DOCSLIB.ORG

FOR the QUBIC CMB David G. Bennett B.Sc

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
FOR the QUBIC CMB David G. Bennett B.Sc ___________________________________________________ DESIGN AND ANALYSIS OF A QUASI-OPTICAL BEAM COMBINER FOR THE QUBIC CMB INTERFEROMETER ___________________________________________________ David G. Bennett B.Sc. Research Supervisor: Dr. Créidhe O'Sullivan Head of Department: Prof. J.A. Murphy A thesis submitted for the degree of Doctor of Philosophy Sub-mm Optics Research Group Department of Experimental Physics National University of Ireland, Maynooth Co. Kildare Ireland 9th July 2014 Contents 1 The Cosmic Microwave Background 8 1.1 A signal from the early Universe . 8 1.2 A brief history of CMB observations . 9 1.3 Modern Cosmology and the CMB . 12 1.3.1 The Big Bang and the expanding Universe . 12 1.3.2 CMB temperature power spectra . 14 1.3.3 Primary temperature anisotropies . 18 1.3.4 Secondary anisotropies . 19 1.3.5 CMB Polarization . 21 1.3.6 The CMB and Inflation . 27 1.4 Recent CMB experiments . 28 1.5 The CMB and the cosmological parameters . 29 1.6 Conclusions . 33 2 QUBIC: An Experiment designed to measure CMB B-mode polarization 35 2.1 Introducing QUBIC . 35 2.2 Interferometry . 35 2.2.1 Interferometers in astronomy . 35 2.2.2 Radio receivers . 37 2.2.3 Additive Bolometric Interferometry . 39 2.3 The QUBIC experiment . 41 2.3.1 QUBIC specifications . 42 2.4 Phase Shifting and equivalent baselines . 49 2.5 Quasi optical analysis techniques . 55 2.5.1 Methods for the optical modeling of CMB experiments . 55 2.5.2 Geometrical optics . 58 2 2.5.3 Physical optics (PO) . 59 2.5.4 Quasi optics . 62 2.5.5 Fourier optics . 66 2.5.6 Modeling lenses . 68 2.6 Thesis outline . 70 2.7 Conclusions . 70 3 Dual reflectors for bolometric Fizeau interferometers 72 3.1 The Optical Combiner for QUBIC . 72 3.1.1 Focal Systems . 73 3.1.2 Performance of a Telescopic Combiner . 75 3.1.3 Disadvantages of lenses of QUBIC . 77 3.1.4 Disadvantages of on-axis reflector designs for QUBIC. 78 3.1.5 Cassegrain versus Gregorian . 80 3.2 Dual reflectors . 80 3.2.1 The geometry off-axis dual reflectors . 81 3.2.2 Designing off-axis dual reflectors . 81 3.2.3 Beam distortion in dual reflectors . 84 3.3 Compensated dual reflectors . 89 3.3.1 Summary of off-axis dual reflectors for implementation in a CMB Fizeau interferometer . 126 3.3.2 Comparison of crossed reflectors for short focal length systems . 129 3.4 Alternative geometries for the combiner in a QUBIC-type experiment . 136 3.4.1 Fold mirror and a crossed Cassegrain dual reflector . 136 3.4.2 Fold mirror and a GCC examined using equivalent baselines . 140 3.4.3 GCC dual reflector and a concave hyperboloid . 144 3.5 Conclusions . 146 4 Optical Combiners for QUBIC 149 4.1 Possible optical combiners for QUBIC . 149 4.1.1 Introduction . 149 4.1.2 General crossed Cassegrain (GCC) . 151 4.1.3 Compensated Gregorian (CG) . 157 4.1.4 Constraints on the mirror dimension in the GCC and CG . 161 4.2 Effect of changes in QUBIC requirements . 162 3 4.2.1 Adjustment to combiners . 163 4.2.2 Zemax optimization to generate Telecentric combiners . 169 4.2.3 Off-axis parabolas . 175 4.2.4 Details of the geometry of the dual reflectors . 184 4.3 Power coupled to the bolometers . 185 4.4 Leakage concerns in a general crossed Cassegrain (GCC). 198 4.5 Conclusions . 200 5 Lens Design 201 5.1 Gaussian beam telescope and CATR combination . 201 5.1.1 Using Zemax to model the fringe patterns generated by a Gaus- sian beam telescope and CATR combiner . 205 5.2 Fully refractive combiner for QUBIC . 208 5.2.1 Telecentric lens combiners. 208 5.2.2 Gaussian and Cooke Triplet designs . 216 5.2.3 Symmetric double lenses that ignore field curvature. 220 5.3 Analysis of refracting combiners . 224 5.3.1 Using Zemax to model the fringe patterns generated by a lens combiner . 224 5.4 Conclusions . 227 6 QUBIC2.0 228 6.1 Introduction . 228 6.2 QUBIC2.0 . 228 6.2.1 Problems with the QUBIC design . 228 6.2.2 Modulating the sky polarization using a rotating half wave plate 235 6.2.3 QUBIC2.0 as a dirty imager . 240 6.2.4 Calibration techniques . 246 6.2.5 Cyrostat upgrades . 249 6.2.6 Remaining issues . 252 6.3 QUBIC2.0 optical combiner . 253 6.3.1 Analysis of optical combiners . 255 6.3.2 PSF of reflector combiners . 255 6.3.3 PSF of lens combiners . 259 6.4 Loss of sensitivity caused by optical combiners . 263 4 6.5 Conclusions . 266 7 Birefringence in CMB Polarimeters 267 7.1 Introduction . 267 7.2 A brief summary of QUaD . 267 7.2.1 The QUaD polarimeter . 267 7.2.2 QUaD model in Zemax . 271 7.2.3 Introduction to birefringence. 271 7.3 Investigation of possible birefringence in QUaD . 274 7.3.1 Using Zemax to investigate birefringence in QUaD . 274 7.4 Optimizations to identify QUaD crystal axes . 293 7.5 Zemax optimizations . 293 7.5.1 Displacements due to optimized crystal axes. 293 7.5.2 Results obtained by randomizing the crystal axis . 300 7.6 Birefringence in QUBIC lens combiners. 301 7.7 Conclusions . 303 8 Conclusions 307 Appendices 326 5 Acknowledgments There are quite simply no words that can express my gratitude to my supervisor Dr. Cr´eidheO'Sullivan. Also to quantify my thanks to Prof. Anthony Murphy and the NUIM Experimental Physics department will require a logarithmic scale. I am deeply grateful to my parents, brother, grandparents and my family. And finally many thanks to my friends and colleagues, both new and old. And finally a special thanks to Lee and Dave who saved the entire day at the last minute !!! Abstract In winter 2009 a number of physicists met in Paris to discuss the prospect of ob- serving the CMB B-mode polarization using a novel technique called bolometric in- terferometry. This was the first meeting of what would later become the QUBIC collaboration. In this thesis we discuss the scientific reasons for CMB observation, we present a detailed explanation of how QUBIC will use bolometric interferometry to measure CMB polarization and in particular we discuss the author's contribution to the project. As part of the sub-mm optics research group in the National University of Ireland Maynooth the author was charged with the design and modeling of the optics that would focus the beam from the sky onto the bolometric detectors. This thesis describes various types of reflecting and refracting optics that were investigated. The results we present are useful not only for the QUBIC instrument, but for the design of imaging experiments in general. Detection of CMB B-mode polarization is one of the supreme goals of modern cosmo- logy. The faintness of this signal, combined with the interferometric observing tech- nique, places extreme performance specifications on the QUBIC optics. Fortunately, as we shall show, there are types of well-known reflecting and refracting telescopes that are suitable for QUBIC. In this thesis I propose a design for the quasi-optical combiner that will perform as required. 1 The Cosmic Microwave Background Between the idea And the reality Between the motion And the act T. S. Eliot 1.1 A signal from the early Universe The Cosmic Microwave Background (CMB) is a highly red-shifted thermal radiation signal from the early Universe. From its initial prediction and detection to current attempts to map its polarization the CMB has profoundly deepened our understand- ing of the Universe. To date the CMB has the most accurately measured black body spectrum in nature. Its black body spectrum corresponds to a temperature of T = 2:7 K and it is responsible for a \glow" across the cosmos not associated with a stellar or galactic source. Initially thought to be spurious systemic noise, the CMB has al- lowed us to quantify the curvature of space time as well as ordinary and dark-matter densities. A plethora of scientific knowledge has emerged from the quantification of CMB temperature anisotropies. Detection of CMB polarization is expected to her- ald a new era of understanding of inflationary cosmology. In this chapter we briefly discuss the characteristics of the Microwave Background from its origin to its tem- perature and polarization spectrum. We also present the case for the further study of the CMB concluding with the importance of detecting the extremely faint B-mode polarization. 8 1.2 A brief history of CMB observations For almost 50 years cosmologists have made remarkable attempts to observe the CMB with greater and greater sensitivity. These efforts culminated in May 2009 with the launch of ESA's Planck satellite [1]. Like many scientific milestones the initial discov- ery of the CMB was purely accidental. Predicted by Alpher, Gamov and Hermann in 1947 [2] as a consequence of a Freidmann-Lema^ıtreUniverse it lay undetected until 1965 when two radio astronomers (Penzias and Willson) encountered excess noise in a well calibrated horn antenna. The signal causing this noise appeared isotropic and they estimated that it corresponded to a temperature of 3.5 ± 1.0 K. Following dis- cussions with various other researchers the noise was linked with the relic black body radiation predicted by Alpher and Herman. In 1965 two papers were published that would dramatically influence the course of far infrared astronomy over the next 50 years. The first by Penzias and Wilson detailed their observations [3].
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.
    [Show full text]
  • 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).
    [Show full text]
  • Cosmic Microwave Background Activities at IN2P3
    Cosmic Microwave Background activities at IN2P3 IN2P3 permanent researchers and research engineers APC: James G. Bartlett (Pr.-UPD – Planck), Pierre Binétruy (Pr.-UPD), Martin Bucher (DR2-CNRS – Planck), Jacques Delabrouille (DR2-CNRS – Planck), Ken Ganga (DR1-CNRS – Planck), Yannick Giraud- Héraud (DR1-CNRS - Planck/QUBIC), Laurent Grandsire (IR-CNRS – QUBIC), Jean-Christophe Hamilton (DR2-CNRS – QUBIC), Jean Kaplan (DR émérite-CNRS – Planck/QUBIC), Maude Le Jeune (IR-CNRS – Planck/POLARBEAR), Guillaume Patanchon (MCF-UPD – Planck), Michel Piat (Pr-UPD - Planck/QUBIC), Damien Prêle (IR-CNRS - QUBIC), Cayetano Santos (IR-CNRS, R&D mm), Radek Stompor (DR1-CNRS – Planck/POLARBEAR), Bartjan van Tent (MCF-UPS – Planck), Fabrice Voisin (IR-CNRS – QUBIC/R&D mm); CSNSM: Laurent Bergé (IR-CNRS – QUBIC/R&D mm), Louis Dumoulin (DR émérite-CNRS – QUBIC/R&D mm), Stefanos Marnieros (CR-CNRS – QUBIC/R&D mm); LAL: François Couchot (DR1- CNRS – Planck/QUBIC), Sophie Henrot-Versillé (CR1-CNRS – Planck/QUBIC), Olivier Perdereau (DR2- CNRS – Planck/QUBIC), Stéphane Plaszczynski (DR2-CNRS – Planck/QUBIC), Matthieu Tristram (CR1- CNRS – Planck/QUBIC); LPSC: Olivier Bourrion (IR1-CNRS – NIKA/NIKA2), Andrea Catalano (CR2-CNRS – Planck/NIKA/NIKA2), Céline Combet (CR2-CNRS – Planck), Juan Francisco Macías-Perez (DR2-CNRS – Planck/NIKA/NIKA2), Frédéric Mayet (MCF-UJF – NIKA/NIKA2), Laurence Perotto (CR1-CNRS – Planck/NIKA/NIKA2), Cécile Renault (CR1-CNRS – Planck), Daniel Santos (DR1-CNRS – Planck) IN2P3 Postdoctoral fellows and PhD students APC: Ranajoy Banerji
    [Show full text]
  • Kinetic Inductance Detectors for the OLIMPO Experiment: In–Flight Operation and Performance
    Prepared for submission to JCAP Kinetic Inductance Detectors for the OLIMPO experiment: in–flight operation and performance S. Masi,a;b;1 P. de Bernardis,a;b A. Paiella,a;b F. Piacentini,a;b L. Lamagna,a;b A. Coppolecchia,a;b P. A. R. Ade,c E. S. Battistelli,a;b M. G. Castellano,d I. Colantoni,d;e F. Columbro,a;b G. D’Alessandro,a;b M. De Petris,a;b S. Gordon, f C. Magneville,g P. Mauskopf, f;h G. Pettinari,d G. Pisano,c G. Polenta,i G. Presta,a;b E. Tommasi,i C. Tucker,c V. Vdovin,l;m A. Volpei and D. Yvong aDipartimento di Fisica, Sapienza Università di Roma, P.le A. Moro 2, 00185 Roma, Italy bIstituto Nazionale di Fisica Nucleare, Sezione di Roma, P.le A. Moro 2, 00185 Roma, Italy cSchool of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, UK dIstituto di Fotonica e Nanotecnologie - CNR, Via Cineto Romano 42, 00156 Roma, Italy ecurrent address: CNR-Nanotech, Institute of Nanotechnology c/o Dipartimento di Fisica, Sapienza Università di Roma, P.le A. Moro 2, 00185, Roma, Italy f School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA gIRFU, CEA, Université Paris-Saclay, F-91191 Gif sur Yvette, France hDepartment of Physics, Arizona State University, Tempe, AZ 85257, USA iItalian Space Agency, Roma, Italy lInstitute of Applied Physics RAS, State Technical University, Nizhnij Novgorov, Russia mASC Lebedev PI RAS, Moscow, Russia E-mail: [email protected] Abstract. We report on the performance of lumped–elements Kinetic Inductance Detector (KID) arrays for mm and sub–mm wavelengths, operated at 0:3 K during the stratospheric flight of the OLIMPO payload, at an altitude of 37:8 km.
    [Show full text]
  • ABSTRACT BOOK – 17Th International Workshop on Low Temperature Detectors
    { ABSTRACT BOOK { 17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan June 28, 2017 Preface The International Workshop on Low Temperature Detectors (LTD) is the biennial meeting to present and discuss latest results on research and development of cryogenic detectors for radiation and particles, and on applications of those detectors. The 17-th workshop will be held at Kurume City Plaza in Kurume city, Fukuoka Japan from 17th of July through 21st. The workshop will be organized with the following six sessions: 1. Keynote talks 2. Sensor Physics & Developments, • TES, MMC, MKIDS, STJ, Semiconductors, Novel detectors, others 3. Readout Techniques & Signal processing • Electronics, Multiplexing, Filtering, Imaging, Microwave circuit, Data analysis, others 4. Fabrication & Implementation Techniques • Fabrication process, MEMS, Pixel array, Microwave wirings, others 5. Cryogenics and Components • Refrigerators, Window techniques, Optical Blocking Filters, others 6. Applications • Electromagnetic wave & photon (mm-wave, THZ, IR, Visible, X-ray, Gamma-ray), Particles, Neutrons, CMB, Dark Matter, Neutrinos, Particle & Nuclear Physics, Rare Event Search, Material Analysis & Life Science Kurume is a fabulous location for the workshop. It is known by good local foods and good Sake (Japanese rice wine), and also for traditional fabric called Kurume Gasuri. The LTD17 workshop provides you a wonderful opportunity to exchange your ideas and extend your experience on the low temperature detectors. We hope you will join and enjoy. LOC of 17th International Workshop on Low Temperature Detectors ii Contents Oral presentations 1 Keynote talks 2 O-1 Low Temperature Detectors (for Dark matter and Neutrinos) 30 Years ago. The Start of a new experimental Technology. (Franz von Feilitzsch) .............................
    [Show full text]
  • Cryogenic Half Wave Plate Rotator, Design and Performances
    Prepared for submission to JCAP QUBIC VI: cryogenic half wave plate rotator, design and performances G. D’Alessandro1,2 L. Mele1,2 F. Columbro1,2 G. Amico1 E.S. Battistelli1,2 P. de Bernardis1,2 A. Coppolecchia1,2 M. De Petris1,2 L. Grandsire3 J.-Ch. Hamilton3 L. Lamagna1,2 S. Marnieros4 S. Masi1,2 A. Mennella5,6 C. O’Sullivan7 A. Paiella1,2 F. Piacentini1,2 M. Piat3 G. Pisano8 G. Presta1,2 A. Tartari9 S.A. Torchinsky3,10 F. Voisin3 M. Zannoni11,12 P. Ade8 J.G. Alberro13 A. Almela14 L.H. Arnaldi15 D. Auguste4 J. Aumont16 S. Azzoni17 S. Banfi11,12 A. Baù11,12 B. Bélier18 D. Bennett7 L. Bergé4 J.-Ph. Bernard16 M. Bersanelli5,6 M.-A. Bigot-Sazy3 J. Bonaparte19 J. Bonis4 E. Bunn20 D. Burke7 D. Buzi1 F. Cavaliere5,6 P. Chanial3 C. Chapron3 R. Charlassier3 A.C. Cobos Cerutti14 G. De Gasperis21,22 M. De Leo1,23 S. Dheilly3 C. Duca14 L. Dumoulin4 A. Etchegoyen14 A. Fasciszewski19 L.P. Ferreyro14 D. Fracchia14 C. Franceschet5,6 M.M. Gamboa Lerena24,33 K.M. Ganga3 B. García14 M.E. García Redondo14 M. Gaspard4 D. Gayer7 M. Gervasi11,12 M. Giard16 V. Gilles1,25 Y. Giraud-Heraud3 M. Gómez Berisso15 M. González15 M. Gradziel7 M.R. Hampel14 D. Harari15 S. Henrot-Versillé4 F. Incardona5,6 E. Jules4 J. Kaplan3 C. Kristukat26 S. Loucatos3,27 T. Louis4 B. Maffei28 W. Marty16 A. Mattei2 A. May25 M. McCulloch25 D. Melo14 L. Montier16 L. Mousset3 L.M. Mundo13 J.A. Murphy7 J.D. Murphy7 F. Nati11,12 E. Olivieri4 C.
    [Show full text]
  • CMB Interferometry Clive Dickinson
    CMB interferometry Clive Dickinson∗† Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics & Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, U.K. E-mail: [email protected] Interferometry has been a very successful tool for measuring anisotropies in the cosmic mi- crowave background. Interferometers provided the first constraints on CMB anisotropies on small angular scales (ℓ ∼ 10000) in the 1980s and then in the late 1990s and early 2000s made ground- breaking measurements of the CMB power spectrum at intermediate and small angular scales covering the ℓ-range ≈ 100–4000. In 2002 the DASI made the first detection of CMB polariza- tion which remains a major goal for current and future CMB experiments. Interferometers have also made major contributions to the detection and surveying of the Sunyaev-Zel’dovich (SZ) effect in galaxy clusters. In this short review I cover the key aspects that made interferometry well-suited to CMB measure- ments and summarise some of the central observations that have been made. I look to the future and in particular to HI intensity mapping at high redshifts that could make use of the advantages of interferometry. arXiv:1212.1729v1 [astro-ph.CO] 7 Dec 2012 Resolving the Sky - Radio Interferometry: Past, Present and Future -RTS2012 April 17-20, 2012 Manchester, UK ∗Speaker. †CD acknowledges an STFC Advanced Fellowship and an EU Marie Curie IRG grant under the FP7. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/ CMB interferometry Clive Dickinson Contents 1.
    [Show full text]
  • Phd Program in Astronomy, Astrophysics and Space Science XXXVII Cycle Available Theses @ Tor Vergata, Sapienza, INAF
    PhD program in Astronomy, Astrophysics and Space Science XXXVII cycle Available theses @ Tor Vergata, Sapienza, INAF 1 Contents 1 University of Rome Tor Vergata 6 1.1 Planetary habitability in the galactic context . 6 1.2 Physical Properties of Transiting Planetary Systems . 6 1.3 Observing gaseous exoplanets in formation around young stars 7 1.4 Witnessing the culmination of structure formation in the Uni- verse from X-ray observations of clusters of galaxies . 7 1.5 Millimetre observations of galaxy clusters . 8 1.6 Advanced X-ray modeling of quasar winds . 9 1.7 Illuminating the Universe with the Cosmic Microwave Back- ground . 9 1.8 Unveiling the accretion mechanisms of pulsating ultralumi- nous X-ray sources . 10 1.9 The PILOT balloon borne experiment: Measurement of po- larised emission of dust in the intergalactic medium at THz frequencies . 11 1.10 The early chemical enrichment of the Galactic Bulge using old stellar tracers . 11 1.11 Cosmic distance scale: from primary to secondary distance indicators . 12 1.12 Improving detection capabilities of coalescing compact binary systems in the next generation interferometric gravitational wave detector Einstein Telescope . 12 1.13 Fostering multimessenger techniques in the Einstein Telescope era . 13 1.14 The solar activity and Sun-Earth System . 14 1.15 The Sun: Magnetic Field and the Turbulent Convection . 14 1.16 Extreme Space Weather Events: Advances in Understanding and Forecasting . 15 1.17 Imaging Spectropolarimetric Instruments for Solar Physics . 15 2 Sapienza Universtity of Rome 17 2.1 Search for the origin of the cosmic neutrino flux with ANTARES and KM3NeT .
    [Show full text]
  • Buzi Daniele
    Polarization issues for CMB devices Observing the Universe with the Cosmic Microwave Background, 22-26 April 2014, L'Aquila, Dr. Daniele Buzi Outline Scientific target Cosmic Microwave Background Polarization B modes Experimental aspects QUBIC (Q & U Bolometric Interferometry for Cosmology) experiment Shields analysis with GRASP Anti Reflection Structures (ARS) Observing the Universe with the Cosmic Microwave Background, 22-26 April 2014, L'Aquila, Dr. Daniele Buzi Outline CMB CMB Polarisation QUBIC ARS Conclusions CMB Polarisation Differently by CMB temperature anisotropy, the polarization is generated only by scattering; when we observe the polarization we are looking directly at the so-called last scattering surface (LSS) of the photons direct probe of the Universe at the epoch of recombination • CMB Polarisation is due to the Thomson scattering of the radiation pattern at the recombination To obtain a net linear polarized signal, a local temperature quadrupole anisotropy pattern in the primordial plasma is needed Only about 10 % of the CMB is polarized few μK Observing the Universe with the Cosmic Microwave Background, 22-26 April 2014, L'Aquila, Dr. Daniele Buzi Outline CMB CMB Polarisation QUBIC ARS Conclusions CMB Polarisation W.Hu 3 Sources of the quadrupole temperature anisotropy @ recombination • Scalar Perturbations: density perturbations in the plasma symmetric quadrupole • Vector Perturbations: vorticity in the plasma (negligible @ recombination) • Tensor Perturbations: due to gravitational waves that stretch and squeeze space and λ of the CMB photons asymmetric quadrupole polarization pattern “handedness” Observing the Universe with the Cosmic Microwave Background, 22-26 April 2014, L'Aquila, Dr. Daniele Buzi Outline CMB CMB Polarisation QUBIC ARS Conclusions E and B modes CMB polarisation sky E>0 B<0 pattern can be E-mode gradient component (even) decomposed into 2 B-mode curl component (odd) components E<0 B>0 Observing the Universe with the Cosmic Microwave Background, 22-26 April 2014, L'Aquila, Dr.
    [Show full text]
  • Analysis of Quasi-Optical Components for Far-Infrared Astronomy
    Analysis of Quasi-Optical Components for Far-Infrared Astronomy Presented by Paul Kelly, B.Sc. A thesis submitted for Degree of Master of Science Department of Experimental Physics NUI Maynooth Co. Kildare Ireland May 2014 Head of Department Professor J. A. Murphy Research Supervisor Dr. Créidhe O'Sullivan Contents Contents ........................................................................................................................ i Abstract ....................................................................................................................... v Acknowledgements .................................................................................................... vi Chapter 1 Introduction .............................................................................................. 1 1.1 Introduction to Terahertz / Submillimetre Astronomy ........................................... 1 1.2 The Big Bang and the CMB ................................................................................... 4 1.2.1 The Big Bang ........................................................................................ 4 1.2.2 The Cosmic Microwave Background .................................................... 5 1.2.3 Temperature Anisotropies in the CMB ................................................. 6 1.2.4 CMB Polarization ................................................................................ 10 1.2.5 CMB Instrument Types ....................................................................... 13 1.2.6 CMB Experiments
    [Show full text]
  • BAYESIAN ANALYSIS of SYSTEMATIC EFFECTS in INTERFEROMETRIC OBSERVATIONS of the COSMIC MICROWAVE BACKGROUND POLARIZATION by Ata K
    BAYESIAN ANALYSIS OF SYSTEMATIC EFFECTS IN INTERFEROMETRIC OBSERVATIONS OF THE COSMIC MICROWAVE BACKGROUND POLARIZATION by Ata Karakci B.Sc., Bogazici University; Istanbul, Turkey, 2002 M.Sc., Bogazici University; Istanbul, Turkey, 2004 Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Department of Physics at Brown University Providence, Rhode Island May 2014 c Copyright 2014 by Ata Karakci This dissertation by Ata Karakci is accepted in its present form by the Department of Physics as satisfying the dissertation requirement for the degree of Doctor of Philosophy. Date Gregory S. Tucker, Advisor Recommended to the Graduate Council Date Ian Dell'Antonio, Reader Date Savvas Koushiappas, Reader Approved by the Graduate Council Date Peter M. Weber, Dean of the Graduate School ii Vitae Ata Karakci was born in Odemi¸s,¨ Izmir,_ Turkey in 1980. He graduated from Istanbul's_ Bo~gazi¸ci Universitesi¨ in 2002 with a Bachelor of Science degree in physics. He received his Master of Science degree in physics from Bo~gazi¸ci Universitesi¨ in 2004. Publications: • Sutter, P. M., Wandelt, B. D., McEwen, J. D., Bunn, E. F., Karakci, A., Korotkov, A., Timbie, P., Tucker, G. S. and Zhang, L. (2013) Probabilistic image reconstruction for radio interferometers, to appear in MNRAS arXiv:1309.1469 • Karakci, A., Zhang, L., Sutter, P. M., Bunn, E. F., Korotkov, A., Timbie, P., Tucker, G. S. and Wandelt, B. D. (2013) Systematic Effects in Interferometric Observations of the CMB Polarization, ApJS 207 14, 2013 arXiv:1302.6608 • Karakci, A., Sutter, P. M., Zhang, L., Bunn, E.
    [Show full text]
  • Vision for European Astronomy and Astrophysics at the Antarctic Station Concordia, Dome C in the Next Decade 2010-2020
    A Vision for European Astronomy and Astrophysics at the Antarctic station Concordia, Dome C In the next decade 2010-2020 Prepared by the antarctic research, a european network ARENA for astrophysics consortium in fulfilment of the work programme of the EC-FP6 contract RICA 026150 Silent with star-dust, yonder it lies - What pilgrims travel the Winter Street? The Winter Street, so fair and so white; Are they not those whom here we miss Winding along through the boundless skies, In the ways and the days that are vacant below? Down heavenly vale, up heavenly height. As the dust of that Street their footfalls kiss Faintly it gleams, like a summer road Does it not brighter and brighter grow? When the light in the west is sinking low, Steps of the children there may stray Silent with star-dust! By whose abode Where the broad day shines to dark earth sleeps, Does the Winter Street in its windings go? And there at peace in the light they play, And who are they, all unheard and unseen - While some one below still wakes and weeps. O, who are they, whose blessed feet Pass over that highway smooth and sheen? Miss Edith Matilda Thomas (1854-1925) Table of contents Table 2 A Vision for European Astronomy and Astrophysics at the Antarctic station Concordia, Dome C (2010‑2020). Table of contents executive summary 6 1 approach and scope 12 1a Context 15 1b Brief historical overview 15 • Windows into geospace 16 • First steps of photonic astronomy in Antarctica 16 • Super seeing conditions on the Antarctic plateau 17 • Towards an observatory at Dome C 19
    [Show full text]