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B-mode from strings Levon Pogosian Simon Fraser University with - PowerPoint PPT Presentation

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B-mode from strings Levon Pogosian Simon Fraser University with H. Tye (Cornell) T. Vachaspati (Case) I. Wasserman (Cornell) M. Wyman (Perimeter) SFU Cosmology V. P. Frolov D. Pogosyan A. V. Frolov L. Pogosian The spectrum Primordial

  1. B-mode from strings Levon Pogosian Simon Fraser University with H. Tye (Cornell) T. Vachaspati (Case) I. Wasserman (Cornell) M. Wyman (Perimeter)

  2. SFU Cosmology V. P. Frolov D. Pogosyan A. V. Frolov L. Pogosian

  3. The spectrum Primordial perturbations: • predominantly passive (not active) • nearly adiabatic • nearly scale-invariant

  4. Active perturbations

  5. CMB temperature anisotropy from strings M.Wyman, L.Pogosian, I.Wasserman, astro-ph/0604141

  6. Strings vs WMAP Wiggly local cosmic strings Inflation String spectrum from Pogosian & Vachaspati, PRD’99

  7. String induced CMB temperature anisotropy can’t exceed ~10% of the total depends on the string model G µ The corresponding bound on Conservatively, G µ < 0.7 � 10 � 6

  8. Do we need cosmic strings? Produced after hybrid inflation I. Tkachev, S. Khlebnikov, L. Kofman, A. Linde (‘95-’98) (KKLMMT, SUSY GUT,…) Source of B-mode polarization

  9. The segment model Straight, randomly oriented, moving string segments Density, correlation length, wiggliness, rms v matched to simulated networks Vincent, Hindmarsh, Sakellariadou (1996) Albrecht, Battye, Robinson (1997) Pogosian & Vachaspati (1999) Good enough for large scale features Incorporated into CMBFAST: publicly available as CMBACT

  10. CMB polarization DASI 2002

  11. E (gradient) and B (curl) modes from M. Zaldarriaga, astro-ph/0305272

  12. Sources of B-mode Lensing of E-mode by large scale structures (scalar modes) The ISW effect from gravity waves (tensor modes) Anisotropic stress produced by defects ( vector and tensor modes) Magnetic fields (vector and tensor modes)

  13. B-mode CMB polarization Lensing by matter Sourced by Sourced by strings Gravity Waves M.Wyman, L.Pogosian, I.Wasserman, astro-ph/0604141

  14. What determines the shape? recombination peak reionization peak Contributing factors: correlation length, velocity, density, tension, wiggliness

  15. Strings at last scattering � G µ v � � t , � � O (1) v � t

  16. Where is the main peak?

  17. Global strings (Seljak, Pen, Turok, PRL’97) “Standard” CDM: h=0.5, Ω M =1, Ω b =0.05

  18. Field theory simulations, local U(1) (Bevis, Hindmarsh, Kunz, Urrestilla, 0704.3800) B

  19. Prospects of detection recombination peak reionization peak r = 10 � 6 , G µ = 10 � 8 from Seljak & Slozar, astro-ph/0604143

  20. Summary In Hybrid Inflation models, including Brane Inflation, string generated vector B-mode can exceed the GW contribution String B-mode spectrum has a distinct shape, with a pronounced main peak at 500<l<1000 The magnitude and the exact peak position are determined by properties of cosmic string networks at last scattering

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