Revisiting gravitino dark matter in thermal leptogenesis Motoo Suzuki Institute for Cosmic Ray Research (ICRR) The University of Tokyo arxiv:1609.06834 JHEP1702(2017)063 In collaboration with Masahiro ibe and Tsutomu. T. Yanagida
R-parity R-parity is introduced for phenomenological consistency in Minimal Supersymmetric Standard Model (MSSM) R-parity charge assignment R=0 R=1 http://www7b.biglobe.ne.jp/~kcy05t/supersymmetry.html A. Prohibiting rapid proton decay B. Stable lightest SUSY particle (dark matter) https://arxiv.org/abs/hep-ph/9709356
Do we have theoretical ground on R-parity?
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!!
However
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 : -2 +1 +1 NR mass : B-L : -1 +1-1 +1 Non-perturbative R-parity is broken in perturbative SO(10) GUT!!
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 : -2 +1 +1 NR mass : B-L : -1 +1-1 +1 R parity is broken in perturbative SO(10) GUT!! Non-perturbative R-parity is broken in perturbative SO(10) GUT!!
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 ' 10 20 7 µ sec >> O(10 17 sec) K. Ishiwata, S. Matsumoto, and T. Moroi (2008) m 3/2 µ 0 2 Gravitino dark matter!!
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. 10 10 GeV W. Buchmuller et al. (2003) K. Kohri et al. (1999) Dark matter abundance Baryon asymmetry https://arxiv.org/pdf/hep-ph/ e.g. gluon and gluino collisions produce gravitino dark matter
Constraining gravitino dark matter in thermal leptogenesis
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-2016-078 (2016) 0 1 m g é = m c é 500 m g m 3/2 excluded region 0 0 200 400 600 800 1000 1200 0êGeV 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
Collider constraints in stau NLSP Stau NLSP stable in detector : long-lived charged particle searches excluded region Current LHC experiment exclude entire region!!
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 1400 1200 1000 800 600 400 200 m 3ê2 = m b éhgut L T R =1.4 10 9 GeV m g é m 3ê2 W 3ê2 h 2 >0.12 0 0 200 400 600 800 m 3ê2 êgev
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Gravitino and gluino mass relation Theoretically predicted gravitino dark matter abundance 3/2 h 2 ' 0.09 m3/2 100 GeV T R 10 10 GeV 1+0.558 r 2 g m2 g 0.011 1+3.062 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 10 10 GeV! m g = r g m 1/2 r g 2.5 m 3/2 m g
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!!
R-parity violation and its constraints R-parity violating superpotential W R = ijkd c i Q j L k + 1 2 B-L L 0 ijkl i E c j L c k + 1 2 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 < 10 25 m SUSY 1TeV 2 ( p+!e + 0 & K. Abe et al. (2011) 10 34 year) R-parity violation must be small
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 ' 10 20 7 µ sec >> O(10 17 sec) K. Ishiwata, S. Matsumoto, and T. Moroi (2008) m 3/2 µ 0 2 Gravitino dark matter!!
Gravitino dark matter abundance e.g. gluon and gluino collisions produce gravitino dark matter g: gluon λ: gluino Ψ: gravitino https://arxiv.org/pdf/hep-ph/0701104.pdf Thermally produced gravitino dark matter abundance 3/2 h 2 m3/2 T R ' 0.09 100 GeV 10 10 1+0.558 r! 2 g m2 g GeV m 2 3/2 0.011 1+3.062 r 2 g m2 g m 2 3/2! apple log J. Ellis et al. (2016) T R 10 10 GeV! m g = r g m 1/2
Assumption A. Bilinear R-parity violation µ 0 µ < 10 11 1TeV 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 < 10 10 GeV Searching this scenario
Gluino mass upper bound
Gluino mass upper bound 3/2 h 2 TR 0.12 Latest reheating temperature upper bound in thermal leptogenesis T R. 1.4 10 9 GeV S. Antusch and A. M. Teixeira (2006) T R =10 9 GeV T R =1.4 10 9 GeV 2000 W 3ê2 h 2 >0.12 1400 W 3ê2 h 2 >0.12 m g éêgev 1500 1000 500 m 3ê2 = m b éhgut L allowed region m g é m 3ê2 m g éêgev 1200 1000 800 600 400 200 m 3ê2 = m b éhgut L allowed region m g é m 3ê2 0 0 200 400 600 800 1000 1200 m 3ê2 êgev 0 0 200 400 600 800 m 3ê2 êgev m g < 2 TeV m g < 1.6 TeV
LHC constraints
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 ' 5 10 3 m3/2 2 1 TeV sec 100GeV m NLSP violating decay into the other SM particles R-parity R 10 NLSP ' 10 12 7 2 µ 1TeV sec µ 0 m NLSP 5. R NLSP << R NLSP NLSP contribution is neglibible for dark matter abundance
Neutralino NLSP Neutralino production by gluino decay all squark decoupled limit no mass degeneracy gluino decaying into two squarks and a neutralino ATLAS-CONF-2016-078 (2016) Neutralino stable in detector c 0 1 & 10 6 m 1TeV m 0 1! 3 10 11 2 µ 10 µ 0 tan 2. K. Hamaguchi et al. (2007) 0 multi-jet with missing momentum search ATLAS-CONF-2016-078 (2016)
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 & 10 7 11 2 µ 10 m µ 0 tan m 2. K. Hamaguchi et al. (2007) long-lived charged particle searches CMS-PAS-EXO-15-010 (2015)
Stau and gluino constraint Stau cross section upper limit Gluino production cross section C. Borschensly et.al. (2014) stau CMS-PAS-EXO-15-010 (2015) Gluino and stau mass constraint by Stau cross section upper bound > Gluino production cross section
Collider constraints in stau NLSP Gluino and stau mass constraint 2000 LHC constraints, stau NLSP m g éêgev 1500 1000 500 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 0 0 200 400 600 800 1000 1200 1400 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 1400 1200 1000 800 600 400 200 m 3ê2 = m b éhgut L T R =1.4 10 9 GeV m g é m 3ê2 W 3ê2 h 2 >0.12 0 0 200 400 600 800 m 3ê2 êgev mass relation excluded region stau-gravitino Current LHC experiment exclude entire region!!
Physical gluino mass and gaugino mass at GUT scale 3.0 2.8 r g é 2.6 2.4 m g = r g m 1/2 2.2 500 1000 1500 2000 2500 3000 m g éêgev 3/2 h 2 ' 0.09 m3/2 100 GeV T R 10 10 GeV 1+0.558 r 2 g m2 g 0.011 1+3.062 r 2 g m2 g m 2 3/2 m 2 3/2!! apple log T R 10 10 GeV!
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
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 10 3 4 )