Goals & Strategy

Survey of Galaxy Clusters through the Sunyaen-Zeldovich Effects

1. AMiBA Medium-Field Survey
2. AMiBA Medium-Field Survey
3. AMiBA Deep Survey

Measurement of Missing Baryons

1. Detecting the Missing Baryons
2. Extracting IGM gas pressure power spectrum

Measurement of CMB Polarization Anisotropy

1. Data Analysis Pipeline:scan a small fraction of the sky and make a polarization sky map.
2. Separate the CMB polarization from the system noise, and the foreground contaminations.
3. The point sources remove by using higher resolution data obtained in the AMiBA long-baseline configuration.
4. The galactic emissions remove by multi-frequency subtraction scheme if necessary.
5. The resulting polarization vectors decompose into the E-mode (electric-like) and the B-mode (magnetic-ike)     polarization.
6. The E-polarization sky map decompose into a sum of spherical harmonics, E(£c, £p)=£Ulm almYlm (£c, £p),     where Cl =£Um |alm|2 is the E-polarization power spectrum.