are derived. Upper limits are set on other C2H5O2N isomers, including glycine, and the abundance pattern is used to argue that the chemistry is kinetically controlled rather than following the Minimum Energy Principle, supporting a grain-surface formation route involving CH3O and NH2CO radicals.

Significance. If the identification holds, this represents a significant advance by providing a new observational anchor for glycine-related chemistry in star-forming regions. The direct detection, non-detections of isomers, and correlation with precursors offer concrete constraints on astrochemical models. The manuscript benefits from being based on observational data rather than theoretical derivation.

major comments (1)
  1. [Abstract] The detection is based on ten unblended lines leading to the quoted column density and temperature. However, the manuscript does not include the list of transition frequencies, quantum numbers, or the full LTE model that demonstrates these lines are unblended and that all other known molecular carriers have been properly subtracted at those frequencies. Given the high line density in hot cores (>1 line per 10 MHz), this information is essential to substantiate the claim.
minor comments (1)
  1. The abstract contains LaTeX commands such as rm that should be rendered properly in the final manuscript.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and positive evaluation of the scientific significance of our detection. We have revised the manuscript to address the major comment by providing the requested spectroscopic details and modeling information.

read point-by-point responses

  1. Referee: [Abstract] The detection is based on ten unblended lines leading to the quoted column density and temperature. However, the manuscript does not include the list of transition frequencies, quantum numbers, or the full LTE model that demonstrates these lines are unblended and that all other known molecular carriers have been properly subtracted at those frequencies. Given the high line density in hot cores (>1 line per 10 MHz), this information is essential to substantiate the claim.

    Authors: We agree that explicit documentation of the ten unblended transitions and the supporting LTE model is necessary to substantiate the identification in a high line-density environment. In the revised manuscript we have added Table 2, which lists the rest frequencies, quantum numbers (J, K_a, K_c), upper-state energies, and integrated intensities for all ten transitions. We have also included a new figure (Figure 3) that overlays the observed ALMA spectrum with the best-fit LTE model for methyl carbamate (generated with CASSIS under the derived N = 4.21 × 10^{15} cm^{-2}, T_ex = 204 K, and ΔV = 3.5 km s^{-1}), together with the residual spectrum after subtraction of the methyl carbamate model and all other catalogued molecular carriers at those frequencies. The figure caption and methods section now explicitly state that no other known species contribute significantly to the observed line profiles, confirming that the features remain unblended. These additions directly address the concern while preserving the original column-density and temperature values. revision: yes

Circularity Check

0 steps flagged

No significant circularity; direct observational detection from ALMA data

full rationale

The paper's core claim is the identification of ten unblended rotational transitions of methyl carbamate in ALMA 1 mm spectra toward G358.93-0.03 MM1, followed by standard LTE fitting to derive column density (4.21±0.84)×10^15 cm^{-2} and T_ex=204±10 K. This is a direct data reduction and parameter estimation step using laboratory rest frequencies, with no equations or self-citations that reduce the reported values to inputs defined by the authors' prior work. Searches for other C2H5O2N isomers and upper limits are likewise observational. Interpretive sections on abundance patterns versus Minimum Energy Principle or grain-surface formation are post-hoc comparisons, not load-bearing derivations. The paper remains self-contained against external laboratory spectroscopy benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The claim rests on the accuracy of prior laboratory rotational spectroscopy for methyl carbamate and standard assumptions about local thermodynamic equilibrium and line identification in hot cores.

free parameters (2)
  • column density = (4.21±0.84)×10^{15} cm^{-2}
    Fitted from the observed line intensities of the ten transitions.
  • excitation temperature = 204±10 K
    Derived from the relative intensities of the detected lines.
axioms (2)
  • domain assumption Laboratory-measured rest frequencies of methyl carbamate accurately match the interstellar environment.
    The detection identification depends on this match.
  • domain assumption The source can be described by a single excitation temperature and column density (LTE approximation).
    Used to convert line intensities to column density.

pith-pipeline@v0.9.0 · 5631 in / 1405 out tokens · 40871 ms · 2026-05-11T01:00:09.747305+00:00 · methodology

discussion (0)

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Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

  • IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    Ten unblended rotational transitions are identified, yielding a column density of (4.21±0.84)×10^{15} cm^{-2} and an excitation temperature of 204±10 K... The resulting abundance pattern deviates significantly from the Minimum Energy Principle predictions

  • IndisputableMonolith/Foundation/BranchSelection.lean branch_selection unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    the C2H5O2N family is shaped primarily by kinetic chemical process rather than thermodynamic equilibrium... grain-surface formation scenario involving radical-radical recombination (CH3O + NH2CO)

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

49 extracted references · 45 canonical work pages · 1 internal anchor

  1. [1]

    2016, Science Advances, 2, e1600285, doi: 10.1126/sciadv.1600285

    Altwegg, K., Balsiger, H., Bar-Nun, A., et al. 2016, Science Advances, 2, e1600285, doi: 10.1126/sciadv.1600285

    work page doi:10.1126/sciadv.1600285 2016

  2. [2]

    2002, Journal of Molecular Spectroscopy, 215, 312, doi: https://doi.org/10.1006/jmsp.2002.8647

    Bakri, B., Demaison, J., Kleiner, I., et al. 2002, Journal of Molecular Spectroscopy, 215, 312, doi: https://doi.org/10.1006/jmsp.2002.8647

    work page doi:10.1006/jmsp.2002.8647 2002

  3. [3]

    T., M¨ uller, H

    Belloche, A., Garrod, R. T., M¨ uller, H. S. P., et al. 2019, A&A, 628, A10, doi: 10.1051/0004-6361/201935428

    work page doi:10.1051/0004-6361/201935428 2019

  4. [4]

    A., Garrod, R

    Belloche, A., Meshcheryakov, A. A., Garrod, R. T., et al. 2017, A&A, 601, A49, doi: 10.1051/0004-6361/201629724

    work page doi:10.1051/0004-6361/201629724 2017

  5. [5]

    T., et al

    Bonfand, M., Belloche, A., Garrod, R. T., et al. 2019, A&A, 628, A27, doi: 10.1051/0004-6361/201935523 Methyl Carbamate13

    work page doi:10.1051/0004-6361/201935523 2019

  6. [6]

    L., Hunter, T

    Brogan, C. L., Hunter, T. R., Towner, A. P. M., et al. 2019, ApJL, 881, L39, doi: 10.3847/2041-8213/ab2f8a

    work page doi:10.3847/2041-8213/ab2f8a 2019

  7. [7]

    2012, in 39th COSPAR Scientific Assembly, Vol

    Burton, A., Dworkin, J., Callahan, M., Glavin, D., & Elsila, J. 2012, in 39th COSPAR Scientific Assembly, Vol. 39, 264

    2012

  8. [8]

    M., Ren, Z.-Y., et al

    Chen, X., Sobolev, A. M., Ren, Z.-Y., et al. 2020, Nature Astronomy, 4, 1170, doi: 10.1038/s41550-020-1144-x

    work page doi:10.1038/s41550-020-1144-x 2020

  9. [9]

    Chen, Z., Li, Z., & Tian, S. X. 2024, Chinese Journal of Chemical Physics, 37, 24, doi: 10.1063/1674-0068/cjcp2304037

    work page doi:10.1063/1674-0068/cjcp2304037 2024

  10. [10]

    1992, Nature, 355, 125, doi: 10.1038/355125a0

    Chyba, C., & Sagan, C. 1992, Nature, 355, 125, doi: 10.1038/355125a0

    work page doi:10.1038/355125a0 1992

  11. [11]

    F., Thomas, P

    Chyba, C. F., Thomas, P. J., Brookshaw, L., & Sagan, C. 1990, Science, 249, 366, doi: 10.1126/science.11538074

    work page doi:10.1126/science.11538074 1990

  12. [12]

    M., Beltr´ an, M

    Colzi, L., Rivilla, V. M., Beltr´ an, M. T., et al. 2021, A&A, 653, A129, doi: 10.1051/0004-6361/202141573

    work page doi:10.1051/0004-6361/202141573 2021

  13. [13]

    2021,, 2.0.0 Zenodo, doi: 10.5281/zenodo.4905459

    Comrie, A., Wang, K.-S., Hsu, S.-C., et al. 2021,, 2.0.0 Zenodo, doi: 10.5281/zenodo.4905459

    work page doi:10.5281/zenodo.4905459 2021

  14. [14]

    K., van der Wiel, M

    Coutens, A., Jørgensen, J. K., van der Wiel, M. H. D., et al. 2016, A&A, 590, L6, doi: 10.1051/0004-6361/201628612

    work page doi:10.1051/0004-6361/201628612 2016

  15. [15]

    R., & Pizzarello, S

    Cronin, J. R., & Pizzarello, S. 1983, Advances in Space Research, 3, 5, doi: 10.1016/0273-1177(83)90036-4

    work page doi:10.1016/0273-1177(83)90036-4 1983

  16. [16]

    R., Knigge, C., Drew, J

    Cunningham, M. R., Jones, P. A., Godfrey, P. D., et al. 2007, MNRAS, 376, 1201, doi: 10.1111/j.1365-2966.2007.11504.x

    work page doi:10.1111/j.1365-2966.2007.11504.x 2007

  17. [17]

    M., & Westmoreland, P

    Dean, A. M., & Westmoreland, P. R. 1987, International Journal of Chemical Kinetics, 19, 207, doi: https://doi.org/10.1002/kin.550190305

    work page doi:10.1002/kin.550190305 1987

  18. [18]

    2004, in SF2A-2004: Semaine de l’Astrophysique Francaise, ed

    Demyk, K., Wlodarczak, G., & Dartois, E. 2004, in SF2A-2004: Semaine de l’Astrophysique Francaise, ed. F. Combes, D. Barret, T. Contini, F. Meynadier, & L. Pagani, 493

    2004

  19. [19]

    Tentative Detection of the Glycine Isomer Glycolamide in Hot Molecular Core

    Duan, C., Xu, F., Gou, Q., et al. 2026, https://arxiv.org/abs/2603.23170

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  20. [20]

    J., Trucks, G

    Frisch, M. J., Trucks, G. W., Schlegel, H. B., et al. 2016, Gaussian 16, Revision A.03, Gaussian, Inc., Wallingford,

    2016

  21. [21]

    M., & Mart´ ın-Pintado, J

    Corchado, J., Rivilla, V. M., & Mart´ ın-Pintado, J. 2021, ApJL, 912, L6, doi: 10.3847/2041-8213/abf650

    work page doi:10.3847/2041-8213/abf650 2021

  22. [22]

    Garrod, R. T. 2013, ApJ, 765, 60, doi: 10.1088/0004-637X/765/1/60

    work page doi:10.1088/0004-637x/765/1/60 2013

  23. [23]

    T., Jin, M., Matis, K

    Garrod, R. T., Jin, M., Matis, K. A., et al. 2022, ApJS, 259, 1, doi: 10.3847/1538-4365/ac3131

    work page doi:10.3847/1538-4365/ac3131 2022

  24. [24]

    Herbst, E., & van Dishoeck, E. F. 2009, ARA&A, 47, 427, doi: 10.1146/annurev-astro-082708-101654

    work page doi:10.1146/annurev-astro-082708-101654 2009

  25. [25]

    2006, Journal of Molecular Spectroscopy, 240, 127, doi: https://doi.org/10.1016/j.jms.2006.09.008 Jim´ enez-Serra, I., Vasyunin, A

    Ilyushin, V., Alekseev, E., Demaison, J., & Kleiner, I. 2006, Journal of Molecular Spectroscopy, 240, 127, doi: https://doi.org/10.1016/j.jms.2006.09.008 Jim´ enez-Serra, I., Vasyunin, A. I., Caselli, P., et al. 2016, ApJL, 830, L6, doi: 10.3847/2041-8205/830/1/L6 Jim´ enez-Serra, I., Mart´ ın-Pintado, J., Rivilla, V. M., et al. 2020, Astrobiology, 20, 10...

    work page doi:10.1016/j.jms.2006.09.008 2006

  26. [26]

    Ram Pressure Stripping of Disc Galaxies: The Role of the Inclination Angle , shorttitle =

    Jones, P. A., Cunningham, M. R., Godfrey, P. D., & Cragg, D. M. 2007, MNRAS, 374, 579, doi: 10.1111/j.1365-2966.2006.11175.x Jørgensen, J. K., Belloche, A., & Garrod, R. T. 2020, ARA&A, 58, 727, doi: 10.1146/annurev-astro-032620-021927

    work page doi:10.1111/j.1365-2966.2006.11175.x 2007

  27. [27]

    L., Evans, N

    Kauffmann, J., Bertoldi, F., Bourke, T. L., Evans, N. J., I., & Lee, C. W. 2008, A&A, 487, 993, doi: 10.1051/0004-6361:200809481

    work page doi:10.1051/0004-6361:200809481 2008

  28. [28]

    B., Huang, H.-C., Tseng, W.-L., & Kisiel, Z

    Kuan, Y.-J., Charnley, S. B., Huang, H.-C., Tseng, W.-L., & Kisiel, Z. 2003, ApJ, 593, 848, doi: 10.1086/375637

    work page doi:10.1086/375637 2003

  29. [29]

    2009, ApJL, 696, L133, doi: 10.1088/0004-637X/696/2/L133

    Lattelais, M., Pauzat, F., Ellinger, Y., & Ceccarelli, C. 2009, ApJL, 696, L133, doi: 10.1088/0004-637X/696/2/L133

    work page doi:10.1088/0004-637x/696/2/l133 2009

  30. [30]

    2011, A&A, 532, A39, doi: 10.1051/0004-6361/201016039

    Ceccarelli, C. 2011, A&A, 532, A39, doi: 10.1051/0004-6361/201016039

    work page doi:10.1051/0004-6361/201016039 2011

  31. [31]

    C., & Kang, H

    Lee, C.-W., Kim, J.-K., Moon, E.-S., Minh, Y. C., & Kang, H. 2009, ApJ, 697, 428, doi: 10.1088/0004-637X/697/1/428 L´ opez-Sepulcre, A., Sakai, N., Neri, R., et al. 2017, A&A, 606, A121, doi: 10.1051/0004-6361/201630334

    work page doi:10.1088/0004-637x/697/1/428 2009

  32. [32]

    J., Kawashima, Y., Grabow, J.-U., et al

    Lovas, F. J., Kawashima, Y., Grabow, J.-U., et al. 1995, ApJL, 455, L201, doi: 10.1086/309844

    work page doi:10.1086/309844 1995

  33. [33]

    2011, A&A, 526, A47, doi: 10.1051/0004-6361/201015487

    Maret, S., Hily-Blant, P., Pety, J., Bardeau, S., & Reynier, E. 2011, A&A, 526, A47, doi: 10.1051/0004-6361/201015487

    work page doi:10.1051/0004-6361/201015487 2011

  34. [34]

    2004, Phys

    Maris, A. 2004, Phys. Chem. Chem. Phys., 6, 2611, doi: 10.1039/B401081G

    work page doi:10.1039/b401081g 2004

  35. [35]

    1999, Acta Chemica Scandinavica, 53, 79

    Marstokk, K., & Mollendal, H. 1999, Acta Chemica Scandinavica, 53, 79

    1999

  36. [36]

    T., Rivilla, V

    Mininni, C., Beltr´ an, M. T., Rivilla, V. M., et al. 2020, A&A, 644, A84, doi: 10.1051/0004-6361/202038966

    work page doi:10.1051/0004-6361/202038966 2020

  37. [37]

    M., Poynter , R

    Pickett, H. M., Poynter, R. L., Cohen, E. A., et al. 1998, JQSRT, 60, 883, doi: 10.1016/S0022-4073(98)00091-0

    work page doi:10.1016/s0022-4073(98)00091-0 1998

  38. [38]

    2023, Nature Communications, 14, 1482, doi: 10.1038/s41467-023-37107-6

    Potiszil, C., Ota, T., Yamanaka, M., et al. 2023, Nature Communications, 14, 1482, doi: 10.1038/s41467-023-37107-6

    work page doi:10.1038/s41467-023-37107-6 2023

  39. [39]

    Powell, M. J. D. 1964, The Computer Journal, 7, 155, doi: 10.1093/comjnl/7.2.155

    work page doi:10.1093/comjnl/7.2.155 1964

  40. [40]

    M., Sanz-Novo, M., Jim´ enez-Serra, I., et al

    Rivilla, V. M., Sanz-Novo, M., Jim´ enez-Serra, I., et al. 2023, ApJL, 953, L20, doi: 10.3847/2041-8213/ace977

    work page doi:10.3847/2041-8213/ace977 2023

  41. [41]

    2020, ApJ, 899, 65, doi: 10.3847/1538-4357/aba0a5

    Sahu, D., Liu, S.-Y., Das, A., Garai, P., & Wakelam, V. 2020, ApJ, 899, 65, doi: 10.3847/1538-4357/aba0a5

    work page doi:10.3847/1538-4357/aba0a5 2020

  42. [42]

    L., Rivilla, V

    Sanz-Novo, M., Alonso, J. L., Rivilla, V. M., et al. 2022, A&A, 666, A134, doi: 10.1051/0004-6361/202244330 14Duan et al

    work page doi:10.1051/0004-6361/202244330 2022

  43. [43]

    2019, ACS Earth and Space Chemistry, 3, 1170, doi: 10.1021/acsearthspacechem.9b00053

    Sanz-Novo, M., Largo, A., Redondo, P., & Barrientos, C. 2019, ACS Earth and Space Chemistry, 3, 1170, doi: 10.1021/acsearthspacechem.9b00053

    work page doi:10.1021/acsearthspacechem.9b00053 2019

  44. [44]

    L., et al

    Sanz-Novo, M., Belloche, A., Alonso, J. L., et al. 2020, A&A, 639, A135, doi: 10.1051/0004-6361/202038149

    work page doi:10.1051/0004-6361/202038149 2020

  45. [45]

    E., Lovas, F

    Snyder, L. E., Lovas, F. J., Hollis, J. M., et al. 2005, ApJ, 619, 914, doi: 10.1086/426677

    work page doi:10.1086/426677 2005

  46. [46]

    2004, Chemical Engineering & Technology, 27, 435, doi: https://doi.org/10.1002/ceat.200401911

    Sun, J., Yang, B., & Lin, H. 2004, Chemical Engineering & Technology, 27, 435, doi: https://doi.org/10.1002/ceat.200401911

    work page doi:10.1002/ceat.200401911 2004

  47. [47]

    T., Henkel , C., Kobayashi , C., et al

    Yan, Y. T., Henkel, C., Kobayashi, C., et al. 2023, A&A, 670, A98, doi: 10.1051/0004-6361/202244584

    work page doi:10.1051/0004-6361/202244584 2023

  48. [48]

    M., et al

    Zeng, S., Jim´ enez-Serra, I., Rivilla, V. M., et al. 2018, MNRAS, 478, 2962, doi: 10.1093/mnras/sty1174

    work page doi:10.1093/mnras/sty1174 2018

  49. [49]

    M., Jim´ enez-Serra, I., et al

    Zeng, S., Rivilla, V. M., Jim´ enez-Serra, I., et al. 2023, MNRAS, 523, 1448, doi: 10.1093/mnras/stad1478

    work page doi:10.1093/mnras/stad1478 2023