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Status Report of the Cmb Task Force STATUS REPORT OF THE CMB TASK FORCE Rainer Weiss, MIT on behalf of the Task Force HEPAP meeting February 15, 2005 Washington DC AAAC meeting February 16, 2005 Arlington, Virginia MEMBERS OF THE CMB TASK FORCE James Bock Caltech / JPL Sarah Church Stanford University Mark Devlin University of Pennsylvania Gary Hinshaw NASA / GSFC Andrew Lange Caltech Adrian Lee University of California at Berkeley / LBNL Lyman Page Princeton University Bruce Partridge Haverford College John Ruhl Case Western Reserve University Max Tegmark University of Pennsylvania / MIT Peter Timbie University of Wisconsin Rainer Weiss (chair) MIT Bruce Winstein University of Chicago Matias Zaldarriaga Harvard University AGENCY OBSERVERS Beverley Berger National Science Foundation Vladimir Papitashvili National Science Foundation Michael Salamon NASA/HDQTS Nigel Sharp National Science Foundation Kathy Turner US Department of Energy Charter of CMB Task Force • OSTP response to Turner Panel “From Quarks to Cosmos” sponsored by DOE,NASA and NSF. • Recommend a program of research of CMB observations to understand the properties of the inflationary epoch of cosmology • Primary objective to present plan to measure CMB polarization • HEPAP and AAAC Committees to receive report • Full report available mid March 2005 THE BASIC QUESTIONS • How did the universe begin Is inflation correct and how can it be tested • What is the fundamental physics What is the energy scale and the interaction What are the constituents of the primeval universe • How did the universe evolve What is the nature of the dark energy What is the geometry of the universe Properties of "standard “ inflation measurable with the CMB • Spectrum of spatial temperature fluctuations – Intrinsic quantum fluctuations both scalar and tensor – Scale invariant spectrum kn, n ~ 1 • Gaussian probability distribution of fluctuations • Tensor gravitational waves generated due to acceleration during inflation, related to energy scale of inflation ∆ T r =≤tensor 0.3 ∆ T scalar – cause quadrupolar density and temperature fluctuations in the primeval plasmas – uniquely measurable in the patterns of the CMB polarization due to Thomson scattering of the CMB by electrons (B modes) M. Tegmark & M. Zaldarriaga Figure 1: The cosmic mean density (solid curve) is diluted as the Universe expands. Inflation is a period when there is almost no dilution, causing the expansion to accelerate. The result is that the curve decrease slower than the dotted diagonal lines of slope –2.T he two triangles lie on the same diagonal, which means that quantum fluctuations generated during inflation at the open triangle have been stretched into the horizon-scale fluctuations that we observe today a tthe filled triangle in the CMB. Detecting inflationary gravitational waves with CMB polarization would directly measure the shape of this csomic density curve in the upper left corner of the plot, just as the porposed Joint Dark Energy mission would directly measure the same curve in the lower right corner. 2.2 Inflation The leading paradigm for what produced these seed fluctuatinos is inflation. Inflation is defined as an epoch when the cosmic expansion accelerated ä( > 0). This corresponds to the density curver (a) in Figure 1 dropping only slowly, with a slope shallower than –2 (dotted lines). This hase merged as the leading scenario for what M. Tegmark & M. Zaldarriaga 2.4 Other inflationary observables Independently o fwhether primordial gravitational waves are detected, a sensitive next-generation CMB satellite could dramatically enhance our undertsanding of the early Universe by measuring three other obsrevables connected with inflation . 1. Departures from scale invariance. 2. Non-Gaussianity. 3. Isocurvature modes. None of these has been detected so fasr,i nce, with a few minor caveats of unclear significance, all measurements to date are conisstent with “vanilla” primordial fluctuations. By this we mean the very simplest case known as scalar scale-invariant Gaussian adiabatic fluctuations, which aer defined by only one free parameter, their amplitude ~10–5. Although creative theorists haveg eneralized the classic inflation models (involving a single slow-rolling scalar field) in many different ways over the past two decades, essentially all oft hese models naturally predict some form of “non-vanilla” Kin Hot spot E Kscat electron H. Edens Gravitational wave strain pattern components of a B mode an example E mode 10.00 A POLAR B EE: DASI CAPMAP CBI synch limit TE: WMAP 30GHz TE DASI 1.00 synch limit 30GHz EE T [µK] ∆ Dust est. (94 GHz) 0.10 Synch est. (94 GHz) BB τ r=0.30 0.01 r=0.01 10.00 C D 1.00 WMAP T [µK] ∆ 0.10 Planck I Future Experiment Future Experiment II 0.01 1 10 100 1000 1 10 100 1000 Multipole moment, l Multipole moment, l Major components of the program • Completion of WMAP and successful launch and operation of PLANCK (TE, EE and foregrounds) • Ground based observations of small angular scale temperature variations (n and SZ effect) • Ground based and balloon borne program to measure polarization of the CMB and develop techniques and technology for a space mission (CMBPOL) in the next decade designed to measure the B modes to a level limited by the ability to model foregrounds. – Program to measure polarized foregrounds – Program to develop polarization sensitive receivers incorporating arrays of 1000s of detectors operating at the background limit of the CMB • Cooperative interagency program of research supported by DOE, NASA, NSF, NIST makes good sense. 2002 2004 2006 2008 2010 2012 2014 2016 WMAP PLANCK- T, P Satellite CMBPOL Boomerang – P PAPPA – P Maxipol – P EBEX – P Balloons CBI – T, SZ, P APEX–T, SZ Large Arrays – P ACT–T, SZ Atacama ACBAR – T, SZ QUAD – P Large Arrays – P DASI – T, P BICEP – P SPT–T, SZ South Pole Bolocam – SZ SuZIE – SZ CSO Compass – P MBI – P Bolometer SZA – SZ OTHER SITES HEMT CAPMAP – P KUPID Bolometer Inteferometer FOREGROUNDS HEMT Inteferometer TECHNOLOGY PSB’s 8 Antenna Coupled Bolometers 5 Large Arrays 5 SQUIDs 6 Time vs. Freq. Based MUX’s 6 MIMIC’s 6 100 mK Cooler for Space 6 Fundamental Receiver Research 2002 2004 2006 2008 2010 2012 2014 2016 100µΚ−s½ Polarization Sensitivity 10µΚ−s½ 1µΚ−s½ 10µΚ Polarization Map Sensitivity 1 x 1 degree 1µΚ 0.1µΚ Maps of Temperature Maps of E-Mode Maps of B-Mode WMAP PLANCK Foregrounds – Synchrotron/Point Sources Ground-Based HEMT Ground-Based HEMT/MIMICS CBI, DASI, CAPMAP Proposed 100 Data 1000 Cryogenic Observing Element Analysis/ Element Techniques Strategies Arrays Comp. Arrays CMBPOL GOAL: Produce a Polarization Ground-Based Bolo. Ground-Based Bolometric Receivers MAP down to the fundamental Acbar, Bolocam BICEP, MBI, QUAD and Proposed astrophysical foreground limits. ¾ First space mission designed to Polarization Antenna- Multiplexing Alternate measure the CMB Polarization SQUID Sensitive Coupled Readout Polarization ¾ 10 times more sensitive Multiplexing Bolometers Bolometers Technology Methods than PLANCK Balloon - Bolometer Balloon – Bolometer Boomerang, Maxipol PAPPA, EBEX Foregrounds - DUST FUNDAMENTAL RECEIVER RESEARCH Kinetic Inductance Detectors, Alternate Polarization Techniques, etc. universe virgo galaxy sun/earth earth Wavelength 10-5 BBN LIGO I (2005) PULSARS LIGO II 10-10 LISA (2013) Ω (f) (2013 ?) GW WMAP-I +SDSS r = 0.36 -15 INFLATION BBO I 10 (2025 ?) CMBPOL r = 0.01 (2016 ?) r = 0.001 BBO Corr (2030 ?) 10-20 10-15 10-10 10-5 10 0 10 5 L. Boyle & P. Steinhardt Frequency (Hz).
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