THE ATACAMA COSMOLOGY TELESCOPE: THE POLARIZATION-SENSITIVE ACTPol INSTRUMENT
R. J. ThorntonDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAP. A. R. AdeSchool of Physics and Astronomy, Cardiff University, The Parade, Cardiff, Wales, CF24 3AA, UKS. AiolaDepartment of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USAF. E. AngilèDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAM. AmiriDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC, V6T 1Z4, CanadaJ. A. BeallNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAD. T. BeckerNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAH-M. ChoSLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USAS. K. ChoiJoseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544, USAP. CorliesDepartment of Physics, Cornell University, Ithaca, NY 14853, USAK. P. CoughlinDepartment of Physics, University of Michigan Ann Arbor, MI 48109, USAR. DattaDepartment of Physics, University of Michigan Ann Arbor, MI 48109, USAM. J. DevlinDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAS. R. DickerDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAR. DünnerInstituto de Astrofísica and Centro de Astro-Ingeniería, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, ChileJ. W. FowlerNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAA. E. FoxNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAP. A. GallardoDepartment of Physics, Cornell University, Ithaca, NY 14853, USAJ. GaoNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAE. GraceJoseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544, USAM. HalpernDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC, V6T 1Z4, CanadaM. HasselfieldDepartment of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USAS. W. HendersonDepartment of Physics, Cornell University, Ithaca, NY 14853, USAG. C. HiltonNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAA. D. HincksDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC, V6T 1Z4, CanadaS. P. HoJoseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544, USAJ. HubmayrNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAK. D. IrwinDepartment of Physics, Stanford University, Stanford, CA 94305, USAJ. KleinDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAB. KoopmanDepartment of Physics, Cornell University, Ithaca, NY 14853, USADale LiSLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USAT. LouisUPMC Univ Paris 06, UMR7095, Institut d’Astrophysique de Paris, F-75014, Paris, FranceM. LunguDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAL. MaurinInstituto deAstrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, ChileJ. McMahonDepartment of Physics, University of Michigan Ann Arbor, MI 48109, USAC. D. MunsonDepartment of Physics, University of Michigan Ann Arbor, MI 48109, USAS. NaessSub-Department of Astrophysics, University of Oxford, Keble Road, Oxford, OX1 3RH, UKF. NatiDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAL. NewburghDunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, Ontario, M5S 3H14, CanadaJ. NibargerNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAM. D. NiemackDepartment of Physics, Cornell University, Ithaca, NY 14853, USAP. NiraulaM. R. NoltaCanadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, M5S 3H8, CanadaL. A. PageJoseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544, USAC. G. PappasJoseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544, USAA. SchillaciJoseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544, USAB. L. SchmittDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAN. SehgalPhysics and Astronomy Department, Stony Brook University, Stony Brook, NY 11794-3800, USAJ. L. SieversAstrophysics and Cosmology Research Unit, School of Chemistry and Physics, University of KwaZulu-Natal, Durban, South Africa National Institute for Theoretical Physics, KwaZulu-Natal, South AfricaS. M. SimonJoseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544, USAS. T. StaggsJoseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544, USAC. TuckerSchool of Physics and Astronomy, Cardiff University, The Parade, Cardiff, Wales, CF24 3AA, UKM. UeharaJ. van LanenNIST Quantum Sensors Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAJ. T. WardDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAE. J. WollackNASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
2016en
ABI
Аннотация
ABSTRACT The Atacama Cosmology Telescope (ACT) makes high angular resolution measurements of anisotropies in the Cosmic Microwave Background (CMB) at millimeter wavelengths. We describe ACTPol, an upgraded receiver for ACT, which uses feedhorn-coupled, polarization-sensitive detector arrays, a 3° field of view, 100 mK cryogenics with continuous cooling, and meta material antireflection coatings. ACTPol comprises three arrays with separate cryogenic optics: two arrays at a central frequency of 148 GHz and one array operating simultaneously at both 97 GHz and 148 GHz. The combined instrument sensitivity, angular resolution, and sky coverage are optimized for measuring angular power spectra, clusters via the thermal Sunyaev–Zel’dovich (SZ) and kinetic SZ signals, and CMB lensing due to large-scale structure. The receiver was commissioned with its first 148 GHz array in 2013, observed with both 148 GHz arrays in 2014, and has recently completed its first full season of operations with the full suite of three arrays. This paper provides an overview of the design and initial performance of the receiver and related systems.
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