Measurements of CMB Polarization Anisotropy and Searches for Galaxy Clusters with Bolometer Arrays
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1 Measurements of CMB Polarization Anisotropy and Searches for Galaxy Clusters with Bolometer Arrays Adrian Lee Department of Physics, LBNL Physics Division University of California, Berkeley
2 CMB Polarization Science Galaxy Cluster Survey Science Development of Bolometer Arrays Experiments POLARBEAR APEX-SZ South Pole Telescope Outline
3 Polarization Science
4
5 Gravity Waves from Inflation Gravity waves put stress on photon-baryon fluid Generation of B-mode polarization Detection => smoking gun of inflation Amplitude of B-mode gives Energy Scale One possibility: GUT level GeV 12 orders of magnitude higher energy than accelerators! Observable evidence of String Theory?
6 E-modes and B-modes E-mode B-mode Density fluct. give scalar perturbations => E-mode Gravity Waves give tensor perturbations=> B, E modes Defects and strings give vector perturbations => B-mode
7 CMB Polarization Spectra W. Hu et al. astro-ph/ We need a large increase in sensitivity!
8 Galaxy Cluster Survey using SZ Effect Science Case
9 SZ Observations In contrast to X-ray emission, SZ surface brightness is independent of cluster redshift, clusters can be seen at any distance!
10 Galaxy Cluster Surveys Probe Dark Energy Cluster surveys probe (1) volume-redshift relation, (2) abundance evolution, (3) structural evolution
11 Large Focal Plane Bolometer-Arrays Approaching single pixel photon noise limit Next Step: Large format bolometer arrays Transition-edge Sensor Bolometer Entire fabrication is by optical photolithography Multiplexed readout in development
12 POLARBEAR J. Borrill, S. Cho, J. Clarke, Matt Dobbs, N. Halverson, W. Holzapfel, A.H. Jaffe, Z. Kermish, T. Lanting, A.T. Lee, M. Myers, R. O brient, P.L. Richards, H. Spieler, R. Stompor, H. Tran, M. White Ground-Based 3 meter Telescope at White Mountain CA Characterize E-modes Search for B-modes First Light LDRD seed funding
13 New Detector Technology: Antenna Coupled Bolometer 1 mm Fabricated in UCB Microlab by M.Meyers Silicon Lens used to focus the beam Filipovic et. al SEE TALK Y08 BY MIKE MYERS
14 POLARBEAR-I Performance A.H. Jaffe 15 x 15 deg. observed 1.2 µk rms per 5 pixel 200 nk rms per 30 pixel (re-pixelized map) T/S = 0.35 assumed
15 CMB Polarization Satellite One of three NASA Einstein Probes in roadmap is for CMB Polarization Study Proposed of mission named Experimental Probe of Inflationary Cosmology EPIC (JPL, CIT, UCB, LBNL, Minn, NIST, UColo,Stanford, CMU,Cardiff, Chicago, Dartmouth, Fermilab, Davis)
16 ALMA Pathfinder Experiment (APEX) Telescope Specifications: 12 m on-axis ALMA prototype. 45 resolution at 150 GHz. Located at 16,500 ft in the Chilean Andes. Assembly near complete in Chile! Berkeley Component NSF funded First light late 2004 MPIfR MPI Munich Berkeley Frank Bertoldi Rolf Guesten Ernst Kreysa Karl Menten Dirk Muders Andrea Racanelli Peter Schilke Hans Bohringer Sherry Cho Matt Dobbs Nils Halverson Bill Holzapfel Paul Richards Tom Plagge Adrian Lee Trevor Lanting Martin Leuker Jared Mehl Mike Myers Dan Schwan Helmuth Spieler Martin White
17 South Pole Telescope S. Cho, J. Carlstrom, P. Cheimets, J. Clarke, T. Crawford, Matt Dobbs, C. Greer, N. Halverson, W. Holzapfel, T. Lanting, A.T. Lee, E. Leitch, S. Myer, J. Mohr, S. Padin, C. Pryke, P.L. Richards, J. Ruhl, M. Runyan, H. Spieler 8m, off-axis design 1.3 resolution 100% time SZ observations Best mm-wave site First light NSF Funded: Chicago, Berkeley, CWRU, SAO APEX/SPT Complementarity: APEX will be operational 2-3 years before SPT, but SPT will have ~5x faster cluster finding rate.
18 TES Bolometer Array 6 identical wedges Array mask 14 cm 3.5 mm
19 Horn Antenna Coupled Bolometers Sunyaev-Zel dovich Effect Surveys 3 mm TES Spider Absorber Bolometer
20 APEX-SZ 54-Bolometer Wedge 7 cm Jared Mehl
21 Cosmology with APEX-SZ APEX-SZ PLANCK courtesy M. White
22 Single SQUID multiplexer One SQUID per row AC-bias => sum signals => demodulate 8-ch prototype tested with resistors Bolometer test SEE TALK E02 BY TREVOR LANTING
23 Conclusion Much more to learn from CMB photons! Polarization: Probe of physics at Gev Galaxy Clusters: Characterize Structure Formation, Dark Energy Needed step in instrumentation is imminent Control of systematic errors will be critical
24 STOP
25 PolarBeaR Performance r = tensor to scalar ratio POLARBEAR-I ( mk) POLARBEAR-II ( mk) n = tilt of primordial spectrum
26 Dark Energy and Mass Limit Systematic Errors Parameter Biases logm Ω E <w> σ 8 +25% % % % % % %
27 Pulse-Tube Cooler Testing 3.5 K 350 mk He10 fridge PTC 250 mk 50 K Closed He gas cycle No cryogens Reduces logistical and personnel demands 250 mk for 50 hours Microphonics tests underway Dan Schwan
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