Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-24T02:23:25.161Z Has data issue: false hasContentIssue false

The water and methanol masers in the face-on accretion system around the high-mass protostar G353.273+0.641

Published online by Cambridge University Press:  07 February 2024

Kazuhito Motogi*
Affiliation:
1Graduate School of Sciences and Technology for Innovation, Yamaguchi University, Yamaguchi, Yamaguchi 753-8512, Japan.
Tomoya Hirota
Affiliation:
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Iwate 023-0861, Japan
Masahiro N. Machida
Affiliation:
Department of Earth and Planetary Sciences, Faculty of Sciences, Kyushu University, Fukuoka, Fukuoka 819-0395, Japan
Kei E. I. Tanaka
Affiliation:
Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Meguro, Tokyo, 152-8551, Japan
Yoshinori Yonekura
Affiliation:
Center for Astronomy, Ibaraki University, Mito, Ibaraki 310-8512, Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We report on a direct comparison of VLBI maser data and ALMA thermal-emission data for the high-mass protostar G353.273+0.641. We detected a gravitationally-unstable disk by dust and a high-velocity jet traced by a thermal CO line by ALMA long-baselines (LB). 6.7 GHz CH3OH masers trace infalling streamlines inside the disk. The innermost maser ring indicates another compact accretion disk of 30 au. Such a nested system could be caused by angular momentum transfer by the spiral arms. 22 GHz H2O masers trace the jet-accelerating region, which are directly connecting the CO jet and the protostar. The recurrent maser flares imply episodic jet ejections per 1–2 yr, while typical separation of CO knots indicates a variation of outflow rate per 100 yr. Our study demonstrates that VLBI maser observations are still a powerful tool to explore detailed structures nearby high-mass protostars by combining ALMA LB.

Type
Contributed Paper
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Burns, R. A., Uno, Y., Sakai, N., et al. 2023, Nature Astronomy, 7, 557 10.1038/s41550-023-01899-wCrossRefGoogle Scholar
Johnston, K. G., Hoare, M. G., Beuther, H., et al. 2020, A&A, 634, L11 10.1051/0004-6361/201937154CrossRefGoogle Scholar
Machida, M. N. & Basu, S. 2019, ApJ, 876, 149 10.3847/1538-4357/ab18a7CrossRefGoogle Scholar
Motogi, K., Sorai, K., Honma, M., et al. 2016, PASJ, 68, 69 10.1093/pasj/psu142CrossRefGoogle Scholar
Motogi, K., Hirota, T., Sorai, K., et al. 2017, ApJ, 849, 23 10.3847/1538-4357/aa8d75CrossRefGoogle Scholar
Motogi, K., Hirota, T., Machida, M. N., et al. 2019, ApJ(Letters), 877, L25 10.3847/2041-8213/ab212fCrossRefGoogle Scholar