Wilkinson Microwave Anisotropy Probe (and Future Directions)
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1 Wilkinson Microwave Anisotropy Probe (and Future Directions) L. Page, 2004
2 Dave Wilkinson (COBE announcement, 4/92)
3 WMAP A partnership between NASA/GSFC and Princeton Science Team: NASA/GSFC Chuck Bennett (PI) Bob Hill Gary Hinshaw Al Kogut Michele Limon Nils Odegard Janet Weiland Ed Wollack WMAP Movie Brown Greg Tucker UBC Mark Halpern CITA Mike Nolta UCLA Ned Wright Chicago Stephan Meyer Hiranya Peiris UT Austin Eiichiro Komatsu Penn Licia Verde Princeton Chris Barnes (Microsoft) Rachel Bean Olivier Dore Norm Jarosik Lyman Page David Spergel
4 K - 22GHz
5 Ka - 33GHz
6 Q - 41GHz
7 V - 61GHz
8 W - 94GHz
9
10 5º
11 cosmic variance Temperature 85% of sky Best fit model z<20 1 deg Temperaturepolarization z=1089 Prediction based on TT, no free params.
12 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. The Einstein-de Sitter model is disfavored by the WMAP CMB data at > 5 sigma. A closed model fits the data but requires H 0 =33 km/sec, in conflict with other non-cmb data. WMAP/NVSS ISW disfavors this as well. SN WMAP
13 Next steps in constraining models of the s universe. Measure n s and the running of the index. Measure or constrain r, the tensor to scalar index.
14 SDSS Movie File too large Mark Subbarao & SDSS Collaboration
15 The spectrum of scalar fluctuations. WMAP z=1089 2D Verde et al dFGRS z<3 3D Lyman alpha and now SDSS as well.
16 The scalar index, n s,with six parameters. Simple models of inflation predict: WMAP +SDSS Tegmark et al SDSS Galaxies and Lya Seljak et al This is significant in that it is a clear departure from scale invariance. We expect n s to 1% by 2008 from the CMB.
17 Running of the scalar index. In the two recent analyses of WMAP plus SDSS there is no evidence for running. SDSS Galaxies Tegmark et al Galaxies and Lya Seljak et al An analysis of CBI+WMAP+LSS shows evidence of running at the 3- sigma level ( /-0.031) but the CBI team does not place a lot of weight on the result. Readhead et al. 2004
18 Science: Growth of structure Equation of state Neutrino mass Ionization history Inflation Power spectrum ACT Atacama Cosmology Telescope Observations: CMB: l>1000 Cluster (SZ, KSZ X-rays, & optical) Diffuse SZ OV Lensing X-ray Optical Theory NSF Funded
19 ACT Collaboration 14 Universities, 3 Government Agencies, 6 Countries Cardiff (UK) Peter Ade Cindy Hunt Phil Mauskopf Haverford Steve Boughn Kayla Gaydosh (UG) Bruce Partridge Ryan Sajac (UG) Sarah Burke (UG) Columbia Amber Miller Will Grainger (PD) INOAE (Mexico) Britt Reichborn-Kjennerud (GS) David Hughes Craig Peters (UG) Jeff Wagg (GS) Dan Harlow (UG) Ben Hooberman (UG) David Tam (UG) CUNY Martin Spergel KwaZulu-Natal (SA) Catherine Cress Kavilan Moodley Gareth Amery Ryan Warne (GS) LLNL/SSL UCB Ed Wishnow NASA/GSFC Dominic Benford Jay Chervenak Harvey Moseley Carl Stahle Ed Wollack NIST/Boulder Randy Doriese Lisa Ferreira (tech) Gene Hilton Kent Irwin Carl Reintsema Leila Vale Yizi Xu (tech)
20 Collaboration cont. Penn Angelica de Oliveira Costa Mark Devlin Dan Swetz (GS) Michelle Caler (GS) Brent Budden (UG) Mohammad Haq (UG) Simon Dicker Bhuvnesh Jain Raul Jimenez Carlos Hernandez- Monteagudo (PD) Jeff Klein Max Tegmark Jose Diego (PD) Licia Verde Princeton Joe Fowler Mihail Amarie (GS) Norm Jarosik Robert Lupton Bob Margolis Princeton cont. Lyman Page Asad Aboobaker (GS) Juan Burwell (GS) Toby Marriage (GS) Judy Lau (GS) Adam Hincks (GS) Josh Burton (UG) Lusanne Wang (UG) Lucy Jacobson (UG) Matt Smith (UG) Uros Seljak Kevin Huffenberger (GS) Hy Trac (PD) David Spergel Rachel Bean Olivier Dore Mario Riquelme (GS) Suzanne Staggs Michael Niemack (GS) Shanker Iyer (UG) Jess Reidel (UG) Blake Dixon (UG) Rutgers Laura Ferrarese Arthur Kosowsky Neelima Sehgal (GS) Matthew Francis (GS) Jack Hughes Ted Williams Univ. of British Columbia Mark Halpern Danica Marsden (UG) Univ. de Catolica Hernan Quintana UMass Grant Wilson Univ. of Toronto Barth Netterfield
21 Arrays of bolometers Bock, JPL/Caltech 3.2 mm Moseley et al, NASA Need picture Completed close-packed 12x32 bolometer array SHARC II 12x32 Popup Array PI D. Dowell Torsional yoke attachment SCUBA 1 mm Lee, Berkeley One element Linear array after of foldingarray
22 Simulations of mm-wave data. Survey area <1% 2% High quality area 150 GHz SZ Simulation MBAC on ACT PLANCK 1.7 beam MAP PLANCK ACT Burwell/Seljak Statisitcal uncertainties SPT and APEX too. de Oliveira-Costa
23 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
24 Ionization History of Universe Polarization generated at decoupling surface. Polarization generated by first stars turning on.
25 Types of Cosmological Perterbations Temperature Scalars:, E polarization Temperature Tensors h (GW strain) E polarization B polarization (Maximum) Khoury et al.
26 CMB anisotropy Gravity Waves Strain PULSAR strain h LISA inflation LIGO BBN Over expanse of universe, one side is displaced 1000 ly with respect to the other From L. Boyle & P. Steinhardt cyclic frequency (Hz)
27 Polarization Spectrum Test inflation & tau Test T predictions Current limit on tensors B modes from tensors only. G-waves decay once inside the horizon. Reionization peak (z r =20) B modes from lensing of E modes. Horizon size at decoupling (z dec =1089)
28 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.
29 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), n s rises to compensate. There is a n s -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.
30 Sensitivity Advances COBE >x60 WMAP >x20 Planck >x50? Inflation Probe
31 Galaxy Removed CMB Map END
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