## DR4 Multifrequency Spectra described in Choi et al. 2020ACTPol 98 and 150 GHz power spectra There are two sets of data product for power spectra in C_ell. deep: deep56, deep1, deep5, deep6 wide: boss, s16 (w0,w1,w3,w4,w5) ell_centers = [350.5, 400.5, 450.5, 500.5, 550.5, 600.5, 650.5, 700.5, 750.5, 800.5, 850.5, 900.5, 950.5, 1000.5, 1050.5, 1100.5, 1150.5, 1200.5, 1250.5, 1300.5, 1350.5, 1400.5, 1450.5, 1500.5, 1550.5, 1600.5, 1650.5, 1700.5, 1750.5, 1800.5, 1850.5, 1900.5, 1950.5, 2000.5, 2075.5, 2175.5, 2275.5, 2375.5, 2475.5, 2625.5, 2825.5, 3025.5, 3325.5, 3725.5, 4125.5, 4525.5, 4925.5, 5325.5, 5725.5, 6125.5, 6725.5, 7525.5] TT power spectra frequency combinations: 98x98, 98x150, and 150x150. TE power spectra frequency combinations: 98x98, 98x150, 150x98, and 150x150. EE power spectra frequency combinations: 98x98, 98x150, and 150x150. ## DR4 CMB-only Spectra described in Choi et al. 2020The ACTPol TT, EE and TE multi-frequency power spectra are used to estimate the deep and wide CMB-only bandpowers, marginalized over astrophysical foregrounds. The deep and wide spectra are binned and co-added, and are given with the following columns: - the mean multipole moment l
- the power spectrum in units of μK
^{2}Dl - the error for the binned value in units of μK
^{2}Dl
These spectra are released for plotting purposes and do not include the full covariance. For statistical comparison to a theory Cl, the theory Cls should be convolved with bandpower window functions. Any likelihood analysis should be performed using the corresponding CMB-only likelihood provided. ## DR4 Cosmic-Birefringence Spectrum described in Namikawa et al. 2020The text file contains bandpowers and error bars for cosmic-birefringence spectrum. These values are obtained from the analysis in Namikawa et al. (2020), corresponding to the red points on Figure 1 of that paper. The spectra are binned, and are given with the following columns: - the multipole bin center l
- the power spectrum in units of deg
^{2} - the error for the binned value in units of deg
^{2}
Please see Namikawa et al. (2020) [https://arxiv.org/abs/2001.10465] for further details. ## DR4 Delensed Spectra described in Han et al. 2020The files 060420_lensed_spectra_dls.txt and 060420_delensed_spectra_dls.txt contain the lensed and delensed data spectra, respectively, used in the Han et al analysis. The spectra are in the form D_l = l(l+1) C_l / 2pi and have units of uK^2.
Note that for all TT spectra, the first two entries (first two bins) are set to zero. This is because we use all 49 bins for TE and EE, but 47 bins for TT, beginning at lbin = 600. |