The Scalar Perturbation Spectral Index n(s): WMAP Sensitivity to Unresolved Point Sources
Precision measurement of the scalar perturbation spectral index, [image], from the Wilkinson Microwave Anisotropy Probe (WMAP) temperature angular power spectrum requires the subtraction of unresolved point-source power. Here we reconsider this issue, attempting to resolve inconsistencies found in t...
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| Published in: | The Astrophysical journal 2008-11, Vol.688 (1), p.1-11 |
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| Main Authors: | , , , , |
| Format: | Article |
| Language: | eng |
| Online Access: | Get full text |
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| Summary: | Precision measurement of the scalar perturbation spectral index, [image], from the Wilkinson Microwave Anisotropy Probe (WMAP) temperature angular power spectrum requires the subtraction of unresolved point-source power. Here we reconsider this issue, attempting to resolve inconsistencies found in the literature. First, we note a peculiarity in the WMAP temperature likelihood's response to the source correction: cosmological parameters do not respond to increased source errors. An alternative and more direct method for treating this error term acts more sensibly, and also shifts [image] by [image]0.3 S closer to unity. Second, we re-examine the source fit used to correct the power spectrum. This fit depends strongly on the Galactic cut and the weighting of the map, indicating that either the source population or masking procedure is not isotropic. Jackknife tests appear inconsistent, causing us to assign large uncertainties to account for possible systematics. Third, we note that the WMAP team's spectrum was computed with two different weighting schemes: uniform weights transition to inverse noise variance weights at [image]. The fit depends on such weighting schemes, so different corrections apply to each multipole range. For the Kp2 mask used in cosmological analysis, we prefer source corrections [image] [mu]K(2) for uniform weighting and [image] [mu]K(2) for [image] weighting. Correcting WMAP's spectrum correspondingly, we compute cosmological parameters with our alternative likelihood, finding [image] and [image]. This [image] is only 1.8 S from unity, compared to the [image]2.6 S WMAP 3 year result. Finally, an anomalous feature in the source spectrum at [image] remains in the 3 year data, most strongly associated with the W band. We note the implications of these results for the 5 year data. |
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| ISSN: | 0004-637X 1538-4357 |