The Planck Newsletter
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
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. -
The Q/U Imaging Experiment (QUIET): the Q-Band Receiver Array Instrument and Observations by Laura Newburgh Advisor: Professor Amber Miller
The Q/U Imaging ExperimenT (QUIET): The Q-band Receiver Array Instrument and Observations by Laura Newburgh Advisor: Professor Amber Miller Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2010 c 2010 Laura Newburgh All Rights Reserved Abstract The Q/U Imaging ExperimenT (QUIET): The Q-band Receiver Array Instrument and Observations by Laura Newburgh Phase I of the Q/U Imaging ExperimenT (QUIET) measures the Cosmic Microwave Background polarization anisotropy spectrum at angular scales 25 1000. QUIET has deployed two independent receiver arrays. The 40-GHz array took data between October 2008 and June 2009 in the Atacama Desert in northern Chile. The 90-GHz array was deployed in June 2009 and observations are ongoing. Both receivers observe four 15◦ 15◦ regions of the sky in the southern hemisphere that are expected × to have low or negligible levels of polarized foreground contamination. This thesis will describe the 40 GHz (Q-band) QUIET Phase I instrument, instrument testing, observations, analysis procedures, and preliminary power spectra. Contents 1 Cosmology with the Cosmic Microwave Background 1 1.1 The Cosmic Microwave Background . 1 1.2 Inflation . 2 1.2.1 Single Field Slow Roll Inflation . 3 1.2.2 Observables . 4 1.3 CMB Anisotropies . 6 1.3.1 Temperature . 6 1.3.2 Polarization . 7 1.3.3 Angular Power Spectrum Decomposition . 8 1.4 Foregrounds . 14 1.5 CMB Science with QUIET . 15 2 The Q/U Imaging ExperimenT Q-band Instrument 19 2.1 QUIET Q-band Instrument Overview . -
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. -
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. -
Maturity of Lumped Element Kinetic Inductance Detectors For
Astronomy & Astrophysics manuscript no. Catalano˙f c ESO 2018 September 26, 2018 Maturity of lumped element kinetic inductance detectors for space-borne instruments in the range between 80 and 180 GHz A. Catalano1,2, A. Benoit2, O. Bourrion1, M. Calvo2, G. Coiffard3, A. D’Addabbo4,2, J. Goupy2, H. Le Sueur5, J. Mac´ıas-P´erez1, and A. Monfardini2,1 1 LPSC, Universit Grenoble-Alpes, CNRS/IN2P3, 2 Institut N´eel, CNRS, Universit´eJoseph Fourier Grenoble I, 25 rue des Martyrs, Grenoble, 3 Institut de Radio Astronomie Millim´etrique (IRAM), Grenoble, 4 LNGS - Laboratori Nazionali del Gran Sasso - Assergi (AQ), 5 Centre de Sciences Nucl´eaires et de Sciences de la Mati`ere (CSNSM), CNRS/IN2P3, bat 104 - 108, 91405 Orsay Campus Preprint online version: September 26, 2018 ABSTRACT This work intends to give the state-of-the-art of our knowledge of the performance of lumped element kinetic inductance detectors (LEKIDs) at millimetre wavelengths (from 80 to 180 GHz). We evaluate their optical sensitivity under typical background conditions that are representative of a space environment and their interaction with ionising particles. Two LEKID arrays, originally designed for ground-based applications and composed of a few hundred pixels each, operate at a central frequency of 100 and 150 GHz (∆ν/ν about 0.3). Their sensitivities were characterised in the laboratory using a dedicated closed-cycle 100 mK dilution cryostat and a sky simulator, allowing for the reproduction of realistic, space-like observation conditions. The impact of cosmic rays was evaluated by exposing the LEKID arrays to alpha particles (241Am) and X sources (109Cd), with a read-out sampling frequency similar to those used for Planck HFI (about 200 Hz), and also with a high resolution sampling level (up to 2 MHz) to better characterise and interpret the observed glitches. -
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). -
The Cosmic Microwave Background Anisotropy Power Spectrum Measured by Archeops
Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20021850 L22 A. Benoˆıt et al.: The cosmic microwave background anisotropy power spectrum measured by Archeops We construct maps by bandpassing the data between 0.3 Table 1. The Archeops CMB power spectrum for the best two pho- and 45 Hz, corresponding to about 30 deg and 15 arcmin scales, tometers (third column). Data points given in this table correspond to respectively. The high–pass filter removes remaining atmo- the red points in Fig. 2. The fourth column shows the power spec- spheric and galactic contamination, the low–pass filter sup- trum for the self difference (SD) of the two photometers as described presses non–stationary high frequency noise. The filtering is in Sect. 4. The fifth column shows the power spectrum for the differ- done in such a way that ringing effects of the signal on ence (D) between the two photometers. bright compact sources (mainly the Galactic plane) are smaller `(`+1)C` 2 2 2 `min `max (µK) SD (µK) D (µK) than 36 µK2 on the CMB power spectrum in the very first (2π) `–bin,∼ and negligible for larger multipoles. Filtered TOI of each 15 22 789 537 21 34 14 34 ± − ± − ± absolutely calibrated detector are co–added on the sky to form 22 35 936 230 6 25 34 21 35 45 1198 ± 262 −69 ± 45 75 ± 35 detector maps. The bias of the CMB power spectrum due to ± − ± − ± filtering is accounted for in the MASTER process through the 45 60 912 224 18 50 9 37 60 80 1596 ± 224 −33 ± 63 8 ± 44 transfer function. -
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). -
PLANCK (Retour D’Expérience Pour Le CS IN2P3)
PLANCK (retour d’expérience pour le CS IN2P3) July 2020 1. Résumé (une page) Planck was an ESA mission to observe the first light in the Universe. Planck was selected in 1995 as the third Medium-Sized Mission (M3) of ESA's Horizon 2000 Scientific Programme, and later became part of its Cosmic Vision Programme. It was designed to image the temperature and polarization anisotropies of the Cosmic Background Radiation Field over the whole sky, with an unprecedented combination of sensitivity and angular resolution. Planck was testing theories of the early universe and the origin of cosmic structure and providing a major source of information relevant to many cosmological and astrophysical issues. Planck was formerly called COBRAS/SAMBA. After the mission was selected and approved (in late 1996), it was renamed in honor of the German scientist Max Planck (1858-1947), Nobel Prize for Physics in 1918. Planck was launched on 14 May 2009, and the minimum requirement for success was for the spacecraft to complete two whole surveys of the sky. In the end, Planck worked perfectly for 30 months, about twice the span originally required, and completed five full-sky surveys with both instruments. Able to work at higher temperatures than the High Frequency Instrument (HFI), the Low Frequency Instrument (LFI) continued to survey the sky for a large part of 2013, providing even more data to improve the Planck final results. Planck was turned off on 23 October 2013. The high-quality data the mission has produced was released in three major sets of papers: ● 2013 data release (PR1) On 21 March 2013, the European-led research team behind the Planck cosmology probe released the mission's all-sky map of the cosmic microwave background together with a set of 32 scientific papers. -
The Cosmic Microwave Background Anisotropy Power Spectrum Measured by Archeops 3
Astronomy & Astrophysics manuscript no. Cl˙letter November 8, 20181 (DOI: will be inserted by hand later) The Cosmic Microwave Background Anisotropy Power Spectrum measured by Archeops A. Benoˆıt1, P. Ade2, A. Amblard3, 24, R. Ansari4, E.´ Aubourg5, 24, S. Bargot4, J. G. Bartlett3, 24, J.–Ph. Bernard7, 16, R. S. Bhatia8, A. Blanchard6, J. J. Bock8, 9, A. Boscaleri10, F. R. Bouchet11, A. Bourrachot4, P. Camus1, F. Couchot4, P. de Bernardis12, J. Delabrouille3, 24, F.–X. D´esert13, O. Dor´e11, M. Douspis6, 14, L. Dumoulin15, X. Dupac16, P. Filliatre17, P. Fosalba11, K. Ganga18, F. Gannaway2, B. Gautier1, M. Giard16, Y. Giraud–H´eraud3, 24, R. Gispert7†⋆, L. Guglielmi3, 24, J.–Ch. Hamilton3, 17, S. Hanany19, S. Henrot–Versill´e4, J. Kaplan3, 24, G. Lagache7, J.–M. Lamarre7,25, A. E. Lange8, J. F. Mac´ıas–P´erez17, K. Madet1, B.Maffei2, Ch. Magneville5, 24, D. P. Marrone19, S. Masi12, F. Mayet5, A. Murphy20, F. Naraghi17, F. Nati12, G. Patanchon3, 24, G. Perrin17, M. Piat7, N. Ponthieu17, S. Prunet11, J.–L. Puget7, C. Renault17, C. Rosset3, 24, D. Santos17, A. Starobinsky21, I. Strukov22, R. V. Sudiwala2, R. Teyssier11, 23, M. Tristram17, C. Tucker2, J.–C. Vanel3, 24, D. Vibert11, E. Wakui2, and D. Yvon5, 24 1 Centre de Recherche sur les Tr`es Basses Temp´eratures, BP166, 38042 Grenoble Cedex 9, France 2 Cardiff University, Physics Department, PO Box 913, 5, The Parade, Cardiff, CF24 3YB, UK 3 Physique Corpusculaire et Cosmologie, Coll`ege de France, 11 pl. M. Berthelot, F-75231 Paris Cedex 5, France 4 Laboratoire de l’Acc´el´erateur Lin´eaire, BP 34, Campus Orsay, 91898 Orsay Cedex, France 5 CEA-CE Saclay, DAPNIA, Service de Physique des Particules, Bat 141, F-91191 Gif sur Yvette Cedex, France 6 Laboratoire d’Astrophysique de l’Obs.