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The Infrared and Submillimetre Sky after COBE
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Series C: Mathematical and Physical Sciences - VoI. 359
The Infrared and Submillimetre Sky after COBE
edited by
M. Signore and
c. Dupraz Ecole normale superieure, Paris, France and Observatoire de Meudon, Meudon, France
Springer-Science+Business Media, B.v.
Proceedings of the NATO Advanced Study Institute on The Infrared and Submillimetre Sky after COBE Les Houches, France March 20-30,1991
ISBN 978-94-010-5080-7 ISBN 978-94-011-2448-5 (eBook) DOI 10.1007/978-94-011-2448-5
AII Rights Reserved © 1992 Springer Science+Business Media Dordrecht Originally published by Kluwer Academic Publishers in 1992 Softcover reprint of the hardcover 1 st edition 1992 No part of the material protected by this copyright notice may be reproduced or utilized in any form or by any means, electronic or mechanical, including photocopying, recording or by any information storage and retrieval system, without written permission from the copyright owner.
TABLE OF CONTENTS
PREFACE vii
LIST OF PARTICIPANTS ix
LIST OF LECTURERS xi
PLATES OF COBE xiii
I. INTRODUCTORY LECTURE
An Overview of the Cosmic Background Explorer (COBE) and its Observations: New Sky Maps of the Early Universe: George F. Smoot 1
II. THE EARLY UNIVERSE
Strings, Gravity, and the Constants of Nature: G. Veneziano 15 First-Order Inflation: Michael S. Turner 35 Inflation, Great Attractor and Anisotropies of the Relic Radiation: V N. Lukash 75 String Theory in Cosmology: N. Sanchez 87 Cosmic Strings: An Introduction to their Formation, Evolution, and their
Microwave Background Signature: Franfois R. Bouchet IGI The Cosmic Microwave Background Radiation: Joseph Silk 129 The Spectral Distortions of the Cosmic Microwave Background Radiation, LEP
and Heavy Neutrinos: P. Salati 143 Dark Matter Candidates and Methods for Detecting Them: G.G. Raffelt 175 Fluctuations and Anisotropies in Integrated Backgrounds: Xavier Barcons 189 The Thermal History of the Cosmological Gas: A. Blanchard 201
III. INFRARED TO SUB MILLIMETRE BACKGROUNDS
Sources of Cosmic Infrared-Submillimetre Background Radiation: B.l. Carr 213 Preliminary Results from the FIRAS and DIRBE Experiments on COBE
EL. Wright 231 Submm Emission from Galaxies and Quasars: Rolf Chini 249 Infrared Emission from the Galaxy: F. Boulanger and F X. Desert 263
vi
IV. ANISOTROPIES OF THE CMB
Linear and Non-linear Gravitational Effects on the CMB Anisotropy E. Martinez-Gonzalez 291
Statistics of the CMB Maps: E. Martinez-Gonzalez and L. Cayon 303 CMB and Galactic Maps in the Millimetric Region
Paolo de Bernardis, Silvia Masi, and Nicola Vittorio 315 COBE DMR Results and Implications: George F. Smoot 331 Cosmic Background Anisotropies in the Millimetric Region
S. Bottani, P. de Bernardis, M. de Petris, S. Masi, B. Melchiorri, F. Melchiorri, and P. Tanzilli 345
Upper Limits on the CMB Variation from 1300 11m Observations: RolfChini 385
V. INSTRUMENTATION
Mapping the Sky with the COBE Differential Microwave Radiometers M.A. Janssen and S. Gulkis
Fundamental and Practical Limits to the Sensitivity of Submillimeter Astronomical Observations: J.M. Lamarre
Observations at (Sub)millimetre Wavelengths: Effect of Atmosphere and Telescope Sidelobes : M. GuBin
VI. CONCLUSION
Early Measurements of the CMB : Pierre Encrenaz Summary of Meeting : BJ. Carr
AUTHOR INDEX
SUBJECT INDEX
391
409
423
445 449
463
465
PREFACE
This volume consists of invited lectures and seminars presented at the NATO Advanced Study Institute "The Infrared and Submillimetre Sky after COBE", which was held at the Centre de Physique Theorique of Les Houches (France) in March 1991.
The school has been planned by a Scientific Organizing Committee. It was organized with the aim of providing students and young researchers with an up-to-date account of the Cosmic Microwave Background, the Cosmic Infrared Background (if any), and the infrared emission of the Galaxy, after the early results from COBE (Cosmic Background Explorer). It was attended by about sixty researchers from many countries.
The lectures and seminars represent a complete coverage of our present knowledge and understanding of: the Early Universe, Large-Scale Structure, Dust in Galaxies, Infrared to Submillimetre Backgrounds, CMB Anisotropies, complementary observations and instrumentation problems, etc. Most of these lectures are reproduced in this volume. Unfortunately, a few lecturers have chosen not to submit their manuscript.
I would like to express my gratitude to the Scientific Affairs Division of NATO (North Atlantic Treaty Organization) and to the Theoretical Physics and Astrophysics Sections of the CNRS (Centre National de la Recherche Scientifique) for their generous support. Further help was obtained from the DRET (Direction des Recherches, Etudes et Techniques), the CNES (Centre National d'Etudes Spatiales) and the IN2P3 (Institut National de Physique Nuc1eaire et de Physique des Particules), which I hereby gratefully acknowledge.
Special thanks are due to Brigitte Rousset and Daniele Choupin for taking care of everyone so well at the Centre de Physique Theorique in the beautiful setting of Les Houches.
Finally, many thanks to all the invited speakers whose papers appear below.
Scientific Organizing Committee :
Monique Signore Director of the School
M.G. HAUSER, USA; F. MELCHIORRI, Italy; D. SCIAMA, Italy; M. SIGNORE, France.
Co-Editors: M. SIGNORE and C. DUPRAZ, France.
vii
LIST OF PARTICIPANTS
Xavier BARCONS : Universidad de Cantabria, Santander, SPAIN James G. BARTLETI: University o/California at Berkeley, Berkeley, USA Alain BLANCHARD: Observatoire de Paris-Meudon, Meudon, FRANCE Samuele BOTIANI: Universita "La Sapienza", Roma, ITALY Fran~ois BOUCHET : Institut d'Astrophysique de Paris, Paris, FRANCE Fran~ois BOULANGER: Ecole Normale Superieure, Paris, FRANCE Alberto CAPPI: Osservatorio Astronomico di Bologna, Bologna, ITALY Bernard CARR: Queen Mary College, London, UNITED KINGDOM Laura CAYON-TRUEBA : Universidad de Cantabria, Santander, SPAIN Rolf CHINI : Max-Planck Institut/ur Radioastronomie, Bonn, GERMANY Fabrice DEBBASCH : Ecole Normale Superieure, Paris, FRANCE Paolo DE BERNARDIS : Universita "La Sapienza", Roma, ITALY Antonella DE LUCA : Universita "La Sapienza", Roma, ITALY Marco DE PETRIS : Universita "La Sapienza", Roma, ITALY Christophe DUPRAZ : Ecole Normale Superieure, Paris, FRANCE Pierre ENCRENAZ : Ecole Normale Superieure, Paris, FRANCE Michele EPIFANI: Universita "La Sapienza", Roma, ITALY Maria-Cristina F AL VELLA: Universita "La Sapienza", Roma, ITALY Massimo GERVASI: Universita "La Sapienza", Roma, ITALY Krzysztof M. GORSKI: Princeton University, Princeton, USA Michel GUELIN : Institut de Radioastronomie Millimerrique, Grenoble, FRANCE Stephen HANCOCK: Cavendish Laboratory, Cambridge, UNITED KINGDOM Robin HARMON: California Institute o/Technology, Pasadena, USA Michael A. JANSSEN: Jet Propulsion Laboratory, Pasadena, USA Roman mSZKIEWICZ: N. Copernicus Astronomical Center, Warszawa, POLAND Jean-Michel LAMARRE: Institut d'Astrophysique Spatiale, Orsay, FRANCE Ariane LANCON: Institut d'Astrophysique de Paris, Paris, FRANCE Anthony LASENBY : Cavendish Laboratory, Cambridge, UNITED KINGDOM Charles LINEWEAVER: Lawrence Berkeley Laboratory, Berkeley, USA Vladimir LUKASH : Space Research Institute, Moscow, USSR Bruno MAFFEI: Institut d'Astrophysique Spatiale, Verrieres-le-Buisson, FRANCE Roberto MAOLI : Universita "La Sapienza", Roma, ITALY Enrique MARTINEZ-GONZALEZ: Universidad de Cantabria, Santander, SPAIN Silvia MASI : Universita "La Sapienza", Roma, ITALY Sophie MAUROGORDATO: Observatoire de Paris-Meudon, Meudon, FRANCE Francesco MELCHIORRI : Universita "La Sapienza", Roma, ITALY Tabar MELLm : lnstitut d'Astrophysique de Paris, Paris, FRANCE
ix
x
Bianca OLIVO-MELCHIORRI : Universita "La Sapienza", Roma, ITALY Jamila OUKBIR : Observatoire de Paris-Meudon, Meudon, FRANCE Georg RAFFELT : MPI fur Physik und Astrophysik, Munchen, GERMANY William T. REACH: University of California at Berkeley, Berkeley, USA Maria SAKELLARIADOU : Universite Libre de Bruxelles, Bruxelles, BELGIUM Pierre SALATI: LAPP, Annecy-le-Vieux, FRANCE Norma SANCHEZ: Observatoire de Paris-Meudon, Meudon, FRANCE Christoph SCHMID: ETH-Honggenberg, Zurich, SWITZERLAND Patrick SEGUIN: Ecole Normale Superieure, Paris, FRANCE Monique SIGNORE: Ecole Normale Superieure, Paris, FRANCE Joseph SILK: University of California at Berkeley, Berkeley, USA Haydeh SIROUSSE-ZIA : Institut Henri-Poincare, Paris, FRANCE George SMOOT: Lawrence Berkeley Laboratory, Berkeley, USA Francesco SYLOS-LABINI: Universita "La Sapienza", Roma, ITALY Luis Francisco TENORIO: Lawrence Berkeley Laboratory, Berkeley, USA Luigi TOFFOLA TTl : Universidad de Cantabrid, Santander, SPAIN Marie-Agnes TREYER : University of California at Berkeley, Berkeley, USA Michael TURNER: Fermi Laboratory, Batavia, USA Gabriele VENEZIANO: CERN, Geneve, SWITZERLAND Boqi WANG: University of California at Berkeley, Berkeley, USA David E. WILLMES : University of Florida, Gainsville, USA Edward L. WRIGHT: University of California at Los Angeles, Los Angeles, USA
LIST OF LECTURERS
Xavier BARCONS Departamento da Fisica Moderna, Universidad de Cantabria Avenida de Los Castros SIN, E-39005 Santander, SPAIN
Alain BLANCHARD DAEC, Observatoire de Paris-Meudon F-92195 Meudon principal Cedex, FRANCE
Franyois BOUCHET InStitut d'Astrophysique de Paris .98bis boulevard Arago, F-75014 Paris, FRANCE
F~ois BOULANGER Laboratoire de Radioastronomie Millimetrique, Ecole Normale Superieure 24 rue Lhomond, F-75231 Paris Cedex 05, FRANCE
Bernard CARR School of Mathematical Sciences, Queen Mary College Mile End Road, London El 4NS, UNITED KINGDOM
RolfCHINI Max-Planck Institut fUr Radioastronomie Auf dem HUgel 69, D-53oo Bonn 1, GERMANY
Paolo DE BERNARDIS Dipartimento di Fisica, Universita "La Sapienza" Piazzale Aldo Mom 2, 1-00185 Roma, ITALY
Pierre ENCRENAZ Laboratoire de Radioastronomie Millimetrique, Ecole Normale Superieure 24 rue Lhomond, F-75231 Paris Cedex 05, FRANCE
Krzysztof M. GORSKI Department of Astrophysical Sciences, Princeton University Peyton Hall, Princeton NJ 08544, USA
Michel GUELIN Institut de Radioastronomie Millimetrique, Domaine Universitaire 300 rue de la Piscine, F-38406 Saint-Martin-d'Heres Cedex, FRANCE
Michael A. JANSSEN Jet Propulsion Laboratory 4800 Oak Grove Drive, Pasadena CA 91109, USA
Roman JUSZKIEWICZ Nicolaus Copernicus Astronomical Center Bartycka 18,00-716 Warszawa, POLAND
Jean-Michel LAMARRE Institut d'Astrophysique Spatiale, Universite Paris-Sud B1itiment 120, F-91405 Orsay, FRANCE
Anthony LASENBY Mullard Radio Astronomy Observatory, Cavendish Laboratory Madingley Road, Cambridge CB3 OHE, UNITED KINGDOM
xi
xii
Vladimir LUKASH Space Research Institute, Academy of Sciences Profsojuznaja 84/32, 117810 Moscow, USSR
Enrique MARTINEZ-GONZALEZ Departamento da Fisica Moderna, Universidad de Cantabrili Avenida de Los Castros SIN, E-39005 Santander, SPAIN
Francesco MELClllORRI Dipartimento di Fisica, Universitli "La Sapienza" Piazzale Aldo Morn 2, 1-00185 Roma, ITALY
Georg RAFFELT Max-Planck Institut flir Physik und Astrophysik Postfach 401212,0-8000 Munchen, GERMANY
Pierre SALA TI Laboratoire d'Annecy-Ie-Vieux de Physique des Particules Chemin de Bellevue, BP 909, F-74029 Annecy-Ie-Vieux Cedex, FRANCE
Norma SANCHEZ DEMIRM, Observatoire de Paris-Meudon F-92195 Meudon principal Cedex, FRANCE
Joseph SILK Astronomy Department, University of California at Berkeley Berkeley CA 94720, USA
George SMOOT Lawrence Berkeley Laboratory MS 50--232, Berkeley CA 94720, USA
Michael TURNER Fermi Laboratory, MS 209 Box 500, Batavia IL 60510, USA
Gabriele VENEZIANO Theoretical Physics Division, CERN CH-1211 Geneve 23, SWITZERLAND
Edward L. WRIGHT Department of Astronomy, University of California at Los Angeles 405 Hilgard Avenue, Los Angeles CA 90024-1562, USA
PLATES OF COBE
PLATE 1. Artist's rendering of the Cosmic Background Explorer (COBE). The three panels of
solar cells are shown deployed from the body of the spacecraft. The white area houses the power systems, telemetry command and data handling, and the bulk of the altitude control system. The upper section is surrounded by the deployed ground shield/sun shade shown in cut away. The large white structure in the centre is the superfluid helium dewar, operating at 1.5 K and containing the FIRAS and DIRBE instruments. The DMR is made of the three radiometer pairs located around the dewar.
PLATE 2. eOBE DIRBE full sky maps in galactic coordinates. Upper portion is the combined
1.2, 2.2 and 3.4 micron maps shown in respective blue, green and red colors. The image shows both the thin disk and central bulge of the Milky Way. The lower portion shows the combined 25, 60 and 100 micron map in respective blue, green and red colors. Both maps are preliminary results of a full sky scan by the DIRBE instrument. The discontinuities apparent are due primarily to the change in zodiacal light, as the spacecraft and earth move around in the interplanetary dust but some part may be due to not having final instrument calibratiuon. The bright spots in the ecliptic are the moon and planets.
A)
PLATE 3. COBE FIRAS instrument maps of sky: A) dust (205 micron) ; B) [NIl] (205 mi
cron) ; C) [CII] (158 micron).
B)
PLATE 3. COBE FIRAS instrument maps of sky: A) dust (205 micron) ; B) [NIl] (205 mi
cron) ; C) [ell] (158 micron),
C)
PLATE 3. COBE FIRAS instrument maps of sky: A) dust (205 micron) ; B) [NIl] (205 mi
cron) ; C) [CII] (158 micron).
A) PLATE 4.
COBE DMR full sky maps ofthe temperature of the sky at 53 GHz (wavelength 5.7 mm). The maps are in galactic coordinates and have been corrected to solar system barycenter. A) Relative sky brightness with mean removed and scaled to about -4 to +4 mK. The dipole anisotropy (± 0.1 %) and the galactic plane are clearly visible. B) Relative sky brightness with monopole and dipole removed. The galactic plane emission is the only significant visible signal. The other structure evident is consistent with instrument observing noise.
PLATE 4. B)
COBE DMR full sky maps of the temperature of the sky at 53 GHz (wavelength 5.7 mm). The maps are in galactic coordinates and have been corrected to solar system barycenter. A) Relative sky brightness with mean removed and scaled to about -4 to +4 mK. The dipole anisotropy (± 0.1 %) and the galactic plane are clearly visible. B) Relative sky brightness with monopole and dipole removed. The galactic plane emission is the only significant visible signal. The other structure evident is consistent with instrument observing noise.
PLATE S. COBE DMR full sky maps of the relative temperature of the sky at frequencies 31.5,
53.0 and 90.0 GHz. The maps are in galactic coordinates and have been corrected to solar system barycenter. The maps show variations in received power and are insensitive to the mean temperature of about 2.735 K. Maps A and B correspond to two different channels at the three frequencies.
