FAUST-XXIX. OCS line emission
The luminosity of embedded protostars is commonly measured via observations of the dust continuum spectral energy distribution from millimetre to infrared wavelengths. However, this method cannot be applied to embedded protostars in binary or multiple systems, where their components are usually unre...
| Autores: | , , , , , , , , , , , , , , , , , , , , , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2026 |
| País: | España |
| Institución: | Universitat Autònoma de Barcelona |
| Repositorio: | Dipòsit Digital de Documents de la UAB |
| Idioma: | inglés |
| OAI Identifier: | oai:ddd.uab.cat:326509 |
| Acceso en línea: | https://ddd.uab.cat/record/326509 https://dx.doi.org/urn:doi:10.1093/mnras/staf2157 |
| Access Level: | acceso abierto |
| Palabra clave: | Astrochemistry Stars: formation ISM: molecules ISM: individual Objects: NGC1333 IRAS4A |
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FAUST-XXIX. OCS line emissiona new method for measuring the luminosity of embedded protostars in binary systemsSaury, GuillaumeBariosco, Vittorio|||0009-0000-7269-8418Ceccarelli, Cecilia|||0000-0001-9664-6292López-Sepulcre, AnaChahine, Layal|||0000-0003-3364-5094De Simone, MartaRimola, Albert|||0000-0002-9637-4554Ugliengo, Piero|||0000-0001-8886-9832Chandler, Claire J.Sakai, NamiCodella, Claudio|||0000-0003-1514-3074Bianchi, Eleonora|||0000-0001-9249-7082Boitard-Crépeau, LiseBouvier, MathildeLe Gal, RomaneLoinard, Laurent|||0000-0002-5635-3345Oya, Yoko|||0000-0002-0197-8751Podio, Linda|||0000-0003-2733-5372Sabatini, Giovanni|||0000-0002-6428-9806Vastel, CharlotteZhang, Ziwei E.Yamamoto, SatoshiAstrochemistryStars: formationISM: moleculesISM: individualObjects: NGC1333 IRAS4AThe luminosity of embedded protostars is commonly measured via observations of the dust continuum spectral energy distribution from millimetre to infrared wavelengths. However, this method cannot be applied to embedded protostars in binary or multiple systems, where their components are usually unresolved over this extended wavelength range. We propose a new method, based on the idea that a molecule formed (mainly) on the grain surfaces only emits lines in the region where it thermally sublimates from the grain mantles, heated by the photons emitted by the embedded source. In this respect, carbonyl sulfide (OCS) is an optimal molecule, because of its low binding energy and rotational lines in the millimetre. We apply the method to the protobinary system NGC1333 IRAS4A, using ALMA high-spatial resolution ( ∼50 au) observations of the OCS(19-18) line as part of the ALMA Large Programme FAUST. We also present new quantum mechanics calculations of the OCS binding energy distribution, essential for the application of the method. We found that the two binary components, A1 and A2, have a comparable luminosity within the error bars, 7.5 ± 2.5 and 7 ± 1 L , respectively. We discuss the reliability of the estimated luminosities and the potential of this new method for measuring the luminosity of embedded protostars in binary and multiple systems. 22026-01-0120262026-01-01Articlehttp://purl.org/coar/resource_type/c_6501VoRhttp://purl.org/coar/version/c_970fb48d4fbd8a85info:eu-repo/semantics/articleapplication/pdfhttps://ddd.uab.cat/record/326509https://dx.doi.org/urn:doi:10.1093/mnras/staf2157reponame:Dipòsit Digital de Documents de la UABinstname:Universitat Autònoma de BarcelonaInglésengEuropean Commission https://doi.org/10.13039/501100000780 741002European Commission https://doi.org/10.13039/501100000780 811312European Commission https://doi.org/10.13039/501100000780 833460open accesshttp://purl.org/coar/access_right/c_abf2Aquest document està subjecte a una llicència d'ús Creative Commons. Es permet la reproducció total o parcial, la distribució, la comunicació pública de l'obra i la creació d'obres derivades, fins i tot amb finalitats comercials, sempre i quan es reconegui l'autoria de l'obra original.https://creativecommons.org/licenses/by/4.0/info:eu-repo/semantics/openAccessoai:ddd.uab.cat:3265092026-06-06T12:50:31Z |
| dc.title.none.fl_str_mv |
FAUST-XXIX. OCS line emission a new method for measuring the luminosity of embedded protostars in binary systems |
| title |
FAUST-XXIX. OCS line emission |
| spellingShingle |
FAUST-XXIX. OCS line emission Saury, Guillaume Astrochemistry Stars: formation ISM: molecules ISM: individual Objects: NGC1333 IRAS4A |
| title_short |
FAUST-XXIX. OCS line emission |
| title_full |
FAUST-XXIX. OCS line emission |
| title_fullStr |
FAUST-XXIX. OCS line emission |
| title_full_unstemmed |
FAUST-XXIX. OCS line emission |
| title_sort |
FAUST-XXIX. OCS line emission |
| dc.creator.none.fl_str_mv |
Saury, Guillaume Bariosco, Vittorio|||0009-0000-7269-8418 Ceccarelli, Cecilia|||0000-0001-9664-6292 López-Sepulcre, Ana Chahine, Layal|||0000-0003-3364-5094 De Simone, Marta Rimola, Albert|||0000-0002-9637-4554 Ugliengo, Piero|||0000-0001-8886-9832 Chandler, Claire J. Sakai, Nami Codella, Claudio|||0000-0003-1514-3074 Bianchi, Eleonora|||0000-0001-9249-7082 Boitard-Crépeau, Lise Bouvier, Mathilde Le Gal, Romane Loinard, Laurent|||0000-0002-5635-3345 Oya, Yoko|||0000-0002-0197-8751 Podio, Linda|||0000-0003-2733-5372 Sabatini, Giovanni|||0000-0002-6428-9806 Vastel, Charlotte Zhang, Ziwei E. Yamamoto, Satoshi |
| author |
Saury, Guillaume |
| author_facet |
Saury, Guillaume Bariosco, Vittorio|||0009-0000-7269-8418 Ceccarelli, Cecilia|||0000-0001-9664-6292 López-Sepulcre, Ana Chahine, Layal|||0000-0003-3364-5094 De Simone, Marta Rimola, Albert|||0000-0002-9637-4554 Ugliengo, Piero|||0000-0001-8886-9832 Chandler, Claire J. Sakai, Nami Codella, Claudio|||0000-0003-1514-3074 Bianchi, Eleonora|||0000-0001-9249-7082 Boitard-Crépeau, Lise Bouvier, Mathilde Le Gal, Romane Loinard, Laurent|||0000-0002-5635-3345 Oya, Yoko|||0000-0002-0197-8751 Podio, Linda|||0000-0003-2733-5372 Sabatini, Giovanni|||0000-0002-6428-9806 Vastel, Charlotte Zhang, Ziwei E. Yamamoto, Satoshi |
| author_role |
author |
| author2 |
Bariosco, Vittorio|||0009-0000-7269-8418 Ceccarelli, Cecilia|||0000-0001-9664-6292 López-Sepulcre, Ana Chahine, Layal|||0000-0003-3364-5094 De Simone, Marta Rimola, Albert|||0000-0002-9637-4554 Ugliengo, Piero|||0000-0001-8886-9832 Chandler, Claire J. Sakai, Nami Codella, Claudio|||0000-0003-1514-3074 Bianchi, Eleonora|||0000-0001-9249-7082 Boitard-Crépeau, Lise Bouvier, Mathilde Le Gal, Romane Loinard, Laurent|||0000-0002-5635-3345 Oya, Yoko|||0000-0002-0197-8751 Podio, Linda|||0000-0003-2733-5372 Sabatini, Giovanni|||0000-0002-6428-9806 Vastel, Charlotte Zhang, Ziwei E. Yamamoto, Satoshi |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
Astrochemistry Stars: formation ISM: molecules ISM: individual Objects: NGC1333 IRAS4A |
| topic |
Astrochemistry Stars: formation ISM: molecules ISM: individual Objects: NGC1333 IRAS4A |
| description |
The luminosity of embedded protostars is commonly measured via observations of the dust continuum spectral energy distribution from millimetre to infrared wavelengths. However, this method cannot be applied to embedded protostars in binary or multiple systems, where their components are usually unresolved over this extended wavelength range. We propose a new method, based on the idea that a molecule formed (mainly) on the grain surfaces only emits lines in the region where it thermally sublimates from the grain mantles, heated by the photons emitted by the embedded source. In this respect, carbonyl sulfide (OCS) is an optimal molecule, because of its low binding energy and rotational lines in the millimetre. We apply the method to the protobinary system NGC1333 IRAS4A, using ALMA high-spatial resolution ( ∼50 au) observations of the OCS(19-18) line as part of the ALMA Large Programme FAUST. We also present new quantum mechanics calculations of the OCS binding energy distribution, essential for the application of the method. We found that the two binary components, A1 and A2, have a comparable luminosity within the error bars, 7.5 ± 2.5 and 7 ± 1 L , respectively. We discuss the reliability of the estimated luminosities and the potential of this new method for measuring the luminosity of embedded protostars in binary and multiple systems. |
| publishDate |
2026 |
| dc.date.none.fl_str_mv |
2 2026-01-01 2026 2026-01-01 |
| dc.type.none.fl_str_mv |
Article http://purl.org/coar/resource_type/c_6501 VoR http://purl.org/coar/version/c_970fb48d4fbd8a85 |
| dc.type.openaire.fl_str_mv |
info:eu-repo/semantics/article |
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article |
| dc.identifier.none.fl_str_mv |
https://ddd.uab.cat/record/326509 https://dx.doi.org/urn:doi:10.1093/mnras/staf2157 |
| url |
https://ddd.uab.cat/record/326509 https://dx.doi.org/urn:doi:10.1093/mnras/staf2157 |
| dc.language.none.fl_str_mv |
Inglés eng |
| language_invalid_str_mv |
Inglés |
| language |
eng |
| dc.relation.none.fl_str_mv |
European Commission https://doi.org/10.13039/501100000780 741002 European Commission https://doi.org/10.13039/501100000780 811312 European Commission https://doi.org/10.13039/501100000780 833460 |
| dc.rights.none.fl_str_mv |
open access http://purl.org/coar/access_right/c_abf2 https://creativecommons.org/licenses/by/4.0/ |
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info:eu-repo/semantics/openAccess |
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open access http://purl.org/coar/access_right/c_abf2 https://creativecommons.org/licenses/by/4.0/ |
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openAccess |
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application/pdf |
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