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  • 1. Ade, Peter
    et al.
    Aguirre, James
    Ahmed, Zeeshan
    Aiola, Simone
    Ali, Aamir
    Alonso, David
    Alvarez, Marcelo A.
    Arnold, Kam
    Ashton, Peter
    Austermann, Jason
    Awan, Humna
    Baccigalupi, Carlo
    Baildon, Taylor
    Barron, Darcy
    Battaglia, Nick
    Battye, Richard
    Baxter, Eric
    Bazarko, Andrew
    Beall, James A.
    Bean, Rachel
    Beck, Dominic
    Beckman, Shawn
    Beringue, Benjamin
    Bianchini, Federico
    Boada, Steven
    Boettger, David
    Bond, J. Richard
    Borrill, Julian
    Brown, Michael L.
    Bruno, Sarah Marie
    Bryan, Sean
    Calabrese, Erminia
    Calafut, Victoria
    Calisse, Paolo
    Carron, Julien
    Challinor, Anthony
    Chesmore, Grace
    Chinone, Yuji
    Chluba, Jens
    Cho, Hsiao-Mei Sherry
    Choi, Steve
    Coppi, Gabriele
    Cothard, Nicholas F.
    Coughlin, Kevin
    Crichton, Devin
    Crowley, Kevin D.
    Crowley, Kevin T.
    Cukierman, Ari
    D'Ewart, John M.
    Dunner, Rolando
    de Haan, Tijmen
    Devlin, Mark
    Dicker, Simon
    Didier, Joy
    Dobbs, Matt
    Dober, Bradley
    Duell, Cody J.
    Duff, Shannon
    Duivenvoorden, Adri
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Dunkley, Jo
    Dusatko, John
    Errard, Josquin
    Fabbian, Giulio
    Feeney, Stephen
    Ferraro, Simone
    Fluxa, Pedro
    Freese, Katherine
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). University of Michigan, U.S.A..
    Frisch, Josef C.
    Frolov, Andrei
    Fuller, George
    Fuzia, Brittany
    Galitzki, Nicholas
    Gallardo, Patricio A.
    Ghersi, Jose Tomas Galvez
    Gao, Jiansong
    Gawiser, Eric
    Gerbino, Martina
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Gluscevic, Vera
    Goeckner-Wald, Neil
    Golec, Joseph
    Gordon, Sam
    Gralla, Megan
    Green, Daniel
    Grigorian, Arpi
    Groh, John
    Groppi, Chris
    Guan, Yilun
    Gudmundsson, Jon E.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Han, Dongwon
    Hargrave, Peter
    Hasegawa, Masaya
    Hasselfield, Matthew
    Hattori, Makoto
    Haynes, Victor
    Hazumi, Masashi
    He, Yizhou
    Healy, Erin
    Henderson, Shawn W.
    Hervias-Caimapo, Carlos
    Hill, Charles A.
    Hill, J. Colin
    Hilton, Gene
    Hilton, Matt
    Hincks, Adam D.
    Hinshaw, Gary
    Hlozek, Renee
    Ho, Shirley
    Ho, Shuay-Pwu Patty
    Howe, Logan
    Huang, Zhiqi
    Hubmayr, Johannes
    Huffenberger, Kevin
    Hughes, John P.
    Ijjas, Anna
    Ikape, Margaret
    Irwin, Kent
    Jaffe, Andrew H.
    Jain, Bhuvnesh
    Jeong, Oliver
    Kaneko, Daisuke
    Karpel, Ethan D.
    Katayama, Nobuhiko
    Keating, Brian
    Kernasovskiy, Sarah S.
    Keskitalo, Reijo
    Kisner, Theodore
    Kiuchi, Kenji
    Klein, Jeff
    Knowles, Kenda
    Koopman, Brian
    Kosowsky, Arthur
    Krachmalnicoff, Nicoletta
    Kuenstner, Stephen E.
    Kuo, Chao-Lin
    Kusaka, Akito
    Lashner, Jacob
    Lee, Adrian
    Lee, Eunseong
    Leon, David
    Leung, Jason S-Y
    Lewis, Antony
    Li, Yaqiong
    Li, Zack
    Limon, Michele
    Linder, Eric
    Lopez-Caraballo, Carlos
    Louis, Thibaut
    Lowry, Lindsay
    Lungu, Marius
    Madhavacheril, Mathew
    Mak, Daisy
    Maldonado, Felipe
    Mani, Hamdi
    Mates, Ben
    Matsuda, Frederick
    Maurin, Loic
    Mauskopf, Phil
    May, Andrew
    McCallum, Nialh
    McKenney, Chris
    McMahon, Jeff
    Meerburg, P. Daniel
    Meyers, Joel
    Miller, Amber
    Mirmelstein, Mark
    Moodley, Kavilan
    Munchmeyer, Moritz
    Munson, Charles
    Naess, Sigurd
    Nati, Federico
    Navaroli, Martin
    Newburgh, Laura
    Ho, Nam
    Niemack, Michael
    Nishino, Haruki
    Orlowski-Scherer, John
    Page, Lyman
    Partridge, Bruce
    Peloton, Julien
    Perrotta, Francesca
    Piccirillo, Lucio
    Pisano, Giampaolo
    Poletti, Davide
    Puddu, Roberto
    Puglisi, Giuseppe
    Raum, Chris
    Reichardt, Christian L.
    Remazeilles, Mathieu
    Rephaeli, Yoel
    Riechers, Dominik
    Rojas, Felipe
    Roy, Anirban
    Sadeh, Sharon
    Sakurail, Yuki
    Salatino, Maria
    Rao, Mayuri Sathyanarayana
    Schaan, Emmanuel
    Schmittfull, Marcel
    Sehgal, Neelima
    Seibert, Joseph
    Seljak, Uros
    Sherwin, Blake
    Shimon, Meir
    Sierra, Carlos
    Sievers, Jonathan
    Sikhosana, Precious
    Silva-Feaver, Maximiliano
    Simon, Sara M.
    Sinclair, Adrian
    Siritanasak, Praween
    Smith, Kendrick
    Smith, Stephen R.
    Spergel, David
    Staggs, Suzanne T.
    Stein, George
    Stevens, Jason R.
    Stompor, Radek
    Suzuki, Aritoki
    Tajima, Osamu
    Takakura, Satoru
    Teply, Grant
    Thomas, Daniel B.
    Thorne, Ben
    Thornton, Robert
    Trac, Hy
    Tsai, Calvin
    Tucker, Carole
    Ullom, Joel
    Vagnozzi, Sunny
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    van Engelen, Alexander
    Van Lanen, Jeff
    Van Winkle, Daniel D.
    Vavagiakis, Eve M.
    Verges, Clara
    Vissers, Michael
    Wagoner, Kasey
    Walker, Samantha
    Ward, Jon
    Westbrook, Ben
    Whitehorn, Nathan
    Williams, Jason
    Williams, Joel
    Wollack, Edward J.
    Xu, Zhilei
    Yu, Byeonghee
    Yu, Cyndia
    Zago, Fernando
    Zhang, Hezi
    Zhu, Ningfeng
    The Simons Observatory: science goals and forecasts2019In: Journal of Cosmology and Astroparticle Physics, ISSN 1475-7516, E-ISSN 1475-7516, no 2, article id 056Article in journal (Refereed)
    Abstract [en]

    The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial con figuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping approximate to 10% of the sky to a white noise level of 2 mu K-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of sigma(r) = 0.003. The large aperture telescope will map approximate to 40% of the sky at arcminute angular resolution to an expected white noise level of 6 mu K-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.

  • 2. Bergman, A. S.
    et al.
    Ade, P. A. R.
    Akers, S.
    Amiri, M.
    Austermann, J. A.
    Beall, J. A.
    Becker, D. T.
    Benton, S. J.
    Bock, J. J.
    Bond, J. R.
    Bryan, S. A.
    Chiang, H. C.
    Contaldi, C. R.
    Domagalski, R. S.
    Dore, O.
    Duff, S. M.
    Duivenvoorden, Adri J.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Eriksen, H. K.
    Farhang, M.
    Filippini, J. P.
    Fissel, L. M.
    Fraisse, A. A.
    Freese, Katherine
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). University of Michigan, USA.
    Galloway, M.
    Gambrel, A. E.
    Gandilo, N. N.
    Ganga, K.
    Grigorian, A.
    Gualtieri, R.
    Gudmundsson, Jón E.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Halpern, M.
    Hartley, J.
    Hasselfield, M.
    Hilton, G.
    Holmes, W.
    Hristov, V. V.
    Huang, Z.
    Hubmayr, J.
    Irwin, K. D.
    Jones, W. C.
    Khan, A.
    Kuo, C. L.
    Kermish, Z. D.
    Li, S.
    Mason, P. V.
    Megerian, K.
    Moncelsi, L.
    Morford, T. A.
    Nagy, J. M.
    Netterfield, C. B.
    Nolta, M.
    Osherson, B.
    Padilla, I. L.
    Racine, B.
    Rahlin, A. S.
    Redmond, S.
    Reintsema, C.
    Romualdez, L. J.
    Ruhl, J. E.
    Runyan, M. C.
    Ruud, T. M.
    Shariff, J. A.
    Shaw, E. C.
    Shiu, C.
    Soler, J. D.
    Song, X.
    Trangsrud, A.
    Tucker, C.
    Tucker, R. S.
    Turner, A. D.
    Ullom, J.
    van der List, J. F.
    Van Lanen, J.
    Vissers, M. R.
    Weber, A. C.
    Wehus, I. K.
    Wen, S.
    Wiebe, D. V.
    Young, E. Y.
    280 GHz Focal Plane Unit Design and Characterization for the SPIDER-2 Suborbital Polarimeter2018In: Journal of Low Temperature Physics, ISSN 0022-2291, E-ISSN 1573-7357, Vol. 193, no 5-6, p. 1075-1084Article in journal (Refereed)
    Abstract [en]

    We describe the construction and characterization of the 280 GHz bolometric focal plane units (FPUs) to be deployed on the second flight of the balloon-borne SPIDER instrument. These FPUs are vital to SPIDER's primary science goal of detecting or placing an upper limit on the amplitude of the primordial gravitational wave signature in the cosmic microwave background (CMB) by constraining the B-mode contamination in the CMB from Galactic dust emission. Each 280 GHz focal plane contains a 16 x 16 grid of corrugated silicon feedhorns coupled to an array of aluminum-manganese transition-edge sensor (TES) bolometers fabricated on 150 mm diameter substrates. In total, the three 280 GHz FPUs contain 1530 polarization-sensitive bolometers (765 spatial pixels) optimized for the low loading environment in flight and read out by time-division SQUID multiplexing. In this paper, we describe the mechanical, thermal, and magnetic shielding architecture of the focal planes and present cryogenic measurements which characterize yield and the uniformity of several bolometer parameters. The assembled FPUs have high yields, with one array as high as 95% including defects from wiring and readout. We demonstrate high uniformity in device parameters, finding the median saturation power for each TES array to be similar to 3 pW at 300 mK with a less than 6% variation across each array at 1 sigma. These focal planes will be deployed alongside the 95 and 150 GHz telescopes in the SPIDER-2 instrument, slated to fly from McMurdo Station in Antarctica in December 2018.

  • 3.
    Duivenvoorden, Adriaan J.
    et al.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Gudmundsson, Jon E.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Rahlin, Alexandra S.
    Full-sky beam convolution for cosmic microwave background applications2019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 486, no 4, p. 5448-5467Article in journal (Refereed)
    Abstract [en]

    We introduce a publicly available full-sky beam convolution code library intended to inform the design of future cosmic microwave background instruments and help current experiments probe potential systematic effects. The code can be used to assess the impact of optical systematics on all stages of data reduction for a realistic experiment, including analyses beyond power spectrum estimation, by generating signal timelines that may serve as input to full analysis pipelines. The design and mathematical framework of the PYTHON code is discussed along with a few simple benchmarking results. We present a simple two-lens refracting telescope design and use it together with the code to simulate a year-long data set for 400 detectors scanning the sky on a satellite instrument. The simulation results identify a number of sub-leading optical non-idealities and demonstrate significant B-mode residuals caused by extended sidelobes that are sensitive to polarized radiation from the Galaxy. For the proposed design and satellite scanning strategy, we show that a full physical optics beam model generates B-mode systematics that differ significantly from the simpler elliptical Gaussian model.

  • 4.
    Duivenvoorden, Adriaan Judocus
    Stockholm University, Faculty of Science, Department of Physics.
    Probing the early Universe with B-mode polarization: The Spider instrument, optical modelling and non-Gaussianity2019Doctoral thesis, comprehensive summary (Other academic)
    Abstract [en]

    One of the main goals of modern observational cosmology is to constrain or detect a stochastic background of primordial gravitational waves. The existence of such a background is a generic prediction of the inflationary paradigm: the leading explanation for the universe's initial perturbations. A detection of the gravitational wave signal would provide strong evidence for the paradigm and would amount to an indirect probe of an energy scale far beyond that of conventional physics. Several dedicated experiments search for the signal by performing highly accurate measurements of a unique probe of the primordial gravitational wave background: the B-mode signature in the polarization of the cosmic microwave background (CMB) radiation. A part of this thesis is devoted to one of these experiments: the balloon-borne Spider instrument. The analysis of the first dataset, obtained in two (95 and 150 GHz) frequency bands during a January 2015 Antarctic flight, is described, along with details on the characterisation of systematic signal and the calibration of the instrument. The case of systematic signal due to poorly understood optical properties is treated in more detail. In the context of upcoming experiments, a study of systematic optical effects is presented as well as a numerically efficient method to consistently propagate such effects through an analysis pipeline. This is achieved by a `beam convolution' algorithm capable of simulating the contribution from the entire sky, weighted by the optical response, to the instrument's time-ordered data. It is described how the algorithm can be employed to forecast the performance of upcoming CMB experiments. In the final part of the thesis, an additional use of upcoming B-mode data is described. Constraints on the non-Gaussian correlation between the large-angular-scale B-mode field and the CMB temperature or E-mode anisotropies on small angular scales constitute a rigorous consistency check of the inflationary paradigm. An efficient statistical estimation procedure, a generalised bispectrum estimator, is derived and the constraining power of upcoming CMB data is explored.

  • 5.
    Duivenvoorden, Adriaan
    et al.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Meerburg, Pieter Daniel
    Freese, Katherine
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    CMB B-mode non-Gaussianity I: Optimal bispectrum estimator and Fisher ForecastsManuscript (preprint) (Other academic)
  • 6. Gualtieri, R.
    et al.
    Filippini, J. P.
    Ade, P. A. R.
    Amiri, M.
    Benton, S. J.
    Bergman, A. S.
    Bihary, R.
    Bock, J. J.
    Bond, J. R.
    Bryan, S. A.
    Chiang, H. C.
    Contaldi, C. R.
    Dore, O.
    Duivenvoorden, Adri J.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Eriksen, H. K.
    Farhang, M.
    Fissel, L. M.
    Fraisse, A. A.
    Freese, Katherine
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). University of Michigan, USA.
    Galloway, M.
    Gambrel, A. E.
    Gandilo, N. N.
    Ganga, K.
    Gramillano, R. V.
    Gudmundsson, Jón E.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Halpern, M.
    Hartley, J.
    Hasselfield, M.
    Hilton, G.
    Holmes, W.
    Hristov, V. V.
    Huang, Z.
    Irwin, K. D.
    Jones, W. C.
    Kuo, C. L.
    Kermish, Z. D.
    Li, S.
    Mason, P. V.
    Megerian, K.
    Moncelsi, L.
    Morford, T. A.
    Nagy, J. M.
    Netterfield, C. B.
    Nolta, M.
    Osherson, B.
    Padilla, I. L.
    Racine, B.
    Rahlin, A. S.
    Reintsema, C.
    Ruhl, J. E.
    Runyan, M. C.
    Ruud, T. M.
    Shariff, J. A.
    Soler, J. D.
    Song, X.
    Trangsrud, A.
    Tucker, C.
    Tucker, R. S.
    Turner, A. D.
    van der List, J. F.
    Weber, A. C.
    Wehus, I. K.
    Wiebe, D. V.
    Young, E. Y.
    SPIDER: CMB Polarimetry from the Edge of Space2018In: Journal of Low Temperature Physics, ISSN 0022-2291, E-ISSN 1573-7357, Vol. 193, no 5-6, p. 1112-1121Article in journal (Refereed)
    Abstract [en]

    SPIDER is a balloon-borne instrument designed to map the polarization of the millimeter-wave sky at large angular scales. Spider targets the B-mode signature of primordial gravitational waves in the cosmic microwave background (CMB), with a focus on mapping a large sky area with high fidelity at multiple frequencies. SPIDER's first long-duration balloon (LDB) flight in January 2015 deployed a total of 2400 antenna-coupled transition-edge sensors (TESs) at 90 GHz and 150 GHz. In this work we review the design and in-flight performance of the SPIDER instrument, with a particular focus on the measured performance of the detectors and instrument in a space-like loading and radiation environment. SPIDER's second flight in December 2018 will incorporate payload upgrades and new receivers to map the sky at 285 GHz, providing valuable information for cleaning polarized dust emission from CMB maps.

  • 7. Nagy, J. M.
    et al.
    Ade, P. A. R.
    Amiri, M.
    Benton, S. J.
    Bergman, A. S.
    Bihary, R.
    Bock, J. J.
    Bond, J. R.
    Bryan, S. A.
    Chiang, H. C.
    Contaldi, C. R.
    Dore, O.
    Duivenvoorden, Adri J.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Eriksen, H. K.
    Farhang, M.
    Filippini, J. P.
    Fissel, L. M.
    Fraisse, A. A.
    Freese, Katherine
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). University of Michigan, USA.
    Galloway, M.
    Gambrel, A. E.
    Gandilo, N. N.
    Ganga, K.
    Gudmundsson, Jón E.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Halpern, M.
    Hartley, J.
    Hasselfield, M.
    Hilton, G.
    Holmes, W.
    Hristov, V. V.
    Huang, Z.
    Irwin, K. D.
    Jones, W. C.
    Kuo, C. L.
    Kermish, Z. D.
    Li, S.
    Mason, P. V.
    Megerian, K.
    Moncelsi, L.
    Morford, T. A.
    Netterfield, C. B.
    Nolta, M.
    Padilla, I. L.
    Racine, B.
    Rahlin, A. S.
    Reintsema, C.
    Ruhl, J. E.
    Runyan, M. C.
    Ruud, T. M.
    Shariff, J. A.
    Soler, J. D.
    Song, X.
    Trangsrud, A.
    Tucker, C.
    Tucker, R. S.
    Turner, A. D.
    Van Der List, J. F.
    Weber, A. C.
    Wehus, I. K.
    Wiebe, D. V.
    Young, E. Y.
    A New Limit on CMB Circular Polarization from SPIDER2017In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 844, no 2, article id 151Article in journal (Refereed)
    Abstract [en]

    We present a new upper limit on cosmic microwave background (CMB) circular polarization from the 2015 flight of SPIDER, a balloon-borne telescope designed to search for B-mode linear polarization from cosmic inflation. Although the level of circular polarization in the CMB is predicted to be very small, experimental limits provide a valuable test of the underlying models. By exploiting the nonzero circular-to-linear polarization coupling of the half-wave plate polarization modulators, data from SPIDER's 2015 Antarctic flight provide a constraint on Stokes V at 95 and 150 GHz in the range 33 < l < 307. No other limits exist over this full range of angular scales, and SPIDER improves on the previous limit by several orders of magnitude, providing 95% C.L. constraints on l (l + 1)C-l(VV) /(2 pi) ranging from 141 to 255 mu K-2 at 150 GHz for a thermal CMB spectrum. As linear CMB polarization experiments become increasingly sensitive, the techniques described in this paper can be applied to obtain even stronger constraints on circular polarization.

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