Convincing detection of the so-called B-mode polarization of cosmic micorwave background anisotropy due to primordial gravitational waves from inflation is thought to provide a definitive proof of inflation.
However, B-mode polarization is also generated by foreground emission from our own Galaxy, which is typically a few (or more) orders of magnitude larger than the primordial B-mode signal (in power).
Therefore, the crucial question is, "how can we reduce the effect of polarized foreground emission and extract the primordial B-mode signal?"
In this workshop, we will discuss:
- Physics of polarized foreground emission: synchrotron and dust, but should we be worried about other components?
- Methods for reducing the effect of polarization foreground emission, such as physical modeling, component separation, and template fitting methods
- How to optimize designs of future polarization missions such as EPIC, (beyond)COrE, PIXIE, and LiteBIRD: how many frequencies do we need? How should we distribute those frequencies?
Summary of the workshop
- Session 1: Physics of polarized foreground emission
- Session 2: Foreground reduction method
- Session 3: Current and future missions
The members of Scientific Organization Committee (SOC) include:
- Anthony Banday (Institut de Recherche en Astrophysique et Planétologie)
- Clive Dickinson (University of Manchester)
- Joanna Dunkley (University of Oxford)
- Torsten Enßlin (Max-Planck-Institut für Astrophysik)
- Eiichiro Komatsu (Max-Planck-Institut für Astrophysik)
- Radek Stompor (Laboratoire Astroparticule et Cosmologie)