S22A0041
S22A0041
Planets form in protoplanetary disks, and the late stage of gas giant planet formation is controlled by the gas supplied from the 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 a pilot program of Keck/OSIRIS integral-field-spectrograph observations at Paβ (1.282 µm) to identify and characterize an accreting planet candidate around SR 21. SR 21 shows a kinked structure in spiral potentially induced by disk–planet interaction, and thus, our searches for planets are more targeted and efficient than blind searches of planets. If successful, we will expand our Keck/OSIRIS imaging survey to other disk systems with kinks to increase the size of the young planet sample, which provides a more complete picture of accreting planets, e.g., whether or not accreting properties of PDS 70 planets are common. Conversely, a non-detection would constrain a ratio of mass accretion rates of an accreting planet and the central star.
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