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Future Probes of the Scalar and Tensor Primordial Perturbation Spectra

Future Probes of the Scalar and Tensor Primordial Perturbation Spectra. Lloyd Knox (UC Davis). with Manoj Kaplinghat (UC Davis) Yong-Seon Song (UC Davis). Special thanks to Tony Tyson & David Wittman. Future Probes of Scalar and Tensor Spectra. Tensor spectra From the CMB

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Future Probes of the Scalar and Tensor Primordial Perturbation Spectra

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  1. Future Probes of the Scalar and Tensor Primordial Perturbation Spectra Lloyd Knox (UC Davis) with Manoj Kaplinghat (UC Davis) Yong-Seon Song (UC Davis) Special thanks to Tony Tyson & David Wittman

  2. Future Probes of Scalar and Tensor Spectra • Tensor spectra • From the CMB • Scalar spectra • From the Ly-a forest • From the CMB • From cosmic shear

  3. Gravitational Wave Generates Temperature Anisotropy and Polarization Imagine a single GW propagating out of the screen, compressing and stretching space as shown by arrows. Resulting temperature pattern Also leads to polarization since unpolarized quadrupole radiation scattered by an electron results in polarization.

  4. Knox & Song, PRL (2002) ; Kesden et al. PRL (2002) Detecting Gravitational Waves Hu and Okamoto, 2002 lensing potential reconstruction Lensing—induced scalar B mode The “B mode” polarization pattern is not generated by scalar perturbations in linear perturbation theory. Residual scalar B mode power

  5. Implication of high t for gravity wave search Tensor signal in B modes rmin/ 1/t Kaplinghat, Knox & Song (2003)

  6. Scalar Perturbations: Why study to high precision? • Discriminant of inflationary models. • Large |dns/dlnk| must be confirmed with other techniques. • It’s the only observable we know for sure that we have! [We might also have higher-order correlations, small amounts of curvature, non-trivial topology, observable tensor perturbations, …] • In doing so, we must also study evolution of spectrum which tells us about the matter content (dark energy, neutrino mass, …) Gold & Albrecht 2003 Peiris et al. 2003

  7. Horizon CMB lD Dynamic Range Last h0/lD ' 1000 Scattering ~h0~1/H0 Surface

  8. The Quest for Dynamic Range Peiris et al. 2003 CMB

  9. Results from CMB+ Lya Forest allCMB: ns=0.97 § 0.03 allCMB: ns=0.91§0.06 dns/dlnk=-0.055§0.038 allCMB+2dF+hi-res Ly-a: ns=0.93§0.03 dns/dlnk=-0.031§0.017 Spergel et al. 2003 CMB + hi-res Lya : ns=1, dns/dlnk=0 is fine! Zaldarriaga, Scoccimarro & Hui 2001 Seljak et al. 2003 Preliminary CMB+lo-res SDSS Lya: nothing firm yet, stay tuned

  10. Horizon CMB Lensing lD Dynamic Range Last h0/lD ' 1000 Scattering h0/(lD /10) ' 104 (with CMB lensing) ~h0~1/H0 Surface

  11. The Quest for Dynamic Range Peiris et al. 2003 CMB lensing CMB

  12. Lensing of the CMB Hu (2001), Hu and Okamoto (2002)

  13. One can reconstruct the deflection angle power spectrum from the trispectrum. Bernardeau 1997 Zaldarriaga 2000 Hu 2001 Hu and Okamoto 2002 Cooray and Kesden 2003

  14. Error boxes for CMBpol (fwhm=3’, DT=3mK-arcmin, Dp=4.2mK-arcmin) CMB Temperature and Polarization Power Spectra

  15. B Mode Hunt Auxiliary Science Goal I Precision measurement of primordial scalar power spectrum.

  16. B Mode Hunt Auxiliary Science Goal II Neutrino oscillation experiments put a lower bound on the sum of neutrino masses; the sum should be greater than about 0.06 eV (Beacom and Bell, PRD 2002).

  17. CMB+Tomographic Cosmic Shear lD Dynamic Range h0/lD ' 103 h0/(lD /10) ' 104 (with CMB lensing) ~h0~1/H0 • It would be great to • Lens something with structure on angular scales smaller than lD/h0, and • Without the projection effect!

  18. Cosmic Shear From A. Refregier

  19. Cosmic Shear Results Cosmic shear detected by many groups in the last two years. Contaldi, Hoekstra & Lewis 2003

  20. Tomography Requires sorting background galaxies into redshift slices.

  21. Lensing Power Spectra

  22. Cross Power Spectra

  23. Tomography Today It’s early days, but tomography with photometric redshifts is being done now! with, e.g., DLS and COMBO-17.

  24. Go Broad and Deep LSST Deep (mV=27) Broad (30,000 sq. deg.)

  25. Results for Planck + LSST Warning: Highly preliminary! Note: LSST restricted to l < 1000 to reduce sensitivity to highly non-linear regime.

  26. Conclusions • No solid evidence yet for dns/dlnk non-zero. Statistical weight may be there in existing data, but the systematics have not yet been tamed. • CMB observations by themselves will easily be able to see the dns/dlnk at the levels that have been suggested. • Cosmic shear combined with CMB will probe well into the regime where dns/dlnk is expected to differ from zero. This combination may provide extremely rich study of scalar perturbation spectrum, providing strong constraints on inflation or whatever generated the fluctuations. • Tensor B modes may or may not be there. Plenty of interesting science along the way.

  27. Let’s go check our inflation!

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