All Tables

Table 1: The optical filtering scheme employed by B03. In order to take advantage of the low backgrounds available at float altitudes, much care must be taken to reduce the background originating from within the cryostat. While the metal mesh filters, which consist of bonded layers of polyethylene, exhibit in-band emissivities at the percent level, the PTFE antireflection coating is several times more emissive. It is crucial that these filters remain well heat-sunk and protected from infrared emission from the warmer stages.
Table 2: Summary of the properties of the B03 receiver. The noise reported in the last column is for a frequency of 1 Hz and is the average noise of all the detectors at that frequency.
Table 3: Spectral and time response calibrations: for all channels (named in Col. 1) we report in the second column the average frequency, and in the third column the optical bandwidth $\Delta \nu = \left( \int e(\nu) {\rm d}\nu \right)^2/\!\int e^2(\nu) \rm d\nu$ . Here $e(\nu )$ are the transmission spectra of Fig. 10. The conversion factor between Specific Brightness and CMB temperature fluctuations, as computed from the same spectra, is reported in the fourth column. Spectral normalizations and flat band optical efficiencies are measured using NDF-up load curve power differences. The spectral normalization $\eta$ (fifth column) is calculated using the spectral response from the FTS measurements. The optical efficiency $\langle \eta e(\nu) \rangle_{\rm band}$ (sixth column) is calculated assuming a flat spectral response. The detectors are assumed to be single-moded. The high optical efficiency of the 345 GHz channels is likely due to propagation of multiple modes to the detector. The time constant $\tau$ is reported in the seventh column, as measured in the laboratory with loading conditions similar to the flight ones.
Table 4: Cross-polarization and principal axis angle measurements for all the channels. The polarization angle and the beam filling values refer to measurements on the complete instrument obtained with the apparatus described in Fig. 12, while the on-axis measurements refer to measurements on the receiver alone, obtained with the apparatus described in Fig. 11 and also in a test cryostat testing single channels.
Table 5: The receiver performance for a typical channel from each of the B OOMERANG bands, computed from a receiver model using the observed average in-flight loading conditions. The performance measured in flight is consistent with these estimates.
Table 6: In flight detectors performance: we report the noise equivalent temperature at 1 Hz, derived from the noise equivalent voltage measured in flight as in Sect. 6.4, from the responsivity estimated as in Sect. 7.2.1 and from the spectral calibrations of Sect. 3.2. In our survey, this frequency corresponds to multipoles $400 \protect \la \ell \protect\la 1200$ . The noise increases at lower and at higher frequencies, as shown in Fig. 22.
Table 7: Absolute value of the noise cross-power-spectrum for the 145 GHz detectors, averaged in the 0.1-2 Hz range. The numerical values have been normalized to the noise auto-power-spectrum of detector 145W1, which is $1.2 \times 10^{-6} V^2/\rm Hz$ at the ADC input.
Table 8: Relative calibration $\mathcal{R}$ of the PSB channels obtained from the pixel-pixel scatter plots with NSIDE = 256 (second column, see Sect. 7.2.1) and from the cross-spectrum (third column, see Sect. 7.2.2), using W₁ as the reference channel. For $\mathcal{R}_{*W_1}^{\rm spectrum}$ , 1- $\sigma$ errors are used. For $\mathcal{R}_{*W_1}^{\rm pixel}$ , we also include in the error the possible bias due to a conservative $\pm$ $20\%$ error in the estimate of the noise.
Table 9: Summary of the different choices made for the two data analysis pipelines.
Table 10: Pixel-space fits of the B03 maps with a combination of a CMB template (from WMAP) and a dust template (from IRAS), see Eq. (39). For the three upper rows, the fit has been performed in the deep survey region ( $74\hbox {$^\circ $ }<\rm RA < 90\hbox {$^\circ $ }$ ; $-50\hbox {$^\circ $ }< {\rm Dec} < -40\hbox {$^\circ $ }$ , $\langle \vert b\vert \rangle \sim 32\hbox{$^\circ$ }$ , for a total of 2172 15 $^\prime$ pixels). In this region, the rms fluctuation of the IRAS/DIRBE map is 0.25 MJy/sr. For the three lower rows, the fit has been done in the part of the Shallow Survey closer to the Galactic Plane ( $90\hbox {$^\circ $ }< {\rm RA} < 105\hbox {$^\circ $ }$ ; $-50\hbox {$^\circ $ }< {\rm Dec} < -40\hbox {$^\circ $ }$ , $\langle \vert b\vert \rangle \sim 23\hbox{$^\circ$ }$ , 2027 pixels of 15 $^\prime$ ). Here the rms fluctuation of the IRAS/DIRBE map is 0.57 MJy/sr. R(A) is the correlation coefficient for the CMB template, while R(B) is the correlation coefficient for the dust template. The last column gives the estimated brightness fluctuation due to the ISD component correlated to the IRAS/DIRBE map, in CMB temperature units.