Planck 2018 results. V. CMB power spectra and likelihoods. (arXiv:1907.12875v2 [astro-ph.CO] UPDATED)

Planck 2018 results. V. CMB power spectra and likelihoods. (arXiv:1907.12875v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Planck/0/1/0/all/0/1">Planck Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Aghanim_N/0/1/0/all/0/1">N. Aghanim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akrami_Y/0/1/0/all/0/1">Y. Akrami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ashdown_M/0/1/0/all/0/1">M. Ashdown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aumont_J/0/1/0/all/0/1">J. Aumont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baccigalupi_C/0/1/0/all/0/1">C. Baccigalupi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ballardini_M/0/1/0/all/0/1">M. Ballardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banday_A/0/1/0/all/0/1">A. J. Banday</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barreiro_R/0/1/0/all/0/1">R. B. Barreiro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartolo_N/0/1/0/all/0/1">N. Bartolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basak_S/0/1/0/all/0/1">S. Basak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benabed_K/0/1/0/all/0/1">K. Benabed</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernard_J/0/1/0/all/0/1">J.-P. Bernard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bersanelli_M/0/1/0/all/0/1">M. Bersanelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bielewicz_P/0/1/0/all/0/1">P. Bielewicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bock_J/0/1/0/all/0/1">J. J. Bock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bond_J/0/1/0/all/0/1">J. R. Bond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borrill_J/0/1/0/all/0/1">J. Borrill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouchet_F/0/1/0/all/0/1">F. R. Bouchet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boulanger_F/0/1/0/all/0/1">F. Boulanger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bucher_M/0/1/0/all/0/1">M. Bucher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burigana_C/0/1/0/all/0/1">C. Burigana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Butler_R/0/1/0/all/0/1">R. C. Butler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calabrese_E/0/1/0/all/0/1">E. Calabrese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cardoso_J/0/1/0/all/0/1">J.-F. Cardoso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carron_J/0/1/0/all/0/1">J. Carron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casaponsa_B/0/1/0/all/0/1">B. Casaponsa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Challinor_A/0/1/0/all/0/1">A. Challinor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiang_H/0/1/0/all/0/1">H. C. Chiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colombo_L/0/1/0/all/0/1">L. P. L. Colombo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Combet_C/0/1/0/all/0/1">C. Combet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crill_B/0/1/0/all/0/1">B. P. Crill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuttaia_F/0/1/0/all/0/1">F. Cuttaia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardis_P/0/1/0/all/0/1">P. de Bernardis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosa_A/0/1/0/all/0/1">A. de Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zotti_G/0/1/0/all/0/1">G. de Zotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delabrouille_J/0/1/0/all/0/1">J. Delabrouille</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delouis_J/0/1/0/all/0/1">J.-M. Delouis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_E/0/1/0/all/0/1">E. Di Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diego_J/0/1/0/all/0/1">J. M. Diego</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dore_O/0/1/0/all/0/1">O. Dor&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Douspis_M/0/1/0/all/0/1">M. Douspis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ducout_A/0/1/0/all/0/1">A. Ducout</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupac_X/0/1/0/all/0/1">X. Dupac</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dusini_S/0/1/0/all/0/1">S. Dusini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Efstathiou_G/0/1/0/all/0/1">G. Efstathiou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elsner_F/0/1/0/all/0/1">F. Elsner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ensslin_T/0/1/0/all/0/1">T. A. En&#xdf;lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eriksen_H/0/1/0/all/0/1">H. K. Eriksen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fantaye_Y/0/1/0/all/0/1">Y. Fantaye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Cobos_R/0/1/0/all/0/1">R. Fernandez-Cobos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finelli_F/0/1/0/all/0/1">F. Finelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frailis_M/0/1/0/all/0/1">M. Frailis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fraisse_A/0/1/0/all/0/1">A. A. Fraisse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franceschi_E/0/1/0/all/0/1">E. Franceschi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frolov_A/0/1/0/all/0/1">A. Frolov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galeotta_S/0/1/0/all/0/1">S. Galeotta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galli_S/0/1/0/all/0/1">S. Galli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ganga_K/0/1/0/all/0/1">K. Ganga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Genova_Santos_R/0/1/0/all/0/1">R. T. G&#xe9;nova-Santos</a>, et al. (108 additional authors not shown)

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.
With more realistic simulations, and better correction and modelling of
systematics, we can now make full use of the High Frequency Instrument
polarization data. The low-multipole 100×143 GHz EE cross-spectrum constrains
the reionization optical-depth parameter $tau$ to better than 15% (in
combination with with the other low- and high-$ell$ likelihoods). We also
update the 2015 baseline low-$ell$ joint TEB likelihood based on the Low
Frequency Instrument data, which provides a weaker $tau$ constraint. At high
multipoles, a better model of the temperature-to-polarization leakage and
corrections for the effective calibrations of the polarization channels
(polarization efficiency or PE) allow us to fully use the polarization spectra,
improving the constraints on the $Lambda$CDM parameters by 20 to 30% compared
to TT-only constraints. Tests on the modelling of the polarization demonstrate
good consistency, with some residual modelling uncertainties, the accuracy of
the PE modelling being the main limitation. Using our various tests,
simulations, and comparison between different high-$ell$ implementations, we
estimate the consistency of the results to be better than the 0.5$sigma$
level. Minor curiosities already present before (differences between $ell$<800
and $ell$>800 parameters or the preference for more smoothing of the $C_ell$
peaks) are shown to be driven by the TT power spectrum and are not
significantly modified by the inclusion of polarization. Overall, the legacy
Planck CMB likelihoods provide a robust tool for constraining the cosmological
model and represent a reference for future CMB observations. (Abridged)

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.
With more realistic simulations, and better correction and modelling of
systematics, we can now make full use of the High Frequency Instrument
polarization data. The low-multipole 100×143 GHz EE cross-spectrum constrains
the reionization optical-depth parameter $tau$ to better than 15% (in
combination with with the other low- and high-$ell$ likelihoods). We also
update the 2015 baseline low-$ell$ joint TEB likelihood based on the Low
Frequency Instrument data, which provides a weaker $tau$ constraint. At high
multipoles, a better model of the temperature-to-polarization leakage and
corrections for the effective calibrations of the polarization channels
(polarization efficiency or PE) allow us to fully use the polarization spectra,
improving the constraints on the $Lambda$CDM parameters by 20 to 30% compared
to TT-only constraints. Tests on the modelling of the polarization demonstrate
good consistency, with some residual modelling uncertainties, the accuracy of
the PE modelling being the main limitation. Using our various tests,
simulations, and comparison between different high-$ell$ implementations, we
estimate the consistency of the results to be better than the 0.5$sigma$
level. Minor curiosities already present before (differences between $ell$<800
and $ell$>800 parameters or the preference for more smoothing of the $C_ell$
peaks) are shown to be driven by the TT power spectrum and are not
significantly modified by the inclusion of polarization. Overall, the legacy
Planck CMB likelihoods provide a robust tool for constraining the cosmological
model and represent a reference for future CMB observations. (Abridged)

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