Revisiting gravitino dark matter in thermal leptogenesis

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1 Revisiting gravitino dark matter in thermal leptogenesis Motoo Suzuki Institute for Cosmic Ray Research (ICRR) The University of Tokyo arxiv: JHEP1702(2017)063 In collaboration with Masahiro ibe and Tsutomu. T. Yanagida

2 R-parity R-parity is introduced for phenomenological consistency in Minimal Supersymmetric Standard Model (MSSM) R-parity charge assignment R=0 R=1 A. Prohibiting rapid proton decay B. Stable lightest SUSY particle (dark matter)

3 Do we have theoretical ground on R-parity?

4 Theoretical ground on R-parity Gravity breaks all global symmetry R-parity can be embedded into gauge symmetry e.g. U(1)B-L gauge symmetry (adding NR) B-L parity (-1) B-L accidentally introduce R-parity SO(10) U(1) B L R-parity ( 1) B L R-parity is acceptable!!

5 However

6 Theoretical ground on R-parity However this framework has tension with perturbative SO(10) GUT There are two possibilities in R-parity breaking (and neutrino mass) A. Unbroken R-parity B. Broken R-parity e.g. VEV of fields in 126 representation e.g. VEV of fields in 16 representation 126 H.16 M.16 M (16 H.16 M )(16 H.16 M ) NR mass : B-L : NR mass : B-L : Non-perturbative R-parity is broken in perturbative SO(10) GUT!!

7 Theoretical ground on R-parity However this framework has tension with perturbative SO(10) GUT There are two possibilities in R-parity breaking (and neutrino mass) A. Unbroken R-parity B. Broken R-parity e.g. VEV of fields in 126 representation e.g. VEV of fields in 16 representation 126 H.16 M.16 M (16 H.16 M )(16 H.16 M ) NR mass : B-L : NR mass : B-L : R parity is broken in perturbative SO(10) GUT!! Non-perturbative R-parity is broken in perturbative SO(10) GUT!!

8 What is dark matter candidate in R-parity violation? In the following, consider bilinear R-parity dominated case Neutralino LSP cannot be dark matter W R = µ 0 il i H u Neutralino lifetime << the age of universe ( e.g. for ) µ 0 µ 10 7 Gravitino LSP can be dark matter [ 3/2! Z,h,Wl] m 3 3/2 192 M 2 PL µ 0 µ 2 Long Lifetime 3 1TeV 10 3/2 ' µ sec >> O(10 17 sec) K. Ishiwata, S. Matsumoto, and T. Moroi (2008) m 3/2 µ 0 2 Gravitino dark matter!!

9 Consistency between gravitino dark matter and baryon asymmetry dark matter abundace 3/2 h 2 (m 3/2,m g,t R ) 0.12 Planck (2015) e.g. T R 10 9 GeV, m 3/2 m g 1 TeV g: gluon λ: gluino Ψ: gravitino Successful thermal leptogenesis occurs in following reheating temperature range 10 9 GeV. T R GeV W. Buchmuller et al. (2003) K. Kohri et al. (1999) Dark matter abundance Baryon asymmetry e.g. gluon and gluino collisions produce gravitino dark matter

10 Constraining gravitino dark matter in thermal leptogenesis

11 Collider constraints in neutralino NLSP Neutralino NLSP stable in detector : multi-jet with missing momentum search 2000 LHC constraints, neutralino NLSP 1500 m g éêgev 1000 excluded region at 95% CL ATLAS-CONF (2016) 0 1 m g é = m c é 500 m g m 3/2 excluded region êGeV m c é 1 neutralino-gluino 3/2 h 2 (m 3/2,m g,t R ) fixed TR 0.12 mass relation neutralino mass < 700 GeV is excluded!! Future LHC experiment may be able to search entire region!! neutralino-gravitino

12 Collider constraints in stau NLSP Stau NLSP stable in detector : long-lived charged particle searches excluded region Current LHC experiment exclude entire region!!

13 Conclusions R-parity can be embeded into B-L gauge symmetry However, R-parity can be broken in perturbative SO(10) GUT In R-parity violation model, gravitino is dark matter candidate Furthermote, gravitino dark matter consistent with thermal leptogenesis Future LHC may settle down this scenario; gravitino dark matter with leptogenesis If R-parity is conserved, constraints get more severe because NLSP always contributes gravitino dark matter abundance tot 3/2 h2 = 3/2 h 2 + Br 3/2 m 3/2 m NLSP NLSP h 2 =1 m g éêgev m 3ê2 = m b éhgut L T R = GeV m g é m 3ê2 W 3ê2 h 2 > m 3ê2 êgev

14 Back Up

15 Gravitino and gluino mass relation Theoretically predicted gravitino dark matter abundance 3/2 h 2 ' 0.09 m3/2 100 GeV T R GeV r 2 g m2 g r 2 g m2 g m 2 3/2 m 2 3/2 Gravitino and gluino mass relation from dark matter abundance 3/2 h 2 TR 0.12!! apple log T R GeV! m g = r g m 1/2 r g 2.5 m 3/2 m g

16 B-L parity breaking and R-parity breaking Broken B-L parity h16 H i = v B L Broken B-L parity induce Broken R parity e.g. W 16 H 16 M 10 H v B L 16 M 10 H v B L LH u Bilinear R-parity breaking!! 10H : SM higgs 16M : SM matter 16H : B-L breaking higgs ε : (small) coupling B-L parity breaking Bilinear R-parity breaking R parity is broken in perturbative SO(10) GUT!!

17 R-parity violation and its constraints R-parity violating superpotential W R = ijkd c i Q j L k B-L L 0 ijkl i E c j L c k L 00 ijkd c i U c j D c k + B + µ 0 il i H u L Constraints of baryon asymmetry Erase, 0, i, j, k : generation indices K. Hamaguchi et al. (2010) 00,µ 0 /µ < O(10 (6 7) ) Rapid proton decay 0 00 < m SUSY 1TeV 2 ( p+!e + 0 & K. Abe et al. (2011) year) R-parity violation must be small

18 What is dark matter candidate in R-parity violation? In the following, consider bilinear R-parity dominated case Neutralino LSP cannot be dark matter Neutralino lifetime << the age of universe ( e.g. for ) µ 0 µ 10 7 Gravitino LSP can be dark matter [ 3/2! Z,h,Wl] m 3 3/2 192 M 2 PL µ 0 µ 2 Long Lifetime 3 1TeV 10 3/2 ' µ sec >> O(10 17 sec) K. Ishiwata, S. Matsumoto, and T. Moroi (2008) m 3/2 µ 0 2 Gravitino dark matter!!

19 Gravitino dark matter abundance e.g. gluon and gluino collisions produce gravitino dark matter g: gluon λ: gluino Ψ: gravitino Thermally produced gravitino dark matter abundance 3/2 h 2 m3/2 T R ' GeV r! 2 g m2 g GeV m 2 3/ r 2 g m2 g m 2 3/2! apple log J. Ellis et al. (2016) T R GeV! m g = r g m 1/2

20 Assumption A. Bilinear R-parity violation µ 0 µ < TeV m 3/2 3/2 E, Carquin et.al. (2016) S. Ando and K. Ishiwata(2016) B. gravitino dark matter in thermal leptogenesis C. m3/2< 1 TeV, 10 9 GeV < TR < GeV Searching this scenario

21 Gluino mass upper bound

22 Gluino mass upper bound 3/2 h 2 TR 0.12 Latest reheating temperature upper bound in thermal leptogenesis T R GeV S. Antusch and A. M. Teixeira (2006) T R =10 9 GeV T R = GeV 2000 W 3ê2 h 2 > W 3ê2 h 2 >0.12 m g éêgev m 3ê2 = m b éhgut L allowed region m g é m 3ê2 m g éêgev m 3ê2 = m b éhgut L allowed region m g é m 3ê m 3ê2 êgev m 3ê2 êgev m g < 2 TeV m g < 1.6 TeV

23 LHC constraints

24 NLSP contribution into dark matter abundance Gravitino dark matter abundance from NLSP decay tot 3/2 h2 = 3/2 h 2 + Br 3/2 m 3/2 m NLSP NLSP h 2. conserving decay into gravitino NLSP R-parity R ' m3/2 2 1 TeV sec 100GeV m NLSP violating decay into the other SM particles R-parity R 10 NLSP ' µ 1TeV sec µ 0 m NLSP 5. R NLSP << R NLSP NLSP contribution is neglibible for dark matter abundance

25 Neutralino NLSP Neutralino production by gluino decay all squark decoupled limit no mass degeneracy gluino decaying into two squarks and a neutralino ATLAS-CONF (2016) Neutralino stable in detector c 0 1 & 10 6 m 1TeV m 0 1! µ 10 µ 0 tan 2. K. Hamaguchi et al. (2007) 0 multi-jet with missing momentum search ATLAS-CONF (2016)

26 Stau NLSP Stau production all squark decoupled limit no mass degeneracy stau cross section gluino cross section direct Drell-Yan stau pair production Stau stable in detector 1TeV 10 c & µ 10 m µ 0 tan m 2. K. Hamaguchi et al. (2007) long-lived charged particle searches CMS-PAS-EXO (2015)

27 Stau and gluino constraint Stau cross section upper limit Gluino production cross section C. Borschensly et.al. (2014) stau CMS-PAS-EXO (2015) Gluino and stau mass constraint by Stau cross section upper bound > Gluino production cross section

28 Collider constraints in stau NLSP Gluino and stau mass constraint 2000 LHC constraints, stau NLSP m g éêgev direct (Drell Yan) excluded region e.g. T R 10 9 GeV, m 3/2 m g 1 TeV m g é = m t é m t éêgev direct + gluino decay stau-gluino e.g. T R 10 9 GeV, m 3/2 m g 1 TeV m g éêgev m 3ê2 = m b éhgut L T R = GeV m g é m 3ê2 W 3ê2 h 2 > m 3ê2 êgev mass relation excluded region stau-gravitino Current LHC experiment exclude entire region!!

29 Physical gluino mass and gaugino mass at GUT scale r g é m g = r g m 1/ m g éêgev 3/2 h 2 ' 0.09 m3/2 100 GeV T R GeV r 2 g m2 g r 2 g m2 g m 2 3/2 m 2 3/2!! apple log T R GeV!

30 R-parity violation model in SO(10) 16 M 10 H 16 H 16 H v B L X m 3/2 R 1 0 1/2 0 1/4 5/2 2 Table 1: R-charges of matter fields, Higgs fields and SO(10) singlets. A. Superpotential W = 10 H 16 M 16 M + 16 H 16 H 16 M 16 M + X(16 H 16 H vb 2 L) B. Bilinear R-parity violation by right-handed sneutrino VEV C. mu-term Yukawa term νr mass term Bilinear R-parity breaking term B-L breaking K = vb 4 L16 M 16 H W m 3/2 vb 5 D E LN R NR ' vb 3 L m 3/2 µ 0 = vb 3 Lm 3/2 W m 3/2 10 H 10 H Finally, µ 0 µ v3 B L

31 R-parity violation model in SO(10) 16 M 10 H 16 H 16 H v B L X m 3/2 R 1 0 1/2 0 1/4 5/2 2 Table 1: R-charges of matter fields, Higgs fields and SO(10) singlets. Bilinear R-parity violation Trilinear R-parity violation W 16 M 16 H W 16 H 16 M 16 M 16 M Small R-parity violation!! µ 0 µ,, 0, 00 v 3 B L (v B L )