Constraining PDS 70b's Formation Mechanism with Multi-hydrogen-emission Observations

Creators: Uyama, Taichi; Hashimoto, Jun; Beichman, Charles A.; Ruffio, Jean-Baptiste; Aoyama, Yuhiko; McElwain, Michael W.; Dong, Ruobing

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Abstract

We present our Keck/OSIRIS observations of the Paβ emission line (1.282 μm) to investigate accretion mechanisms of PDS 70 planetary system. Our spectral differential imaging reduction to remove the stellar PSF resulted in null detection of Paβ at the locations of PDS 70b and c. The 5σ detection limit of Paβ compared with the theoretical model of Aoyama & Ikoma (2019) indicates the gas velocity onto PDS 70b is smaller than 70 km s⁻¹, which suggests MUSE-based Hα studies overestimated the gas velocity and the mass of PDS 70b.

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© 2021. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 January 11; Accepted 2021 January 12; Published 2021 January 13. We thank Jim Lyke for kindly helping to confirm the OSIRIS FoV settings. We wish to acknowledge the critical importance of the current and recent Maunakea Observatories daycrew, technicians, telescope operators, computer support, and office staff employees, especially during the challenging times presented by the COVID-19 pandemic. The authors also wish to acknowledge the significant cultural role and reverence that the summit of Maunakea has within the indigenous Hawaiian community.

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