Joint Planck PR1 + WMAP CMB Map

Joint Planck and WMAP9 CMB Map Reconstruction using LGMCA

The LGMCA method has been used to reconstruct the Cosmic Microwave Background (CMB) image from WMAP 9 year and Planck-PR1 data. Based on the sparse modeling of signals - a framework recently developed in applied mathematics - the proposed component separation method is well-suited for the extraction of foreground emissions. A joint WMAP9 year and Planck PR1 CMB has been reconstructed for the first time and produce a very high quality CMB map, especially on the galactic center where it is the most difficult due to the strong foreground emissions of our Galaxy. This webpage provides some comparisons between the PR1 and WPR1 maps and codes to recompute the map in the spirit of reproducible research. 

Joint WMAP9 and Planck PR1 CMB map
First joint joint reconstruction from WMAP9 and Planck PR1 data with LGMCA

Comparison with other CMB Planck PR1 maps

CMB maps from Planck PR1
CMB maps from Planck PR1

Comparison on Galactic Center

Galactic center region, centered at (l,b)=(37.7,0). Top, PR1 NILC and SEVEM CMB maps, and bottom, PR1 SMICA and WPR1 LGMCA CMB maps.
Galactic center region, centered at (l,b)=(37.7,0). Top, PR1 NILC and SEVEM CMB maps, and bottom, PR1 SMICA and WPR1 LGMCA CMB maps.

Quality maps

Quality maps

It is usually hard to derive a discriminative criterion from real data. For that purpose, the quality map measures an excess of power in the estimated CMB map in the wavelet domain with the respect to the expected power of the CMB. The expected CMB power is computed from the Planck best-fit power spectrum assuming a fiducial cosmology.

The LGMCA CMB map does not contain noticeable tSZ residual

Coma cluster area. PR1 LGMCA CMB map and HFI-217 GHz map.

Difference map between HFI-217GHz and CMB maps, respectively PR1 NILC, SEVEM, SMICA and WPR1 LGMCA. As the SZ vanishes at 217GHz, the presence of residuals of tSZ in the difference reveals a tSZ contamination in the estimated CMB map.

Power Spectra

 

Left, estimated power spectrum of the WPR1 LGMCA map (red) and official PR1 power spectrum (green). The solid black line is the Planck-only best-fit C_\ell provided by the Planck consortium. Right, power spectrum in logarithmic scale. Error bars are set to 1 sigma.
Left, difference between the power spectrum estimated from the WPR1 LGMCA map (red) (resp. official PR1 power spectrum (green)) and the Planck-only best-fit provided by the Planck consortium. Right, difference between the estimated and theoretical power spectra in logarithmic scale. Error bars are set to 1 sigma.
Left, difference between the power spectrum estimated from the WPR1 LGMCA map (red) (resp. official PR1 power spectrum (green)) and the Planck-only best-fit provided by the Planck consortium. Right, difference between the estimated and theoretical power spectra in logarithmic scale. Error bars are set to 1 sigma.

This clean and truly full-sky estimate of the CMB map is a very good candidate for galactic studies. Being free of noticeable remainings of thermal SZ, it will be helpful for kinetic SZ studies. As well, following the philosophy of reproducible research, the LCS makes available all the codes used to estimate and evaluate the CMB map.

Reference

Joint WMAP9 and Planck PR1 Products

The same products has also been computed by applying LGMCA from Planck only data.

Reproducible Research

Reproducible research philosophy consists in providing codes and scripts that have used to provided the results.