The tension between the best fit parameters derived by the Planck team and a number of other astronomical measurements suggests either systematics in the astronomical measurements , systematics in the Planck data , the need for new physics , or a combination thereof .
We re-analyze the Planck data and find that the 217 \text { GHz } \times 217 \text { GHz } detector set spectrum used in the Planck analysis is responsible for some of this tension .
We use a map-based foreground cleaning procedure , relying on a combination of 353 GHz and 545 GHz maps to reduce residual foregrounds in the intermediate frequency maps used for cosmological inference .
For our baseline data analysis , which uses 47 % of the sky and makes use of both 353 and 545 GHz data for foreground cleaning , we find the \Lambda CDM cosmological parameters \Omega _ { c } h ^ { 2 } = 0.1170 \pm 0.0025 , n _ { s } = 0.9686 \pm 0.0069 , H _ { 0 } = 68.0 \pm 1.1 \mathrm { km } ~ { } \mathrm { s } ^ { -1 } \mathrm { Mpc } ^ { -1 } , \Omega _ { b } h ^ { 2 } = 0.02197 \pm 0.00026 , \ln 10 ^ { 10 } A _ { s } = 3.082 \pm 0.025 , and \tau = 0.090 \pm 0.013 .
While in broad agreement with the results reported by the Planck team , these revised parameters imply a universe with a lower matter density of \Omega _ { m } = 0.302 \pm 0.015 , and parameter values generally more consistent with pre-Planck CMB analyses and astronomical observations .
We compare our cleaning procedure with the foreground modeling used by the Planck team and find good agreement .
The difference in parameters between our analysis and that of the Planck team is mostly due to our use of cross-spectra from the publicly available survey maps instead of their use of the detector set cross-spectra which include pixels only observed in one of the surveys .
We show evidence suggesting residual systematics in the detector set spectra used in the Planck likelihood code , which is substantially reduced for our spectra .
Using our cleaned survey cross-spectra , we recompute the limit on neutrino species and find N _ { \text { eff } } = 3.34 \pm 0.35 .
We also recompute limits on the n _ { s } - r plane , and neutrino mass constraints .