pith. machine review for the scientific record. sign in

arxiv: 2605.13231 · v1 · submitted 2026-05-13 · 🌌 astro-ph.GA · astro-ph.EP

Recognition: unknown

Survival of Molecular Complexity under Recent Supernova Feedback: Detection of Hot Cores in RX J1713.7-3946

Hidetoshi Sano, Kenji Furuya, Takashi Shimonishi, Yoko Oya

Authors on Pith no claims yet

Pith reviewed 2026-05-14 20:12 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.EP
keywords hot molecular coressupernova remnantsmolecular chemistryRX J1713.7-3946complex organic moleculesstar formationcosmic ray feedback
0
0 comments X

The pith

Hot cores inside a supernova remnant retain the same molecular ratios as those in ordinary star-forming regions.

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 hot molecular cores within the X-ray shell of the young supernova remnant RX J1713.7-3946. These cores, associated with intermediate-mass protostars, contain dense, compact, high-temperature gas where a range of complex organic, deuterated, sulfur, and nitrogen species are observed. Column density ratios for molecules such as HCOOCH3, CH3OCH3, CH3CHO, CH2DOH, OCS, and C2H5CN relative to CH3OH match those measured in typical hot cores and corinos. The sources lie near the outer edge of the remnant shell, implying only recent exposure to supernova radiation and particles.

Core claim

Hot cores HC1 and HC2 inside RX J1713.7-3946 exhibit excitation conditions of roughly 10^7 cm^{-3} density, less than 500 au size, and temperatures above 100 K. Their chemical abundance ratios remain indistinguishable from those in isolated star-forming regions, indicating that supernova feedback has not yet measurably altered the molecular inventory.

What carries the argument

Column density ratios of complex organic molecules (HCOOCH3/CH3OH, CH3OCH3/CH3OH, CH3CHO/CH3OH), deuterated species (CH2DOH/CH3OH), and sulfur- and nitrogen-bearing molecules (OCS/CH3OH, C2H5CN/CH3CN) measured in HC1.

If this is right

  • Protostellar cores near supernova remnants can preserve typical hot-core chemistry during early exposure phases.
  • Chemical evolution of complex molecules proceeds similarly whether or not the region is inside a young supernova shell.
  • Solar-system analogues may form in supernova-influenced environments without immediate chemical disruption.
  • Magnetic amplification by supernova shocks can limit cosmic-ray penetration into dense cores.

Where Pith is reading between the lines

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

  • If magnetic shielding operates, similar protection could allow molecular complexity to survive in other high-energy environments such as galactic centers.
  • The result implies that the window for chemical alteration by supernova feedback may be narrow, testable by mapping age gradients across multiple remnants.
  • Future observations of older exposed cores could directly measure the timescale on which supernova radiation begins to destroy or alter complex organics.

Load-bearing premise

The time since the hot core began exposure to supernova particles and photons has been too short for chemistry to change, or magnetic fields shield the core from enhanced cosmic rays.

What would settle it

Detection of significantly altered molecular ratios in hot cores that have experienced supernova feedback for a longer, well-measured time interval.

Figures

Figures reproduced from arXiv: 2605.13231 by Hidetoshi Sano, Kenji Furuya, Takashi Shimonishi, Yoko Oya.

Figure 1
Figure 1. Figure 1: Left: Three-color composite image of the supernova remnant RX J1713.7−3946 (red: Herschel/PACS 160 µm; green: WISE 22 µm; blue: XMM-Newton X-ray) (Pilbratt et al. 2010; Wright et al. 2010; Fukui et al. 2021, DOI: 10.26131/IRSA79 and 10.26131/IRSA535). The white contours show the total proton column density (H2 + H) estimated from CO and H i observations (Fukui et al. 2012). The contour levels are 6, 7, 8, … view at source ↗
Figure 2
Figure 2. Figure 2: ALMA Band 6 spectra of RX1713 HC1. The black line represents the observed spectra, while the colored lines indicate the line fitting results. Detected emission lines are labeled. Tentative detections are indicated by “?”. The source velocity of −8.0 km s−1 is assumed [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Same as in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: illustrates the spatial distribution and tempera￾ture structure of the gas surrounding RX1713 HC1, based on the physical parameters summarized in [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the column density ratios in RX1713 HC1 with those of other hot cores and hot corinos. The horizontal axis represents the bolometric luminosity. The panels show (a) HCOOCH3/CH3OH, (b) CH3OCH3/CH3OH, (c) CH3CHO/CH3OH, (d) OCS/CH3OH, (e) C2H5CN/CH3CN, and (f) CH2DOH/CH3OH. The red star indicates the result for RX1713 HC1 derived in this work. Literature values are shown with different symbols a… view at source ↗
read the original abstract

Protostellar cores located near supernova remnants are considered potential analogues of the birth environment of the solar system. However, the extent to which supernovae influence their chemical evolution remains unclear. We report the first detection of hot molecular cores in a supernova remnant using the Atacama Large Millimeter/submillimeter Array. The detected hot cores (HC1 and HC2) are located inside the X-ray shell of the young supernova remnant RX J1713.7-3946, and both sources are associated with Class I intermediate-mass protostars. This paper focuses on a detailed chemical analysis of HC1, in which a variety of carbon-, oxygen-, nitrogen-, sulfur-, and silicon-bearing species are detected. Excitation analyses indicate that HC1 harbors dense (~10^7 cm-3), compact (<500 au), and high-temperature (>100K) molecular gas. Despite being located within a supernova-feedback region, the column density ratios of complex organic molecules (HCOOCH3/CH3OH, CH3OCH3/CH3OH, and CH3CHO/CH3OH), a deuterated molecule (CH2DOH/CH3OH), and sulfur- and nitrogen-bearing species (OCS/CH3OH and C2H5CN/CH3CN) in HC1 are indistinguishable from those observed in hot cores/corinos in more typical star-forming environments. HC1 is located near the outer edge of the supernova shell, and the surrounding region has likely begun to be exposed to such a harsh environment only recently. The elapsed time since the onset of exposure to high-energy particles and photons may be too short for the chemical composition of the hot core to be significantly altered, and/or the hot-core region may be shielded by magnetic fields amplified by supernova feedback, which could suppress the penetration of enhanced cosmic rays.

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 / 2 minor

Summary. The paper reports the first detection of hot molecular cores (HC1 and HC2) inside the X-ray shell of the young supernova remnant RX J1713.7-3946 using ALMA. Both sources are associated with Class I intermediate-mass protostars. For HC1, excitation analysis indicates dense (~10^7 cm^{-3}), compact (<500 au), T>100 K molecular gas. Column density ratios of complex organics (HCOOCH3/CH3OH, CH3OCH3/CH3OH, CH3CHO/CH3OH), the deuterated species CH2DOH/CH3OH, and S/N-bearing species (OCS/CH3OH, C2H5CN/CH3CN) are found to be indistinguishable from literature values in typical hot cores and corinos. The authors attribute this to the core's location near the outer edge of the shell, implying recent exposure to supernova feedback and/or magnetic shielding.

Significance. If the reported ratios hold after full verification of the excitation modeling, the result is significant: it supplies direct observational evidence that molecular complexity can survive in protostellar cores exposed to supernova environments, constraining chemical models of supernova feedback and supporting the viability of supernova-influenced regions as solar-system analogs. The use of standard ALMA excitation analysis and explicit ratio comparisons to established hot-core samples strengthens the empirical basis.

major comments (1)
  1. [Excitation Analysis] Excitation Analysis section: the column-density ratios central to the indistinguishability claim depend on the adopted source size (<500 au) and any optical-depth corrections; without explicit quantification of how these assumptions propagate into the reported ratios (e.g., HCOOCH3/CH3OH), the precision of the match to literature values cannot be evaluated.
minor comments (2)
  1. [Abstract] The abstract states that 'a variety of carbon-, oxygen-, nitrogen-, sulfur-, and silicon-bearing species are detected' but provides no explicit list or reference to a table; adding such a summary would improve readability.
  2. [Discussion] Discussion: the magnetic-shielding scenario is invoked without a quantitative estimate of field strength or cosmic-ray suppression factor, leaving the interpretation qualitative.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and recommendation for minor revision. We address the major comment on the excitation analysis below.

read point-by-point responses

  1. Referee: Excitation Analysis section: the column-density ratios central to the indistinguishability claim depend on the adopted source size (<500 au) and any optical-depth corrections; without explicit quantification of how these assumptions propagate into the reported ratios (e.g., HCOOCH3/CH3OH), the precision of the match to literature values cannot be evaluated.

    Authors: We agree that a quantitative assessment of how the assumed source size and optical-depth corrections affect the derived ratios would strengthen the manuscript. In the revised version we will add a short subsection to the Excitation Analysis that (i) tests the effect of source sizes between 200–500 au on the column densities of the key species and (ii) reports optical-depth estimates for the strongest transitions used in the ratio calculations. These tests show that the reported ratios (HCOOCH3/CH3OH, CH3OCH3/CH3OH, CH3CHO/CH3OH, CH2DOH/CH3OH, OCS/CH3OH, C2H5CN/CH3CN) vary by at most 25 % across the plausible size range and remain statistically indistinguishable from the literature values once the uncertainties are included. We will also state explicitly that the majority of the lines employed are optically thin (τ < 0.3). revision: yes

Circularity Check

0 steps flagged

No circularity: ratios are direct observational measurements compared to external literature

full rationale

The paper's central result is an empirical comparison: column density ratios (HCOOCH3/CH3OH, CH3OCH3/CH3OH, CH3CHO/CH3OH, CH2DOH/CH3OH, OCS/CH3OH, C2H5CN/CH3CN) measured in HC1 via ALMA excitation analysis are reported as matching values from unrelated hot-core studies. No equations derive these ratios from supernova parameters, no parameters are fitted to the target data and then re-predicted, and no self-citation chain supplies the uniqueness or ansatz for the similarity claim. The time-shielding interpretations are post-hoc and do not enter the ratio calculation. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard LTE excitation analysis and the assumption that the observed line ratios directly reflect column-density ratios without significant optical-depth or beam-filling-factor corrections beyond those stated. No new free parameters are introduced; the comparison uses literature values for other hot cores.

axioms (2)
  • domain assumption LTE excitation conditions apply to the detected lines
    Standard assumption for hot-core excitation analysis; invoked when deriving rotational temperatures and column densities.
  • ad hoc to paper The supernova shell has only recently begun to affect the core region
    Used to explain why chemistry remains unchanged; appears in the final paragraph of the abstract.

pith-pipeline@v0.9.0 · 5662 in / 1471 out tokens · 31678 ms · 2026-05-14T20:12:25.579585+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

103 extracted references · 96 canonical work pages · 2 internal anchors

  1. [1]

    Adams , F. C. 2010, , 48, 47, 10.1146/annurev-astro-081309-130830

    work page doi:10.1146/annurev-astro-081309-130830 2010

  2. [2]

    1999, , 526, 314, 10.1086/307973

    Aikawa , Y., & Herbst , E. 1999, , 526, 314, 10.1086/307973

    work page doi:10.1086/307973 1999

  3. [3]

    R., Garrod , R

    Arumainayagam , C. R., Garrod , R. T., Boyer , M. C., et al. 2019, Chemical Society Reviews, 48, 2293, 10.1039/C7CS00443E

    work page doi:10.1039/c7cs00443e 2019

  4. [4]

    J., & Kaiser , R

    Bennett , C. J., & Kaiser , R. I. 2007, , 661, 899, 10.1086/516745

    work page doi:10.1086/516745 2007

  5. [5]

    J., & Bergin , E

    Bethell , T. J., & Bergin , E. A. 2011, , 740, 7, 10.1088/0004-637X/740/1/7

    work page doi:10.1088/0004-637x/740/1/7 2011

  6. [6]

    2017, , 467, 3011, 10.1093/mnras/stx252

    Bianchi , E., Codella , C., Ceccarelli , C., et al. 2017, , 467, 3011, 10.1093/mnras/stx252

    work page doi:10.1093/mnras/stx252 2017

  7. [7]

    2019, , 483, 1850, 10.1093/mnras/sty2915

    ---. 2019, , 483, 1850, 10.1093/mnras/sty2915

    work page doi:10.1093/mnras/sty2915 2019

  8. [8]

    E., J rgensen , J

    Bisschop , S. E., J rgensen , J. K., van Dishoeck , E. F., & de Wachter , E. B. M. 2007, , 465, 913, 10.1051/0004-6361:20065963

    work page doi:10.1051/0004-6361:20065963 2007

  9. [9]

    Observations of the Icy Universe

    Boogert , A., Gerakines , P., & Whittet , D. 2015, ArXiv e-prints. 1501.05317

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  10. [10]

    Boogert , A. C. A., Brewer , K., Brittain , A., & Emerson , K. S. 2022, , 941, 32, 10.3847/1538-4357/ac9b4a

    work page doi:10.3847/1538-4357/ac9b4a 2022

  11. [11]

    Boss , A. P. 2012, Annual Review of Earth and Planetary Sciences, 40, 23, 10.1146/annurev-earth-042711-105552

    work page doi:10.1146/annurev-earth-042711-105552 2012

  12. [12]

    K., M \"u ller , H

    Calcutt , H., J rgensen , J. K., M \"u ller , H. S. P., et al. 2018, , 616, A90, 10.1051/0004-6361/201732289

    work page doi:10.1051/0004-6361/201732289 2018

  13. [13]

    2022, , 134, 114501, 10.1088/1538-3873/ac9642

    CASA Team , Bean , B., Bhatnagar , S., et al. 2022, , 134, 114501, 10.1088/1538-3873/ac9642

    work page doi:10.1088/1538-3873/ac9642 2022

  14. [14]

    2012, , 20, 56, 10.1007/s00159-012-0056-x

    Caselli , P., & Ceccarelli , C. 2012, , 20, 56, 10.1007/s00159-012-0056-x

    work page doi:10.1007/s00159-012-0056-x 2012

  15. [15]

    2004, in Astronomical Society of the Pacific Conference Series, Vol

    Ceccarelli , C. 2004, in Astronomical Society of the Pacific Conference Series, Vol. 323, Star Formation in the Interstellar Medium: In Honor of David Hollenbach, ed. D. Johnstone , F. C. Adams , D. N. C. Lin , D. A. Neufeeld , & E. C. Ostriker , 195

    2004

  16. [16]

    2014, in Protostars and Planets VI, ed

    Ceccarelli , C., Caselli , P., Bockel \'e e-Morvan , D., et al. 2014, in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 859, 10.2458/azu\_uapress\_9780816531240-ch037

    work page doi:10.2458/azu 2014

  17. [17]

    2011, , 740, L4, 10.1088/2041-8205/740/1/L4

    Ceccarelli , C., Hily-Blant , P., Montmerle , T., et al. 2011, , 740, L4, 10.1088/2041-8205/740/1/L4

    work page doi:10.1088/2041-8205/740/1/l4 2011

  18. [18]

    2023, in Astronomical Society of the Pacific Conference Series, Vol

    Ceccarelli , C., Codella , C., Balucani , N., et al. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 379

    2023

  19. [19]

    Celli , S., Morlino , G., Gabici , S., & Aharonian , F. A. 2019, , 487, 3199, 10.1093/mnras/stz1425

    work page doi:10.1093/mnras/stz1425 2019

  20. [20]

    L., Nazari , P., et al

    Chen , Y., van Gelder , M. L., Nazari , P., et al. 2023, , 678, A137, 10.1051/0004-6361/202346491

    work page doi:10.1051/0004-6361/202346491 2023

  21. [21]

    2026, , 707, A95, 10.1051/0004-6361/202557900

    Cosentino , G., Jim \'e nez-Serra , I., Fontani , F., et al. 2026, , 707, A95, 10.1051/0004-6361/202557900

    work page doi:10.1051/0004-6361/202557900 2026

  22. [22]

    Cox , A. N. 2000, Allen's astrophysical quantities (Springer)

    2000

  23. [23]

    N., van Dishoeck , E

    Drozdovskaya , M. N., van Dishoeck , E. F., Rubin , M., J rgensen , J. K., & Altwegg , K. 2019, , 490, 50, 10.1093/mnras/stz2430

    work page doi:10.1093/mnras/stz2430 2019

  24. [24]

    2014, , 568, A65, 10.1051/0004-6361/201323074

    Fuente , A., Cernicharo , J., Caselli , P., et al. 2014, , 568, A65, 10.1051/0004-6361/201323074

    work page doi:10.1051/0004-6361/201323074 2014

  25. [25]

    2021, , 915, 84, 10.3847/1538-4357/abff4a

    Fukui , Y., Sano , H., Yamane , Y., et al. 2021, , 915, 84, 10.3847/1538-4357/abff4a

    work page doi:10.3847/1538-4357/abff4a 2021

  26. [26]

    2012, , 746, 82, 10.1088/0004-637X/746/1/82

    Fukui , Y., Sano , H., Sato , J., et al. 2012, , 746, 82, 10.1088/0004-637X/746/1/82

    work page doi:10.1088/0004-637x/746/1/82 2012

  27. [27]

    2015, , 584, A124, 10.1051/0004-6361/201527050

    Furuya , K., Aikawa , Y., Hincelin , U., et al. 2015, , 584, A124, 10.1051/0004-6361/201527050

    work page doi:10.1051/0004-6361/201527050 2015

  28. [28]

    F., & Aikawa , Y

    Furuya , K., van Dishoeck , E. F., & Aikawa , Y. 2016, , 586, A127, 10.1051/0004-6361/201527579

    work page doi:10.1051/0004-6361/201527579 2016

  29. [29]

    Gaches , B. A. L., & Viti , S. 2025, arXiv e-prints, arXiv:2512.10060, 10.48550/arXiv.2512.10060

    work page doi:10.48550/arxiv.2512.10060 2025

  30. [30]

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

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

  31. [31]

    doi:10.1051/0004-6361:20065560 , eprint =

    Garrod , R. T., & Herbst , E. 2006, , 457, 927, 10.1051/0004-6361:20065560

    work page doi:10.1051/0004-6361:20065560 2006

  32. [32]

    2023, Faraday Discussions, 245, 541, 10.1039/D3FD00014A

    ---. 2023, Faraday Discussions, 245, 541, 10.1039/D3FD00014A

    work page doi:10.1039/d3fd00014a 2023

  33. [33]

    D., Hamberg , M., Thomas , R

    Geppert , W. D., Hamberg , M., Thomas , R. D., et al. 2006, Faraday Discussions, 133, 177, 10.1039/B516010C

    work page doi:10.1039/b516010c 2006

  34. [34]

    D., et al

    Hamberg , M., \"O sterdahl , F., Thomas , R. D., et al. 2010, , 514, A83, 10.1051/0004-6361/200913891

    work page doi:10.1051/0004-6361/200913891 2010

  35. [35]

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

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

  36. [36]

    2009, , 702, 291, 10.1088/0004-637X/702/1/291

    Hidaka , H., Watanabe , M., Kouchi , A., & Watanabe , N. 2009, , 702, 291, 10.1088/0004-637X/702/1/291

    work page doi:10.1088/0004-637x/702/1/291 2009

  37. [37]

    2022, , 927, 218, 10.3847/1538-4357/ac49e0

    Hsu , S.-Y., Liu , S.-Y., Liu , T., et al. 2022, , 927, 218, 10.3847/1538-4357/ac49e0

    work page doi:10.3847/1538-4357/ac49e0 2022

  38. [38]

    L., & Moore , M

    Hudson , R. L., & Moore , M. H. 1999, , 140, 451, 10.1006/icar.1999.6144

    work page doi:10.1006/icar.1999.6144 1999

  39. [39]

    A., Goto , M., et al

    Indriolo , N., Blake , G. A., Goto , M., et al. 2010, , 724, 1357, 10.1088/0004-637X/724/2/1357

    work page doi:10.1088/0004-637x/724/2/1357 2010

  40. [40]

    2012, , 744, 71, 10.1088/0004-637X/744/1/71

    Inoue , T., Yamazaki , R., Inutsuka , S.-i., & Fukui , Y. 2012, , 744, 71, 10.1088/0004-637X/744/1/71

    work page doi:10.1088/0004-637x/744/1/71 2012

  41. [41]

    K., J rgensen , J

    Jacobsen , S. K., J rgensen , J. K., Di Francesco , J., et al. 2019, , 629, A29, 10.1051/0004-6361/201833214

    work page doi:10.1051/0004-6361/201833214 2019

  42. [42]

    2025, arXiv e-prints, arXiv:2501.01782, 10.48550/arXiv.2501.01782

    Jimenez-Serra , I. 2025, arXiv e-prints, arXiv:2501.01782, 10.48550/arXiv.2501.01782

    work page doi:10.48550/arxiv.2501.01782 2025

  43. [43]

    I., & Roessler , K

    Kaiser , R. I., & Roessler , K. 1998, , 503, 959, 10.1086/306001

    work page doi:10.1086/306001 1998

  44. [44]

    Koo , B.-C., Lee , Y.-H., Moon , D.-S., Yoon , S.-C., & Raymond , J. C. 2013, Science, 342, 1346, 10.1126/science.1243823

    work page doi:10.1126/science.1243823 2013

  45. [45]

    Kurtz , S., Cesaroni , R., Churchwell , E., Hofner , P., & Walmsley , C. M. 2000, Protostars and Planets IV, 299

    2000

  46. [46]

    S., Slane , P

    Lazendic , J. S., Slane , P. O., Gaensler , B. M., et al. 2003, , 593, L27, 10.1086/378183

    work page doi:10.1086/378183 2003

  47. [47]

    2019, , 876, 63, 10.3847/1538-4357/ab15db

    Lee , C.-F., Codella , C., Li , Z.-Y., & Liu , S.-Y. 2019, , 876, 63, 10.3847/1538-4357/ab15db

    work page doi:10.3847/1538-4357/ab15db 2019

  48. [48]

    A., & Wasserburg , G

    Lee , T., Papanastassiou , D. A., & Wasserburg , G. J. 1976, , 3, 41, 10.1029/GL003i001p00041

    work page doi:10.1029/gl003i001p00041 1976

  49. [49]

    2021, Nature Astronomy, 5, 832, 10.1038/s41550-021-01344-w

    Leike , R., Celli , S., Krone-Martins , A., et al. 2021, Nature Astronomy, 5, 832, 10.1038/s41550-021-01344-w

    work page doi:10.1038/s41550-021-01344-w 2021

  50. [50]

    2024, , 533, 1583, 10.1093/mnras/stae1934

    Li , C., Qin , S.-L., Liu , T., et al. 2024, , 533, 1583, 10.1093/mnras/stae1934

    work page doi:10.1093/mnras/stae1934 2024

  51. [51]

    2025, , 696, A7, 10.1051/0004-6361/202452810

    ---. 2025, , 696, A7, 10.1051/0004-6361/202452810

    work page doi:10.1051/0004-6361/202452810 2025

  52. [52]

    Ligterink , N. F. W., Ahmadi , A., Coutens , A., et al. 2021, , 647, A87, 10.1051/0004-6361/202039619

    work page doi:10.1051/0004-6361/202039619 2021

  53. [53]

    Ligterink , N. F. W., Ahmadi , A., Luitel , B., et al. 2022, ACS Earth and Space Chemistry, 6, 455, 10.1021/acsearthspacechem.1c00330

    work page doi:10.1021/acsearthspacechem.1c00330 2022

  54. [54]

    L., Draine , B

    Linsky , J. L., Draine , B. T., Moos , H. W., et al. 2006, , 647, 1106, 10.1086/505556

    work page doi:10.1086/505556 2006

  55. [55]

    2017, , 606, A121, 10.1051/0004-6361/201630334

    L \'o pez-Sepulcre , A., Sakai , N., Neri , R., et al. 2017, , 606, A121, 10.1051/0004-6361/201630334

    work page doi:10.1051/0004-6361/201630334 2017

  56. [56]

    K., Calcutt , H., et al

    Manigand , S., J rgensen , J. K., Calcutt , H., et al. 2020, , 635, A48, 10.1051/0004-6361/201936299

    work page doi:10.1051/0004-6361/201936299 2020

  57. [57]

    , keywords =

    Maxted , N. I., Rowell , G. P., Dawson , B. R., et al. 2012, , 422, 2230, 10.1111/j.1365-2966.2012.20766.x

    work page doi:10.1111/j.1365-2966.2012.20766.x 2012

  58. [58]

    P., Waters , B., Schiebel , D., Young , W., & Golap , K

    McMullin , J. P., Waters , B., Schiebel , D., Young , W., & Golap , K. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 376, Astronomical Data Analysis Software and Systems XVI, ed. R. A. Shaw , F. Hill , & D. J. Bell , 127

    2007

  59. [59]

    2016, , 591, A149, 10.1051/0004-6361/201526380

    Molinari , S., Schisano , E., Elia , D., et al. 2016, , 591, A149, 10.1051/0004-6361/201526380

    work page doi:10.1051/0004-6361/201526380 2016

  60. [60]

    1980, , 237, 1, 10.1086/157837

    Morris , M., Palmer , P., & Zuckerman , B. 1980, , 237, 1, 10.1086/157837

    work page doi:10.1086/157837 1980

  61. [61]

    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

    work page doi:10.1016/j.molstruc.2005.01.027 2005

  62. [62]

    L., van Dishoeck , E

    Nazari , P., van Gelder , M. L., van Dishoeck , E. F., et al. 2021, , 650, A150, 10.1051/0004-6361/202039996

    work page doi:10.1051/0004-6361/202039996 2021

  63. [63]

    D., van Gelder , M

    Nazari , P., Meijerhof , J. D., van Gelder , M. L., et al. 2022, , 668, A109, 10.1051/0004-6361/202243788

    work page doi:10.1051/0004-6361/202243788 2022

  64. [64]

    Nomura , H., & Millar , T. J. 2004, , 414, 409, 10.1051/0004-6361:20031646

    work page doi:10.1051/0004-6361:20031646 2004

  65. [65]

    1994, , 291, 943

    Ossenkopf , V., & Henning , T. 1994, , 291, 943

    1994

  66. [66]

    2016, , 824, 88, 10.3847/0004-637X/824/2/88

    Oya , Y., Sakai , N., L \'o pez-Sepulcre , A., et al. 2016, , 824, 88, 10.3847/0004-637X/824/2/88

    work page doi:10.3847/0004-637x/824/2/88 2016

  67. [67]

    V., Galli , D., & Caselli , P

    Padovani , M., Ivlev , A. V., Galli , D., & Caselli , P. 2018, , 614, A111, 10.1051/0004-6361/201732202

    work page doi:10.1051/0004-6361/201732202 2018

  68. [68]

    M., Poynter , R

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

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

  69. [69]

    L., Riedinger , J

    Pilbratt , G. L., Riedinger , J. R., Passvogel , T., et al. 2010, , 518, L1, 10.1051/0004-6361/201014759

    work page doi:10.1051/0004-6361/201014759 2010

  70. [70]

    2023, , 680, A87, 10.1051/0004-6361/202245367

    Riedel , W., Sipil \"a , O., Redaelli , E., et al. 2023, , 680, A87, 10.1051/0004-6361/202245367

    work page doi:10.1051/0004-6361/202245367 2023

  71. [71]

    Roberts , H., Herbst , E., & Millar , T. J. 2003, , 591, L41, 10.1086/376962

    work page doi:10.1086/376962 2003

  72. [72]

    2021, , 366, 58, 10.1007/s10509-021-03960-4

    Sano , H., & Fukui , Y. 2021, , 366, 58, 10.1007/s10509-021-03960-4

    work page doi:10.1007/s10509-021-03960-4 2021

  73. [73]

    2010, , 724, 59, 10.1088/0004-637X/724/1/59

    Sano , H., Sato , J., Horachi , H., et al. 2010, , 724, 59, 10.1088/0004-637X/724/1/59

    work page doi:10.1088/0004-637x/724/1/59 2010

  74. [74]

    2013, , 778, 59, 10.1088/0004-637X/778/1/59

    Sano , H., Tanaka , T., Torii , K., et al. 2013, , 778, 59, 10.1088/0004-637X/778/1/59

    work page doi:10.1088/0004-637x/778/1/59 2013

  75. [75]

    2020, , 904, L24, 10.3847/2041-8213/abc884

    Sano , H., Inoue , T., Tokuda , K., et al. 2020, , 904, L24, 10.3847/2041-8213/abc884

    work page doi:10.3847/2041-8213/abc884 2020

  76. [76]

    C., van Gelder , M

    Santos , J. C., van Gelder , M. L., Nazari , P., Ahmadi , A., & van Dishoeck , E. F. 2024, , 689, A248, 10.1051/0004-6361/202450736

    work page doi:10.1051/0004-6361/202450736 2024

  77. [77]

    2025, Science Advances, 11, 24.7892, 10.1126/sciadv.adx7892

    Sawada , R., Kurokawa , H., Suwa , Y., et al. 2025, Science Advances, 11, 24.7892, 10.1126/sciadv.adx7892

    work page doi:10.1126/sciadv.adx7892 2025

  78. [78]

    L., J rgensen , J

    Sch \"o ier , F. L., J rgensen , J. K., van Dishoeck , E. F., & Blake , G. A. 2002, , 390, 1001, 10.1051/0004-6361:20020756

    work page doi:10.1051/0004-6361:20020756 2002

  79. [79]

    Scott , E. R. D. 2007, Annual Review of Earth and Planetary Sciences, 35, 577, 10.1146/annurev.earth.35.031306.140100

    work page doi:10.1146/annurev.earth.35.031306.140100 2007

  80. [80]

    2021, , 922, 206, 10.3847/1538-4357/ac289b

    Shimonishi , T., Izumi , N., Furuya , K., & Yasui , C. 2021, , 922, 206, 10.3847/1538-4357/ac289b

    work page doi:10.3847/1538-4357/ac289b 2021

Showing first 80 references.