General Analysis of Anti-Deuteron Dark Matter Search Yanou Cui - PowerPoint PPT Presentation

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections General Analysis of Anti-Deuteron Dark Matter Search Yanou Cui Harvard University with John Mason and Lisa Randall (To appear soon) PHENO 2010 Symposium, May 10, University of Wisconsin, Madison

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections Outline Introduction 1 Anti-D Cosmic Ray Flux 2 Experimental Reach for Various Final States 3 General Bounds/Features of DM Related to its 4 Detections ¯ D Detection Prospect for Specific Models 5 Conclusions 6

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections Search Paths for Dark Matter Existence of DM � – Macroscopic effects: galaxy rotation curve, gravitational lensing... What is DM? Microscopic feature?–Little is known... Familiar search Paths: Direct Detection: DM scatters off target nucleus, better control/estimation of background � (CDMS, XENON...) But rate may be highly suppressed: current bound SI elastic σ χ p � 10 − 7 pb for 10 − 100 GeV DM, could get more stringent in coming years (XENON100/1T, Super-CDMS) Indirect Detection: Cosmic Ray SM particles produced from DM annihilation, s-wave annihilation � σ ann v � thermal = 1 pb � ( Ω DM ) But most IdDt channels ( e + , γ, ¯ p ): large astrophysical bkg, uncertainties, hard to ‘confirm’ as DM origin (e.g.controversies after PAMELA, FERMI excess)

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections Low Background Channel for IdDt? ⇒ Low energy ¯ D ! (Bottino, Donato, Fornengo and Salati, 1998) Conventional DM: color multiplicity → significant BR(ann) to hadrons (‘Conservative’ about PAMELA excess) . Advantages compared with ¯ p : Higher threshold energy for secondary astrophysical production: ( pH ) , ( pH e ) collision, E th (¯ p ) = 7 m p , E th (¯ D ) = 17 m p , suppression from cosmic ray p number distribution N p ∼ E − 2 . 7 D ∼ 2 GeV . K ¯ p Suppressed tertiary production of low E ¯ D : ‘slow-down’ during inelastic scattering off galactic nucleus: ¯ p � , Not for ¯ D ! ‘Fragility’: E binding (¯ D ) = 2 . 2 MeV ⇒ Breaking apart instead of losing energy High sensitivity experiments coming soon! –AMS-02 (2010), GAPS (LDB2011, ULDB2014, SAT)

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections Our Goal Most existing anti-D related DM study: signal for particular DM models, e.g. SUSY ˜ χ 0 (Donato, Fornengo, Salati, 1999; Baer and Profumo 2005, etc.) Our goal: Take a broader view– + general analysis for general DM candidates Anti-D flux from various SM final states, mass reach at AMS-02, GAPS Generic scalar, fermion, vector DM models: correlation between thermal relic density, DiDt and IdDt, operator analysis

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections Injection Spectrum D injection spectrum: m DM , final states composition ( ¯ ¯ tt , ¯ bb , h 0 h 0 , gg , W + W − ) –hadronization simulated by PYTHIA6.4 Formation of ¯ D from ¯ p − ¯ n (coalescence model): in ¯ n rest 1 p < B , or | � n − � 2 ∼ p 0 ∼ 70 MeV ⇒ ¯ frame, K ¯ k ¯ k ¯ p | < ( 2 m p B ) D ! more accurately, p 0 by fitting ALEPH Z decay data: p 0 = 160 MeV Different Spectral features for different final states–colored ( ¯ bb , ¯ tt ): hadronize in rest frame, peak at low K even at large m DM –favored by ¯ D search ; color-neutral ( h 0 h 0 , W + W − ): hadronize in boosted frame, peak at higher K esp. at high m DM

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections 0.001 5 � 10 � 4 1 � 10 � 4 5 � 10 � 5 1 � 10 � 5 5 � 10 � 6 1 � 10 � 6 0.2 0.5 1.0 2.0 5.0 10.0 20.0 dN � dT � Number � GeV � vs. T � GeV � � hh � 0.001 0.001 5 � 10 � 4 5 � 10 � 4 1 � 10 � 4 1 � 10 � 4 5 � 10 � 5 5 � 10 � 5 1 � 10 � 5 1 � 10 � 5 5 � 10 � 6 5 � 10 � 6 1 � 10 � 6 1 � 10 � 6 0.2 0.5 1.0 2.0 5.0 10.0 20.0 0.2 0.5 1.0 2.0 5.0 10.0 20.0 dN � dT � Number � GeV � vs. T � GeV � � tt � dN � dT � Number � GeV � vs. T � GeV � � bb � Figure: The anti-D injection spectrum as a function of Kinetic Energy, T , for W + W − , hh (115 GeV ), ¯ tt , b ¯ b final states. m DM = 100 GeV ( blue / solid ) , 200 GeV ( green / dashed ) , 300 GeV ( red / dottd ) , 400 GeV ( black 500 GeV ( black / solid ) , 600 GeV ( blue / solid ) , 700 GeV ( green / dashed ) , 800 GeV ( red/dotted

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections Anti-D Flux: Propagation from galactic halo to us 2D diffusion model. The diffusion equation for charged cosmic rays (Uncertainty in model parameters: MIN, MED, MAX): d 2 3 n He ) ψ ( r , z , E ) dt ψ ( r , z , E ) = Q ( r , z , E ) − 2 h δ ( z )Γ ann ( E )( n H + 4 � ∂ 2 � ∂ z 2 + 1 ∂ r r ∂ ∂ ∂ + K ( E ) ψ ( r , z , E ) − V C ∂ z ψ ( r , z , E ) r ∂ r primary source Q obtained from DM ¯ D injection spectrum ( dN dT ) � 2 dN � ρ ( r , z ) 1 Q ( r , z , T ) = 2 � σ v � dT . m DM �� r � α � α � � � r ⊙ � ρ Ein ( r ) = ρ ⊙ exp − 2 − /α r s r s Solar Modulation: 2 mT � + T 2 Φ � ( T � ) = � T = T � + e φ F . 2 mT + T 2 Φ( T ) ,

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections Experimental Reach for Certain Final States ( BR = 1 , � σ v � = 1 pb ) Mass reach: the largest DM mass (GeV) for which the anti-D flux yields N crit –number for 2 σ or 5 σ signal at certain experiment. ¯ h 0 h 0 W + W − ¯ Experiment qq tt N crit AMS-02 high (2 σ ) 110 < m t < m h < m W 1 AMS-02 low (2 σ ) 150 220 150 140 1 GAPS (LDB) (2 σ ) 150 220 150 120 1 GAPS (ULDB) (2 σ ) 360 560 300 200 1 GAPS (SAT) (2 σ ) 700 1000 550 270 4 AMS-02 high (5 σ ) 50 < m t < m h < m W 6 AMS-02 low (5 σ ) 70 < m t < m h < m W 4 GAPS (LDB) (5 σ ) 75 < m t < m h < m W 3 GAPS (ULDB) (5 σ ) 150 220 150 120 5 GAPS (SAT) (5 σ ) 360 550 300 200 14

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections General Bounds/Features of DM related to its detections Features of general DM: spin (0 , 1 / 2 , 1), interaction with SM (operator), mass ⇒ Ω DM → � σ | v |� therm = 1 pb , � σ | v |� ann (IdDt), σ SI � 10 − 7 pb (XENON, CDMS bound), σ SD (DiDt) ⇒ � σ | v |� therm ≥ 10 7 σ SI Correlation between � σ | v |� therm and σ SI via crossing symmetry of Feynman diagram ⇒ Tension E.g. DM χ interacts with quarks, leptons, W/Z with ‘unbiased’ universal couplings, mediator couplings to DM and SM state g 1 , g 2 . To relate to both � σ | v |� therm and DiDt, focus on e.g. u quark. Effective Fermi coupling for the related operator χ † χ ¯ qq g 1 g 2 G = χ − M 2 ) 2 + Γ 2 [( 4 m 2 M M 2 ] 1 / 2

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections BR(u) for annihilation ∼ 10 % ⇒ 3 ( g 1 g 2 ) 2 � σ | v |� u M M 2 ] = 10 − 37 cm 2 . therm = χ − M 2 ) 2 + Γ 2 4 π [( 4 m 2 Crossing the Feynman diagram ⇒ associated process/rate for DiDt(SI) 2   m 2 ( g 1 g 2 ) 2 1 m p m p 2 p  � f p � 27 f p σ χ p = Tq + TG  ( m χ + m p ) 2 M 4 4 π m q m q q = u , d , s q = c , b , t m 2 ( g 1 g 2 ) 2 1 p ∼ 10 − 41 cm 2 ≈ π m 2 M 4 χ f p TG , f p Tq ∝ gluon and quark matrix element in the nucleon However, current DiDt bound ⇒ σ χ p � 10 − 43 cm 2 for EW mass DM ⇒ naive estimation ∼ O ( 100 ) real � σ | v |� therm (more severe if null result in σ SI near future XENON100/1T...)

Introduction Anti-D Cosmic Ray Flux Experimental Reach for Various Final States General Bounds/Features of DM Related to its Detections Realistic Models: Mechanisms Affecting � σ | v |� therm -1 σ SI Enhance � σ | v |� therm : S-Channel Resonance Coannihilation with mass degenerate partner, particularly useful when self-annihilation p-wave suppressed Suppress SI coupling Suppression from Flavor Dependent Couplings: Suppressed coupling to light quark, while other efficient channels (t, lepton, W/Z) maintains � σ | v |� therm . ‘Classic’ example--Yukawa coupling via h-like mediator: Go back to SI σ χ p , replace the universal g 2 by y q : 2   m 2 ( g 1 ) 2 1 m p m p m q y q 2 p  � m q y q f p � 27 f p = Tq + σ χ p  ( m χ + m p ) 2 M 4 TG 4 π q = u , d , s q = c , b , t m 2 ( g 1 ) 2 1 M 4 ( m p p v ) 2 · 0 . 2 ≈ 10 − 45 cm 2 ≈ m 2 π χ around the reach of XENON100/XENON1T, Super-CDMS!