This archive contain release of Boomerang LDB power spectrum data, published in P. deBernardis et al., Nature, 404, p.955, (2000). --------------------------------------------------- See the file "CONTENTS" for a description of the files in this archive. This README file contains a summary of the data. --------------------------------------------------- Web References: http://oberon.roma1.infn.it/boomerang/ http://www.physics.ucsb.edu/~boomerang --------------------------------------------------- Brief summary of the data for band powers: ------------ Power in multipole bands and the error bars ---------- Column 0: Just a counter. Column 1: l_min. Minimum multipole included in the bin Column 2: l_max. Maximum multipole included in the bin. Column 3: l_bar. Center multipole for the bin. Column 4: (dT_bin)^2. The power in this bin, l(l+1)C_l/2pi, in units of (micro-K)^2 Column 5: sigma_bin. The uncertainty in column 4, in units of (micro-K)^2 Column 6: 'xb' Parameter. See, for example, Bond, Jaffe and Knox 1998, astro-ph/9808264 (0) (1) (2) (3) (4) (5) (6) 1 26 75 50.00 1140.55 259.174 3.90026 2 76 125 100.00 3110.66 491.820 8.35781 3 126 175 150.00 4155.12 547.354 18.7338 4 176 225 200.00 4703.71 538.811 35.6949 5 226 275 250.00 4304.85 462.634 71.2736 6 276 325 300.00 2641.50 309.740 127.931 7 326 375 350.00 1554.30 221.784 248.283 8 376 425 400.00 1310.24 219.366 392.760 9 426 475 450.00 1356.59 250.142 606.110 10 476 525 500.00 1442.61 293.052 874.743 11 526 575 550.00 1750.30 369.735 1230.15 12 576 625 600.00 1535.63 420.665 1690.98 ----------------- Inverse Likelihood curvature matrix ------------- Following is the correlation matrix for the points above. The units are ((micro-K)^2)^2 (yes, squared twice). Note that the square-root of the diagonals should be the error-bars listed in the table above column (5). 7.79e+04 -1.17e+04 1.21e+02 -2.92e+02 -1.11e+02 -4.57e+01 -2.22e+01 -1.66e+01 -1.52e+01 -1.53e+01 -1.52e+01 -1.62e+01 -1.17e+04 2.36e+05 -2.29e+04 9.92e+01 -4.83e+02 -1.50e+02 -6.89e+01 -4.73e+01 -4.12e+01 -3.95e+01 -4.27e+01 -4.01e+01 1.21e+02 -2.29e+04 2.94e+05 -2.56e+04 7.09e+01 -3.59e+02 -1.26e+02 -7.84e+01 -6.42e+01 -5.84e+01 -6.00e+01 -6.02e+01 -2.92e+02 9.92e+01 -2.56e+04 2.94e+05 -2.17e+04 2.42e+01 -2.57e+02 -1.29e+02 -9.24e+01 -8.06e+01 -7.78e+01 -7.54e+01 -1.11e+02 -4.83e+02 7.09e+01 -2.17e+04 2.15e+05 -1.24e+04 1.68e+00 -2.19e+02 -1.35e+02 -9.77e+01 -9.39e+01 -8.43e+01 -4.57e+01 -1.50e+02 -3.59e+02 2.42e+01 -1.24e+04 9.39e+04 -6.05e+03 -2.82e+01 -1.70e+02 -1.19e+02 -8.72e+01 -8.22e+01 -2.22e+01 -6.89e+01 -1.26e+02 -2.57e+02 1.68e+00 -6.05e+03 4.89e+04 -4.30e+03 -5.75e+01 -1.38e+02 -1.04e+02 -6.64e+01 -1.66e+01 -4.73e+01 -7.84e+01 -1.29e+02 -2.19e+02 -2.82e+01 -4.30e+03 4.71e+04 -4.74e+03 -6.46e+01 -1.37e+02 -9.98e+01 -1.52e+01 -4.12e+01 -6.42e+01 -9.24e+01 -1.35e+02 -1.70e+02 -5.75e+01 -4.74e+03 6.08e+04 -6.30e+03 -7.28e+01 -1.51e+02 -1.53e+01 -3.95e+01 -5.84e+01 -8.06e+01 -9.77e+01 -1.19e+02 -1.38e+02 -6.46e+01 -6.30e+03 8.51e+04 -9.20e+03 -1.00e+02 -1.52e+01 -4.27e+01 -6.00e+01 -7.78e+01 -9.39e+01 -8.72e+01 -1.04e+02 -1.37e+02 -7.28e+01 -9.20e+03 1.33e+05 -1.37e+04 -1.62e+01 -4.01e+01 -6.02e+01 -7.54e+01 -8.43e+01 -8.22e+01 -6.64e+01 -9.98e+01 -1.51e+02 -1.00e+02 -1.37e+04 1.84e+05 --------------- Calibration ---------------------------------------- The calibration uncertainty is 10% (in temperature units), dominated by systematic uncertainty. (See deBernardis, et al. 2000). --------------- Beam ----------------------------------------------- Exact l-dependence of the beam is given in the file 'beam' of the archive, which includes effects of pixelization. The pixelization used is HEALPix (www.eso.org/~kgorski/healpix), with a parameter Nside = 256 (=13.7 arcmin pixel size) The beam is roughly a Gaussian with FWHM \theta_s=10 arcmin. We estimate beam FWHM uncertainty to be +-1 arcmin (1-sigma gaussian error); see (deBernardis etal 2000) for details. The following way to account for beam uncertainty has been used in Lange et al (astro-ph/0005004) and is sufficiently accurate: The bandpower is I(C_L W_L)/I(W_L), where the "logarithmic integral" I(f_L) = sum_L f_L (L+1/2)/(L(L+1)) for any function f_L, and W_L is the beam function. Uncertainty in the beam leads to uncertainty in bandpowers as I(C_L W_L exp(-(L+0.5)^2 [\delta(\theta_s^2)] )/I(W_L), where \delta(theta_s^2) is the Gaussian beam uncertainty squared. \delta(\theta_s^2) = 2 \theta_s ( \delta \theta_s ) We assume that \delta \theta_s is gaussian distributed with standard deviation 1 arcmin. Note, that approximate FWHM theta_s=10 arcmin value is used only to compute beam uncertainty. The main term W_L is given by the accurate shape in the file 'beam' ------------------------------------------------------------------ Last Modified Sept 30, 2000