Description of CBI polarization fine-bin data (astro-ph/:0509203)

The spectrum is contained in CBIpol_2.0_final.newdat 
This data file should work as-is with current versions of COSMOMC
(Lewis & Bridle, 2002) 


File format:
first line - location of window functions (should be properly set).
second line - total bands in each polarization. Order is
       TT,EE,BB,TB,TE,EB
next lines (BAND_SELECTION) - select which bands are to be used in
     parameter fitting.  As mentioned in the paper, we drop the lowest
     T bin (both in TT and TE).
next line:  (1 1.00 0.026) - only number of relevance is 0.026, which
     is the CBI calibration uncertainty in power (1.3% in amplitude)
(ignorable line)
iliketype - COSMOMC/.newdat format support offset-lognormal
	  approximation to the likelihood (Bond, Jaffe, and Knox 2000).
	  iliketype=2 lets the use of the offset-lognormal
	  approximation be specified for each band individually.  We
	  turn it on for TT, EE, and BB, and turn it off for TE.

Next is a block for each polarization in the file.  This contains the
name of the polarization, then one line containing the spectrum for
each band power in the polarization.  The fields are:
1) Band #
2) Power spectrum (l(l+1)C_l/2pi, in uK^2)
3) and 4) - error bars.
5) noise spectrum, used in the offset-lognormal approximation.
6) and 7) the lower/upper ell range contained in the band
8) the iliketype flag for the band.  1 means use offset-lognormal, 0
   means Gaussian.
Then a block containing the same-band correlations between
band-powers.  Ones along the diagonal, with the off-diagonal terms the
degree of correlation between bands.

Finally, the Fisher matrix for the entire spectrum (all
polarizations).  Units are in uK^4.  This full matrix is used when
calculating the likelihood of a spectrum in COSMOMC.

There is also a directory "windows" - in it are the band-power window
functions.  There is one file for each band.  Columns are 
1) ell
2)-5) W_ell/ell for each polarization.  Columns are normalized, so
      expected C_ell is sum(W_ell,PP')C_ell,PP' over ell and
      polarizations PP'.




