The Balloon-Borne Large-Aperture Submillimeter Telescope For
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Proceedings of Spie
PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie Survey strategy optimization for the Atacama Cosmology Telescope De Bernardis, F., Stevens, J., Hasselfield, M., Alonso, D., Bond, J. R., et al. F. De Bernardis, J. R. Stevens, M. Hasselfield, D. Alonso, J. R. Bond, E. Calabrese, S. K. Choi, K. T. Crowley, M. Devlin, J. Dunkley, P. A. Gallardo, S. W. Henderson, M. Hilton, R. Hlozek, S. P. Ho, K. Huffenberger, B. J. Koopman, A. Kosowsky, T. Louis, M. S. Madhavacheril, J. McMahon, S. Næss, F. Nati, L. Newburgh, M. D. Niemack, L. A. Page, M. Salatino, A. Schillaci, B. L. Schmitt, N. Sehgal, J. L. Sievers, S. M. Simon, D. N. Spergel, S. T. Staggs, A. van Engelen, E. M. Vavagiakis, E. J. Wollack, "Survey strategy optimization for the Atacama Cosmology Telescope," Proc. SPIE 9910, Observatory Operations: Strategies, Processes, and Systems VI, 991014 (15 July 2016); doi: 10.1117/12.2232824 Event: SPIE Astronomical Telescopes + Instrumentation, 2016, Edinburgh, United Kingdom Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 06 Oct 2020 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use Survey strategy optimization for the Atacama Cosmology Telescope F. De Bernardisa, J. R. Stevensa, M. Hasselfieldb,c, D. Alonsod, J. R. Bonde, E. Calabresed, S. K. Choif, K. T. Crowleyf, M. Devling, J. Dunkleyd, P. A. Gallardoa, S. W. Hendersona, M. Hiltonh, R. Hlozeki, S. P. Hof, K. Huffenbergerj, B. J. Koopmana, A. Kosowskyk, T. Louisl, M. S. Madhavacherilm, J. McMahonn, S. Naessd, F. Natig, L. Newburghi, M. D. Niemacka, L. A. Pagef, M. Salatinof, A. -
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 -
Maturity of Lumped Element Kinetic Inductance Detectors For
Astronomy & Astrophysics manuscript no. Catalano˙f c ESO 2018 September 26, 2018 Maturity of lumped element kinetic inductance detectors for space-borne instruments in the range between 80 and 180 GHz A. Catalano1,2, A. Benoit2, O. Bourrion1, M. Calvo2, G. Coiffard3, A. D’Addabbo4,2, J. Goupy2, H. Le Sueur5, J. Mac´ıas-P´erez1, and A. Monfardini2,1 1 LPSC, Universit Grenoble-Alpes, CNRS/IN2P3, 2 Institut N´eel, CNRS, Universit´eJoseph Fourier Grenoble I, 25 rue des Martyrs, Grenoble, 3 Institut de Radio Astronomie Millim´etrique (IRAM), Grenoble, 4 LNGS - Laboratori Nazionali del Gran Sasso - Assergi (AQ), 5 Centre de Sciences Nucl´eaires et de Sciences de la Mati`ere (CSNSM), CNRS/IN2P3, bat 104 - 108, 91405 Orsay Campus Preprint online version: September 26, 2018 ABSTRACT This work intends to give the state-of-the-art of our knowledge of the performance of lumped element kinetic inductance detectors (LEKIDs) at millimetre wavelengths (from 80 to 180 GHz). We evaluate their optical sensitivity under typical background conditions that are representative of a space environment and their interaction with ionising particles. Two LEKID arrays, originally designed for ground-based applications and composed of a few hundred pixels each, operate at a central frequency of 100 and 150 GHz (∆ν/ν about 0.3). Their sensitivities were characterised in the laboratory using a dedicated closed-cycle 100 mK dilution cryostat and a sky simulator, allowing for the reproduction of realistic, space-like observation conditions. The impact of cosmic rays was evaluated by exposing the LEKID arrays to alpha particles (241Am) and X sources (109Cd), with a read-out sampling frequency similar to those used for Planck HFI (about 200 Hz), and also with a high resolution sampling level (up to 2 MHz) to better characterise and interpret the observed glitches. -
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. -
Arxiv:1412.0626V1 [Astro-Ph.CO] 1 Dec 2014 Versity, 3400 N
Draft: December 2, 2014 Preprint typeset using LATEX style emulateapj v. 05/12/14 THE ATACAMA COSMOLOGY TELESCOPE: LENSING OF CMB TEMPERATURE AND POLARIZATION DERIVED FROM COSMIC INFRARED BACKGROUND CROSS-CORRELATION Alexander van Engelen1,2, Blake D. Sherwin3, Neelima Sehgal2, Graeme E. Addison4, Rupert Allison5, Nick Battaglia6, Francesco de Bernardis7, J. Richard Bond1, Erminia Calabrese5, Kevin Coughlin8, Devin Crichton9, Rahul Datta8, Mark J. Devlin10, Joanna Dunkley5, Rolando Dunner¨ 11, Emily Grace12, Megan Gralla9, Amir Hajian1, Matthew Hasselfield13,4, Shawn Henderson7, J. Colin Hill14, Matt Hilton15, Adam D. Hincks4, Renee´ Hlozek13, Kevin M. Huffenberger16, John P. Hughes17, Brian Koopman7, Arthur Kosowsky18, Thibaut Louis5, Marius Lungu10, Mathew Madhavacheril2, Lo¨ıc Maurin11, Jeff McMahon8, Kavilan Moodley15, Charles Munson8, Sigurd Naess5, Federico Nati19, Laura Newburgh20, Michael D. Niemack7, Michael R. Nolta1, Lyman A. Page12, Christine Pappas12, Bruce Partridge21, Benjamin L. Schmitt10, Jonathan L. Sievers22,23,12, Sara Simon12, David N. Spergel13, Suzanne T. Staggs12, Eric R. Switzer24,1, Jonathan T. Ward10, Edward J. Wollack24 Draft: December 2, 2014 ABSTRACT We present a measurement of the gravitational lensing of the Cosmic Microwave Background (CMB) temperature and polarization fields obtained by cross-correlating the reconstructed convergence signal from the first season of ACTPol data at 146 GHz with Cosmic Infrared Background (CIB) fluctu- ations measured using the Planck satellite. Using an overlap area of 206 square degrees, we detect gravitational lensing of the CMB polarization by large-scale structure at a statistical significance of 4:5σ. Combining both CMB temperature and polarization data gives a lensing detection at 9:1σ sig- nificance. A B-mode polarization lensing signal is present with a significance of 3:2σ. -
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. -
A Bit of History Satellites Balloons Ground-Based
Experimental Landscape ● A Bit of History ● Satellites ● Balloons ● Ground-Based Ground-Based Experiments There have been many: ABS, ACBAR, ACME, ACT, AMI, AMiBA, APEX, ATCA, BEAST, BICEP[2|3]/Keck, BIMA, CAPMAP, CAT, CBI, CLASS, COBRA, COSMOSOMAS, DASI, MAT, MUSTANG, OVRO, Penzias & Wilson, etc., PIQUE, Polatron, Polarbear, Python, QUaD, QUBIC, QUIET, QUIJOTE, Saskatoon, SP94, SPT, SuZIE, SZA, Tenerife, VSA, White Dish & more! QUAD 2017-11-17 Ganga/Experimental Landscape 2/33 Balloons There have been a number: 19 GHz Survey, Archeops, ARGO, ARCADE, BOOMERanG, EBEX, FIRS, MAX, MAXIMA, MSAM, PIPER, QMAP, Spider, TopHat, & more! BOOMERANG 2017-11-17 Ganga/Experimental Landscape 3/33 Satellites There have been 4 (or 5?): Relikt, COBE, WMAP, Planck (+IRTS!) Planck 2017-11-17 Ganga/Experimental Landscape 4/33 Rockets & Airplanes For example, COBRA, Berkeley-Nagoya Excess, U2 Anisotropy Measurements & others... It’s difficult to get integration time on these platforms, so while they are still used in the infrared, they are no longer often used for the http://aether.lbl.gov/www/projects/U2/ CMB. 2017-11-17 Ganga/Experimental Landscape 5/33 (from R. Stompor) Radek Stompor http://litebird.jp/eng/ 2017-11-17 Ganga/Experimental Landscape 6/33 Other Satellite Possibilities ● US “CMB Probe” ● CORE-like – Studying two possibilities – Discussions ongoing ● Imager with India/ISRO & others ● Spectrophotometer – Could include imager – Inputs being prepared for AND low-angular- the Decadal Process resolution spectrophotometer? https://zzz.physics.umn.edu/ipsig/ -
Far Sidelobes from Baffles and Telescope Support Structures in the Atacama Cosmology Telescope
Far Sidelobes from Baffles and Telescope Support Structures in the Atacama Cosmology Telescope Patricio A. Gallardoa, Nicholas F. Cothardb, Roberto Pudduc, Rolando Dünnerd, Brian J. Koopmana, Michael D. Niemacka, Sara M. Simone, and Edward J. Wollackf aDepartment of Physics, Cornell University, Ithaca, NY 14853 USA bDepartment of Applied and Engineering Physics, Cornell University, Ithaca, NY 14853 USA cInstituto de Astrofísica, Pontificia Universidad Católica de Chile, Macul, Santiago, Chile dInstituto de Astrofísica y Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile, 7820436 Macul, Santiago, Chile eDepartment of Physics, University of Michigan, Ann Arbor, MI, 48103 fNASA/Goddard Space Flight Center, Greenbelt, MD, USA ABSTRACT The Atacama Cosmology Telescope (ACT) is a 6 m telescope located in the Atacama Desert, designed to measure the cosmic microwave background (CMB) with arcminute resolution. ACT, with its third generation polarization sensitive array, Advanced ACTPol, is being used to measure the anisotropies of the CMB in five frequency bands in large areas of the sky (∼ 15; 000 deg2). These measurements are designed to characterize the large scale structure of the universe, test cosmological models and constrain the sum of the neutrino masses. As the sensitivity of these wide surveys increases, the control and validation of the far sidelobe response becomes increasingly important and is particularly challenging as multiple reflections, spillover, diffraction and scattering become difficult to model and characterize at the required levels. In this work, we present a ray trace model of the ACT upper structure which is used to describe much of the observed far sidelobe pattern. This model combines secondary mirror spillover measurements with a 3D CAD model based on photogrammetry measurements to simulate the beam of the camera and the comoving ground shield. -
Development and Preliminary Results of Point Source Observations
The Atacama Cosmology Telescope: Development and Preliminary Results of Point Source Observations Ryan P. Fisher A DISSERTATION PRESENTED TO THE FACULTY OF PRINCETON UNIVERSITY IN CANDIDACY FOR THE DEGREE OF DOCTOR OF PHILOSOPHY RECOMMENDED FOR ACCEPTANCE BY THE DEPARTMENT OF PHYSICS [Adviser: Joseph W. Fowler] November 2009 c Copyright by Ryan Patrick Fisher, 2009. All rights reserved. Abstract The Atacama Cosmology Telescope (ACT) is a six meter diameter telescope designed to measure the millimeter sky with arcminute angular resolution. The instrument is cur- rently conducting its third season of observations from Cerro Toco in the Chilean Andes. The primary science goal of the experiment is to expand our understanding of cosmology by mapping the temperature fluctuations of the Cosmic Microwave Background (CMB) at angular scales corresponding to multipoles up to ` ∼ 10000: The primary receiver for current ACT observations is the Millimeter Bolometer Ar- ray Camera (MBAC). The instrument is specially designed to observe simultaneously at 148 GHz, 218 GHz and 277 GHz. To accomplish this, the camera has three separate de- tector arrays, each containing approximately 1000 detectors. After discussing the ACT experiment in detail, a discussion of the development and testing of the cold readout elec- tronics for the MBAC is presented. Currently, the ACT collaboration is in the process of generating maps of the microwave sky using our first and second season observations. The analysis used to generate these maps requires careful data calibration to produce maps of the arcminute scale CMB tem- perature fluctuations. Tests and applications of several elements of the ACT calibrations are presented in the context of the second season observations. -
THE ATACAMA Cosi'vl0logy TELESCOPE: the RECEIVER and INSTRUMENTATION L2 D
https://ntrs.nasa.gov/search.jsp?R=20120002550 2019-08-30T19:06:35+00:00Z CORE Metadata, citation and similar papers at core.ac.uk Provided by NASA Technical Reports Server THE ATACAMA COSi'vl0LOGY TELESCOPE: THE RECEIVER AND INSTRUMENTATION L2 D. S. SWETZ , P. A. R. ADE\ j'vI. A !\fIRrl, J. \V'. ApPEL" E. S. BATTISTELLlfi,j, B. BURGERI, J. CHERVENAK', 2 lVI. J. DEVLIN], S. R. DICKER]. \V. B. DORIESE , R. DUNNER', T. ESSINGER-HILEMAN'. R. P. FISHER:', J. \V. FOWLER'. 4 2 1 lVI. HALPERN ,!.VI. HASSELFIELD4, G. C. HILTON , A. D. HINCKS\ K. D. IRWIN2. N. JAROSIK', M. KAlIL', J. KLEIN , . ull 11 I2 l l u 1 J. J\1. LAd "" M. LIMON , T. A. l'vIARRIAGE . D. MARSDEN , K. J\IARTOCCI : , P. J\IAUSKOPF: , H. MOSELEY', I4 2 C. B. NETTERFIELD , J\1. D. NIEMACK " l'vI. R. NOLTA ,L. A. PAGE". L. PARKER'. S. T. STAGGS", O. STRYZAK', 1 U jHi E. R. SWlTZER : , R. THORNTON • C. TUCKER'], E. \VOLLACK', Y. ZHAO" Draft version July 5, 2010 ABSTRACT The Atacama Cosmology Telescope was designed to measure small-scale anisotropies in the Cosmic Microwave Background and detect galaxy clusters through the Sunyaev-Zel'dovich effect. The instru ment is located on Cerro Taco in the Atacama Desert, at an altitude of 5190 meters. A six-met.er off-axis Gregorian telescope feeds a new type of cryogenic receiver, the Millimeter Bolometer Array Camera. The receiver features three WOO-element arrays of transition-edge sensor bolometers for observations at 148 GHz, 218 GHz, and 277 GHz.