Stella Yimiao Zhang, Center for Astrophysics & Space Sciences
Gaspard Duchêne, University of California, Berkeley
Robert J. De Rosa, European Southern Observatory Santiago
Megan Ansdell, National Aeronautics and Space Administration
Quinn Konopacky, Center for Astrophysics & Space Sciences
Thomas Esposito, University of California, Berkeley
Eugene Chiang, University of California, Berkeley
Malena Rice, Yale University
Brenda Matthews, National Research Council Canada
Paul Kalas, University of California, Berkeley
Bruce Macintosh, Kavli Institute for Particle Astrophysics and Cosmology
Franck Marchis, SETI Institute
Stan Metchev, Western University
Jenny Patience, School of Earth and Space Exploration
Julien Rameau, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG)
Kimberly Ward-Duong, Smith CollegeFollow
Schuyler Wolff, The University of Arizona
Michael P. Fitzgerald, University of California, Los Angeles
Vanessa P. Bailey, California Institute of Technology
Travis S. Barman, The University of Arizona
Joanna Bulger, University Hawaii Institute for Astronomy
Christine H. Chen, Space Telescope Science Institute
Jeffrey K. Chilcotte, University of Notre Dame
Tara Cotten, University of Georgia
René Doyon, Institut de Recherche sur les Exoplanètes
Katherine B. Follette, Amherst College
Benjamin L. Gerard, University of Victoria
Stephen Goodsell, Durham University
James R. Graham, University of California, Berkeley
Alexandra Z. Greenbaum, Infrared Processing & Analysis Center
Pascale Hibon, European Southern Observatory Santiago
Li Wei Hung, US National Park Service

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Publication Title

Astronomical Journal


The HR 2562 system is a rare case where a brown dwarf companion resides in a cleared inner hole of a debris disk, offering invaluable opportunities to study the dynamical interaction between a substellar companion and a dusty disk. We present the first ALMA observation of the system as well as the continued Gemini Planet Imager monitoring of the companion's orbit with six new epochs from 2016 to 2018. We update the orbital fit, and in combination with absolute astrometry from GAIA, place a 3σ upper limit of 18.5 M J on the companion's mass. To interpret the ALMA observations, we used radiative transfer modeling to determine the disk properties. We find that the disk is well resolved and nearly edge-on. While the misalignment angle between the disk and the orbit is weakly constrained, due to the short orbital arc available, the data strongly support a (near) coplanar geometry for the system. Furthermore, we find that the models that describe the ALMA data best have inner radii that are close to the companion's semimajor axis. Including a posteriori knowledge of the system's SED further narrows the constraints on the disk's inner radius and places it at a location that is in reasonable agreement with (possibly interior to) predictions from existing dynamical models of disk truncation by an interior substellar companion. HR 2562 has the potential over the next few years to become a new test bed for dynamical interaction between a debris disk and a substellar companion.









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Creative Commons Attribution 4.0 International License
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© 2023. The Author(s).


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