Quantum Universe V. Mukhanov
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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. -
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). -
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 Large Scale Polarization Explorer (LSPE) for CMB Measurements: Performance Forecast
Prepared for submission to JCAP The large scale polarization explorer (LSPE) for CMB measurements: performance forecast The LSPE collaboration G. Addamo,a P. A. R. Ade,b C. Baccigalupi,c A. M. Baldini,d P. M. Battaglia,e E. S. Battistelli, f;g A. Baù,h P. de Bernardis, f;g M. Bersanelli,i; j M. Biasotti,k;l A. Boscaleri,m B. Caccianiga, j S. Caprioli,i; j F. Cavaliere,i; j F. Cei, f;n K. A. Cleary,o F. Columbro, f;g G. Coppi,p A. Coppolecchia, f;g F. Cuttaia,q G. D’Alessandro, f;g G. De Gasperis,r;s M. De Petris, f;g V. Fafone,r;s F. Farsian,c L. Ferrari Barusso,k;l F. Fontanelli,k;l C. Franceschet,i; j T.C. Gaier,u L. Galli,d F. Gatti,k;l R. Genova-Santos,t;v M. Gerbino,D;C M. Gervasi,h;w T. Ghigna,x D. Grosso,k;l A. Gruppuso,q;H R. Gualtieri,G F. Incardona,i; j M. E. Jones,x P. Kangaslahti,o N. Krachmalnicoff,c L. Lamagna, f;g M. Lattanzi,D;C M. Lumia,a R. Mainini,h D. Maino,i; j S. Mandelli,i; j M. Maris,y S. Masi, f;g S. Matarrese,z A. May,A L. Mele, f;g P. Mena,B A. Mennella,i; j R. Molina,B D. Molinari,q;E;C;D G. Morgante,q U. Natale,C;D F. Nati,h P. Natoli,C;D L. Pagano,C;D A. Paiella, f;g F. -
Asymfast, a Method for Convolving Maps with Asymmetric Main Beams
Asymfast, a method for convolving maps with asymmetric main beams M. Tristram,∗ J. F. Mac´ıas-P´erez, and C. Renault Laboratoire de Physique Subatomique et de Cosmologie, 53 Avenue des Martyrs, 38026 Grenoble Cedex, France J-Ch. Hamilton Laboratoire de Physique Nucl´eaire et de Hautes Energies, 4 place Jussieu, 75252 Paris Cedex 05, France (Dated: October 24, 2018) We describe a fast and accurate method to perform the convolution of a sky map with a general asymmetric main beam along any given scanning strategy. The method is based on the decomposi- tion of the beam as a sum of circular functions, here Gaussians. It can be easily implemented and is much faster than pixel-by-pixel convolution. In addition, Asymfast can be used to estimate the effective circularized beam transfer functions of CMB instruments with non-symmetric main beam. This is shown using realistic simulations and by comparison to analytical approximations which are available for Gaussian elliptical beams. Finally, the application of this technique to Archeops data is also described. Although developped within the framework of Cosmic Microwave Background observations, our method can be applied to other areas of astrophysics. PACS numbers: 95.75.-z, 98.80.-k I. INTRODUCTION asymmetric beam, the convolved map at a given pointing direction on the sky would depend both on the relative With the increasing in accuracy and angular scale orientation of the beam on the sky and on the shape of coverage of the recent Cosmic Microwave Background the beam pattern. This makes brute-force convolution (CMB) experiments, a major objective is to include beam particularly painful and slow (e.g. -