The Inflaton portal to PeV-EeV dark matter In collaboration with Fei - PowerPoint PPT Presentation

The Inflaton portal to PeV-EeV dark matter In collaboration with Fei Huang , 1806.XXXX Lucien HEURTIER March 8th 2018 LPT Orsay IRN – Terascale, Strasbourg, May 31th, 2018

The dark sector dynamics remains obscure…

The dark sector dynamics remains obscure… Its production mechanism remains unknown (Thermal Freeze Out, Non-thermal/Freeze-In, dynamical dark matter, Hidden dark sector …)

The dark sector dynamics remains obscure… Its production mechanism remains unknown (Thermal Freeze Out, Non-thermal/Freeze-In, dynamical dark matter, Hidden dark sector …) A large class of models requires unnatural choices of parameters (small kinetic mixings, tiny portal interactions…)

The dark sector dynamics remains obscure… Its production mechanism remains unknown (Thermal Freeze Out, Non-thermal/Freeze-In, dynamical dark matter, Hidden dark sector …) A large class of models requires unnatural choices of parameters (small kinetic mixings, tiny portal interactions…) Primordial production of the dark matter bath is barely discussed …

The standard cosmological History Homogeneous, flat Universe Primordial Universe 𝑛 𝜚 ~10 13 GeV

The standard cosmological History 𝑓𝑟 (𝑈) 𝜍 𝑇𝑁 𝑈 = 𝜍 𝑇𝑁 Inflaton Decay : Reheating Inflation Dark Standard Matter Model Being explicit about the reheating lagrangian fixes initial conditions for dark matter production … When is it relevant to DM production ?

Thermal scenario of Dark matter production : Reheating Inflation Standard Model ? Dark SM Matter SM DM SM DM SM DM DM Ωℎ 2 = 0.12

Thermal scenario of Dark matter production : Reheating Inflation Standard Model 𝜏𝑤 ? Dark Requires the presence of a Matter mediator or small coupling : 𝑎′ , Higgs portal, etc.

Thermal scenario of Dark matter production : Reheating Inflation Standard Model 𝜏𝑤 ? Dark Requires the presence of a Matter mediator or small coupling : 𝑎′ , Higgs portal, etc. More and more disfavored WIMP miracle: by direct detection experiments … 𝜏𝑤 ~ 𝜏𝑤 𝐹𝑋 and 𝑛 𝐸𝑁 ~ 𝒫 100 GeV ⇓ Ωℎ 2 ~0.12

Thermal scenario of Dark matter production : Reheating Inflation Standard Model 𝜏𝑤 ? Dark Requires the presence of a Matter mediator or small coupling : 𝑎′ , Higgs portal, etc. More and more disfavored WIMP miracle: by direct detection experiments … 𝜏𝑤 ~ 𝜏𝑤 𝐹𝑋 and 𝑛 𝐸𝑁 ~ 𝒫 100 GeV ⇓ Ωℎ 2 ~0.12

Non-Thermal scenario of Dark matter production : Reheating Inflation Standard Model SM DM SM DM DM SM DM SM DM DM Ωℎ 2 = 0.12

Non-Thermal scenario of Dark matter production : Reheating Inflation Standard Model 𝜏𝑤 Requires the presence of a DM mediator or small coupling : 𝑎′ , Higgs portal, etc. 𝜏𝑤 𝑜𝑝𝑜−𝑈ℎ ≪ 𝜏𝑤 𝑈ℎ

Non-Thermal scenario of Dark matter production : Reheating Inflation Standard Model 𝜏𝑤 Requires the presence of a DM mediator or small coupling : 𝑎′ , Higgs portal, etc. 𝜏𝑤 𝑜𝑝𝑜−𝑈ℎ ≪ 𝜏𝑤 𝑈ℎ No reason a priori to suppress the production of DM through inflaton decay …

Decoupled Hidden sector [Hooper et al., ‘16] Reheating Inflation Standard Model SM 𝑇 DM SM 𝑇 SM 𝑇 𝑈 ℎ ~ 𝑛 𝐸𝑁 Non rel. DM 𝑇 Late decay Non rel. SM DM DM DM Ωℎ 2 = 0.12

Decoupled Hidden sector [Hooper et al., ‘16] Reheating Inflation Standard Model Sufficient Entropy dilution SM 𝜚 ℎ ⇓ Tune a coupling to be VERY small DM SM 𝜚 ℎ SM 𝑇 𝑈 ℎ ~ 𝑛 𝐸𝑁 Non rel. DM 𝑇 Late decay Non rel. SM DM DM DM Ωℎ 2 = 0.12

The inflaton portal to DM Inflation 𝑛 𝜚 ~10 13 GeV Dark Standard Matter Model [Dev, Mazumdar, Qutub 13’], [ Heurtier 17’]

The inflaton portal to DM Inflation 𝑛 𝜚 ~10 13 GeV Dark Standard Matter Model 𝑛 𝜚 ~10 13 GeV  Annihilation cross section feeble  No possible thermal scenario [Dev, Mazumdar, Qutub 13’], [ Heurtier 17’]

The inflaton portal to DM Highly decoupled sectors? Inflation 𝑛 𝜚 ~10 13 GeV 𝜓 , 𝑇 Standard 𝜓 𝑇 Model 𝑛 𝜚 ~10 13 GeV Late decay of the hidden sector

The Model [F.Huang, L.H., coming soon] 𝑛 𝜚 = 10 13 𝐻𝑓𝑊 Thermal decoupling of dark Natural suppression of the hidden scalar matter in the dark sector decay width … 𝑕 ℎ /𝑕 𝑤 𝑈 ℎ /𝑈 𝑤 after inflation

Relic Density [F.Huang, L.H., coming soon] Thermal decoupling Entropy Suppression in the dark sector Inflaton suppressed decay rate

Relic Density [F.Huang, L.H., coming soon] Generic range of masses

Relic Density [F.Huang, L.H., coming soon] Generic range of masses The Inflaton WIMP miracle miracle !!!

Relic Density [F.Huang, L.H., coming soon]

Experimental signatures ? Dark matter features : • 10 PeV – EeV dark matter • Very feeble interaction with the standard model No Direct Detection constraints • Significant annihilation into dark scalars • Dark scalar lifetime < 0.01s Indirect Detection ?

Experimental signatures ? 𝑂 𝑆 𝜉 𝑀 , 𝐼 Sommerfeld Enhancement High Energetic At the 10 PeV – EeV scale ! Cosmic Rays

Experimental signatures ? Deposited - Equivalent Energy (GeV) Illustration for 𝑛 𝐸𝑁 = 3 𝑄𝑓𝑊 , 𝑤 𝑠𝑓𝑚 = 10 −3 , 𝜇 = 2.8 Unfortunately 𝑛 𝐸𝑁 > 10 𝑄𝑓𝑊 … To be continued …

Conclusion • Dark matter production usually requires fine tuning or the introduction of arbitrary mass scales • We propose an inflaton portal to a highly decoupled dark sector Reheating process explicitely present in the scenario Natural choices of couplings lead to the correct relic abundance • The model escapes direct detection • Indirect detection may be relevant in the neutrino sector (IceCube? ANITA?...)