S22B0006
S22B0006
The late stage of gas giant planet formation is controlled by the gas supplied from the protoplanetary disk. Since robust detections of accreting planets have been limited to PDS 70b and c to date, it remains still unclear how proto-giant planets receive mass from surroundings in detail. Thus, direct imaging of more young planets forming in protoplanetary disks is necessary to understand gas giant planet formation. Here we propose Keck/OSIRIS integral-field-spectrograph observations at Paβ (1.282 µm) to characterize an accreting planet AB Aur b newly discovered by Subaru/SCExAO. Our purpose is to derive accretion properties of AB Aur b, especially for the filling factor ff. In our previous studies of PDS 70b&c, as the filling factor is small (i.e., ff <<1), PDS 70b&c’s planetary accretion process can be still described with the framework of stellar accretion processes. If we find AB Aur b with ff ∼1, this planet will support a new paradigm of the accreting process of meridional flows from the circumstellar disk. Therefore, our observations would expand our understanding of planet formation.
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