Systematic effects in CMB data of ESA’s satellite Planck Tarun Souradeep (IUCAA, Pune) & Francois...
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Transcript of Systematic effects in CMB data of ESA’s satellite Planck Tarun Souradeep (IUCAA, Pune) & Francois...
Systematic effects Systematic effects in CMB data of in CMB data of
ESA’s satellite PlanckESA’s satellite Planck
Tarun Souradeep (IUCAA, Pune)
& Francois Bouchet (IAP, Paris)
CEFIPRA mid-term presentation (Mussoorie, Oct. 27, 2007)
Quantum fluctuations
super adiabatic amplified by
inflation (rapid expansio
n)
Galaxy & Large sc
ale
Structure fo
rmation
Via gravitational insta
bility
Early Universe
Present Universe
The Cosmic screen
Cosmic Microwave backgroundCosmic Microwave background
George SmootJohn Mather
COBE
Cosmic Background Explorer
First detection of CMB
anisotropy (1992)
2003 Second NASA CMB Satellite mission
First NASA CMB Satellite mission
-200 K < T < 200 KTrms ¼ 70 K
CMB temperature Tcmb = 2.725 K
Saha et al 2006
WMAP map of CMB anisotropy
Hence, a powerful tool for constraining cosmological parameters.
Fig. M. White 1997
The Angular power spectrum of CMB anisotropy dependssensitively on Cosmological parameters
lC
Multi-parameter Joint likelihood (MCMC)
NASA/WMAP science team
Total energy density
Baryonic matter density
Dawn of Precision cosmology !!
Dark energy density
Good old Cosmology, … New trend !
Underlying statistics: Gaussian
Power spectrum : ‘Nearly’ Scale invariant /scale free form
Spin characteristics: (Scalar) Density perturbations
Type of scalar perturbation: Adiabatic -- no entropy fluctuations
The nature of initial/primordial perturbations
The Background universe Homogeneous & isotropic space: Cosmological principle
Flat (Euclidean) Geometry … but global topology?
… but are there features ?
… cosmic (Tensor) Gravity waves ?
Early Universe in CMB
CMB Task force report 2005
Timeline of CMB researchWMAP-1yr
nowWMAP-3yr
WMAP-8yrPlanck (ESA)
Next Gen. spaceCMBPOL/Sampan
Angular power spectrum
estimation : Evading modeling
systematics in foreground removal
1. CMB anisotropy power spectrum using linear combinations of WMAP maps Authors: Rajib Saha, Simon Prunet, Pankaj Jain, Tarun Souradeep Submitted to Phys. Rev D. (under review) arXiv:0706.3567
2. Angular power spectrum of CMB anisotropy from WMAP Authors: Tarun Souradeep (IUCAA), Rajib Saha (IITK, IUCAA), Pankaj Jain (IITK) New Astron.Rev. 50 (2006) 854-860
3. A re-analysis of the 3-year WMAP temperature power spectrum & likelihood Authors: (IUCAA+IITK )+ 4 international groups (JPL, Oslo, UIUC,UCDavis)Astrophys.J. 656 (2007) 641-652
1 DA 2 DA
1 DA
2 DA4 DA
WMAP multi-frequency maps
Template Based foreground removal
Haslam 408GHz MapFDS Dust Map at 3000 Ghz
extrpolated to 94GHz
Subtract the best fit Galactic foreground templates from CMB maps
Frequency (in GHz)
IIT Kanpur + IUCAA
Independent, self contained analysis of WMAP multi-frequency maps Blind estimation - free of uncertainties in knowledge & model of foregrounds
Saha, Jain, Souradeep(WMAP1: Apj Lett 2006)
WMAP3 : Eriksen et al. ApJ. 2006 (5 international groups)
Estimate foreground cleanedWMAP
Polarization maps & powerSpectra (Indo-French Collab.)
WMAP power spectrum estimate
Study Biases in the Cl estimation:
Foreground induced at low multipoles
(ongoing: Rajib Saha, Simon Prunet, P. Jain,TS)
Bias: -( 1)2 1
Sl
c
Cn
l
Controlling other SystematicsNon-circular beam effect in CMB measurements
(S. Mitra, A. Sengupta, Souradeep, PRD 2004)WMAP Q beam Eccentricity =0.7
Close to the corrections in the WMAP 2nd data
release
(Hinshaw et al. 2006)
Bias Matrix
ll
ll lAC C
Status of ongoing projectsStatus of ongoing projects
• AAll’ll’ for NC beam + incomplete/weighted sky for NC beam + incomplete/weighted sky Mitra, Sengupta, Ray, Saha, & TS
(arXiv:astro-ph/0702100 Phys. Rev. D submitted)
• Fast implementation of Fast implementation of AAll’ll’ computation computation
Mitra, Sengupta, Ray, Prunet & TS : in progress
• NC beam deconvolution at map-makingNC beam deconvolution at map-making Basak, Prunet, Bouchet & TS : in progress
• NC beam effect in Weak lensing of CMBNC beam effect in Weak lensing of CMB Aich, Basak, Benabed & TS : in progress
Planck Surveyor SatelliteEuropean Space Agency: Launch Aug. 2008
Francois Bouchet : Deputy PI of Planck-HFI +Simon Prunet, Karim Benabed : members of core
team
30 GHz 44 GHz 70 GHz
100 GHz 143 GHz 217 GHz
353 GHz 545 GHz 857 GHz
CMB Maps at the NINE Planck Frequencies
30Ghz 44Ghz
77Ghz 100Ghz
143Ghz 217Ghz
Combination of
Planck Channel maps(work in progress)
(R. Saha, T. Ghosh, P. Jain , TS
S. Prunet, F. Bouchet )
Input Simulated CMB map(in k unit)
Recovered foreground cleaned map(in mk unit)
Expected performance for Planck
Expected performance for Planck
(R. Saha, T. Ghosh, P. Jain , TS
S. Prunet, F. Bouchet )
Thompson scattering at redshift z=1100 (surface of last scattering)
generates a linear polarization pattern in the CMB sky.
CMB Polarization
Two polarization modes E&B
Four CMB spectra : ClTT, Cl
EE,ClBB,Cl
TE
(ongoing: Rajib Saha, Simon Prunet, P. Jain,TS)
WMAP CMB Polarization challenge
(ongoing: Rajib Saha, Simon Prunet, P. Jain,TS)
WMAP CMB Polarization challenge
100% WMAP noise10% WMAP noise1% WMAP noise
Related Publications (2006-07)
1. CMB anisotropy power spectrum using linear combinations of WMAP maps Authors: Rajib Saha, Simon Prunet, Pankaj Jain, Tarun Souradeep Journal ref: Submitted to Phys. Rev D. (under review) arXiv:0706.3567
2. Angular power spectrum of CMB anisotropy from WMAP Authors: Tarun Souradeep (IUCAA), Rajib Saha (IITK, IUCAA), Pankaj Jain (IITK) Journal ref: New Astron.Rev. 50 (2006) 854-860
3. CMB power spectrum estimation with non-circular beam and incomplete sky coverage
Authors: Sanjit Mitra (IUCAA), Anand S. Sengupta (Cardiff), Subharthi Ray (IUCAA), Rajib Saha (IITK, IUCAA), Tarun Souradeep (IUCAA)
Journal ref: Submitted to Phys. Rev D. (under review) arXiv:astro-ph/0702100
4. Non-Circular beam correction to the CMB power spectrum Authors: Tarun Souradeep (IUCAA), Sanjit Mitra (IUCAA), Anand Sengupta (Cardiff),
Subharthi Ray (IUCAA), Rajib Saha (IITK, IUCAA) Journal ref: New Astron.Rev. 50 (2006) 1030-1035 5. A re-analysis of the three-year WMAP temperature power spectrum and likelihood Authors: H. K. Eriksen, Greg Huey, R. Saha, F. K. Hansen, J. Dick, A. J. Banday, K. M. Gorski, P. Jain, J. B. Jewell, L. Knox, D. L. Larson, I. J. O'Dwyer, T. Souradeep, B. D. Wandelt Journal ref: Astrophys.J. 656 (2007) 641-652
Researchers
Exchange visits
Equipment
DL 320s NAS server
• HP Proliant DL320s storage server 3TB SATA Model. Intel Dual core 3070 Xeon processor
• 2.67 Ghz / 1067 Mhz FSB standard - 4 MB L2 Cache / 1 GB / hardware RAID/ 12 x 250
• GB SATA Drives/ Windows Storage Server 2003 R2 standard edition (AG650A)
• The NAS should have at least 2 network cards and should support NFS.
Planck Satellite on display at Cannes, France (on Feb. 1, 2007 , launch Aug 15,2008)
Thank Thank you !!!you !!!
1992
20032006
Cosmic “Super–IMAX” theater
Transparent universe
Opaque universe
14 GPc
Here & Now(14 Gyr)
0.5 Myr
WMAP 5: Angular power spectra
Pramoda Samal, R. Saha, J. Delabrouille, S. Prunet, P. Jain, TSarXiv:0903.3634(ApJ , press)
IPSE can recover the WMAP Polarization spectra after a bias correction (based on PSMForeground model)
Bias in the IPSE method
Bias arises when foreground & noisedominate over common angular scales-- weights are influenced by noise(Analytic study: Saha et al. PRD 08)
DAPSE: redressing the bias in IPSE method
DAPSE: Redressing the bias in IPSE(Direct angular power spectrum estimation)
Solution for weights :
Consider the 24 pairs of linear combinations of maps c & c’ that have no common detectors (DA)
1
/i n
c i i ilm l lm l
i
a w a B
[ ][ ][ ]
cc c c i ij il lm lm l l lij
C Tl
Fl
C a a w C w
C W WC
1
1
[ ] [ ]
[ ][ ][ ]
T Tl
Tl
C eW
e C e
[ ] 1 1 .. .. 1e
Minimize power in the Cross correlation power spectra1
/i n
c i i ilm l lm l
i
a w a B
1
1
[ ] [ ]
[ ][ ][ ]
Tl
Tl
C eW
e C e
Planck Sky Model (PSM) Different Model Comparison
DAPSE will have advantage compare to IPSE to those angular scales where foreground and noise start dominating compare to the signal. As, in DAPSE, we take cross correlation, the weights get less bias due to noise term.
WMAP7 EE Power SpectrumT. Ghosh, S.Prunet and T.Souradeep (in progress)
EE Power Spectrum from Simulations
T. Ghosh, S.Prunet and T.Souradeep (in progress)
WMAP7 low l EE Power Spectrum
T. Ghosh, S.Prunet and T.Souradeep (in progress)
TT Power Spectrum from Simulations
T. Ghosh, S.Prunet and T.Souradeep (in progress)
TT Low Multipole Bias
( 1)
2 1clean cmb cmbcl l l
nC C C
l
2 1fcmb cmb
l l
nC C
l
Analytic expression of bias at low multipoles
Saha et. al. PRD,2008
nf=2
Min (nc,nf)
T. Ghosh, S.Prunet and T.Souradeep (in progress)
WMAP7 TT Power SpectrumT. Ghosh, S.Prunet and T.Souradeep (in progress)
WMAP 7 TE Power Spectrum
T. Ghosh, S.Prunet and T.Souradeep (in progress)
IPSE & DAPSE: Cl estimate sans foreground
modeling
• IPSE & DAPSE : Internal estimation of the CMB angular spectrum without recourse to foreground models. I.e., evade systematics due to modeling uncertainties/ inadequacies. Especially useful for CMB polarization where foreground uncertainties are larger.
• Implemented successfully on WMAP1 & 3 for TT • TT, TE & EE for WMAP 5 (IPSE with bias correction) [Samal et al, PRD 09]
• Residuals consistent with known foreground [Ghosh et al, PRD 09]
• Analytic understanding of biases and variances in IPSE [Saha et al PRD 08]
• IPSE: WMAP EE power spectrum is a challenge due to noise being important even at low multipole. Noise in autocorrelation affects weight determination.
• DAPSE: resolves the above problem (by minimizing power in cross-correlation spectra) [Tuhin Ghosh, SP, TS, in progress]
• Exploring appropriate schemes for Planck. [T. Ghosh, TS, SP in progress]
Model Independent Foreground Maps
We obtained the best possible foreground maps at WMAP frequencies using popular techniques like “Wiener filtering” and “Needlet Analysis”.
T. Ghosh, J. Delabrouille, M. Remazellies, J. F. Cardoso and T.Souradeep
Model Independent
Estimate of Foregrounds Maps
T. Ghosh, R. Saha, P. Jain and T. Souradeep, PRD 2009
)]ˆˆ(exp[)(),( 212
21 qqnikPqqCn
LR
n
Preferred Directions in the universeCorrelation function on a Torus (periodic box)
SI violation at low wave-number, k q¿ 1
])(1[),( 22 021 i
ii qCqqC
20 )()( 20 ii
(Hajian & Souradeep 2003)
ˆ( ) ( )[1 ( ) ( )]LM LMP k A k g k Y k
(Pullen & Kamionkowski 2008)
More generally,
*' '( ) ( , ) ( , )LM
ll LM o o
dkD A k g k k
k
2
ˆ ˆˆ ˆ( , , , ) ( , , )
Legendre Expansion
( , )
( ) ( , )
k k p k k p
k
dkC P k k
k
1 1
1 1
1 1 1 1
'
*' '' ' ' '
' '
' '' '
ˆ ˆˆ ˆ( , , , ) ( , , )
Bipolar SH Expansion
( , )
( ) ( , ) ( , )
LM
LM L Mm m o o
LML M m
LM L Mm m m m
k k p k k p
k
dka a P k k k
k
C C
Statistical Isotropy: CMB Photon Statistical Isotropy: CMB Photon distributiondistribution
FT ˆˆ ˆ ˆ( , , ) ( , , ) ( , , , )x p k p k k p
(Moumita Aich & TS, in progress)
Statistical Isotropy: CMB Photon Statistical Isotropy: CMB Photon distributiondistribution
Free stream0
200 '0
''
(( , )
( ,
, )
... ( )) ll
rec
ecl
r
k
j k C
k
k
1 2
1
3 4
3 4
1
3 4
Free stream0
4 30 00 0 0 0
1 2
( ( , )
... ( )
, )
( , )
LLMrec
LMre
M
Ll
c
L
k
Lk C
k
k
j Cl
Statistical isotropy
General:Non-Statistical isotropy
(Moumita Aich & TS, PRD, in press)
Statistical Isotropy: CMB Photon Statistical Isotropy: CMB Photon distributiondistribution
3 1
4 2 1 2
1
2 1
2
1 2
4 3 ( )Large ( ) ( )
1 2
,,
,0
...
( , ) ... ( ( , )) LMl l r
lsl L
l l l LLMel
lc
LC
s l s s
k j k k
Non-Statistical isotropic terms also free-stream to large multipole values
(Moumita Aich & TS, PRD, in press)