Abstract
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.
Highlights
Ou r spectral differential imaging reduction to remove the stella r PSF resulted in null detection of Pa/3 at the locations of PDS 70b and c
The Sa detection li mit of Pa/3 compared with the theoretical model of Aoyama & lkoma (2019) indicates t he gas velocit y onto PDS70b is smaller than 70 km s- 1, which suggests MUSE-based Ha studies overestimated the gas velocity a nd the mass of PDS 70b
The masses estimated for PDS 70bc d iffe r as measured by different techniques: broad-band observations at near-infrared combined with atmospheric models (e.g., Allard e t at 2.Q12) suggest ;S 4 MJup (Stolker e t al. 2Q2Q; Wang et al .2.Q2Q) while VLT/ MUSE-Ha observations combined with a hydrogen-emissio n model (Aoyama & lkoma 2212) favor higher mass (- 10 M.1up: Hashimoto et al 2Q2Q)
Summary
Constraining PDS 70b's Fo rmation Mechanism wit h Mult ihydrogen-emissio n Observations.
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