Table 3
Quadrupole (ℓ = 2) power and corresponding probability of the quadrupole power being so low.
| Map | Quadrupole | Probability | Expected |
| power | theoretical | ||
| (μK2) | (%) | value (μK2) | |
|
|
|||
| 1) | |||
| W7 best fit | 210.3 | 3.0 | |
| W9 best fit | 157.7 | 1.6 | |
|
|
|||
| 2) | |||
| TOH W1 | 203.2 | 2.8 | |
| ILC W3 | 250.5 | 4.4 | |
| ILC W5 | 246.9 | 4.3 | |
| ILC W7 | 245.4 | 4.2 | |
| ILC W9 | 248.2 | 4.3 | |
| TOH W1 (inp) | 154.5 | 1.5 | 1161.3 |
| ILC W3 (inp) | 102.1 | 0.58 | |
| ILC W5 (inp) | 117.0 | 0.80 | |
| Dela W5 (inp) | 112.7 | 0.73 | |
| ILC W7 (inp) | 115.4 | 0.78 | |
| ILC W9 (inp) | 124.7 | 0.93 | |
|
|
|||
| 3) ISW subtracted | |||
| (measured amplitude | |||
| 2MASS + NVSS) | |||
| TOH W1 − ISW | 182.5 | 4.9 | |
| ILC W3 − ISW | 189.1 | 5.3 | |
| ILC W5 − ISW | 194.0 | 5.6 | |
| ILC W7 − ISW | 189.6 | 5.4 | |
| ILC W9 − ISW | 194.8 | 5.7 | |
| TOH W1 (inp) − ISW | 129.8 | 2.4 | 800.3 |
| ILC W3 (inp) − ISW | 60.7 | 0.41 | |
| ILC W5 (inp) − ISW | 77.6 | 0.73 | |
| Dela W5 (inp) − ISW | 71.5 | 0.60 | |
| ILC W7 (inp) − ISW | 71.9 | 0.61 | |
| ILC W9 (inp) − ISW | 81.7 | 0.83 | |
|
|
|||
| 4) | |||
| W3-ISW | |||
| 2MASS only | 600.7 | 19.8 | 1251.8 |
| FP10 | |||
Notes. 1) For the best fit of WMAP 7th year and 9th year data. 2) For 11 different CMB maps. 3) After subtraction of the reconstructed ISW signal due to 2MASS and NVSS galaxies. 4) Results from FP10 (Francis & Peacock 2010, bottom row). Probabilities in this work are calculated using the expected theoretical value given in the last column taken from WMAP 9 best-fit results, whereas FP10 use best-fit results from WMAP 3.
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