FAUST

Context. During the early stages of star formation, accretion processes such as infall from the envelope and molecular streamers and ejection of matter through winds and jets take place simultaneously and distribute the angular momentum of the parent molecular cloud. The Class 0/I binary [BHB2007] 11 shows evidence for accretion and ejection at the scales of the circumbinary disk and the inner close binary. Recent observations of H 2 CO, however, have shown two elongated structures with indications of outflowing motion almost perpendicular to the main CO outflow, which is launched from the circumbinary disk. Aims. We study the kinematics of the molecular gas at intermediate scales of ~50–3000 au around [BHB2007] 11 to verify the nature of these elongated structures. Methods. We analyzed the line emission of H 13 CO + , CCH, c-C 3 H 2 , and SiO observed with the Atacama Large Millimeter/submillimeter Array (ALMA) within the large program called Fifty AU STudy of the chemistry in the disc/envelope system of Solar-like protostars (FAUST). These molecules trace the material that moves at velocities close to that of the ambient cloud, which could not be probed in previous observations of the self-absorbed emission of CO. Results. The images of H 13 CO + , CCH, and c-C 3 H 2 show clear elongated structures similar to those previously detected in H 2 CO, whose gas kinematics are consistent with outflowing motions and with rotation in the opposite sense to the main CO outflow. The derived mass-loss rate from these large-scale structures is (1.7 ± 0.5) × 10 −6 M ⊙ yr −1 , which agrees with the rates measured in outflows driven by Class 0/I protostars. The SiO image reveals compact emission close to the binary system, with a slight elongation that is aligned with the larger-scale structures. This suggests that SiO is released from the sputtering of dust grains in the shocked material at the base of the potential new outflow, with a relative abundance of ≥(0.11–2.0) × 10 −9 . However, higher angular and spectral resolution observations are needed to accurately estimate the outflow-launching radius and its powering source. Based on the location and the abundance of the SiO emission, we propose that the second outflow may be launched from inside the circumbinary disk, likely by the less massive companion that actively accretes material from its surroundings.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-06-16
DOI
https://doi.org/10.1051/0004-6361/202554755
Citations
2
Primary Topic
Radioactive element chemistry and processing
Type
article
Field-Weighted Citation Impact
1.07

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article

FAUST

G. Moellenbrock, Dominique Segura-Cox, Lucy Evans, Mathilde Bouvier et al.
2 citations
Astronomy and Astrophysics
Radioactive element chemistry and processing
1.07
article

FAUST

G. Moellenbrock, Dominique Segura-Cox, Lucy Evans, Mathilde Bouvier, J. E. Pineda, Laurent Loinard, F. Fontani, C. Codella, L. Podio, Takeshi Sakai, G. Sabatini, F. O. Alves, Brian Svoboda, Satoshi Ohashi, Doug Johnstone, Nicolás Cuello, María José Maureira, Nami Sakai, C. J. Chandler, S. Yamamoto, Tomoyuki Hanawa, Antonio Martínez-Henares, C. Vastel, M. De Simone, I. Jiménez-Serra, E. Bianchi, Yuri Aikawa, P. Caselli, C. Ceccarelli
article en
2 citations

Abstract

Context. During the early stages of star formation, accretion processes such as infall from the envelope and molecular streamers and ejection of matter through winds and jets take place simultaneously and distribute the angular momentum of the parent molecular cloud. The Class 0/I binary [BHB2007] 11 shows evidence for accretion and ejection at the scales of the circumbinary disk and the inner close binary. Recent observations of H 2 CO, however, have shown two elongated structures with indications of outflowing motion almost perpendicular to the main CO outflow, which is launched from the circumbinary disk. Aims. We study the kinematics of the molecular gas at intermediate scales of ~50–3000 au around [BHB2007] 11 to verify the nature of these elongated structures. Methods. We analyzed the line emission of H 13 CO + , CCH, c-C 3 H 2 , and SiO observed with the Atacama Large Millimeter/submillimeter Array (ALMA) within the large program called Fifty AU STudy of the chemistry in the disc/envelope system of Solar-like protostars (FAUST). These molecules trace the material that moves at velocities close to that of the ambient cloud, which could not be probed in previous observations of the self-absorbed emission of CO. Results. The images of H 13 CO + , CCH, and c-C 3 H 2 show clear elongated structures similar to those previously detected in H 2 CO, whose gas kinematics are consistent with outflowing motions and with rotation in the opposite sense to the main CO outflow. The derived mass-loss rate from these large-scale structures is (1.7 ± 0.5) × 10 −6 M ⊙ yr −1 , which agrees with the rates measured in outflows driven by Class 0/I protostars. The SiO image reveals compact emission close to the binary system, with a slight elongation that is aligned with the larger-scale structures. This suggests that SiO is released from the sputtering of dust grains in the shocked material at the base of the potential new outflow, with a relative abundance of ≥(0.11–2.0) × 10 −9 . However, higher angular and spectral resolution observations are needed to accurately estimate the outflow-launching radius and its powering source. Based on the location and the abundance of the SiO emission, we propose that the second outflow may be launched from inside the circumbinary disk, likely by the less massive companion that actively accretes material from its surroundings.

Astronomy and AstrophysicsVol. 699
Leiden University (NL), Herzberg Institute of Astrophysics (CA), Centre National de la Recherche Scientifique (FR), University of Leeds (GB), Woodwell Climate Research Center (US), European Southern Observatory (DE), Université Toulouse III - Paul Sabatier (FR), Harvard University (US), Chiba University (JP), Université Fédérale de Toulouse Midi-Pyrénées (FR), The Graduate University for Advanced Studies, SOKENDAI (JP), University of Electro-Communications (JP), University of Victoria (CA), National Radio Astronomy Observatory (US), Arcetri Astrophysical Observatory (IT), Max Planck Institute for Extraterrestrial Physics (DE), Pioneer (Japan) (JP), RIKEN (JP), Centro de Astrobiología (ES), Ausonius Institut de Recherche sur l'Antiquité et le Moyen age (FR), National Astronomical Observatory of Japan (JP), Universidad Autónoma de Madrid (ES), The University of Tokyo (JP), Universidad Nacional Autónoma de México (MX), Université Grenoble Alpes (FR)
Ministerio de Ciencia e Innovación
Openalex Percentile: Top 23%
Radioactive element chemistry and processing
1.07
DOIOpen Access PDFOpenAlex
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