Table 24.
Amplitude and direction of the low-ℓ dipole-asymmetry signal determined from the QML analysis for the range ℓ = 2 − 64.
| Direction | ||
|---|---|---|
| Data | Amplitude | (l, b) [Deg] |
| 2015 TT | ||
| Commander...... |
 |
(213, −26) ± 28 |
| NILC...... |
 |
(209, −25) ± 28 |
| SEVEM...... |
 |
(211, −25) ± 28 |
| SMICA...... |
 |
(213, −26) ± 28 |
| 2018 TT | ||
| Commander...... |
 |
(221, −22) ± 31 |
| NILC...... |
 |
(221, −24) ± 31 |
| SEVEM...... |
 |
(221, −22) ± 31 |
| SMICA...... |
 |
(221, −22) ± 31 |
| 2018 EE | ||
| Commander...... |
 |
(192, 3) ± 103 |
| NILC...... |
 |
(267, −5) ± 105 |
| SEVEM...... |
 |
(245, 37) ± 105 |
| SMICA...... |
 |
(215, 11) ± 108 |
| 2018 TT,EE | ||
| Commander...... |
 |
(217, −18) ± 29 |
| NILC...... |
 |
(225, −23) ± 31 |
| SEVEM...... |
 |
(219, −17) ± 31 |
| SMICA...... |
 |
(221, −19) ± 31 |
| 2018 TT,TE,EE | ||
| Commander...... |
 |
(218, −19) ± 29 |
| NILC...... |
 |
(225, −23) ± 31 |
| SEVEM...... |
 |
(219, −17) ± 31 |
| SMICA...... |
 |
(221, −19) ± 31 |
Notes. The errors are calculated from the FFP10 simulations. Recall that the expectation for noise-free Gaussian skies (the “cosmic variance of dipole modulation”, see Eq. (50) in PCIS15) corresponds to an amplitude of approximately 3%. The polarization data on their own show no evidence of modulation, and the addition of polarization has very little effect on the temperature asymmetry signal.
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