Particle Physics and Cosmology: The Interface NATO Science Series

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Series II: Mathematics, Physics and Chemistry – Vol. 188 Particle Physics and Cosmology: The Interface

edited by

D. Kazakov JINR, Dubna and ITEP, Moscow, Russia and G. Smadja Université Claude Bernard, Lyon 1, France

Published in cooperation with NATO Public Diplomacy Division Proceedings of the NATO Advanced Study Institute on Particle Physics and Cosmology: The Interface Cargèse, France 4– 16 August 2003

A C.I.P.Catalogue record for this book is available from the Library of Congress.

ISBN 1-4020-3160-2 (PB) ISBN 1-4020-3159-9 (HB) ISBN 1-4020-3161-0 (e-book)

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Printed in the Netherlands. Contents

Contributing Authors vii Foreword ix Preface xi Acknowledgments xii

ElectroWeak Symmetry Breaking as of 2003, on the way to the Large Hadron Collider 1 Riccardo Barbieri

Current Status of the CKM Matrix and the CP Violation 31 Achille Stocchi

Neutrino Masses 83 Stefan Pokorski

Neutrinos 111 Jacques Bouchez

Baryo- and Leptogenesis (outline) 171 Wilfried Buchm¨uller

Scalar Fields in Particle Physics in Cosmology 181 Pierre Binetruy

Inflation, Quantum Fluctuations and Cosmological Perturbations 235 David Langlois

Cosmic Microwave Background Cosmology; New Economy Model Universe 279 George F. Smoot

Cosmology with Supernovae 1a 311 Smadja G´erard

v vi PARTICLE PHYSICS AND COSMOLOGY: THE INTERFACE

Dark Matter and Galaxy Formation 329 Joseph Silk

Supersymmetric Extension of the Standard Model 349 Dimitri Kazakov

Gaugino Condensation and SUSY Breakdown 397 Hans Peter Nilles

Is Dark Matter Supersymmetric? 435 Wim de Boer

Cargese Lectures on Extra-Dimensions 461 Riccardo Rattazzi Contributing Authors

Riccardo Barbieri Professor at Scuole Normale Superiore, Pisa

Pierre Binetruy Professor at University Paris 11 and Paris 7

Jacques Bouchez Research staff at DAPNIA, CEN Saclay

Wilfried Buchmuller Professor at the University of Hamburg and DESY staff.

Wim De Boer Professor at the University of Karlsruhe

Dimitri Kazakov Research staff at JINR (Dubna) and ITEP (Moscow, Russia)

David Langlois Research staff at IAP (Paris)

Hans-Peter Nilles Professor at the university of Bonn

Stefan Pokorski Professor at the University of Warsaw

Riccardo Rattazzi Research staff at CERN (Geneva)

Joseph Silk Professor at the University of Oxford

Gerard Smadja Professor at the University Claude Bernard (Lyon 1)

George Smoot Professor at the University of California at Berkeley

Achille Stocchi Research staff at LAL-Orsay (CNRS)

vii Foreword

This Carg`ese school of Particle physics is meant to bridge the narrow- ing gap between astrophysical observations and particle physics. The lectures supply the students with a theoretical background which covers several aspects of the cosmological scenario: matter-antimatter asymme- try, the nature of dark matter, the acceleration of the expansion and the cosmological constant and the geometry of the universe as well as mod- ern views on particle physics including supersymmetry, extra dimensions scenarii and neutrino oscillations.

ix Preface

The investigation of nuclear abundances by Alpher, Bethe, and Gamow (1948) was the first intrusion of subatomic physics into cosmology. In contrast with their assumption, most nuclear species are now known to be produced in stars, but their bold step led to predictions which have largely been proven to be right: -a crude estimate of the densities during primordial nucleosynthesis -the presence of a residual 3K radiation today. the issues they addressed are still relevant. The origin of matter is not fully understood,and the CMB has grown into a powerful tool to inves- tigate the early eras of the universe. The progress of cosmological observations has now led to a ’standard’ slow-roll inflation model, which accounts quantitatively for many ob- served features of the universe. As the lectures will show, it still leaves large unchartered areas, and the underlying particle physics aspects are yettobeelucidated. At the same time despite the unprecedented success of the Stan- dard Model of fundamental interactions there are still remaining ”white spots”. Possible physics beyond the SM may have its manifestation in astrophysics and cosmology which may serve as a sky laboratory to reveal the new features of the microworld. The present volume contains the collection of lectures on the hottest topics in particle physics and cosmology given by the experts which describe the modern status and the perspectives of development of ex- perimental and theoretical activities in these fields.

xi Acknowledgments The school has been supported by the following institutions: NATO, CNRS (Formation permanente, IN2P3, INSU/PNC, Collectivit´e Territoriale Corse, DAPNIA/CEN-Saclay

We also want to acknowledge the major contribution of the IPNL staff who helped organize the school: M. Chartoire, M. Croiz´e, D. Jarroux- D´eclais, S. Flor`es, and Anne-Marie Ferrer, who took care of all finan- cial problems. At the Carg`ese Institute, Brigitte Cassegrain, Nathalie Bedjai, and Pierre Grossi were very helpful and ensured the smooth operation of the lectures and the distribution of the teaching material.

xii ELECTROWEAK SYMMETRY BREAKING AS OF 2003, ON THE WAY TO THE LARGE HADRON COLLIDER∗

Riccardo Barbieri Scuola Normale Superiore and INFN, Pisa, Italy [email protected]

Abstract I review the status of the ElectroWeak Symmetry Breaking problem. The lectures are naturally divided into two parts. The first is mostly de- voted to overview the impact of current data on the issue of EWSB. The tools are known, the latest data are included. Always in the first part, I say why I care about the ”little hierarchy” problem and I summarize how some proposals for EWSB, recent and less recent, are confronted with this problem. Motivated by these considerations, in the second part I describe the essential features of a proposal for breaking super- symmetry, and consequently the electroweak symmetry, by boundary conditions on an extra dimension.

Keywords: Electroweak, Symmetry, Breaking, Higgs mass, Supersymmetry, Kaluza- Klein, MSSM

The data (their interpretation) summarized There are several good reasons for being interested in the problem of how the electroweak symmetry gets broken. Above all, the physical origin of the Fermi scale has not been identified, yet. Consequently, and not less importantly, this ignorance acts as a cloud on every attempt to design a theory of the fundamental interactions beyond the Standard Model (SM). Last, but not least, the exploration of the TeV scale of energy expected at the Large Hadron Collider (LHC) should finally allow

∗Lectures given at the Cargese School of Physics and Cosmology - August 2003 - Cargese - France

1

D. Kazakov and G. Smadja (eds.), Particle Physics and Cosmology: The Interface, 1–29. © 2005 Springer. Printed in the Netherlands. 2 PARTICLE PHYSICS AND COSMOLOGY: THE INTERFACE a direct comparison with experiment of every theoretical idea on this matter. These are not the first lectures on the subject of ElectroWeak Sym- metry Breaking (EWSB). Nevertheless, I find that it may be useful to overview the present status of the subject when we still have a few years before the start of the LHC and when the program of the ElectroWeak Precision Tests (EWPT), in particular with the completion of most of the data analyses by the LEP experiments, is in a mature stage. The EWPT are still the most important source of experimental in- formation, although indirect, on EWSB. It so happens that I already lectured in Cargese on the EWPT in 1992, when the accumulation of significant experimental results on the EWPT was about to start and the top quark had not yet been discovered. At that time the bulk of the radiative effects seen in the data was still of electromagnetic origin. Now we know that several per-mil effects of pure electroweak nature are crucial in allowing an effective description of the data and that these effects are contained in the SM. Things might have gone differently. What is it then that we learn on the EWSB problem? Among the conclusions of my 92 lectures, I argued that the program of the EWPT should have made possible to discriminate between a perturbative and a strongly interacting picture of EWSB, the prototype examples for the two cases being respectively supersymmetry and technicolor. It is now pretty clear that the data support a perturbative more than a non per- turbative description of EWSB, as illustrated more precisely later on. Inside this framework, a relevant piece of information, also coming from the EWPT is the indication for a light Higgs, most likely lighter than about 200 GeV. All this seems in fact to make a rather coherent picture of EWSB, and maybe it does. I will argue, however, that the direct lower limit on the Higgs mass, mH > 115 GeV [1], and the absence so far on any deviation from the expectations of the SM may also require some interpretation with a possible impact on the picture of EWSB. The lectures are naturally divided into two parts, to be found in Sec- tions 2 and 3 respectively. The first is mostly devoted to overview the impact of current data on the issue of EWSB. The tools are known, the latest data are included. Always in the first part, I will illustrate why I care about the ”little hierarchy” problem and I will summarize how some proposals for EWSB, recent and less recent, are confronted with this problem. Motivated by these considerations, in the second part I will describe the essential features of a proposal for breaking su- persymmetry, and consequently the electroweak symmetry, by boundary conditions on an extra dimension. In Section 4 I summarize the line of reasoning that motivates mostly these lectures and I conclude. ElectroWeak Symmetry Breaking as of 2003 3 1. Un updated overview 1.1 The data (their interpretation) summarized Experiment versus theory with generic ”oblique” corrections. I begin by referring to the data on the EWPT from the LEP, TEVA- TRON and SLC experiments, as summarized by the LEP ElectroWeak Working Group in the summer of 2003 [2]. These data allow a stringent test of the SM, sensitive to the radiative corrections of electroweak na- ture. The test is successful, with no serious reason of concern, in my view, for those measurements that appear in some tension with the SM prediction. The EWSB sector of the SM has some impact on this test. For this very reason, taking into account that this is the physics whose nature we are wondering about, one has advocated since the beginning of the experimental program an analysis valid in a broader class of theories. Such are those theories that differ from the SM only in the so called ”oblique” corrections [3], i.e. those corrections that come from vacuum polarization amplitudes of the vector bosons. To this purpose one has de- fined three dimensionless experimental quantities, i,i=1, 2, 3, [4] with the property that they encapsulate, among other effects, the ”oblique” corrections. Furthermore, since one of them, 2, is unlikely to contain new physics, one often freezes it to its SM value 1.Fig.1showsthe determination of the two remaining parameters, 1 and 3, with their correlation, as obtained from the set of data mentioned above. In the same Figure, the SM prediction is indicated for different values of the Higgs mass. The ”oblique” contributions to 1 and 3 can be expressed in terms of the transverse components of the usual vacuum polarization amplitudes 2 Πa,b(q ), with a, b =1, 2, 3 for the SU(2) or a, b = B for the U(1) gauge bosons, as Π33(0) − Π11(0) ∆1 = 2 , (1) MW g ∆ = Π (0), (2) 3 g 3B where g and g are the SU(2) and U(1) gauge couplings. The data speak by themselves. The agreement with the SM is remark- able and constitutes indirect evidence for the existence of the Higgs. It has even become difficult, if not impossible at all, to try to reconcile

1 The slight dependence of 2 on mH is practically irrelevant. Here 2 is taken at mH = 115 GeV .