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A New Window into Stochastic Gravity Waves

A New Window into Stochastic Gravity Waves. Aditya Rotti. Supervisor: Tarun Souradeep. Indo-UK Meet 11 th August 2011. The Current Landscape. No Probe. Lensing. Lensing. Direction of photon arrival changed. Let denote the displacement on the sphere. .

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A New Window into Stochastic Gravity Waves

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  1. A New Window into Stochastic Gravity Waves Aditya Rotti Supervisor: TarunSouradeep Indo-UK Meet 11thAugust 2011

  2. The Current Landscape No Probe

  3. Lensing

  4. Lensing Direction of photon arrival changed Let denote the displacement on the sphere. Angular power spectrum of photon displacements A. Stebbins, arXiv:astro-ph/p609149

  5. Lensing Modifications to CMB Lensing induces power transfer between the two polarization spectra Lensing Kernel

  6. Hints !! • Current lensing considerations are only due to scalar perturbations. • The scalar power spectrum is already well measured. • A huge difference between current upper limits on the BB spectra and the expected signal.

  7. Hints !! QUAD/BICEP ? arXiv:0903-1003v3

  8. Just a Reminder Scalar Perturbations (LSS) Tensor Perturbations (Gravity Waves) Toy model : Power Spectrum of the projected lensing potential =

  9. A Comparison : GW more efficient !

  10. Can we constrain Gravitational Waves Power Spectra ? Gravitational waves !!

  11. GW Power Spectra Deflection Power Spectra C. Li and A. Cooray, PRD 74, 023521(2006) P(k)=Constant GW sourced at different z

  12. Constraining the deflection power spectra Sensitivity of the lensed BB spectra to the deflection angular power spectra !! The best constraints on the deflection power in the specific bins will come from the measurements of the spectra at the location of the respective peaks. RMS deflection power is kept constant : Scalar Perturbations

  13. Constraints on the GW power spectra. Preliminary Results I am close to getting the constraints. I will hopefully have a picture to put here for tomorrow’s mock talk 

  14. A New Window into Gravitational Waves !! 10-16 – 10-14 Hz k = 0.001 – 1 Mpc-1 Vol 460 | 20 August 2009 | doi:10.1038/nature08278

  15. Summary : • Tensors are more efficient at transferring power from EE  BB spectra. • From current and future experiments which will • measure the CMB polarization spectra, it will be • possible to put constraints on the Gravitational • Waves spectra. • This probe provides a new window into • Gravitational Waves which has not been • previously explored. Thank you for your attention 

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