LILC Reduced-Foreground Map
The data made available through this page has been updated. The most recent version of this data may be accessed through https://lambda.gsfc.nasa.gov/product/wmap/current/
Eriksen et al. produced a reduced-foreground map from the first-year WMAP data using a variant of the ILC algorithm that employed a Lagrange multiplier (hence the term LILC) and also used a slightly different region selection than was used by the WMAP team. The result is a map that differs slightly from the original ILC map. The authors performed an extensive error analysis of this foreground removal approach and published the results in:
The following is the abstract of their paper:
We study the Internal Linear Combination (ILC) method presented by the Wilkinson Microwave Anisotropy Probe (WMAP) science team, with the goal of determining whether it may be used for cosmological purposes, as a template-free alternative to existing foreground correction methods. We conclude that the method does have the potential to do just that, but great care must be taken both in implementation, and in a detailed understanding of limitations caused by residual foregrounds which can still affect cosmological results. As a first step we demonstrate how to compute the ILC weights both accurately and efficiently by means of Lagrange multipliers, and apply this method to the observed data to produce a new version of the ILC map. Next we describe how to generate Monte Carlo simulations of the ILC map, and find that these agree well with the observed map on angular scales up to l~200. Finally we make two comments to the on-going debates concerning the large-scale properties of the WMAP data. First, we note that the Galactic south-eastern quadrant is associated with notably different ILC weights than the other three quadrants, possibly indicating a foreground related anisotropy. Second, we study the properties of the quadrupole and octopole (amplitude, alignment and planarity), and confirm the previously reported anomalies. Even more interestingly, we find that the l=5 mode is spherically symmetric at about 3 sigma, and that the l=6 mode is planar at the 2 sigma level. However, we also assess the impact of residual foregrounds on these statistics, and find that the ILC map is not clean enough to allow for cosmological conclusions. Alternative methods must be developed to study these issues further.
The authors have also made available a suite of simulated LILC maps for use by researchers employing this map for cosmological analyses. These maps are also available on LAMBDA.