Cosmic Microwave Background Space Science Discipline Working Group
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Instrumental Performance and Results from Testing of the BLAST-TNG Receiver, Submillimeter Optics, and MKID Arrays
Instrumental performance and results from testing of the BLAST-TNG receiver, submillimeter optics, and MKID arrays Nicholas Galitzkia, Peter Adeb, Francesco E. Angil`ea, Peter Ashtonc, Jason Austermannd, Tashalee Billingsa, George Chee, Hsiao-Mei Chof, Kristina Davise, Mark Devlina, Simon Dickera, Bradley J. Dobera, Laura M. Fisselc, Yasuo Fukuig, Jiansong Gaod, Samuel Gordone, Christopher E. Groppie, Seth Hillbranda, Gene C. Hiltond, Johannes Hubmayrd, Kent D. Irwinh, Jeffrey Kleina, Dale Lif, Zhi-Yun Lii, Nathan P. Louriea, Ian Lowea, Hamdi Manie, Peter G. Martinj, Philip Mauskopfe, Christopher McKenneyd, Federico Natia, Giles Novakc, Enzo Pascaleb, Giampaolo Pisanob, Fabio P. Santosc, Douglas Scottk, Adrian Sinclaire, Juan D. Solerl, Carole Tuckerb, Matthew Underhille, Michael Vissersd, and Paul Williamsc aUniversity of Pennsylvania, 209 S 33rd St, Philadelphia, PA, USA bUniversity of Cardiff, The Parade, Cardiff, United Kingdom cCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics & Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA dNational Institute of Standards and Technology, 325 Broadway, Boulder, CO, USA eArizona State University, PO Box 871404, Tempe, AZ, USA fSLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, USA gNagoya University, Furocho, Chikusa Ward, Nagoya, Aichi Prefecture, Japan hStanford University, 382 Via Pueblo Mall, Stanford, CA, USA iUniversity of Virginia, 530 McCormick Road, Charlottesville, VA, USA jUniversity of Toronto, 60 St. George Street, Toronto, ON, Canada lUniversity of British Columbia, 6224 Agricultural Road, Vancouver, BC, Canada kLaboratoire AIM, Paris-Saclay, CEA/IRFU/SAp - CNRS - Universit´eParis Diderot, 91191, Gif-sur-Yvette Cedex, France ABSTRACT Polarized thermal emission from interstellar dust grains can be used to map magnetic fields in star forming molecular clouds and the diffuse interstellar medium (ISM). -
Detection of Polarization in the Cosmic Microwave Background Using DASI
Detection of Polarization in the Cosmic Microwave Background using DASI Thesis by John M. Kovac A Dissertation Submitted to the Faculty of the Division of the Physical Sciences in Candidacy for the Degree of Doctor of Philosophy The University of Chicago Chicago, Illinois 2003 Copyright c 2003 by John M. Kovac ° (Defended August 4, 2003) All rights reserved Acknowledgements Abstract This is a sample acknowledgement section. I would like to take this opportunity to The past several years have seen the emergence of a new standard cosmological model thank everyone who contributed to this thesis. in which small temperature di®erences in the cosmic microwave background (CMB) I would like to take this opportunity to thank everyone. I would like to take on degree angular scales are understood to arise from acoustic oscillations in the hot this opportunity to thank everyone. I would like to take this opportunity to thank plasma of the early universe, sourced by primordial adiabatic density fluctuations. In everyone. the context of this model, recent measurements of the temperature fluctuations have led to profound conclusions about the origin, evolution and composition of the uni- verse. Given knowledge of the temperature angular power spectrum, this theoretical framework yields a prediction for the level of the CMB polarization with essentially no free parameters. A determination of the CMB polarization would therefore provide a critical test of the underlying theoretical framework of this standard model. In this thesis, we report the detection of polarized anisotropy in the Cosmic Mi- crowave Background radiation with the Degree Angular Scale Interferometer (DASI), located at the Amundsen-Scott South Pole research station. -
Analysis and Measurement of Horn Antennas for CMB Experiments
Analysis and Measurement of Horn Antennas for CMB Experiments Ian Mc Auley (M.Sc. B.Sc.) A thesis submitted for the Degree of Doctor of Philosophy Maynooth University Department of Experimental Physics, Maynooth University, National University of Ireland Maynooth, Maynooth, Co. Kildare, Ireland. October 2015 Head of Department Professor J.A. Murphy Research Supervisor Professor J.A. Murphy Abstract In this thesis the author's work on the computational modelling and the experimental measurement of millimetre and sub-millimetre wave horn antennas for Cosmic Microwave Background (CMB) experiments is presented. This computational work particularly concerns the analysis of the multimode channels of the High Frequency Instrument (HFI) of the European Space Agency (ESA) Planck satellite using mode matching techniques to model their farfield beam patterns. To undertake this analysis the existing in-house software was upgraded to address issues associated with the stability of the simulations and to introduce additional functionality through the application of Single Value Decomposition in order to recover the true hybrid eigenfields for complex corrugated waveguide and horn structures. The farfield beam patterns of the two highest frequency channels of HFI (857 GHz and 545 GHz) were computed at a large number of spot frequencies across their operational bands in order to extract the broadband beams. The attributes of the multimode nature of these channels are discussed including the number of propagating modes as a function of frequency. A detailed analysis of the possible effects of manufacturing tolerances of the long corrugated triple horn structures on the farfield beam patterns of the 857 GHz horn antennas is described in the context of the higher than expected sidelobe levels detected in some of the 857 GHz channels during flight. -
SPIDER Experiment
Searching for the echoes of inflation with H. Cynthia Chiang University of KwaZulu-Natal Madrid: CMB, LSS, 21cm June 24, 2016 B mode polarization in the CMB E modes are the CMB's “intrinsic polarization” We expect them to be there because of scattering processes in the CMB Temperature anisotropies predict E-mode spectra with almost no extra information Not only that, but “standard” CMB scattering physics generates ONLY E modes. Why do we care about B modes? Inflation: exponential expansion of universe (x 1025) at 10-35 sec after big bang creates a gravitational wave background that leaves a B-mode imprint on CMB polarization. Gravitational lensing by large scale structure converts some of the E-mode polarization to B-mode. Use this to study structure formation, “weigh” neutrinos. How can we tell the difference between the above two? Degree vs. arcminute angular scales. The moral of the story: B modes tell us things about the universe that temperature and E modes can't. Inflation scorecard Inflation predicts: Our universe (Planck 2015): A flat universe Ωk = 0.000 ± 0.0025 with nearly scale-invariant ns = 0.968 ± 0.006 density fluctuations, well described by a power law, dns / d lnk = -0.0065 ± 0.0076 with scalar perturbations r0.002 < 0.01 (at 2σ) that are Gaussian fNL = 2.5 ± 5.7 and adiabatic, βiso < 0.03 (at 2σ) with a negligible contribution from topological defects f10 < 0.04 (Adapted from Martin White) Constraining inflation Planck 2015 CMB polarization power spectra E-mode E-mode is mainly sourced by density fluctuations and is the intrinsic polarization of the CMB Degree-scale B-mode from gravitational waves, amplitude described by the tensor-to-scalar ratio r. -
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. -
CMB S4 Stage-4 CMB Experiment
Cosmic Microwave Background past and future June 3rd, 2016 28th Rencontres de Blois Akito KUSAKA Lawrence Berkeley National Laboratory Light New TeV Particle? Higgs 5th force? Yukawa Inflation n Dark Dark Energy 퐵 /퐵 Matter My summary of “Snowmass Questions” 2014 2.7K blackbody What is CMB? Light from Last Scattering Surface LSS: Boundary between plasma and neutral H COBE/FIRAS Mather et. al. (1990) Planck Collaboration (2014) The Universe was 1100 times smaller Fluctuations seeding “us” 2015 Planck Collaboration (2015) Wk = 0 0.005 (w/ BAO) Gaussian Planck Collaboration (2014) Polarization Quadrupole anisotropy creates linear polarization via Thomson scattering http://background.uchicago.edu/~whu/polar/webversion/polar.html Polarization – E modes and B modes E modes: curl free component 푘 B modes: divergence free component 푘 CMB Polarization Science Inflation / Gravitational Waves Gravitational Lensing / Neutrino Mass Light Relativistic Species And more… B-mode from Inflation It’s about the stuff here A probe into the Early Universe Hot High Energy ~3000K (~0.25eV) Photons 1016 GeV ? ~1010K (~1MeV) Neutrinos Gravitational waves Sound waves Source of GW? : inflation Inflation › Rapid expansion of universe Quantum fluctuation of metric during inflation › Off diagonal component (T) primordial gravitational waves Unique probe into gravity quantum mechanics connection Ratio to S (on-diagonal): r=T/S Lensing B-mode Deflection by lensing (Nearly) Gaussian Non-Gaussian (Nearly) pure E modes Non-zero B modes It’s about the stuff here Lensing B-mode Abazajian et. al. (2014) Deflection by lensing (Nearly) Gaussian Non-Gaussian (Nearly) pure E modes Non-zero B modes Accurate mass measurement may resolve neutrino mass hierarchy. -
JUAN DIEGO SOLER Address: Max-Planck-Institut Für Astronomie
JUAN DIEGO SOLER Address: Max-Planck-Institut für Astronomie Königstuhl 17 D-69117 Heidelberg Germany Phone: +49-(0)176 64475267 Email: [email protected] Citizenship: Colombian Webpage: http://www.mpia.de/homes/soler/ EDUCATION Sep. 2007 - Sep. 2013 Ph.D. Astronomy and Astrophysics University of Toronto. Toronto, Canada. “In Search of an Imprint of Magnetization in the Balloon-borne Observations of the Polarized Dust Emission from Molecular Clouds” Advisor: Pr. Barth Netterfield Jury: Pr. M. Houde, Pr. P. Martin, Pr. D.-S. Moon, Pr. C. Matzner. Sep. 2004 - Sep. 2006 M.Sc. Physics Universidad de los Andes. Bogotá, Colombia. “Imaging and tomography with silicon microstrip detectors” Advisor: Pr. Carlos A. Avila Sep. 1999 - Sep. 2004 B.Sc. Physics Universidad de los Andes. Bogotá, Colombia. PROFESSIONAL APPOINTMENTS Jan. 2017 - present Post-doctoral Fellow. Max-Planck-Institut für Astronomie, Germany. ERC project “The HI/OH/Recombination line survey of the inner Milky Way (THOR)” directed by Dr. Henrik Beuther. Sep. 2015 - Jan. 2017 Post-doctoral Fellow. Service d’Astrophysique, CEA, France. ERC project “From the magnetized diffuse interstellar medium to the stars” directed by Dr. Patrick Hennebelle. Sep. 2013 - Sep. 2015 Post-doctoral Fellow. Institut d’Astrophysique Spatiale. France. ERC project “Mastering the dusty and magnetized interstellar screen to test inflation cosmology” directed by Dr. Francois Boulanger. Sep. 2008 - Sep. 2013 Research Assistant. University of Toronto. Toronto, Canada. Sep. 2007 - Sep. 2008 Teaching Assistant. University of Toronto. Toronto, Canada. Sep. 2006 - Sep. 2007 Research Assistant. CIEMAT. Madrid, Spain. Study of intensity-modulated radiation therapy (IMRT) in the Unit of Medical Physics directed by Dr. -
Rhodri Evans
Rhodri Evans The Cosmic Microwave Background How It Changed Our Understanding of the Universe Astronomers’ Universe More information about this series at http://www.springer.com/series/6960 Rhodri Evans The Cosmic Microwave Background How It Changed Our Understanding of the Universe 123 Rhodri Evans School of Physics & Astronomy Cardiff University Cardiff United Kingdom ISSN 1614-659X ISSN 2197-6651 (electronic) ISBN 978-3-319-09927-9 ISBN 978-3-319-09928-6 (eBook) DOI 10.1007/978-3-319-09928-6 Springer Cham Heidelberg New York Dordrecht London Library of Congress Control Number: : 2014957530 © Springer International Publishing Switzerland 2015 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. Exempted from this legal reservation are brief excerpts in connection with reviews or scholarly analysis or material supplied specifically for the purpose of being entered and executed on a computer system, for exclusive use by the purchaser of the work. Duplication of this publication or parts thereof is permitted only under the provisions of the Copyright Law of the Publisher’s location, in its current version, and permission for use must always be obtained from Springer. Permissions for use may be obtained through RightsLink at the Copyright Clearance Center. Violations are liable to prosecution under the respective Copyright Law. -
Arxiv:1911.11210V1 [Astro-Ph.IM] 25 Nov 2019
Robust diffraction-limited NIR-to-NUV wide-field imaging from stratospheric balloon-borne platforms – SuperBIT science telescope commissioning flight & performance L. Javier Romualdez,1, a) Steven J. Benton,1 Anthony M. Brown,2, 3 Paul Clark,2 Christopher J. Damaren,4 Tim Eifler,5 Aurelien A. Fraisse,1 Mathew N. Galloway,6 Ajay Gill,7, 8 John W. Hartley,9 Bradley Holder,4, 8 Eric M. Huff,10 Mathilde Jauzac,3, 11 William C. Jones,1 David Lagattuta,3 Jason S.-Y. Leung,7, 8 Lun Li,1 Thuy Vy T. Luu,1 Richard J. Massey,2, 3, 11 Jacqueline McCleary,10 James Mullaney,12 Johanna M. Nagy,8 C. Barth Netterfield,7, 8, 9 Susan Redmond,1 Jason D. Rhodes,10 Jürgen Schmoll,2 Mohamed M. Shaaban,8, 9 Ellen Sirks,11 and Sut-Ieng Tam3 1)Department of Physics, Princeton University, Jadwin Hall, Princeton, NJ, USA 2)Centre for Advanced Instrumentation (CfAI), Durham University, South Road, Durham DH1 3LE, UK 3)Centre for Extragalactic Astronomy, Department of Physics, Durham University, Durham DH1 3LE, UK 4)University of Toronto Institute for Aerospace Studies (UTIAS), 4925 Dufferin Street, Toronto, ON, Canada 5)Department of Astronomy/Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA 6)Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway 7)Department of Astronomy, University of Toronto, 50 St. George Street, Toronto, ON, Canada 8)Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON, Canada 9)Department of Physics, University of Toronto, 60 St. George Street, -
The Antarctic Sun, December 24, 2006
December 24, 2006 HowHow McMurdo Got Its Groove On Local music scene heats up By Peter Rejcek Sun staff OTHER RIFFS t’s possibly the cool- Even Shackleton got the est music scene on the blues, page 10 planet. McMurdo Station Pole, Palmer also jam, is certainly the hub page 11 Iof operations for the U.S. AntarcticI Program (USAP) wise, this is a real hotbed of with an austral summer popu- potential.” lation of a thousand people Fox is a pretty good judge or more. But in the last 10 or of what makes a music scene 15 years, it’s become a cross- pulse. He came of age dur- roads for musicians playing ing punk rock’s angry genesis in just about every genre in the late 1970s and early imaginable in their leisure 1980s, playing bass for the time, from reggae to rock and band United Mutation in the from blues to bluegrass. It’s Washington, D.C., area. (See a scene where a punk rocker the Dec. 18, 2005, issue of can share the night’s billing The Antarctic Sun at antarc- with a folk singer and a blues ticsun.usap.gov for a related guitarist – and the audience is story.) there to see them all. A conversation with Fox is “We have been really itself like listening to a punk lucky down here,” said Jay rock set – briefly intense out- Peter Rejcek / The Antarctic Sun Fox, the retail supervisor for bursts, each riff a variation Barb Propst plays guitar at the McMurdo Station Coffee House. -
Design and Performance of the Spider Instrument
Design and performance of the Spider instrument M. C. Runyana, P.A.R. Adeb, M. Amiric,S.Bentond, R. Biharye,J.J.Bocka,f,J.R.Bondg, J.A. Bonettif, S.A. Bryane, H.C. Chiangh, C.R. Contaldii, B.P. Crilla,f,O.Dorea,f,D.O’Deai, M. Farhangd, J.P. Filippinia, L. Fisseld, N. Gandilod, S.R. Golwalaa, J.E. Gudmundssonh, M. Hasselfieldc,M.Halpernc, G. Hiltonj, W. Holmesf,V.V.Hristova, K.D. Irwinj,W.C.Jonesh , C.L. Kuok,C.J.MacTavishl,P.V.Masona,T.A.Morforda, T.E. Montroye, C.B. Netterfieldd, A.S. Rahlinh, C.D. Reintsemaj, J.E. Ruhle, M.C. Runyana,M.A.Schenkera, J. Shariffd, J.D. Solerd, A. Trangsruda, R.S. Tuckera,C.Tuckerb,andA.Turnerf aDivision of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA; bSchool of Physics and Astronomy, Cardiff University, Cardiff, UK; cDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC, Canada; dDepartment of Physics, University of Toronto, Toronto, ON, Canada; eDepartment of Physics, Case Western Reserve University, Cleveland, OH, USA; fJet Propulsion Laboratory, Pasadena, CA, USA; gCanadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada; hDepartment of Physics, Princeton University, Princeton, NJ, USA; iDepartment of Physics, Imperial College, University of London, London, UK; jNational Institute of Standards and Technology, Boulder, CO, USA; kDepartment of Physics, Stanford University, Stanford, CA, USA; lKavli Institute for Cosmology, University of Cambridge, Cambridge, UK ABSTRACT Here we describe the design and performance of the Spider instrument. Spider is a balloon-borne cosmic microwave background polarization imager that will map part of the sky at 90, 145, and 280 GHz with sub- degree resolution and high sensitivity. -
The EBEX Balloon Borne Experiment-Optics, Receiver, and Polarimetry
The EBEX Balloon Borne Experiment - Optics, Receiver, and Polarimetry The EBEX Collaboration: Asad M. Aboobaker1, Peter Ade2, Derek Araujo3, Fran¸cois Aubin4, Carlo Baccigalupi5;6, Chaoyun Bao4, Daniel Chapman3, Joy Didier3, Matt Dobbs7;8, Christopher Geach4, Will Grainger9, Shaul Hanany4;∗, Kyle Helson10, Seth Hillbrand3, Johannes Hubmayr11, Andrew Jaffe12, Bradley Johnson3, Terry Jones4, Jeff Klein4, Andrei Korotkov10, Adrian Lee13, Lorne Levinson14, Michele Limon3, Kevin MacDermid7, Tomotake Matsumura4;15, Amber D. Miller3, Michael Milligan4, Kate Raach4, Britt Reichborn-Kjennerud3, Ilan Sagiv14, Giorgio Savini16, Locke Spencer2;17, Carole Tucker2, Gregory S. Tucker10, Benjamin Westbrook11, Karl Young4, Kyle Zilic4 ABSTRACT The E and B Experiment (EBEX) was a long-duration balloon-borne cosmic mi- crowave background polarimeter that flew over Antarctica in 2013. We describe the experiment's optical system, receiver, and polarimetric approach, and report on their in-flight performance. EBEX had three frequency bands centered on 150, 250, and 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 2School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United Kingdom 3Physics Department, Columbia University, New York, NY 10027 4University of Minnesota School of Physics and Astronomy, Minneapolis, MN 55455 5Astrophysics Sector, SISSA, Trieste, 34014, Italy 6INFN, Sezione di Trieste, Via Valerio 2, I-34127 Trieste, Italy 7McGill University, Montreal, Quebec, H3A 2T8, Canada 8Canadian Institute for