Dark matter, Neutrino masses in MSSM after sattelite experiments

Transcription

1 Dark matter, Neutrino masses in MSSM after sattelite experiments Ts. Enkhbat (NTU) 2 nd International Workshop on Dark Matter, Dark Energy and Matter-Antimatter Asymmetry Based on: arxiv: B. Bajc, Ts. E, D. K. Ghosh, G. Senjanovic, Y. Zhang

2 Outline Introduction: Evidences for Dark matter Decaying gravitino as the MSSM dark matter Simple case Pamela and Fermi-LAT vs MSSM Phenomenological and cosmological implications Conclusions

3 Introduction: Energy content of the Universe E. Komatsu et al, 7-year WMAP result,

4 Missing Mass Problem: Fritz Zwicky, Coma cluster, 1933 ~10 to 100 times more masses are required to explain rotation curve Text Vera Rubin & Kent Ford, ~60 spheroidal galaxies, 1970s 90% of the mass is unaccounted for by visible matter

5 Gravitational lensing Hubble Space Telescope, Abell1689, 2003 ~2mln light years(l.y.) wide at 2.2bln l.y. distance Embedding of Dark matter to explain the lensing (in purple)

6 Bullet cluster: Center of visible matter is more then 8 σ off from the mass center from lensing D. Clowe et al, Chandra X-ray, 2006 MACS J cluster Hubble ST,

7 Direct searches: DAMA/LIBRA (Beijing-Rome-Frascati)- 8.9 σ signal of annual modulation R. Bernabei et al, arxiv: CDMSII(Berkley) - 2events (consistent with background) Z. Ahmed et al, arxiv: CoGent- 100 s of events at very low energy C. E. Aalseth et al, arxiv: These can be compatible with dark matter particle 5-10GeV and See for exampe A. L. Fitzpatrick et al, arxiv: XENON10- null result and others. J. Angle et al, arxiv: XENON10 threshold might have been overestimated and, if true, could rule out CoGent. XENON100 could resolve the issue P. Sorensen, arxiv:

8 MSSM & Satellite experiments 8

9 Virtues of the MSSM The MSSM* is the main extension of the SM

10 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy

11 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings

12 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate

13 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide

14 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV

15 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008]

16 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008] Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985]

17 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008] Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985] Inflation along the same flat directions [Allahverdi, 2006]

18 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008] Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985] Inflation along the same flat directions [Allahverdi, 2006] *Here we define the MSSM as supersymmetrization of the SM + gravitino

19 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008] Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985] Inflation along the same flat directions [Allahverdi, 2006] *Here we define the MSSM as supersymmetrization of the SM + gravitino The last item is the topic of the present talk:

20 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008] Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985] Inflation along the same flat directions [Allahverdi, 2006] *Here we define the MSSM as supersymmetrization of the SM + gravitino The last item is the topic of the present talk: The dark matter candidate in light of recent Sattillete experiments:

21 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008] Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985] Inflation along the same flat directions [Allahverdi, 2006] *Here we define the MSSM as supersymmetrization of the SM + gravitino The last item is the topic of the present talk: The dark matter candidate in light of recent Sattillete experiments:

22 Virtues of the MSSM The MSSM* is the main extension of the SM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008] Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985] Inflation along the same flat directions [Allahverdi, 2006] *Here we define the MSSM as supersymmetrization of the SM + gravitino The last item is the topic of the present talk: The dark matter candidate in light of recent Sattillete experiments:

23 Satellite experiments Pamela: 1.5 to 100GeV antiproton &positron flux PAMELA collaboration, arxiv:

24 Fermi-LAT Measures electron spectrum from 7GeV to 1TeV Fermi LAT collaboration, arxiv: ,

25 While the (anti)proton flux is consistent with the expectation (anti)electron flux is in excess. 12

26 Possible interpretations

27 Possible interpretations Astrophysical sources

28 Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT

29 Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration]

30 Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration] - Nearby pulsars

31 Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration] - Nearby pulsars e.g. D. Hooper et al, 2009; P. Blasi, 2009; S. Profumo, 2008

32 Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration] - Nearby pulsars e.g. D. Hooper et al, 2009; P. Blasi, 2009; S. Profumo, 2008 Dark Matter

33 Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration] - Nearby pulsars e.g. D. Hooper et al, 2009; P. Blasi, 2009; S. Profumo, 2008 Dark Matter - Annihilating DM

34 Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration] - Nearby pulsars e.g. D. Hooper et al, 2009; P. Blasi, 2009; S. Profumo, 2008 Dark Matter - Annihilating DM - Decaying DM

35 Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration] - Nearby pulsars e.g. D. Hooper et al, 2009; P. Blasi, 2009; S. Profumo, 2008 Dark Matter - Annihilating DM - Decaying DM A viable mechanism must induce excess leptons not hadrons.

36 MSSM & decaying gravitino In its most general form, MSSM contains W /R = 1 2 λllec + λ QLd c λ u c d c d c Nucleon decay constraint λ λ A. Y. Smirnov & F. Vissani, 1996 n n oscillation constraint λ m 300GeV 2 +µ LH 2 m q 2 m χ 1/2 100GeV 100GeV S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

37 MSSM & decaying gravitino In its most general form, MSSM contains W /R = 1 2 λllec + λ QLd c λ u c d c d c Nucleon decay constraint λ λ A. Y. Smirnov & F. Vissani, 1996 n n oscillation constraint λ m 300GeV 2 +µ LH 2 m q 2 m χ 1/2 100GeV 100GeV S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

38 MSSM & decaying gravitino In its most general form, MSSM contains W /R = 1 2 λllec + λ QLd c λ u c d c d c Nucleon decay constraint λ λ A. Y. Smirnov & F. Vissani, 1996 n n oscillation constraint λ m 300GeV 2 +µ LH 2 m q 2 m χ 1/2 100GeV 100GeV S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

39 MSSM & decaying gravitino In its most general form, MSSM contains W /R = 1 2 λllec + λ QLd c λ u c d c d c Nucleon decay constraint λ λ A. Y. Smirnov & F. Vissani, 1996 n n oscillation constraint λ m 300GeV 2 +µ LH 2 m q 2 m χ 1/2 100GeV 100GeV S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

40 MSSM & decaying gravitino In its most general form, MSSM contains W /R = 1 2 λllec + λ QLd c λ u c d c d c Nucleon decay constraint λ λ A. Y. Smirnov & F. Vissani, 1996 n n oscillation constraint λ m 300GeV 2 +µ LH 2 m q 2 m χ 1/2 100GeV 100GeV S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

41 MSSM & decaying gravitino In its most general form, MSSM contains W /R = 1 2 λllec + λ QLd c λ u c d c d c Nucleon decay constraint λ λ A. Y. Smirnov & F. Vissani, 1996 n n oscillation constraint λ m 300GeV 2 +µ LH 2 m q 2 m χ 1/2 100GeV 100GeV S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

42 MSSM & decaying gravitino In its most general form, MSSM contains W /R = 1 2 λllec + λ QLd c λ u c d c d c Nucleon decay constraint λ λ A. Y. Smirnov & F. Vissani, 1996 n n oscillation constraint λ m 300GeV 2 +µ LH 2 m q 2 m χ 1/2 100GeV 100GeV S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

43 m ν Neutrino masses λ 2 m 2 m τ 3λ 2 m 2 LR 16π 2 m 2 ; 16π 2 m 2 LR m τ ; g2 < ν > m χ λ (or λ ) dominates : λ 10 3 m mν 1/2 m 2 LR 1TeV 1eV (100GeV) dominates : It is a seesaw mechanism with the gaugino playing the role of the right handed neutrinos.

44 The size of the neutrino masses τ χ 0 LSP O(1)sec

45 The size of the neutrino masses τ χ 0 LSP O(1)sec

46 The size of the neutrino masses Large values for RPV couplings τ χ 0 LSP O(1)sec

47 The size of the neutrino masses Large values for RPV couplings τ χ 0 LSP O(1)sec

48 The size of the neutrino masses Large values for RPV couplings τ χ 0 LSP O(1)sec: Neutralinos cannot be DM!

49 The size of the neutrino masses Large values for RPV couplings τ χ 0 LSP O(1)sec: Neutralinos cannot be DM!

50 The size of the neutrino masses Large values for RPV couplings τ χ 0 LSP O(1)sec : Neutralinos cannot be DM! The only viable candidate for DM is the Gravitino!

51 Gravitino decays Relevant gravitino interactions in SUGRA L = 1 χ L γ µ γ n ud ν φ 2MPl i 4 λ a γ µ σ νρ Fνρ a ψ µ + h.c. 2 L eff Effective 2&3-body decay operators 2 body = iλ m 2 LR 96π 2 m 2 M Pl g 2 νp Rγ µ σ νρ W 3νρ g νp R γ µ σ νρ B νρ + P R γ µ σ νρ Wνρ ψ µ body = λ L PR γ 2m 2 M µ γ ν ψ µ LPR e + Pl L eff ē P L γ µ γ ν ψ µ Lc P L L + h.c.

52 Mass ranges Gravitino decay modes m 3/2 >m h 0 m 3/2 >M W ±,Z 0 m 3/2 >m hadrons m 3/2 >m + m m 3/2 < 2m e h 0 + ν W ± +,Z 0 + ν q + q + /ν + + /ν γ + ν

53 Photon & Neutrino mode If neutrino mass is dominated by sneutrino VEV m3/2 Γ (ψ γν) 1 32π m ν m γ m 3 3/2 M 2 Pl Takayama & Yamaguchi, GeV 5GeV 3 1TeV m γ Monochromatic photons and neutrinos No such signal observed by Fermi-LAT Γ 3/ GeV or m 3/2 5GeV This case cannot explain PAMELA or Fermi-LAT!

54 2 & 3-body decay rates Γ ψ W ± g2 λ π 5 2 m 2 LR m 4 m 3 3/2 M 2 Pl Γ ψ Z 0 ν 1 2 cos 2 θ W Γ ψ W ± Γ ψ h 0 ν m2 3/2 864M 2 W Γ ψ W ± Γ ψ + ν λ π 3 m 4 3/2 m 4 m 3 3/2 M 2 Pl

55 2&3-body diagrams Neutrino channels

56 Charged lepton channels Higgs channels Three-body decay channels

57 Criteria to fit neutrino mass and PAMELA and/or Fermi-LAT 0.03eV m ν 0.3eV GeV Γ GeV Γ 2 Γ 3 /10 λ 2 4π (ν mass) (PAMELA/Fermi-LAT) (leptophilic DM) (perturbativity bound)

58 The lower and upper bound on the slepton mass m 600TeV m 2 3/2 400GeV 5/2 mν 0.1eV 1/2 Γ GeV λ m /4 m 2 5/2 1/4 3/2 Γ 3 TeV 4π 400GeV GeV The upper limit on the gravitino mass m3/2 3TeV m 2 3/2 3TeV 2 1/4 λ 2 4π 1/3 mν 3/2 Γ 3 0.1eV GeV 1/3 this leaves narrow range for gravitino mass An optimal fit for Fermi-LAT for

59 Allowed region compatible with PAMELA m GeV, m slepton 2 LR 200GeV 2 Log 10 Λ Br Μ 3e Br Μ 3e Log 10 m slepton TeV The dashed line is the perturbativity bound. Blue (red) region is excluded by the gravitino (neutrino) mass. 25

60 Allowed region for Fermi-LAT m TeV, m slepton 2 LR 2.5 TeV Log 10 Λ Log 10 m slepton TeV The dashed line is the perturbativity bound

61 The fit for PAMELA only m 3/2 = 400GeV, τ 3/2 = sec, (Γ 3 = GeV), m ν =0.2eV

62 The allowed region in the plane (for PAMELA) 9 Log 10 m slepton GeV Λ 2 4Π 4 M Ν 0.03eV and GeV Log m GeV Br Μ 3e PAMELA excl.

63 The simultaneous fit for PAMELA positron excess and Fermi-LAT due to 3-body gravitino decay Fit for PAMELA m 3/2 =3.3TeV, τ 3/2 = sec, (Γ 3 = GeV), m ν =0.03eV

64 The fit for Fermi-LAT m 3/2 =3.3TeV, τ 3/2 = sec, (Γ 3 = GeV), m ν =0.03eV

65 Phenomenological consequences There is no LHC signatures if both PAMELA and Fermi-LAT are to be explained by gravitino decay: Phenomenologically interesting case is if gravitino is behind PAMELA only Gaugino NLSP: Γ χ 0 + ν = g2 λ π 3 m 5 χ0 m 4 = 6g2 M 2 Pl m5 χ 0 m 7 3/2 τ χ 0 m 10 7 χ 0 5 sec d χ 0 600GeV 30meters for m 3/2 = 400GeV, Γ 3 = GeV Sizable amount decays inside detector. If charged wino is NLSP, leave highly ionized tracks.

66 Light slepton with Γ NLSP = λ2 1m NLSP 8π If charged If sneutrino GeV mnlsp 5 m3/ GeV 400GeV Displaced vertex /ionizing track, dilepton+ 2 charged lepton final states Light slepton (with vanishing RPV coupling) as NLSP Γ 1 + ν g4 λ 2 m π 5 m 2 χ m M Pl 2 m 1 m 2 χ 0 0 m 2 τ χ sec 1 m χ 0 600GeV 1TeV m 3/2 In this case the NLSP decays outside the detector 7 Γ 3/2

67 Conclusions The MSSM even if taken as the theory of the neutrino masses it explain PAMELA excess. The sleptons are heavy with masses in the range 500 to 10^6 TeV The gravitino mass can be as light as 300 GeV Phenomenologically there is no constraint on the squark masses The Fermi-LAT data can be explaind only if the gravitino is around 3TeV. Perturbativity pushes the gravitino to lighter values. The decaying gravitino as the explanation of Fermi-LAT will kill any chance of MSSM being in the LHC range If direct searches are confirmed, would rule out gravitino DM