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...

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Detalles Bibliográficos
Autores: 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
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
Descripción
Sumario: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.

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