04/21/2017 Lattice for BSM Chiral Dark Sector Keisuke Harigaya (UC Berkeley, LBNL) KH, Yasunori Nomura 1603.03430 Raymond Co, KH, Yasunori Nomura 1610.03848
Plan of Talk Introduction Set up of our model Phenomenology
Introduction
Dark matter
WIMP Dark matter DM DM DM DM DM DM DM DM DM DM DM DM
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?
Bonus: Mass scale m DM < 100 TeV M Pl Confinement g 2 (E) generates a WIMP scale E
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
Setup of our model
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
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)
Mass spectrum Nambu-Goldstone bosons, dark photon Rho mesons, baryons,
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
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?
Higher resonances mesons (rho,eta, ) : decays into pions and photons baryons : stable, DM candidate m B Nm D Lattice?
Baryon DM
Abundance of baryon baryons mesons v = 4 m B 2 < 1 4 v unitality bound DM / 1 v m DM 100 TeV??
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
Indirect detection A D baryons mesons ~~~~~ f SM v now = v fo S v fo 0.1 Possibility of Boost v now 0.001 via pion exchange??
Indirect detection 1 Lattice? Important for other scenario, including Composite Higgs δ 10-1 10-2 Ω B Ω DM 10-2 10-1 1 CTA prospect for S=3 CTA prospect for S=10 CTA prospect for S=1 10-3 NFW 10-4 10 3 10 4 10 5 m B (GeV)
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
Charged pion DM
Abundance of pion Assume m >m AD ~~~~~ ~~~~~ A D
Indirect detection ~~~~~ ~~~~~ A D ~~~~~ f SM
Indirect detection 1 ed (1+a) Ω ϕ Ω DM 10-2 10-1 1 CTA prospect Fermi-LAT 10-yr prosepct Fermi-LAT NFW 10-1 GAPS prospect 10 10 2 10 3 10 4 m ϕ (GeV)
Direct detection (cm 2 ) 10-44 10-45 10-46 HL-LHC14 LUX 2014-16 XENON1T 2017 LZ prospect ' DM σ ϕ SI 10-47 ϵ 10-2 10-48 10-3 10-4 10-5 Neutrino floor 10-49 1 10 10 2 10 3 10 4 m ϕ (GeV)
Other comments
Dark radiation SU(N)N N N N 1 2 1 2 U(1) D 1-1 -a a a =0! SU(2) R symmetry m 2 / a =0
Dark radiation and direct detection B B ~~~~~ / e D m 2 A D SM SM T D $ N e $ B,n B,n
Dark radiation and direct detection 10-43 ϵ e D ( 1 TeV m AD ) 2 10-44 10-1 10-2 (cm 2 ) σ B SI 10-45 10-46 Planck 2015 1σ Planck 2015 2σ 10-47 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 ΔN eff
Dark Unification? SO(10)! SU(4) SU(2) SU(2) 16 = (4, 2, 1) + ( 4, 1, 2) SU(4) 1 2 1 2 4 4 4 4 SU(2) 2 SU(2) 2 Raymond Co, KH (in preparation)
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
Summary The mass spectrum The annihilation X section of baryons in larger N Its velocity dependence
Dark matter from thermal bath Lee and Weinberg DM SM DM SM Particle Dark Matter
Symmetry structure u d ū d SU(N) N N N N U(1) D U(1) P 1-1 -1 1 1-1 -a a U(1) P SU(2) V SU(2) L SU(2) R gauging U(1) D U(1) D U(1) P
Abundance of pion m >m AD ~~~~~ ~~~~~ A D ε can be very small Secluded dark matter scenario Pospelov, Ritz (2006)
Pion& Baryon (σv)eff (cm 3 /s) 10-24 10-25 10-26 10-27 δ 10-3 10-2 10-1 1 e D 0.1 0.3 1 Ω ϕ h 2 =0.11 Ω B h 2 =0.11 10 10 2 10 3 10 4 10 5 CMB constraint GAPS prospect Fermi-LAT Fermi-LAT 10-yr prospect CTA prospect B + = DM m DM (GeV)
Decaying DM N c =4 L = 1 M 2 uudd 10 14 year M M Pl 4 100 TeV M B 5
Small mass scale m < 10 GeV
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
Abundance of pion m <m AD ~~~~~ f SM v / v 2 Direct detection is not efficient due to small recoil energy
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 -3.0-3.5-4.0 N ν,eff e - N e - NA D, A D ϕϕ π 0 γa D, A D ϕϕ BBN -4.5-2.5-2.0-1.5-1.0-0.5 0.0 0.5 pn e D >1 σ e = 10-38 cm 2 σ e = 10-40 cm 2 σ e = 10-42 cm 2 log 10 (m AD /GeV)
Muon g-2? 4m 2 ~~~~~ f SM 1 Near pole annihilation smaller m 2 A D e D A D log 10 ϵ -2.0-2.5-3.0-3.5-4.0 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 = 10-38 cm 2 A D ϕϕ π 0 γa D, A D ϕϕ -4.5-2.5-2.0-1.5-1.0-0.5 0.0 0.5 σ e = 10-40 cm 2 log 10 (m AD /GeV) BBN pn σ e = 10-42 cm 2 e D >1
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 = 10-37 cm 2 σ e = 10-39 cm 2 σ e = 10-41 cm 2 e - N e - e + e - N -4.5-2.5-2.0-1.5-1.0-0.5 0.0 0.5 log 10 (m AD /GeV) CMB A D ff
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