FAUST

Year: 2025

Type: article

Abstract: Context. While protostellar outflows are important in terms of mass accretion and angular momentum transport in star formation processes, high-resolution observations of outflows in protobinary systems are still sparse. Aims. We aim to reveal outflow structures traced by millimeter SiO emission in a low-mass protobinary system, L483. Methods. We observed the SiO (J = 5−4) line in L483 with the Atacama Large Millimeter/submillimeter Array (ALMA) as part of the large program FAUST (Fifty AU STudy of the chemistry in the disk/envelope systems of Solar-like protostars). The spatial and spectral resolutions were 0.39′′×0.30′′ (780 au×60 au) and 122 kHz (0.17 km s−1 at 217 GHz), respectively. The spectral lines of SO, CS, and C18O were also used to study the physical and dynamical properties of the SiO emitting regions. Results. Two SiO emission peaks are identified in the central part of L483, which have offsets of 100 au and 200 au toward the northeast (SiO-peak) and north (SiO-N), respectively, from the continuum peak. The SiO-peak shows only blueshifted emission with a broad linewidth of 5 km s−1, while that of SiO-N corresponds to the systemic velocity. Furthermore, weak and compact SiO emission components are distributed up to 2400 au away from the continuum position. They have narrow linewidths of ∼1 km s−1. One of these components is a blueshifted isolated emission feature, 2400 au northeast of the continuum peak, NE-cloud, located outside the east-west outflow lobes. The SiO abundances relative to H2 are 10−10−10−9 and 10−10 in the central part and more widely distributed components, respectively. These are intermediate values between those of strongly shocked regions caused by high-velocity outflows and quiescent molecular clouds. Conclusions. The central SiO emission could be interpreted as either two different outflows driven by both protostars or as an outflow ejected from one of the circumstellar disks in the binary system. The NE-cloud region is most likely explained as a remnant of an old shock produced by past outflow activity, as has been proposed for the low-mass protostar IRAS 15398–3359. The complex structures of the outflows traced by the SiO line could reflect dynamical processes of the newly formed protobinary system in L483.

Source: Astronomy and Astrophysics

DOI: 10.1051/0004-6361/202453386

Institutions: The Graduate University for Advanced Studies, SOKENDAI, National Astronomical Observatory of Japan, Centre National de la Recherche Scientifique, Université de Bordeaux, Laboratoire d'Astrophysique de Bordeaux, Kyoto University, Yukawa Institute for Theoretical Physics, Leiden University, Leiden Observatory, Institut de Radioastronomie Millimétrique, Institut de Planétologie et d'Astrophysique de Grenoble, Université Grenoble Alpes, European Southern Observatory, Université Toulouse III - Paul Sabatier, Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, National Radio Astronomy Observatory, Arcetri Astrophysical Observatory, National Institute for Astrophysics, RIKEN, The University of Tokyo, University of Perugia, Max Planck Institute for Extraterrestrial Physics, Université Paris Sciences et Lettres, Observatoire de Paris, Sorbonne Université, Laboratoire d’Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères, CY Cergy Paris Université, University of Leeds, Xiamen University, Chiba University, University of Virginia, Rice University, Herzberg Institute of Astrophysics, University of Victoria, National Taiwan Normal University, National Sun Yat-sen University, Harvard University, Universidad Nacional Autónoma de México, Hokkaido University, Universitat Autònoma de Barcelona, University of Electro-Communications, The University of Texas at Austin, University of Arizona, University of Bologna, Shibaura Institute of Technology, Shanghai Jiao Tong University

Language: English

Topic: Astrophysics and Star Formation Studies

Subfield: Astronomy and Astrophysics

Field: Physics and Astronomy

Domain: Physical Sciences

Open Access status: gold

Estimated APC paid: $1,865

Funders: National Science Foundation, National Radio Astronomy Observatory, European Commission, Ministry of Education, Culture, Sports, Science and Technology, Consejo Nacional de Ciencia y Tecnología, Korea Astronomy and Space Science Institute, National Astronomical Observatory of Japan, National Science and Technology Council, Horizon 2020 Framework Programme, HORIZON EUROPE Framework Programme, Japan Society for the Promotion of Science, Dirección General de Asuntos del Personal Académico, Universidad Nacional Autónoma de México, National Institutes of Natural Sciences, European Regional Development Fund, Agencia Estatal de Investigación

Awards: G1088400374, 惑星系形成円盤における元素組成の分布と進化：系外惑星大気の起源に迫る, Chemical Composition of Disk Forming Regions of Solar-type Protostars and its Evolution to Planetary Systems, G1507096846, G1743472294, Observational Study of Protostellar Disk Formation with Machine Learnings and Physical Models -Development of Methodology and Its Application-, G2058985095, G2107196950, G220577813, G2262748287, On the possible formation of nucleic acids on the early Earth: Derivery of source materials from extraterrestrial environments, G2628364946, G265104915, G3055077951, G3480869486, G3681454997, G4042783231, G4048070418, G425668148, G4434283826, G451917667, G4937468798, From Protoplanetary Disks to the Solar System: Chemical Evolution of Organic Molecules, AstroChemical Origins, G5939753358, G5967599077, G6464617006, G6675271965, G6677884157, G683931746, 清浄なアモルファス鉱物表面を用いた実験による星間塵の化学吸着と触媒反応の解明, G7200771947, 古代説話における諸寺縁起の研究, G7689440551, G7881495189, G7898826618, G8616911079, G8782591868, G8870153366

OpenAlex ID: W4408883279