Improving Planet Detection with Disk Modeling: Keck/NIRC2 Imaging of the HD 34282 Single-armed Protoplanetary Disk. (arXiv:2111.12708v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Quiroz_J/0/1/0/all/0/1">Juan Quiroz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wallack_N/0/1/0/all/0/1">Nicole L. Wallack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ren_B/0/1/0/all/0/1">Bin Ren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_R/0/1/0/all/0/1">Ruobing Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xuan_J/0/1/0/all/0/1">Jerry W. Xuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mawet_D/0/1/0/all/0/1">Dimitri Mawet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Millar_Blanchaer_M/0/1/0/all/0/1">Maxwell A. Millar-Blanchaer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruane_G/0/1/0/all/0/1">Garreth Ruane</a>

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
non-detection of companions for HD 34282, this direct disk modeling improves
planet detection sensitivity by up to a factor of 2 in flux ratio and ${sim}10
M_{rm Jupiter}$ 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.

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
non-detection of companions for HD 34282, this direct disk modeling improves
planet detection sensitivity by up to a factor of 2 in flux ratio and ${sim}10
M_{rm Jupiter}$ 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.

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