Exoplanets around dusty stars

In 2010, with collaborators from Caltech, JPL and GSFC, we initiated an ambitious high contrast imaging follow-up of young stars identified by Spitzer (and WISE) to have strong IR excess emission at 70 (or 22) μm, indicative of a dusty debris disk, and thus of massive planetary systems (e.g. β Pictoris, HR8799, HD95086, ...), making such targets ideal for planet searches. We have surveyed hundreds of stars using both Keck-NIRC2 and VLT-NACO. I was responsible for the Southern hemisphere observations, the common data reduction pipeline, common proper motion and statistical analysis. At its output are a full astrometric and photometric characterization of putative candidate companions, as well as de-biased detection limits. 

With Dr. Tiffany Meshkat (IPAC, Caltech) and Marta Bryan (Caltech graduate students), we wrapped up the first part of this study in October 2017, see:



Co-Investigators: T. Meshkat (JPL/Caltech), M. Bryan (Caltech), S. Hinkley (Exeter), B. Bowler (UT Austin), K. Stapelfeldt (JPL/Caltech), K. Batigyn (Caltech), M. Morales (JPL/Caltech), D. Padgett (GSFC), E. Serabyn (JPL/Caltech), V. Christiaens (U. Chile), T. Brandt (UCSB), Z. Wahhaj (ESO)

© Dimitri Mawet 2017