Georg-August-University Gttingen Laura Covi [ q,p ]= ih - PowerPoint PPT Presentation

WIN2017 Workshop - Irvine, 22.06.2017 Dark Matter theory: Status and news Georg-August-University Göttingen Φ Laura Covi [ q,p ]= ih Institute for Theoretical Physics

Outline Theoretical guiding principle: Dark Matter production mechanisms WIMP DM: from EFT (back) to (simplified)Models Decaying DM: FIMP/SWIMPs in the sky and LHC More than gravity: looking for Dark Interactions in structure formation Outlook

(Theoretical) guiding principles

DARK MATTER candidates [Roszkowski 04] Too many different (non) candidates... sneutrino KK neutrino “Standard” DM KK DM production paradigms: LTP techniWIMP WIMPs (i.e. neutralino) & “FIMP/SuperWIMPs” (i.e. gravitino) & KK graviton Misalignment (i.e. axion/condensate)

THE WIMP CONNECTION Early Universe: Ω CDM h 2 Direct Detection: DM DM DM any DM q q ⟨ σ v ⟩ ∼ 1 pb Colliders: LHC/ILC Indirect Detection: e, q DM DM e, q,W,Z, γ e, q,W,Z, γ e, q DM DM γ 3 different ways to check this hypothesis !!!

SuperWIMP/FIMP paradigms Add to the BE a small decaying rate for the WIMP into a much more weakly interacting (i.e. decaying !) DM particle: 1 m Σ =100 TeV m Σ =10 TeV m Σ =1 TeV 0.01 m Σ =500 GeV WIMP [Hall et al 10] [Feng et al 04] 0.0001 1e-06 FIMP SuperWIMP SuperWIMP 1e-08 DM DM Y FIMP 1e-10 produced produced 1e-12 by WIMP by WIMP 1e-14 decay in decay after DM 1e-16 equilibrium freeze-out 0.1 1 10 100 1000 10000 100000 1e+06 1e+07 1e+08 ω Two mechanism naturally giving “right” DM density depending on WIMP/DM mass & DM couplings

F/SWIMP CONNECTION Early Universe: Ω CDM h 2 Direct Detection: any WIMP NONE... DM Colliders: LHC/ILC Indirect Detection: WIMP DM e, q DM e, q,W,Z, γ e, q,W,Z, γ SM e, q decaying DM ! DM 3 different ways to check this hypothesis !!!

Black Hole DM ? Not easy to produce them in the Early Universe..., e.g. need funny power spectra from inflation for primordial Black Holes; if they are produced by collapse and mergers, after BBN/CMB then DM still needed...

Black Hole DM ? [Carr et al. 1705.05567] Not easy to produce them in the Early Universe..., e.g. need funny power spectra from inflation for primordial Black Holes; if they are produced by collapse and mergers, after BBN/CMB then DM still needed...

WIMP DM: from EFT to simplified models

EFT for Dark Matter [ Beltram et al 2000, Goodman et al 2000 & 2001, Bai et al 2001,....] Consider the production of a pair of DM particles together with ISR of a SM particle: gluon, photon, W/Z, top, etc... EFT: Many different effective operators are possible !

Caveat for the EFT: s While the use of EFT for the case of non-relativistic scattering with matter in DM direct detection is well-justified, at LHC energies one has to be more careful... [Fox et al 11, Busoni et al 13, O.Buchmuller et al 13, ...] [O.Buchmuller et al 1308.6799] The bound is valid only for large mediator mass !

LHC: simplified models [ CMS collaboration, EPJC 75 (2015) 235] Vector mediator

LHC: simplified models II [CMS, EXO-16-039-pas] Very strong bounds for the axial vector case !

Caveat for the EFT: t In the case of t-channel mediation, there is no resonant enhancement, but instead more channels for monojets as well as dijets show up, e.g. for scalar mediator: [ An et al. 2013, Papucci et al 2014] Mono-jet without ISR Dijet and MET Complementary limits from Mono-jets & Di-jets ! In some cases direct searches for the mediator or di-jets can be more effective than monojets (i.e. also for Z’). [Fradsen et al. 2012, Chala et al. 2015]

LHC limits from dijets [ATLAS coll. 2016] DM Simplified Model Exclusions ATLAS Preliminary August 2016 DM Mass [TeV] < 0.12 Axial-vector mediator, Dirac DM 1.2 g = 0.25, g = 1 2 q DM = 0.12 h s c s Ω a 2 M h r Ω o c t Thermal relic a 1 i d e ATLAS-CONF-2016-070 ATLAS-CONF-2016-030 M = s Dijet+ISR Dijet TLA s a M M D × 0.8 2 2 1 . 0 = 2 h Ω c c i DM Simplified Model Exclusions ATLAS Preliminary August 2016 l e r l a 0.6 m DM Mass [TeV] r e h Phys. Rev. D. 91 052007 (2015) T Perturbative unitarity 1.2 Phys. Rev. D. 91 052007 (2015) Dijet 8 TeV 0.4 miss E +jet ATLAS-CONF-2016-069 Dijet 8 TeV T 1 arXiv:1604.07773 ATLAS-CONF-2016-030 Dijet TLA 0.2 Dijet = 0.12 miss 2 E + γ h 0.8 Ω T DM Mass = Mediator Mass Thermal relic y c t i r JHEP 06 (2016) 059 a t i n u e 0 0.5 1 1.5 2 2.5 v i t a b r u 0.6 t r × = 0.12 e 2 Mediator Mass [TeV] P 2 h Ω Thermal relic c 0.4 miss E + γ 0.2 T JHEP 06 (2016) 059 miss Axial-vector mediator, Dirac DM E +jet T g = 0.1, g = 1.5 arXiv:1604.07773 q DM 0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 Mediator Mass [TeV]

Jet substructure for DM In case of a positive signal, the jet substructure could help to disentangle the operator and type of coupling: [Agrawal & Rentala 1312.5325] Di-jet angular distribution could also vary for loop operators ! [Haisch et al 1311.7131]

Effective Theory for DD [Riccardo Catena WIN-2015] [Fitzpatrick et al. 2012]

Effective Theory for DD Interference matters ! [Catena & Gondolo 2015]

Effective Theory for DD Interference matters ! [Catena & Gondolo 2015] More Ops can contribute to solar capture: [Catena 2015]

SUSY models still alive [Barr & Liu 2016] pMSSM points surviving after LHC-13 data Higgsino band Wino band Wino DM challenged by Indirect Detection, but Higgsino parameter space still viable (and also some Bino-like...)

Gravitino vs neutralino DM The neutralino compositions is very different, so only half the neutralino DM points will be excluded by LHC-14, while 75% of the gravitino DM points... [Arbey et al. 1505.04595] 14TeV , 300 fb − 1 14TeV , 300 fb − 1

decaying Dark Matter

A simple wimp/swimp model [G. Arcadi & LC 1305.6587] Consider a simple model where the Dark Matter, a Majorana SM singlet fermion, is coupled to the colored sector via a renormalizable interaction and a new colored scalar : Σ R d R Σ † u c λ ψ ¯ ψ d R Σ + λ Σ ¯ Try to find a cosmologically interesting scenario where the scalar particle is produced at the LHC and DM decays with a lifetime observable by indirect detection. Then the possibility would arise to measure the parameters of the model in two ways ! FIMP/SWIMP connection

A simple wimp/swimp model [G. Arcadi & LC 1305.6587] No symmetry is imposed to keep DM stable, but the decay is required to be sufficiently suppressed. For : m Σ � m ψ d R d R ψ Σ u c R Decay into 3 quarks via both couplings ! To avoid bounds from the antiproton flux require then m 4 τ ψ ∝ λ − 2 ψ λ − 2 ∼ 10 28 s Σ Σ m 5 ψ

A simple wimp/swimp model Ω ψ h 2 = 0 . 11 Log ( λ Σ ) DM decay observable FIMP in indirect detection � 8 0.01 & right abundance BR( Σ → ψ ) & sizable BR in DM 0.1 � 10 0.99 λ ψ ∼ λ Σ Log 10 Λ ' But unfortunately � 12 10 27 s decays outside Σ the detector @ LHC! 10 29 s � 14 Perhaps visible SWIMP DM lifetime 10 31 s decays with a bit of � 14 � 12 � 10 � 8 hierarchy... Log ( λ ψ ) Log 10 Λ [G. Arcadi & LC 1305.6587]

Combined detection Σ Still possible to have [G. Arcadi, LC & F. Dradi 1408.1005] multiple detection of - DM decay: Γ ψ → λλ 0 m ψ - displaced vertices Γ Σ ,SM → λ 0 m Σ - metastable tracks Γ Σ ,SM < X → λ 0 m Σ with stopped tracks maybe both Γ Σ ,SM , Γ Σ ,DM It is possible to over-constraint the model and check the hypothesis of FIMP production !

ID of FIMP/SWIMP DM [LC, Eckner & Gustafsson, work in progress] λλ 0 = 10 − 18 m Σ = 1TeV Unfortunately bounds strongly depend on propagation...

Baryogenesis in RPV SUSY [Sundrum & Cui 12, Cui 13, Rompineve 13, ...] Realization of good old baryogenesis via out-of-equilibrium decay of a superpartner, possibly WIMP-like, e.g. in the model by Cui with Bino decay via RPV B-violating coupling. λ 00 λ 00 CP violation arises from diagrams with on-shell gluino lighter than the Bino. To obtain right baryon number the RPC decay has to be suppressed, i.e. due to heavy squarks, the RPV coupling large and the Bino density very large...

Baryogenesis & SW DM [Arcadi, LC & Nardecchia 1312.5703] In such scenario it is also possible to get gravitino DM via the SuperWIMP mechanism and the baryon and DM densities can be naturally of comparable order due to the suppression by the CP violation and Branching Ratio respectively... Ω ∆ B = m p � ⇥ Ω τ →∞ � ⇧ → / ⇥ ⇥ CP BR B χ m χ Small numbers Ω DM = m DM BR ( ⇧ → DM + anything ) Ω τ →∞ χ m χ independent of m p � CP BR ( ⇥ → B / ) Ω ∆ B = Bino density m DM BR ( ⇥ → DM + anything) Ω DM Gravitino DM: BR is naturally small and DM stable enough !

Baryogenesis in RPV SUSY [Arcadi, LC & Nardecchia 1507.05584, Arcadi, LC & Kirk work in progress] Unfortunately realistic models are more complicated than expected: wash-out effects play a very important role !!! 10 7 GeV Heavy !!! G. Arcadi