A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph

Creators: Wallack, Nicole L.^{1, 2}; Ruffio, Jean-Baptiste³; Ruane, Garreth⁴; Ren 任, Bin B. 彬^{2, 5, 6}; Xuan, Jerry W.²; Villenave, Marion^{4, 7}; Mawet, Dimitri^{2, 4}; Stapelfeldt, Karl⁴; Wang, Jason J.^{2, 8}; Liu, Michael C.⁹; Absil, Olivier¹⁰; Alvarez, Carlos¹¹; Bae, Jaehan^{1, 12}; Bond, Charlotte¹³; Bottom, Michael⁹; Calvin, Benjamin^{2, 14}; Choquet, Élodie¹⁵; Christiaens, Valentin¹⁰; Cook, Therese¹⁴; Femenía Castellá, Bruno^{16, 17}; Gomez Gonzalez, Carlos¹⁸; Guidi, Greta¹⁹; Huby, Elsa²⁰; Kastner, Joel²¹; Knutson, Heather²; Meshkat, Tiffany²²; Ngo, Henry²³; Ragland, Sam¹¹; Reggiani, Maddalena²⁴; Ricci, Luca²⁵; Serabyn, Eugene⁴; Uyama, Taichi²²; Williams, Jonathan P.⁹; Wizinowich, Peter¹¹; Zawol, Zoe²; Zhang, Shangjia²⁶; Zhu, Zhaohuan²⁶

1. Carnegie Institution for Science
2. California Institute of Technology
3. University of California, San Diego
4. Jet Propulsion Lab
5. Lagrange Laboratory
6. Grenoble Alpes University
7. University of Milan
8. Northwestern University
9. University of Hawaii at Manoa
10. University of Liège
11. W.M. Keck Observatory
12. University of Florida
13. Science and Technology Facilities Council
14. University of California, Los Angeles
15. Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
16. Instituto de Astrofísica de Canarias
17. University of La Laguna
18. Barcelona Supercomputing Center
19. International Research Institute for Radio Astronomy
20. Laboratory of Space Studies and Instrumentation in Astrophysics
21. Rochester Institute of Technology
22. Infrared Processing and Analysis Center
23. Herzberg Institute of Astrophysics
24. KU Leuven
25. California State University, Northridge
26. University of Nevada, Las Vegas

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Abstract

Recent Atacama Large Millimeter/submillimeter Array (ALMA) observations of protoplanetary disks in the millimeter continuum have shown a variety of radial gaps, cavities, and spiral features. These substructures may be signposts for ongoing planet formation, and therefore these systems are promising targets for direct imaging planet searches in the near-infrared. To this end, we present results from a deep imaging survey in the L′ band (3.8 μm) with the Keck/NIRC2 vortex coronagraph to search for young planets in 43 disks with resolved features in the millimeter continuum or evidence for gaps/central cavities from their spectral energy distributions. Although we do not detect any new point sources, using the vortex coronagraph allows for high sensitivity to faint sources at small angular separations (down to ∼01), allowing us to place strong upper limits on the masses of potential gas giant planets. We compare our mass sensitivities to the masses of planets derived using ALMA observations, and while we are sensitive to ∼1 M_Jup planets in the gaps in some of our systems, we are generally not sensitive to planets of the masses expected from the ALMA observations. In addition to placing upper limits on the masses of gas giant planets that could be interacting with the dust in the disks to form the observed millimeter substructures, we are also able to map the micron-sized dust as seen in scattered light for 8 of these systems. Our large sample of systems also allows us to investigate limits on planetary accretion rates and disk viscosities.

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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.

Acknowledgement

This research is partially supported by NASA ROSES XRP, award 80NSSC19K0294. The Infrared Pyramid Wavefront Sensor at W. M. Keck Observatory was developed with support from the National Science Foundation under grants AST-1611623 and AST-1106391, as well as the Heising Simons Foundation under the Keck Planet Imager and Characterizer project. 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. The computations presented here were conducted in the Resnick High Performance Center, a facility supported by the Resnick Sustainability Institute at the California Institute of Technology. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. We thank the anonymous referee for their comments that improved the clarity of this work. Part of this research has received funding from the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101103114. Part of this research has received funding from the European Research Council (ERC) under the European Union's FP7 and Horizon 2020 research and innovation programs (grant agreements No. 337569 and 819155), and from the Wallonia-Brussels Federation (grant for Concerted Research Actions). M.V. research was supported by an appointment to the NASA Postdoctoral Program at the NASA Jet Propulsion Laboratory, administered by the Universities Space Research Association under contract with NASA. K.R.S. acknowledges support from the JPL Researchers on Campus Program. G.G. acknowledges the financial support of the Swiss National Science Foundation in the framework of the NCCR PlanetS. J.K.'s research on disks orbiting nearby young stars is supported by NASA Exoplanets Program grant 80NSSC19K0292 to RIT. This project has received funding from the European Research Council (ERC) under the European Union's Horizon Europe research and innovation program (grant agreement No. 101039651, project DiscEvol, PI G. Rosotti).

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