Abstract
Abstract Formed in protoplanetary disks around young stars, giant planets can leave observational features such as spirals and gaps in their natal disks through planet–disk interactions. Although such features can indicate the existence of giant planets, protoplanetary disk signals can overwhelm the innate luminosity of planets. Therefore, in order to image planets that are embedded in disks, it is necessary to remove the contamination from the disks to reveal the planets possibly hiding within their natal environments. We observe and directly model the detected disk in the Keck/NIRC2 vortex coronagraph L′-band observations of the single-armed protoplanetary disk around HD 34282. Despite a nondetection of companions for HD 34282, this direct disk modeling improves planet detection sensitivity by up to a factor of 2 in flux ratio and ∼10 M Jupiter in mass. This suggests that performing disk modeling can improve directly imaged planet detection limits in systems with visible scattered light disks, and can help to better constrain the occurrence rates of self-luminous planets in these systems.
Highlights
The most recent generation high-contrast imaging surveys that utilize extreme adaptive optics systems have obtained an occurrence rate of 10% for young self-luminous giant planets (i.e., Nielsen et al 2019; Vigan et al 2021)
Formed in protoplanetary disks around young stars, giant planets can leave observational features such as spirals and gaps in their natal disks through planet-disk interactions. Such features can indicate the existence of giant planets, protoplanetary disk signals can overwhelm the innate luminosity of planets
Motivated by the recovery of the PDS 70c planet via disk modeling in Wang et al (2020), we investigate the affect of disk modeling in planet detection using HD 34282
Summary
The most recent generation high-contrast imaging surveys that utilize extreme adaptive optics systems have obtained an occurrence rate of 10% for young self-luminous giant planets (i.e., Nielsen et al 2019; Vigan et al 2021) Despite their low direct occurrence rates using contemporary instruments, giant planets can gravitationally interact with their surrounding gaseous protoplanetary disks and leave their mark as observational signatures in the disk structure (e.g., spirals, gaps: Dong et al 2015b,c; Bae et al 2018). In J-band polarized light observations using VLT/SPHERE, de Boer et al (2021) identified two rings with a ∼56◦ inclination and a ∼119◦ position angle, and a possible tightly-wound single-arm spiral which resembles the pattern driven by a sub-Jupiter to Jupiter mass planet (e.g., Dong et al 2015c; Dong & Fung 2017).
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