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The Inflaton portal to PeV-EeV dark matter
Lucien HEURTIER
March 8th 2018 LPT Orsay
In collaboration with Fei Huang, 1806.XXXX
IRN – Terascale, Strasbourg, May 31th, 2018
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 - - 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
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The dark sector dynamics remains obscure…
(Thermal Freeze Out, Non-thermal/Freeze-In, dynamical dark matter, Hidden dark sector…)
Its production mechanism remains unknown
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The dark sector dynamics remains obscure…
(Thermal Freeze Out, Non-thermal/Freeze-In, dynamical dark matter, Hidden dark sector…)
Its production mechanism remains unknown A large class of models requires unnatural choices of parameters
(small kinetic mixings, tiny portal interactions…)
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The dark sector dynamics remains obscure…
(Thermal Freeze Out, Non-thermal/Freeze-In, dynamical dark matter, Hidden dark sector…)
Its production mechanism remains unknown 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
…
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The standard cosmological History
Primordial Universe
Homogeneous, flat Universe
𝑛𝜚~1013GeV
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Inflation
Standard Model Dark Matter
𝜍𝑇𝑁 𝑈 = 𝜍𝑇𝑁
𝑓𝑟 (𝑈)
The standard cosmological History
Inflaton Decay : Reheating
Being explicit about the reheating lagrangian fixes initial conditions for dark matter production …
When is it relevant to DM production ?
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Inflation
Reheating
? Standard Model Dark Matter
SM
SM DM DM SM DM
SM
DM Ωℎ2 = 0.12
Thermal scenario of Dark matter production :
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Inflation
Reheating
? Standard Model Dark Matter
𝜏𝑤 Requires the presence of a mediator or small coupling : 𝑎′, Higgs portal, etc.
Thermal scenario of Dark matter production :
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Thermal scenario of Dark matter production : Inflation
Reheating
? Standard Model Dark Matter Ωℎ2~0.12
𝜏𝑤 Requires the presence of a mediator or small coupling : 𝑎′, Higgs portal, etc.
WIMP miracle:
𝜏𝑤 ~ 𝜏𝑤 𝐹𝑋 and 𝑛𝐸𝑁 ~ 𝒫 100 GeV
⇓
More and more disfavored by direct detection experiments…
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Thermal scenario of Dark matter production : Inflation
Reheating
? Standard Model Dark Matter Ωℎ2~0.12
𝜏𝑤 Requires the presence of a mediator or small coupling : 𝑎′, Higgs portal, etc.
WIMP miracle:
𝜏𝑤 ~ 𝜏𝑤 𝐹𝑋 and 𝑛𝐸𝑁 ~ 𝒫 100 GeV
⇓
More and more disfavored by direct detection experiments…
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Inflation
Reheating
Standard Model
DM
SM
SM
DM
DM SM DM
SM
DM Ωℎ2 = 0.12
DMNon-Thermal scenario of Dark matter production :
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Inflation
Reheating
Standard Model
DM𝜏𝑤 Requires the presence of a mediator or small coupling : 𝑎′, Higgs portal, etc. 𝜏𝑤 𝑜𝑝𝑜−𝑈ℎ ≪ 𝜏𝑤 𝑈ℎ
Non-Thermal scenario of Dark matter production :
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Inflation
Reheating
Standard Model
DM𝜏𝑤 Requires the presence of a 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…
Non-Thermal scenario of Dark matter production :
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Inflation
Reheating
Standard Model
SM
SM DM DM
SM
DM
𝑈ℎ ~ 𝑛𝐸𝑁
SM
DM Ωℎ2 = 0.12
𝑇 𝑇 Non rel. 𝑇
DM
𝑇 Non rel.
Late decay
Decoupled Hidden sector [Hooper et al., ‘16]
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Decoupled Hidden sector [Hooper et al., ‘16] Inflation
Reheating
Standard Model
SM
SM DM DM
SM
DM
𝑈ℎ ~ 𝑛𝐸𝑁
SM
DM Ωℎ2 = 0.12
𝜚ℎ 𝑇 Non rel. 𝜚ℎ
DM
𝑇 Non rel.
Late decay
Sufficient Entropy dilution ⇓ Tune a coupling to be VERY small
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Inflation
𝑛𝜚~1013GeV
Standard Model Dark Matter
The inflaton portal to DM
[Dev, Mazumdar, Qutub 13’], [Heurtier 17’]
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Inflation
𝑛𝜚~1013GeV
Standard Model Dark Matter
The inflaton portal to DM
𝑛𝜚~1013GeV Annihilation cross section feeble No possible thermal scenario
[Dev, Mazumdar, Qutub 13’], [Heurtier 17’]
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Highly decoupled sectors?
Inflation
𝑛𝜚~1013GeV
Standard Model
𝜓, 𝑇
𝜓 𝑇
𝑛𝜚~1013GeV Late decay of the hidden sector
The inflaton portal to DM
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The Model
[F.Huang, L.H., coming soon]
Thermal decoupling of dark matter in the dark sector 𝑛𝜚= 1013𝐻𝑓𝑊 Natural suppression of the hidden scalar decay width… ℎ/𝑤 𝑈ℎ/𝑈
𝑤 after inflation
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Relic Density
[F.Huang, L.H., coming soon]
Thermal decoupling in the dark sector Entropy Suppression Inflaton suppressed decay rate
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Relic Density
[F.Huang, L.H., coming soon]
Generic range of masses
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Relic Density
[F.Huang, L.H., coming soon]
Generic range of masses WIMP miracle
The Inflaton miracle !!!
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Relic Density
[F.Huang, L.H., coming soon]
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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 ?
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Experimental signatures ?
𝑂𝑆 𝜉𝑀 , 𝐼
Sommerfeld Enhancement High Energetic Cosmic Rays
At the 10 PeV – EeV scale !
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Experimental signatures ?
Illustration for 𝑛𝐸𝑁 = 3 𝑄𝑓𝑊 , 𝑤𝑠𝑓𝑚 = 10−3 , 𝜇 = 2.8
Deposited - Equivalent Energy (GeV)
Unfortunately 𝑛𝐸𝑁 > 10 𝑄𝑓𝑊 … To be continued…
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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