PRODIGE – envelope to disk with NOEMA Article Swipe
L. A. Busch
,
J. E. Pineda
,
O. Sipilä
,
Dominique Segura-Cox
,
P. Caselli
,
María José Maureira
,
C. Gieser
,
Timothy H. Hsieh
,
M. T. Valdivia-Mena
,
L. Bouscasse
,
Th. Henning
,
D. Semenov
,
A. Fuente
,
M. Tafalla
,
J.J. Miranzo-Pastor
,
L. Colzi
,
Y.-R. Chou
,
S. Guilloteau
·
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.1051/0004-6361/202554104
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.1051/0004-6361/202554104
Context . The 12 C/ 13 C isotope ratio has been derived towards numerous cold clouds (~20-50 K) and a couple of protoplanetary disks and exoplanet atmospheres. However, direct measurements of this ratio in the warm gas (>100 K) around young low-mass protostars remain scarce but are required to study its evolution during star and planet formation. Aims . We aim to derive 12 C/ 13 C ratios from the isotopologues of the complex organic molecules (COMs) CH 3 OH and CH 3 CN in the warm gas towards seven Class 0/I protostellar systems to improve our understanding of the evolution of the 12 C/ 13 C ratios during star and planet formation. Methods . We used the data that were taken as part of the PROtostars & DIsks: Global Evolution (PRODIGE) large program with the Northern Extended Millimetre Array (NOEMA) at 1 mm. The 13 C isotopologue of CH 3 OH was detected towards seven sources of the sample, those of CH 3 CN were detected towards six sources. The emission spectra were analysed by deriving synthetic spectra and population diagrams assuming conditions of local thermodynamic equilibrium. Results . The emission of CH 3 OH and CH 3 CN is spatially unresolved in the PRODIGE data with a resolution of ~1″(~300 au) for the seven targeted systems. Rotational temperatures derived from both COMs exceed 100 K, telling us that they trace the gas of the hot corino, where CH 3 CN probes hotter regions than CH 3 OH on average (290 K versus 180 K). The column density ratios between the 12 C and 13 C isotopologues range from 4 to 30, which is lower by factors of a few up to an order of magnitude than the expected isotope ratio of the local interstellar medium of ~68. We conducted astrochemical models to understand the origins of the observed low ratios. We studied potential precursor molecules of CH 3 OH and CH 3 CN since the model does not include COMs, assuming that the ratio is transferred in reactions from the precursors to the COMs. The model predicts 12 C/ 13 C ratios close to the ISM value for CO and H 2 CO, precursors of CH 3 OH, in contrast to our observational results. For the potential precursors of CH 3 CN (CN, HCN, and HNC), the model predicts low 12 C/ 13 C ratios close to the protostar (<300 au). Hence, they may also be expected for CH 3 CN. Conclusions . Our results show that an enrichment in 13 C in COMs at the earliest protostellar stages is likely inherited from the precursor species of the COMs, whose 12 C/ 13 C ratios are set during the prestellar stage via isotopic exchange reactions. This also implies that low 12 C/ 13 C ratios observed at later evolutionary stages such as protoplanetary disks and exoplanetary atmospheres could at least partially be inherited. A definitive conclusion on 12 C/ 13 C ratios in protostellar environments requires observations at higher angular and spectral resolution that simultaneously cover a broad bandwidth, to tackle current observational limitations, and additional modelling efforts.
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Metadata
- Type
- article
- Language
- en
- Landing Page
- https://doi.org/10.1051/0004-6361/202554104
- OA Status
- hybrid
- Cited By
- 3
- References
- 89
- Related Works
- 10
- OpenAlex ID
- https://openalex.org/W4411338079
All OpenAlex metadata
Raw OpenAlex JSON
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https://openalex.org/W4411338079Canonical identifier for this work in OpenAlex
- DOI
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https://doi.org/10.1051/0004-6361/202554104Digital Object Identifier
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PRODIGE – envelope to disk with NOEMAWork title
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articleOpenAlex work type
- Language
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enPrimary language
- Publication year
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2025Year of publication
- Publication date
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2025-06-16Full publication date if available
- Authors
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L. A. Busch, J. E. Pineda, O. Sipilä, Dominique Segura-Cox, P. Caselli, María José Maureira, C. Gieser, Timothy H. Hsieh, M. T. Valdivia-Mena, L. Bouscasse, Th. Henning, D. Semenov, A. Fuente, M. Tafalla, J.J. Miranzo-Pastor, L. Colzi, Y.-R. Chou, S. GuilloteauList of authors in order
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https://doi.org/10.1051/0004-6361/202554104Publisher landing page
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YesWhether a free full text is available
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hybridOpen access status per OpenAlex
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https://doi.org/10.1051/0004-6361/202554104Direct OA link when available
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Physics, Astrophysics, Envelope (radar), Astronomy, Radar, Computer science, TelecommunicationsTop concepts (fields/topics) attached by OpenAlex
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3Total citation count in OpenAlex
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2025: 3Per-year citation counts (last 5 years)
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10Other works algorithmically related by OpenAlex
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| abstract_inverted_index.CO | 360 |
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| abstract_inverted_index.30, | 272 |
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| abstract_inverted_index.ISM | 357 |
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| abstract_inverted_index.its | 50 |
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| abstract_inverted_index.our | 96, 373 |
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| abstract_inverted_index.HCN, | 385 |
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| abstract_inverted_index.also | 406, 458 |
| abstract_inverted_index.au). | 402 |
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| abstract_inverted_index.show | 417 |
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| abstract_inverted_index.they | 230, 404 |
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| abstract_inverted_index.COMs. | 345 |
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| abstract_inverted_index.close | 354, 397 |
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| abstract_inverted_index.cover | 507 |
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| abstract_inverted_index.local | 185, 294 |
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| abstract_inverted_index.ratios | 67, 107, 259, 353, 396, 446, 466, 493 |
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| abstract_inverted_index.tackle | 512 |
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| abstract_inverted_index.derived | 11, 220 |
| abstract_inverted_index.factors | 277 |
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| abstract_inverted_index.sample, | 159 |
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| abstract_inverted_index.species | 437 |
| abstract_inverted_index.spectra | 172, 178 |
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| abstract_inverted_index.efforts. | 519 |
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| abstract_inverted_index.exchange | 455 |
| abstract_inverted_index.expected | 289, 408 |
| abstract_inverted_index.isotopic | 454 |
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| abstract_inverted_index.conducted | 300 |
| abstract_inverted_index.evolution | 51, 100 |
| abstract_inverted_index.exoplanet | 25 |
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| abstract_inverted_index.PROtostars | 126 |
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| abstract_inverted_index.definitive | 486 |
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| abstract_inverted_index.protoplanetary | 22, 474 |
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