Cosmic Background Imager |

Here we present supplementary numerical data that were not included
in the papers reporting the CBI results from the 2000 observing
season. *If you use these data in a publication, please cite the
appropriate papers and also give the URL of this web page and the
date of publication (given at the bottom of this page)*.

Band powers for the joint (3-field) deep data set are given in
Table 3. There are two alternate binnings of the power spectrum, which
are *not independent*.

- Standard binning: 7 bins,
*l*= 0-500, 500-880, 880-1445, 1445-2010, 2010-2388, 2388-3000, and > 3000. - Alternate binning: 6 bins,
*l*= 0-690, 690-1162, 1162-1728, 1728-2199, 2199-2694, and > 2694. - We also combined the highest 3 bins of the standard binning into a
"big bin" 2010 <
*l*.

The upper limit on *l* in
all the binnings is set by the data to ~ 4000.

Window functions are given in Mason et al. Fig. 2. The file deep_windows.tar.gz (compressed tar file) contains 14 files, one for each band:

- joint_3deep_std2_best_window_* (7 files).
- joint_3deep_alt2_best_window_* (6 files).
- joint_3deep_bigbin_best_window_5 (1 file).

The window functions are tabulated in bins of width 90 in *l*, i.e.,
*l* = 1-90, 91-180, ...; and the tabulated values should be
divided by 90 to get the quantity plotted,
*W ^{B}(l)/l*.

The file deep.tar.gz (compressed tar file) contains 9 files, 3 each for the standard, alternate, and "big" binnings:

joint_3deep_alt2_best_invfish joint_3deep_alt2_best_otherps joint_3deep_alt2_best_qb joint_3deep_bigbin_best_invfish joint_3deep_bigbin_best_otherps joint_3deep_bigbin_best_qb joint_3deep_std2_best_invfish joint_3deep_std2_best_otherps joint_3deep_std2_best_qb

These files should be interpreted as follows:

**qb**file- There are 7 (std2) or 6 (alt2) entries, one for each band. Column 1 is the band number; column 2 is the band power
*q*, and column 3 is the uncertainty on the band power (square root of the diagonal element of the covariance matrix). Band powers are dimensionless; multiply by^{B}*T*_{cmb}^{2}to put them in temperature units. **invfish**file- Ignore the first 6 lines in this file. The first 7 (std2) or 6 (alt2) columns of the next 7 (std2) or 6 (alt2) lines give the 7 by 7 or 6 by 6 band-power covariance matrix. This is the inverse of the curvature (Hessian) matrix as given in equation 75 of Myers et al., and it can be used directly to give a gaussian approximation to the likelihood function.
**otherps**file- It is better to use an offset lognormal approximation to the likelihood function (Sievers et al., equation 2), for which you need the offsets
*q*. The offsets are given in the_{Nt}^{B}**otherps**file, which contains 7 (or 6) entries, one for each bin. There are 4 columns giving the component band-powers for noise and discrete sources. You should add all four components to get the required band-power offset.

Band powers for the joint (3 field) mosaic data set are given in
Table 2. A small fraction of the data are common with the deep data
set (see the papers). There are again two alternate binnings of the
power spectrum, which are *not independent*; in both the bin
width is 200 in *l* except for the first bin.

- Even binning: 14 bins:
*l*= 0-400, 400-600, 600-800, ..., 2800-3000. - Odd binning: 14 bins:
*l*= 0-300, 300-500, 500-700, ..., 2700-2900.

Window functions are given in Pearson et al. Fig. 11. The file mosaic_windows.tar.gz (compressed tar file) contains 28 files, one for each band:

- joint_window_iso_0.08_200_even_deep_3level_feb_window_* (14 files).
- joint_window_iso_0.08_200_odd_deep_3level_feb_window_* (14 files).

The window functions are tabulated in bins of width 25 in *l*,
with the first bin starting at *l* = 101, i.e.,
*l* = 101-125, 126-150, ...; and the tabulated values should be
divided by 25 to get the quantity plotted,
*W ^{B}(l)/l*.

The file mosaic.tar.gz (compressed tar file) contains 6 files, 3 each for the odd and even binnings:

joint_final_iso_0.08_200_even_invfish joint_final_iso_0.08_200_even_otherps joint_final_iso_0.08_200_even_qb joint_final_iso_0.08_200_odd_invfish joint_final_iso_0.08_200_odd_otherps joint_final_iso_0.08_200_odd_qb

These files should be interpreted as follows:

**qb**file- There are 16 entries, one for each band; ignore the bands numbered 15 and 16. Column 1 is the band number; column 2 is the band power
*q*, and column 3 is the uncertainty on the band power (square root of the diagonal element of the covariance matrix). Band powers are dimensionless; multiply by^{B}*T*_{cmb}^{2}to put them in temperature units (as given in Table 2 of Pearson et al.). **invfish**file- Ignore the first 6 lines in this file. The first 14 columns of the next 14 lines give the 14 by 14 band-power covariance matrix. This is the inverse of the curvature (Hessian) matrix as given in equation 75 of Myers et al., and it can be used directly to give a gaussian approximation to the likelihood function.
**otherps**file- It is better to use an offset lognormal approximation to the likelihood function (Sievers et al., equation 2), for which you need the offsets
*q*. The offsets are given in the_{Nt}^{B}**otherps**file, which contains 16 entries, one for each bin; ignore bins 15 and 16. There are 4 columns giving the component band-powers for noise and discrete sources. You should add all four components to get the required band-power offset.

Last update: 2002 August 8.