Planck 2013 results. XVI. Cosmological parameters
Citations
10,728 citations
9,720 citations
4,688 citations
3,438 citations
2,228 citations
References
16,838 citations
16,674 citations
14,295 citations
14,013 citations
13,884 citations
"Planck 2013 results. XVI. Cosmologi..." refers methods in this paper
...Since the pioneering work of Peebles (1968) and Zeldovich et al. (1969), which identified the main physical processes involved in recombination, there has been significant progress in numerically modelling the many relevant atomic transitions and processes that can affect the details of the recombination process (Hu et al. 1995; Seager et al. 2000; Wong et al. 2008; Hirata & Switzer 2008; Switzer & Hirata 2008; Rubino-Martin et al. 2009; Grin & Hirata 2010; Chluba & Thomas 2011; Ali-Haimoud et al. 2010; Ali-Haimoud & Hirata 2011)....
[...]
...However, the recombination history can be computed even more rapidly by using the simple effective three-level atom model developed by Seager et al. (2000) and implemented in the recfast code8, with appropriately chosen small correction functions calibrated to the full numerical results (Wong et al. 2008; Rubino-Martin et al. 2009; Shaw & Chluba 2011)....
[...]
...We check that the spread in the means between chains is small compared to the standard deviation, using the standard Gelman and Rubin (Gelman & Rubin 1992) criterion 12As described in Planck Collaboration XV (2013), we use spectra calculated on different masks to isolate the contribution of Galactic cirrus at each frequency, which we subtract from the 143× 143, 143× 217 and 217× 217 power spectra (i.e., the correction is applied to the power spectra, not in the map domain)....
[...]
...We check that the spread in the means between chains is small compared to the standard deviation, using the standard Gelman and Rubin (Gelman & Rubin 1992) criterion 12As described in Planck Collaboration XV (2013), we use spectra calculated on different masks to isolate the contribution of…...
[...]
...Although the main processes that lead to recombination at z ≈ 1090 are well understood, cosmological parameters from Planck can be sensitive to sub-percent differences in the ionization fraction xe (Hu et al. 1995; Lewis et al. 2006; Planck Collaboration: Cosmological parameters Rubino-Martin et al. 2009; Shaw & Chluba 2011)....
[...]