Dark matter and missing energy - what is there apart from SUSY?

Transcription

1 Dark matter and missing energy - what is there apart from SUSY? Koichi Hamaguchi (Tokyo U.) at LHC New Physics Forum, Heidelberg, February 09

2 long-lived charged particle { Dark matter and missing energy - what is there apart from SUSY? Koichi Hamaguchi (Tokyo U.) standard at LHC New Physics Forum, Heidelberg, February 09

3 long-lived charged particle { Dark matter and missing energy - what is there apart from SUSY? Koichi Hamaguchi (Tokyo U.) standard at LHC New Physics Forum, Heidelberg, February 09 based on... S.Asai, KH, S.Shirai, arxiv: today!!

4 Suppose that we will see long-lived charged massive particle at the LHC, e.g., stau NLSP in SUSY models. τ τ If its lifetime is long (> 1 sec), can we see its decay??

5 Suppose that we will see long-lived charged massive particle at the LHC, e.g., stau NLSP in SUSY models. τ τ If its lifetime is long (> 1 sec), can we see its decay?? Yes! with additional stoppers. KH, Kuno, Nakaya, Nojiri, 04 Feng, Smith, 04 KH, Nojiri, De Roeck, 06

6 Suppose that we will see long-lived charged massive particle at the LHC, e.g., stau NLSP in SUSY models. τ τ If its lifetime is long (> 1 sec), can we see its decay?? Yes! with additional stoppers. KH, Kuno, Nakaya, Nojiri, 04 Feng, Smith, 04 KH, Nojiri, De Roeck, 06 Yes! without additional material. Asai, KH, Shirai, 09

7 Suppose that we will see long-lived charged massive particle at the LHC, e.g., stau NLSP in SUSY models. τ τ If its lifetime is long (> 1 sec), can we see its decay?? Yes! with additional stoppers. KH, Kuno, Nakaya, Nojiri, 04 Feng, Smith, 04 KH, Nojiri, De Roeck, 06 Yes! without additional material. Asai, KH, Shirai, 09 this talk

8 before presenting our proposal,... Motivation --- why long-lived charged particle?? --- why its lifetime is so important??

9 before presenting our proposal,... Motivation --- why long-lived charged particle?? --- why its lifetime is so important?? (1) Li7 problem in Big-Bang Nucleosynthesis ( model independent)

10 before presenting our proposal,... Motivation --- why long-lived charged particle?? --- why its lifetime is so important?? (1) Li7 problem in Big-Bang Nucleosynthesis ( model independent) (2) SUSY models with gravitino LSP

11 Motivation (1) Li7 problem in Big-Bang Nucleosynthesis ( model independent)

12 Fig. from Review of Particle Physics

13 If there is a long-lived charged particle... affects the BBN!! 1. decay s effect 2. catalysis effect Fig. from Review of Particle Physics

14 If there is a long-lived charged particle... affects the BBN!! 1. decay s effect 2. catalysis effect Fig. from Review of Particle Physics

15 Catalyzed BBN (CBBN) Pospelov 06 If there were negatively charged particle, X - at BBN,... bound states with positively charged nuclei. new catalyzed reactions occur!

16 Catalyzed BBN (CBBN) Pospelov 06 If there were negatively charged particle, X - at BBN,... bound states with positively charged nuclei. new catalyzed reactions occur! (1) strong constraints on X lifetime and abundance. standard BBN catalyzed BBN O(10 9 ) enhancement!!! too much Li6!!! Pospelov 06;...; KH, Hatsuda, Kamimura, Kino, Yanagida 07

17 Catalyzed BBN (CBBN) Pospelov 06 If there were negatively charged particle, X - at BBN,... bound states with positively charged nuclei. new catalyzed reactions occur! (1) strong constraints on X lifetime and abundance. (2) there may already exist a hint of this CBBN. Li7 problem.

18 Fig. from Review of Particle Physics

19 Li-7 problem Fig. from Review of Particle Physics

20 recently, reanalyzed by Cyburt, Fields, Olive, Li-7 problem Fig. from Review of Particle Physics

21 recently, reanalyzed by Cyburt, Fields, Olive, Abstract: The Li problem remains and indeed exacerbated; the discrepancy is now 4.2σ - 5.3σ. Li-7 problem Fig. from Review of Particle Physics

22 Catalyzed BBN (CBBN) Pospelov 06 If there were negatively charged particle, X - at BBN,... bound states with positively charged nuclei. new catalyzed reactions occur! (1) strong constraints on X lifetime and abundance. (2) there may already exist a hint of this CBBN. Li7 problem.

23 Catalyzed BBN (CBBN) Pospelov 06 If there were negatively charged particle, X - at BBN,... bound states with positively charged nuclei. new catalyzed reactions occur! (1) strong constraints on X lifetime and abundance. (2) there may already exist a hint of this CBBN. Li7 problem. CBBN can solve it! ( 7 Be X - )+p ( 8 B X - )+Υ Pospelov, 06; + Bird, Koopmans, Pospelov, 07 (+ many others) + Kamimura, Kino, Hiyama, 08

24 Catalyzed BBN (CBBN) Pospelov 06 If there were negatively charged particle, X - at BBN,... bound states with positively charged nuclei. new catalyzed reactions occur! (1) strong constraints on X lifetime and abundance. (2) there may already exist a hint of this CBBN. Li7 problem. CBBN can solve it! ( 7 Be X - )+p ( 8 B X - )+Υ Pospelov, 06; + Bird, Koopmans, Pospelov, 07 (+ many others) + Kamimura, Kino, Hiyama, if X lifetime is O(1000) sec.

25 Catalyzed BBN (CBBN) Pospelov 06 If there were negatively charged particle, X - at BBN,... bound states with positively charged nuclei. new catalyzed reactions occur! (1) strong constraints on X lifetime and abundance. (2) there may already exist a hint of this CBBN. Li7 problem. CBBN can solve it! ( 7 Be X - )+p ( 8 B X - )+Υ Pospelov, 06; + Bird, Koopmans, Pospelov, 07 (+ many others) + Kamimura, Kino, Hiyama, if X lifetime is O(1000) sec. Such a long-lived charged particle naturally arises in SUSY models with gravitino LSP + stau NLSP!!

26 Motivation (2) SUSY models with gravitino LSP

27 What is Gravitino?

28 What is Gravitino?

29 What is Gravitino? Superstring 1 extremely weakly interacting

30 Compare it with Electroweak Symmetry

31 Compare it with Electroweak Symmetry

32 Compare it with Electroweak Symmetry gauge boson mass mv = g!ϕ" gauge coupling Higgs VEV gravitino mass mge = 1 3MP "F # SUGRA coupling SUSY breaking VEV

33 Why Gravitino LSP?

34 Why Gravitino LSP?... among 29 SUSY particles? squarks : ( ũl d L ) i ũ R i d R i gauginos and higgssinos : χ0 i, sleptons : χ ± i, g ( νlẽl ) i ẽ R i gravitino : G

35 Why Gravitino LSP? Dark Matter in SUSY In SUSY models + R-parity, LSP (=Lightest SUSY Particle) is stable. If neutral, Dark Matter candidate!

36 Why Gravitino LSP? Dark Matter candidates in SUSY Standard Model In SUSY Standard Model in SUGRA,... squarks : ( ũl d L ) i ũ R i d R i gauginos and higgssinos : χ0 i, sleptons : χ ± i, g ( νlẽl ) i ẽ R i gravitino : G

37 Why Gravitino LSP? Dark Matter candidates in SUSY Standard Model In SUSY Standard Model in SUGRA,... squarks : ( ũl d L ) i ũ R i d R i gauginos and higgssinos : χ0 i, sleptons : χ ± i, g ( νlẽl ) i ẽ R i gravitino : G neutral and color-singlet

38 Why Gravitino LSP? Dark Matter candidates in SUSY Standard Model In SUSY Standard Model in SUGRA,... squarks : ( ũl d L ) i ũ R i d R i gauginos and higgssinos : χ0 i, sleptons : χ ± i, g ( νlẽl ) i ẽ R i gravitino : G neutral and color-singlet excluded by direct detection experiments (cf. Falk, Olive, Srednicki, 94)

39 Why Gravitino LSP? Dark Matter candidates in SUSY Standard Model In SUSY Standard Model in SUGRA,... squarks : ( ũl d L ) i ũ R i d R i gauginos and higgssinos : χ0 i, sleptons : χ ± i, g ( νlẽl ) i ẽ R i gravitino : G neutral and color-singlet excluded by direct detection experiments (cf. Falk, Olive, Srednicki, 94) Only Neutralino and Gravitino are viable candidates!

40 Why Gravitino LSP? experimental bound naturalness Other SUSY particle masses = O(100 GeV)-O(1 TeV) Gravitino mass... model dependent. Gravitino mass ev kev MeV GeV TeV GMSB gmsb AMSB, mmsb gravity-msb

41 Why Gravitino LSP? experimental bound naturalness Other SUSY particle masses = O(100 GeV)-O(1 TeV) Gravitino mass... model dependent. Gravitino mass ev kev MeV GeV TeV GMSB gmsb AMSB, mmsb gravity-msb

42 Why Gravitino LSP? experimental bound naturalness Other SUSY particle masses = O(100 GeV)-O(1 TeV) Gravitino mass... model dependent. Gravitino mass ev kev MeV GeV TeV GMSB gmsb AMSB, mmsb gravity-msb Gravitino LSP

43 Why Gravitino LSP? experimental bound naturalness Other SUSY particle masses = O(100 GeV)-O(1 TeV) Gravitino mass... model dependent. Gravitino mass ev kev MeV GeV TeV PAMELA & ATIC? (with decaying composite DM) GMSB PAMELA & ATIC? (with decaying gravitino DM) gmsb AMSB, mmsb gravity-msb Gravitino LSP

44 Why Gravitino LSP? experimental bound naturalness Other SUSY particle masses = O(100 GeV)-O(1 TeV) Gravitino mass... model dependent. Gravitino mass ev kev MeV GeV TeV GMSB gmsb AMSB, mmsb gravity-msb Gravitino LSP

45 Why Gravitino LSP? SUSY models neutralino LSP gravitino LSP others fifty-fifty?

46 NLSP (Next-to-Lightest SUSY Particle) In Gravitino LSP scenario, the NLSP is long-lived. extremely weak interaction Lifetime e.g. for mnlsp! 200 GeV τnlsp O(day) for mge 10 GeV τnlsp O(10 min) for mge 1 GeV τnlsp O(10 sec) for mge 0.1 GeV

47 Why Stau NLSP?

48 Why Stau NLSP?... among 28 NLSP candidates? squarks : ( ũl d L ) i ũ R i d R i gauginos and higgssinos : χ0 i, sleptons : χ ± i, g ( νlẽl ) i ẽ R i stau (i=3) gravitino : G

49 Why Stau NLSP? In general, from RGE, tendency is M(color singlet) < M(colored) l sleptons q squarks typical RG evolution (from S.P.Martin, hep-ph/ ) gaugino Higgsino gluino

50 Why In Stau NLSP? general, from RGE, tendency is M(color singlet) < M(colored) M(weak singlet) < M(weak charged) typical RG evolution (from S.P.Martin, hep-ph/ )!!r!!! sleptons ν"l ""L gaugino Higgsino # gluino q! squarks

51 Why In Stau NLSP? general, from RGE, tendency is M(color singlet) < M(colored) M(weak singlet) < M(weak charged) M(3rd family) < M(1st and 2nd family) τ!1!!r!r e!r, µ!!! sleptons typical RG evolution (from S.P.Martin, hep-ph/ ) ν"l ""L gaugino Higgsino # gluino q! squarks

52 Why In Stau NLSP? general, from RGE, tendency is M(color singlet) < M(colored) M(weak singlet) < M(weak charged) M(3rd family) < M(1st and 2nd family) τ!1!!r!r e!r, µ!!! sleptons typical RG evolution (from S.P.Martin, hep-ph/ ) ν"l ""L gaugino Higgsino # gluino q! squarks In most cases, either Stau or Neutralino is the NLSP

53 Why Stau NLSP? SUSY models neutralino LSP Stau NLSP gravitino LSP Neutralino NLSP others Gravitino LSP and Stau NLSP is a natural choice.

54 Why Stau NLSP? SUSY models neutralino LSP Stau NLSP = Long-lived charged particle. gravitino LSP Neutralino NLSP others Gravitino LSP and Stau NLSP is a natural choice.

55 NLSP Lifetime Γ(τ G τ ) " m5τ 2 48πm2G Mpl! 1 m2g m2τ Lifetime (decay length) of NLSP stau mg ττ cττ ev e.g., for mτ = 100 GeV, MeV GeV kev ps mm ns m "4 μs km ms sec day

56 NLSP Lifetime Γ(τ G τ ) " m5τ 2 48πm2G Mpl! 1 m2g m2τ "4 Lifetime (decay length) of NLSP stau mg ev kev e.g., for mτ = 100 GeV, MeV GeV Lifetimeps measurement ns μs ms sec ττ mm m km scale SUSY breaking cτ τ gravitino mass mge F = day 3 mge MP

57 NLSP Lifetime Γ(τ G τ ) " m5τ 2 48πm2G Mpl! 1 m2g m2τ Lifetime (decay length) of NLSP stau mg ττ cττ ev e.g., for mτ = 100 GeV, MeV GeV kev ps mm ns m "4 μs km ms sec day

58 NLSP Lifetime Γ(τ G τ ) " m5τ 2 48πm2G Mpl! 1 m2g m2τ "4 Lifetime (decay length) of NLSP stau mg ev ττ cττ prompt decay e.g., for mτ = 100 GeV, MeV GeV kev ps mm ns m Detector Size μs ms sec day km No In-flight decay, but maybe accessible.

59 Side Remark Planck scale measurement W.Buchmüller, K.Hamaguchi, M.Ratz, T.Yanagida 04

60 Side Remark Planck scale measurement W.Buchmüller, K.Hamaguchi, M.Ratz, T.Yanagida 04

61 Side Remark Planck scale measurement W.Buchmüller, K.Hamaguchi, M.Ratz, T.Yanagida 04

62 Stop and Decay of Long-lived charged massive particles (CHAMPs) at the LHC detectors S.Asai, KH, S.Shirai, arxiv:

63 typically most of CHAMPs have large velocity and escape from detector. τ τ

64 typically most of CHAMPs have large velocity and escape from detector. some of them have sufficiently small velocity and stop at calorimeters.

65 typically most of CHAMPs have large velocity and escape from detector. some of them have sufficiently small velocity and stop at calorimeters. example of SUSY model point SPS7 ( σ SUSY = 3.5 pb ) assume: Fe 1440mm (barrel) Cu 1400mm (end-cap) stopped events about 1% of total SUSY events a few per day

66 but their late-time decay has wrong timing and wrong direction; difficult to reject backgrounds difficult to trigger.

67 but their late-time decay has wrong timing and wrong direction; difficult to reject backgrounds difficult to trigger.... during pp collision.

68 Idea: stop the pp collision!!...and optimize the trigger to detect CHAMP decay. for short lifetime: for long lifetime: use beam-damp signal. use winter shutdown.

69 for short lifetime: use beam-damp signal. (I) select the stopping event by online Event Filter. SUSY stopped!! events time

70 for short lifetime: use beam-damp signal. (I) select the stopping event by online Event Filter. (1) missing ET > 100 GeV (2) 1 jet PT > 100 GeV + 2 jets PT > 50 GeV standard SUSY cuts (3) isolated track with PT > 0.1 m(champ). (4) extrapolate the track to calorimeter and energy deposit < 0.2 p(champ). (5) extrapolate the track to muon system and no muon track. SUSY stopped!! events CHAMP candidate select stopping events time

71 for short lifetime: use beam-damp signal. (I) select the stopping event by online Event Filter. SUSY stopped!! events time

72 for short lifetime: use beam-damp signal. (I) select the stopping event by online Event Filter. (II) send a beam-damp signal, which immediately stops the pp collision. trigger beam-damp SUSY stopped!! events time

73 for short lifetime: use beam-damp signal. (I) select the stopping event by online Event Filter. (II) send a beam-damp signal, which immediately stops the pp collision. (III) change the trigger menu to the one optimized for CHAMP decay. trigger beam-damp SUSY stopped!! events change trigger menu time

74 for short lifetime: use beam-damp signal. (I) select the stopping event by online Event Filter. (II) send a beam-damp signal, which immediately stops the pp collision. (III) change the trigger menu to the one optimized for CHAMP decay. (IV) wait for CHAMP decay. trigger beam-damp SUSY stopped!! events change trigger menu time

75 Δt for short lifetime: use beam-damp signal. (I) select the stopping event by online Event Filter. (II) send a beam-damp signal, which immediately stops the pp collision. (III) change the trigger menu to the one optimized for CHAMP decay. (IV) wait for CHAMP decay. trigger beam-damp SUSY stopped!! events change trigger menu decay!! time

76 Δt for short lifetime: use beam-damp signal. (I) select the stopping event by online Event Filter. (II) send a beam-damp signal, which immediately stops the pp collision. (III) change the trigger menu to the one optimized for CHAMP decay. (IV) wait for CHAMP decay. trigger beam-damp restart pp collision SUSY stopped!! events change trigger menu decay!! SUSY events time

77 for long lifetime: use winter shutdown running (pp collision) winter shutdown stopped time

78 for long lifetime: use winter shutdown running (pp collision) winter shutdown stopped change trigger menu time

79 for long lifetime: use winter shutdown running (pp collision) winter shutdown stopped change trigger menu decay!! time

80 lifetime measurement: SUMMARY short assumption long dead time: 1 sec waiting time: 30 min. running: 200 days shutdown: 100 days O(0.1 sec years) can be probed!!

81 Summary If we will see long-lived charged massive particle at the LHC, the lifetime measurement is important both for cosmology and particle physics. The discovery of late decay, and the lifetime measurement is possible for a very wide range, from O(0.1 sec) to O(100 years)!!! Future works: study of decay products (energy? particle IDs?) what about long-lived colored particle (R-hadrons)?

82

83

84 Backup Slides

85 Suppose that we will see long-lived charged massive particle at the LHC, e.g., stau NLSP in SUSY models. τ τ

86 Suppose that we will see momentum measurement p long-lived charged massive particle at the LHC, TOF (time of flight) measurement T + NLSP e.g., stau in SUSY models. velocity β = L/T τ mass m = p/(βγ) cf. De Roeck, Ellis, Gianotti, Moortgat, Olive, Pape, 05 mτe mτe τ = p p βγ 2 t L O(1000) τ! " 10 20% mτe mτe in each event < 1% Properties of other particles can also be studied from kinematical information. then, the next target is the lifetime!!! ( Note: searches inside sea water exclude completely stable massive charged particle.)

87 What is Gravitino? Compare it with Electroweak Symmetry

88 What is Gravitino? Compare it with Electroweak Symmetry gauge boson mass mv = g!ϕ" gauge coupling Higgs VEV gravitino mass mge = 1 3MP "F # SUGRA coupling SUSY breaking VEV