anomalies of low multipoles of wmap and planck missions: what are they ? oleg verkhodanov special...

Anomalies of low multipoles of WMAP and Planck missions: what are they ?

Oleg Verkhodanov Special astrophysical observatory of Russian Academy of Sciences

Wilkinson Microwave Anisotropy Probe (WMAP, NASA)

5 frequencies:23, 33, 41, 61, 94 GHz

Best determination of cosmological parameters in 2011 !

2001-2011

Planck mission, ESA

Low Frequency Instrument: 30,44,70HFI: 100, 143, 217, 353, 545, 857 GHz

Zeldovich-Sunyaev effect

3) Gravitational waves in the B-mode of polarization ?

2010-20131)

2)

Observations

Data analysis of CMB

Registration: time odered data: T(t)=T(l,b) Pixelization: map-making and restoration data in pixels Component separation Multipole analysis Pixel statistics of the CMB map Angular power spectrum analysis and determination of cosmological parameters

Component separation

WMAP observational bands

Component separation:Signal = (CMB + Synchrotron+dust+FreeFree+radiosouces)*Beam + Noise

Two basic properties of CMB:1) Black body emission — same temperature at all wavelengthes;2) Correlation of CMB and foregrounds should be close to zero: because CMB is a random gaussian process

The maps

WMAP 9, Lmax=150(Hinshaw et al., 2012)

Planck, Lmax=150

Planck collaboration, 2013

Lmax = 150

Masks

Angular power spectrum of CMB

The spectra

WMAP 9,2012

Planck2013

Let us go to data

Legacy Planck Archive (LPA)http://www.sciops.esa.int/index.php?page=Planck_Legacy_Archive&project=planck

1) 4 CMB maps2) maps at observational bands (30, 44, 70, 100, 143, 217, 353,545, 857 GHz)3) CO emission maps 4) Maps of dust5) Maps of galactic low frequency emission (synchrotron + free-free)6) Zodiac light maps7) Maps of gravitational lensing8) y-comptonization maps9) Masks

Planck maps

Observational frequency maps

30GHz 44GHz 70GHz

100GHz 143GHz 217GHz

353GHz 545GHz 857GHz

Planck maps: component separation

Legacy Planck Archive (LPA)http://www.sciops.esa.int/index.php?page=Planck_Legacy_Archive&project=planck

Maps WMAP9 of Planck mission

Power spectrum

Cosmological results: WMAP9 and Planck data

http://lambda.gsfc.nasa.gov

No revolution...

CMB for neutrino parameters

1)

2)

3)

4)

«Bad» spots...

WMAP CMB anomalies

1) Cold Spot2) Axis of Evil3) Primirdial non-gaussinity (low limit by Planck data)4) Violation of the power spectrum parity5) Asymmetry 'North — South' in galactic coordinate system

6) New anomaly: too low amplitude of low harmonics

Let us look at some anomalies...

Cold Spot

Part of octupole

Cold Spot < -5sigma

1) Huge Sachs-Wolfe effect (Rudnick et al, 2007)2) Anistropic expansion (Jaffe et al., 2005)3) Topological defect [texture] (Cruz et al., 2007,2008, Planck 2013 ?)4) Artifact ?5) Galactic phenomena (M.Hansen et al., 2012)

CMB NVSSRadio sources

(Rudnick et al., 2007)

Axis of Evil

Problems of WMAP quadrupole

AmplitudeAxis of Evil: planarity + alignment(Land & Magueijo, 2005)

What is the reason ?1) Component separation (Doroshkevich, Verkhodanov, 2010)2) Kouper Belt (Hansen et al. 2011)3) Moving in Local Group of galaxies? (Tegmark et al., 2004)4) Something else...5) It is absent...

Axis of Evil(Planck data)

Copi et al., arXiv:1311.4562: direction of our motion exists

Primordial non-gaussianity ?

Primordial non-gaussianity ?

1) Obtained with bispectrum2) Low multimoples anomalies exist

Low multipoles in Planck

L=2 L=3 L=4

L=5 L=6 L=7

L=8 L=9 L=10

Low multipoles in WMAP

L=2 L=3 L=4

L=5 L=6 L=7

L=8 L=9 L=10

Asimmetry North-South

Planck CMB CMB and Bianchi 7h anisotropy model ?

Violation of power spectrum parity

Power spectrum and separate multipoles

SMICA

SEVEM

NILC

WMAP9

Maps, L<=100

Power spectrum C(l), l<=50

Planck, WMAP

-

=

Planck, SMICAWMAP

L=5

-

=

Planck, SMICAWMAP

L=7

-

=

Planck, SMICAWMAP

L=11

Planck, SMICA

WMAP

L=70

NILC

SEVEM

Cosmology with Suynaev-Zeldovich effect ?

Problem with cluster parameters ?Planck: optic and mm/submm centers differ from X-ray.

Missed sources in the Planck data: radio sources at sigma level < 3 sigma

Awaited source of the secondary anistropy: >20000 radio galaxies ?

0015+0501

0225+0506

0226+0512

0302+0456

0311+0507, z=4.514

0427+0457 1113+0436RG in cluster ?

SZ-effect

30 44 70 100 143 217 353 545 CMB

0702+0440

0748+0452

0756+0506

0924+0508

1022+0450

Observational channel of 217 GHz: what is unusual ?

Data of 217 GHz: what is unusual ?

1) Very close to CMB map outside the Galactic plane, but let us remember WMAP bands:

Data of 217 GHz: what is unusual ?

1) Close to the CMB map

2) Calibration problem ? (Spergel et al., arXiv:1312.3313)

If remove the 217 GHz channel, then it can be obtained accurate restoration of the WMAP cosmology

Stephen Hawking «stamp» :)

WMAP

Planck,SMICA

What have we wait for ? and what to do ?

1) WMAP and Planck data have practically the same low multipole anomalies

2) The difference of power spectra looks like one due to systematic effects of maps prepartion

3) We are waiting for a new release in June 2014: Maps of temperature anisotropy and polarization

4) Data are comparatively good (in resolution and sensetivity) when we take into account strangeness

Summary

Корреляция: (Chаnnel — CMB) * CMB

Карты(и их характеристика)

Карты

SMICA

SEVEM

NILC

Фазы

Фазы

SEVEM

NILC

SMICA

Фазы, L<=4096

SEVEMSMICA

Фазы, L<=256

SEVEMSMICA

Чтобы не забыть...

(Chiang et al. 2003)

WMAP:2 картыТегмарка

Космологические результаты WMAP9 и Planck

http://lambda.gsfc.nasa.gov

Революции нет ... Так это прекрасно !

Приложения

Мультипольное разложение

Приложение 1.

Multipole expansion

L = 2 (quadrupole) L =3 (octupole)

L = 4 L = 5

L=2 (2,0)

(2,1) (2,2)

=

+ +

+

Квадруполь

Октуполь

= +

+ +

(3,0)

(3,1) (3,2) (3,3)

L=3

Для простейшей инфляционной модели

Возмущения плотности -> возмущения CMB:

Первичная негауссовость

Приложение 2: негауссовость