WIMP dark matter and Baryogenesis

Transcription

1 WIMP dark matter and Baryogenei Lorenzo Ubaldi Bethe Center for Theoretical Phyic & Phyikaliche Intitut der Univerität Bonn, Germany with N. Bernal and F Joe-Michaux JCAP 1301 (013) 034 BLV April 9th, 013

2 Fact Baryon Aymmetry of the Univere (BAU) YB nb / 8.5 x Baryonic matter abundance (pot Planck) ΩBh = ± Dark matter (DM) abundance (pot Planck) ΩDMh = ±

3 Coincidence? ΩDM / ΩB ~ 5 Aymmetric Dark Matter WIMP miracle ΩDMh = 0.1

4 Coincidence? ΩDM / ΩB ~ 5 Aymmetric Dark Matter WIMP miracle ΩDMh = 0.1

5 Keep the WIMP miracle and ak the quetion: can we have a framework where the baryon aymmetry can be related to the thermal WIMP relic abundance?

6 WIMPy Baryogenei Cui, Randall, Shuve, JHEP 104 (01) 075

7 WIMPy Baryogenei Cui, Randall, Shuve, JHEP 104 (01) 075 Two miracle in one framework! 1.WIMP miracle weak-cale DM, thermal relic abundance.wimpy baryogenei miracle DM annihilation generate the baryon aymmetry

8 WIMPy Baryogenei Cui, Randall, Shuve, JHEP 104 (01) 075 Two miracle in one framework! 1.WIMP miracle weak-cale DM, thermal relic abundance.wimpy baryogenei miracle DM annihilation generate the baryon aymmetry

9 Cui, Randall, Shuve JHEP 104 (01) 075 Prediction for ΩB / ΩDM? 10 6 < B DM < 10 Thi i no prediction, but the oberved value 0. i eaily accommodated in uch a range.

10 Cui, Randall, Shuve JHEP 104 (01) 075 The idea DM exotic antibaryon B violating decay DM SM baryon

11 The model JCAP 1301 (013) 034

12 A et of minimal ingredient for WIMPy baryogenei SU(3) c SU() L Q U(1)y Q U(1)B Z i i 3 1 +/3 +1/ /3 1/3 +1 n or /3 1/3 1 d /3 1/3 1

13 A et of minimal ingredient for WIMPy baryogenei Dark matter SU(3) c SU() L Q U(1)y Q U(1)B Z i i 3 1 +/3 +1/ /3 1/3 +1 n or /3 1/3 1 d /3 1/3 1

14 A et of minimal ingredient for WIMPy baryogenei Dark matter Exotic heavy quark SU(3) c SU() L Q U(1)y Q U(1)B Z i i 3 1 +/3 +1/ /3 1/3 +1 n or /3 1/3 1 d /3 1/3 1

15 A et of minimal ingredient for WIMPy baryogenei Dark matter Exotic heavy quark Sterile majorana fermion SU(3) c SU() L Q U(1)y Q U(1)B Z i i 3 1 +/3 +1/ /3 1/3 +1 n or /3 1/3 1 d /3 1/3 1

16 A et of minimal ingredient for WIMPy baryogenei Dark matter Exotic heavy quark Sterile majorana fermion SU(3) c SU() L Q U(1)y Q U(1)B Z i i 3 1 +/3 +1/ /3 1/3 +1 n or /3 1/3 1 d /3 1/3 1 All the SM quark have charge -1, while the lepton and the Higg are neutral under the Z4

17 DM annihilation WO WO kinematic imply mx > mψ Aymmetry = (! )+ (! ) (! ) (! ) (! )+ (! )+ (! )+ (! ) / Im( WO ) ( m ) 16 Λ ~ 1-10 TeV

18 Decay of the exotic heavy quark! d dn The decay violate baryon number. The exotic quark ha to decay in order to avoid overcloing the univere. The SM-inglet fermion n ha to be very light. We take it to be male. We require thi decay to be fat enough o that ψ i in thermal equilibrium during DM annihilation. Thi implifie the Boltzmann Equation.

19 Sakharov condition 1. B-number violation. CP violation 3. Out of thermal equilibrium

20 Wahout procee 1,,t 1,,t WO WO

21 Cui, Randall, Shuve JHEP 104 (01) 075 Central reult If wahout procee freeze out before WIMP freezeout, then a large baryon aymmetry may accumulate, and it final value i proportional to the WIMP abundance at the time that wahout become inefficient. One way to achieve thi: mψ > mx

22 LHC bound q q m g ψ ψ φ φ d d n n & 800 GeV quark ma [GeV] 000 d 1800 CL oberved 95% C.L. limit Search for quark and gluino with the ATLAS CL detector median expected uing limit final t with jet and miing tranvere momentum and Expected 4.7limit fb±1 1 σof = 7T d 1600 proton-proton colliion data ATLAS EPS L dt = 4.71 fb, =7 TeV ATLAS NOTE ATLAS-CONF March 11, 01 Squark-gluino-neutralino model, m(χ 0 ) = 0 GeV 1 ATLAS ATLAS Collaboration Combined Preliminary σ SUSY σ SUSY = 1 fb = 10 fb m x & 400 GeV LAS-CONF arch Abtract 800 σ SUSY = 100 fb A earch for quark and gluino in final tate containing jet, miing tranvere momentum and no high-p T electron or muon i preented. The data repreent the complete ample recorded 600 in 011 by the ATLAS experiment in p = 7 TeV proton-proton colliion at the Large Hadron 600 Collider, 800with1000 a total integrated 100 luminoity 1400 of fb No exce 000 above the Standard Model background expectation i oberved. Gluino gluino mae ma below [GeV] 940 GeV, and quark mae below 1380 GeV are excluded at the 95% confidence level in implified

23 Updated LHC bound See S. Caron talk ATLAS-CONF Augut 01 quark ma [GeV] Squark-gluino-neutralino model, m( 0 1 ) = 0 GeV ATLAS -1 L dt = 5.8 fb, 0-lepton combined Preliminary =8 TeV SUSY Oberved limit (±1 ) theory Expected limit (±1 exp ) -1 Oberved limit (4.7 fb, 7 TeV) gluino ma [GeV]

24 DM relic denity + BAU L ()( ) + + t ( )() WO ( )( ) Fixed: = 10 TeV = 4 Re( WO )=Im( WO ) Large CP phae!

25 Take home meage Two conceptually different approache when trying to explain baryogenei and DM in a unified framework: Aymmetric Dark Matter, baed on the ΩDM / ΩB ~ 5 coincidence; WIMPy baryogenei, baed on the WIMP miracle. WIMPy model, after experimental contraint are taken into account, work in a good portion of the parameter pace. They provide a viable mechanim for low energy thermal baryogenei.

26 Thank you

27 Direct detection bound 1 ( 7()( )+ 8( )( )+h.c.) Tranlated into 4-component-pinor notation ( µ Ū µ U + µ Ū µ 5 U) ( µ 5 Ū µ U + µ 5 Ū µ 5 U)

28 Direct detection bound 1 ( 7()( )+ 8( )( )+h.c.) Tranlated into 4-component-pinor notation ( µ Ū µ U + µ Ū µ 5 U) ( µ 5 Ū µ U + µ 5 Ū µ 5 U) Spin Independent Spin Dependent

29 Direct detection bound 1 ( 7()( )+ 8( )( )+h.c.) Tranlated into 4-component-pinor notation ( µ Ū µ U + µ Ū µ 5 U) ( µ 5 Ū µ U + µ 5 Ū µ 5 U) Spin Independent Spin Dependent Very mild contraint

30 Direct detection bound One-loop contribution

31 Direct detection bound One-loop contribution The diagram cancel!!

32 Direct detection bound One-loop contribution The diagram cancel!! Similar tory for t-channel operator.

33 Direct detection bound One-loop contribution The diagram cancel!! Similar tory for t-channel operator. NO BOUNDS FROM DIRECT DETECTION