(Rajib Saha,Pankaj Jain,Tarun Souradeep, astro-ph/0508383)

A Blind Estimation of AngularPower Spectrum of CMB

Anisotropy from WMAP

IIT Kanpur + IUCAA

Saha, Jain,Souradeep 2005(astro-ph/0508383)

Independent, self contained analysis of WMAP multi-frequency maps Blind estimation : no extraneous foreground info. ! I.e., free of uncertainty of foreground modeling

Black: IITK+IUCAA

Red : WMAP team

Saha, Jain,Souradeep 2006(preliminary)

Model free Foreground removalModel free Foreground removalC F n

lm l lm l lm lma B a B a a

Foreground cleaned map:

• Linear combinations of maps of different frequency channels, i.

1

ii ni lm

lm l ii l

aa w

B

• CMB anisotropy is achromatic :( ) constantC i

lma

Such that CMB signal is untouched

in the final map ) 1

1

ni

i

ilw

* [ ][ ][ ]Tl lm lm lC a a W C W • Determine weights

that minimize total power

[ ][ ][ ]

[ ][ ][ ]

TT l

l Tl

C eW

e C e

[ ] 1 1 .. .. 1e

• For each frequency channel, i :

1 DA 2 DA

1 DA

2 DA4 DA

(K,Ka)+Q1+V2+W12= (C13,CA13)(K,Ka)+Q1+V2+W13= (C14,CA14)(K,Ka)+Q1+V2+W14= (C15,CA15)(K,Ka)+Q1+V2+W23= (C16,CA16)(K,Ka)+Q1+V2+W24= (C17,CA17)(K,Ka)+Q1+V2+W34= (C18,CA18)

(K,Ka)+Q2+V1+W12= (C19,CA19)(K,Ka)+Q2+V1+W13= (C20,CA20)(K,Ka)+Q2+V1+W14= (C21,CA21)(K,Ka)+Q2+V1+W23= (C22,CA22)(K,Ka)+Q2+V1+W24= (C23,CA23)(K,Ka)+Q2+V1+W34= (C24,CA24)

(K,Ka)+Q2+V2+W12= (C7,CA7)(K,Ka)+Q2+V2+W13= (C8,CA8) (K,Ka)+Q2+V2+W14= (C9,CA9)(K,Ka)+Q2+V2+W23= C10,CA10)(K,Ka)+Q2+V2+W24= (C11,CA11)(K,Ka)+Q2+V2+W34= (C12,CA12)

(K,Ka)+Q1+V1+W12= (C1,Ca1)(K,Ka)+Q1+V1+W13= (C2,CA2)(K,Ka)+Q1+V1+W14= (C3,CA3)(K,Ka)+Q1+V1+W23= (C4,CA4)(K,Ka)+Q1+V1+W24= (C5,CA5)(K,Ka)+Q1+V1+W34= (C6,CA6)

48 CLEANED MAPS

One of the 40 cleaned maps obtained from combing the 10 difference assemblies of WMAP

24 Cross-correlation power spectra

Cross-correlation power spectra without correcting for point source residuals

WMAP team Our method

Residual power from unresolved point source

IIT Kanpur + IUCAA

Saha, Jain,Souradeep 2005(astro-ph/0508383)

Independent, self contained analysis of WMAP multi-frequency maps Blind estimation : no extraneous foreground info. ! I.e., free of uncertainty of foreground modeling

Black: IITK+IUCAA

Red : WMAP team

(48.3 1.2, 544 17)

(48.8 0.9, 546 10)

(41.7 1.0, 419.2 5.6)

(41.0 0.5, 411.7 3.5)

(74.10.3, 219.80.8)

(74.7 0.5, 220.1 0.8

Peaks of the angular power spectrum

Saha, Jain,Souradeep 2006(preliminary)

Correlation matrix for the Binned power spectrum

'

2 2'( ) ( )

b b

b b

C C

C C

30Ghz 44Ghz

77Ghz 100Ghz

143Ghz 217Ghz

Combination ofPlanck Channel maps

Input randomrealization of CMB map(in k unit)

Recovered foreground cleaned map(in mk unit)

Retaining beam and pixel window smoothing

Difference between input & recovered maps

No beam and pixel window smoothing

Difference between input & recovered maps

BiPS Diagnostics of cleaned maps

FiltersBIPS: filter ABIPS: filter B

C6: clean C9: cleaner

A B

Saha,Hajian, Souradeep, Jain

(in progress )

Maps from Saha et al. astro-ph/0508383 (see poster)

Anisotropic Noise• Simplest case:

ijiijC 2

lmlmlm

N

mlmL

nYfnnC

f

)ˆ()ˆ,ˆ(

|| 2

Anisotropic Noise• Simplest case:

ijiijC 2