Chiral Dark Sector. Keisuke Harigaya (UC Berkeley, LBNL) KH, Yasunori Nomura Raymond Co, KH, Yasunori Nomura 1610.

Transcription

1 04/21/2017 Lattice for BSM Chiral Dark Sector Keisuke Harigaya (UC Berkeley, LBNL) KH, Yasunori Nomura Raymond Co, KH, Yasunori Nomura

2 Plan of Talk Introduction Set up of our model Phenomenology

3 Introduction

4 Dark matter

5 WIMP Dark matter DM DM DM DM DM DM DM DM DM DM DM DM

6 Why is it stable? A possible answer: composite dark matter Some composites states may be accidentally stable. In the standard model QCD, Baryon Charged pion (if EW scale is large) Dark matter from a new QCD-like theory?

7 Bonus: Mass scale m DM < 100 TeV M Pl Confinement g 2 (E) generates a WIMP scale E

8 Features of our model A simple setup with chiral gauge symmetry (Strong coupling is vector-like) Constituent quark mass is forbidden, and the dynamical scale is the unique mass scale High predictability, but I cannot calculate observables Lattice information is crucial

9 Setup of our model

10 Matter contents u d ū d SU(N) N N N N U(1) D 1-1 -a a a =1 Mass terms are forbidden Techni color-like theory

11 Coupling to SM Dark U(1) D U(1) Y ~~~~~~~~~~~~~~ X SM L 2cos W B µ A µ D Goldberg, Hall (1986) Fayet (2007) Pospelov, Ritz and Voloshin (2007)

12 Mass spectrum Nambu-Goldstone bosons, dark photon Rho mesons, baryons,

13 NGBs <uū>=< d d >6= 0 SU(2) L SU(2) R ± : pseudo NGB dark pion stable, DM candidate SU(2) V 0 : eaten by A µ D U(1) D dark photon

14 Dark pion/photon masses u d ū d SU(N) N N N N U(1) D 1-1 -a a m e D 4 m D 6aln2 < J µ D J D > vector dominance m AD e D 4 m D N(1 a) 1 f 2 f ' D µ U(D µ U) p N 4 m D Lattice?

15 Higher resonances mesons (rho,eta, ) : decays into pions and photons baryons : stable, DM candidate m B Nm D Lattice?

16 Baryon DM

17 Abundance of baryon baryons mesons v = 4 m B 2 < 1 4 v unitality bound DM / 1 v m DM 100 TeV??

18 Abundance of baryon baryons mesons v = 4 m B 2 exp( N) large N behavior (Witten, 1980) smaller DM mass may be OK Important for other scenario, including Composite Higgs Lattice? Probably difficult, but interesting

19 Indirect detection A D baryons mesons ~~~~~ f SM v now = v fo S v fo 0.1 Possibility of Boost v now via pion exchange??

20 Indirect detection 1 Lattice? Important for other scenario, including Composite Higgs δ Ω B Ω DM CTA prospect for S=3 CTA prospect for S=10 CTA prospect for S= NFW m B (GeV)

21 Thermal effect? For N=3, the X section is close to the unitarily limit T fo ' m DM /30 T c ' m DM /6 ' 5T fo Thermal effect would be small

22 Charged pion DM

23 Abundance of pion Assume m >m AD ~~~~~ ~~~~~ A D

24 Indirect detection ~~~~~ ~~~~~ A D ~~~~~ f SM

25 Indirect detection 1 ed (1+a) Ω ϕ Ω DM CTA prospect Fermi-LAT 10-yr prosepct Fermi-LAT NFW 10-1 GAPS prospect m ϕ (GeV)

26 Direct detection (cm 2 ) HL-LHC14 LUX XENON1T 2017 LZ prospect ' DM σ ϕ SI ϵ Neutrino floor m ϕ (GeV)

27 Other comments

28 Dark radiation SU(N)N N N N U(1) D 1-1 -a a a =0! SU(2) R symmetry m 2 / a =0

29 Dark radiation and direct detection B B ~~~~~ / e D m 2 A D SM SM T D $ N e $ B,n B,n

30 Dark radiation and direct detection ϵ e D ( 1 TeV m AD ) (cm 2 ) σ B SI Planck σ Planck σ ΔN eff

31 Dark Unification? SO(10)! SU(4) SU(2) SU(2) 16 = (4, 2, 1) + ( 4, 1, 2) SU(4) SU(2) 2 SU(2) 2 Raymond Co, KH (in preparation)

32 Summary The mass scale and the stability of dark matter are understood in our model Rich phenomenology: Indirect/direct detection, collider, dark radiation Lattice information is crucial

33 Summary The mass spectrum The annihilation X section of baryons in larger N Its velocity dependence

34 Dark matter from thermal bath Lee and Weinberg DM SM DM SM Particle Dark Matter

35 Symmetry structure u d ū d SU(N) N N N N U(1) D U(1) P a a U(1) P SU(2) V SU(2) L SU(2) R gauging U(1) D U(1) D U(1) P

36 Abundance of pion m >m AD ~~~~~ ~~~~~ A D ε can be very small Secluded dark matter scenario Pospelov, Ritz (2006)

37 Pion& Baryon (σv)eff (cm 3 /s) δ e D Ω ϕ h 2 =0.11 Ω B h 2 = CMB constraint GAPS prospect Fermi-LAT Fermi-LAT 10-yr prospect CTA prospect B + = DM m DM (GeV)

38 Decaying DM N c =4 L = 1 M 2 uudd year M M Pl TeV M B 5

39 Small mass scale m < 10 GeV

40 Abundance of pion m >m AD ~~~~~ ~~~~~ A D effective around recombination m. 10 GeV is excluded (Energy injection) / m DM n 2 DM / 1 m DM

41 Abundance of pion m <m AD ~~~~~ f SM v / v 2 Direct detection is not efficient due to small recoil energy

42 m <m AD /2-2.0 m ϕ =0.4 m AD K + π + A D ~~~~~ f SM -2.5 a=1/2 (g-2) e e + e - γ A D A D! log 10 ϵ N ν,eff e - N e - NA D, A D ϕϕ π 0 γa D, A D ϕϕ BBN pn e D >1 σ e = cm 2 σ e = cm 2 σ e = cm 2 log 10 (m AD /GeV)

43 Muon g-2? 4m 2 ~~~~~ f SM 1 Near pole annihilation smaller m 2 A D e D A D log 10 ϵ m K + π + ϕ =0.45 m AD A D e + e - γ A D a=1/2 (g-2) e N ν,eff e - N e - NA D, σ e = cm 2 A D ϕϕ π 0 γa D, A D ϕϕ σ e = cm 2 log 10 (m AD /GeV) BBN pn σ e = cm 2 e D >1

44 m AD /2 <m <m AD -2.0 m ϕ =0.6 m AD a=1/2 e + e - γ e + e - A D! -2.5 (g-2) e -3.0 π 0 γ e + e - log 10 ϵ -3.5 N ν,eff BBN pn e D >1-4.0 σ e = cm 2 σ e = cm 2 σ e = cm 2 e - N e - e + e - N log 10 (m AD /GeV) CMB A D ff

45 Dark rho meson? dark rho meson mixes with dark photon µ D J µ em 4 N e D e + e ~~~~~~~~ ~~~~~~~~ D 0 > 10 4 may be probed. Essig, Mardon, Papucci, Volansky and Zhong (2013) Monophoton e.g. at Belle II see Hochberg, Kuflik and Murayama (2015) for rigorous discussion