Presentation on latest science from the Dark Energy Survey

Presentation on latest science from the Dark Energy Survey, UK National Astronomical Meeting, 28th June 2016

Transcript

1. Dark Energy Survey 1 Donnacha Kirk Including work by: Yuuki Omori, A. Benoit-Levy, R. Cawthon, C. Chang, P. Larsen and many others SPT collaborators include: G. Holder, B.Benson, L. Bleem, K. Story DARK ENERGY SURVEY Cross-Correlation of Gravitational Lensing from DES SV, SPT and Planck
2. Two multicolor surveys: - 300 M galaxies over 5000 deg2 - grizY to 24th mag - 3500 supernovae (30 sq deg) THE DARK ENERGY SURVEY New camera for CTIO Blanco 4m telescope - 570 Mpixels - 3 deg2 FOV - Facility instrument Five-year Survey - 525 nights (Sept.-Feb.) - Science Verification (SV): Nov 2012-Feb 2013 Four cosmic probes - Large-scale structure - Weak Gravitational Lensing - Galaxy Clusters
3. Two multicolor surveys: - 300 M galaxies over 5000 deg2 - grizY to 24th mag - 3500 supernovae (30 sq deg) THE DARK ENERGY SURVEY New camera for CTIO Blanco 4m telescope - 570 Mpixels - 3 deg2 FOV - Facility instrument Five-year Survey - 525 nights (Sept.-Feb.) - Science Verification (SV): Nov 2012-Feb 2013 Four cosmic probes - Large-scale structure - Weak Gravitational Lensing - Galaxy Clusters
4. !15 — FOOTPRINT SPT OVERLAP DES SV DATA: DARK ENERGY SURVEY THE DARK ENERGY SURVEY 10m CMB telescope - SPT SZ survey (2008-2011) - Tri-band (90,150,220 GHz) - Footprint 2500deg2 - Upgrade to SPT3G soon…
8. LSS + WL: DES and SPT Large-Scale Structure (LSS) Galaxy number density from DES Weak Lensing (WL) Galaxy shape measurements from DES CMB Lensing (CMB-WL) Lensing measurements from SPT-SZ (and Planck 2015) Giannantonio & Fosalba et al. 2015 1507.05551 Kirk & Omori et al. 2015 1512.04535 Baxter et al. 2016 1602.07384 Kwan et al. 2016 1604.07871 Clampitt et al. 1603.05790
9. LSS + WL: DES and SPT Weak Lensing (WL) Galaxy shape measurements from DES CMB Lensing (CMB-WL) Lensing measurements from SPT-SZ (and Planck 2015) Kirk & Omori et al. 2015 1512.04535
10. Weak Lensing x CMB Lensing Cross-correlation — !9 — GALAXY LENSING - CMB LENSING CROSS-CORRELATION kernels matter power spectrum BACKGROUND Cϵϵ (ℓ) = C GG (ℓ) + C IG (ℓ) + C IG (ℓ) + C II ( Cij nn (ℓ) = Cij gg (ℓ) + Cij gm (ℓ) + Cji gm (ℓ) + Cij mm Cij nϵ (ℓ) = Cij gG (ℓ) + Cij gI (ℓ) + Cji mG (ℓ) + Cij mI CXY (ℓ) = dχ χ2 WX WY P(ℓ/χ, z) Wg[χ(z)] = bg (χ)n(χ) WGW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ′ χH dχ′ns(χ′) WCMBW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ∗ − χ χ∗ — !10 — GALAXY LENSING - CMB LENSING CROSS-CORRELATION kernels matter power spectrum BACKGROUND
11. Weak Lensing x CMB Lensing Cross-correlation — !9 — GALAXY LENSING - CMB LENSING CROSS-CORRELATION kernels matter power spectrum BACKGROUND Cϵϵ (ℓ) = C GG (ℓ) + C IG (ℓ) + C IG (ℓ) + C II ( Cij nn (ℓ) = Cij gg (ℓ) + Cij gm (ℓ) + Cji gm (ℓ) + Cij mm Cij nϵ (ℓ) = Cij gG (ℓ) + Cij gI (ℓ) + Cji mG (ℓ) + Cij mI CXY (ℓ) = dχ χ2 WX WY P(ℓ/χ, z) Wg[χ(z)] = bg (χ)n(χ) WGW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ′ χH dχ′ns(χ′) WCMBW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ∗ − χ χ∗ Matter Power Spectrum — !10 — GALAXY LENSING - CMB LENSING CROSS-CORRELATION kernels matter power spectrum BACKGROUND
12. Weak Lensing x CMB Lensing Cross-correlation — !9 — GALAXY LENSING - CMB LENSING CROSS-CORRELATION kernels matter power spectrum BACKGROUND Cϵϵ (ℓ) = C GG (ℓ) + C IG (ℓ) + C IG (ℓ) + C II ( Cij nn (ℓ) = Cij gg (ℓ) + Cij gm (ℓ) + Cji gm (ℓ) + Cij mm Cij nϵ (ℓ) = Cij gG (ℓ) + Cij gI (ℓ) + Cji mG (ℓ) + Cij mI CXY (ℓ) = dχ χ2 WX WY P(ℓ/χ, z) Wg[χ(z)] = bg (χ)n(χ) WGW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ′ χH dχ′ns(χ′) WCMBW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ∗ − χ χ∗ Matter Power Spectrum Kernels for each observable — !10 — GALAXY LENSING - CMB LENSING CROSS-CORRELATION kernels matter power spectrum BACKGROUND Gµν = 8πGTµν + Λ Gµν = 8πGTµν + Λ Cij ϵϵ (ℓ) = Cij GG (ℓ) + Cij IG (ℓ) + Cji IG (ℓ) + Cij II (ℓ) Cij nn (ℓ) = Cij gg (ℓ) + Cij gm (ℓ) + Cji gm (ℓ) + Cij mm (ℓ) Cij nϵ (ℓ) = Cij gG (ℓ) + Cij gI (ℓ) + Cji mG (ℓ) + Cij mI (ℓ) CXY (ℓ) = dχ χ2 WX WY P(ℓ/χ, z) Wg[χ(z)] = bg (χ)n(χ) WGW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ′ χH dχ′ns(χ′) χ′ − χ χ′ WCMBW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ∗ − χ χ∗
13. Weak Lensing x CMB Lensing Cross-correlation — !9 — GALAXY LENSING - CMB LENSING CROSS-CORRELATION kernels matter power spectrum BACKGROUND Cϵϵ (ℓ) = C GG (ℓ) + C IG (ℓ) + C IG (ℓ) + C II ( Cij nn (ℓ) = Cij gg (ℓ) + Cij gm (ℓ) + Cji gm (ℓ) + Cij mm Cij nϵ (ℓ) = Cij gG (ℓ) + Cij gI (ℓ) + Cji mG (ℓ) + Cij mI CXY (ℓ) = dχ χ2 WX WY P(ℓ/χ, z) Wg[χ(z)] = bg (χ)n(χ) WGW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ′ χH dχ′ns(χ′) WCMBW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ∗ − χ χ∗ Matter Power Spectrum Kernels for each observable — !11 — GALAXY LENSING - CMB LENSING CROSS-CORRELATION kernels matter power spectrum BACKGROUND Gµν = 8πGTµν + Λ Gµν = 8πGTµν + Λ Cij ϵϵ (ℓ) = Cij GG (ℓ) + Cij IG (ℓ) + Cji IG (ℓ) + Cij II (ℓ) Cij nn (ℓ) = Cij gg (ℓ) + Cij gm (ℓ) + Cji gm (ℓ) + Cij mm (ℓ) Cij nϵ (ℓ) = Cij gG (ℓ) + Cij gI (ℓ) + Cji mG (ℓ) + Cij mI (ℓ) CXY (ℓ) = dχ χ2 WX WY P(ℓ/χ, z) Wg[χ(z)] = bg (χ)n(χ) WGW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ′ χH dχ′ns(χ′) χ′ − χ χ′ WCMBW L[χ(z)] = 3H2 0 Ωm 2c2 χ a(χ) χ∗ − χ χ∗
14. Measurement of the Cross-correlation • Angular power spectrum Cl using PolSpice harmonic space estimator. Fix cosmology, use theory prediction to fit cross-correlation amplitude. 1992), these take the form of integrals over the non-linear matter power spectrum, P (`/ (z), z), and a pair of appro- priately chosen window functions. We are interested in the cross-correlation between GWL and CMBWL, C GWL,CMBWL (`) = Z hor 0 d (z)2 W GWL [ (z)] W CMBWL [ (z)]P ✓ ` (z) , z ◆ , (1) C GWL,CMBWL (`) = A⇥ Z hor 0 d (z)2 W GWL [ (z)] W CMBWL [ (z)]P ✓ ` (z) , z ◆ , (2) where (z) is the comoving distance to redshift z and hor is the distance to the horizon. Here W GWL and W CMBWL are the GWL and CMBWL window functions. The GWL window function, also known as the lensing e ciency function or lensing kernel, takes the form W GWL [ (z)] = 3H2 0 ⌦ m 2c2 a( ) Z hor d 0n( 0) 0 0 , (3) where H 0 is the Hubble parameter, c the speed of light, ⌦ m the total matter density and n( 0) is the galaxy redshift distribution. We have assumed a flat universe, as we will throughout the paper. The CMBWL window function takes a similar form but CROSS-CORRELATION RESULTS: GALAXY LENSING - CMB LENSING CROS
15. CROSS-CORRELATION RESULTS: GALAXY LENSING - CMB LENSING CROS Measurement of the Cross-correlation Redshift Range 0 . 3 < z < 1 . 3 CMB E A 2/ d.o.f. ngmix ⇥ SPT 0 . 88+0.30 0.30 0.93 ngmix ⇥ Planck 0 . 86+0.39 0.39 1.52 Table 1. Summary of constraints on the cross-co • Angular power spectrum Cl using PolSpice harmonic space estimator. Fix cosmology, use theory prediction to fit cross-correlation amplitude. • Evidence for cross-correlation at the 3 sigma level. • DES x SPT and DES x Planck are consistent. • Measured cross-correlation is consistent with the expectation from theory using Planck 2015 cosmology. 1992), these take the form of integrals over the non-linear matter power spectrum, P (`/ (z), z), and a pair of appro- priately chosen window functions. We are interested in the cross-correlation between GWL and CMBWL, C GWL,CMBWL (`) = Z hor 0 d (z)2 W GWL [ (z)] W CMBWL [ (z)]P ✓ ` (z) , z ◆ , (1) C GWL,CMBWL (`) = A⇥ Z hor 0 d (z)2 W GWL [ (z)] W CMBWL [ (z)]P ✓ ` (z) , z ◆ , (2) where (z) is the comoving distance to redshift z and hor is the distance to the horizon. Here W GWL and W CMBWL are the GWL and CMBWL window functions. The GWL window function, also known as the lensing e ciency function or lensing kernel, takes the form W GWL [ (z)] = 3H2 0 ⌦ m 2c2 a( ) Z hor d 0n( 0) 0 0 , (3) where H 0 is the Hubble parameter, c the speed of light, ⌦ m the total matter density and n( 0) is the galaxy redshift distribution. We have assumed a flat universe, as we will throughout the paper. The CMBWL window function takes a similar form but
16. Beyond detection: exploiting the power of cross-correlations • Calibrate systematics that hold back our ‘standard’ probes. e.g. intrinsic alignments, shear measurement bias, photo-z error… • Measure cosmology as part of a full, multi-probe analysis. Cross-correlations help break parameter degeneracies. CMB lensing acts like a new high-z tomographic bin. • Map massive structures in the high- redshift universe. Subtracting a DES lensing map from an SPT lensing map removes low-z structure.
17. — FUTURE WORK FUTURE WORK Galaxy density x CMB lensing forecast Galaxy lensing x CMB lensing foreca Future Plans & Priorities 2016: SPT-3G ~ 15,200 detectors 100, 150, 220 GHz + Polarisation SPT-SZ 960 detectors 100, 150, 220 GHz The South Pole Telescope (SPT) 10-meter sub-mm quality wavelength telescope At 100, 150, 220 GHz, angular resolution of 1.6, 1.2, 1.0 arcmin The South Pole Telescope (SPT) •10-meter sub-mm quality wavelength telescope • At 100, 150, 220 GHz, angular resolution of 1.6, 1.2, 1.0 arcmi • Y1: 1500deg2, slightly shallower than SV. • Y5: 5000deg2 on the same timescale as the SPT-3G upgrade. • In the future we will have >30 sigma detection of this signal.
18. Cross-Correlations
19. Cross-Correlations