A Spatially-resolved Large Cavity of the J0337 Protoplanetary Disk in Perseus

Creators: Uyama, Taichi; Ruane, Garreth; Lawson, Kellen; Muto, Takayuki; Beichman, Charles; van der Marel, Nienke

Abstract

We present Keck/NIRC2 KₚLₚ high-contrast imaging observations of a J0337 protoplanetary disk. The data discover the spatially-resolved large cavity, which is the second report among protoplanetary disks in the Perseus star-forming region after the LkHα 330 system. Our data and forward modeling using RADMC-3D suggests ∼80 au for the cavity radius. There is discrepancy between J0337's spectral energy distribution (SED) and the modeled SED at ∼10 μm and this suggests an unseen inner disk. We also searched for companions around J0337 but did not detect any companion candidates at separations between 0farcs1 and 2farcs5. The Lp-band detection limit corresponds to ∼20Mⱼᵤₚ at 60 au, ∼9–10Mⱼᵤₚ at 90 au, and ∼3Mⱼᵤₚ at >120 au. Compared with other young systems with large cavities such as PDS 70 and RX J1604, multiple Jovian planets, a single eccentric Jovian planet, or a massive brown dwarf at an inner separation could exist within the cavity.

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 December 15; revised 2022 January 24; accepted 2022 January 27; published 2022 April 11. The authors would like to thank the anonymous referees for the constructive comments and suggestions to improve the quality of the paper. We are grateful to Jason Wang for suggestions on the pyKLIP parameters. We thank Akimasa Kataoka for helpful comments to develop the RADMC-3D modeling. T.U. is supported by Grant-in-Aid for Japan Society for the Promotion of Science (JSPS) Fellows and JSPS KAKENHI grant No. JP21J01220. T.M. is supported by JSPS KAKANHI grant Nos. 17H01103, 18H05441 and 19K03932. 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. This research has made use of the Keck Observatory Archive (KOA; O'Meara 2020), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported by the Spanish MINECO through grant AyA2017-84089. VOSA has been partially updated by using funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement No. 776403 (EXOPLANETS-A).

Attached Files

Published - Uyama_2022_AJ_163_204.pdf

Accepted Version - 2201.11771.pdf

Files

Uyama_2022_AJ_163_204.pdf

Files (2.6 MB)

Name	Size	Download all
Uyama_2022_AJ_163_204.pdf md5:813e08fc1642f29e958f2323bbbbf039	1.3 MB	Preview Download
2201.11771.pdf md5:096263651d6e2cca95460b83e802277f	1.4 MB	Preview Download

Additional details

	All versions	This version
Views	0	0
Downloads	0	0
Data volume	0 Bytes	0 Bytes