Beyond the WIMP Miracle

Transcription

1 Beyond the WIMP Miracle Shufang Su U. of Arizona S. Su PittPACC LDM workshop Nov 16, 2011

2 Beyond the WIMP Miracle WIMP miracle WIMPless general framework light dark matter collider signature superwimp S. Su

3 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) HEPAP/AAAC DMSAG Subpanel (2007) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant S. Su mass (GeV) 2

4 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) HEPAP/AAAC DMSAG Subpanel (2007) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant S. Su mass (GeV) 2

5 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) HEPAP/AAAC DMSAG Subpanel (2007) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant S. Su mass (GeV) 2

6 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) HEPAP/AAAC DMSAG Subpanel (2007) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla Black Hole Remnant S. Su mass (GeV) 2

7 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) HEPAP/AAAC DMSAG Subpanel (2007) 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 mass (GeV) 2

8 WIMP Weak Interacting Massive Particle WIMP m WIMP m weak g weak 2 S. Su 3

9 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 WIMP appears in many BSM scenarios lightest supersymmetric particles in SUSY models lightest KK particles in extra dimension models... S. Su 4

10 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 WIMP appears in many BSM scenarios lightest supersymmetric particles in SUSY models lightest KK particles in extra dimension models... S. Su 4

11 WIMP m WIMP m weak g weak 2 Is it necessary to have both? S. Su 5

12 WIMP m WIMP m weak g weak 2 Is it necessary to have both? WIMPless S. Su 5

13 WIMPless miracle Ω X 1 σv m2 X g 4 X only fixes one combination of dark matter mass and coupling mx/gx 2 ~ mweak/gweak 2, Ωh 2 ~ 0.3 could have mx mweak as long as the relation holds WIMPless DM J.L. Feng and J. Kumar, PRL 101, (2008) J.L. Feng, H. Tu and H. Yu, JCAP 0810, 043 (2008) Feng, Shadmi, PRD 83, (2011) Feng, Rentala, Surujon, dark matter: no SM gauge interactions, not WIMP naturally obtain right relic density: similar to WIMP S. Su 6

14 WIMPless miracle J.L. Feng and J. Kumar, PRL 101, (2008) Dark matter is hidden no SM interactions DM sector has its own particle content, mass mx, coupling gx Connected to SUSY breaking sector WIMPs m X g 2 X m g 2 F 16π 2 M Ω X 1 σv m2 X g 4 X WIMPless DM right relic density! (irrespective of its mass) S. Su 7

15 WIMPless: not hidden If no direct coupling to SM: interact only through gravity impact on structure formation no direct/indirect/collider signals S. Su 8

16 WIMPless: not hidden If no direct coupling to SM: interact only through gravity impact on structure formation no direct/indirect/collider signals my max (mweak, mx) interaction λ XYf S. Su 8

17 WIMPless: not hidden If no direct coupling to SM: interact only through gravity impact on structure formation no direct/indirect/collider signals my max (mweak, mx) interaction λ XYf indirect detection XX ff, YY direct detection Xf Xf collider: 4th generation fermions S. Su 8

18 WIMPless: not hidden If no direct coupling to SM: interact only through gravity impact on structure formation no direct/indirect/collider signals my max (mweak, mx) interaction λ XYf indirect detection XX ff, YY direct detection Xf Xf open new possibility for DM model parameters new experimental search windows collider: 4th generation fermions S. Su 8

19 WIMPless: not hidden If no direct coupling to SM: interact only through gravity impact on structure formation no direct/indirect/collider signals my max (mweak, mx) interaction λ XYf light dark matter indirect detection XX ff, YY direct detection Xf Xf open new possibility for DM model parameters new experimental search windows collider: 4th generation fermions S. Su 8

20 WIMPless: not hidden If no direct coupling to SM: interact only through gravity impact on structure formation no direct/indirect/collider signals my max (mweak, mx) interaction λ XYf indirect detection XX ff, YY direct detection Xf Xf collider: 4th generation fermions light dark matter open new possibility for DM model parameters new experimental search windows provide a framework that guarantee DM relic density allow freedom in DMSM interaction S. Su 8

21 Light dark matter WIMPNucleon Cross Section [cm 2 ] DAMA/Na CoGeNT DAMA/I CDMS (2011) CDMS (2010) XENON10 (S2 only, 2011) EDELWEISS (2011) XENON100 (2011) observed limit (90% CL) Expected limit of this run: ± 1! expected ± 2! expected XENON100 (2010) Trotta et al. small mass, large σsi DAMA vs. CoGeNT? reconcile with CDMS/XENON? Buchmueller et al WIMP Mass [GeV/c ] XENON 100: S. Su 9

22 Light dark matter light DM with large σsi not generic in typical WIMP SI : chirality flip, proportional to Yukawa coupling A. Bottino, F. Donato, N. Fornengo and S. Scopel, PRD 68, (2003); PRD 77, (2008); PRD 78, (2008). can be easily accommodated in WIMPless model with connector Y J.L. Feng, J. Kumar and L.E. Strigari, PLB 670, 37 (2008) W = i (λ i qxy ql q i L + λ i uxy ur u i R + λ i dxy dr d i R) QYqL L : TYuR R : B R : YdR 3, 2, 1 6 3, 1, 2 S. Su , 1, 1 3.

23 Light dark matter light DM with large σsi not generic in typical WIMP SI : chirality flip, proportional to Yukawa coupling A. Bottino, F. Donato, N. Fornengo and S. Scopel, PRD 68, (2003); PRD 77, (2008); PRD 78, (2008). can be easily accommodated in WIMPless model with connector Y J.L. Feng, J. Kumar and L.E. Strigari, PLB 670, 37 (2008) W = i (λ i qxy ql q i L + λ i uxy ur u i R + λ i dxy dr d i R) not chirality opposite chirality of SM quark QYqL L : TYuR R : B R : YdR 3, 2, 1 6 3, 1, 2 S. Su , 1, 1 3.

24 Light dark matter light DM with large σsi not generic in typical WIMP SI : chirality flip, proportional to Yukawa coupling A. Bottino, F. Donato, N. Fornengo and S. Scopel, PRD 68, (2003); PRD 77, (2008); PRD 78, (2008). can be easily accommodated in WIMPless model with connector Y J.L. Feng, J. Kumar and L.E. Strigari, PLB 670, 37 (2008) W = i (λ i qxy ql q i L + λ i uxy ur u i R + λ i dxy dr d i R) not chirality opposite chirality of SM quark QYqL L : TYuR R : B R : YdR 3, 2, 1 6 3, 1, 2 Exotic mirror quarks S. Su , 1, 1 3.

25 Connector couple with first two gen. first two generations, tree level scattering λ ~ 0.03 X X X Q X YL YR X Q q q q q g q g J.L. Feng and J. Kumar, PRL 101, (2008) S. Su 11

26 Connector couple with third gen. third generation loop level scattering, λ ~ 0.31, more natural less constrained by FCNC X Q X q q g q g S. Su J.L. Feng, J. Kumar and L.E. Strigari, PLB , 37 (2008)

27 Isospin violating dark matter DM scattering off a nucleus: coherent σa ~ (fp Z + fn (AZ)) 2 Giuliano (2005); Chang, Liu, Pierce, Weiner, Yavin (2010) Feng, Kumar, Marfatia, Sanford (2011) usual assumptions: fp = fn σa ~ (fpa) 2 results for various target nuclei in (m, σp) plane A 2 scaling isospin violation fp fn could appear in many BSM decouple one exp with fn/fp=z/(az) not exact cancellation due to isotopes Z N p i iso. 2 2 i A Z f i n fp Ai Z i i 2 2 A i i A S. Su 13

28 Isospin violating dark matter f n /f p = 1 f n /f p = Feng, Kumar, Marfatia, Sanford (2011) 1 7 hard to fit all three signals CDMS, CoGeNT both Germanium based SIMPLE gets tighter S. Su 14

29 Realization of IVDM in WIMPless at nucleon level: fp fn at quark level: W = i (λ i qxy ql q i L + λ i uxy ur u i R + λ i dxy dr d i R) X X YL YR X Q q q SI operators isospin violating O i = λ i qλ i uxxū i u i /m Y + λ i qλ i dxx d i d i /m Y f p,n /M 2 = i (λi qλ i ub p,n u +λ i qλ i i d Bp,n d )/( πm i X m Y ) B p,n are integrated nuclear form factors, including fn/fp ~ 0.7 λ 1 u 1.08 λ1 d, < λ1 q λ1 d < S. Su 15

30 Collider constraints O i = λ i qλ i uxxū i u i /m Y + λ i qλ i dxx d i d i /m Y Tevatron: λq λu,d < 1, two orders of magnitude too weak Feng, Kumar, Marfatia, Sanford, Tevatron and LHC, 1 fb 1 : tension with IVDM Rajaramam, Shepherd, Tait, Wijangco, X: fermion (vs. scalar) minimal flavor violation SU(2) breaking term ~ mq S. Su 16

31 Collider constraints O i = λ i qλ i uxxū i u i /m Y + λ i qλ i dxx d i d i /m Y Tevatron: λq λu,d < 1, two orders of magnitude too weak Feng, Kumar, Marfatia, Sanford, Tevatron and LHC, 1 fb 1 : tension with IVDM Rajaramam, Shepherd, Tait, Wijangco, X: fermion (vs. scalar) minimal flavor violation SU(2) breaking term ~ mq IVDM (with scalar) is still a viable solution... S. Su 16

32 Collider signature: exotic quarks Y particle appears as exotic mirror quarks Q DM p Qʼ p Qʼ q DM q Collider Signal (4th gen) T T ttxx, B B bbxx J. Alwall, J.L. Feng, J. Kumar, SS ; differ from SUSY searches: cascade decay differ from usual 4th generation quark T Wb, B Wt S. Su 17

33 Collider Signature: exotic quarks Collider Signal: T T ttxx, B B bbxx Connection to solution for Hierarchy problem need top partner the lighter, the more natural decay straight to invisible particles bottom partner appears in a general set of new physics scenarios light stop/sbottom asymmetric dark matter little Higgs with Tparity B. Dutta and J. Kumar, arxiv: H.C. Cheng and I. Low, JHEP 0408, 061 (2004) baryon and lepton number as gauge symmetry... relevant for reexamine of naturalness based on LHC data, light stop/sbottom signatures. P. Fileviez Perez and M. B. Wise, arxiv: S. Su 18

34 Constraints perturbativity constraints: mq = yq v, mq 600 GeV (if through Yukawa) precision electroweak data: mt mb ~ 50 GeV (for SU(2) doublet) direct searches limits B B bbxx, similar to sbottom pair production with (pb) 2 "! B D0, L=5.2 fb (a) LQ NLO cross section, B%BF(LQ $b# )=1 LQ NLO cross section, B=1 0.5!F 3 Observed limits Expected limits sp Neutralino Mass (GeV) D0, L=5.2 fb (b) m b ~ 1 Observed Expected = m b + m & ' 0 LEP 1 s=208 GeV D0 Run I 1 92 pb CDF Run I 1 88 pb D0 Run II fb CDF Run II pb D0 Run II pb Leptoquark Mass (GeV) Bottom Squark Mass (GeV) S. Su V. M. Abazov et al. [D0 Collaboration],

35 Constraints perturbativity constraints: mq = yq v, mq 600 GeV (if through Yukawa) precision electroweak data: mt mb ~ 50 GeV (for SU(2) doublet) direct searches limits B B bbxx, similar to sbottom pair production with (pb) 2 "! B D0, L=5.2 fb (a) LQ NLO cross section, B%BF(LQ $b# )=1 LQ NLO cross section, B=1 0.5!F 3 Observed limits Expected limits msb > 247 GeV sp Neutralino Mass (GeV) mb 60 > 365 GeV D0, L=5.2 fb (b) m b ~ 1 Observed Expected = m b + m & ' 0 LEP 1 s=208 GeV D0 Run I 1 92 pb CDF Run I 1 88 pb D0 Run II fb CDF Run II pb D0 Run II pb Leptoquark Mass (GeV) Bottom Squark Mass (GeV) S. Su V. M. Abazov et al. [D0 Collaboration],

36 B : Tevatron Reach J. Alwall, J.L. Feng, J. Kumar, SS Signal: B B bbxx optimal cuts (after precuts) S/B > 0.1, more than 2 events Bg: W(lν)jj, Z(νν) jj,wz, ttbar, single top. Poisson statistics (GeV) m X Exclusion for B B! b X b X at Tevatron (GeV) m X Discovery for B B! b X b X at Tevatron m B = m X + m b 20 fb 10 fb 1 5 fb m B = m X + m b 20 fb 10 fb 1 5 fb m B m B S. Su 20 (GeV) (GeV)

37 B : Tevatron Reach J. Alwall, J.L. Feng, J. Kumar, SS Signal: B B bbxx optimal cuts (after precuts) S/B > 0.1, more than 2 events Bg: W(lν)jj, Z(νν) jj,wz, ttbar, single top. Poisson statistics (GeV) m X Exclusion for B B! b X b X at Tevatron (GeV) m X Discovery for B B! b X b X at Tevatron m B = m X + m b 20 fb 10 fb 1 5 fb m B = m X + m b 20 fb 10 fb 1 5 fb mb > 440 GeV with 5 fb m B m B S. Su 20 (GeV) (GeV)

38 LHC reach J. Alwall, J.L. Feng, J. Kumar, SS B B bbxx optimal cuts (after precuts) S/B > 0.1, more than 2 events Poisson statistics (GeV) m X Exclusion for B B! b X b X at 7 TeV LHC m B = m X + m b (GeV) m X Discovery for B B! b X b X at 7 TeV LHC m B = m X + m b pb pb pb pb pb pb m B m B (GeV) S. Su 21 (GeV)

39 Simulation MadGraph Pythia PGS Signal: T T t ( ) X t ( ) X bw + X bw X hadronic channel: large cross section SM backgrounds, tt, W, have MET with lepton irreducible background: Z νν + jets semileptonic channel: isolated lepton, suppress QCD background purely leptonic channel: suppressed cross section Similar analyses in the literature semileptonic mode, high mass, large luminosity T. Han, R. Mahbubani, D. G. E. Walker and L. T. E. Wang, JHEP 0905, 117 (2009) hadronic mode, spin and mass determination P. Meade and M. Reece, Phys. Rev. D 74, (2006). S. Su 22

40 Tevatron exclusion optimal cuts (after precuts) S/B > 0.1, more than 2 events Poisson statistics (GeV) m X J. Alwall, J.L. Feng, J. Kumar, SS, Exclusion for T T! t X t X at the Tevatron fb m T 10 fb 1 5 fb = m X + m t 1 20 fb 1 Semileptonic channel (GeV) m X Exclusion for T T! t X t X at the Tevatron m T 1 2 fb = m X + m t 20 fb 1 10 fb 1 5 fb Hadronic channel S. Su m T (GeV) m T (GeV)

41 Tevatron exclusion optimal cuts (after precuts) S/B > 0.1, more than 2 events Poisson statistics T. Aaltonen et al. [CDF Collaboration], arxiv: (GeV) m X J. Alwall, J.L. Feng, J. Kumar, SS, Exclusion for T T! t X t X at the Tevatron fb m T 10 fb 1 5 fb = m X + m t 1 20 fb 1 Semileptonic channel ] 2 [ GeV/c m X (GeV) m X Expected exclusion Exclusion for T T! t X t X at the Tevatron Observed exclusion m 200 t =m T m X m T 2 fb mt > 365 GeV = m X + m t 5 fb 1 20 fb 1 10 fb Hadronic channel 1 Semileptonic fb1 95% C.L. [ GeV/c m T ] Cross section upper limit [fb] S. Su m T (GeV) m T (GeV)

42 ATLAS (b) Constraints: direct search ATLAS, 1.04 fb 1, ttbar+met, 1 lepton, >=4 j, + MET FIG. 2: Excluded region (under the curve) at the 95% confidence level as a function of T and A 0 masses, compared with the CDF exclusion [10, 11]. Theoretical uncertainties on the T T crosssection are not included in the limit, but the effect of these uncertainties is shown. The gray contours show the excluded crosssection times branching ratio as a function of 4the two masses. 10 ATLAS 200 ATLAS 1! L dt=1.04 fb s=7 TeV 1 150! L dt=1.04 fb s=7 TeV : (a) Transverse mass of the lepton andexpected missing Limit energy (±1") (b) ET miss after applying all selection criteria except the Obs. Limit (Theory Unc.) A 0 Mass = 10 GeV n the variable shown. MC background contributions are 50 Expected Limit (±1") ed on top of each other and normalized CDF according Exclusionto the Observed Limit driven corrections discussed in the text. The lines with 1 NNLO Spin1/2 TT Theory ±1" Excl. " $ BR(TT#ttA rrows indicate the selection criteria that define the signal 0 A 0 ) 10 NLO Scalar TT Theory ±1" n (m T > GeV 350and 400 ET miss > GeV). 500 Other 550Back nds includes both multijet backgrounds and T Mass Z+jets, [GeV] T Mass [GeV] e top and diboson production. Expectations from two l mass points are stacked separately on top of the SM ATLAS, FIG. ground. 2: Excluded The last bin region includes (under the the overflow. curve) at the 95% confifigdence level as a function of T and A 0 masses, compared with level versus T mass for an A 0 mass of 10 GeV. 3: Crosssection times branching ratio excluded at the mt > 420 GeV for 95% mx<10 confidence GeV the CDF exclusion [10, 11]. Theoretical uncertainties on thetheoretical predictions for both spin 1 and scalar T pair production are also shown. 2 T T crosssection are not included in mt the > limit, 370 but GeV the effect for mx<140 GeV of cethese leveluncertainties for S. Su a T mass is of shown. 420 (370) The gray GeVcontours and anshow A 0 the 24 sexcluded of 10 (140) crosssection GeV. The timestimated branching acceptance ratio as a function times of iency the two formasses. spin 1 T T models is consistent within sys like objects decaying to a top quark and a heavy neu Mass [GeV] A 0 m(t)m(a 0 ) < m(t) 3pb 2pb 1.5pb 1pb A 0 A 0 ) [pb] BR(TT#tt " $

43 WIMP m WIMP m weak g weak 2 S. Su 25

44 WIMP m WIMP m weak g weak 2 WIMPLESS Ω X 1 σv m2 X g 4 X follow WIMP relation S. Su 25

45 WIMP m WIMP m weak g weak 2 WIMPLESS Ω X 1 σv m2 X g 4 X follow WIMP relation Not follow WIMP relation, DM interaction << Weak interaction. Possible? S. Su 25

46 WIMP m WIMP m weak g weak 2 WIMPLESS Ω X 1 σv m2 X g 4 X follow WIMP relation Not follow WIMP relation, DM interaction << Weak interaction. Possible? superwimp S. Su 25

47 SuperWIMP / Extremely WIMP Not follow WIMP relation, DM interaction << Weak interaction. Possible? CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting (much weaker than weak interaction) S. Su 26

48 Nonthermal production: WIMP decay WIMP superwimp + SM particles Feng, Rajaraman, Takayama (2003); Bi, Li, Zhang (2003); 3487<"F;((M(" Ellis, Olive, Santoso, Spanos (2003); Wang, Yang (2004); $9>"=<"9<9=?L Feng, Su, Takayama (2004); Buchmuller, hamaguchi, Ratz, Yanagida (2004); Roszkowski, Ruiz de Austri, Choi (2004); Brandeburg, Covi, hamaguchi, Roszkowski, Steffen (2005);... Feng, ARAA (2010) superwimp e.g. Gravitino LSP LH9>">B()"C(I=@" LKK graviton >$"<9:(;3487< axino WIMP! 7?+ N! neutral 3O P"&Q O R&Q S < charged S. Su 27

49 Nonthermal production: WIMP decay WIMP superwimp + SM particles Feng, Rajaraman, Takayama (2003); Bi, Li, Zhang (2003); 3487<"F;((M(" Ellis, Olive, Santoso, Spanos (2003); Wang, Yang (2004); $9>"=<"9<9=?L Feng, Su, Takayama (2004); Buchmuller, hamaguchi, Ratz, Yanagida (2004); Roszkowski, Ruiz de Austri, Choi (2004); Brandeburg, Covi, hamaguchi, Roszkowski, Steffen (2005);... Feng, ARAA (2010) superwimp e.g. Gravitino LSP LH9>">B()"C(I=@" LKK graviton >$"<9:(;3487< axino WIMP! 7?+ N! neutral 3O P"&Q O R&Q S < charged S. Su 27

50 Nonthermal production: WIMP decay WIMP superwimp + SM particles Feng, Rajaraman, Takayama (2003); Bi, Li, Zhang (2003); 3487<"F;((M(" Ellis, Olive, Santoso, Spanos (2003); Wang, Yang (2004); $9>"=<"9<9=?L Feng, Su, Takayama (2004); Buchmuller, hamaguchi, Ratz, Yanagida (2004); Roszkowski, Ruiz de Austri, Choi (2004); Brandeburg, Covi, hamaguchi, Roszkowski, Steffen (2005);... Feng, ARAA (2010) superwimp e.g. Gravitino LSP LH9>">B()"C(I=@" LKK graviton >$"<9:(;3487< axino WIMP! 7?+ N! neutral 3O P"&Q O R&Q S < charged S. Su 27

51 Nonthermal production: WIMP decay WIMP superwimp + SM particles 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);... superwimp e.g. Gravitino LSP LKK graviton axino WIMP neutral charged S. Su 27

52 superwimp in SUSY Feng, Rajaraman, Takayama (2003); J. Feng, SS, F. Takayama (2004) SUSY case WIMP superwimp + SM particles Charged slepton Superpartner of lepton Gravitino Superpartner of graviton superwimp EM, had. cascade WIMP 1 m pl change CMB spectrum change light element SM particle abundance predicted Decay lifetime m pl2 /m 3 G ~ by BBN Strong constraints! S. Su 28

53 Neutralino LSP vs. gravitino LSP WIMP SuperWIMP G ~ χ, ~ ~ l WIMP χ, ~ ~ l LSP (DM) WIMP (DM) LSP G ~ S. Su 29

54 stau NLSP fix Ω~ G = GeV δm GeV m ~ G 200 GeV δm solve 7 Li anomaly S. Su J. Feng, SS, F. Takayama 30(2004)

55 NLSP NLSP NLSP NLSP NLSP S. Su 31

56 SM ~ G SM ~ G SM ~ G SM ~ G SM ~ G S. Su 31

57 Decay life time SM particle energy/angular distribution m~ G m pl SM ~ G SM ~ G SM ~ G SM ~ G SM ~ G S. Su 31

58 Decay life time SM particle energy/angular distribution m~ G m pl SM ~ G SM ~ G SM ~ G Probes gravity in a particle physics experiments! BBN, CMB in the lab SM ~ G SM ~ G Precise test of supergravity: gravitino is a graviton partner S. Su 31

59 Conclusion dark matter candidates naturally obtain relic density WIMP, WIMPless, superwimp,... WIMPless miracle: hidden sector dark matter with m X/gX 2 ~ mweak/gweak 2 with connector fields, allow DMSM interactions direct detection: light dark matter, IVDM,... collider signatures: 4th generation quarks, T, B superwimp: WIMP superwimp + SM particles S. Su 32