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dc.contributor.authorVAN DER WIEL, M. H. D.
dc.contributor.authorJACOBSEN, S. K.
dc.contributor.authorJØRGENSEN, J. K.
dc.contributor.authorBOURKE, T. L.
dc.contributor.authorKRISTENSEN, L. E.
dc.contributor.authorBJERKELI, P.
dc.contributor.authorMURILLO, N. M.
dc.contributor.authorCALCUTT, H.
dc.contributor.authorMÜLLER, H. S. P.
hal.structure.identifierAMOR 2019
dc.contributor.authorCOUTENS, Audrey
dc.contributor.authorDROZDOVSKAYA, M. N.
dc.contributor.authorFAVRE, C.
dc.contributor.authorWAMPFLER, S. F.
dc.date.issued2019
dc.identifier.issn0004-6361
dc.description.abstractEn[Abridged] The majority of stars form in binary or higher order systems. The Class 0 protostellar system IRAS16293-2422 contains two protostars, 'A' and 'B', separated by ~600 au and embedded in a single, 10^4 au scale envelope. Their relative evolutionary stages have been debated. We aim to study the relation and interplay between the two protostars A and B at spatial scales of 60 to ~1000 au. We selected molecular gas line transitions of CO, H2CO, HCN, CS, SiO, and CCH from the ALMA-PILS spectral imaging survey (329-363 GHz) and used them as tracers of kinematics, density, and temperature in the IRAS16293-2422 system. The angular resolution of the PILS data set allows us to study these quantities at a resolution of 0.5 arcsec (60 au [..]). Line-of-sight velocity maps of both optically thick and optically thin molecular lines reveal: (i) new manifestations of previously known outflows emanating from protostar A; (ii) a kinematically quiescent bridge of dust and gas spanning between the two protostars, with an inferred density between 4 10^4 and 3 10^7 cm^-3; and (iii) a separate, straight filament seemingly connected to protostar B seen only in CCH, with a flat kinematic signature. Signs of various outflows, all emanating from source A, are evidence of high-density and warmer gas; none of them coincide spatially and kinematically with the bridge. We hypothesize that the bridge arc is a remnant of filamentary substructure in the protostellar envelope material from which protostellar sources A and B have formed. One particular morphological structure appears to be due to outflowing gas impacting the quiescent bridge material. The continuing lack of clear outflow signatures unambiguously associated to protostar B and the vertically extended shape derived for its disk-like structure lead us to conclude that source B may be in an earlier evolutionary stage than source A.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enThe ALMA-PILS survey: Gas dynamics in IRAS 16293$-$2422 and the connection between its two protostars
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201833695
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1903.12606
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A93
bordeaux.volume626
bordeaux.peerReviewedoui
hal.identifierhal-02087465
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02087465v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2019&rft.volume=626&rft.spage=id.A93&rft.epage=id.A93&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=VAN%20DER%20WIEL,%20M.%20H.%20D.&JACOBSEN,%20S.%20K.&J%C3%98RGENSEN,%20J.%20K.&BOURKE,%20T.%20L.&KRISTENSEN,%20L.%20E.&rft.genre=article


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