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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20150319T103000
DTEND;TZID=Atlantic/Canary:20150319T113000
UID:iactalks-766
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/766
CREATED:2015-03-19T10:30:00+00:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY: Probing the Dark Flow signal in WMAP 9 yr and PLANCK cosmic microw
 ave background maps.
DESCRIPTION: Probing the Dark Flow signal in WMAP 9 yr and PLANCK cosmic mi
 crowave background maps.\nDr. Fernando Atrio Barandela\n\nThe ``dark flow'
 ' dipole is a statistically significant dipole found at the position of ga
 laxy clusters in filtered maps of Cosmic Microwave Background (CMB) temper
 ature anisotropies. The dipole measured in  WMAP 3, 5 and 7 yr data releas
 es was roughly aligned with the all-sky CMB dipole and correlated with clu
 ster X-ray luminosity. We analyzed the final  WMAP 9 yr and the first  Pla
 nck data releases using a catalog of 980 clusters outside the Kp0 mask to 
 test our earlier findings. The dipoles measured on these new data sets are
  fully compatible with our earlier estimates, being similar in amplitude a
 nd direction to our previous results and in disagreement with the results 
 of an earlier study by the  Planck Collaboration. Further, in  Planck data
  dipoles are independent of frequency, ruling out the Thermal Sunyaev-Zeld
 ovich as the source of the effect. The signal is dominated by the most mas
 sive clusters, with a statistical significance better than 99%, slightly l
 arger than in  WMAP.  Since both data sets differ in foreground contributi
 ons, instrumental noise and other systematics, the agreement between WMAP 
 and Planck dipoles argues against them being due to systematic effects in 
 either of the experiments.
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