A Large Double-ring Disk Around the Taurus M Dwarf J04124068+2438157

Creators: Long, Feng; Ren, Bin B.; Wallack, Nicole L.; Harsono, Daniel; Herczeg, Gregory J.; Pinilla, Paola; Mawet, Dimitri; Liu, Michael C.; Andrews, Sean M.; Bai, Xue-Ning; Cabrit, Sylvie; Cieza, Lucas A.; Johnstone, Doug; Leisenring, Jarron M.; Lodato, Giuseppe; Liu, Yao; Manara, Carlo F.; Mulders, Gijs D.; Ragusa, Enrico; Sallum, Steph; Shi, Yangfan; Tazzari, Marco; Uyama, Taichi; Wagner, Kevin; Wilner, David J.; Xuan, Jerry W.

Abstract

Planet formation imprints signatures on the physical structures of disks. In this paper, we present high-resolution (∼50 mas, 8 au) Atacama Large Millimeter/submillimeter Array observations of 1.3 mm dust continuum and CO line emission toward the disk around the M3.5 star 2MASS J04124068+2438157. The dust disk consists of only two narrow rings at radial distances of 0."47 and 0."78 (∼70 and 116 au), with Gaussian σ widths of 5.6 and 8.5 au, respectively. The width of the outer ring is smaller than the estimated pressure scale height by ∼25%, suggesting dust trapping in a radial pressure bump. The dust disk size, set by the location of the outermost ring, is significantly larger (by 3σ) than other disks with similar millimeter luminosity, which can be explained by an early formation of local pressure bump to stop radial drift of millimeter dust grains. After considering the disk's physical structure and accretion properties, we prefer planet–disk interaction over dead zone or photoevaporation models to explain the observed dust disk morphology. We carry out high-contrast imaging at the L' band using Keck/NIRC2 to search for potential young planets, but do not identify any source above 5σ. Within the dust gap between the two rings, we reach a contrast level of ∼7 mag, constraining the possible planet below ∼2–4 M_(Jup). Analyses of the gap/ring properties suggest that an approximately Saturn-mass planet at ∼90 au is likely responsible for the formation of the outer ring, which can potentially be revealed with JWST.

Additional Information

© 2023. 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. F.L. thanks Rixin Li and Shangjia Zhang for insightful discussions. Support for F.L. was provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51512.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. F.L. and S.A. acknowledge funding support from the National Aeronautics and Space Administration under grant No. 17-XRP17 _ 2-0012 issued through the Exoplanets Research Program. D.H. is supported by Center for Informatics and Computation in Astronomy (CICA) grant and grant No. 110J0353I9 from the Ministry of Education of Taiwan. D.H. also acknowledges support from the National Science and Technology Council of Taiwan through grant No. 111B3005191. G.J.H and Y.S. are supported by grant 12173003 from the National Natural Science Foundation of China. G.D.M. acknowledges support from FONDECYT project 11221206, from ANID—Millennium Science Initiative—ICN12_009, and the ANID BASAL project FB210003. D.J. is supported by NRC Canada and by an NSERC Discovery Grant. Y.L. acknowledges the financial support by the Natural Science Foundation of China (grant No. 11973090). L.C. was supported by ANID through the Milennium Science Initiative Program (NCN2021_080) and the FONDECYT Grant 1211656. E.R. acknowledges financial support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 864965, PODCAST) C.F.M is funded by the European Union (ERC, WANDA, 101039452). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council Executive Agency. Neither the European Union nor the granting authority can be held responsible for them. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (PROTOPLANETS, grant agreement No. 101002188). This research was funded in part by the Gordon and Betty Moore Foundation through grant GBMF8550 to M. Liu. K.W. is supported by NASA through the NASA Hubble Fellowship grant HST- HF2-51472.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. J.L. acknowledges funding from JWST/NIRCam contract to the University of Arizona, NAS5-02105 This research is partially supported by NASA ROSES XRP, award 80NSSC19K0294. 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 Resnick Sustainability Institute at the California Institute of Technology. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.00566.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Facilities: ALMA - Atacama Large Millimeter Array, Keck II (NIRC2). - Software: emcee (Foreman-Mackey et al. 2013), CASA (CASA Team et al. 2022), pynrc (Leisenring et al. 2022), VIP (Gomez Gonzalez et al. 2017).

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