1. Systematic effects in CMB data of ESA’s satellite Planck Tarun Souradeep (IUCAA, Pune) & Francois Bouchet (IAP, Paris) CEFIPRA mid-term presentation (Mussoorie, Oct. 27, 2007)

2. Quantum fluctuations super adiabatic amplified by inflation (rapid expansion) Galaxy & Large scale Structure formation Via gravitational instability Early Universe Present Universe The Cosmic screen Cosmic Microwave background

3. George Smoot John Mather COBE Cosmic Background Explorer First detection of CMB anisotropy (1992)

4. 2003 Second NASA CMB Satellite mission First NASA CMB Satellite mission

5. -200  K <  T < 200  K  T rms ¼ 70  K CMB temperature T cmb = 2.725 K Saha et al 2006 WMAP map of CMB anisotropy

6. Hence, a powerful tool for constraining cosmological parameters. Fig. M. White 1997 The Angular power spectrum of CMB anisotropy depends sensitively on Cosmological parameters Multi-parameter Joint likelihood (MCMC)

7. NASA/WMAP science team Total energy density Baryonic matter density Dawn of Precision cosmology !! Dark energy density Good old Cosmology, … New trend !

8. 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

9. CMB Task force report 2005 Timeline of CMB research WMAP-1yr now WMAP-3yr WMAP-8yr Planck (ESA) Next Gen. space CMBPOL/Sampan

10. 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

11. 1 DA 2 DA 1 DA 2 DA 4 DA WMAP multi-frequency maps

12. Template Based foreground removal Haslam 408GHz Map FDS Dust Map at 3000 Ghz extrpolated to 94GHz Subtract the best fit Galactic foreground templates from CMB maps Frequency (in GHz)

13. 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 cleaned WMAP Polarization maps & power Spectra (Indo-French Collab.) WMAP power spectrum estimate

14. Study Biases in the C l estimation: Foreground induced at low multipoles (ongoing: Rajib Saha, Simon Prunet, P. Jain,TS)

15. Controlling other Systematics Non-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 2 nd data release (Hinshaw et al. 2006) Status of ongoing projects A ll’ for NC beam + incomplete/weighted skyA ll’ for NC beam + incomplete/weighted sky Mitra, Sengupta, Ray, Saha, & TS ( arXiv:astro-ph/0702100 Phys. Rev. D submitted) Fast implementation of A ll’ computationFast implementation of A ll’ 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

16. Planck Surveyor Satellite European Space Agency: Launch Aug. 2008 Francois Bouchet : Deputy PI of Planck-HFI +Simon Prunet, Karim Benabed : members of core team

17. 30 GHz44 GHz70 GHz 100 GHz143 GHz217 GHz 353 GHz545 GHz857 GHz CMB Maps at the NINE Planck Frequencies

18. 30Ghz44Ghz 77Ghz 100Ghz 143Ghz217Ghz Combination of Planck Channel maps (work in progress) (R. Saha, T. Ghosh, P. Jain, TS S. Prunet, F. Bouchet )

19. Input Simulated CMB map (in  k unit) Recovered foreground cleaned map (in mk unit) Expected performance for Planck

20. (R. Saha, T. Ghosh, P. Jain, TS S. Prunet, F. Bouchet )

21. 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 : C l TT, C l EE,C l BB,C l TE

22. (ongoing: Rajib Saha, Simon Prunet, P. Jain,TS) WMAP CMB Polarization challenge

23. (ongoing: Rajib Saha, Simon Prunet, P. Jain,TS) WMAP CMB Polarization challenge 100% WMAP noise10% WMAP noise1% WMAP noise

24. Related Publications (2006-07) 1. CMB anisotropy power spectrum using linear combinations of WMAP maps Authors: Rajib Saha, Simon Prunet, Pankaj Jain, Tarun SouradeepRajib SahaSimon PrunetPankaj JainTarun Souradeep Journal ref: Submitted to Phys. Rev D. (under review) arXiv:0706.3567arXiv:0706.3567 2. Angular power spectrum of CMB anisotropy from WMAP Authors: Tarun Souradeep (IUCAA), Rajib Saha (IITK, IUCAA), Pankaj Jain (IITK)Tarun SouradeepRajib SahaPankaj Jain 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)Sanjit MitraAnand S. SenguptaSubharthi RayRajib SahaTarun Souradeep Journal ref: Submitted to Phys. Rev D. (under review) arXiv:astro-ph/0702100arXiv: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)Tarun SouradeepSanjit MitraAnand SenguptaSubharthi RayRajib Saha 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,H. K. EriksenGreg HueyR. SahaF. K. HansenJ. DickA. J. Banday K. M. GorskiK. M. Gorski, P. Jain, J. B. Jewell, L. Knox, D. L. Larson, I. J. O'Dwyer, T. Souradeep,P. JainJ. B. JewellL. KnoxD. L. LarsonI. J. O'DwyerT. Souradeep B. D. Wandelt Journal ref: Astrophys.J. 656 (2007) 641-652

25. Researchers

26. Exchange visits

27. 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.

28. Planck Satellite on display at Cannes, France (on Feb. 1, 2007, launch Aug 15,2008) Thank you !!!

29. 1992 2003 2006

30. Cosmic “Super–IMAX” theater Transparent universe Opaque universe 14 GPc Here & Now (14 Gyr) 0.5 Myr

31. WMAP 5: Angular power spectra Pramoda Samal, R. Saha, J. Delabrouille, S. Prunet, P. Jain, TS arXiv:0903.3634 (ApJ, press) IPSE can recover the WMAP Polarization spectra after a bias correction (based on PSM Foreground model)

32. Bias in the IPSE method Bias arises when foreground & noise dominate over common angular scales -- weights are influenced by noise (Analytic study: Saha et al. PRD 08) ‏

33. DAPSE: redressing the bias in IPSE method

34. 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) ‏ Minimize power in the Cross correlation power spectra

35. 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.

36. WMAP7 EE Power Spectrum T. Ghosh, S.Prunet and T.Souradeep (in progress)

37. EE Power Spectrum from Simulations T. Ghosh, S.Prunet and T.Souradeep (in progress)

38. WMAP7 low l EE Power Spectrum T. Ghosh, S.Prunet and T.Souradeep (in progress)

39. TT Power Spectrum from Simulations T. Ghosh, S.Prunet and T.Souradeep (in progress)

40. TT Low Multipole Bias Analytic expression of bias at low multipoles Saha et. al. PRD,2008 n f =2 Min (n c,n f ) T. Ghosh, S.Prunet and T.Souradeep (in progress)

41. WMAP7 TT Power Spectrum T. Ghosh, S.Prunet and T.Souradeep (in progress)

42. WMAP 7 TE Power Spectrum T. Ghosh, S.Prunet and T.Souradeep (in progress)

43. IPSE & DAPSE: C l 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]

44. 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

45. Preferred Directions in the universe Correlation function on a Torus (periodic box) SI violation at low wave-number, k  q ¿ 1 (Hajian & Souradeep 2003) (Pullen & Kamionkowski 2008) More generally,

46. Statistical Isotropy: CMB Photon distribution (Moumita Aich & TS, in progress)

47. Statistical Isotropy: CMB Photon distribution Statistical isotropy General: Non- Statistical isotropy (Moumita Aich & TS, PRD, in press)

48. Statistical Isotropy: CMB Photon distribution Non-Statistical isotropic terms also free-stream to large multipole values (Moumita Aich & TS, PRD, in press)