The Aim of This Workshop

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)COrEPIXIE, and LiteBIRD: how many frequencies do we need? How should we distribute those frequencies?

Summary of the workshop

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)