Cosmic Microwave Background Polarization and Temperature Power Spectra Estimation Using Linear Combination of WMAP 5 Year Maps

We estimate cosmic microwave background (CMB) polarization and temperature power spectra using Wilkinson Microwave Anisotropy Probe (WMAP) 5 year foreground contaminated maps. The power spectrum is estimated by using a model-independent method, which does not utilize directly the diffuse foreground...

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Bibliographic Details
Published in:The Astrophysical journal 2010-05, Vol.714 (1), p.840-851
Main Authors: Samal, Pramoda Kumar, Saha, Rajib, Delabrouille, Jacques, Prunet, Simon, Jain, Pankaj, Souradeep, Tarun
Format: Article
Language:English
Subjects:
ANISOTROPY
Astronomy
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BACKGROUND RADIATION
COMPUTERIZED SIMULATION
Cosmology and Extra-Galactic Astrophysics
DATA ANALYSIS
Earth, ocean, space
ELECTROMAGNETIC RADIATION
Exact sciences and technology
MICROWAVE RADIATION
Physics
POINT SOURCES
POLARIZATION
RADIATION SOURCES
RADIATIONS
RELICT RADIATION
Sciences of the Universe
SIMULATION
SPECTRA
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Summary:We estimate cosmic microwave background (CMB) polarization and temperature power spectra using Wilkinson Microwave Anisotropy Probe (WMAP) 5 year foreground contaminated maps. The power spectrum is estimated by using a model-independent method, which does not utilize directly the diffuse foreground templates nor the detector noise model. The method essentially consists of two steps: (1) removal of diffuse foregrounds contamination by making linear combination of individual maps in harmonic space and (2) cross-correlation of foreground cleaned maps to minimize detector noise bias. For the temperature power spectrum we also estimate and subtract residual unresolved point source contamination in the cross-power spectrum using the point source model provided by the WMAP science team. Our TT, TE, and EE power spectra are in good agreement with the published results of the WMAP science team. We perform detailed numerical simulations to test for bias in our procedure. We find that the bias is small in almost all cases. A negative bias at low l in TT power spectrum has been pointed out in an earlier publication. We find that the bias-corrected quadrupole power (l(l + 1)Cl /2π) is 532 μK2, approximately 2.5 times the estimate (213.4 μK2) made by the WMAP team.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/714/1/840