THE ATACAMA Cosi'vl0logy TELESCOPE: the RECEIVER and INSTRUMENTATION L2 D
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The Atacama Cosmology Telescope: Extragalactic Sources at 148 Ghz in the 2008 Survey
Haverford College Haverford Scholarship Faculty Publications Astronomy 2011 The Atacama Cosmology Telescope: Extragalactic Sources at 148 GHz in the 2008 Survey Tobias A. Marriage Jean-Baptise Juin Yen-Ting Lin Bruce Partridge Haverford College, [email protected] Follow this and additional works at: https://scholarship.haverford.edu/astronomy_facpubs Repository Citation The Atacama Cosmology Telescope: Extragalactic Sources at 148 GHz in the 2008 Survey Marriage, Tobias A.; Baptiste Juin, Jean; Lin, Yen-Ting; Marsden, Danica; Nolta, Michael R.; Partridge, Bruce; Ade, Peter A. R.; Aguirre, Paula; Amiri, Mandana; Appel, John William; Barrientos, L. Felipe; Battistelli, Elia S.; Bond, John R.; Brown, Ben; Burger, Bryce; Chervenak, Jay; Das, Sudeep; Devlin, Mark J.; Dicker, Simon R.; Bertrand Doriese, W.; Dunkley, Joanna; Dünner, Rolando; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Halpern, Mark; Hasselfield, Matthew; Hernández-Monteagudo, Carlos; Hilton, Gene C.; Hilton, Matt; Hincks, Adam D.; Hlozek, Renée; Huffenberger, Kevin M.; Handel Hughes, David; Hughes, John P.; Infante, Leopoldo; Irwin, Kent D.; Kaul, Madhuri; Klein, Jeff; Kosowsky, Arthur; Lau, Judy M.; Limon, Michele; Lupton, Robert H.; Martocci, Krista; Mauskopf, Phil; Menanteau, Felipe; Moodley, Kavilan; Moseley, Harvey; Netterfield, Calvin B.; Niemack, Michael .;D Page, Lyman A.; Parker, Lucas; Quintana, Hernan; Reid, Beth; Sehgal, Neelima; Sherwin, Blake D.; Sievers, Jon; Spergel, David N.; Staggs, Suzanne T.; Swetz, Daniel S.; Switzer, Eric R.; Thornton, Robert; Trac, Hy; Tucker, Carole; Warne, Ryan; Wilson, Grant; Wollack, Ed; Zhao, Yue The Astrophysical Journal, Volume 731, Issue 2, article id. 100, 15 pp. (2011). This Journal Article is brought to you for free and open access by the Astronomy at Haverford Scholarship. -
A Measurement of the Cosmic Microwave Background B-Mode Polarization with Polarbear
Publications of the Korean Astronomical Society pISSN: 1225-1534 30: 625 ∼ 628, 2015 September eISSN: 2287-6936 c 2015. The Korean Astronomical Society. All rights reserved. http://dx.doi.org/10.5303/PKAS.2015.30.2.625 A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND B-MODE POLARIZATION WITH POLARBEAR The Polarbear collaboration: P.A.R. Ade29, Y. Akiba33, A.E. Anthony2,5, K. Arnold14, M. Atlas14, D. Barron14, D. Boettger14, J. Borrill3,32, S. Chapman9, Y. Chinone17,13, M. Dobbs25, T. Elleflot14, J. Errard32,3, G. Fabbian1,18, C. Feng14, D. Flanigan13,10, A. Gilbert25, W. Grainger28, N.W. Halverson2,5,15, M. Hasegawa17,33, K. Hattori17, M. Hazumi17,33,20, W.L. Holzapfel13, Y. Hori17, J. Howard13,16, P. Hyland24, Y. Inoue33, G.C. Jaehnig2,15, A.H. Jaffe11, B. Keating14, Z. Kermish12, R. Keskitalo3, T. Kisner3,32, M. Le Jeune1, A.T. Lee13,27, E.M. Leitch4,19, E. Linder27, M. Lungu13,8, F. Matsuda14, T. Matsumura17, X. Meng13, N.J. Miller22, H. Morii17, S. Moyerman14, M.J. Myers13, M. Navaroli14, H. Nishino20, A. Orlando14, H. Paar14, J. Peloton1, D. Poletti1, E. Quealy13,26, G. Rebeiz6, C.L. Reichardt13, P.L. Richards13,31, C. Ross9, I. Schanning14, D.E. Schenck2,5, B.D. Sherwin13,21, A. Shimizu33, C. Shimmin13,7, M. Shimon30,14, P. Siritanasak14, G. Smecher34, H. Spieler27, N. Stebor14, B. Steinbach13, R. Stompor1, A. Suzuki13, S. Takakura23,17, T. Tomaru17, B. Wilson14, A. Yadav14, O. Zahn27 1AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cit´e,France 2Center for Astrophysics and Space -
The Q/U Imaging Experiment (QUIET): the Q-Band Receiver Array Instrument and Observations by Laura Newburgh Advisor: Professor Amber Miller
The Q/U Imaging ExperimenT (QUIET): The Q-band Receiver Array Instrument and Observations by Laura Newburgh Advisor: Professor Amber Miller Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2010 c 2010 Laura Newburgh All Rights Reserved Abstract The Q/U Imaging ExperimenT (QUIET): The Q-band Receiver Array Instrument and Observations by Laura Newburgh Phase I of the Q/U Imaging ExperimenT (QUIET) measures the Cosmic Microwave Background polarization anisotropy spectrum at angular scales 25 1000. QUIET has deployed two independent receiver arrays. The 40-GHz array took data between October 2008 and June 2009 in the Atacama Desert in northern Chile. The 90-GHz array was deployed in June 2009 and observations are ongoing. Both receivers observe four 15◦ 15◦ regions of the sky in the southern hemisphere that are expected × to have low or negligible levels of polarized foreground contamination. This thesis will describe the 40 GHz (Q-band) QUIET Phase I instrument, instrument testing, observations, analysis procedures, and preliminary power spectra. Contents 1 Cosmology with the Cosmic Microwave Background 1 1.1 The Cosmic Microwave Background . 1 1.2 Inflation . 2 1.2.1 Single Field Slow Roll Inflation . 3 1.2.2 Observables . 4 1.3 CMB Anisotropies . 6 1.3.1 Temperature . 6 1.3.2 Polarization . 7 1.3.3 Angular Power Spectrum Decomposition . 8 1.4 Foregrounds . 14 1.5 CMB Science with QUIET . 15 2 The Q/U Imaging ExperimenT Q-band Instrument 19 2.1 QUIET Q-band Instrument Overview . -
19 International Workshop on Low Temperature Detectors
19th International Workshop on Low Temperature Detectors Program version 1.24 - British Summer Time 1 Date Time Session Monday 19 July 14:00 - 14:15 Introduction and Welcome 14:15 - 15:15 Oral O1: Devices 1 15:15 - 15:25 Break 15:25 - 16:55 Oral O1: Devices 1 (continued) 16:55 - 17:05 Break 17:05 - 18:00 Poster P1: MKIDs and TESs 1 Tuesday 20 July 14:00 - 15:15 Oral O2: Cold Readout 15:15 - 15:25 Break 15:25 - 16:55 Oral O2: Cold Readout (continued) 16:55 - 17:05 Break 17:05 - 18:30 Poster P2: Readout, Other Devices, Supporting Science 1 20:00 - 21:00 Virtual Tour of NIST Quantum Sensor Group Labs Wednesday 21 July 14:00 - 15:15 Oral O3: Instruments 15:15 - 15:25 Break 15:25 - 16:55 Oral O3: Instruments (continued) 16:55 - 17:05 Break 17:05 - 18:30 Poster P3: Instruments, Astrophysics and Cosmology 1 18:00 - 19:00 Vendor Exhibitor Hour Thursday 22 July 14:00 - 15:15 Oral O4A: Rare Events 1 Oral O4B: Material Analysis, Metrology, Other 15:15 - 15:25 Break 15:25 - 16:55 Oral O4A: Rare Events 1 (continued) Oral O4B: Material Analysis, Metrology, Other (continued) 16:55 - 17:05 Break 17:05 - 18:30 Poster P4: Rare Events, Materials Analysis, Metrology, Other Applications 20:00 - 21:00 Virtual Tour of NIST Cleanoom Monday 26 July 23:00 - 00:15 Oral O5: Devices 2 00:15 - 00:25 Break 00:25 - 01:55 Oral O5: Devices 2 (continued) 01:55 - 02:05 Break 02:05 - 03:30 Poster P5: MMCs, SNSPDs, more TESs Tuesday 27 July 23:00 - 00:15 Oral O6: Warm Readout and Supporting Science 00:15 - 00:25 Break 00:25 - 01:55 Oral O6: Warm Readout and Supporting Science -
CMB Telescopes and Optical Systems to Appear In: Planets, Stars and Stellar Systems (PSSS) Volume 1: Telescopes and Instrumentation
CMB Telescopes and Optical Systems To appear in: Planets, Stars and Stellar Systems (PSSS) Volume 1: Telescopes and Instrumentation Shaul Hanany ([email protected]) University of Minnesota, School of Physics and Astronomy, Minneapolis, MN, USA, Michael Niemack ([email protected]) National Institute of Standards and Technology and University of Colorado, Boulder, CO, USA, and Lyman Page ([email protected]) Princeton University, Department of Physics, Princeton NJ, USA. March 26, 2012 Abstract The cosmic microwave background radiation (CMB) is now firmly established as a funda- mental and essential probe of the geometry, constituents, and birth of the Universe. The CMB is a potent observable because it can be measured with precision and accuracy. Just as importantly, theoretical models of the Universe can predict the characteristics of the CMB to high accuracy, and those predictions can be directly compared to observations. There are multiple aspects associated with making a precise measurement. In this review, we focus on optical components for the instrumentation used to measure the CMB polarization and temperature anisotropy. We begin with an overview of general considerations for CMB ob- servations and discuss common concepts used in the community. We next consider a variety of alternatives available for a designer of a CMB telescope. Our discussion is guided by arXiv:1206.2402v1 [astro-ph.IM] 11 Jun 2012 the ground and balloon-based instruments that have been implemented over the years. In the same vein, we compare the arc-minute resolution Atacama Cosmology Telescope (ACT) and the South Pole Telescope (SPT). CMB interferometers are presented briefly. We con- clude with a comparison of the four CMB satellites, Relikt, COBE, WMAP, and Planck, to demonstrate a remarkable evolution in design, sensitivity, resolution, and complexity over the past thirty years. -
The Design of the Ali CMB Polarization Telescope Receiver
The design of the Ali CMB Polarization Telescope receiver M. Salatinoa,b, J.E. Austermannc, K.L. Thompsona,b, P.A.R. Aded, X. Baia,b, J.A. Beallc, D.T. Beckerc, Y. Caie, Z. Changf, D. Cheng, P. Chenh, J. Connorsc,i, J. Delabrouillej,k,e, B. Doberc, S.M. Duffc, G. Gaof, S. Ghoshe, R.C. Givhana,b, G.C. Hiltonc, B. Hul, J. Hubmayrc, E.D. Karpela,b, C.-L. Kuoa,b, H. Lif, M. Lie, S.-Y. Lif, X. Lif, Y. Lif, M. Linkc, H. Liuf,m, L. Liug, Y. Liuf, F. Luf, X. Luf, T. Lukasc, J.A.B. Matesc, J. Mathewsonn, P. Mauskopfn, J. Meinken, J.A. Montana-Lopeza,b, J. Mooren, J. Shif, A.K. Sinclairn, R. Stephensonn, W. Sunh, Y.-H. Tsengh, C. Tuckerd, J.N. Ullomc, L.R. Valec, J. van Lanenc, M.R. Vissersc, S. Walkerc,i, B. Wange, G. Wangf, J. Wango, E. Weeksn, D. Wuf, Y.-H. Wua,b, J. Xial, H. Xuf, J. Yaoo, Y. Yaog, K.W. Yoona,b, B. Yueg, H. Zhaif, A. Zhangf, Laiyu Zhangf, Le Zhango,p, P. Zhango, T. Zhangf, Xinmin Zhangf, Yifei Zhangf, Yongjie Zhangf, G.-B. Zhaog, and W. Zhaoe aStanford University, Stanford, CA 94305, USA bKavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94305, USA cNational Institute of Standards and Technology, Boulder, CO 80305, USA dCardiff University, Cardiff CF24 3AA, United Kingdom eUniversity of Science and Technology of China, Hefei 230026 fInstitute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049 gNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 hNational Taiwan University, Taipei 10617 iUniversity of Colorado Boulder, Boulder, CO 80309, USA jIN2P3, CNRS, Laboratoire APC, Universit´ede Paris, 75013 Paris, France kIRFU, CEA, Universit´eParis-Saclay, 91191 Gif-sur-Yvette, France lBeijing Normal University, Beijing 100875 mAnhui University, Hefei 230039 nArizona State University, Tempe, AZ 85004, USA oShanghai Jiao Tong University, Shanghai 200240 pSun Yat-Sen University, Zhuhai 519082 ABSTRACT Ali CMB Polarization Telescope (AliCPT-1) is the first CMB degree-scale polarimeter to be deployed on the Tibetan plateau at 5,250 m above sea level. -
Clover: Measuring Gravitational-Waves from Inflation
ClOVER: Measuring gravitational-waves from Inflation Executive Summary The existence of primordial gravitational waves in the Universe is a fundamental prediction of the inflationary cosmological paradigm, and determination of the level of this tensor contribution to primordial fluctuations is a uniquely powerful test of inflationary models. We propose an experiment called ClOVER (ClObserVER) to measure this tensor contribution via its effect on the geometric properties (the so-called B-mode) of the polarization of the Cosmic Microwave Background (CMB) down to a sensitivity limited by the foreground contamination due to lensing. In order to achieve this sensitivity ClOVER is designed with an unprecedented degree of systematic control, and will be deployed in Antarctica. The experiment will consist of three independent telescopes, operating at 90, 150 or 220 GHz respectively, and each of which consists of four separate optical assemblies feeding feedhorn arrays arrays of superconducting detectors with phase as well as intensity modulation allowing the measurement of all three Stokes parameters I, Q and U in every pixel. This project is a combination of the extensive technical expertise and experience of CMB measurements in the Cardiff Instrumentation Group (Gear) and Cavendish Astrophysics Group (Lasenby) in UK, the Rome “La Sapienza” (de Bernardis and Masi) and Milan “Bicocca” (Sironi) CMB groups in Italy, and the Paris College de France Cosmology group (Giraud-Heraud) in France. This document is based on the proposal submitted to PPARC by the UK groups (and funded with 4.6ML), integrated with additional information on the Dome-C site selected for the operations. This document has been prepared to obtain an endorsement from the INAF (Istituto Nazionale di Astrofisica) on the scientific quality of the proposed experiment to be operated in the Italian-French base of Dome-C, and to be submitted to the Commissione Scientifica Nazionale Antartica and to the French INSU and IPEV. -
Planck Early Results. XX. New Light on Anomalous Microwave Emission from Spinning Dust Grains
A&A 536, A20 (2011) Astronomy DOI: 10.1051/0004-6361/201116470 & c ESO 2011 Astrophysics Planck early results Special feature Planck early results. XX. New light on anomalous microwave emission from spinning dust grains Planck Collaboration: P. A. R. Ade72, N. Aghanim46,M.Arnaud58, M. Ashdown56,4, J. Aumont46, C. Baccigalupi70,A.Balbi28, A. J. Banday77,7,63,R.B.Barreiro52, J. G. Bartlett3,54,E.Battaner79, K. Benabed47, A. Benoît45,J.-P.Bernard77,7, M. Bersanelli25,41, R. Bhatia5, J. J. Bock54,8, A. Bonaldi37,J.R.Bond6,J.Borrill62,73,F.R.Bouchet47, F. Boulanger46, M. Bucher3,C.Burigana40,P.Cabella28, B. Cappellini41, J.-F. Cardoso59,3,47,S.Casassus76, A. Catalano3,57, L. Cayón18, A. Challinor49,56,10, A. Chamballu43, R.-R. Chary44,X.Chen44,L.-Y.Chiang48, C. Chiang17,P.R.Christensen67,29,D.L.Clements43, S. Colombi47, F. Couchot61, A. Coulais57, B. P. Crill54,68, F. Cuttaia40,L.Danese70, R. D. Davies55,R.J.Davis55,P.deBernardis24,G.deGasperis28,A.deRosa40, G. de Zotti37,70, J. Delabrouille3, J.-M. Delouis47, C. Dickinson55, S. Donzelli41,50,O.Doré54,8,U.Dörl63, M. Douspis46, X. Dupac32, G. Efstathiou49,T.A.Enßlin63,H.K.Eriksen50, F. Finelli40, O. Forni77,7, M. Frailis39, E. Franceschi40,S.Galeotta39, K. Ganga3,44,R.T.Génova-Santos51,30,M.Giard77,7, G. Giardino33, Y. Giraud-Héraud3, J. González-Nuevo70,K.M.Górski54,81,S.Gratton56,49, A. Gregorio26, A. Gruppuso40,F.K.Hansen50,D.Harrison49,56,G.Helou8, S. Henrot-Versillé61, D. Herranz52,S.R.Hildebrandt8,60,51,E.Hivon47, M. -
Muse: a Novel Experiment for CMB Polarization Measurement Using Highly Multimoded Bolometers
The Atacama B-mode Search Status and Prospect CMB 2013 June 11th, 2013, Okinawa, Japan Akito Kusaka (Princeton University) for ABS Collaboration Before starting my talk… Atmosphere is unpolarized ABS (Atacama B-mode Search) Princeton, Johns Hopkins, NIST, UBC, U. Chile What is ABS? Ground based CMB polarization (with T sensitivity) Angular scale: l~100(~2), B-mode from GW TES bolometer at 150 GHz › 240 pixel / 480 bolometers › ~80% of channels are regularly functional › NEQ ~ 30 mKs (w/ dead channels, pol. efficiency included) Unique Systematic error mitigation › Cold optics › Continuously rotating half-wave plate Site Chile, Cerro Toco › ~5150 m. › Extremely low moisture › Year-round access › Observing throughout the year › And day and night ACT, ABS, PolarBear, CLASS Cerro Chajnantor 5612 m (5150 m) Cerro Toco 5600 m TAO, CCAT Google Earth / Google Map / Google Earth 1 km APEX QUIET, CBI ALMA (5050 m) ASTE & NANTEN2 (4800 m) Possible combined analysis among CMB experiments Many figures / pictures are from theses of ABS instrument T. Essinger-Hileman and J. W. Appel (+ K. Visnjic and L. P. Parker soon) Optics 4 K cooled side-fed Dragone dual reflector. ~60 cm diameter mirrors. 25 cm aperture diameter. Optics Aperture The optics maximize throughput for small aperture 12 radius field of view Good image quality across the wide field of view ABS focal plane Feedhorn coupled Focal plane ~300 mK Polarization sensitive TES Ex TES Inline filter OMT Ey TES 1.6 mm 5 mm ~30 cm Fabricated at NIST Focal Plane Elements Individually machined -
A Ground-Based Probe of Cosmic Microwave Background Polarization
Q/U Imaging ExperimenT (QUIET): a ground-based probe of cosmic microwave background polarization Immanuel Buder for the QUIET Collaboration Department of Physics, U. of Chicago, 933 E. 56th St., Chicago, IL USA 60637 ABSTRACT QUIET is an experimental program to measure the polarization of the Cosmic Microwave Background (CMB) radiation from the ground. Previous CMB polarization data have been used to constrain the cosmological parameters that model the history of our universe. The exciting target for current and future experiments is detecting and measuring the faint polarization signals caused by gravity waves from the inflationary epoch which 30 occurred < 10− s after the Big Bang. QUIET has finished an observing season at 44 GHz (Q-Band); observing at 95 GHz (W-Band) is ongoing. The instrument incorporates several technologies and approaches novel to CMB experiments. We describe the observing strategy, optics design, detector technology, and data acquisition. These systems combine to produce a polarization sensitivity of 64 (57) µK for a 1 s exposure of the Phase I Q (W) Band array. We describe the QUIET Phase I instrument and explain how systematic errors are reduced and quantified. Keywords: QUIET, cosmic microwave background, cosmology observations, instrumentation: polarimeters 1. INTRODUCTION QUIET is an experimental program to measure the polarization anisotropy of the Cosmic Microwave Background (CMB). In the last few years, increasingly precise measurements1–4 of the polarization have helped both to verify the standard cosmological model and to provide some constraints on cosmological parameters. The polarization of the CMB is uniquely sensitive to primordial gravity waves, which create characteristic degree scale divergence free polarization patterns on the sky known as B-modes. -
The Cℓover Experiment
Invited Paper The CℓOVER Experiment L. Piccirillo1, P. Ade2, M. D. Audley3, C. Baines1, R. Battye1, M. Brown3, P. Calisse2, A. Challinor5,6, W. D. Duncan7, P. Ferreira4, W. Gear2, D. M. Glowacka3, D. Goldie3, P.K. Grimes4, M. Halpern8, V. Haynes1, G. C. Hilton7, K. D. Irwin7, B. Johnson4, M. Jones4, A. Lasenby3, P. Leahy1, J. Leech4, S. Lewis1, B. Maffei1, L. Martinis1, P. D. Mauskopf2, S. J. Melhuish1, C. E. North4, D. O'Dea3, S. Parsley2, G. Pisano1, C. D. Reintsema7, G. Savini2, R.V. Sudiwala2, D. Sutton4, A. Taylor4, G. Teleberg2, D. Titterington3, V. N. Tsaneva3, C. Tucker2, R. Watson1, S. Withington3, G. Yassin4, J. Zhang2 1 School of Physics and Astronomy, University of Manchester, UK 2 School of Physics and Astronomy, Cardiff University, UK 3 Cavendish Laboratory, University of Cambridge, Cambridge, UK 4 Astrophysics, University of Oxford, Oxford, UK 5 Institute of Astronomy, University of Cambridge, Cambridge, UK 6 DAMTP, University of Cambridge, Cambridge, UK 7 National Institute of Standards and Technology, USA 8 University of British Columbia, Canada CℓOVER is a multi-frequency experiment optimised to measure the Cosmic Microwave Background (CMB) polarization, in particular the B- mode component. CℓOVER comprises two instruments observing respectively at 97 GHz and 150/225 GHz. The focal plane of both instruments consists of an array of corrugated feed-horns coupled to TES detectors cooled at 100 mK. The primary science goal of CℓOVER is to be sensitive to gravitational waves down to r ~ 0.03 (at 3σ) in two years of operations. 1 Introduction The Cosmic Microwave Background (CMB) Radiation is a very powerful tool to study the origin and evolution of the Universe. -
No Slide Title
Program for Small Scale Anisotropy Measurements and the Ability to set Limits on Inflation. A. Lee, L.Page and J. Ruhl 1 l>1000 CMB/SZ Experiments ACBAR (Bolometric feed array) ACT SPT AMiBA (Taiwan, Interferometer) SuZie Upgrade AMI (UK, Interferometer) SZA (Interferometer) APEX VSA (Interferometer) Bolocam (Bolometric Camera, CSO) CBI (Interferometer) 2 Selected Bolometer-Array and SZ Roadmap APEX SCUBA2 (~400 bolometers) (12000 bolometers) SZA Chile (Interferometer) Owens Valley ACT (3000 bolometers) Chile CMBPOL 2003 2005 2007 2004 2006 2008 SPT ALMA Polarbear-I (1000 bolometers) (Interferometer) (300 bolometers) South Pole Chile California Planck (50 bolometers) L2 3 ACT Collaboration Cardiff NASA/GSFC Princeton Peter Ade Domonic Benford Joe Fowler Cindy Hunt Jay Chervenak Norm Jarosik Phil Mauskopf Harvey Moseley Robert Lupton Carl Stahle Bob Margolis Columbia Ed Wollack Lyman Page Uros Seljak Amber Miller Penn David Spergel CUNY Angelica de Oliveira Costa Suzanne Staggs Martin Spergel Mark Devlin Simon Dicker Rutgers Haverford Bhuvnesh Jain Laura Ferrarese Steve Boughn Raul Jimenez Arthur Kosowsky Bruce Partridge Jeff Klein Jack Hughes Max Tegmark Ted Williams INOAE Licia Verde David Hughes Univ. de Catolica UMass Hernan Quintana NIST/Boulder Grant Wilson Univ. of Toronto Randy Doriese Univ. of British Columbia Kent Irwin Barth Netterfield Mark Halpern 4 Science: Observations: AtacamaACT Cosmology Telescope Growth of structure CMB: l>1000 Eqn. of state Cluster (SZ, KSZ X-rays, & optical) Neutrino mass Diffuse SZ Ionization history