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SUMMARY:Disks and Dynamics of Protoplanetary Systems - Ian Czekala (Berkel
 ey)
DTSTART:20200611T150000Z
DTEND:20200611T160000Z
UID:TALK141691@talks.cam.ac.uk
CONTACT:Dr Annelies Mortier
DESCRIPTION:The sensitivity and resolution of the Atacama Large Millimeter
 /Submillimeter Array (ALMA) have enabled detailed study of protoplanetary 
 disk structure and kinematics. By forward modeling the interferometric mea
 surement sets from ALMA we can infer the disk velocity field\, empirically
  measure stellar masses\, and unlock pre-main sequence system architecture
 s. Our observations of protoplanetary disks in binary star systems have pr
 ovided context needed to understand the circumbinary planet population as 
 probed by the Kepler Mission\, an effort that has historically been hamper
 ed by the fact that occurrence rate is degenerate with assumptions about t
 he typical misalignment between the binary and planetary orbital planes. O
 ur survey of 20 spatially-resolved circumbinary protoplanetary and debris 
 disks includes several spectroscopic binaries (P < 40 days) whose disks we
  have resolved with ALMA for the first time and are the only protoplanetar
 y systems comparable in scale to the Kepler circumbinary planet hosts. We 
 use a hierarchical Bayesian model to infer that the mutual inclination dis
 tribution of circumbinary disks around spectroscopic binaries is intrinsic
 ally low\, suggesting that Kepler did not miss a large population of mis-a
 ligned circumbinary planets\, and that circumbinary planets occur at a sim
 ilar rate as those around single stars. Throughout my talk\, I will discus
 s several of the data driven and forward modeling techniques that we devel
 oped to probe the planet forming environment with exquisite precision\, in
 cluding template-free spectroscopic disentangling with Gaussian processes 
 and regularized maximum likelihood image reconstruction. Techniques like t
 hese will be indispensable for sensing the velocity field with sufficient 
 precision to infer protoplanet properties from their kinematic perturbatio
 ns.
LOCATION:ONLINE - Details will be sent by email
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