Table 2
Estimated dipole coefficients (Cols. 2−4) and velocity magnitude (Col. 5) using the all-sky method.
| v x | v y | v z | v | ||||||
| Maps | [km s-1] | [km s-1] | [km s-1] | [km s-1] | |||||
|
|
|||||||||
| MCXC positions | |||||||||
| HFI | −188 | (147) | 384 | (414) | 441 | (494) | 614 | (662) | |
| PSM diffuse | 116 | (307) | 436 | (327) | 276 | (295) | 529 | (537) | |
| tSZ | 238 ± 37 | (232 ± 42) | −302 ± 37 | (−319 ± 41) | −239 ± 26 | (−253 ± 27) | <531 | (<549) | |
| instr. noise + CMB | 0 ± 189 | (0 ± 206) | −3 ± 195 | (−1 ± 217) | 6 ± 140 | (6 ± 143) | <543 | (<577) | |
| instr. noise + CMB + tSZ | 232 ± 187 | (229 ± 207) | −303 ± 185 | (−318 ± 207) | −234 ± 142 | (−248 ± 145) | <893 | (<929) | |
|
|
|||||||||
| Shifted positions | |||||||||
| HFI | −112 ± 214 | (171 ± 225) | 348 ± 274 | ( 304 ± 285) | 290 ± 136 | (338 ± 103) | 552 ± 221 | (591 ± 161) | |
| PSM diffuse | 73 ± 154 | (229 ± 156) | 470 ± 189 | ( 367 ± 170) | 199 ± 77 | (191 ± 73) | 553 ± 164 | (520 ± 112) | |
Notes. The values in parentheses are determinations using the more restrictive mask which includes 1321 clusters. The “HFI” row reports the results obtained for the actual data; as discussed in the text, this estimate is significantly contaminated by Galactic foregrounds and tSZ. “PSM diffuse” reports the contribution from the diffuse Galactic component found in the PSM simulation. In the rows corresponding to thermal SZ (tSZ), instrumental noise, and CMB, the first three columns report the mean and 68% confidence region error bars, while the last column indicates the 95% upper limit. The bottom part of the table refers to results found using “shifted positions” for each cluster. These are randomly selected between 30′ and 1deg from each of the MCXC clusters outside the mask region. The notation is as in the noise simulations, but it is relative to the distribution found for different choices of shifted positions. The velocity magnitude (Col. 5) represents the mean and 68% error in the distribution. These rows indicate the size of the apparent dipole that one could find using this method, even without a cosmological dipole existing.
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