Dark Matter II. Marco Cirelli. (CNRS IPhT Saclay) December th TRR Winter School - Passo del Tonale. Reviews on Dark Matter: NewDark
|
|
|
- Caroline Lester
- 6 years ago
- Views:
Transcription
1 10-14 December th TRR Winter School - Passo del Tonale Dark Matter II Marco Cirelli (CNRS IPhT Saclay) in collaboration with: A.Strumia (Pisa) N.Fornengo (Torino) M.Tamburini (Pisa) R.Franceschini (Pisa) M.Raidal (Tallin) M.Kadastik (Tallin) Gf.Bertone (IAP Paris) M.Taoso (Padova) C.Bräuninger (Saclay) P.Panci (L Aquila + Saclay + CERN) F.Iocco (Saclay + IAP Paris) P.Serpico (CERN) NewDark Reviews on Dark Matter: Jungman, Kamionkowski, Griest, Phys.Rept. 267, , 1996 Bertone, Hooper, Silk, Phys.Rept. 405, , 2005 Einasto, Bergstrom , Cirelli, Strumia arxiv: yymm.nnnn (upcoming)
2 How was Dark Matter produced?
3 Contents 1. Introduction and 'cosmology' - basic properties of - evidences -- galactic rotation curves -- weak lensing [qualitative idea] -- 'precision cosmology' [qualitative] - alternatives (Machos, MOND) - production -- freeze-out & the WIMP miracle -- asymmetric - particle physics candidates 2. Indirect Detection - basics - observables -- charged particle fluxes: production & propagation -- gamma rays: production & propagation -- neutrinos: production & propagation - current status: hints, constraints 3. Direct Detection - basics - observables (recoil spectrum, detection strategies) - current status: hints, constraints 4. Collider Searches - basics - observables (missing energy, monojets) - complementarity
4 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance
5 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance Kolb,Turner, The Early Universe, 1995
6 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance f f Kolb,Turner, The Early Universe, 1995
7 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance f f f f Kolb,Turner, The Early Universe, 1995
8 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance f f f f... Kolb,Turner, The Early Universe, 1995
9 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt cosmology particle physics
10 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) H freeze-out
11 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N tot freeze-out
12 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 rad = 2 30 g T 4 g = X bos g i Ti T X fer g i Ti T 4
13 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g M Pl T 2 f.o. ann
14 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g Tf.o. 2 Define Y X = n X M Pl ann s s = g st 3
15 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = n X ' ann H = r g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r g T 2 Define Y X = n X M Pl ann s q g g s M Pl 1 ann T f.o.
16 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q g g s 1 = M Pl ann T f.o. M Pl ann T f.o. M Pl T f.o. m X /20 g ' g s ' 100 # ann m X
17 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = n X ' ann H = r g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r g T 2 Define Y X = n X M Pl ann s q g g s X = X crit = m Xn X crit 1 = M Pl ann T f.o. M Pl ann T f.o. = m XY today s today crit M Pl = m X # ann m X M Pl # ann m X s today crit
18 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = n X ' ann H = r g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r g T 2 Define Y X = n X M Pl ann s q g g s X = X crit = m Xn X crit 1 = M Pl ann T f.o. M Pl ann T f.o. = m XY today s today crit M Pl = m X # ann m X M Pl # m X cancels out ann m X s today crit
19 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q g g s 1 = M Pl ann T f.o. M Pl ann T f.o. M Pl # ann m X X ' 0.2 pb ann
20 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q g g s 1 = M Pl ann T f.o. M Pl ann T f.o. M Pl # ann m X X ' 0.2 pb ann or Ω X cm 3 s 1 σ ann v
21 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X cm 3 s 1 σ ann v Relic 0.23 for ann v = cm 3 /sec
22 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X cm 3 s 1 σ ann v Relic 0.23 for ann v = cm 3 /sec Weak cross section: g w g w f M f
23 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X cm 3 s 1 σ ann v Relic 0.23 for ann v = cm 3 /sec Weak cross section: g w g w f M f h ann vi (g2 w/4 ) 2 M cm 3 /sec WIMP miracle!
24 Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism:
25 Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism: Baryogenesis: B = n B n n B Darko genesis: = = n n n BBN, CMB...? = B B / m B B / m
26 Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism: Baryogenesis: B = n B n n B Darko genesis: = = n n n BBN, CMB...? = B B / m B B / m m ' 5 GeV Is this the of DAMA, CoGeNT, CRESST?!?
27 Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism: Baryogenesis: B = n B n n B Darko genesis: = = n n n BBN, CMB...? = B A variety of specific models/ideas: transferring or co-genesis cfr J. March-Russell via leptogenesis stores the anti-b number connection to neutrino masses
28 Asymmetric : a completely different relic Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - Asymmetric abundance - large annihilation cross sec Comoving density Y x f f! f f? Y Y x m T Y pb m 4.5 GeV density Y x Y Y no osc pb m 1000 GeV m 10 4 ev 2
29 Asymmetric : a completely different relic Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - Asymmetric abundance - large annihilation cross sec Comoving density Y x f f! f f? Y Y x m T Y pb m 4.5 GeV density Y x Y Y no osc pb m 1000 GeV m 10 4 ev 2
30 Asymmetric : a completely different relic Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - Asymmetric abundance - large annihilation cross sec Comoving density Y x f f! f f? Y Y x m T Y pb m 4.5 GeV density Y x Y Y no osc pb m 1000 GeV m 10 4 ev 2
31 Asymmetric : a completely different relic Consider a particle χ: X ' m X s crit 0!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - Asymmetric abundance - large annihilation cross sec Comoving density Y x density Y x f f! f f? Y Y Y Y x m T no osc Y pb m 4.5 GeV m 25 pb m 1000 X GeV m 10 4 ev The relic abundance is determined by and. 0 2
32 Particle Physics candidates for Dark Matter
33 Contents 1. Introduction and 'cosmology' - basic properties of - evidences -- galactic rotation curves -- weak lensing [qualitative idea] -- 'precision cosmology' [qualitative] - alternatives (Machos, MOND) - production -- freeze-out & the WIMP miracle -- asymmetric - particle physics candidates 2. Indirect Detection - basics - observables -- charged particle fluxes: production & propagation -- gamma rays: production & propagation -- neutrinos: production & propagation - current status: hints, constraints 3. Direct Detection - basics - observables (recoil spectrum, detection strategies) - current status: hints, constraints 4. Collider Searches - basics - observables (missing energy, monojets) - complementarity
34 Candidates A matter of perspective:
35 Candidates A matter of perspective: SuSy Non SuSy
36 Candidates A matter of perspective: SuSy Non SuSy?
37 Candidates A matter of perspective: SuSy neutralino other exotic candidates
38 SuSy in 2 minutes h
39 SuSy in 2 minutes h m h ' 125 GeV
40 SuSy in 2 minutes h m h ' 125 GeV h t h m h GeV
41 SuSy in 2 minutes ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ h h2 h1 ~ h2 ~ m h ' 125 GeV h t h m h GeV h ~t h m h GeV
42 SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ h1 ~ h2 ~ m h ' 125 GeV h t h m h GeV h ~t h m h GeV
43 SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 h1 ~ h2 ~ m h ' 125 GeV R = 1 h t h m h GeV h ~t h m h GeV
44 SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 h1 ~ h2 ~ m h ' 125 GeV R = 1 h t h m h GeV h ~t h m h GeV
45 SuSy in 2 minutes 2 TeV ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 ~ ~ ~ ~ m h ' 125 GeV R = 1 h1 ~ h2 ~ h t h m h GeV h ~t h m h GeV
46 Candidates A matter of perspective: SuSy neutralino other exotic candidates
47 Candidates A matter of perspective: SuSy neutralino
48 Candidates A matter of perspective: SuSy neutralino
49 Candidates A matter of perspective: SuSy neutralino SuSy e.g. RH sneutrino
50 Candidates A matter of perspective: SuSy neutralino SuSy Weak e.g. RH sneutrino WIMP
51 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV e.g. RH sneutrino WIMP TC some KK
52 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle e.g. RH sneutrino WIMP TC some KK
53 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK
54 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK gravitino?
55 Candidates A matter of perspective: SuSy neutralino SuSy gravitino? e.g. RH sneutrino Weak WIMP TeV particle sub-gev axion TC some KK
56 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP gravitino? axion TC some KK
57 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
58 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
59 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
60 Candidates A matter of perspective: Caveat: no categorization is perfect.
61 Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: em weak strong-ish other none (other than gravity)
62 Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: em weak strong-ish other none (other than gravity)
63 Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: em weak strong-ish neutralino etc Little Higgs KK Inert Doublet Minimal TC mirror } a other none (other than gravity) secluded WIMPless singlet scalar sterile neutrino gravitino axion
64 Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: naturalness-inspired em weak strong-ish neutralino etc Little Higgs KK Inert Doublet Minimal TC mirror } a other none (other than gravity) secluded WIMPless singlet scalar sterile neutrino gravitino axion
65 Candidates A matter of perspective: Interactions: em weak strong-ish naturalness-inspired neutralino etc Little Higgs KK Inert Doublet Minimal TC mirror } a Caveat: no categorization is perfect. Production mechanism? thermal freeze out thermal freeze out thermal freeze out thermal freeze out thermal freeze out exhaustion Stability? R parity T parity K parity Z2 symmetry gauge sym Tbaryon # Z2 symmetry other secluded WIMPless sort of freeze out sort of freeze out some symmetry some symmetry singlet scalar thermal freeze out Z2 symmetry none (other than gravity) sterile neutrino gravitino mixing thermal or decay just long lived R parity or just long lived axion misalignment? just long lived
66 Candidates A matter of perspective: plausible mass ranges (1 TeV) ev
67 Candidates A matter of perspective: plausible mass ranges only 90 orders of magnitude!
68 How do we search for Dark Matter?
Dark Matter. Marco Cirelli. (CNRS IPhT Saclay) December th TRR Winter School - Passo del Tonale. Reviews on Dark Matter: NewDark
10-14 December 2012 6 th TRR Winter School - Passo del Tonale Dark Matter Marco Cirelli (CNRS IPhT Saclay) in collaboration with: A.Strumia (Pisa) N.Fornengo (Torino) M.Tamburini (Pisa) R.Franceschini
DARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1
DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark
Relating the Baryon Asymmetry to WIMP Miracle Dark Matter
Brussels 20/4/12 Relating the Baryon Asymmetry to WIMP Miracle Dark Matter PRD 84 (2011) 103514 (arxiv:1108.4653) + PRD 83 (2011) 083509 (arxiv:1009.3227) John McDonald, LMS Consortium for Fundamental
WIMPs and superwimps. Jonathan Feng UC Irvine. MIT Particle Theory Seminar 17 March 2003
WIMPs and superwimps Jonathan Feng UC Irvine MIT Particle Theory Seminar 17 March 2003 Dark Matter The dawn (mid-morning?) of precision cosmology: Ω DM = 0.23 ± 0.04 Ω total = 1.02 ± 0.02 Ω baryon = 0.044
MICROPHYSICS AND THE DARK UNIVERSE
MICROPHYSICS AND THE DARK UNIVERSE Jonathan Feng University of California, Irvine CAP Congress 20 June 2007 20 June 07 Feng 1 WHAT IS THE UNIVERSE MADE OF? Recently there have been remarkable advances
Overview of Dark Matter models. Kai Schmidt-Hoberg
Overview of Dark Matter models. Kai Schmidt-Hoberg Evidence for dark matter. Compelling evidence for dark matter on all astrophysical scales: Galactic scales: Rotation curves of Galaxies Kai Schmidt-Hoberg
IMPLICATIONS OF PARTICLE PHYSICS FOR COSMOLOGY
IMPLICATIONS OF PARTICLE PHYSICS FOR COSMOLOGY Jonathan Feng University of California, Irvine 28-29 July 2005 PiTP, IAS, Princeton 28-29 July 05 Feng 1 Graphic: N. Graf OVERVIEW This Program anticipates
Project Paper May 13, A Selection of Dark Matter Candidates
A688R Holly Sheets Project Paper May 13, 2008 A Selection of Dark Matter Candidates Dark matter was first introduced as a solution to the unexpected shape of our galactic rotation curve; instead of showing
Dark Matter in Particle Physics
High Energy Theory Group, Northwestern University July, 2006 Outline Framework - General Relativity and Particle Physics Observed Universe and Inference Dark Energy, (DM) DM DM Direct Detection DM at Colliders
Kaluza-Klein Theories - basic idea. Fig. from B. Greene, 00
Kaluza-Klein Theories - basic idea Fig. from B. Greene, 00 Kaluza-Klein Theories - basic idea mued mass spectrum Figure 3.2: (Taken from [46]). The full spectrum of the UED model at the first KK level,
M. Lattanzi. 12 th Marcel Grossmann Meeting Paris, 17 July 2009
M. Lattanzi ICRA and Dip. di Fisica - Università di Roma La Sapienza In collaboration with L. Pieri (IAP, Paris) and J. Silk (Oxford) Based on ML, Silk, PRD 79, 083523 (2009) and Pieri, ML, Silk, MNRAS
Constraining minimal U(1) B L model from dark matter observations
Constraining minimal U(1) B L model from dark matter observations Tanushree Basak Physical Research Laboratory, India 10th PATRAS Workshop on Axions, WIMPs and WISPs CERN Geneva, Switzerland July 3, 2014
Making Dark Matter. Manuel Drees. Bonn University & Bethe Center for Theoretical Physics. Making Dark Matter p. 1/35
Making Dark Matter Manuel Drees Bonn University & Bethe Center for Theoretical Physics Making Dark Matter p. 1/35 Contents 1 Introduction: The need for DM Making Dark Matter p. 2/35 Contents 1 Introduction:
Particle Cosmology. V.A. Rubakov. Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University
Particle Cosmology V.A. Rubakov Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University Topics Basics of Hot Big Bang cosmology Dark matter: WIMPs Axions Warm
DARK MATTER MEETS THE SUSY FLAVOR PROBLEM
DARK MATTER MEETS THE SUSY FLAVOR PROBLEM Work with Manoj Kaplinghat, Jason Kumar, John Learned, Arvind Rajaraman, Louie Strigari, Fumihiro Takayama, Huitzu Tu, Haibo Yu Jonathan Feng University of California,
The Story of Wino Dark matter
The Story of Wino Dark matter Varun Vaidya Dept. of Physics, CMU DIS 2015 Based on the work with M. Baumgart and I. Rothstein, 1409.4415 (PRL) & 1412.8698 (JHEP) Evidence for dark matter Rotation curves
Dark Matter from Non-Standard Cosmology
Dark Matter from Non-Standard Cosmology Bhaskar Dutta Texas A&M University Miami 2016 December 16, 2016 1 Some Outstanding Issues Questions 1. Dark Matter content ( is 27%) 2. Electroweak Scale 3. Baryon
Asymmetric WIMP DM. Luca Vecchi. Aspen (CO) 2/2011. in collaboration with Michael Graesser and Ian Shoemaker (LANL)
Asymmetric WIMP DM Luca Vecchi in collaboration with Michael Graesser and Ian Shoemaker (LANL) Aspen (CO) 2/2011 Outline 1 Motivations 2 The relic abundance of asymmetric species 3 Asymmetric WIMP Dark
Baryon-Dark Matter Coincidence. Bhaskar Dutta. Texas A&M University
Baryon-Dark Matter Coincidence Bhaskar Dutta Texas A&M University Based on work in Collaboration with Rouzbeh Allahverdi and Kuver Sinha Phys.Rev. D83 (2011) 083502, Phys.Rev. D82 (2010) 035004 Miami 2011
Week 3 - Part 2 Recombination and Dark Matter. Joel Primack
Astro/Phys 224 Spring 2012 Origin and Evolution of the Universe Week 3 - Part 2 Recombination and Dark Matter Joel Primack University of California, Santa Cruz http://pdg.lbl.gov/ In addition to the textbooks
Dark Matter and Dark Energy components chapter 7
Dark Matter and Dark Energy components chapter 7 Lecture 3 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,
Non-Thermal Dark Matter from Moduli Decay. Bhaskar Dutta. Texas A&M University
Non-Thermal Dark Matter rom Moduli Decay Bhaskar Dutta Texas A&M University Allahverdi, Dutta, Sinha, PRD87 (2013) 075024, PRDD86 (2012) 095016, PRD83 (2011) 083502, PRD82 (2010) 035004 Allahverdi, Dutta,
Cosmology/DM - I. Konstantin Matchev
Cosmology/DM - I Konstantin Matchev What Do We Do? Trying to answer the really big questions: 1. What is the Universe made of?... 5. Can the laws of Physics be unified? 16. What is the cause of the terrible
Asymmetric Sneutrino Dark Matter
Asymmetric Sneutrino Dark Matter Stephen West Oxford University Asymmetric Sneutrino Dark Matter and the Ω b /Ω dm Puzzle; hep-ph/0410114, PLB, Dan Hooper, John March- Russell, and SW from earlier work,
INTRODUCTION TO DARK MATTER
Universität Heidelberg Carl Zeiss Stiftung INTRODUCTION TO DARK MATTER Susanne Westhoff 2nd Colima Winter School on High Energy hysics! January 8-19, 2018 Colima, Mexico GALAXY VELOCITIES IN CLUSTERS Redshift
Thermal Dark Matter Below an MeV
Thermal Dark Matter Below an MeV ASHER BERLIN TeVPA, Ohio State University August 9, 2017 Collaboration with Nikita Blinov, arxiv: 1706.07046 Dark Matter Mass dwarf galaxies MACHO 10-31 GeV 10 58 GeV Dark
Big-Bang nucleosynthesis, early Universe and relic particles. Alexandre Arbey. Moriond Cosmology La Thuile, Italy March 23rd, 2018
Big-Bang nucleosynthesis, early Universe and relic particles Alexandre Arbey Lyon U. & CERN TH Moriond Cosmology 2018 La Thuile, Italy March 23rd, 2018 Introduction Alexandre Arbey Moriond Cosmology 2018
New Physics beyond the Standard Model: from the Earth to the Sky
New Physics beyond the Standard Model: from the Earth to the Sky Shufang Su U. of Arizona Copyright S. Su CERN (Photo courtesy of Maruša Bradač.) APS4CS Oct 24, 2009 Let s start with the smallest scale:
Supersymmetric dark matter with low reheating temperature of the Universe
Supersymmetric dark matter with low reheating temperature of the Universe Sebastian Trojanowski National Center for Nuclear Research, Warsaw COSMO 204 Chicago, August 29, 204 L. Roszkowski, ST, K. Turzyński
Learning from WIMPs. Manuel Drees. Bonn University. Learning from WIMPs p. 1/29
Learning from WIMPs Manuel Drees Bonn University Learning from WIMPs p. 1/29 Contents 1 Introduction Learning from WIMPs p. 2/29 Contents 1 Introduction 2 Learning about the early Universe Learning from
Introduction Motivation WIMP models. WIMP models. Sebastian Belkner. University of Bonn - University of Cologne. June 24, 2016
WIMP models Sebastian Belkner University of Bonn - University of Cologne June 24, 2016 1 / 27 A brief history of the universe 2 / 27 Outline 1 Motivation On galactic scales On cosmological scales 2 WIMP
Thermal decoupling of WIMPs
PPC 2010, Torino, 12-15 July 2010 A link between particle physics properties and the small-scale structure of (dark) matter Outlook Chemical vs kinetic decoupling of WIMPs Kinetic decoupling from first
Dark Matter Decay and Cosmic Rays
Dark Matter Decay and Cosmic Rays Christoph Weniger Deutsches Elektronen Synchrotron DESY in collaboration with A. Ibarra, A. Ringwald and D. Tran see arxiv:0903.3625 (accepted by JCAP) and arxiv:0906.1571
November 24, Scalar Dark Matter from Grand Unified Theories. T. Daniel Brennan. Standard Model. Dark Matter. GUTs. Babu- Mohapatra Model
Scalar from November 24, 2014 1 2 3 4 5 What is the? Gauge theory that explains strong weak, and electromagnetic forces SU(3) C SU(2) W U(1) Y Each generation (3) has 2 quark flavors (each comes in one
The Four Basic Ways of Creating Dark Matter Through a Portal
The Four Basic Ways of Creating Dark Matter Through a Portal DISCRETE 2012: Third Symposium on Prospects in the Physics of Discrete Symmetries December 4th 2012, Lisboa Based on arxiv:1112.0493, with Thomas
The WIMPless Miracle and the DAMA Puzzle
The WIMPless Miracle and the DAMA Puzzle Jason Kumar University of Hawaii w/ Jonathan Feng, John Learned and Louis Strigari (0803.4196,0806.3746,0808.4151) Relic Density matter in early universe in thermal
SUPERSYMETRY FOR ASTROPHYSICISTS
Dark Matter: From the Cosmos to the Laboratory SUPERSYMETRY FOR ASTROPHYSICISTS Jonathan Feng University of California, Irvine 29 Jul 1 Aug 2007 SLAC Summer Institute 30 Jul 1 Aug 07 Feng 1 Graphic: N.
SUSY AND COSMOLOGY. Jonathan Feng UC Irvine. SLAC Summer Institute 5-6 August 2003
SUSY AND COSMOLOGY Jonathan Feng UC Irvine SLAC Summer Institute 5-6 August 2003 Target Audience From the organizers: graduate students, junior postdocs ¾ experimentalists, ¼ theorists Students enjoy the
Astroparticle Physics at Colliders
Astroparticle Physics at Colliders Manuel Drees Bonn University Astroparticle Physics p. 1/29 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/29 Contents 1) Introduction:
Dark Matter Models. Stephen West. and. Fellow\Lecturer. RHUL and RAL
Dark Matter Models Stephen West and Fellow\Lecturer RHUL and RAL Introduction Research Interests Important Experiments Dark Matter - explaining PAMELA and ATIC Some models to explain data Freeze out Sommerfeld
DM Signatures generated by anomalies in hidden sectors
DM Signatures generated by anomalies in hidden sectors ann Mambrini Laboratoire de Physique Théorique Orsay, Université Paris I E. Dudas, S. Pokorski,, A. Romagnoni GGI, Florence,, May 20 th 2010 Where
Chern-Simons portal Dark Matter
Chern-Simons portal Dark Matter III Saha Theory Workshop: Aspects of Early Universe Cosmology Mathias Pierre Laboratoire de Physique Théorique d Orsay In collaboration with G. Arcadi, G.Bhattacharyya,
Wino dark matter breaks the siege
Wino dark matter breaks the siege Shigeki Matsumoto (Kavli IPMU) In collaboration with M. Ibe, K. Ichikawa, and T. Morishita 1. Wino dark matter (Motivation & Present limits) 2. Wino dark matter is really
Beyond the WIMP Alternative dark matter candidates. Riccardo Catena. Chalmers University
Beyond the WIMP Alternative dark matter candidates Riccardo Catena Chalmers University April 3, 2017 Outline WIMPs and the thermal production mechanism Generalized WIMPs Other candidates / production mechanisms
arxiv: v2 [hep-ph] 19 Nov 2013
![arxiv: v2 [hep-ph] 19 Nov 2013](/thumbs/86/93477012.jpg "arxiv: v2 [hep-ph] 19 Nov 2013")
Asymmetric Dark Matter: Theories, Signatures, and Constraints Kathryn M. Zurek 1 1 Michigan Center for Theoretical Physics, Department of Physics, University of Michigan, Ann Arbor, Michigan 48109 USA
Dark-matter bound states
Dark-matter bound states Kallia Petraki Université Pierre et Marie Curie, LPTHE, Paris Recontres du Vietnam, Quy Nhon 27 July 2017 Long-range interactions mediated by massless or light particles Bound
Models of New Physics for Dark Matter
Models of New Physics for Dark Matter Carlos Muñoz instituto de física teórica ift-uam/csic departamento de física teórica dft-uam 1 PPC 2010, Torino, July 12-16 Crucial Moment for SUSY in next few years:
Supersymmetry in Cosmology
Supersymmetry in Cosmology Raghavan Rangarajan Ahmedabad University raghavan@ahduni.edu.in OUTLINE THE GRAVITINO PROBLEM SUSY FLAT DIRECTIONS AND THEIR COSMOLOGIAL IMPLICATIONS SUSY DARK MATTER SUMMARY
Symmetric WIMP Dark Matter and Baryogenesis
Symmetric WIMP Dark Matter and Baryogenesis based on NB, François-Xavier Josse-Michaux and Lorenzo Ubaldi To appear soon... Nicolás BERNAL Bethe Center for Theoretical Physics and Physikalisches Institut
kev sterile Neutrino Dark Matter in Extensions of the Standard Model
kev sterile Neutrino Dark Matter in Extensions of the Standard Model Manfred Lindner Max-Planck-Institut für Kernphysik, Heidelberg F. Bezrukov, H. Hettmannsperger, ML, arxiv:0912.4415, PRD81,085032 The
Pangenesis in a Baryon-Symmetric Universe: Dark and Visible Matter via the Affleck-Dine Mechanism
Pangenesis in a Baryon-Symmetric Universe: Dark and Visible Matter via the Affleck-Dine Mechanism Kalliopi Petraki University of Melbourne (in collaboration with: R. Volkas, N. Bell, I. Shoemaker) COSMO
Gravitino LSP as Dark Matter in the Constrained MSSM
Gravitino LSP as Dark Matter in the Constrained MSSM Ki Young Choi The Dark Side of the Universe, Madrid, 20-24 June 2006 Astro-Particle Theory and Cosmology Group The University of Sheffield, UK In collaboration
On Symmetric/Asymmetric Light Dark Matter
On Symmetric/Asymmetric Light Dark Matter Hai-Bo Yu University of Michigan, Ann Arbor Exploring Low-Mass Dark Matter Candidates PITT PACC, 11/16/2011 Motivations Traditionally, we focus on O(100 GeV) dark
Particle Physics and Cosmology II: Dark Matter
Particle Physics and Cosmology II: Dark Matter Mark Trodden Center for Particle Cosmology University of Pennsylvania Second Lecture Puerto Vallarta Mexico 1/13/2011 Problems of Modern Cosmology Is cosmic
Revisiting gravitino dark matter in thermal leptogenesis
Revisiting gravitino dark matter in thermal leptogenesis Motoo Suzuki Institute for Cosmic Ray Research (ICRR) The University of Tokyo arxiv:1609.06834 JHEP1702(2017)063 In collaboration with Masahiro
The Linear Collider and the Preposterous Universe
The Linear Collider and the Preposterous Universe Sean Carroll, University of Chicago 5% Ordinary Matter 25% Dark Matter 70% Dark Energy Why do these components dominate our universe? Would an Apollonian
LHC searches for momentum dependent DM interactions
LHC searches for momentum dependent interactions Daniele Barducci w/ A. Bharucha, Desai, Frigerio, Fuks, Goudelis, Kulkarni, Polesello and Sengupta arxiv:1609.07490 Daniele Barducci LHC searches for momentum
DARK MATTERS. Jonathan Feng University of California, Irvine. 2 June 2005 UCSC Colloquium
DARK MATTERS Jonathan Feng University of California, Irvine 2 June 2005 UCSC Colloquium 2 June 05 Graphic: Feng N. Graf 1 WHAT IS THE UNIVERSE MADE OF? An age old question, but Recently there have been
Cosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity
Cosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity Masaki Asano The Graduate University for Advanced Studies Collaborated with Shigeki Matsumoto Nobuchika Okada Yasuhiro
Astroparticle Physics and the LC
Astroparticle Physics and the LC Manuel Drees Bonn University Astroparticle Physics p. 1/32 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/32 Contents 1) Introduction:
PoS(idm2008)089. Minimal Dark Matter (15 +5 )
Institut de Physique Théorique, CNRS, URA 2306 & CEA/Saclay, F-91191 Gif-sur-Yvette, France E-mail: marco.cirelli@cea.fr Alessandro Strumia Dipartimento di Fisica dell Università di Pisa & INFN, Italia
The first one second of the early universe and physics beyond the Standard Model
The first one second of the early universe and physics beyond the Standard Model Koichi Hamaguchi (University of Tokyo) @ Colloquium at Yonsei University, November 9th, 2016. Credit: X-ray: NASA/CXC/CfA/M.Markevitch
Distinguishing Dark Matter Candidates from Direct Detection Experiments
Distinguishing Dark Matter Candidates from Direct Detection Experiments Chung-Lin Shan Department of Physics, National Cheng Kung University International Workshop on DM, DE and Matter-Antimatter Asymmetry
3.5 kev X-ray line and Supersymmetry
Miami-2014, Fort Lauderdale, Florida Bartol Research Institute Department Physics and Astronomy University of Delaware, USA in collaboration with Bhaskar Dutta, Rizwan Khalid and Qaisar Shafi, JHEP 1411,
LHC searches for dark matter.! Uli Haisch
LHC searches for dark matter! Uli Haisch Evidence for dark matter Velocity Observed / 1 p r Disk 10 5 ly Radius Galaxy rotation curves Evidence for dark matter Bullet cluster Mass density contours 10 7
Dark Matter WIMP and SuperWIMP
Dark Matter WIMP and SuperWIMP Shufang Su U. of Arizona S. Su Dark Matters Outline Dark matter evidence New physics and dark matter WIMP candidates: neutralino LSP in MSSM direct/indirect DM searches,
Measuring Dark Matter Properties with High-Energy Colliders
Measuring Dark Matter Properties with High-Energy Colliders The Dark Matter Problem The energy density of the universe is mostly unidentified Baryons: 5% Dark Matter: 20% Dark Energy: 75% The dark matter
Kaluza-Klein Dark Matter
Kaluza-Klein Dark Matter Hsin-Chia Cheng UC Davis Pre-SUSY06 Workshop Complementary between Dark Matter Searches and Collider Experiments Introduction Dark matter is the best evidence for physics beyond
Dark matter: evidence and candidates
.... Dark matter: evidence and candidates Zhao-Huan Yu ( 余钊焕 ) Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, CAS March 14, 2014 Zhao-Huan Yu (IHEP) Dark matter: evidence and
Dark matter and LHC: complementarities and limitations
Dark matter and LHC: complementarities and limitations,1,2, F. Mahmoudi 1,2,3, A. Arbey 1,2,3, M. Boudaud 4 1 Univ Lyon, Univ Lyon 1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574,
Cosmological Production of Dark Matter
Dark Matter & Neutrino School ICTP-SAIFR July 23-27, 2018 Cosmological Production of Dark Matter Farinaldo Queiroz International Institute of Physics & ICTP-SAIFR Outline 1. Introduction Cold and hot thermal
The Dark Matter Puzzle and a Supersymmetric Solution. Andrew Box UH Physics
The Dark Matter Puzzle and a Supersymmetric Solution Andrew Box UH Physics Outline What is the Dark Matter (DM) problem? How can we solve it? What is Supersymmetry (SUSY)? One possible SUSY solution How
Exotic Charges, Multicomponent Dark Matter and Light Sterile Neutrinos
Exotic Charges, Multicomponent and Light Sterile Neutrinos Julian Heeck Max-Planck-Institut für Kernphysik, Heidelberg 2.10.2012 based on J.H., He Zhang, arxiv:1210.xxxx. Sterile Neutrinos Hints for ev
Gravitinos, Reheating and the Matter-Antimatter Asymmetry of the Universe
Gravitinos, Reheating and the Matter-Antimatter Asymmetry of the Universe Raghavan Rangarajan Physical Research Laboratory Ahmedabad with N. Sahu, A. Sarkar, N. Mahajan OUTLINE THE MATTER-ANTIMATTER ASYMMETRY
f (R) Cosmology and Dark Matter
f (R) Cosmology and Dark Matter Dark side of the Universe Kyoto, December 14-18, 2015 G. Lambiase Università di Salerno Dipartimento di Fisica E.R. Caianiello & INFN - Naples Italy in collaboration with
A Minimal Supersymmetric Cosmological Model
A Minimal Supersymmetric Cosmological Model Ewan Stewart KAIST COSMO/CosPA 2010 University of Tokyo 29 September 2010 EDS, M Kawasaki, T Yanagida D Jeong, K Kadota, W-I Park, EDS G N Felder, H Kim, W-I
DarkSUSY. Joakim Edsjö With Torsten Bringmann, Paolo Gondolo, Lars Bergström, Piero Ullio and Gintaras Duda. APS Meeting
DarkSUSY Joakim Edsjö edsjo@fysik.su.se With Torsten Bringmann, Paolo Gondolo, Lars Bergström, Piero Ullio and Gintaras Duda APS Meeting 160830 Ways to search for dark matter Accelerator searches LHC Rare
Decaying Dark Matter and the PAMELA anomaly
Decaying Dark Matter and the PAMELA anomaly Alejandro Ibarra Technische Universität München In collaboration with Wilfried Buchmüller, Gianfranco Bertone, Laura Covi, Michael Grefe, Koichi Hamaguchi, Tetsuo
Invisible Sterile Neutrinos
Invisible Sterile Neutrinos March 25, 2010 Outline Overview of Sterile Neutrino Dark Matter The Inert Doublet Model with 3 Singlet Fermions Non-thermal Dark Matter Conclusion Work done in collaboration
Dark Matter and Dark Energy components chapter 7
Dark Matter and Dark Energy components chapter 7 Lecture 4 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,
Entropy, Baryon Asymmetry and Dark Matter from Heavy Neutrino Decays.
Entropy, Baryon Asymmetry and Dark Matter from Heavy Neutrino Decays. Kai Schmitz Deutsches Elektronen-Synchrotron DESY, Hamburg, Germany Based on arxiv:1008.2355 [hep-ph] and arxiv:1104.2750 [hep-ph].
Production of WIMPS in early Universe
Production of WIMPS in early Universe Anjishnu Bandyopadhyay Universität Bonn July 5, 2013 Anjishnu Bandyopadhyay Production of WIMPS in early Universe 1 / 30 1 2 Generalized Equation Equation for relics
Surprises in (Inelastic) Dark Matter
Surprises in (Inelastic) Dark Matter David Morrissey Harvard University with Yanou Cui, David Poland, Lisa Randall (hep-ph/0901.0557) Cornell Theory Seminar, March 11, 2009 Outline Evidence and Hints for
Dark Matter Electron Anisotropy: A universal upper limit
Seminari teorici del venerdì Enrico Borriello Università degli Studi di Napoli Federico II & INFN Sezione di Napoli Dark Matter Electron Anisotropy: A universal upper limit Based on Borriello, Maccione,
LHC Impact on DM searches
LHC Impact on DM searches Complementarity between collider and direct searches for DM Outline Introduction (complementarity of DM searches) Dark Matter signals at the LHC (missing ET, jets, etc... ) Particular
The inert doublet model in light of LHC and XENON
The inert doublet model in light of LHC and XENON Sara Rydbeck 24 July 212 Identification of Dark Matter, IDM 212, Chicago 1 The CERN Large Hadron Collider Only discovery so far. If no new strongly interacting
Cosmological Constraint on the Minimal Universal Extra Dimension Model
Cosmological Constraint on the Minimal Universal Extra Dimension Model Mitsuru Kakizaki (Bonn University) September 7, 2007 @ KIAS In collaboration with Shigeki Matsumoto (Tohoku Univ.) Yoshio Sato (Saitama
Dark Radiation from Particle Decay
Dark Radiation from Particle Decay Jörn Kersten University of Hamburg Based on Jasper Hasenkamp, JK, JCAP 08 (2013), 024 [arxiv:1212.4160] Jörn Kersten (Uni Hamburg) Dark Radiation from Particle Decay
components Particle Astrophysics, chapter 7
Dark matter and dark energy components Particle Astrophysics, chapter 7 Overview lecture 3 Observation of dark matter as gravitational ti effects Rotation curves galaxies, mass/light ratios in galaxies
Antiproton Limits on Decaying Gravitino Dark Matter
Antiproton Limits on Decaying Gravitino Dark Matter Michael Grefe Departamento de Física Teórica Instituto de Física Teórica UAM/CSIC Universidad Autónoma de Madrid Particle Theory Journal Club Rudolf
Signatures of clumpy dark matter in the global 21 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:
Signatures of clumpy dark matter in the global 2 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:0808.088 Daniel Grin Ay. Journal Club /23/2009 /8 Signatures of clumpy dark matter in
RECENT DEVELOPMENTS IN PARTICLE DARK MATTER
RECENT DEVELOPMENTS IN PARTICLE DARK MATTER KISS Dark Matter Workshop 15 July 2009 Jonathan Feng UC Irvine Feng 1 EVIDENCE FOR DARK MATTER There is now overwhelming evidence that normal (standard model)
Searching for sneutrinos at the bottom of the MSSM spectrum
Searching for sneutrinos at the bottom of the MSSM spectrum Arindam Chatterjee Harish-Chandra Research Insitute, Allahabad In collaboration with Narendra Sahu; Nabarun Chakraborty, Biswarup Mukhopadhyay
SFB 676 selected theory issues (with a broad brush)
SFB 676 selected theory issues (with a broad brush) Leszek Motyka Hamburg University, Hamburg & Jagellonian University, Krakow Physics of HERA and goals of the Large Hadron Collider The Higgs boson Supersymmetry
Feebly Interacting Massive Particles and their signatures
Feebly Interacting Massive Particles and their signatures Geneviève Bélanger LAPTH Annecy-le-Vieux See : GB, Boudjema, Goudelis, Pukhov, Zaldivar, 1801.03509 GB, Desai, Goudelis, Harz, Lessa, No, Pukhov,
SUSY Phenomenology & Experimental searches
SUSY Phenomenology & Experimental searches Slides available at: Alex Tapper http://www.hep.ph.ic.ac.uk/~tapper/lecture.html Objectives - Know what Supersymmetry (SUSY) is - Understand qualitatively the
Lecture 12. Dark Matter. Part II What it could be and what it could do
Dark Matter Part II What it could be and what it could do Theories of Dark Matter What makes a good dark matter candidate? Charge/color neutral (doesn't have to be though) Heavy We know KE ~ kev CDM ~
The Standard Model of particle physics and beyond
The Standard Model of particle physics and beyond - Lecture 3: Beyond the Standard Model Avelino Vicente IFIC CSIC / U. Valencia Physics and astrophysics of cosmic rays in space Milano September 2016 1
Possible Connections in Colliders, Dark Matter, and Dark Energy
Possible Connections in Colliders, Dark Matter, and Dark Energy 0704.3285 [hep-ph] 0706.2375 [hep-ph] Daniel Chung (U. Wisconsin Madison) Collaborators: L. Everett, K. Kong, K. Matchev Quiz Which of the
Physics Enters the Dark Age
Physics Enters the Dark Age Brooks Thomas University of Hawaii Colloquium at Macalester College, April 29th, 211 A Tour of the Dark Side of the Universe: Past, Present, and Future 1). A brief history of