In the spectral range covered by PLANCK we can identify three regions characterized by the predominance of drastically different classes of extragalactic sources:
In addition, studies of the anisotropies of the diffuse background at these wavelengths will constrain galaxy counts to faint flux levels and, consequently lead to strong constraints on models of galaxy evolution.
|31||10||30||40||50||60||350 - 2500|
|53||6||18||40||50||57||250 - 2000|
|90||3||12||80||50||90||130 - 1000|
|125||2.4||10||210||40||81||50 - 300|
|217||1.4||7.5||15||5||66||400 - 2000|
|353||0.85||4.5||20||16||15||3000 - 15000|
|545||0.55||4.5||32||40||3||7000 - 50000|
|857||0.35||4.5||190||100||-||5000 - 20000|
1 Standard deviation of the pixel brightness fluctuations due to galaxies,
after removal of the brightest pixels, i.e. those with signal .
2 Sky variance induced by CMB anisotropies corresponding to .
3 Expected number of sources with flux in 70% of the sky. The lower value is without evolution, the upper one for the RG and PLE models.