Big-Bang Nucleosynthesis (BBN) & Supersymmetric Model with Heavy Sfermions

Transcription

1 Big-Bang Nucleosynthesis (BBN) & Supersymmetric Model with Heavy Sfermions Takeo Moroi (Tokyo) Helsinki ( )

2 1. Introduction & Outline

3 Today, I discuss: BBN constraints on the decaying gravitino (with observational data as well as calculation being updated) A suggested SUSY scenario, and DM (i.e., Wino) Outline 1. Introduction & Outline 2. BBN and Gravitino 3. Suggestion to SUSY Breaking 4. Wino DM 5. A New LHC Signal 6. Summary

4 2. BBN and Gravitino [Kawasaki, Kohri, TM & Takaesu, arxiv: ]

5 BBN is an important check point in cosmology D/H = (2.53 ± 0.04) 10 5 [Cooke et al. ( 14)] 3 He/D < [Geiss & Gloeckler ( 03)] Y BBN = ± [Aver, Olive & Skillman, ( 15)] Cf.: Y BBN = ± [Izotov, Thuan & Guseva ( 14)] In our old study in 05: D/H = ( ) 10 5 Y BBN = ±

6 Standard BBN occurs at t sec 7Be ( α, γ ) 6 Li 7 Li (D, p) 3 He 4 He p (H) (n, γ ) D T ( αγ, ) n If the n/p ratio is changed after the neutron freeze-out, 4 He abundance is affected With the dissociations of 4 He, D and 3 He are produced Dissociations of D and 3 He may be also important

7 We consider long-lived particle X X Important quantities 1. Lifetime τ X 2. Primordial abundance (yield) Y X [ nx s ] t τ X 3. Spectra of decay products dn i de i with i = SM particles (gluon, photon, quarks, )

8 We have studied the BBN with long-lived particle X 1. We adopt the most recent observational constraints on the light element abundances 2. We updated the reaction rates of the standard BBN processes [Serpico et al. ( 04); NACRE Collaboration ( 13); ] 3. Evolution of hadronic shower is studied in more detail p n interconversion via inelastic scatterings Hadronic shower induced by anti-nucleons 4. Energy spectra of hadrons from the hadronization are calculated with PYTHIA 8.2 package

9 Hadronic processes in our analysis (1) & : Energetic nucleons

10 Hadronic processes in our analysis (2)

11 Upper bound on the yield variable (for m X = 1 TeV) Y X [n X /s] t τx

12 Unstable gravitino may affect the light-element abundances [Weinberg ( 82); Ellis, Kim & Nanopoulos ( 84); Khlopov & Linde ( 84); Lindley ( 85); Ellis, Nanopoulos & Sarkar ( 85); Ellis, Gelmini, Lopez, Nanopoulos & Sarkar ( 90); Kawasaki & TM ( 95); Jedamzik ( 00); Cyburt, Ellis, Fields & Olive ( 03); Kawasaki, Kohri & TM ( 05); ] Interaction of gravitino is Planck suppressed Mpl g~ Mpl q ψ μ ψ μ g q~ Gravitinos produced after inflation may decay during or after the BBN epoch τ 3/2 (ψ µ g + g) 50 sec ( ) m3/ TeV

13 Gravitino production after inflation Gravitino production rate σ prod v rel α gauge M 2 Pl Γ prod σ prod v rel T 3 Yield variable (s: entropy density) Y 3/2 n 3/2 s Γ prod H 1 α gauget R M Pl Result of the detailed calculation (for M i m 3/2 ) [with σ prod v rel by Bolz, Brandenburg & Buchmuller; Pradler & Steffen] n 3/2 s ( T R GeV ) with T R ( ) 10 1/4 g π 2M PlΓ 2 2 Φ The gravitino abundance is proportional to the reheating temperature T R

14 Gravitino decay produces lots of hadrons (p, p, n, n, π, ) 1. Produced hadrons affects the n/p ratio 4 He may be overproduced 2. Emitted hadrons induce hadronic shower Energetic nucleons in the shower cause hadrodissociation of 4 He, resulting in overproduction of D At high enough temperature, nucleons are stopped by scattering off CMB 3. Energetic photons induce photodissociation processes Gravitino decay is studied with viable MSSM mass spectrum MadGraph5 amc@nlo v2.1 PYTHIA 8.2

15 95 % C.L. upper bound on T R with decaying gravitino Sfermions are assumed to be heavier than gravitino ΩLSP 4 He 4 He (ITG) 4 He 4 He (ITG) 3 He / D D M1 = 0.9 TeV M2 = 0.5 TeV M3 = 2.0 TeV D M1 = 1.4 TeV M2 = 1.0 TeV M3 = 3.0 TeV [Kawasaki, Kohri, TM, Takaesu] m 3/2 > 10 TeV & T R > 10 9 GeV seems interesting

16 3. Suggestion to SUSY Breaking

17 m > 3/2 10 TeV & T > R 10 9 GeV The Leptogenesis scenario requires T > R 10 9 GeV [See, for example, Buchmuller, Di Bari & Plumacher ( 02); Giudice, Notari, Raidal, Riotto & Strumia ( 03)] Observed Higgs mass suggests stop masses of O( ) TeV [GeV] m h tanβ = 10 tanβ = 5 tanβ = 4 tanβ = 3 tanβ = 2.5 M S [TeV] 3 10

18 A natural scenario: Pure gravity mediation (PGM) [Ibe, TM & Yanagida; Ibe & Yanagida; Arkani-Hamed et al.] MSSM D = 6 Kahler interaction Sfermions SUSY breaking sector (No singlet) Giudice-Masiero Anomaly mediation Higgsinos Gauginos Mass spectrum Masses of gravitino, sfermions, and Higgsinos are of O(10) TeV Gaugino masses are from anomaly-mediation, and are O(100 GeV 1 TeV) [Giudice, Luty, Murayama & Rattazzi; Randall & Sundrum]

19 Gaugino masses in the PGM model M 1 g2 1 16π 2 M 2 g2 2 16π 2 M 3 g2 3 16π 2 ( 11m3/2 + L ) ( m3/2 + L ) ( 3m3/2 ) m 2 A L µ sin 2β µ 2 m 2 A ln µ2 m 2 A Wino (gaugino for SU(2) L ) is likely to be the LSP Sfermions and Higgsinos are extremely heavy (so we give up naturalness)

20 4. Wino DM

21 Thermal relic abundance of Wino Annihilation cross section of Wino is sizable Ω (Wino) [Hisano, Matsumoto, Nagai, Nojiri & Saito] Perturbative Non perturbative Ω (thermal) W 0 Ω c, if m W 3 TeV Wino Mass (TeV) [Hisano, Matsumoto, Nagai, Nojiri & Saito] If Bino is the LSP, Ω (thermal) B Ω c in PGM (as far as µ M 1 ) Bino DM is unlikely

22 The Wino is also produced by the gravitino decay [Giudice, Luty, Murayama & Rattazzi] Ω W = Ω c is realized with a relevant value of T R [TM, Nagai & Takimoto] If m 3/2 O(10 100) TeV, the gravitino decays after the Wino freezes out

23 Approximated formula for Ω W (for small enough m 3/2 ) [TM, Nagai & Takimoto] Ω W Ω (thermal) W Ω c ( mlsp 1 TeV ) ( T R 10 9 GeV ) Wino can be dark matter even if Ω (thermal) W Ω c T R O(10 9 ) GeV is needed, if m W 1 TeV Such a scenario is consistent with (simple) leptogenesis Leptogenesis requires T R > 10 9 GeV to make enough amount of baryon number [See, for example, Buchmuller, Di Bari & Plumacher]

24 Wino annihilates via s-wave process W 0 W 0 W + W Winos annihilate even after the freeze-out Sizable amount of energetic particles are produced Energetic particles are produced Check points: BBN p in the cosmic ray γ-ray from dwarf spheroidal galaxies (dsphs)

25 Effects on BBN: upper bound on σv DM+DM W + +W [Jedamzik ( 04); Hisano, Kawasaki, Kohri & Nakayama ( 09); Kawasaki, Kohri, TM, Takaesu ( 15)] 4 He Excluded D Wino annihilation cross section 320 GeV < m W < 2.3 TeV or m W > 2.5 TeV [Kawasaki, Kohri, TM, Takaesu ]

26 Effects on the fluxes of cosmic rays [Hamaguchi, TM, Nakayama ( 15)] [Ibe, Matsumoto, Shirai, Yanagida ( 15)] Signal only Background AMS-02 ( 15) M = 2.9 TeV M = 1.7 TeV Anti-proton flux from the Wino annihilation is consistent with the AMS-02 result [Hamaguchi, TM & Nakayama ( 15); Ibe, Matsumoto, Shirai & Yanagida ( 15)] γ-ray flux from dsph is an important check point

27 Bounds on the Wino mass (assuming Wino DM) BBN : 320 GeV < m < W 2.3 TeV or m > W 2.5 TeV Anti-proton : 230 GeV < m < W 2.2 TeV or m > W 2.5 TeV γ from dsph : 440 GeV < m < W 2.1 TeV or m > W 2.6 TeV # [Bhattacherjee et al. ( 15)] LHC : m W > 430 GeV [ATLAS-CONF ] # A more stringent bound is claimed by Magic+Fermi [Magic + Fermi-LAT ] They assume NFW DM distribution in dsphs Wino DM based on PGM seems an attractive possibility

28 5. A New LHC Signal [Ito, Jinnouchi, TM, Nagata & Otono, arxiv: ]

29 Hereafter, we consider SUSY models with: Gluino mass is a few TeV Sfermion masses are O(100) TeV or higher Decay length of the gluino may become relatively long _ q ~ g q cτ g 200 µm ( m q 10 3 TeV ~ q ) 4 ( 2 TeV m g Displaced vertices (DVs) in gluino events ) 5 W ~

30 Vertex resolution of the ATLAS detector Each jet contains many charged tracks The primary vertex is estimated as a point nearest to all the tracks Resolution x resolution [μm] Our modeling ATLAS (Data) ATLAS (MC) z resolution [μm] Our modeling ATLAS (Data) ATLAS (MC) Number of Tracks Number of Tracks

31 DV information can be used for gluino search Jet Jet Proton New Particle R12 Proton New Particle Jet Jet Each signal events should have two DVs We can use the distance of the DVs R 12 as a discrimination parameter

32 Our proposal: Use DV information on top of standard cuts Jet Jet Proton? R12 Proton Jet Jet Use leading 4 jets Assume two of the jets originate from a vertex V 1, while other two are from a vertex V 2 Find the best pairings of the jets and the best-fit points of vertices (to minimize χ 2 )

33 Reconstructed R 12 r 1 r 2 distribution for various cτ g Arbitrary units / 10 μm μm 50 μm 100 μm 200 μm Background r DV1 -r DV2 [μm] Results of MC simulation ATLAS DV search algorithm is adopted

34 We performed MC with the cuts [Meff-4j-2600] E (miss) T > 250 GeV, p T (j 1 ) > 200 GeV and p T (j 4 ) > 150 GeV ϕ(j 1,2,3,4, E (miss) T ) min > 0.4 Aplanarity larger than 0.04 E (miss) T /m eff (4) > 0.2 m eff (4): scalar sum of E (miss) T of leading 4-jets and the transverse momenta m eff (incl.) > 2600 GeV m eff (incl.): scalar sum of E (miss) T of jets with p T > 50 GeV and the transverse momenta Using ATLAS DV search algorithm to identify the decay vertices of gluinos, we calculate R 12

35 Discovery reach with the current data We concentrate on the signal region Meff-4j-2600 For each cτ g, we optimize r cut to maximize the significance of discovery [GeV] m g ~ Observed 95% CL limits With new selection cut -1 13TeV, 13.3 fb ATLAS gluino searches Displaced vertices (PRD92, ; 8 TeV, 20.3 fb -1 Pixel de/dx (PRD93, ; 13 TeV, 3.2 fb ) -1 Prompt (ATLAS-CONF ; 13TeV, 13.3 fb ) -1 ) cτ g ~ 10 6 [μm]

36 Discovery reach (future prospects) [GeV] m g ~ Expected 5σ discovery reach and 95% CL limits fb fb fb fb cτ g ~ 10 6 [μm] The reach may improve a few hundred GeV, if we use the DV information

37 6. Summary

38 Today, I discussed: Updated BBN constraints on decaying gravitino Cosmology with Wino DM A new LHC signal (sub-millimeter DVs) Wino DM is interesting because: Wino LSP is suggested in PGM SUSY breaking scenario T R O(10 9 ) GeV is suggested (if m W consistent with leptogenesis < 3 TeV), which is New LHC signals (based on DVs) may exist

39 Back Up

40 Deuterium D/H is inferred from D absorption in damped Lyα systems (DLAs) Observer (us) Cloud QSO E (n) H α2 2n m e m p vs. E (n) D α2 2n 2 ( 1 me + 1 ) 1 m D E(n) H E (n) D E (n) H δv 80 km/sec

41 Observation of DLA toward QSO SDSS J [Cooke et al., Astrophys.J. 781 (2014) 31]

42 Primordial abundance of D D/H = (2.53 ± 0.04) 10 5 [Cooke et al., Astrophys.J. 781 (2014) 31]

43 Helium-4 4 He abundance is inferred from observation of emission lines from extra galactic HII regions 0.28 Final Dataset Y Y p Y p = / d(y)/d(o/h) = 79 +/ O/H x 10 5 Y BBN = ± [Aver, Olive & Skillman, JCAP 1507 (2015) 011] Y BBN = ± [Izotov, Thuan & Guseva, MNRAS 445 ( 14) 778]

44 Lithium-7 7 Li has been observed in Pop-II old halo stars [Li] = Log ( 7 10 Li / H ) + 12 [Bonifacio and Malaro, MNRAS 285 (1997) 847] In stars with high surface temperature, 7 Li abundance was though to be almost constant (Spike plateau)

45 Currently, the situation is more controversial about 7 Li ( 7 Li/H) is not constant in stars with very low metallicity Asplund et al. ( 06) Aoki et al. ( 09) Gonzarez Hernandez et al. ( 08) Sbordone et al. ( 10) [Fe/H] log 10 (Fe/H) (Fe/H) [Sbordone et al., Astron.Astrophys. 522 (2010) A26] We do not use 7 Li to test BBN

46 Flow-chart of our analysis Decay of exotic particle Hadronic Partons (quarks, gluon) Radiative Photon / Charged leptons Hadronization Mesons Energetic Hadrons p, n, p, n Energy-loss Energy-loss Decay Hadronic Shower Electromagnetic Shower Hadro-Dissociation Photo-Dissociation p n Interconversion 4He Destruction D, 3He, 6 Li, 7Li Destruction D, 3He, 6Li, 7Li Production

47 Bound on the reheating temperature for leptogenesis [Giudice, Notari, Raidal, Riotto & Strumia ] SM MSSM TRH in GeV allowed TRH in GeV allowed m N1 in GeV m N1 in GeV

48 dsph constraint on Wino DM from Magic + Fermi /s] 3 [cm 95% <σ v> UL W W All dsphs [Fermi + Magic] H 0 H 0 H 0 median 68% containment 95% containment Fermi-LAT+MAGIC Segue 1 MAGIC Segue 1 Fermi-LAT Thermal relic cross section m DM [GeV]) 5 [Magic + Fermi-LAT ] They combine the constraints from (15 + 1) dsph samples They assume NFW DM distribution in dsphs

49 The fraction of events with R 12 > r cut Fraction of events μm 50 μm 100 μm 200 μm Background r cut [μm] The signal may be distinguished from the background, if cτ g > 100 µm