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Likelihood Code



We make available on this page data products related to the cosmological parameters analysis of the SPT+Planck 2500 square-degrees lensing measurement presented in Simard et al. (2017), based on results presented in Omori et al. (2017). The lensing bandpowers used for the cosmological analysis cover the lensing angular multipole range 50 <= L <= 1991; chains can be run within the CosmoMC infrastructure with the likelihood files provided below.

If you have any questions regarding this data set or its use, please contact Gabrielle Simard (simard_dot_gabrielle_at_gmail_dot_com).




Individual figures are available in PDF format here. Below we show a couple of example figures.

SPT + Planck lensing bandpowers along with earlier lensing estimates from the SPT-SZ survey (van Engelen et al. 2012) and recent lensing bandpowers obtained from temperature and polarization measurements from SPTpol (Story et al. 2015). Also plotted are the most recent lensing autospectrum measurements from BICEP-Keck (BICEP/Keck Collaboration 2016) Planck (Planck Collaboration 2016), Polarbear (Polarbear Collaboration 2014} and ACTpol (Sherwin et al. 2016), and a prediction for the lensing power spectrum using the best-fit cosmological parameters from the Planck TT + lowP + lensing cosmology.

Lensing constraints on sigma8 and Omega_m from optical surveys (KiDS-450, CFHTLens, DES) and CMB measurements (ACTPol, Planck full sky, SPT + Planck 2500 square degrees). Also shown are constraints from the Planck primary CMB power spectra. This work is in good agreement with both CMB and optical surveys.




Bandcenters, bandpowers, and bandpower errors for plotting are provided in a text file here.

Bandpowers and uncertainties are given in [L_b(L_b + 1)]^2 /2/pi units. Each row is one ell-bin. The columns are (1) bin number, (2) L_min, (3) L_max, (4) center of bin, (5) estimated clpp bandpower, (6) sigma on the estimated clpp bandpower, (7) lensing amplitude compared to the base_plikHM_TT_lowTEB_lensing cosmology.

These bandpowers are foreground subtracted, where the lensing foreground model has been taken from van Engelen et al. (2014) (astro-ph/1310.7023). Note that the lensing bandpowers plotted in Fig. 5 of Omori et al. (2017) are not foreground subtracted, whereas the ones in Fig. 1 of Simard et al. (2017) are.


Likelihood Code


The attached directory can be added to the November 2016 version of CosmoMC. The CosmoMC dataset contains the foreground template removed lensing bandpowers, the corresponding lensing bandpowers covariance matrix and the lensing linear corrections. The appropriate batch files are provided as well. A simple README file provides details on where to place these files within a working CosmoMC environnement. No recompilation of CosmoMC is required, as this likelihood uses a generic Gaussian likelihood structure existing within CosmoMC.

sptplanck_lenslike v1.1: December 7th, 2017. Initial version to be released with the arXiv submission.




The chains computed in the context of this analysis are available here. The directory base.zip containts chains in the LCDM model for the SPT+Planck lensing data only and in combination with the Planck TT + lowP likelihoods. Each directory base_X.zip contains chains in the LCDM model with the X parameter(s) varied for the SPT+Planck lensing data in combination with the Planck TT + lowP likelihoods.

The chains samples in the root.txt files contain the burn-in phase; the first 30% of the rows should be removed. The format of each row in the root.txt files follows the habitual CosmoMC format, where the first column corresponds to the weight, the second column to the -log(likelihood) and the following columns to the value of the primary and derived parameters listed in the corresponding root.paramnames file.

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Last update:


September 7, 2011