Testing the Interaction Between a Substellar Companion and a Debris Disk in the HR 2562 System

Kavli Affiliate: Bruce Macintosh

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| Summary:

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 GPI
monitoring of the companion’s orbit with 6 new epochs from 2016 to 2018. We
update the orbital fit and, in combination with absolute astrometry from GAIA,
place a 3$sigma$ 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 an inner radius that is close
to the companion’s semi-major axis. Including a posteriori knowledge of the
system’s SED further narrows the constraints on the disk’s inner radius and
place 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 testbed for dynamical interaction between a debris disk
and a substellar companion.

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