Theoretical Aspects on Dark Matter and Its Detection
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1 Theoretical Aspects on Dark Matter and Its Detection Shufang Su U. of Arizona S. Su Dark Matters IWDD09, Shanghai June 15, 2009
2 Outline Dark matter evidence New physics and dark matter Dark matter candidates WIMP WIMPless superwimp Dark Matter Study direct/indirect DM searches, collider studies synergy between astrophysics and particle physics Conclusion S. Su Dark Matters 2
3 We are living through a revolution in our understanding of the Universe on the largest scales For the first time in history, we have a complete picture of the Universe S. Su Dark Matters 3
4 DM evidence: rotation curves Rotation curves of galaxies and galactic clusters V c const NGC 2403 Dark matter in halo Constrain Ω m V c 1/r 1/2 Ω i =ρ i /ρ c S. Su Dark Matters 4
5 Dark matter evidence: supernovae Supernovae Constrain Ω m Ω Λ S. Su Dark Matters 5
6 Dark matter evidence: CMB Cosmic Microwave Background Constrain Ω Λ +Ω m then now S. Su Dark Matters 6
7 Additional evidence S. Su Dark Matters 7
8 Synthesis Ω 0.5% Ω 0.5% Ω 3% Ω=23% ± 4% Ω=73% ± 4% Remarkable agreement Remarkable precision (~10%) S. Su Dark Matters 8
9 Synthesis Ω 0.5% Ω 0.5% Ω 3% Ω=23% ± 4% Ω=73% ± 4% Remarkable agreement Remarkable precision (~10%) S. Su Dark Matters 8
10 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H S. Su Dark Matters 9
11 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H SM is a very successful theoretical framework describes all experimental observations to date S. Su Dark Matters 9
12 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H S. Su Dark Matters 9
13 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H Not for cosmology observations Dark Matter Cosmology constant Baryon asymmetry S. Su Dark Matters 9
14 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H S. Su Dark Matters 9
15 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements S. Su Dark Matters 9
16 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su Dark Matters 9
17 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su Dark Matters 9
18 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su Dark Matters 9
19 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su Dark Matters 9
20 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su Dark Matters 9
21 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su Dark Matters 9
22 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su Dark Matters 9
23 Standard Model Quarks Leptons Gauge boson (force carrier) Higgs u c t d s b ν e ν µ ν τ e µ τ γ W ±,Z g H CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting No good candidates for CDM in SM S. Su Dark Matters 9
24 New physics beyond SM DM problem provide precise, unambiguous evidence for new physics Independent motivation for new physics in particle physics S. Su Dark Matters 10
25 New physics beyond SM DM problem provide precise, unambiguous evidence for new physics Independent motivation for new physics in particle physics! New physics to protect electroweak scale new symmetry: supersymmetry new space dimension: extradimension S. Su Dark Matters 10
26 Dark matter in new physics Dark Matter: new stable particle in many theories, dark matter is easier to explain than no dark matter there are usually many new weak scale particle constraints (proton decay, large EW corrections) discrete symmetry stability good dark matter candidate S. Su Dark Matters 11
27 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant S. Su Dark Matters mass (GeV) 12
28 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant S. Su Dark Matters mass (GeV) 12
29 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant S. Su Dark Matters mass (GeV) 12
30 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant S. Su Dark Matters mass (GeV) 12
31 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant appear in particle physics models motivated independently by attempts to solve EWSB relic density are determined by m pl and m weak naturally around the observed value no need to introduce and adjust new energy scale S. Su Dark Matters mass (GeV) 12
32 WIMP Boltzmann equation expansion χχ ff ff χχ S. Su Dark Matters 13
33 WIMP Boltzmann equation Thermal expansion equilibrium χχ ff ff χχ χχ ff WIMP S. Su Dark Matters 13
34 WIMP Boltzmann equation expansion χχ ff ff χχ Universe cools: n=n EQ e m/t WIMP S. Su Dark Matters 13
35 WIMP Boltzmann equation expansion χχ ff ff χχ Freeze out, n/s const WIMP S. Su Dark Matters 13
36 WIMP Boltzmann equation expansion χχ ff ff χχ S. Su Dark Matters 13
37 WIMP miracle WIMP: Weak Interacting Massive Particle m WIMP m weak σ an α weak 2 m weak 2 Ω h naturally around the observed value S. Su Dark Matters 14
38 Neutralino relic density 0.1 Ω χ h (prewmap) CMSSM S. Su Dark Matters 15
39 Neutralino relic density 0.1 Ω χ h (prewmap) CMSSM S. Su Dark Matters 15
40 Neutralino relic density 0.1 Ω χ h (prewmap) CMSSM S. Su Dark Matters 15
41 Neutralino relic density 0.1 Ω χ h (prewmap) CMSSM S. Su Dark Matters 15
42 Neutralino relic density 0.1 Ω χ h (prewmap) CMSSM S. Su Dark Matters 15
43 Neutralino relic density 0.1 Ω χ h (prewmap) CMSSM Cosmology excludes much of the parameter space Ω χ too big cosmology focuses attention on particular regions Ω χ just right S. Su Dark Matters 15
44 WIMPless? Feng and Kumar (2008) Ω X 1 σv m2 X g 4 X (m X,g X ) (m weak, g weak ), Ωh only fixes one combination of dark matter mass and coupling could have mx mweak as long as the relation holds S. Su Dark Matters 16
45 WIMPless miracle m X g 2 X m g 2 F 16π 2 M Ω X 1 σv m2 X g 4 X right relic density! (irrespective of its mass) 10 3 < g X < 3 10 MeV < m X < 10 TeV if no direct coupling to SM: interact only through gravity impact on structure formation no direct/indirect/collider signals S. Su Dark Matters 17
46 WIMPless DM: not hidden S. Su Dark Matters 18
47 WIMPless DM: not hidden my max (mweak, mx) interaction λ XYf S. Su Dark Matters 18
48 WIMPless DM: not hidden my max (mweak, mx) interaction λ XYf indirect detection XX ff, YY direct detection Xf Xf collider: 4th generation fermions light DM: mx << mweak Ω = n m: m, n enhanced indirect detection mweak 2 /mx 2 over WIMP signal S. Su Dark Matters 18
49 WIMPless DM resonance enhancement S. Su Dark Matters 19
50 SuperWIMP / Extremely WIMP DM interaction << Weak interaction. Possible? CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting (much weaker than electroweak) S. Su Dark Matters 20
51 SuperWIMP / Extremely WIMP DM interaction << Weak interaction. Possible? CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting (much weaker than electroweak) But the relic density argument strongly prefers WIMPtype masscoupling relation. S. Su Dark Matters 20
52 SuperWIMP / Extremely WIMP DM interaction << Weak interaction. Possible? CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting (much weaker than electroweak) But the relic density argument strongly prefers WIMPtype masscoupling relation. Ω DM 1/ σv m 2 /g 4 S. Su Dark Matters 20
53 SuperWIMP / Extremely WIMP DM interaction << Weak interaction. Possible? CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting (much weaker than electroweak) But the relic density argument strongly prefers WIMPtype masscoupling relation. Ω DM 1/ σv m 2 /g 4 for superweak coupling σv too small ΩDM too big overclose the Universe S. Su Dark Matters 20
54 SuperWIMP / Extremely WIMP if the Universe is never hot enough, low T R Thermal production: plasma scattering Nonthermal process: WIMP decay out of equilibrium S. Su Dark Matters 21
55 Thermal production Gravitino Bolz, Brandenburg and buchmuller (2001) g a G g a g b g c + G g a G g a G g c + g b g a g b + g c g b ( ) 100 GeV ( ) ( ) 2 Ω Thermal m g T R 0.2 G m 3/2 1 TeV GeV g c g b g c Ω upper bound on T R Leptogenesis: TR>10 9 GeV m3/2 > 10 GeV m3/2 min TR mgluino 2 Axino Covi, Kim, Kim and Roszkowski (2001); Brandenburg and Steffen (2004) Ω Thermal ã 0.6 ( mã 0.1 GeV ) ( GeV f a ) 2 ( TR ) 10 4 GeV S. Su Dark Matters 22
56 Nonthermal production: WIMP decay WIMP superwimp + SM particles Kim, Masiero, Nanopoulos (1984) Covi, Kim, Roszkowski (1999) Feng, Rajaraman, Takayama (2003); Bi, Li, Zhang (2003); Ellis, Olive, Santoso, Spanos (2003); Wang, Yang (2004); Feng, Su, Takayama (2004); Buchmuller, hamaguchi, Ratz, Yanagida (2004); Roszkowski, Ruiz de Austri, Choi (2004); Brandeburg, Covi, hamaguchi, Roszkowski, Steffen (2005);... S. Su Dark Matters 23
57 Nonthermal production: WIMP decay WIMP superwimp + SM particles WIMP S. Su Dark Matters 23
58 Nonthermal production: WIMP decay WIMP superwimp + SM particles WIMP S. Su Dark Matters 23
59 Nonthermal production: WIMP decay WIMP superwimp + SM particles SWIMP SM S. Su Dark Matters 23
60 Nonthermal production: WIMP decay WIMP superwimp + SM particles S. Su Dark Matters 23
61 Nonthermal production: WIMP decay WIMP superwimp + SM particles superwimp e.g. Gravitino LSP LKK graviton axino WIMP neutral charged S. Su Dark Matters 23
62 Dark matter detection DM f DM f DM annihilation Ω 1/<σv> Not overclose universe Efficient annihilation then S. Su Dark Matters 24
63 Dark matter detection DM DM DM annihilation f f Cross symmetry DM f DM f Ω 1/<σv> DM scattering Not overclose universe Efficient annihilation then S. Su Dark Matters 24
64 Dark matter detection DM DM DM annihilation f f Cross symmetry DM f DM f Ω 1/<σv> Not overclose universe Efficient annihilation then DM scattering Efficient scattering now direct DM direction S. Su Dark Matters 24
65 Dark matter detection DM DM DM annihilation f f Cross symmetry DM f DM f Ω 1/<σv> Not overclose universe Efficient annihilation then DM scattering Efficient scattering now direct DM direction Efficient annihilation now indirect DM direction S. Su Dark Matters 24
66 Direct detection sun halo bulge disk Scatter from a Nuclei in a Terrestrial particle detector Measure nuclear recoil energy DM The Milky Way detector S. Su Dark Matters 25
67 Direct detection sun halo bulge disk Scatter from a Nuclei in a Terrestrial particle detector Measure nuclear recoil energy DM The Milky Way detector Number of target nuclei in detector S. Su Dark Matters 25
68 Direct detection sun halo bulge disk Scatter from a Nuclei in a Terrestrial particle detector Measure nuclear recoil energy DM The Milky Way detector Number of target nuclei in detector Local WIMP density (astro physics) S. Su Dark Matters 25
69 Direct detection halo sun bulge disk Scatter from a Nuclei in a Terrestrial particle detector Measure nuclear recoil energy DM The Milky Way detector Number of target nuclei in detector scattering cross section (particle physics) Local WIMP density (astro physics) S. Su Dark Matters 25
70 Direct detection halo sun bulge disk Scatter from a Nuclei in a Terrestrial particle detector Measure nuclear recoil energy DM The Milky Way detector Number of target nuclei in detector scattering cross section (particle physics) Local WIMP density (astro physics) <E> ~ 30 KeV rate < 0.01/kg/day S. Su Dark Matters 25
71 Dark matter in the galactic halo galactic center Sun 230 km/s June Dec. Exploit movement of Earth/Sun through DM halo Direction of recoil most events should be opposite Earth/Sun direction Annual modulation harder spectrum in summer than in winter Spergel (1988) Drukier, Freese and Spergel (1986) Log(rate) Dec ~2% seasonal effect June S. Su Dark Matters 26 E recoil
72 Recoil energy rgy r WIMP 10% energy Ionization Target Phonons/heat 100% energy slowest cryogenics Light 1% energy fastest no surface effects WIMP S. Su Dark Matters from Dan Akerib s talk at CERCA DM workshop 27
73 Spin independent limits spin independent scattering couples to scalar density of quarks and gluons scales as A 2 dominant for heavy atom target S. Su Dark Matters 28 see dmtools.berkeley.edu
74 Spin dependent limits spin dependent scattering dominate by axial couplings to unpaired nucleon couples to spin multiple form factors does not scale with A coupling to proton Science 318, 933 (2008) S. Su Dark Matters 29
75 Spin dependent limits n SD (pb) DAMA/NaI allowed COUPP (2007) (this work) CDMS Si ( ) CDMS Ge ( ) Tokyo CaF 2 (2005) PICASSO (2005) KIMS (2007) NAIAD (2005) SIMPLE (2005) DAMA/Xe (2000) coupling to neutron Science 318, 933 (2008) ZEPLINII (2007) Edelweiss 1 (2000/2/3) S. Su Dark Matters 30
76 Spin dependent limits n SD (pb) DAMA/NaI allowed COUPP (2007) (this work) Science 318, 933 (2008) CDMS Si ( ) CDMS Ge ( ) Tokyo CaF 2 (2005) PICASSO (2005) KIMS (2007) NAIAD (2005) SIMPLE (2005) ZEPLINII (2007) Edelweiss 1 (2000/2/3) DAMA/Xe (2000) WIMP Mass [GeV/c 2 ] S. Su Dark Matters 30 SD pure neutron cross section [cm 2 ] 10!34 10!36 10!38 10!40 coupling to neutron XENON10, DAMA KIMS ZEPLINII CDMSII XENON
77 DAMA Crosssection [cm 2 ] (normalised to nucleon) WIMP Mass [GeV/c 2 ] Gaitskell,Mandic,Filippini DAMA/NaI ( ) annual 6.3σ DAMA/LIBRA (2003+) annual 8.2σ x x x DATA listed top to bottom on plot DAMA/LIBRA sigma, no ion channeling CDMS (Soudan) 2005 Si (7 kev threshold) Edelweiss I final limit, 62 kgdays Ge limit WARP 2.3L, 96.5 kgdays 55 kev threshold DAMA/LIBRA sigma, no ion channeling ZEPLIN II (Jan 2007) result CRESST kgday CaWO4 CDMS (Soudan) Ge (7 kev threshold) ZEPLIN III (Dec 2008) result CDMS: (reanalysis) Ge XENON (Net 136 kgd) CDMS Soudan 2007 projected SuperCDMS (Projected) 2ST@Soudan SuperCDMS (Projected) 25kg (7ST@Snolab) Trotta et al 2008, CMSSM Bayesian: 68% contour Trotta et al 2008, CMSSM Bayesian: 95% contour Ellis et. al Theory region postlep benchmark points Baltz and Gondolo 2003 Baltz and Gondolo, 2004, Markov Chain Monte Carlos generated using DM plotter S. Su Dark Matters 31
78 DAMA results Bernabei et al. (2008) Bernabei et. al. (2008) DAMA/NaI and DAMA/LIBRA modulation amplitude (26 kevee) Sm=0.0131± /kg/day/kevee S. Su Dark Matters 32
79 DAMA interpretation Backgrounds/systematics: temperature, neutrons+other bgs, radon, detector noise... none produce all signal characteristics or capable of producing level of signal Explanation/effects low mass WIMPS (NaI 30 GeV cutoff) spindependent couplings channeling Migdal effect inelastic scattering mirror matter... parameter spaces remain: compatible with DAMA and all null results spinindependent: 710 GeV spindependent (proton): 310 GeV spindependent (neutron): 79 GeV spindependent (mixed): 310 GeV Freese, Gelmini, Gondolo and Savage, S. Su Dark Matters 33
80 DAMA interpretation of these shaped pulses is an efficient tag for microphonic 2 events [10]. These software cuts, applied on the digitized and stored amplifier traces, are trained on datasets conbackgrounds/systematics: sisting of asymptomatic lowenergy signals from an electronic detector pulser. The goal is to obtain temperature, neutrons+other bgs, radon, noise... the maximum signal acceptance for the best possible microphonic rejection. none produce all signal characteristics or capable of applied producing levelto of signal A correction is also to the data, compensate for the modest signal acceptance losses (few percent) imposed by this method. The energy resolution and calexplanation/effects ibration were obtained using the cosmogenic activation in 71 Ge (T1/2 =11.4 d), leading to intense peaks at 1.29 low mass WIMPS (NaI 30 GeV cutoff) kev and kev following installation, and a 133 Ba source providing five auxiliary lines below 400 kev. An spindependent couplings excellent linearity was observed. The energy resolution σ channeling below 10 kev is approximated by σ 2 = σn2 + (2.35)2 EηF, where σn =69.7 ev is the intrinsic electronic noise, E is Migdal effect parameter spaces remain: compatible the energy in ev, η= 2.96 ev is the average energy recogent inelastic scattering to create pair in Ge at 80 K, with quired DAMA and an allelectronhole null results and F 0.06 is the measured Fano factor. mirror matter 710 GeV FIG. 2: Parameter space region (crosshatched) able to ex spinindependent: The spectrum of energy depositions so obtained can plain the... DAMA modulation via spinindependent couplings then be compared with (proton): expected signals fromgev a stanspindependent 310 from an isothermal lightwimp halo [5]. Lines delimit the isothermal galactic WIMP halo. The spectrum of coupling (σsi ) vs. WIMP mass (mχ ) regions excluded by dard spindependent (neutron): 79 GeV[11], WIMPinduced recoil energies is generated following relevant experiments [5]. All regions are defined at the 90% 3 a local WIMP density of 0.3 GeV/cm, agev halo veconfidence level. Inset: PPC spectrum used for the extrac using spindependent (mixed): 310 tion of present limits. Lines display the signals expected from locity dispersion of 230 km/s, an Earthhalo velocity of 2 some reference WIMP candidates (dotted: mχ = 8 GeV/c, 244 km/s and a galactic escape velocity of 650 km/s. The Freese, Gelmini, Gondolo and Savage, σsi = 10 4 pb. Dashed: mχ = 6 GeV/c2, σsi = pb. quenching factor (i.e., the fraction of recoil energy meadashdotted: mχ = 4 GeV/c2, σsi = 10 2 pb). S. Su Dark Matters surable as ionization) for subkev germanium recoils has 33 been measured with this PPC, using a dedicated 24 kev neutron beam [12]. It was found to be in excellent agree
81 DAMA interpretation Backgrounds/systematics: temperature, neutrons+other bgs, radon, detector noise... none produce all signal characteristics or capable of producing level of signal Explanation/effects low mass WIMPS (NaI 30 GeV cutoff) spindependent couplings channeling Migdal effect inelastic scattering mirror matter... parameter spaces remain: compatible with DAMA and all null results spinindependent: 710 GeV spindependent (proton): 310 GeV spindependent (neutron): 79 GeV spindependent (mixed): 310 GeV Freese, Gelmini, Gondolo and Savage, S. Su Dark Matters 33
82 Talks in this workshop on DM direct detection Youngduk Kim: KIMS Henry Wong: TEXONO Neil Spooner: DRIFT Juan Collar: COUPP Gilles Gerbier: EDELWEISS Kazuyoshi Kobayashi: XMASS Elena Aprile: XENON Richard Gaitskell: LUX James White: high pressure TPC Cristiano Galbiati: depleted argon S. Su Dark Matters 34
83 Indirect detection DM DM Γ A n DM 2 detector S. Su Dark Matters 35
84 Indirect detection DM DM Γ A n DM 2 Dark Matter annihilate detector recipe in (amplifier) to, a place some particles which are detected by. an experiment S. Su Dark Matters 35
85 Dark Matter annihilates recipe in center of the sun to neutrinos, a place some particles which are detected by AMANDA, ICECUBE. an experiment earth ν µ Dark matter density in the sun, capture rate S. Su Dark Matters 36
86 IceCube reach AMANDA IceCube (22 strings) SuperK full IceCube reach S. Su Dark Matters 37
87 Indirect detection: neutrino MSSM icecube Hooper and Wang (2003) S. Su Dark Matters 38
88 Dark Matter annihilates in galactic center to photons, recipe a place some particles which are detected by FERMI, HESS. an experiment HESS FERMI Dark matter density in the center of the galaxy S. Su Dark Matters 39
89 Indirect detection: gamma ray MSSM EGRET GLAST Hooper and Wang (2003) S. Su Dark Matters 40
90 Dark Matter annihilates in the halo to positrons, a place some particles recip e which are detected by AMS, HEAT, PAMELA. an experiment Dark matter density profile in the halo S. Su Dark Matters 41
91 PAMELA PAMELA, arxiv: S. Su Dark Matters 42
92 PAMELA PAMELA, arxiv: astrophysical expectation (secondary production) S. Su Dark Matters 42
93 PAMELA rapid climb above 10 GeV indicates the presence of a primary source of cosmic ray positrons PAMELA, arxiv: astrophysical expectation (secondary production) S. Su Dark Matters 42
94 PAMELA no excess in antip PAMELA, arxiv: PAMELA, arxiv: astrophysical expectation (secondary production) S. Su Dark Matters 42
95 ATIC ATIC Nature Wefel et al., 2008 S. Su Dark Matters 43
96 FERMI and HESS s 1 m 2 sr 1 ) " E ± 15% 2 dn/de (GeV 3 E 10 2 ATIC PPBBETS Kobayashi H.E.S.S. H.E.S.S. lowenergy analysis Systematic error Systematic error lowenergy analysis Broken powerlaw fit FERMI, arxiv: Energy (GeV) HESS, arxiv: S. Su Dark Matters 44
97 Fermi PAMELA, ATIC, FERMI and HESS increased spectrum for e+ flat spectrum for e (above BG) antip consistent with BG PAMELA arxiv: Adriani et al., 2008 Pulsars particle physics: dark matter Background background? Note : S. Su Dark Matters 45 Lot Dark of matter e+,every little p astrophysics: pulsars...
98 Particle physics interpretation very hard spectrum: dark matter mass: ~ multitev large annihilation cross section Sommerfeld enhancement Nonthermal production Asymmetric dark matter Decay... no excess in antip: like lepton better than quark hadron heavier than lepton: kinematics leptonic dark sector: symmetry... Goh, Hall and Kumar, arxiv: ArkaniHamed et. al., arxiv: Cirelli, Strumia, arxiv: Fox and Poppitz, arxiv: ArkaniHamed, Finkbeiner, Slatyer and Weiner, arxiv: ,... S. Su Dark Matters 46
99 Annihilation into leptons annihilate into e,μ,τ Bergstrom, Edsjo, Zaharijas, 2009 Cholis et. al., arxiv: S. Su Dark Matters 47
100 Light force carrier dark force: mϕ < GeV ArkaniHamed, Finkbeiner, Slatyer and Weiner, arxiv: DM ϕ e,μ,τ τ DM ϕ τ DM ϕ τ S. Su Dark Matters 48 τ
101 Leptonic Higgs Leptonic Higgs Goh, Hall and Kumar, arxiv: DM H lep e,μ,τ τ DM annihilation or decay H lep H lep τ τ S. Su Dark Matters 49 τ
102 Astrophysical solutions a boost factor of 10 3 narrow diffusion region Hopper and Silk, hepph/ a large nearby clump of dark matter Hooper, Stebbins and Zurek, arxiv: nearby pulsars Hooper, Blasi and Serpico, arxiv: the current set of data does not allow us to identify the origin of PAMELA and FERMI signals PAMELA result is consistent with being the first detection of particle dark matter further complementary measurements are required to answer the questions of these particles origin S. Su Dark Matters 50
103 Collider study of dark matter Can study those regions at colliders Tevatron LHC p p p p ILC Now 2009 Precise determination of new particle mass and coupling Determine DM mass, relic density S. Su Dark Matters 51
104 Synergy S. Su Dark Matters 52
105 Synergy Collider Inputs Weakscale Parameters DM Annihilation DMN Interaction S. Su Dark Matters 52
106 Synergy Collider Inputs Weakscale Parameters DM Annihilation DMN Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs S. Su Dark Matters 52
107 Synergy parts per mille agreement for Ω χ " discovery of dark matter Collider Inputs Weakscale Parameters DM Annihilation DMN Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs S. Su Dark Matters 52
108 Synergy parts per mille agreement for Ω χ " discovery of dark matter Collider Inputs Weakscale Parameters local DM density and velocity profile DM Annihilation DMN Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs S. Su Dark Matters 52
109 Synergy parts per mille agreement for Ω χ " discovery of dark matter Collider Inputs Weakscale Parameters local DM density and velocity profile DM Annihilation DMN Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs eliminate particle physics uncertainty do real astrophysics S. Su Dark Matters 52
110 Conclusion We now know the composition of the Universe No known particle in the SM can be DM precise, unambiguous evidence for new physics New physics new stable particle as DM candidate Many dark matter candidates Dark matter detection direct/indirect DM searches, collider studies Synergy between astrophysics and particle phycics S. Su Dark Matters 53
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