PARTICLE DARK MATTER Observations, Models and...

PARTICLE DARK MATTERObservations, Models and Searches

Dark matter is among the most important open problems in modern physics.Aimed at graduate students and researchers, this book describes the theo-retical and experimental aspects of the dark matter problem in particlephysics, astrophysics and cosmology. Featuring contributions from 46 lead-ing theorists and experimentalists, it presents many aspects, from astrophys-ical observations to particle physics candidates, and from the prospects fordetection at colliders to direct and indirect searches.

The book introduces observational evidence for dark matter along with adetailed discussion of the state-of-the-art of numerical simulations and alter-native explanations in terms of modified gravity. It then moves on to the can-didates arising from theories beyond the Standard Model of particle physics,and to the prospects for detection at accelerators. It concludes by lookingat direct and indirect dark matter searches, and the prospects for detectingthe particle nature of dark matter with astrophysical experiments.

Gianfranco Bertone is Coordinator of the Theoretical Physics groupat the Institut d’Astrophysique de Paris, and Visiting Professor at theInstitute for Theoretical Physics, University of Zurich. His technical workmainly focuses on theoretical and phenomenological aspects of the dark mat-ter problem, and he participates in important experimental collaborationson the elaboration of optimal strategies for the detection of dark matterparticles.

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PARTICLE DARK MATTER

Observations, Models and Searches

Edited by

GIANFRANCO BERTONEInstitut d’Astrophysique de Paris






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ISBN 978-0-521-76368-4 (Hardback)1. Dark matter (Astronomy) 2. Mass (Physics) I. Bertone, Gianfranco, 1975–

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Contents

List of contributors page xiiPreface xviiAcknowledgements xxList of symbols and abbreviations xxi

Part I Dark matter in cosmology 1

1 Particle dark matter G. Bertone and J. Silk 31.1 Introduction 31.2 The baryon budget 41.3 The case for cold dark matter: good news and bad news 51.4 Portrait of a suspect 71.5 Observing cold dark matter 101.6 The future 12

2 Simulations of cold dark matter haloes B. Moore

and J. Diemand 142.1 From cold collapse to hierarchical clustering – a brief

history 142.2 Results from collisionless simulations 172.3 Predictions for direct and indirect detection experiments 34

3 Milky Way satellites J. Bullock, M. Kaplinghat

and L. Strigari 383.1 Satellite galaxies 383.2 Streams 463.3 Central profiles and the nature of dark matter 483.4 Indirect detection of dark matter from Milky Way

satellites 513.5 Future prospects 55

v






vi Contents

4 Gravitational lensing and dark matter Y. Mellier 564.1 Introduction 564.2 Gravitational lensing theory 574.3 Evidence for dark matter from strong lenses 634.4 Cold dark matter confronted to gravitational lenses 654.5 Hot dark matter: limits on neutrino masses from lensing 774.6 Dark matter or modified gravity? 784.7 Conclusion and outlook 80

5 Dark matter at the centres of galaxies D. Merritt 835.1 Phenomenology of galactic nuclei 835.2 Dark matter models 865.3 Dark matter in collisionless nuclei 885.4 Dark matter in collisional nuclei 925.5 The Galactic centre 945.6 Dwarf spheroidal galaxies 97

6 Modified gravity as an alternative to dark matterJ. D. Bekenstein 99

6.1 Missing mass in galaxies and clusters of galaxies 996.2 The MOND scheme 1026.3 Modified gravity theory for MOND 1056.4 TeVeS and other relativistic MOND theories 1096.5 Gravitational lenses and cosmology in TeVeS 112

Part II Candidates 119

7 DM production mechanisms G. Gelmini

and P. Gondolo 1217.1 Dark matter particles: relics from the pre-BBN era 1217.2 Thermal production in the standard cosmology 1237.3 Non-thermal production in the standard cosmology 1307.4 Thermal and non-thermal production in non-standard

cosmologies 133

8 Supersymmetric dark matter candidates J. Ellis

and K. A. Olive 1428.1 Motivations 1428.2 The MSSM and R-parity 1448.3 Possible supersymmetric dark matter candidates 1478.4 Renormalization-group equations and electroweak

symmetry breaking 1518.5 The CMSSM 153






Contents vii

8.6 mSUGRA 1598.7 Other possibilities 1618.8 Summary 162

9 Dark matter at the electroweak scale:non-supersymmetric candidates G. Servant 164

9.1 New symmetries at the TeV scale and dark matter 1669.2 Dark matter from extra dimensions: Kaluza–Klein DM 1679.3 Little Higgs dark matter 1829.4 Dark matter in technicolour and composite Higgs theories 1839.5 Mirror dark matter 1839.6 ‘Minimal’ approaches 1849.7 WIMPonium 1889.8 Connecting dark matter and the baryon asymmetry 1889.9 Conclusion 189

10 Non-WIMP candidates J. L. Feng 19010.1 Motivations 19010.2 SuperWIMP dark matter 19110.3 WIMPless dark matter 198

11 Axions P. Sikivie 20411.1 Introduction 20411.2 Axion production in the early Universe 20811.3 Relic density and primordial velocity dispersion 21911.4 Axion miniclusters 22211.5 Axion isocurvature perturbations 224

12 Sterile neutrinos M. Shaposhnikov 22812.1 Particle physics motivation 22812.2 Cosmological and astrophysical constraints on sterile

neutrino dark matter 23212.3 Sterile neutrino production in the early Universe 23912.4 Conclusions 247

Part III Collider searches 249

13 SUSY searches at the LHC T. Plehn and G. Polesello 25113.1 Discovery channels 25213.2 LHC measurements 25513.3 Parameter extraction 26413.4 Dark matter and the LHC 27413.5 Outlook 275






viii Contents

14 Supersymmetric dark matter at colliders M. Battaglia

and M.E. Peskin 27614.1 Introduction 27614.2 Questions for the collider experiments 27914.3 Dark matter at hadron colliders 28514.4 Dark matter at lepton colliders 29314.5 Collider measurements and astrophysical questions 303

15 Extra dimensions at the LHC K. Kong, K. Matchev

and G. Servant 30615.1 Flat extra dimensions (UED) 30615.2 Warped extra dimensions 31115.3 SUSY–UED discrimination at the LHC 317

16 SUSY tools F. Boudjema, J. Edsjo and P. Gondolo 32516.1 Annihilation cross-section and the relic density 32616.2 Direct detection 33116.3 Indirect detection 33416.4 Exploring the parameter space 33816.5 Interface with collider and precision

measurements codes 340

Part IV Direct detection 345

17 Direct detection of WIMPs D.G. Cerdeno

and A. M. Green 34717.1 Introduction 34717.2 Event rate 34717.3 Astrophysics input 35317.4 Signals 35617.5 Particle physics input 362

18 Annual modulation signature with large mass highlyradiopure NaI(Tl) R. Bernabei and P. Belli 370

18.1 The annual modulation signature and thetarget material 370

18.2 The DAMA/NaI and DAMA/LIBRA experiments 37318.3 The model-independent results 37418.4 The corollary quests for the candidate particle(s) 37918.5 Comparison with other activities 38018.6 Future perspectives 381






Contents ix

19 Particle dark matter and the DAMA/NaI and DAMA/LIBRA annual modulation effect N. Fornengo 383

19.1 The DAMA annual modulation effect 38319.2 Supersymmetric candidates 38619.3 Additional candidates 389

20 Cryogenic detectors G. Gerbier and J. Gascon 39120.1 Introduction 39120.2 Principles of operation of solid state cryogenic

detectors 39220.3 Single parameter detectors 39820.4 Ionization phonon bolometers 40120.5 Scintillation phonon bolometers 40420.6 MACHe3 40920.7 Prospects for 1 ton detectors 410

21 Liquid noble gases E. Aprile and L. Baudis 41321.1 Noble liquids for dark matter detection 41321.2 Two-phase XeTPCs: XENON, ZEPLIN and LUX 42021.3 Two-phase ArTPCs: WArP and ArDM 42821.4 Single-phase detectors: XMASS, DEAP/CLEAN 432

22 Directional detectors N. Spooner 43722.1 Direct dark matter detection technologies and directionality43722.2 The directional signature and statistics 43822.3 Directional detector concepts 44022.4 Gas detector physics – diffusion and straggling 44222.5 TPC gamma background rejection and energy

threshold 44722.6 TPC neutron background rejection, solar neutrinos

and radon 45022.7 Electronic noise and other background 45222.8 WIMP detection and directional sensitivity

in practice 45222.9 Head–tail recoil discrimination, theory and experiment 45622.10 Experimental status and readout technology 45722.11 Scale-up and a future WIMP telescope 463

23 Axion searches S. Asztalos 46723.1 Constraints on axion properties 46823.2 Conclusions 487






x Contents

Part V Indirect detection and astrophysical constraints 489

24 Gamma-rays L. Bergstrom and G. Bertone 49124.1 Annihilation 49124.2 Decaying dark matter 49624.3 Galactic centre 49724.4 Substructures 49924.5 The extragalactic signal 50424.6 Connection between antimatter and gamma-ray signal 505

25 High-energy neutrinos from WIMP annihilationsin the Sun F. Halzen and D. Hooper 507

25.1 Searching for dark matter with neutrinos 50725.2 The capture and annihilation of WIMPs in the Sun 50925.3 The neutrino spectrum 51125.4 Neutrino telescopes 51325.5 The case of neutralino dark matter 51625.6 The case of Kaluza–Klein dark matter 518

26 Indirect dark matter detection with cosmic antimatterP. Salati, F. Donato and N. Fornengo 521

26.1 Production of antimatter in the Galaxy 52126.2 Propagation of antinuclei in the Galaxy 52126.3 Antiprotons in cosmic rays 52426.4 Antideuterons in cosmic rays 53226.5 Positrons in cosmic rays 53726.6 Conclusions 546

27 Multi-wavelength studies S. Profumo and P. Ullio 54727.1 Introduction 54727.2 The multi-wavelength approach and galaxy clusters 55627.3 The multi-wavelength approach and dwarf galaxies 55927.4 The multi-wavelength approach and the Milky Way 56127.5 Radio observations 56327.6 Conclusions and overview 564

28 Particle dark matter and Big Bang nucleosynthesisK. Jedamzik and M. Pospelov 565

28.1 Introduction 56528.2 Standard BBN theory 56728.3 Observed light element abundances 56928.4 Cascade nucleosynthesis from energy injection 57328.5 Residual DM annihilation during BBN 576






Contents xi

28.6 Catalysed BBN (CBBN) 57928.7 DM production during BBN: NLSP→LSP example 583

29 Dark matter and stars G. Bertone 58629.1 DM capture and annihilation in stars 58729.2 The Earth and other planets 58929.3 Main-sequence stars 59129.4 Compact objects 59329.5 Pop III stars 599

References 602Index 736






Contributors

Elena Aprile1016 Pupin Hall/Nevis, MC 5231, Box 31, 538 W 120 St, New York, NY10027, USA

Stephen AsztalosLawrence Livermore National Laboratory, High Energy Physics and Accel-erator Technology Group, L-50 Livermore, CA 94551, USA

Marco BattagliaLawrence Berkeley National Laboratory, Physics Division, 1, Cyclotron Road,Mail Stop 50A2161, Berkeley, CA 94720-8143, USA

Laura BaudisUniversity of Zurich, Physik Institut, Winterthurerstrasse 190, CH-8057Zurich, Switzerland

Jacob BekensteinRacah Institute of Physics, The Hebrew University of Jerusalem, Givat Ram,Jerusalem 91904, Israel

Pierluigi BelliUniversita degli Studi di Roma ‘Tor Vergata’, Via della ricerca Scientifica1, 00133 Roma, Italy

Lars BergstromDepartment of Physics, Stockholm University, AlbaNova University Centre,S-106 91 Stockholm, Sweden

Rita BernabeiUniversita degli Studi di Roma ‘Tor Vergata’, Via della ricerca Scientifica1, 00133 Roma, Italy

xiii






xiv List of contributors

Gianfranco BertoneInstitut d’Astrophysique de Paris, 98 bis Bd Arago, 75014 Paris, France

Fawzi BoudjemaLAPTH CNRS, Chemin de Bellevue, F-74941 Annecy-le-Vieux, France

James BullockPhysics and Astronomy Department, 4168 Frederick Reines Hall, Universityof California, Irvine, CA 92697-4575, USA

David CerdenoDepartmento de Fısica Teorica, Universidad Autonoma de Madrid, ModuloC-Xl, 608, Cantoblanco, Madrid 28049, Spain

Juerg DiemandDepartment of Astronomy and Astrophysics, University of California, SantaCruz, CA 95064, USA

Fiorenza DonatoUniversity of Turin, via Giuria 1, 10125, Italy

Joakim EdsjoDepartment of Physics, AlbaNova, Stockholm University, SE-106 91 Stock-holm, Sweden

John EllisCERN, Theory Division, CH-1211 Geneva 23, Switzerland

Jonathan FengPhysics and Astronomy Department, 4168 Frederick Reines Hall, Universityof California, Irvine, CA 92697-4575, USA

Nicolao FornengoUniversity of Turin, via Giuria 1, 10125 Torino, Italy

Jules GasconInstitut de Physique Nucleaire, 4 rue Enrico Fermi, 69622 Villeurbannecedex, France

Graciela GelminiUCLA Physics and Astronomy, Box 951547, PAB 7-320, Los Angeles, CA90095-1547, USA






List of contributors xv

Gilles GerbierCentre d’Etudes de Saclay (CEA-Saclay), Orme des Merisiers, F-91191Gif-sur-Yvette Cedex, France

Paolo GondoloThe University of Utah, Department of Physics, 115 S 1400 E, Salt LakeCity, UT 84112-0830, USA

Anne GreenThe School of Physics and Astronomy, University of Nottingham, UniversityPark, Nottingham NG7 2RD, UK

Francis HalzenUniversity of Wisconsin-Madison, Department of Physics, PhenomenologyInstitute, 5293 Chamberlin Hall, Madison, Wisconsin, USA

Dan HooperWilson Hall 6 West, Fermilab, PO Box 500, Batavia, IL 60510, USA

Karsten JedamzikLaboratoire Physique Theorique & Astroparticules, Universite de Montpel-lier II, Place Eugene Bataillon, FR 34095 Montpellier Cedex 5, France

Manoj KaplinghatPhysics and Astronomy Department, 4168 Frederick Reines Hall, Universityof California, Irvine, CA 92697-4575, USA

Kyoungchul KongFermilab, Theory Department, PO Box 500 MS 106, Batavia, IL 60510, USA

Konstantin MatchevDepartment of Physics, University of Florida, PO Box 118440, Gainesville,FL 32611-8440, USA

Yannick MellierInstitut d’Astrophysique de Paris, 98 bis Bd Arago, 75014 Paris, France

David MerrittDepartment of Physics, 85 Lomb Memorial Drive, Rochester Institute ofTechnology, Rochester, NY 14623-5604, USA

Ben MooreInstitute for Theoretical Physics, University of Zurich, Winterthurerstrasse190, CH-8057 Zurich, Switzerland






xvi List of contributors

Keith OliveWilliam I. Fine Theoretical Physics Institute, School of Physics and Astron-omy, University of Minnesota, 116 Church Street SE, Minneapolis, MN55455, USA

Michael PeskinTheory Group, MS 81, SLAC, Stanford University, 2575 Sand Hill Road,Menlo Park, CA 94025, USA

Tilman PlehnInstitute for Theoretical Physics, Heidelberg University, Philosophenweg 16,69120 Heidelberg, Germany

Giacomo PoleselloINFN Sezione di Pavia, Via Bassi 6, 27100 Pavia, Italy

Maxim PospelovDepartment of Physics and Astronomy, University of Victoria, Victoria, BC,V8P 1A1, Canada

Stefano ProfumoDepartment of Physics, ISB 325, University of California, 1156 High Street,Santa Cruz, CA 95064, USA

Pierre SalatiLAPTH, 9 Chemin de Bellevue BP 110, 74941 Annecy le Vieux Cedex,France

Geraldine ServantCERN, Theory Division, CH-1211 Geneva 23, Switzerland

Mikhail ShaposhnikovEcole polytechnique federale de Lausanne, Institut de theorie des phenomenesphysiques, LPPC, BSP - Dorigny, CH-1015 Lausanne, Switzerland

Pierre SikiviePhysics Department, University of Florida, Gainesville, FL 32611, USA

Joseph SilkUniversity of Oxford, Department of Physics, Denys Wilkinson Building,Keble Road, Oxford, UK






List of contributors xvii

Neil SpoonerRoom E23, Hicks Building, Dept of Physics and Astronomy, University ofSheffield, Sheffield S3 7RH, UK

Louis StrigariKavli Institute (KIPAC), Physics Department, Stanford University, SLAC2575 Sand Hill Road, M/S 29, Menlo Park, CA 94025, USA

Piero UllioSISSA, via Beirut, 2–4, 34014 Trieste TS, Italy






Preface

Dark matter (DM) is one of the pillars of the Standard Cosmological Model,but the nature of this elusive component of the matter budget of the Universeremains unknown, despite the compelling evidence at all astrophysical scales.The possible connection with theories beyond the Standard Model of particlephysics makes DM one of the most important open problems in moderncosmology and particle physics, as witnessed by the enormous theoreticaland experimental effort that is being put towards its identification.

Many different strategies have been devised to achieve this goal. First,the Large Hadron Collider, which is just starting operations, is expectedto provide insights of paramount importance into possible extensions of theStandard Model of particle physics. Whether or not a specific candidateis “observed” at the LHC, any evidence for new physics (or lack thereof)will inevitably change our understanding of physics, and in particular ourunderstanding of DM. If DM candidates are actually found, the questionwill arise of whether they actually are the DM in the Universe.

A convincing identification can probably be obtained only by combiningthe results of accelerator searches with astrophysical searches, based on thedirect or indirect detection of DM particles in the local Universe. Direct DMsearches are based on the measurement of the recoil energy of nuclei struckby DM particles in large detectors. This field has evolved dramatically inthe past decade, and the different experimental strategies (cryogenic, liquidnoble gases, superheated) developed over the years have led to a spectacularimprovement of the constraints on DM–nucleon interactions. Alternatively,DM could be detected indirectly, through the detection of its annihilation ordecay products. With this aim, many important instruments are currentlytaking data, in particular in the energy range between 1 GeV and 1 TeV,like the antimatter satellite PAMELA and the gamma-ray satellite Fermi,launched in June 2008.

xviii






Preface xix

The material is arranged in five parts: Dark matter in cosmology; Candi-dates; Accelerator searches; Direct detection; Indirect detection and astro-physical constraints. The interested reader will find an introduction to theDM problem and a detailed overview of the contents of the book inChapter 1.

In brief, Part I is devoted to the astrophysical and cosmological aspects ofthe DM problem. The current understanding of the distribution of DM in theUniverse, based on numerical simulations and astrophysical observations, isreviewed here, along with the most recent lensing observations that providea ‘direct’ proof of the existence of DM, and a discussion of alternative the-ories that seek to dispense with DM. The chapters on DM distribution areparticularly important for the reader interested in the indirect DM searchesdiscussed in Part V.

The particle physics aspects of the DM problem are discussed in PartII. This part contains a discussion of the production mechanisms of DM inthe early Universe, including among others thermal production, relevant forthe broad class of candidates generically referred to as weakly interactingmassive particles (WIMPs). The most widely discussed extension of theStandard Model of particle physics, supersymmetry (SUSY), and the mostwidely discussed DM candidate, the neutralino, are also introduced here. Thediscussion is, however, enlarged to include a systematic review of alternativeextensions of the Standard Model, and alternative DM candidates, includingnon-SUSY WIMPs, and non-WIMP candidates.

Parts III, IV and V are dedicated to DM searches. Accelerator searches fornew physics are discussed in Part III. Of particular importance for the readerinterested in the DM problem are the chapters on strategies to discover andidentify extensions of the Standard Model of particle physics at the LHC,and on the techniques that may allow, in case of detection, the identificationof possible DM candidates. Part III also contains a chapter on DM ‘tools’,software that has been developed over the years by many different groups inan effort to allow systematic scans of the parameter space of new theories,along with the determination of physical quantities relevant for cosmologyand accelerator, direct and indirect searches in each of the models exploredin random scans.

Direct detection – the detection of DM through the measurement of therecoil energy of nuclei struck by DM in low-background detectors – is pre-sented in Part IV. The main avenues in this field of research, cryogenicdetectors and detectors using liquid noble gases, are presented here, alongwith a phenomenological overview and a discussion of ‘directional’ detectorscurrently under study.






xx Preface

Finally, Part V contains a discussion of the prospect for detecting DM‘indirectly’, that is, through the observation of the products of its annihi-lation or decay. This is a field that is witnessing an explosion of interest,owing to the new data of the Fermi and PAMELA satellites, and it is antici-pated that the excitement will remain high in the upcoming years, when anew generation of experiments will become available. A critical assessmentof the possible DM interpretation of existing data is presented in this lastpart of the book, along with a discussion of the strategies that may providethe long-awaited smoking-gun signature for DM.

This book aims at presenting in a coherent way the state-of-the-art of therelevant aspects of the disciplines involved in the DM problem (astrophysics,cosmology and particle physics), along with the detection strategies, in orderto build a common language among the different communities and, we hope,to prepare for the age of discoveries. It is more than a collection of reviewpapers, in the sense that particular care has been taken to ensure a coherentand complete presentation of the DM problem, and to bear in mind as itseventual readers graduate students and researchers who want to obtain abetter understanding of the many different aspects of the DM puzzle. The46 authors who joined the project met the challenge of summarizing inchapters of 15 to 20 pages an entire field of research, in an effort to be atthe same time accessible and complete. I thus believe that it can become atool to increase exchanges among the different communities involved in DMsearches, and to pave the road to a truly multidisciplinary approach to DM.

As is the case for all major endeavours, it is by no means certain thatthe search for DM will succeed. But this is how scientific research proceeds.If all our attempts fail, we will have to perform a radical revision of ourunderstanding of Nature. But if one or more of the strategies so far devisedturns out to be successful, the discovery of DM may well be remembered asone of the most exciting adventures in the history of science.






Acknowledgements

This book is the result of the collaborative effort of 46 authors. I am gratefulto all of them for the great quality of their contributions, and for keeping upwith the tight schedule I have imposed. I am indebted to Lars Bergstrom,Enzo Branchini, Marco Cirelli, Stephane Colombi, Gilles Esposito Farese,Nicolao Fornengo, Fabio Iocco, Yannick Mellier, Lidia Pieri, Pasquale Ser-pico, Volker Springel, Marco Taoso and Matteo Viel for reading parts ofthe book and providing very useful comments. It is a pleasure to thankSimon Capelin of Cambridge University Press, who solicited a book on darkmatter on the occasion of the PASCOS’08 conference at the Perimeter Insti-tute, and his assistant Laura Clark, who assisted me during the completionof this book. I also thank the Galileo Galilei Institute of Theoretical Physicsin Florence, where the final touches were put to this project. Finally, thanksto Nadia. She knows why.

xxi






Symbols and abbreviations

Symbols

Throughout the book, quantities describing the properties of DM particlesare denoted with the subscript χ, unless otherwise specified. Here are someof the most frequently used symbols:

mχ, mass of the DM particleσSI

p , spin-independent scattering cross-section off protonsσSI

n , spin-independent scattering cross-section off neutronsσSD

p , spin-dependent scattering cross-section off protonsσSD

n , spin-dependent scattering cross-section off neutrons〈σv〉, thermal average of the annihilation cross-section(σv), annihilation cross-section in the non-relativistic limitMGUT, Grand-unification scaleMPl, Planck scaleMSUSY, Supersymmetry scaleR0, Galactocentric radius of the Sunρcrit, critical density of the Universeρχ, DM densityρχ(R0) ≡ ρ0, DM density in the solar neighbourhoodΩχ, relic abundance of DM (in units of ρcrit)ΩM, relic abundance of matter (same units)Ωb, relic abundance of baryons (same units)ao, MOND parameterrvir, virial radiusMvir, virial masscvir, virial concentrationδvir, virial overdensity

xxii






List of symbols and abbreviations xxiii

Acronyms and abbreviations

AQUAL, Aquadratic Lagrangian (theory)BAO, Baryon Acoustic OscillationBBN, Big Bang NucleosynthesisBSM, (theories) Beyond the Standard ModelcMSSM, constrained MSSMCDM, Cold Dark MatterCMB, Cosmic Microwave BackgroundCrest, Collisionally Regenerated StructureDM, Dark MatterDSph, Dwarf Spheroidal GalaxyEM, ElectroweakFP, Fokker–Planck (equation)GEM, Gas Electron MultiplierGC, Galactic centreGR, General RelativityIDM, Inert Doublet ModelIMBH, Intermediate Mass Black HoleKK, Kaluza–KleinLHC, Large Hadron ColliderLMC, Large Magellanic CloudLSP, Lightest supersymmetric particleLKP, Lightest Kaluza–Klein particleLTP, Lightest T -odd ParticleLZP, Lightest Z3 ParticleLTR, Low-Temperature Reheating (models)MOND, Modified Newtonian DynamicsMSSM, Minimal Supersymmetric Standard ModelMW, Milky WayNFW, Navarro, Frenk and White (profile)NS, Neutron StarmSUGRA, Minimal SupergravityNTD, Neutron Transmutation Doped (germanium sensors)SD, Spin-Dependent (coupling)SDSS, Sloan Digital Sky SurveySI, Spin-Independent (coupling)SM, Standard ModelSMC, Small Magellanic CloudSMBH, Supermassive Black Hole






xxiv List of symbols and abbreviations

SNR, Signal-to-Noise RatioSQUID, Superconducting QUantum Interference DeviceSUSY, SupersymmetryTES, Transition Edge SensorsTeVeS, Tensor Vector Scalar theoryTPC, Time Projection ChamberUED, Universal Extra DimensionsWD, White DwarfWDM, Warm Dark MatterWIMP, Weakly Interacting Massive Particle






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