The ALMA-PILS survey: gas dynamics in IRAS 16293-2422 and the connection between its two protostars
Journal article, 2019

Context. The majority of stars form in binary or higher order systems. The evolution of each protostar in a multiple system may start at different times and may progress differently. The Class 0 protostellar system IRAS 16293-2422 contains two protostars, "A" and "B", separated by similar to 600 au and embedded in a single, 10(4) au scale envelope. Their relative evolutionary stages have been debated. Aims. We aim to study the relation and interplay between the two protostars A and B at spatial scales of 60 au up to similar to 10(3) au. Methods. We selected molecular gas line transitions of the species CO, H2CO, HCN, CS, SiO, and C2H from the ALMA-PILS spectral imaging survey (329-363 GHz) and used them as tracers of kinematics, density, and temperature in the IRAS 16293-2422 system. The angular resolution of the PILS data set allows us to study these quantities at a resolution of 0.5 '' (60 au at the distance of the source). Results. 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 x 10(4) cm(-3) and similar to 3 x 10(7) cm(-3); and (iii) a separate, straight filament seemingly connected to protostar B seen only in C2H, 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. Conclusions. 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.

ISM: jets and outflows

circumstellar matter

stars: formation

ISM: individual objects: IRAS 16293-2422

Author

M. H. D. van der Wiel

University of Copenhagen

Netherlands Institute for Radio Astronomy (ASTRON)

S. K. Jacobsen

University of Copenhagen

J. K. Jorgensen

University of Copenhagen

T. L. Bourke

Jodrell Bank Observatory

L. E. Kristensen

University of Copenhagen

Per Bjerkeli

University of Copenhagen

Chalmers, Space, Earth and Environment, Astronomy and Plasmaphysics, Galactic Astrophysics

N. M. Murillo

Leiden University

Hannah Calcutt

University of Copenhagen

H. S. P. Mueller

University of Cologne

A. Coutens

University of Bordeaux

M. N. Drozdovskaya

University of Bern

C. Favre

Arcetri Astrophysical Observatory

S. F. Wampfler

University of Bern

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 626 A93

Protostellar Interferometric Line Survey (PILS)

European Research Council (ERC), 2019-10-30 -- .

Subject Categories

Astronomy, Astrophysics and Cosmology

Atom and Molecular Physics and Optics

Other Physics Topics

Infrastructure

Onsala Space Observatory

DOI

10.1051/0004-6361/201833695

More information

Latest update

12/16/2019