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Improving Planet Detection with Disk Modeling: Keck/NIRC2 Imaging of the HD 34282 Single-armed Protoplanetary Disk

Quiroz, Juan and Wallack, Nicole L. and Ren, Bin and Dong, Ruobing and Xuan, Jerry W. and Mawet, Dimitri and Millar-Blanchaer, Maxwell A. and Ruane, Garreth (2022) Improving Planet Detection with Disk Modeling: Keck/NIRC2 Imaging of the HD 34282 Single-armed Protoplanetary Disk. Astrophysical Journal Letters, 924 (1). Art. No. L4. ISSN 2041-8205. doi:10.3847/2041-8213/ac3e62.

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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.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Quiroz, Juan0000-0001-8037-3779
Wallack, Nicole L.0000-0003-0354-0187
Ren, Bin0000-0003-1698-9696
Dong, Ruobing0000-0001-9290-7846
Xuan, Jerry W.0000-0002-6618-1137
Mawet, Dimitri0000-0002-8895-4735
Millar-Blanchaer, Maxwell A.0000-0001-6205-9233
Ruane, Garreth0000-0003-4769-1665
Additional Information:© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 October 4; revised 2021 November 23; accepted 2021 November 24; published 2022 January 4. We thank the anonymous referee for comments that improved this Letter. This research is partially supported by NASA ROSES XRP award 80NSSC19K0294. We thank Jean-Baptiste Ruffio, Jason Wang, Christian Ginski, and Myriam Benisty for discussions on calculating contrast curves. R.D. acknowledges financial support provided by the Natural Sciences and Engineering Research Council of Canada through a Discovery Grant as well as the Alfred P. Sloan Foundation through a Sloan Research Fellowship. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Part of the computations presented here were conducted in the Resnick High Performance Computing Center, a facility supported by the Resnick Sustainability Institute at the California Institute of Technology. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program 096.C-0248(A). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the SVO Filter Profile Service ( supported from the Spanish MINECO through grant AYA2017-84089. Facilities: Keck II (NIRC2) - , VLT:Melipal (SPHERE). Software: DebrisDiskFM (Ren et al. 2019), emcee (Foreman-Mackey et al. 2013), IRDAP (van Holstein et al. 2020), VIP (Gomez Gonzalez et al. 2017).
Group:Astronomy Department, Resnick Sustainability Institute
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2017-84089
Subject Keywords:Protoplanetary disks; Coronagraphic imaging; Planetary system formation
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Protoplanetary disks (1300); Coronagraphic imaging (313); Planetary system formation (1257)
Record Number:CaltechAUTHORS:20220114-265889000
Persistent URL:
Official Citation:Juan Quiroz et al 2022 ApJL 924 L4
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:112929
Deposited By: George Porter
Deposited On:18 Jan 2022 16:27
Last Modified:18 Jan 2022 16:27

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