- #1
Tanelorn
- 888
- 15
One of the major concerns in any Cosmic Microwave Background (CMB) anisotropy analysis is to determine which fraction of the observed signal is due to some foreground contaminant. Two sources of foreground contamination have been firmly identified: the diffuse Galactic emission and unresolved point sources.
https://www.cfa.harvard.edu/~adeolive/foreground.html
Have there been any further developments regarding this, and can anyone quantify the impact on the CMBR measurements? How do we know when we are looking at a foreground signal?
https://www.cfa.harvard.edu/~adeolive/foreground.html
Have there been any further developments regarding this, and can anyone quantify the impact on the CMBR measurements? How do we know when we are looking at a foreground signal?