DOCSLIB.ORG

Ian Browne Jodrell Bank Centre for Astrophysics, the University of Manchester

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Ian Browne Jodrell Bank Centre for Astrophysics, the University of Manchester Battye, Browne, Dickinson, Heron, Maffei, Pourtsidou 2013 MNRAS, 434, 1239 [arXiv:1209.0343] BINGO: A novel experiment for HI intensity mapping at z=0.1-0.5 Ian Browne Jodrell Bank Centre for Astrophysics, The University of Manchester BINGO : BINGO Players BAOs from JBCA, Manchester Brazil Richard Battye Filipe Abdalla (UCL) Integrated Marie-Anne Bigot-Sazy Elcio Abdalla (Sao Paolo) Michael Brown Raul Abramo (Sao Paolo) Ian Browne Alex Wueunsche (INPE) Neutral Michael D’Cruze Thryso Villela (INPE) Peter Dewdney (SKA PO) +engineers (INPE) Richard Davis Gas Clive Dickinson Uruguay Keith Grainge Gonzalo Tancredi Bruno Maffei Manuel Caldas Alkistis Portsidou (->Portsmouth) Emilio Falco Observations Peter Wilkinson Ana Mosquera KACST, Saudi Arabia Zurich (ETH) Yaser Hafez Alex Refregier Adam Amara Christian Monstein Outline • Very brief background • BINGO approach • Current design • Expected performance • Where we are now • L-BASS as a test platform (Battye, Weller & Davies, 2004; Peterson 2006) Consider cell at z=0.5 (30 arcmin)2 Equivalent to (8h-1Mpc)3 s 8 ~ 1 Dfobs = 1MHz 10 Average HI mass in side the cell = 1.2 x 10 Msun Brightness Temp = approx 100 mK with fluctuations = O(1) Typical Noise Level on 1MHz is 50mKs1/2 -> around 3days to detect 100 mK BINGO approach • Let’s try and make life as easy as possible – Build on CMB experience – No moving parts – Room temperature amplifiers – Sidelobes as low as possible – Low cross polarization – observe in circular • Build quickly! Tenerife Experiment (circa 1990-6) JBO/Cambridge/IAC CMB expt led by Rod Davies History, but an inspiration for BINGO and L-BASS BINGO concept • Correlation receiver • Use celestial pole as reference • Long focal length to get wide field of view with single dish • Multiple scalar horn feeds to give coverage and clean beams • Exploit local landscape for structural support and RFI screening Single dish limitations • Resolution limited by size and size limited by money (<50m) • Mobile phones 900MHz to 950MHz combined with resolution => observations between 960MHz and 1260MHz • Field of view is modest (~15 degrees) even with long focal length • Need big feed horns • Need a clear view of celestial pole BINGO concept (revised) Key specifications Dish diameter : 40m Resolution : 0.67 deg Frequency range : 960 - 1260MHz (z=0.12 - 0.48) Number of feeds : ~50-70 (dual pol.) No cryogenics : Tsys ≈ 50K Digital correlation receiver <<50 MHz channel resolution (Δz<0.05) Most r/x components “off-the-shelf” Survey Design Observation time : several years Area : 10 x 200 deg2 – drift scan Static telescope with 2 ≈40m Guiding principle : simplicity ! wire-mesh dishes (No moving parts) BINGO site selected: Quarry Castrillon is almost perfect (Minas Corrales, N. Uruguay) Precise optimization of the optics suggests that we can fit in a bigger focal plane array – at least 15 deg x 15 deg – subject to cost Horn array (detectors) ≈40m Primary Secondary mirror mirror Courtesy Bruno Maffei & Adrian Galtress Castrillon RFI tests – looks good! Courtesy Christian Monstein, Gonzalo Tancredi, Manuel Caldas Clean spectrum Above 960 MHz Correlation receiver (Celestial pole) Reference Phase A/ D beam switch L/ O Computer Science Phase A/ D beam switch Hybrid Hybrid Mixer • 1/f knee frequency of typical receivers is ≈1 Hz • Perfect correlation r/x can remove the 1/f if well balanced • Plan to use Celestial Pole as reference • To achieve 1mHz we need : - Input matching to < 3% - Hybrid accurate to < 1.5% Prototype receiver being • Replace function of second hybrid with digital tested at Jodrell Bank backend. BINGO beams Edge pixel – co-polar Edge pixel – cross-polar Projected BAO detection ≈5 sigma detection should be achievable in 1 year on sky (probably 2 years real time) (we have been conservative in our error budget) 1 full year of observations (2000 sq deg.,0.7 deg FWHM) 50 feeds (dual pol) Tsys=50K Measurement of acoustic scale to dkA/kA≈ 0.024 (2.4%) (comparable to the current best optical surveys at present) BAO “Hubble diagram” BINGO BINGO w=-0.84 w=-0.93 We have to be unconventional Horn ideas and must coat lightweight materials with conducting surfaces. Insulating foams Glass reinforced fibre (GRP) Stacked aluminium sections Vacuum deposition Flame spraying Metal tape Paint 3D printing Foam sheets – second test of concept. Feed statistics • The real thing needs to be 4.5m long and 1.7m diameter! • The test horn is 2m by 0.55m • Made from 78 sheets of builder’s insulation board each 25mm thick. Plus copper tape • Constructed by hand • It works! • (Circular to rectangular transition also made from foam and copper tape) Return loss Insertion loss. Red is transition alone The next step • Make an instrument at Jodrell that can test BINGO concept – Test horns – Test receiver stability – Test noise performance – Test digital backends • Do some astronomical observations – L-BASS L-BASS; L-Band All Sky Survey • Learning exercise for BINGO • CMB foregrounds • Checking ARCADE 2 result • Two identical large horns. One looks at NCP while the other pointed in elevation • ~15 degree resolution L-BASS players: • Circular polarization Peter Wilkinson • Correlation receiver measures Ian Browne sky minus reference Bruno Maffei • 50 MHz band around 1420MHz Et al. • Cold load for absolute calibration Summary of the ARCADE 2 result presented in Hooper et al., 2012 (arxiv.org:1203.3547) Possible ARCADE explanations • Sources. Need to be completely new population several times larger than extrapolation. • Incorrect temperature accounting. Has the Galactic component been properly subtracted? (L-BASS should do better job) • Dark Matter decay? • ???? Horn 5m Horn 5m Axle Support Support frame frame Hybrid and Flexible receiver cable L-BASS • Two logical steps: – Map the sky relative to NCP – Measure the absolute brightness of NCP but postpone this • Both horns identical with circular beams. Use foam sheets as a test for BINGO • Both can point at NCP so “self-referencing” can be done during mapping • Need a well calibrated and reliable connection between horns and static Magic-tee. Use cables! • For absolute calibration replace alternative horns with a temperature-monitored matched load in a dewar. BINGO additional science • Life history of hydrogen - First detection of an FRB - from the strength of signal as a function of redshift. • Fast Radio Bursts (FRBS) -- A completely new area. Detection machine and in a BINGO phase-2 we could add outriggers and do astrometry. • Radio recombination lines – come for free and will be an order of magnitude deeper than anything before. • Other Galactic science Concluding remarks • BINGO is a competitive BAO experiment using intensity mapping idea - total build cost $4M - proposals in to FAPESP and MERCORSUR • Cosmology is presently systematics limited • S/N is not the only driver and checking the BAO measurement made in the optical is important • There is plenty of additional science to be done, including FRBs • Building L-BASS as a working test-bed for BINGO instrumentation is the plan for this summer .
Load more

Recommended publications
  • George Harrison
    COPYRIGHT 4th Estate An imprint of HarperCollinsPublishers 1 London Bridge Street London SE1 9GF www.4thEstate.co.uk This eBook first published in Great Britain by 4th Estate in 2020 Copyright © Craig Brown 2020 Cover design by Jack Smyth Cover image © Michael Ochs Archives/Handout/Getty Images Craig Brown asserts the moral right to be identified as the author of this work A catalogue record for this book is available from the British Library All rights reserved under International and Pan-American Copyright Conventions. By payment of the required fees, you have been granted the non-exclusive, non-transferable right to access and read the text of this e-book on-screen. No part of this text may be reproduced, transmitted, down-loaded, decompiled, reverse engineered, or stored in or introduced into any information storage and retrieval system, in any form or by any means, whether electronic or mechanical, now known or hereinafter invented, without the express written permission of HarperCollins. Source ISBN: 9780008340001 Ebook Edition © April 2020 ISBN: 9780008340025 Version: 2020-03-11 DEDICATION For Frances, Silas, Tallulah and Tom EPIGRAPHS In five-score summers! All new eyes, New minds, new modes, new fools, new wise; New woes to weep, new joys to prize; With nothing left of me and you In that live century’s vivid view Beyond a pinch of dust or two; A century which, if not sublime, Will show, I doubt not, at its prime, A scope above this blinkered time. From ‘1967’, by Thomas Hardy (written in 1867) ‘What a remarkable fifty years they
    [Show full text]
  • The Iau Historic Radio Astronomy Working Group
    THE IAU HISTORIC RADIO ASTRONOMY WORKING GROUP. 2: PROGRESS REPORT This Progress Report follows the inaugural report of the Working Group (WG), which appeared in the April 2004 ICHA Newsletter and was published in the June 2004 issue of the Journal of Astronomical History and Heritage (see Orchiston et al., 2004, below). Role of the WG This WG was formed at the 2003 General Assembly of the IAU as a joint initiative of Commissions 40 (Radio Astronomy) and 41 (History of Astronomy), in order to: • assemble a master list of surviving historically-significant radio telescopes and associated instrumentation found worldwide; • document the technical specifications and scientific achievements of these instruments; • maintain an on-going bibliography of publications on the history of radio astronomy; and • monitor other developments relating to the history of radio astronomy (including the deaths of pioneering radio astronomers). New Committee Members Since the last report was prepared we have added two further members to the Committee of the WG. As Chair of the WG, I am delighted to offer a warm welcome to Richard Wielebinski from the Max Planck Institute for Radioastronomy, representing Germany, and Jasper Wall (University of British Columbia), who represents Canada. Further Publications on the History of Radio Astronomy Balick, B., 2005. The discovery of Sagittarius A*. In Orchiston, 2005b, 183-190. Beekman, G., 1999. Een verjaardag zonder jarige. Zenit, 26(4), 154-157. Cohen, M., 2005. Dark matter and the Owens Valley Radio Observatory. In Orchiston, 2005b, 169-182. Davies, R.D., 2003. Fred Hoyle and Manchester. Astrophysics and Space Science, 285, 309- 319.
    [Show full text]
  • August to December 2011 ALTERNATIVE COSMOLOGY GROUP
    1 ALTERNATIVE COSMOLOGY GROUP www.cosmology.info Monthly Notes of the Alternative Cosmology Group – 2011 Part Two: August to December 2011 The ACG Webmaster who distributes this newsletter to subscribers would prefer not to receive related correspondence. Please address all correspondence to MNACG Editor, Hilton Ratcliffe: [email protected]. The ACG newsletter is distributed gratis to subscribers. Get onto our mailing list without obligation at www.cosmology.info/newsletter. The current newsletter is a review of more than 12,000 papers published on arXiv under astro-ph, together with 6500 under gen-phys, for the months of April to December, 2011. We now include papers archived elsewhere, provided access is full and open. The Alternative Cosmology Group draws its mandate from the open letter published in New Scientist, 2004 (www.cosmologystatement.org), and these monthly notes seek to publicise recently published empirical results that are aligned with that ethos. In other words, what observations seem anomalous in terms of the Standard Model of Cosmology? We prefer observational results and tend to avoid complete cosmologies and purely theoretical work. Discussion of method is welcome. If you would like to suggest recently published or archived papers for inclusion, please send the arXiv, viXra or other direct reference and a brief exposition to Hilton Ratcliffe ([email protected]). Note that our spam filter rejects slash and colon in the text, so please write web addresses commencing “www”. I. Editorial comment I apologise most profusely again for the delay in getting the MNACG out to you. This newsletter and one that preceded it cover several months each, so please pardon their lengthiness.
    [Show full text]
  • The Very Small Array: Latest Results and Future Plans
    The Very Small Array: latest results and future plans Keith Grainge Astrophysics Group, Cavendish Laboratory, Cambridge Rencontres de Moriond, 31 March 2004 OVERVIEW The Very Small Array (VSA) • Current primordial observations • The S-Z effect • Planned upgrades to the instrument • Future science at high ` • Summary • 1 THE VSA CONSORTIUM Cavendish Astrophysics Group Roger Boysen Tony Brown Chris Clementson Mike Crofts Jerry Czeres Roger Dace Keith Grainge (PM) Mike Hobson (PI) Mike Jones Rüdiger Kneissl Katy Lancaster Anthony Lasenby Klaus Maisinger Ian Northrop Guy Pooley Vic Quy Nutan Rajguru Ben Rusholme Richard Saunders Richard Savage Anna Scaife Jack Schofield Paul Scott (Former PI) Clive Shaw Anze Slosar Angela Taylor David Titterington Elizabeth Waldram Brian Wood Jodrell Bank Observatory Colin Baines Richard Battye Eddie Blackhurst Pedro Carreira Kieran Cleary Rod Davies Richard Davis Clive Dickinson Yaser Hafez Mark Polkey Bob Watson Althea Wilkinson Instituto de Astrofísica de Canarias Jose Alberto Rubiño-Martin Carlos Guiterez Rafa Rebolo Lopez Pedro Sosa-Molina Ricardo Genova-Santos 2 THE VERY SMALL ARRAY (VSA) Sited on Observatorio del Teide, Tenerife • 14 antennas 91 baselines • ) Observing frequency ν = 26 36 GHz; bandwidth ∆ν = 1:5 GHz • − Compact configuration: 143 mm horns; ` = 150 800; ∆` 90 (without • − ≈ mosaicing); Sept 2000 – Sept 2001 Extended configuration: 322 mm horns; ` = 300 1800; ∆` 200 (without • − ≈ mosaicing); Sept 2001 – present 3 COMPARISON WITH OTHER CMB EXPERIMENTS Different systematics from “single-dish” experiments: • – negligible pointing error – negligible beam uncertainty Different from other CMB interferometers (DASI, CBI): • – RT survey and dedicated source subtraction 2-element interferometer remove effect of extragalactic point sources ) – tracking elements rather than comounted can apply fringe rate filter to remove unwanted signals.
    [Show full text]
  • C-Band All Sky Survey (C-BASS)
    C-Band All Sky Survey (C-BASS) J. P. Leahy (PI, Manchester), M. E. Jones (PI, Oxford) Clive Dickinson (JPL) AIMS: • Definitive survey of Galactic synchrotron radiation and its polarization • Anchor for synchrotron emission in future CMB polarimetry experiments up to CMBPOL. • Prototype for possible ground-based surveys at frequencies up to CMB band: 10, 15, 30… GHz • New window on Galactic magnetic field and cosmic rays BPOL workshop 27th October 2006 Galactic foregrounds WMAP polarized brightness: 23 GHz, 4° beam • Sky is full of polarized interstellar synchrotron emission – 91% of pixels detected at this resolution • All components have significant spectral variations We must have more measurements than parameters! BPOL workshop 27th October 2006 Foreground brightness • Smoothing removes emission that fluctuates on scales smaller than the beam – E.g. CMB ‘E-modes’ • Similar amplitudes at 2° and 4°: – Looking at signal, not noise! – Polarization has little small- scale structure. • (Foreground, high latitude) • At 4° resolution, polarization clearly detected in 91% of pixels • Median: 15 µK @ 22.5 GHz • Histogram of polarization values at 22.5 GHz, 4° beam, with various masks BPOL workshop 27th October 2006 4° Pol. Maps in other bands 33 GHz 41 GHz 61 GHz 94 GHz BPOL workshop 27th October 2006 C-BASS motivation • CMB polarization splits T into orthogonal modes: • E-modes fix optical depth to re-ionization – dramatic reduction in parameter degeneracy • B-modes define energy E scale of inflation • Obscured by Galactic B foreground emission – minimum at ~60 GHz – synchrotron below – dust above. BPOL workshop 27th October 2006 C-BASS motivation: 60 GHz • E-modes fix optical depth to re-ionization C-BASS – dramatic reduction in E parameter degeneracy 60 GHz • B-modes define energy scale of B inflation • Obscured by Galactic r = 0.1 foreground emission – minimum at ~60 GHz g in – synchrotron below s n e – dust above.
    [Show full text]
  • Under the Radar Astrophysics and Space Science Library
    Under the Radar Astrophysics and Space Science Library EDITORIAL BOARD Chairman W. B. BURTON, National Radio Astronomy Observatory, Charlottesville, Virginia, U.S.A. ([email protected]); University of Leiden, The Netherlands ([email protected]) F. BERTOLA, University of Padua, Italy J. P. CASSINELLI, University of Wisconsin, Madison, U.S.A. C. J. CESARSKY, European Southern Observatory, Garching bei Mu¨nchen, Germany P. EHRENFREUND, Leiden University, The Netherlands O. ENGVOLD, University of Oslo, Norway A. HECK, Strasbourg Astronomical Observatory, France E. P. J. VAN DEN HEUVEL, University of Amsterdam, The Netherlands V. M. KASPI, McGill University, Montreal, Canada J. M. E. KUIJPERS, University of Nijmegen, The Netherlands H. VAN DER LAAN, University of Utrecht, The Netherlands P. G. MURDIN, Institute of Astronomy, Cambridge, UK F. PACINI, Istituto Astronomia Arcetri, Firenze, Italy V. RADHAKRISHNAN, Raman Research Institute, Bangalore, India B. V. SOMOV, Astronomical Institute, Moscow State University, Russia R. A. SUNYAEV, Space Research Institute, Moscow, Russia W.M. Goss l Richard X. McGee Under the Radar The First Woman in Radio Astronomy: Ruby Payne-Scott Prof. W. M. Goss Dr. Richard X. McGee National Radio Astronomy Commonwealth Scientific& Observatory Industrial 1003 Lopezville Road P.O.Box O Research Organisation Socorro NM 87801 (CSIRO) USA Radiophysics Laboratory [email protected] Epping NSW 1710 Australia ISSN 0067-0057 ISBN 978-3-642-03140-3 e-ISBN 978-3-642-03141-0 DOI 10.1007/978-3-642-03141-0 Springer Heidelberg Dordrecht London New York Library of Congress Control Number: 2009931715 # Springer-Verlag Berlin Heidelberg 2010, 2nd corrected printing This work is subject to copyright.
    [Show full text]
  • The Iau Historic Radio Astronomy Working Group
    Journal of Astronomical History and Heritage, 12(3), 249-253 (2009). THE IAU HISTORIC RADIO ASTRONOMY WORKING GROUP. 3: PROGRESS REPORT (2006-2009) This Progress Report follows the publication of two et al., 2009—see details, the listing in Section 6, earlier Progress Reports (Orchiston, et al., 2004; 2005) below). Two further papers, completing this series, and a Triennial Report of the Working Group for will be published in March 2010. 2003-2006 (Orchiston, et al., 2006), all of which appeared in the Journal of Astronomical History and 5 Research on the History of Radio Astronomy Heritage. Colleagues who actively researched aspects of radio astronomical history during 2005-2009 included: the 1 Role of the Working Group late Émile-Jacques Blum (France), André Boischot This WG was formed at the 2003 General Assembly of (France), the late Ron Bracewell (USA), Wim Brouw the IAU as a joint initiative of Commissions 40 (Radio (The Netherlands), Geoffrey Burbidge (USA), Bernard Astronomy) and 41 (History of Astronomy), in order Burke (USA), Ron Burman (Australia), Jessica Chap- to: man (Australia), Marshall Cohen (USA), Nan Dieter • assemble a master list of surviving historically- Conklin (USA), R.D. Dagkesamanskii (Russia), Rod significant radio telescopes and associated instru- Davies (United Kingdom), Suzanne Débarbat mentation found worldwide; (France), Jean Delannoy (France), John Dickel (USA), • document the technical specifications and scien- Martin George (Australia), Miller Goss (USA), Dave tific achievements of these instruments; Green (United Kingdom), Alastair Gunn (United • maintain an on-going bibliography of public- Kingdom), Dave Jauncey (Australia), Ken Kellermann cations on the history of radio astronomy; and (USA), A.A.
    [Show full text]
  • Application of Novel Analysis Techniques to Cosmic Microwave
    Application of novel analysis techniques to Cosmic Microwave Background astronomy Aled Wynne Jones Mullard Radio Astronomy Observatory and King’s College, Cambridge. A dissertation submitted for the degree of Doctor of Philosophy in the University of Cambridge. arXiv:astro-ph/9903173v1 11 Mar 1999 i Preface This dissertation is the result of work undertaken at the Mullard Radio Astronomy Observatory, Cambridge between October 1994 and September 1997. The work described here is my own, unless specifically stated otherwise. To the best of my knowledge it has not, nor has any similar dissertation, been submitted for a degree, diploma or other qualification at this, or any other university. This dissertation does not exceed 60 000 words in length. Aled Wynne Jones To Isabel and Ffion ii I am not sure how the universe was formed. But it knew how to do it, and that is the important thing. Anon. (child) It is enough just to hold a stone in your hand. The universe would have been equally incomprehensible if it had only consisted of that one stone the size of an orange. The question would be just as impenetrable: where did this stone come from? Jostein Gaarder (in ‘Sophie’s World’) Acknowledgements Firstly I would like to thank the two people who have introduced me to the immense field of microwave background anisotropies, Anthony Lasenby and Stephen Hancock. Without them I would not have begun to uncover the beauty at the beginning of time. I would also like to thank Joss Bland-Hawthorn whose supervision and enthusiasm during my time in Australia has made me more inquisitive in my field.
    [Show full text]
  • Legitimating Astronomy
    University of Wollongong Research Online University of Wollongong Thesis Collection 1954-2016 University of Wollongong Thesis Collections 2004 Legitimating Astronomy Graham Howard University of Wollongong Follow this and additional works at: https://ro.uow.edu.au/theses University of Wollongong Copyright Warning You may print or download ONE copy of this document for the purpose of your own research or study. The University does not authorise you to copy, communicate or otherwise make available electronically to any other person any copyright material contained on this site. You are reminded of the following: This work is copyright. Apart from any use permitted under the Copyright Act 1968, no part of this work may be reproduced by any process, nor may any other exclusive right be exercised, without the permission of the author. Copyright owners are entitled to take legal action against persons who infringe their copyright. A reproduction of material that is protected by copyright may be a copyright infringement. A court may impose penalties and award damages in relation to offences and infringements relating to copyright material. Higher penalties may apply, and higher damages may be awarded, for offences and infringements involving the conversion of material into digital or electronic form. Unless otherwise indicated, the views expressed in this thesis are those of the author and do not necessarily represent the views of the University of Wollongong. Recommended Citation Howard, Graham, Legitimating Astronomy , PhD thesis, School of Social Science, Media and Communication, University of Wollongong, 2004. http://ro.uow.edu.au/theses/333 Research Online is the open access institutional repository for the University of Wollongong.
    [Show full text]
  • Progress Report
    Journal of Astronomical History and Heritage, 7: 53-56 (2004) The IAU Historic Radio Astronomy Working Group. 1: Progress Report Wayne Orchiston Anglo-Australian Observatory, and Australia Telescope National Facility, PO Box 296, Epping, NSW 2121, Australia E-mail: [email protected] Rod Davies Jodrell Bank, University of Manchester, Macclesfield, SK11 9DL, U.K. E-mail: [email protected] Jean-Francois Denisse 48 rue Mr Le Prince, 75006 Paris, France E-mail messages to: [email protected] Ken Kellermann National Radio Astronomy Observatory, 520 Edgemont Rd., Charlotteville, VA 22903-2475, U.S.A. E-mail: [email protected] Masaki Morimoto Nishi Harima Astronomical Observatory, 407 2 Nishi Kawachi, Sayoh Cho, Hyohgo 679 5313, Japan E-mail: [email protected] Slava Slysh Astronomy Space Center, Lebedev Physical Institute, PrBoxsojuznaya Ul 84/32, 117810 Moscow, Russia E-mail: [email protected] Govind Swarup NCRA TIFR, Pune University Campus Pb3, Ganeshkind, Pune 411 007, India E-mail: [email protected] Hugo van Woerden Kapteyn Sterrekundig Instituut, University of Groningen, Box 800, 9700 AV Groningen, The Netherlands E-mail: [email protected] This new Working Group was established at the Australia’s pioneering efforts in international radio July 2003 IAU General Assembly in Sydney, with a astronomy, it was only natural that such sessions view to: should form part of the program at the Sydney GA, (1) assembling a master list of surviving and it was pleasing to see that they drew capacity historically-significant radio telescopes and audiences. Science Meeting 2, on “The Early associated instrumentation found world- Development of Australian Radio Astronomy”, ran wide; all day on July 21, and attracted the following oral (2) documenting the technical specifications and and poster papers: scientific achievements of such instruments; (3) maintaining an on-going bibliography of Sullivan, W.
    [Show full text]
  • Observational and Theoretical Advances in Cosmological Foreground Emission
    Observational and Theoretical Advances in Cosmological Foreground Emission Thesis by Matthew A. Stevenson In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy California Institute of Technology Pasadena, California 2014 (Defended July 12, 2013) ii © 2014 Matthew A. Stevenson All Rights Reserved iii Dedicated to Jennifer, Bronson, and Edmund. iv Acknowledgments I carry a debt of gratitude to many people. First I must thank my supervisor Tony Readhead for his support of this work and his patience for the variety of crazy ideas I came up with (and sometimes discarded) along the way. I must also thank Tim Pearson, who acted as my mentor in the day-to-day grind of actually getting this work done. His patience was inexhaustible, despite my many false starts and dead ends. Being a part of C-BASS has afforded me the pleasure of working with many smart people. Fore- most is Oliver King, my analog counterpart, with whom I have enjoyed many frantic troubleshooting sessions. Jaya John John set me on the path of FPGA programming, which has been great fun. Clive Dickinson's insights and support of my efforts have been a huge inspiration. Stephen Mu- chovej's tireless work on the telescope, control system, and pipeline were indispensable. This project has also given me the privilege of working with Rachana Bhatawdekar, Roy Booth, Charles Copley, Rod Davies, Richard Davis, Paul Grimes, Yaser Hafez, Christian Holler, Melis Irfan, Justin Jonas, Dayton Jones, Mike Jones, Paddy Leahy, Jamie Leech, Erik Leitch, Angela Taylor, and Joe Zuntz. Outside of the C-BASS collaboration, I have had the opportunity to work with many other fine people.
    [Show full text]
  • FAS 09 Spring 90Electronic.Pub
    FAS Newsletter Federation of Astronomical Societies http://www.fedastro.org.uk Scotland selects two dark sky sites To celebrate the International Year of Astronomy 2009, the world's first Dark Sky Discovery Sites were announced in Scotland. Provided by Science and Technology Council, UK he Dark Sky Scotland partnership named the two sites as Newbattle Abbey College in Dalkeith and Highland Council's Glen Nevis Visitor Center grounds, near Fort William. The two sites, which are relatively free of light Tpollution, tall buildings, and are safe and accessible, were chosen following a winter of community astronomy activities led by the John Muir Trust, the Highland Council Countryside Rangers, and the Forestry Commission Scotland. "Many of us live in light polluted towns and cities yet in every community there is somewhere that is the best local place to go to look up and discover the stars," said Dan Hiller from the Royal Observatory Edinburgh Visitor Center. "From these places, which might be a park or playing field, you can see planets, hundreds of stars, space satellites, and other wonders of the night sky. The organizations that have identified these first two Dark Sky Discovery Sites have taken a world leading role in helping people to discover the Students study the stars at Newbattle Abbey College in universe that is on their doorsteps." Dalkeith. Forestry Commission Scotland The announcement of the sites took place March 25 at Newbattle it adds a natural feel to the whole experience of stargazing." Abbey College, Scotland's only adult education residential college. "There are wonderful opportunities in the Highlands to view and "Woodlands are a fantastic place to view the stars," said Jeremy experience the fascination of planets and space," said Iain Ross of The Thompson of Forestry Commission Scotland, which works closely Highland Council's Planning, Environment, and Development with Newbattle Abbey College.
    [Show full text]