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Wilkinson Microwave Anisotropy Probe (And Future Directions)

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Wilkinson Microwave Anisotropy Probe (And Future Directions) Wilkinson Microwave Anisotropy Probe (and Future Directions) L. Page, Texas@Stanford, 2004 Dave Wilkinson (COBE announcement, 4/92) WMAP A partnership between NASA/GSFC and Princeton Science Team: NASA/GSFC Chuck Bennett (PI) Bob Hill Gary Hinshaw WMAP Al Kogut Michele Limon Movie Nils Odegard Janet Weiland Ed Wollack UCLA Brown Ned Wright Greg Tucker Chicago Princeton Stephan Meyer UBC Chris Barnes (Microsoft) Mark Halpern Hiranya Peiris Penn Rachel Bean Licia Verde Lyman Page Olivier Dore David Spergel CITA UT Austin Norm Jarosik Mike Nolta Eiichiro Komatsu K - 22GHz Ka - 33GHz Q - 41GHz V - 61GHz W - 94GHz 5º Temperature cosmic variance 85% of sky Best fit model 1 deg Temperature- z<20 polarization z=1089 Prediction based on TT, no free params. Fundamental Findings A simple flat model with six parameters fits 1,000,000 data points remarkably well. We see there must be superhorizon fluctuations from the TE data. SN The Einstein-de Sitter model is disfavored by the WMAP CMB data at > 5 sigma. WMAP A closed model fits the data but requires H0=33 km/sec, in conflict with other non-CMB data. WMAP/NVSS ISW disfavors this as well. Next steps in constraining models of the 10-35 s universe. Measure ns and the running of the index. Measure or constrain r, the tensor to scalar index. SDSS Movie File too large Mark Subbarao & SDSS Collaboration The spectrum of scalar fluctuations. WMAP z=1089 2D Verde et al. 2003 z<3 2dFGRS 3D and now Lyman SDSS as alpha well. The scalar index, ns,with six parameters. WMAP +SDSS Tegmark et al. 2004 +SDSS Galaxies and Lya Seljak et al. 2004 Simple models of inflation predict: This is significant in that it is a clear departure from scale invariance. We expect ns to 1% by 2008 from the CMB. Running of the scalar index. SDSS Galaxies In the two recent analyses of WMAP Tegmark et al. 2004 plus SDSS there is no evidence for Galaxies and Lya running. Seljak et al. 2004 An analysis of CBI+WMAP+LSS shows evidence of running at the 3- Readhead et al. 2004 sigma level (-0.085+/-0.031) but the CBI team does not place a lot of weight on the result. Science: Observations: Growth of structure CMB: l>1000 ACT Cluster (SZ, KSZ Equation of state Atacama Cosmology Telescope X-rays, & optical) Neutrino mass Diffuse SZ Ionization history OV Inflation Lensing Power spectrum X-ray Optical Theory NSF Funded ACT Collaboration 14 Universities, 3 Government Agencies, 6 Countries Cardiff (UK) LLNL/SSL UCB Haverford Ed Wishnow Peter Ade Steve Boughn Cindy Hunt Kayla Gaydosh (UG) NASA/GSFC Phil Mauskopf Bruce Partridge Dominic Benford Ryan Sajac (UG) Jay Chervenak Columbia Sarah Burke (UG) Harvey Moseley Amber Miller Carl Stahle Will Grainger (PD) INOAE (Mexico) Ed Wollack Britt Reichborn-Kjennerud (GS) David Hughes Craig Peters (UG) Jeff Wagg (GS) NIST/Boulder Dan Harlow (UG) Randy Doriese Ben Hooberman (UG) Lisa Ferreira (tech) David Tam (UG) KwaZulu-Natal (SA) Gene Hilton Catherine Cress Kent Irwin CUNY Kavilan Moodley Carl Reintsema Martin Spergel Gareth Amery Leila Vale Ryan Warne (GS) Yizi Xu (tech) Collaboration cont. Penn Princeton cont. Angelica de Oliveira Costa Mark Devlin Lyman Page Rutgers Dan Swetz (GS) Asad Aboobaker (GS) Laura Ferrarese Michelle Caler (GS) Juan Burwell (GS) Arthur Kosowsky Brent Budden (UG) Toby Marriage (GS) Neelima Sehgal (GS) Mohammad Haq (UG) Judy Lau (GS) Matthew Francis (GS) Simon Dicker Adam Hincks (GS) Jack Hughes Bhuvnesh Jain Josh Burton (UG) Ted Williams Raul Jimenez Lusanne Wang (UG) Carlos Hernandez- Lucy Jacobson (UG) Univ. of British Columbia Monteagudo (PD) Matt Smith (UG) Mark Halpern Jeff Klein Uros Seljak Danica Marsden (UG) Max Tegmark Kevin Huffenberger (GS) Jose Diego (PD) Hy Trac (PD) Univ. de Catolica Licia Verde David Spergel Hernan Quintana Rachel Bean Princeton Olivier Dore UMass Mario Riquelme (GS) Grant Wilson Joe Fowler Suzanne Staggs Mihail Amarie (GS) Michael Niemack (GS) Norm Jarosik Univ. of Toronto Shanker Iyer (UG) Barth Netterfield Robert Lupton Jess Reidel (UG) Bob Margolis Blake Dixon (UG) Arrays of bolometers Moseley et al, NASA Bock, JPL/Caltech 3.2 mm Need picture SHARCCom IIpleted “close-12x32packed” 12x32 Popup bolometer array Array PI D. Dowell Torsional yoke attachment SCUBA 1 mm Lee, Berkeley One elementLinear array aft erof folding array Simulations of mm-wave data. <1% 1.40 Survey area ≈ 2% High quality area 150 GHz SZ Simulation MBAC on ACT PLANCK Burwell/Seljak 1.7’ beam MAP ACT PLANCK Statisitcal uncertainties SPT and APEX too. de Oliveira-Costa From Wayne Hu CMB Polarization Polarization of the CMB is produced by Thompson scattering of a quadrupolar radiation pattern. A component of the polarization is correlated with the temperature anisotropy. Whenever there are free electrons, the CMB is polarized. 2 deg Seljak & Zaldarriaga Ionization History of Universe Polarization generated at decoupling surface. Polarization generated by first stars turning on. Types of Cosmological Perterbations Temperature Scalars: , E polarization Temperature Tensors h (GW strain) E polarization B polarization (Maximum) Khoury et al. CMB anisotropy Gravity Waves -8 10 Strain 10-6 -12 1010-10 PULSAR -14 10 h -18 LISA ∆ 10 Over expanse of ain universe, one side is -22 10 LIGO BBN str in displaced 1000 ly with fl -26 at respect to the other. 10 io n -30 10 cyclic -34 10 -15 -10 -5 0 5 10 10 10 10 10 10 10 frequency (Hz) From L. Boyle & P. Steinhardt Polarization Test inflation & tau Test T predictions Spectrum Current limit G-waves on tensors decay once inside the B modes from horizon. tensors only. B modes from lensing of E modes. Reionization peak Horizon size at decoupling (z =1089) (zr=20) dec On the Verge of Detecting r? Spergel et al, 2003 Spergel et al, 2003 Tegmark et al, 2004 Seljak et al, 2004 All come from the temperature anisotropy and will improve. Simple models of inflation are being leaned on! A possible 95% cl limit on r from TT is roughly 0.1. Kosowsky, ‘04 The window for using B modes to detect r will open soon. The tensor to scalar ratio is being constrained by the low l region of the TT spectrum. When r is added to the mix of parameters (making 7), ns rises to compensate. There is a ns-r degeneracy*. WMAP WMAP+SDSS Tegmark et al WMAP+SDSS+Lya Seljak et al This is starting to lean on r=0.27 for simple models of inflation. *and tau, A too. Sensitivity Advances COBE >x60 WMAP >x20 Planck >x50? Inflation Probe Galaxy Removed CMB Map END.
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