cosmos.lbl.gov              

      Phone : (1)-510-846-6513 Fax :(1)-510-486-7149 eMail      sricciardi_at_lbl.gov sara.ricciardi_at_roma1.infn.it
My Web log here
 

  This is the procedure:

  1. generate the maps for all the components according to Planck reference sky at WMAP frequency.
  2. co-adding the component maps [5 map ]
  3. convolving with a beam to mimic the smearing due to the beam cl/(bb)^2 [where bb is the window function in l space provided by WMAP team]
  4. calculate the power spectra of the WMAP maps and Reference sky maps with the same cut

I ran the calculation for different cuts in the sky:

  1. on the first column for the all sky maps
  2. on the second column for a cut out the galactic plane [+-5 deg]
  3. on the third column for a cut into the galactic plane [+-5 deg]
To use a gaussian beam instead the one supplied by WMAP team don't change a lot. If you are interested to check this effect I plotted both correction in the first column.

To read the plots:

  1. dashed WMAP
  2. solid reference sky
  3. gray reference sky # beam

Comments: in all the plots the power spectra of the Planck reference sky is lower then the WMAP power spectra. These effect is more intense in the band where the foregrounds are dominant instead in the W map this effect is negligible. Outside the galactic plane the Planck reference sky is a worse respect to inside. This is not surprising because often our knowledge about foreground and our foregrounds templates are better into the galactic plane. [Historically there are much more galactic survey then non-galactic.]

Copyright - sara - 2006