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dc.contributor.authorFuente, A.-
dc.contributor.authorGerin, M.-
dc.contributor.authorPety, J.-
dc.contributor.authorCommerçon, B.-
dc.contributor.authorAgúndez, Marcelino-
dc.contributor.authorCernicharo, José-
dc.contributor.authorMarcelino, Nuria-
dc.contributor.authorRoueff, E.-
dc.contributor.authorLis, D.C.-
dc.contributor.authorWootten, H. A.-
dc.date.accessioned2019-08-12T10:54:03Z-
dc.date.available2019-08-12T10:54:03Z-
dc.date.issued2017-10-
dc.identifier.citationAstronomy and Astrophysics 606: L3 (2017)-
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10261/188048-
dc.description.abstractThe extremely young Class 0 object B1b-S and the first hydrostatic core (FSHC) candidate, B1b-N, provide a unique opportunity to study the chemical changes produced in the elusive transition from the prestellar core to the protostellar phase. We present 40″ × 70″ images of Barnard 1b in the CO 1 → 0, CO 1 → 0, NHD 1a→ 1s, and SO 3→ 2 lines obtained with the NOEMA interferometer. The observed chemical segregation allows us to unveil the physical structure of this young protostellar system down to scales of ~500 au. The two protostellar objects are embedded in an elongated condensation, with a velocity gradient of ~0.2-0.4 m s au in the east-west direction, reminiscent of an axial collapse. The NHD data reveal cold and dense pseudo-disks (R ~ 500-1000 au) around each protostar. Moreover, we observe evidence of pseudo-disk rotation around B1b-S. We do not see any signature of the bipolar outflows associated with B1b-N and B1b-S, which were previously detected in HCO and CHOH, in any of the imaged species. The non-detection of SO constrains the SO/CHOH abundance ratio in the high-velocity gas.-
dc.description.sponsorshipWe thank the Spanish MINECO for funding support from grants CSD2009-00038, AYA2012-32032, AYA2016-75066-C2-1/2-P, and ERC under ERC-2013-SyG, G. A. 610256 NANOCOSMOS. E.R. and M.G. thank the INSU/CNRS program PCMI for funding.-
dc.publisherEDP Sciences-
dc.relationinfo:eu-repo/grantAgreement/EC/FP7/610256-
dc.relationMINECO/ICTI2013-2016/AYA2016-75066-C2-2-P-
dc.rightsclosedAccess-
dc.subjectISM: clouds-
dc.subjectStars: formation-
dc.subjectStars: low-mass-
dc.subjectISM: kinematics and dynamics-
dc.subjectAstrochemistry-
dc.subjectISM: individual objects: Barnard 1b-
dc.titleChemical segregation in the young protostars Barnard 1b-N and S: evidence of pseudo-disk rotation in Barnard-
dc.typeartículo-
dc.identifier.doi10.1051/0004-6361/201730963-
dc.relation.publisherversionhttps://doi.org/10.1051/0004-6361/201730963-
dc.identifier.e-issn1432-0746-
dc.date.updated2019-08-12T10:54:03Z-
dc.language.rfc3066eng-
dc.contributor.funderEuropean Research Council-
dc.contributor.funderCentre National de la Recherche Scientifique (France)-
dc.contributor.funderInstitut national des sciences de l'Univers (France)-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.relation.csic-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004617es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004794es_ES
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