Research Article a Characterization of the Diffuse Galactic Emissions in the Anticenter of the Galaxy
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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. -
La Radiación Del Fondo Cósmico De Microondas Abstracts
Simposio Internacional: La radiación del Fondo Cósmico de Microondas: mensajera de los orígenes del universo International Symposium: CMB Radiation: Messenger of the Origins of Our Universe Madrid, 6 de noviembre de 2014 Madrid, November 6, 2014 I The seeds of structure: A view of the Cosmic Microwave Background, Joseph Silk The shape of the universe as seen by Planck, Enrique Martínez-González Deciphering the beginnings of the universe with CMB polarization, Matías Zaldarriaga 30 years of Cosmic Microwave Background experiments in Tenerife: From temperature to polarization maps, Rafael Rebolo Cosmology from Planck: Do we need a new Physics?, Nazzareno Mandolesi FUNDACIÓN RAMÓN ARECES Simposio Internacional: La radiación del Fondo Cósmico de Microondas: mensajera de los orígenes del universo International Symposium: CMB Radiation: Messenger of the Origins of Our Universe Madrid, 6 de noviembre de 2014 Madrid, November 6, 2014 The seeds of structure: A view of the Cosmic Microwave Background, Joseph Silk One of our greatest challenges is understanding the origin of the structure of the universe.I will describe how the fossil radiation from the beginning of the universe, the cosmic microwave background, has provided a window for probing the initial conditions from which structure evolved. Infinitesimal variations in temperature on the sky, first discovered in 1992, provide the fossil fluctuations that seeded the formation of the galaxies. The cosmic microwave background radiation has now been mapped with ground-based, balloon-borne and satellite telescopes. These provide the basis for our current ``precision cosmology'' in which the universe not only contains Dark Matter but also ``DarkEnergy'', which has accelerated its expansion exponentially in the last 4 billion years. -
Planck 2015 Results. XII. Full Focal Plane Simulations Planck Collaboration: P
Astronomy & Astrophysics manuscript no. A14˙Simulations c ESO 2016 August 13, 2016 Planck 2015 results. XII. Full Focal Plane simulations Planck Collaboration: P. A. R. Ade87, N. Aghanim60, M. Arnaud75, M. Ashdown71;5, J. Aumont60, C. Baccigalupi86, A. J. Banday95;9, R. B. Barreiro66, J. G. Bartlett1;68, N. Bartolo31;67, E. Battaner97;98, K. Benabed61;94, A. Benoˆıt58, A. Benoit-Levy´ 25;61;94, J.-P. Bernard95;9, M. Bersanelli34;49, P. Bielewicz84;9;86, J. J. Bock68;11, A. Bonaldi69, L. Bonavera66, J. R. Bond8, J. Borrilly14;90, F. R. Bouchet61;89, F. Boulanger60, M. Bucher1, C. Burigana48;32;50, R. C. Butler48, E. Calabrese92, J.-F. Cardoso76;1;61, G. Castex1, A. Catalano77;74, A. Challinor63;71;12, A. Chamballu75;16;60, H. C. Chiang28;6, P. R. Christensen85;37, D. L. Clements56, S. Colombi61;94, L. P. L. Colombo24;68, C. Combet77, F. Couchot73, A. Coulais74, B. P. Crill68;11, A. Curto66;5;71, F. Cuttaia48, L. Danese86, R. D. Davies69, R. J. Davis69, P. de Bernardis33, A. de Rosa48, G. de Zotti45;86, J. Delabrouille1, J.-M. Delouis61;94, F.-X. Desert´ 54, C. Dickinson69, J. M. Diego66, K. Dolag96;81, H. Dole60;59, S. Donzelli49, O. Dore´68;11, M. Douspis60, A. Ducout61;56, X. Dupac39, G. Efstathiou63, F. Elsner25;61;94, T. A. Enßlin81, H. K. Eriksen64, J. Fergusson12, F. Finelli48;50, O. Forni95;9, M. Frailis47, A. A. Fraisse28, E. Franceschi48, A. Frejsel85, S. Galeotta47, S. Galli70, K. Ganga1, T. Ghosh60, M. Giard95;9, Y. Giraud-Heraud´ 1, E. Gjerløw64, J. Gonzalez-Nuevo´ 20;66, K. -
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. -
ELIA STEFANO BATTISTELLI Curriculum Vitae
ELIA STEFANO BATTISTELLI Curriculum Vitae Place: Rome, Italy Date: 03/09/2019 Part I – General Information Full Name ELIA STEFANO BATTISTELLI Date of Birth 29/03/1973 Place of Birth Milan, Italy Citizenship Italian Work Address Physics Dep., Sapienza University of Rome, P.le Aldo Moro 5, 00185, Rome, Italy Work Phone Number +39 06 49914462 Home Address Via Romolo Gigliozzi, 173, scala B, 00128, Rome, Italy Mobile Phone Number +39 349 6592825 E-mail [email protected] Spoken Languages Italian (native), English (fluent), Spanish (fluent), French (basic) Part II – Education Type Year Institution Notes (Degree, Experience,..) University graduation 1999 Sapienza University (RM, IT) Physics 1996 University of Leeds, UK Erasmus project Post-graduate studies 2000 SIGRAV (CO, IT) Graduate School in Relativity 2000 INAF (Asiago, VI, IT) Scuola Nazionale Astrofisica 2001 INAF/INFN (FC, IT) Scuola Nazionale Astroparticelle 2004 Società Italiana Fisica (CO, IT) International Fermi School 2006 Princeton University (NJ,USA) Summer School on Gal. Cluster PhD 2004 Sapienza University (RM, IT) PhD in Astronomy (XV cycle) Training Courses 2007 University of British Columbia 40-hours course in precision (BC, CA) machining 2009 Programma Nazionale Ricerche 2 weeks training course for the in Antartide (PNRA) Antarctic activity in remote camps Qualification 2013 Ministero della Pubblica National scientific qualification for Istruzione Associate Professor 2012, SSD 02/C1 (ASN-2012) Part III – Appointments IIIA – Academic Appointments Start End Institution Position 11/2018 present Sapienza University of Rome, Physics Associate Professor;Physics Department Department (Rome, Italy) SSD 02/C1-FIS/05 (Astrophysics) 11/2015 11/2018 Sapienza University of Rome, Physics Tenure track assistant professor Department (Rome, Italy) (Ricercatore a Tempo Determinato RTD- B-type). -
Small-Scale Anisotropies of the Cosmic Microwave Background: Experimental and Theoretical Perspectives
Small-Scale Anisotropies of the Cosmic Microwave Background: Experimental and Theoretical Perspectives Eric R. Switzer 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: Lyman Page] November 2008 c Copyright by Eric R. Switzer, 2008. All rights reserved. Abstract In this thesis, we consider both theoretical and experimental aspects of the cosmic microwave background (CMB) anisotropy for ℓ > 500. Part one addresses the process by which the universe first became neutral, its recombination history. The work described here moves closer to achiev- ing the precision needed for upcoming small-scale anisotropy experiments. Part two describes experimental work with the Atacama Cosmology Telescope (ACT), designed to measure these anisotropies, and focuses on its electronics and software, on the site stability, and on calibration and diagnostics. Cosmological recombination occurs when the universe has cooled sufficiently for neutral atomic species to form. The atomic processes in this era determine the evolution of the free electron abundance, which in turn determines the optical depth to Thomson scattering. The Thomson optical depth drops rapidly (cosmologically) as the electrons are captured. The radiation is then decoupled from the matter, and so travels almost unimpeded to us today as the CMB. Studies of the CMB provide a pristine view of this early stage of the universe (at around 300,000 years old), and the statistics of the CMB anisotropy inform a model of the universe which is precise and consistent with cosmological studies of the more recent universe from optical astronomy. -
Cosmic Microwave Background
1 29. Cosmic Microwave Background 29. Cosmic Microwave Background Revised August 2019 by D. Scott (U. of British Columbia) and G.F. Smoot (HKUST; Paris U.; UC Berkeley; LBNL). 29.1 Introduction The energy content in electromagnetic radiation from beyond our Galaxy is dominated by the cosmic microwave background (CMB), discovered in 1965 [1]. The spectrum of the CMB is well described by a blackbody function with T = 2.7255 K. This spectral form is a main supporting pillar of the hot Big Bang model for the Universe. The lack of any observed deviations from a 7 blackbody spectrum constrains physical processes over cosmic history at redshifts z ∼< 10 (see earlier versions of this review). Currently the key CMB observable is the angular variation in temperature (or intensity) corre- lations, and to a growing extent polarization [2–4]. Since the first detection of these anisotropies by the Cosmic Background Explorer (COBE) satellite [5], there has been intense activity to map the sky at increasing levels of sensitivity and angular resolution by ground-based and balloon-borne measurements. These were joined in 2003 by the first results from NASA’s Wilkinson Microwave Anisotropy Probe (WMAP)[6], which were improved upon by analyses of data added every 2 years, culminating in the 9-year results [7]. In 2013 we had the first results [8] from the third generation CMB satellite, ESA’s Planck mission [9,10], which were enhanced by results from the 2015 Planck data release [11, 12], and then the final 2018 Planck data release [13, 14]. Additionally, CMB an- isotropies have been extended to smaller angular scales by ground-based experiments, particularly the Atacama Cosmology Telescope (ACT) [15] and the South Pole Telescope (SPT) [16]. -
Physics of the Cosmic Microwave Background Anisotropy∗
Physics of the cosmic microwave background anisotropy∗ Martin Bucher Laboratoire APC, Universit´eParis 7/CNRS B^atiment Condorcet, Case 7020 75205 Paris Cedex 13, France [email protected] and Astrophysics and Cosmology Research Unit School of Mathematics, Statistics and Computer Science University of KwaZulu-Natal Durban 4041, South Africa January 20, 2015 Abstract Observations of the cosmic microwave background (CMB), especially of its frequency spectrum and its anisotropies, both in temperature and in polarization, have played a key role in the development of modern cosmology and our understanding of the very early universe. We review the underlying physics of the CMB and how the primordial temperature and polarization anisotropies were imprinted. Possibilities for distinguish- ing competing cosmological models are emphasized. The current status of CMB ex- periments and experimental techniques with an emphasis toward future observations, particularly in polarization, is reviewed. The physics of foreground emissions, especially of polarized dust, is discussed in detail, since this area is likely to become crucial for measurements of the B modes of the CMB polarization at ever greater sensitivity. arXiv:1501.04288v1 [astro-ph.CO] 18 Jan 2015 1This article is to be published also in the book \One Hundred Years of General Relativity: From Genesis and Empirical Foundations to Gravitational Waves, Cosmology and Quantum Gravity," edited by Wei-Tou Ni (World Scientific, Singapore, 2015) as well as in Int. J. Mod. Phys. D (in press). -
Implicaciones Cosmológicas De Las
DEPARTAMENTO DE F´ISICAMODERNA INSTITUTODEF´ISICA DE CANTABRIA UNIVERSIDAD DE CANTABRIA IFCA (UC-CSIC) IMPLICACIONES COSMOLOGICAS´ DE LAS ANISOTROP´IAS DE TEMPERATURA Y POLARIZACION´ DE LA RFCM Y LA ESTRUCTURA A GRAN ESCALA DEL UNIVERSO Memoria presentada para optar al t´ıtulo de Doctor otorgado por la Universidad de Cantabria por Ra´ul Fern´andez Cobos Declaraci´on de Autor´ıa Patricio Vielva Mart´ınez, Doctor en Ciencias F´ısicas y Profesor Contratado Doctor de la Universidad de Cantabria y Enrique Mart´ınez Gonz´alez, Doctor en Ciencias F´ısicas y Profesor de Investigaci´on del Consejo Superior de Investigaciones Cient´ıficas, CERTIFICAN que la presente memoria Implicaciones cosmol´ogicas de las anisotrop´ıas de temperatura y polarizaci´on de la RFCM y la estructura a gran escala del universo ha sido realizada por Ra´ul Fern´andez Cobos bajo nuestra direcci´on en el Instituto de F´ısica de Cantabria, para optar al t´ıtulo de Doctor por la Universidad de Cantabria. Consideramos que esta memoria contiene aportaciones cient´ıficas suficientemente rele- vantes como para constituir la Tesis Doctoral del interesado. En Santander, a 19 de septiembre de 2014, Patricio Vielva Mart´ınez Enrique Mart´ınez Gonz´alez A mis padres. Creo que seremos inmortales, que sembraremos las estrellas y viviremos eternamente en la carne de nuestros hijos. Ray Bradbury. Agradecimientos La realizaci´on de esta tesis doctoral ha servido de excusa para llevar a cabo un proyecto mucho m´as amplio, que se ha saldado con unos a˜nos de impagable crecimiento personal y del que estas p´aginas constituyen solo la peque˜na parte tangible. -
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/ -
The Primordial Inflation Explorer (PIXIE)
The Primordial Inflation Explorer (PIXIE) Alan Koguta, Jens Chlubab, Dale J. Fixsenc,StephanMeyerd,andDavidSpergele aCode 665, NASA Goddard Space Flight Center, Greenbelt, MD USA 20771 bJodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester M13 9PL, UK cUniversity of Maryland, College Park MD USA dDept of Astronomy & Astrophysics, University of Chicago, Chicago, IL, USA eDept of Astrophysical Sciences, Princeton University, Princeton, NJ, USA 08544 ABSTRACT The Primordial Inflation Explorer is an Explorer-class mission to open new windows on the early universe through measurements of the polarization and absolute frequency spectrum of the cosmic microwave background. PIXIE will measure the gravitational-wave signature of primordial inflation through its distinctive imprint in linear polarization, and characterize the thermal history of the universe through precision measurements of distortions in the blackbody spectrum. PIXIE uses an innovative optical design to achieve background-limited sensitivity in 400 spectral channels spanning over 7 octaves in frequency from 30 GHz to 6 THz (1 cm to 50 micron wavelength). Multi-moded non-imaging optics feed a polarizing Fourier Transform Spectrometer to produce a set of interference fringes, proportional to the di↵erence spectrum between orthogonal linear polarizations from the two input beams. Multiple levels of symmetry and signal modulation combine to reduce systematic errors to negligible levels. PIXIE will map the full sky in Stokes I, Q, and U parameters with angular resolution 2.6◦ and sensitivity 70 nK per 1◦ square pixel. The principal science goal is the detection and characterization of linear 3 polarization from an inflationary epoch in the early universe, with tensor-to-scalar ratio r<10− at 5 standard deviations. -