Which redshifts contribute most?

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3 Which redshifts contribute most? Some text z >1 z <5 z > 5 z <1 The deflection field receives contribution from a wide range of redshifts: 0.5<z<5. 3

4 Which scales contribute the most? Matter Power spectrum Most contribution comes from linear and quasilinear scales in the matter power spectrum. 4

5 Clearly see lensing in smearing now Ryan

6 First Internal Measurements are coming in... Joe Blake Alex

7 First Applications... Lambda from CMB alone Blake

8 Astrophysical Foregrounds Stephen

9 Galactic Foregrounds Aurelien+Typhaine

10 Mike

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12 Kimmy

13 Kimmy

14 Tinier but exciting signals.. also E-\phi. Duncan

15 Massively Scalable Simulations Guilio

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17 Galaxy Bias ˆd galaxies Large Scale Structure (LSS) surveys measure autocorrelations of galaxies. From this, we try to infer the correlations among dark matter halos. Such inferences are limited by our lack of understanding of bias - or how luminous matter traces dark matter. If we cross-correlate the reconstructed deflection field with the galaxy number counts, we go one step closer to the truth by directly measuring the galaxy-dark matter correlation. CMB lensing is particularly relevant for high z objects, behind which there are no galaxies to be lensed!

18 Galaxy Bias ˆd galaxies Great Signal-to-noise! Acquavivia, Hajian, Spergel and Das, PRD 78, (2008)

19 GR Test From Galaxy Bias Acquavivia, Hajian, Spergel and Das, PRD 78, (2008)

20 Herschel Galaxies The Herschel mission is mapping Far IR and sub-mm galaxies at 1< z < 3. Steep number counts imply strong negative K-corrections and magnification bias. PolarBear-I C κκ C gκ Golden candidates for cross-correlation with Planck lensing reconstruction. (Even for SPT and ACT) Cross-correlation signal can improve parameter constraints. Das and de Putter (in prep)

21 SuperPolarBear Herschel Galaxies The Herschel mission is mapping Far IR and sub-mm galaxies at 1< z < 3. Steep number counts imply strong negative K-corrections and magnification bias. C κκ C gκ Golden candidates for cross-correlation with Planck lensing reconstruction. (Even for SPT and ACT) Cross-correlation signal can improve parameter constraints. Das and de Putter (in prep)

22 Herschel Galaxies The Herschel mission is mapping Far IR and sub-mm galaxies at 1< z < 3. PB2 only + PB2 X Herschel Steep number counts imply strong negative K-corrections and magnification bias. Golden candidates for cross-correlation with Planck lensing reconstruction. (Even for SPT and ACT) Cross-correlation signal can improve parameter constraints. Das and de Putter (in prep)

23 Alexie SUDEEP DAS

24 Measuring distances Should be doable on Stripe-82 (CFHTLS); also with Subaru HSC/ LSST Das and Spergel (2008) SUDEEP DAS

25 f the Measuring foreground distribution distances narrow in redshift 2so t it can be approximated by a delta function, W f (η) η the f ), foreground then the ratio distribution of the above is narrow two cross-correlation in redshift so it sures, can be which approximated we call theby lensing-ratio, a delta function, reduces Experiment W f (η) to, Type (S/N) cross η f ), then the ratio of the above r Cκ CMBΣ l C κ = g two cross-correlation ures, which we call the lensing-ratio, CMB(η f ) reduces to, (8) galσ g gal (η f ) l ch is simply r Cκ CMBΣ l the C geometrical κ = g CMB(η f ) ratio of the source (8) galσ g gal (η f ) disution kernels. If the background galaxy distribution, FWHM l Planck: 7, h is is sufficiently simply the narrow geometrical in redshift ratio ofaround the source z = distion becomes, kernels. If the background galaxy distribution, FWHM z gal, CMBPOL: 3 is sufficiently narrow r = d in redshift around z = z gal, becomes, A(η 0 η f )d A (η gal ) d A (η gal η f )d A (η 0 ). f sky (9) 0.65 e that this r is= independent d A(η 0 l η f )d A (η gal ) d of the angular scale, tracer A (η gal η f )d A (η 0 ). (9) s and the power spectrum. Therefore, measurements everal that this multipoles is independent can beof combined the angular to constrain scale, tracer the and ing-ratio. the power Since spectrum. the distance Therefore, ratios measurements depend on the mology veral Das multipoles and and specifically Spergel can (2008) beon combined the dark energy to constrain model, SUDEEP the this DAS ng-ratio. be used tosince constrain the distance dark energy ratios parameters. depend on the Cl r/r(%) Planck POL TT CMBPOL POL TT (57)µK -arcmin in Temp (Pol) 1.0(1.4)µK-arcmin in Temp (Pol)

26 f the Measuring foreground distribution distances narrow in redshift 2so t it can be approximated by a delta function, W f (η) η the f ), foreground then the ratio distribution of the above is narrow two cross-correlation in redshift so it sures, can be which approximated we call theby lensing-ratio, a delta function, reduces Experiment W f (η) to, Type (S/N) cross η f ), then the ratio of the above r Cκ CMBΣ l C κ = g two cross-correlation ures, which we call the lensing-ratio, CMB(η f ) reduces to, (8) galσ g gal (η f ) l ch is simply r Cκ CMBΣ l the C geometrical κ = g w/o ratio CMB(η f ) ratio of the w/ratio source (8) galσ g gal (η f ) disution kernels. If the background galaxy distribution, FWHM l Planck: 7, h is is sufficiently simply the narrow geometrical in redshift ratio ofaround the source z = distion becomes, kernels. If the background galaxy distribution, FWHM z gal, CMBPOL: 3 is sufficiently narrow r = d in redshift around z = z gal, becomes, A(η 0 η f )d A (η gal ) d A (η gal η f )d A (η 0 ). f sky (9) 0.65 e that this r is= independent d A(η 0 l η f )d A (η gal ) d of the angular scale, tracer A (η gal η f )d A (η 0 ). (9) s and the power spectrum. Therefore, measurements everal that this multipoles is independent can beof combined the angular to constrain scale, tracer the and ing-ratio. the power Since spectrum. the distance Therefore, ratios measurements depend on the mology veral Das multipoles and and specifically Spergel can (2008) beon combined the dark energy to constrain model, SUDEEP the this DAS ng-ratio. be used tosince constrain the distance dark energy ratios parameters. depend on the Cl r/r(%) Planck POL TT CMBPOL POL TT (57)µK -arcmin in Temp (Pol) 1.0(1.4)µK-arcmin in Temp (Pol)

27 Measuring Growth SUDEEP DAS

28 Ly-alpha Forest And CMB Lensing ˆd Ly α The Ly-alpha absorption features in quasar spectra probe small scale density fluctuations. Lensing probes the long wavelength modes. Cross-correlation is a potentially powerful cosmological tool! Relevant for the BOSS survey: 200,000 QSOs. S/N ~ 10 for PLANCK Vallinotto, Das, Spergel & Viel, PRL,103:091304, 2009

29 Alberto

30 Lots To Do... Lots Of Papers To Write... Lets Discuss Some Questions Now...