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On the abiotic origin of dimethyl sulfide: discovery of DMS in the Interstellar Medium

T0 review · 2 major / 6 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read Dimethyl sulfide, a molecule proposed as an exoplanet biosignature, has been detected for the first time in the interstellar medium, with an abundance that matches purely chemical formation.

desk verdict Solid first detection of interstellar DMS, but the LTE-based abundance and the 'conclusive abiotic' framing are softer than the abstract claims. read the letter →

arxiv 2501.08892 v2 pith:HQTRU2YR submitted 2025-01-15 astro-ph.GA

Miguel Sanz-Novo , Víctor M. Rivilla , Christian P. Endres , Valerio Lattanzi , Izaskun Jiménez-Serra , Laura Colzi , Shaoshan Zeng , Andrés Megías
show 9 more authors
Álvaro López-Gallifa Antonio Martínez-Henares David San Andrés Belén Tercero Pablo de Vicente Sergio Martín Miguel A. Requena-Torres Paola Caselli Jesús Martín-Pintado
This is my paper · ORCID
classification astro-ph.GA
keywords dimethylsulfideinterstellarmediumastrochemistryGalacticcentersulfurchemistrybiomarkerexoplanetatmospheresrotationalspectroscopy
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 first detection of dimethyl sulfide (CH₃SCH₃, DMS), the molecule once proposed as a sign of life on habitable exoplanets, in the interstellar medium, toward the Galactic Center cloud G+0.693-0.027. Using ten clean rotational lines from an ultradeep survey with the Yebes 40 m and IRAM 30 m telescopes, the authors derive a column density of $(2.6 \pm 0.3)\times10^{13}$ cm$^{-2}$, an abundance of ~$1.9\times10^{-10}$ relative to H₂, and an excitation temperature near 13 K. The central claim is that this detection proves DMS can be produced efficiently by abiotic interstellar chemistry, so its presence alone is not evidence for biology on an exoplanet. A sympathetic reader would care because the same molecule is a suggested biosignature for worlds like K2-18b, and its tentative detection there now needs an abiotic explanation.

What carries the argument

The load-bearing tool is a new astronomical line catalogue for DMS built from the most complete laboratory data (Ilyushin et al. 2020), converted to a standard catalog format with partition functions summed over all four internal-rotation substates (AA, EE, EA, AE). DMS has two equivalent methyl rotors, so every rotational level splits into four symmetry substates whose closely spaced transitions coalesce into enhanced line clusters at the broad (~20 km s$^{-1}$) linewidths of this cloud; this auto-blending strengthens the combined signal. The astronomical analysis compares the observed spectra against synthetic LTE spectra of DMS plus all ~130 previously identified molecules in the survey using the SLIM/Autofit tools, with column density and excitation temperature as free parameters and a rotational-diagram analysis as an independent check. The LTE assumption is defended by the cloud's sub-thermal but well-behaved excitation, and is acknowledged as the only viable method because no collisional rate coefficients for DMS exist.

What would settle it

Measure DMS-H₂ collisional rate coefficients and rerun the excitation modeling of the same ten lines; if a non-LTE calculation drives the column density well below the LTE value, or shifts the derived DMS/CH₃OH ratio far from the cometary value, the abundance claim and the comet-connection argument would need revision. A simpler check is a high-angular-resolution observation of one of the brightest lines, which would show whether the emission is truly extended on the scale assumed here.

Watch

Extended reading notes

Core claim

Dimethyl sulfide, the C₂H₆S isomer whose m/z signature was attributed to DMS in comet 67P, is present in the interstellar medium at an abundance of about $(1.9 \pm 0.4) \times 10^{-10}$ relative to H₂ in G+0.693-0.027. The detection rests on ten unblended R- and Q-branch lines consistent with the laboratory spectrum across 31–173 GHz, with about 50 further lines consistent with the same LTE model. The paper further establishes that DMS is ~1.6 times less abundant than its structural isomer ethanethiol and ~30 times less abundant than its oxygen analogue dimethyl ether, matching the O/S trends of related pairs; and that the DMS/CH₃OH ratio in the cloud, $(1.7 \pm 0.4) \times 10^{-3}$, matches the cometary C₂H₆S/CH₃OH ratio of $(1.3 \pm 0.4) \times 10^{-3}$. The authors conclude that DMS is efficiently formed abiotically in space, even before star formation begins, and that its use as a unique biomarker for exoplanet life needs caution.

Load-bearing premise

The derived abundance and the comet comparison assume the DMS lines can be modeled in local thermodynamic equilibrium with the emitting gas filling the telescope beams; the authors have no collisional rate coefficients to test the first part, and non-LTE effects are plausible for a large molecule in the low-density gas of this cloud.

Editorial extensions

If this is right

  • DMS is part of the interstellar sulfur inventory: it exists in a Galactic Center cloud before any star has formed, so its synthesis does not require a planet or a biosphere.
  • The near-agreement of the DMS/CH₃OH ratio between G+0.693 and comet 67P adds a data point to the case that comets inherit their organic sulfur inventory from the parental cloud.
  • Proposals to treat DMS as an unambiguous biosignature in exoplanet atmospheres must be revised, because abiotic production in the interstellar medium is now an observationally supported alternative channel.
  • The O/S abundance trends predict that other sulfur analogues of common oxygen-bearing molecules should be detectable in G+0.693 and similar shocked clouds, extending the pattern this detection fits.

Reading between the lines

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

  • The same LTE caveat means the ~30-fold DME/DMS ratio is more robust than the absolute DMS abundance, because both molecules would suffer similar beam and excitation biases; the ratio, not the column density, is the safer quantity to compare across sources.
  • A testable prediction follows from the proposed formation routes: if DMS forms on grains via CH₃ + CH₃S, its abundance should track CH₃SH and methanol desorption, whereas gas-phase routes would predict a transient early enhancement like that of dimethyl ether.
  • The tentative DMS signal in K2-18b's atmosphere becomes a test of delivery rate: interstellar DMS that survives cloud-to-comet inheritance could be delivered to planets and then destroyed or recycled by photochemistry, so atmospheric DMS would need replenishment at a rate that future time-series observations could bound.
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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 the first detection of dimethyl sulfide (CH3SCH3, DMS) in the interstellar medium, toward the Galactic Center cloud G+0.693-0.027, using ultradeep Yebes 40 m and IRAM 30 m spectral surveys. The authors identify ten clean b-type lines with integrated S/N >= 6, supplemented by roughly fifty additional blended or lower-S/N transitions, and find no missing lines in the survey coverage. From an LTE fit and a rotational diagram they derive N(DMS) = (2.6 +/- 0.3) x 10^13 cm^-2 and Tex = 13 +/- 3 K, corresponding to a fractional abundance of ~1.9 x 10^-10 relative to H2. They compare DMS abundances with related species in the same cloud and with comet 67P, finding DMS/CH3OH ~ 1.7 x 10^-3, and argue that the detection provides conclusive evidence for efficient abiotic DMS production in the ISM, with implications for the use of DMS as an exoplanet biomarker. The paper also provides a new spectroscopic catalogue of DMS, including partition function values at several temperatures, and reports all observed transitions in the appendices.

Significance. If the detection holds, this is the first identification of dimethyl sulfide in the interstellar medium, a significant addition to the inventory of interstellar organosulfur molecules and directly relevant to the ongoing debate about DMS as a biosignature. The observational case is strong: ten unblended transitions with S/N >= 6, a consistent rotational diagram, additional blended but consistent lines, and no missing lines across the survey. The paper also ships a new catalogue built from the most recent laboratory spectroscopy, with partition functions at multiple temperatures, which is a reproducible and useful resource. The quantitative abundance and the comparison with comet 67P rest on LTE assumptions and an extended-source filling factor that are acknowledged in the text but not quantified; these caveats matter for the claimed 'conclusive' wording but do not undermine the detection itself.

major comments (2)
  1. [Section 3, Table 1, Figure 2] The LTE-derived column density and excitation temperature are the basis for the fractional abundance, the DMS/CH3OH ratio, and the comparison with comet 67P, yet the same section states that the H2 density of G+0.693 is low enough to produce non-LTE effects and that no collisional rate coefficients for DMS exist. The fitted Tex = 13 +/- 3 K is far below the kinetic temperature of 70-140 K, so the populations are demonstrably sub-thermal; the single rotational temperature is an empirical fitting device rather than a physical guarantee. The quoted uncertainty of +/- 0.3 x 10^13 cm^-2 is statistical only and does not include the systematic bias from the LTE assumption, which could shift N(DMS) and hence the DMS/CH3OH ratio used for the comet comparison. Please quantify this bias if possible (for example, by rescaling collisional rates from a similar molecule such as DME), or at minimum state explicitly in the abstract and Section 4 that the quantitative abundance ratios are LTE-based values with potentially large unquantified systematics, and soften the word 'conclusive' accordingly.
  2. [Section 2, Section 3] The spectra are presented in antenna temperature units under the assumption that the molecular emission toward G+0.693 is extended compared to the telescope beam, but no dedicated map of DMS is shown to justify this filling factor for this specific molecule. If the DMS emission is partly compact, the derived column density would increase, and the comparison with CH3OH (which may have a different spatial distribution) could shift. The extended-source assumption is therefore load-bearing for the absolute abundance and for the comet ratio. Please provide a brief justification that DMS follows the extended emission pattern of the cloud, or state explicitly how a compact component would change the derived quantities.
minor comments (6)
  1. [Section 4, first paragraph] The text refers to 'the presence in the atmosphere of K2-12b'; this appears to be a typo for K2-18b, the exoplanet discussed in the introduction and in the cited Madhusudhan et al. (2023) work.
  2. [Section 1, introduction] The phrase 'O-protonated cabonyl sulfide' contains a typo; it should read 'O-protonated carbonyl sulfide'.
  3. [Section 4, paragraph 2] The word 'stablish' should be 'establish' in the sentence 'aiming to stablish general trends'.
  4. [Section 3, Table 1] The text says 'a total of ten clean b-type lines' but Table 1 includes one line labeled 'slightly blended' (at 97.022 GHz). Please clarify the wording: for example, 'ten lines used in the fit, of which nine are unblended and one is slightly blended according to the criterion defined in the text.'
  5. [Section 3, paragraph after Eq. for Tex] The sentence 'we derived a Tex = 13 +/- 3 K, in agreement with the sub-thermal excitation conditions found for many other molecules toward G+0.693' could be misread as agreement with thermal equilibrium; consider rephrasing to clarify that the agreement is with the low excitation temperatures found for other molecules under the same sub-thermal conditions.
  6. [Appendix A] In the expression for the line intensity, the constant 4.16231 x 10^-5 should be verified for consistency with the stated units (nm^2 MHz) and the adopted dipole moment; adding a reference for the numerical conversion factor would help reproducibility.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the DMS detection and LTE column density are a direct observational measurement, not a derivation that reduces to its own inputs.

full rationale

The paper reports the first interstellar detection of dimethyl sulfide toward G+0.693-0.027 and derives its column density from a multi-line LTE fit. The free parameters of the fit, N and Tex, are obtained from the observed integrated intensities of ten unblended transitions, and the result is independently corroborated by a rotational diagram analysis that gives N(DMS) = (2.8 +/- 0.4) x 10^13 cm^-2 and Tex = 11.4 +/- 0.7 K. No quantity is defined in terms of the claim it is used to support: the DMS abundance is not used to predict the same transitions it was fitted from, nor is any fitted parameter renamed as a prediction. The comparison of DMS/CH3OH with comet 67P is an interpretive juxtaposition of measured abundances, not a circular derivation. Self-citations to earlier work on G+0.693-0.027, such as Sanz-Novo et al. (2024a) for O/S trends, provide context and external measurements but are not load-bearing inputs to the DMS fit. The adopted N(H2) from Martin et al. (2008) is an independent H2 column density estimate based on C18O, not derived from DMS. The LTE assumption, noted by the authors as the only viable method given the lack of collisional rate coefficients, is a modeling assumption that may carry systematic uncertainty, but uncertainty in a physical assumption is a correctness risk, not circularity. The central claim, that DMS is present in the interstellar medium and can form abiotically, rests on the spectroscopic line identification and measured abundance, which are self-contained in this observational work.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

No new physical entities are introduced. The free parameters are the standard outputs of an LTE spectral fit, which are themselves assumptions for converting observed line intensities into abundances. The most consequential assumption is LTE, acknowledged by the authors as the only viable method because collision rates are unavailable.

free parameters (4)
  • Column density N(DMS) = (2.6 +/- 0.3) x 10^13 cm^-2
    Fitted by LTE Autofit and confirmed by rotational diagram; central to the reported abundance and ratios.
  • Excitation temperature Tex = 13 +/- 3 K (Autofit); 11.4 +/- 0.7 K (rotational diagram)
    Fitted free parameter in the LTE model; affects conversion from line intensities to column density.
  • FWHM = 20 km/s (fixed)
    Fixed in the LTE fit based on prior measurements of other species toward G+0.693-0.027; if different, the integrated intensities and fit change.
  • vLSR = 67 km/s (fixed)
    Fixed in the LTE fit to match other S-bearing species; a different value would shift the fit but not the detection.
assumptions (6)
  • domain assumption DMS rotational population is in local thermodynamic equilibrium at a single Tex
    Used for SLIM/Autofit and rotational diagram; no collisional rate coefficients for DMS exist (Section 3).
  • domain assumption DMS emission is extended relative to the telescope beams, so no beam dilution correction is applied
    Stated in Section 2, citing Jones et al. 2012, Li et al. 2020, and Zheng et al. 2024; affects absolute column density.
  • domain assumption N(H2) = 1.35 x 10^23 cm^-2 from C18O with C18O/H2 = 1.7 x 10^-7
    Used to convert column density to fractional abundance (Section 3 and Table 2).
  • ad hoc to paper Line blending criterion of <=25% residual area defines 'unblended' lines
    Threshold introduced in Section 3; lines with up to 25% contamination are included as clean.
  • domain assumption The spectroscopic catalogue built from Ilyushin et al. 2020 with a 1.5 D dipole moment from Pierce and Hayashi 1961 is accurate
    Used for all line frequencies and intensities (Appendix A).
  • domain assumption Comet 67P C2H6S signal is attributed to DMS rather than its isomer
    The DMS/CH3OH comparison depends on the Hanni et al. 2024 assignment (Table 3).

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Pith. "Pith review of On the abiotic origin of dimethyl sulfide: discovery of DMS in the Interstellar Medium." pith.science (2026). https://pith.science/paper/HQTRU2YR

@misc{pith2026250108892,
  author       = {Pith},
  title        = {Pith review of: On the abiotic origin of dimethyl sulfide: discovery of DMS in the Interstellar Medium},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HQTRU2YR}},
  note         = {Machine review of arXiv:2501.08892}
}
abstract

Following the discovery of dimethyl sulfide (CH$_3$SCH$_3$, DMS) signatures in comet 67P/Churyumov-Gerasimenko, we report the first detection of this organosulfur species in the interstellar medium, during the exploration of an ultradeep molecular line survey performed toward the Galactic Center molecular cloud G+0.693-0.027 with the Yebes 40$\,$m and IRAM 30$\,$m telescopes. We derive a molecular column density of $N$ = (2.6 $\pm$ 0.3)$\times$10$^{13}$ cm$^{-2}$, yielding a fractional abundance relative to H$_2$ of $\sim$1.9$\times$10$^{-10}$. This implies that DMS is a factor of $\sim$1.6 times less abundant than its structural isomer CH$_3$CH$_2$SH and $\sim$30 times less abundant than its O-analogue dimethyl ether (CH$_3$OCH$_3$) toward this cloud, in excellent agreement with previous results on various O/S pairs. Furthermore, we find a remarkable resemblance between the relative abundance of DMS/CH$_3$OH in G+0.693-0.027 ($\sim$1.7$\times$10$^{-3}$) and in the comet ($\sim$1.3$\times$10$^{-3}$). Although the chemistry of DMS beyond Earth is yet to be fully disclosed, this discovery provides conclusive observational evidence on its efficient abiotic production in the interstellar medium, casting doubts about using DMS as a reliable biomarker in exoplanet science.

Figures

Figures reproduced from arXiv: 2501.08892 by the authors.

Figure 1
Figure 1. (a) Selected transitions of DMS identified toward the GC molecular cloud G+0.693–0.027, which were used to derive the LTE physical parameters of the molecule (see text; listed in [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Rotational diagram of DMS toward G+0.693 (blue dots, including 1σ errors). The best linear fit to the data points is shown using a gray dotted line. The derived values for the molecular column density, N, and the excita￾tion temperature, Tex, are shown in blue. Sanz-Novo et al. 2024a,b). The fit of the individual tran￾sitions of DMS are shown in red lines in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗

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Works this paper leans on

79 extracted references · 21 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [4]

    2015, Science, 347, 1261952, 10.1126/science.1261952

    Altwegg , K., Balsiger , H., Bar-Nun , A., et al. 2015, Science, 347, 1261952, 10.1126/science.1261952

    doi:10.1126/science.1261952 2015

  4. [5]

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

    ---. 2016, Science Advances, 2, e1600285, 10.1126/sciadv.1600285

    doi:10.1126/sciadv.1600285 2016

  5. [6]

    J., et al

    Altwegg , K., Balsiger , H., Berthelier , J. J., et al. 2017, Philosophical Transactions of the Royal Society of London Series A, 375, 20160253, 10.1098/rsta.2016.0253

    arXiv 2017

  6. [7]

    J., & Scott, P

    Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, , 47, 481

    2009

  7. [8]

    2019, The Astrophysical Journal Letters, 887, L14, 10.3847/2041-8213/ab59dc

    Benneke, B., Wong, I., Piaulet, C., et al. 2019, The Astrophysical Journal Letters, 887, L14, 10.3847/2041-8213/ab59dc

    doi:10.3847/2041-8213/ab59dc 2019

  8. [9]

    2016, , 462, S253, 10.1093/mnras/stw2601

    Calmonte, U., Altwegg, K., Balsiger, H., et al. 2016, , 462, S253, 10.1093/mnras/stw2601

    doi:10.1093/mnras/stw2601 2016

Show all 79 references
  1. [10]

    I., & Herbst , E

    Caselli , P., Hasegawa , T. I., & Herbst , E. 1993, , 408, 548, 10.1086/172612

    1993 doi

  2. [11]

    C., Krissansen-Totton, J., Kiang, N

    Catling, D. C., Krissansen-Totton, J., Kiang, N. Y., et al. 2018, Astrobiology, 18, 709, 10.1089/ast.2017.1737

    2018

  3. [12]

    B., Kress, M

    Charnley, S. B., Kress, M. E., Tielens, A. G. G. M., & Millar, T. J. 1995, Astrophysical Journal v.448, 448, 232

    1995

  4. [13]

    M., et al

    Colzi, L., Martín-Pintado, J., Rivilla, V. M., et al. 2022, The Astrophysical Journal Letters, 926, L22, 10.3847/2041-8213/ac52ac

    2022 doi

  5. [14]

    2024, , 690, A121, 10.1051/0004-6361/202451382

    Colzi , L., Mart \' n-Pintado , J., Zeng , S., et al. 2024, , 690, A121, 10.1051/0004-6361/202451382

    2024 doi

  6. [15]

    1980, Journal of Molecular Spectroscopy, 83, 391

    Demaison, J., Schwoch, D., Tan, B., & Rudolph, H. 1980, Journal of Molecular Spectroscopy, 83, 391

    1980

  7. [16]

    Dreizler, H., & Rudolph, H. D. 1962, Zeitschrift f \"u r Naturforschung A, 17, 712

    1962

  8. [17]

    N., van Dishoeck, E

    Drozdovskaya, M. N., van Dishoeck, E. F., Jørgensen, J. K., et al. 2018, Monthly Notices of the Royal Astronomical Society, 476, 4949, 10.1093/mnras/sty462

    2018 doi

  9. [18]

    P., Schlemmer , S., Schilke , P., Stutzki , J., & M \"u ller , H

    Endres , C. P., Schlemmer , S., Schilke , P., Stutzki , J., & M \"u ller , H. S. P. 2016, Journal of Molecular Spectroscopy, 327, 95, 10.1016/j.jms.2016.03.005

    2016 doi

  10. [19]

    Faure , A., Lique , F., & Remijan , A. J. 2018, Journal of Physical Chemistry Letters, 9, 3199, 10.1021/acs.jpclett.8b01431

    2018 doi

  11. [20]

    J., Szalewicz, K., & Wiesenfeld, L

    Faure, A., Remijan, A. J., Szalewicz, K., & Wiesenfeld, L. 2014, , 783, 72

    2014

  12. [21]

    A., Langer, W

    Frerking, M. A., Langer, W. D., & Wilson, R. W. 1982, The , 262, 590, 10.1086/160451

    1982 doi

  13. [22]

    J., Trucks, G

    Frisch, M. J., Trucks, G. W., Schlegel, H. B., et al. 2016, Gaussian˜16 R evision C .01

    2016

  14. [23]

    2023, , 670, A114, 10.1051/0004-6361/202244843

    Fuente , A., Rivi \`e re-Marichalar , P., Beitia-Antero , L., et al. 2023, , 670, A114, 10.1051/0004-6361/202244843

    2023 doi

  15. [24]

    2006, Faraday Discussions, 133, 51

    Garrod, R., Hee Park, I., Caselli, P., & Herbst, E. 2006, Faraday Discussions, 133, 51

    2006

  16. [25]

    G., Bally , J., Barnes , A., et al

    Ginsburg , A. G., Bally , J., Barnes , A., et al. 2018, ArXiv e-prints. 1801.04941

    2018 arXiv

  17. [26]

    Glein, C. R. 2024, The Astrophysical Journal Letters, 964, L19, 10.3847/2041-8213/ad3079

    2024 doi

  18. [27]

    F., & Langer , W

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

    1999

  19. [28]

    2022, Nature Communications, 13, 3639, 10.1038/s41467-022-31346-9

    H \"a nni , N., Altwegg , K., Combi , M., et al. 2022, Nature Communications, 13, 3639, 10.1038/s41467-022-31346-9

    2022 doi

  20. [29]

    2024, The Astrophysical Journal, 976, 74, 10.3847/1538-4357/ad8565

    Hänni, N., Altwegg, K., Combi, M., et al. 2024, The Astrophysical Journal, 976, 74, 10.3847/1538-4357/ad8565

    2024 doi

  21. [30]

    2020, Journal of Molecular Structure, 1200, 127114, https://doi.org/10.1016/j.molstruc.2019.127114

    Ilyushin, V., Armieieva, I., Dorovskaya, O., et al. 2020, Journal of Molecular Structure, 1200, 127114, https://doi.org/10.1016/j.molstruc.2019.127114

    2020

  22. [31]

    Jabri , A., Van , V., Nguyen , H. V. L., et al. 2016, , 589, A127, 10.1051/0004-6361/201628074

    2016 doi

  23. [32]

    M., Caro, G

    Jim \'e nez-Escobar, A., Giuliano, B. M., Caro, G. M. M., Cernicharo, J., & Marcelino, N. 2014, , 788, 19

    2014

  24. [33]

    F., Mart \' n-Pintado , J., et al

    Jim \'e nez-Serra , I., Rodr \' guez-Almeida , L. F., Mart \' n-Pintado , J., et al. 2022, , 663, A181, 10.1051/0004-6361/202142699

    2022 doi

  25. [34]

    A., Burton , M

    Jones , P. A., Burton , M. G., Cunningham , M. R., et al. 2012, , 419, 2961, 10.1111/j.1365-2966.2011.19941.x

    2012

  26. [35]

    C., & Caselli , P

    Laas , J. C., & Caselli , P. 2019, , 624, A108, 10.1051/0004-6361/201834446

    2019 doi

  27. [36]

    2020, , 492, 556, 10.1093/mnras/stz3337

    Li, J., Wang, J., Qiao, H., et al. 2020, , 492, 556, 10.1093/mnras/stz3337

    2020 doi

  28. [37]

    J., Lutz, H., & Dreizler, H

    Lovas, F. J., Lutz, H., & Dreizler, H. 1979, Journal of Physical and Chemical Reference Data, 8, 1051

    1979

  29. [38]

    M., Beltrán, M

    López-Gallifa, A., Rivilla, V. M., Beltrán, M. T., et al. 2024, Monthly Notices of the Royal Astronomical Society, 529, 3244, 10.1093/mnras/stae676

    2024 doi

  30. [39]

    Madhusudhan, N., Piette, A. A. A., & Constantinou, S. 2021, The Astrophysical Journal, 918, 1, 10.3847/1538-4357/abfd9c

    2021 doi

  31. [40]

    2023, , 956, L13, 10.3847/2041-8213/acf577

    Madhusudhan , N., Sarkar , S., Constantinou , S., et al. 2023, , 956, L13, 10.3847/2041-8213/acf577

    2023 doi

  32. [41]

    J., et al

    Mahjoub, A., Altwegg, K., Poston, M. J., et al. 2023, Science Advances, 9, eadh0394, 10.1126/sciadv.adh0394

    2023 doi

  33. [42]

    2019, , 631, A159

    Mart \' n , S., Mart \' n-Pintado , J., Blanco-S \'a nchez , C., et al. 2019, , 631, A159

    2019

  34. [43]

    A., Mart\'in-Pintado, J., & Mauersberger, R

    Mart\'in, S., Requena-Torres, M. A., Mart\'in-Pintado, J., & Mauersberger, R. 2008, The , 678, 245

    2008

  35. [44]

    M., et al

    Mart \' n-Dom \'e nech , R., Jim \'e nez-Serra , I., Mu \ n oz Caro , G. M., et al. 2016, , 585, A112, 10.1051/0004-6361/201526271

    2016 doi

  36. [45]

    u ller , H. S. P., Schl \

    M \"u ller , H. S. P., Schl \"o der , F., Stutzki , J., & Winnewisser , G. 2005, Journal of Molecular Structure, 742, 215, 10.1016/j.molstruc.2005.01.027

    2005 doi

  37. [46]

    Pickett, H. M. 1991, J. Mol. Spectrosc., 148, 371

    1991

  38. [47]

    M., Poynter, R

    Pickett, H. M., Poynter, R. L., Cohen, E. A., et al. 1998, Journal of Quantitative Spectroscopy and Radiative Transfer, 60, 883

    1998

  39. [48]

    1961, , 35, 479

    Pierce, L., & Hayashi, M. 1961, , 35, 479

    1961

  40. [49]

    Pilcher, C. B. 2003, Astrobiology, 3, 471, 10.1089/153110703322610582

    2003 doi

  41. [50]

    J., Fedoseev , G., et al

    Qasim , D., Chuang , K. J., Fedoseev , G., et al. 2018, , 612, A83, 10.1051/0004-6361/201732355

    2018 doi

  42. [51]

    A., Mart\'in-Pintado, J., Mart\'in, S., & Morris, M

    Requena-Torres, M. A., Mart\'in-Pintado, J., Mart\'in, S., & Morris, M. R. 2008, The , 672, 352

    2008

  43. [52]

    A., Mart\'in-Pintado, J., Rodr\'iguez-Franco, A., et al

    Requena-Torres, M. A., Mart\'in-Pintado, J., Rodr\'iguez-Franco, A., et al. 2006, A&A, 455, 971, 10.1051/0004-6361:20065190

    2006 doi

  44. [53]

    2024, The Astrophysical Journal, 975, 174, 10.3847/1538-4357/ad736e

    Rey-Montejo, M., Jiménez-Serra, I., Martín-Pintado, J., et al. 2024, The Astrophysical Journal, 975, 174, 10.3847/1538-4357/ad736e

    2024 doi

  45. [54]

    M., Drozdovskaya , M

    Rivilla , V. M., Drozdovskaya , M. N., Altwegg , K., et al. 2020, , 492, 1180. 1911.11647

    2020 arXiv

  46. [55]

    M., Jim \'e nez-Serra , I., Mart \' n-Pintado , J., et al

    Rivilla , V. M., Jim \'e nez-Serra , I., Mart \' n-Pintado , J., et al. 2021, Proceedings of the National Academy of Science, 118, 2101314118

    2021

  47. [56]

    M., Colzi , L., Jim \'e nez-Serra , I., et al

    Rivilla , V. M., Colzi , L., Jim \'e nez-Serra , I., et al. 2022, , 929, L11

    2022

  48. [57]

    M., Jiménez-Serra, I., Martín-Pintado, J., et al

    Rivilla, V. M., Jiménez-Serra, I., Martín-Pintado, J., et al. 2022c, Frontiers in Astronomy and Space Sciences, 9, 10.3389/fspas.2022.876870

    2022

  49. [58]

    M., Sanz-Novo , M., Jim \'e nez-Serra , I., et al

    Rivilla , V. M., Sanz-Novo , M., Jim \'e nez-Serra , I., et al. 2023, , 953, L20, 10.3847/2041-8213/ace977

    2023 doi

  50. [59]

    F., Jim \'e nez-Serra , I., Rivilla , V

    Rodr \' guez-Almeida , L. F., Jim \'e nez-Serra , I., Rivilla , V. M., et al. 2021, , 912, L11

    2021

  51. [60]

    2023, Monthly Notices of the Royal Astronomical Society, 526, 4209, 10.1093/mnras/stad3005

    Rubin, M., Altwegg, K., Berthelier, J.-J., et al. 2023, Monthly Notices of the Royal Astronomical Society, 526, 4209, 10.1093/mnras/stad3005

    2023 doi

  52. [61]

    1960, Zeitschrift Naturforschung Teil A, 15, 742

    Rudolph, H., Dreizler, H., & Maier, W. 1960, Zeitschrift Naturforschung Teil A, 15, 742

    1960

  53. [62]

    R., Carlson , R., Gurnett , D., & Hord , C

    Sagan , C., Thompson , W. R., Carlson , R., Gurnett , D., & Hord , C. 1993, , 365, 715, 10.1038/365715a0

    1993 doi

  54. [63]

    M., Colzi , L., et al

    San Andr \'e s , D., Rivilla , V. M., Colzi , L., et al. 2024, , 967, 39, 10.3847/1538-4357/ad3af3

    2024 doi

  55. [64]

    C., Enrique-Romero , J., Lamberts , T., Linnartz , H., & Chuang , K.-J

    Santos , J. C., Enrique-Romero , J., Lamberts , T., Linnartz , H., & Chuang , K.-J. 2024, ACS Earth and Space Chemistry, 8, 1646, 10.1021/acsearthspacechem.4c00150

    2024 doi

  56. [65]

    M., Jim \'e nez-Serra , I., et al

    Sanz-Novo , M., Rivilla , V. M., Jim \'e nez-Serra , I., et al. 2023, , 954, 3, 10.3847/1538-4357/ace523

    2023 doi

  57. [66]

    2024 a , , 965, 149, 10.3847/1538-4357/ad2c01

    ---. 2024 a , , 965, 149, 10.3847/1538-4357/ad2c01

    2024 doi

  58. [67]

    M., M \"u ller , H

    Sanz-Novo , M., Rivilla , V. M., M \"u ller , H. S. P., et al. 2024 b , , 965, L26, 10.3847/2041-8213/ad3945

    2024 doi

  59. [68]

    2013, The Astrophysical Journal, 777, 95, 10.1088/0004-637X/777/2/95

    Seager, S., Bains, W., & Hu, R. 2013, The Astrophysical Journal, 777, 95, 10.1088/0004-637X/777/2/95

    2013 doi

  60. [69]

    2016, Astrobiology, 16, 465, 10.1089/ast.2015.1404

    Seager, S., Bains, W., & Petkowski, J. 2016, Astrobiology, 16, 465, 10.1089/ast.2015.1404

    2016

  61. [70]

    2019, , 482, 3567, 10.1093/mnras/sty2903

    Skouteris , D., Balucani , N., Ceccarelli , C., et al. 2019, , 482, 3567, 10.1093/mnras/sty2903

    2019 doi

  62. [71]

    E., Buhl, D., Schwartz, P

    Snyder, L. E., Buhl, D., Schwartz, P. R., et al. 1974, Astrophysical Journal, 191, L79

    1974

  63. [72]

    S., & Charnley, S

    Taquet, V., Wirström, E. S., & Charnley, S. B. 2016, The , 821, 46, 10.3847/0004-637X/821/1/46

    2016 doi

  64. [73]

    A., Gallego , J

    Tercero , F., L \'o pez-P \'e rez , J. A., Gallego , J. D., et al. 2021, , 645, A37, 10.1051/0004-6361/202038701

    2021 doi

  65. [74]

    2002, The , 571, L173, 10.1086/341412

    Watanabe, N., & Kouchi, A. 2002, The , 571, L173, 10.1086/341412

    2002 doi

  66. [75]

    L., & Rood, R

    Wilson, T. L., & Rood, R. 1994, , 32, 191, 10.1146/annurev.aa.32.090194.001203

    1994

  67. [76]

    F., Batalha, N

    Wogan, N. F., Batalha, N. E., Zahnle, K. J., et al. 2024, The Astrophysical Journal Letters, 963, L7, 10.3847/2041-8213/ad2616

    2024 doi

  68. [77]

    S., Aponte , J

    Zeichner , S. S., Aponte , J. C., Bhattacharjee , S., et al. 2023, Science, 382, 1411, 10.1126/science.adg6304

    2023 doi

  69. [78]

    M., et al

    Zeng , S., Jim \'e nez-Serra , I., Rivilla , V. M., et al. 2018, , 478, 2962

    2018

  70. [79]

    2020, , 497, 4896, 10.1093/mnras/staa2187

    Zeng, S., Zhang, Q., Jiménez-Serra, I., et al. 2020, , 497, 4896, 10.1093/mnras/staa2187

    2020 doi

  71. [80]

    2024, , 961, 58, 10.3847/1538-4357/ad072c

    Zheng, S., Li, J., Wang, J., et al. 2024, , 961, 58, 10.3847/1538-4357/ad072c

    2024 doi

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