The QUIJOTE Experiment: Project Overview and First Results
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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. -
A Bayesian Method for Point Source Polarisation Estimation D
A&A 651, A24 (2021) Astronomy https://doi.org/10.1051/0004-6361/202039741 & c ESO 2021 Astrophysics A Bayesian method for point source polarisation estimation D. Herranz1, F. Argüeso2,4, L. Toffolatti3,4, A. Manjón-García1,5, and M. López-Caniego6 1 Instituto de Física de Cantabria, CSIC-UC, Av. de Los Castros s/n, 39005 Santander, Spain e-mail: [email protected] 2 Departamento de Matemáticas, Universidad de Oviedo, C. Federico García Lorca 18, 33007 Oviedo, Spain 3 Departamento de Física, Universidad de Oviedo, C. Federico García Lorca 18, 33007 Oviedo, Spain 4 Instituto Universitario de Ciencias y Tecnologías Espaciales de Asturias (ICTEA), Escuela de Ingeniería de Minas, Materiales y Energía de Oviedo, C. Independencia 13, 33004 Oviedo, Spain 5 Departamento de Física Moderna, Universidad de Cantabria, 39005 Santander, Spain 6 ESAC, Camino Bajo del Castillo s/n, 28692 Villafranca del Castillo, Madrid, Spain Received 22 October 2020 / Accepted 2 March 2021 ABSTRACT The estimation of the polarisation P of extragalactic compact sources in cosmic microwave background (CMB) images is a very important task in order to clean these images for cosmological purposes –for example, to constrain the tensor-to-scalar ratio of primordial fluctuations during inflation– and also to obtain relevant astrophysical information about the compact sources themselves in a frequency range, ν ∼ 10–200 GHz, where observations have only very recently started to become available. In this paper, we propose a Bayesian maximum a posteriori approach estimation scheme which incorporates prior information about the distribution of the polarisation fraction of extragalactic compact sources between 1 and 100 GHz. -
The Design of the Ali CMB Polarization Telescope Receiver
The design of the Ali CMB Polarization Telescope receiver M. Salatinoa,b, J.E. Austermannc, K.L. Thompsona,b, P.A.R. Aded, X. Baia,b, J.A. Beallc, D.T. Beckerc, Y. Caie, Z. Changf, D. Cheng, P. Chenh, J. Connorsc,i, J. Delabrouillej,k,e, B. Doberc, S.M. Duffc, G. Gaof, S. Ghoshe, R.C. Givhana,b, G.C. Hiltonc, B. Hul, J. Hubmayrc, E.D. Karpela,b, C.-L. Kuoa,b, H. Lif, M. Lie, S.-Y. Lif, X. Lif, Y. Lif, M. Linkc, H. Liuf,m, L. Liug, Y. Liuf, F. Luf, X. Luf, T. Lukasc, J.A.B. Matesc, J. Mathewsonn, P. Mauskopfn, J. Meinken, J.A. Montana-Lopeza,b, J. Mooren, J. Shif, A.K. Sinclairn, R. Stephensonn, W. Sunh, Y.-H. Tsengh, C. Tuckerd, J.N. Ullomc, L.R. Valec, J. van Lanenc, M.R. Vissersc, S. Walkerc,i, B. Wange, G. Wangf, J. Wango, E. Weeksn, D. Wuf, Y.-H. Wua,b, J. Xial, H. Xuf, J. Yaoo, Y. Yaog, K.W. Yoona,b, B. Yueg, H. Zhaif, A. Zhangf, Laiyu Zhangf, Le Zhango,p, P. Zhango, T. Zhangf, Xinmin Zhangf, Yifei Zhangf, Yongjie Zhangf, G.-B. Zhaog, and W. Zhaoe aStanford University, Stanford, CA 94305, USA bKavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94305, USA cNational Institute of Standards and Technology, Boulder, CO 80305, USA dCardiff University, Cardiff CF24 3AA, United Kingdom eUniversity of Science and Technology of China, Hefei 230026 fInstitute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049 gNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 hNational Taiwan University, Taipei 10617 iUniversity of Colorado Boulder, Boulder, CO 80309, USA jIN2P3, CNRS, Laboratoire APC, Universit´ede Paris, 75013 Paris, France kIRFU, CEA, Universit´eParis-Saclay, 91191 Gif-sur-Yvette, France lBeijing Normal University, Beijing 100875 mAnhui University, Hefei 230039 nArizona State University, Tempe, AZ 85004, USA oShanghai Jiao Tong University, Shanghai 200240 pSun Yat-Sen University, Zhuhai 519082 ABSTRACT Ali CMB Polarization Telescope (AliCPT-1) is the first CMB degree-scale polarimeter to be deployed on the Tibetan plateau at 5,250 m above sea level. -
The QUIJOTE CMB Experiment: Status and First Results with the Multi-Frequency Instrument
The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument M. L´opez-Caniegoa, R. Rebolob;c;h, M. Aguiarb, R. G´enova-Santosb;c, F. G´omez-Re~nascob, C. Gutierrezb, J.M. Herrerosb, R.J. Hoylandb, C. L´opez-Caraballob;c, A.E. Pelaez Santosb;c, F. Poidevinb, J.A. Rubi~no-Mart´ınb;c, V. Sanchez de la Rosab, D. Tramonteb, A. Vega-Morenob, T. Viera-Curbelob, R. Vignagab, E. Mart´ınez-Gonzaleza, R.B. Barreiroa, B. Casaponsa a, F.J. Casasa, J.M. Diegoa, R. Fern´andez-Cobosa, D. Herranza, D. Ortiza, P. Vielvaa, E. Artald, B. Ajad, J. Cagigasd, J.L. Canod, L. de la Fuented, A. Mediavillad, J.V. Ter´and, E. Villad, L. Piccirilloe, R. Battyee, E. Blackhurste, M. Browne, R.D. Daviese, R.J. Davise, C. Dickinsone, K. Graingef , S. Harpere, B. Maffeie, M. McCulloche, S. Melhuishe, G. Pisanoe, R.A. Watsone, M. Hobsonf , A. Lasenbyf;g, R. Saundersf , and P. Scottf aInstituto de F´ısica de Cantabria, CSIC-UC, Avda. los Castros, s/n, E-39005 Santander, Spain bInstituto de Astrof´ısica de Canarias, C/Via Lactea s/n, E-38200 La Laguna, Tenerife, Spain cDepartamento de Astrof´ısica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain dDepartamento de Ingenier´ıade COMunicaciones (DICOM), Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain eJodrell Bank Centre for Astrophysics, University of Manchester, Oxford Rd, Manchester M13 9PL, UK f Astrophysics Group, Cavendish Laboratory, University of Cambridge, Cambridge CB3 0HE, UK gKavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA hConsejo Superior de Investigaciones Cient´ıficas, Spain arXiv:1401.4690v2 [astro-ph.IM] 5 Feb 2014 The QUIJOTE (Q-U-I JOint Tenerife) CMB Experiment is designed to observe the polar- ization of the Cosmic Microwave Background and other Galactic and extragalactic signals at medium and large angular scales in the frequency range of 10{40 GHz. -
Calibration of a Polarimetric Microwave Radiometer Using a Double Directional Coupler
remote sensing Article Calibration of a Polarimetric Microwave Radiometer Using a Double Directional Coupler Luisa de la Fuente 1,* , Beatriz Aja 1 , Enrique Villa 2 and Eduardo Artal 1 1 Departamento de Ingeniería de Comunicaciones, Universidad de Cantabria, 39005 Santander, Spain; [email protected] (B.A.); [email protected] (E.A.) 2 IACTEC, Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain; [email protected] * Correspondence: [email protected] Abstract: This paper presents a built-in calibration procedure of a 10-to-20 GHz polarimeter aimed at measuring the I, Q, U Stokes parameters of cosmic microwave background (CMB) radiation. A full-band square waveguide double directional coupler, mounted in the antenna-feed system, is used to inject differently polarized reference waves. A brief description of the polarimetric microwave radiometer and the system calibration injector is also reported. A fully polarimetric calibration is also possible using the designed double directional coupler, although the presented calibration method in this paper is proposed to obtain three of the four Stokes parameters with the introduced microwave receiver, since V parameter is expected to be zero for the CMB radiation. Experimental results are presented for linearly polarized input waves in order to validate the built-in calibration system. Keywords: radiometer; polarimeter calibration; microwave polarimeter; radiometer calibration; radio astronomy receiver; cosmic microwave background receiver; Stokes parameters Citation: de la Fuente, L.; Aja, B.; Villa, E.; Artal, E. Calibration of a 1. Introduction Polarimetric Microwave Radiometer Remote sensing applications employ sensitive instruments to fulfill the scientific goals Using a Double Directional Coupler. of dedicated missions or projects, either space or terrestrial. -
Wide-Survey of the QUIJOTE CMB Experiment Presented By: Federica Guidi (IAC, ULL), on Behalf of the QUIJOTE Collaboration
Wide-survey of the QUIJOTE CMB experiment Presented by: Federica Guidi (IAC, ULL), on behalf of the QUIJOTE collaboration. I present the status and the recent results of the QUIJOTE (Q-U-I JOint TEnerife) experiment. QUIJOTE is a project that operates from the Teide Observatory, with the aim to characterize the emission of the galactic foregrounds at microwave wavelengths, and to study the polarization of the Cosmic Microwave Background, targeting the detection of the primordial gravitational waves, the so called ”B-modes”, down to a value of the tensor to scalar ratio of r = 0.05. Recently, one of the two instruments of QUIJOTE, the Multi Frequency Instrument (MFI), concluded a wide-survey campaign, during which we observed the full northern sky, at 11, 13, 17 and 19 GHz. The wide survey maps of QUIJOTE will be delivered soon to the community. Here I present the current status of the maps, and I summarize few scientific results related to them, with special emphasis on the low frequency Galactic foregrounds, such as the Synchrotron and the Anomalous Microwave Emission. XIV.0 Reunión Científica 13-15 julio 2020 Context of the research: QUIJOTE: a polarimetric CMB experiment for the characterization of the low frequency galactic foregrounds ● CMB polarization experiments are searching for the polarization pattern imprinted by primordial gravitational waves: the “B-modes”. ● QUIJOTE is a polarimetric CMB experiment installed at the Teide observatory since 2012. ● QUIJOTE extends the Planck and WMAP coverage to low frequency, with two instruments: ○ Multi Frequency Instrument (MFI): 11, 13, 17, 19 GHz; ○ Thirty and Forty GHz Instrument (TFGI): Q Q Q Q J J 30-40 GHz. -
The QUIJOTE Experiment: Project Overview and First Results
Highlights of Spanish Astrophysics VIII, Proceedings of the XI Scientific Meeting of the Spanish Astronomical Society held on September 8–12, 2014, in Teruel, Spain. A. J. Cenarro, F. Figueras, C. Hernández-Monteagudo, J. Trujillo Bueno, and L. Valdivielso (eds.) The QUIJOTE experiment: project overview and first results R. G´enova-Santos1;6, J. A. Rubi~no-Mart´ın1;6, R. Rebolo1;6;7, M. Aguiar1, F. G´omez-Re~nasco1, C. Guti´errez1;6, R. J. Hoyland1, C. L´opez-Caraballo1;6;8, A. E. Pel´aez-Santos1;6, M. R. P´erez-de-Taoro1, F. Poidevin1;6 , V. S´anchez de la Rosa1, D. Tramonte1;6, A. Vega-Moreno1, T. Viera-Curbelo1, R. Vignaga1;6, E. Mart´ınez-Gonz´alez2, R. B. Barreiro2, B. Casaponsa2, F. J. Casas2, J. M. Diego2, R. Fern´andez-Cobos2, D. Herranz2, M. L´opez-Caniego2, D. Ortiz2, P. Vielva2, E. Artal3, B. Aja3, J. Cagigas3, J. L. Cano3, L. de la Fuente3, A. Mediavilla3, J. V. Ter´an3, E. Villa3, L. Piccirillo4, R. Davies4, R. J. Davis4, C. Dickinson4, K. Grainge4, S. Harper4, B. Maffei4, M. McCulloch4, S. Melhuish4, G. Pisano4, R. A. Watson4, A. Lasenby5;9, M. Ashdown5;9, M. Hobson5, Y. Perrott5, N. Razavi-Ghods5, R. Saunders6, D. Titterington6 and P. Scott6 1 Instituto de Astrofis´ıcade Canarias, 38200 La Laguna, Tenerife, Canary Islands, Spain 2 Instituto de F´ısicade Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, 39005 Santander, Spain 3 Departamento de Ingenieria de COMunicaciones (DICOM), Laboratorios de I+D de Telecomunicaciones, Universidad de Cantabria, Plaza de la Ciencia s/n, E-39005 Santander, Spain 4 Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, U.K 5 Astrophysics Group, Cavendish Laboratory, University of Cambridge, J.J. -
Optimal Reconstruction of Cosmological Density Fields by Benjamin A. Horowitz a Dissertation Submitted in Partial Satisfaction O
Optimal Reconstruction of Cosmological Density Fields By Benjamin A. Horowitz Adissertationsubmittedinpartialsatisfactionofthe requirements for the degree of Doctor of Philosophy in Physics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Uros Seljak, Chair Professor Aaron Parson Professor Martin White Fall 2019 Optimal Reconstruction of Cosmological Density Fields Copyright 2019 by Benjamin A. Horowitz 1 Abstract Optimal Reconstruction of Cosmological Density Fields by Benjamin A. Horowitz Doctor of Philosophy in Physics University of California, Berkeley Professor Uros Seljak, Chair Akeyobjectiveofmoderncosmologyistodeterminethecompositionanddistributionof matter in the universe. While current observations seem to match the standard cosmological model with remarkable precision, there remains tensions between observations as well as mysteries relating to the true nature of dark matter and dark energy. Despite the recent in- creased availability of cosmological data across a wide redshift, these tensions have remained or been further worsened. With the explosion of astronomical data in the coming decade, it has become increasingly critical to extract the maximum possible amount of information available across all available scales. As the available volume for analysis increases, we are no longer sample variance limited and existing summary statistics (as well as related estima- tors) need to be re-examined. Fortunately, parallel with the construction of these surveys there is significant development in the computational techniques used to analyze that data. Algorithmic developments over the past decade and expansion of computational resources allow large cosmological simulations to be run with relative simplicity and parallel theoretical developments motivate increased interest in recovering the underlying large scale structure of the universe beyond the power spectra. -
Planck 2011 Conference the Millimeter And
PLANCK 2011 CONFERENCE THE MILLIMETER AND SUBMILLIMETER SKY IN THE PLANCK MISSION ERA 10-14 January 2011 Paris, Cité des Sciences (Abstracts version Jan 14th) Planck mission status, Performances, Cross-calibration Herschel - update with a Planck perspective Pilbratt Goran, European Space Agency The Herschel Space Observatory was launched together with Planck on 14 May 2009. Herschel carries a 3.5 m diameter Cassegrain telescope and three instruments: PACS, SPIRE, and HIFI. It covers the wavelength range ~55-671 um for photometry and spectroscopy, with an angular resolution of approximately 7"/100 um. Early Herschel science performance and science results will be presented, with an attempt of a Planck perspective. The observing opportunities for follow-up of Planck results, in particular the ERCSC, will be outlined. Radio sources A Bayesian technique to detect point sources in CMB maps Argueso Francisco, Departamento de Matematicas. Universidad de Oviedo and E. Salerno, D. Herranz, J. L. Sanz, E. Kuruoglu, K. Kayabol; IFCA, CSIC, Santander, Spain. ISTI, CNR, Pisa, Italy The detection and flux estimation of point sources in cosmic microwave background (CMB) maps is a very important task in order to clean the maps and also to obtain relevant astrophysical information. We propose a new strategy based on Bayesian methodology which can be applied to the blind detection of point sources in CMB maps. The method incorporates three prior distributions: a uniform distribution on the source locations, an extended power law on the source fluxes, following the De Zotti counts model, and a Poisson distribution on the number of point sources per patch. Together with a Gaussian likelihood, these priors produce a posterior distribution. -
The Effect of a Scanning Flat Fold Mirror on a CMB B-Mode Experiment
The effect of a scanning flat fold mirror on a CMB B-mode experiment William F. Grainger, Chris E. North, Peter. A. R. Ade Astronomy Instrumentation Group, Cardiff University. (Dated: November 19, 2018) We investigate the possibility of using a flat-fold beam steering mirror for a CMB B-mode exper- iment. An aluminium flat-fold mirror is found to add ∼0.075% polarization, which varies in a scan synchronous way. Time-domain simulations of a realistic scanning pattern are performed, and the effect on the power-spectrum illustrated and a possible method of correction applied. I. INTRODUCTION a fiducal scan strategy and simulation pipeline. Results from this pipeline are then presented and discussed, along with other potential problems in Section IV. The prevailing ΛCDM cosmological model has been very successful in explaining many observations of the universe. However, inflation - exponential expansion II. METHOD within the first 10−35 s - has many uncertain details; indeed it lacks strong∼ confirmation. Inflationary models predict a background of gravity waves [1, 9, 20, 22, 23] For this investigation, we consider a horn fed receiver which produce a curl-like, or “B-mode” pattern of po- and compact range antenna (CRA), placed in a ground- larization on the cosmic microwave background (CMB) screen, nominally observing the horizon. The output on scales greater than 1◦, which cannot be produced by beam of the CRA is then steered to the sky with a single, density perturbations [11, 25]. The amplitude of this sig- flat, fold mirror. Although the flat mirror would be large; 4 4 m, such a system can be considered. -
The Thirty Gigahertz Instrument Receiver for the Q-U-I Joint Tenerife Experiment: Concept and Experimental Results Enrique Villa,1,A) Juan L
REVIEW OF SCIENTIFIC INSTRUMENTS 86, 024702 (2015) The thirty gigahertz instrument receiver for the Q-U-I Joint Tenerife experiment: Concept and experimental results Enrique Villa,1,a) Juan L. Cano,1 Jaime Cagigas,1 David Ortiz,2 Francisco J. Casas,2 Ana R. Pérez,1 Beatriz Aja,1 J. Vicente Terán,1 Luisa de la Fuente,1 Eduardo Artal,1 Roger Hoyland,3 and Ángel Mediavilla1 1Departamento Ingeniería de Comunicaciones, Universidad de Cantabria, Plaza de la Ciencia s/n, Santander 39005, Spain 2Instituto de Física de Cantabria, Avda. Los Castros s/n, Santander 39005, Spain 3Instituto de Astrofísica de Canarias, Vía Láctea s/n, La Laguna 38205, Spain (Received 12 December 2014; accepted 19 January 2015; published online 4 February 2015) This paper presents the analysis, design, and characterization of the thirty gigahertz instrument receiver developed for the Q-U-I Joint Tenerife experiment. The receiver is aimed to obtain polarization data of the cosmic microwave background radiation from the sky, obtaining the Q, U, and I Stokes parameters of the incoming signal simultaneously. A comprehensive analysis of the theory behind the proposed receiver is presented for a linearly polarized input signal, and the functionality tests have demonstrated adequate results in terms of Stokes parameters, which validate the concept of the receiver based on electronic phase switching. C 2015 AIP Publishing LLC. [http://dx.doi.org/10.1063/1.4907015] I. INTRODUCTION the moment right after the Big Bang.6 Among ground-based projects, QUIET7 and FARADAY8 have developed sensitive The Cosmic Microwave Background (CMB) is the ther- radiometers based on the schemes of previous receivers per- mal radiation from the Big Bang explosion, which fills the forming high-quality sky maps.