|
- CMB spectrum and likelihood code - Planck PLA Wiki
The likelihood code (and the data that comes with it) used to compute the likelihood of a model that predicts the CMB power spectra, lensing power spectrum, together with some foreground and some instrumental parameters
- Planck 2018 results. V. CMB power spectra and likelihoods
This paper describes the 2018 Planck CMB likelihoods, following a hybrid approach similar to the 2015 one, with different approximations at low and high multipoles, and implementing several methodological and analysis refinements
- Planck 2018 results. V. CMB power spectra and likelihoods
We describe the legacy Planck cosmic microwave background (CMB) likelihoods derived from the 2018 data release The overall approach is similar in spirit to the one retained for the 2013 and 2015 data release, with a hybrid method using different approximations at low (ℓ < 30) and high (ℓ ≥ 30) multipoles, implementing several
- CMB power spectra and cosmological parameters from Planck PR4 with . . .
We present angular power spectra and cosmological parameter constraints derived from the Planck PR4 (NPIPE) maps of the cosmic microwave background NPIPE, released by the Planck Collaboration in 2020, is a new processing pipeline for producing calibrated frequency maps from Planck data
- ESA Science Technology - Planck 2013 results. XV. CMB power spectra . . .
We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters
- Planck: Measuring the Cosmic Microwave Background - IRSA
The main goal of Planck is to measure the CMB polarization better than before Planck does this by measuring the E-mode polarization with uncertainties small enough to recover harmonic content, and to detect the B-mode polarization
- Planck 2018 results V. CMB power spectra and likelihoods
We describe the legacy Planck cosmic microwave background (CMB) likelihoods derived from the 2018 data release The overall approach is similar in spirit to the one retained for the 2013 and 2015 data release, with a hybrid method using different approximations at low (ℓ < 30) and high (ℓ ≥ 30) multipoles, implementing several
- CMB spectra and likelihood code - Planck Legacy Archive Wiki
We also provide best-fit LCDM CMB power spectra from the baseline Planck TT,TE,EE+lowE+lensing The spectra must be divided by the best-fit Planck map-based calibration parameter squared, calPlanck**2, to be compared to the coadded CMB spectra
|
|
|