Our models are compared to a suite of observational data for thermal and scattered light emission, ranging from the ALMA radial surface brightness profile at 1.3 mm to
polarisation measurements in the visible.
Not exact matches
In addition to the observations with the SINFONI instrument the team has also made a long series of
measurements of the
polarisation of the light coming from the supermassive black hole region using the NACO instrument on the VLT.
If the wave function is real, then a single experiment should not be able to determine its
polarisation — it can have both until you take more
measurements.
In a complicated setup that involved pairs of photons and hundreds of very accurate
measurements, the team showed that the wave function must be real: not enough information could be gained about the
polarisation of the photons to imply they were in particular states before
measurement.
1:20 PM Liu - Abundance Studies of Stellar Hosts of Terrestrial Planets 1:40 PM Kitiashvili - 3D Realistic Modeling of Stellar Convection as a Tool to Study Effects of Stellar Jitter on RV
Measurements 2:00 PM Crossfield - Planet Densities (invited) 2:30 PM Break and Poster Viewing 3:00 PM Guyon - Coronagraphs for Planet Detection (invited) 3:30 PM Martins - Exoplanet Reflections in the era of Giant Telescopes 3:50 PM Close - Direct Detection of Exoplanets with GMT AO: A proof of concept design for a GMT Phase A ExAO planet imager 4:10 PM Direct Imaging Discussion - Led by Jared Males 5:20 PM End of meeting for the day 5:30 PM Buses depart for Monterey Bay Aquarium 6:00 PM Conference Banquet Wednesday, September 28 7:30 - 9:00 AM Breakfast 9:00 AM Lewis - JWST - ELT Synergy (invited) 9:30 AM Greene - Characterizing exoplanet atmospheres with JWST 9:50 AM Morzinski - Breaking degeneracies in understanding fundamental exoplanet properties with ELTs 10:10 AM Break and Poster Viewing 11:00 AM Cotton - Detecting Clouds in Hot Jupiters with Linear
Polarisation 11:20 AM Boss - Summary