The ALMA-PILS survey: Gas dynamics in IRAS 16293$-$2422 and the connection between its two protostars
dc.contributor.author | VAN DER WIEL, M. H. D. | |
dc.contributor.author | JACOBSEN, S. K. | |
dc.contributor.author | JØRGENSEN, J. K. | |
dc.contributor.author | BOURKE, T. L. | |
dc.contributor.author | KRISTENSEN, L. E. | |
dc.contributor.author | BJERKELI, P. | |
dc.contributor.author | MURILLO, N. M. | |
dc.contributor.author | CALCUTT, H. | |
dc.contributor.author | MÜLLER, H. S. P. | |
hal.structure.identifier | AMOR 2019 | |
dc.contributor.author | COUTENS, Audrey | |
dc.contributor.author | DROZDOVSKAYA, M. N. | |
dc.contributor.author | FAVRE, C. | |
dc.contributor.author | WAMPFLER, S. F. | |
dc.date.issued | 2019 | |
dc.identifier.issn | 0004-6361 | |
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.iso | en | |
dc.publisher | EDP Sciences | |
dc.subject.en | Astrophysics - Astrophysics of Galaxies | |
dc.title.en | The ALMA-PILS survey: Gas dynamics in IRAS 16293$-$2422 and the connection between its two protostars | |
dc.type | Article de revue | |
dc.identifier.doi | 10.1051/0004-6361/201833695 | |
dc.subject.hal | Planète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO] | |
dc.identifier.arxiv | 1903.12606 | |
bordeaux.journal | Astronomy and Astrophysics - A&A | |
bordeaux.page | id.A93 | |
bordeaux.volume | 626 | |
bordeaux.peerReviewed | oui | |
hal.identifier | hal-02087465 | |
hal.version | 1 | |
hal.popular | non | |
hal.audience | Internationale | |
hal.origin.link | https://hal.archives-ouvertes.fr//hal-02087465v1 | |
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