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The Post-Inflationary Universe After Planck
ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy (Syracuse)
Scott Watson Syracuse University
(and LHC)
Main point of this talk
Universe without SUSY
Universe with SUSY
We can improve inflation constraints by including dark matter constraints.
SUSY and Hierarchies after LHC
No sign of SUSY yet.
SUSY can stabilize the Electroweak Hierarchy
SUSY and Hierarchies after LHC
SUSY can still stabilize the Electroweak Hierarchy and
be “natural” (At cost of complex model building)
Scalars heavy, fermions can be light
Split SUSY
✓ Gauge Coupling Unification
✓ Dark Matter
✓ No Flavor, CP problems
J. Wells (hep-ph/0306127) N. Arkani-Hamed and S. Dimopoulos (hep-th/0405159)
Scalars heavy, Fermions light (Fermions carry R-symmetry, scalars do not.)
✓ Unification
✓ Dark Matter
✓ No Flavor, CP problems
✓ No moduli problems
Moduli get masses:
m3/2 =⇤2SUSY
mp
m� ' m3/2 ' 100� 1000 TeV
Dark Matter
UV Completions of SUSY (Top-down Approaches add Moduli)S. Watson (Arxiv:0912.3003) with B. Acharya, G. Kane, P. Kumar (Arxiv:0908.2430)
Which cosmological history results from this framework?
Split SUSY and Top-Down approaches both seem to favor a Non-thermal History for Dark Matter
How can we test which history occurred?
TeV
eV
GeV
MeV
Infla
tion
Baryo
gene
sis(p
)rehe
atin
g
GUTs
Quant
um G
ravit
y
Nucleo
synt
hesis
CMB
Stru
cture
form
ation
Dark E
nerg
y
Firs
t Sta
rs
Cosmic Dark Age
Planck has constrained models of inflation to an impressive level of accuracy
Tr = 108 GeV
Tr = 700 GeV
weff = �1/3 . . . 1/3
weff = �1/3 . . . 1
Instant ReheatingModel History 1 History 2
History 1 (Blue)
History 2 (Grey)
Planck Bayesian Analysis for post-inflation model selection
weff
ns ns ns
weff weff
Consider a different approach.
Theory Prior: SupersymmetryI.e., we need to address the (big) hierarchy problem, dark mater, gauge coupling unification, Coleman–Mandula, yada yada yada
ArXiv:1307.2453 with R. Easther, R. Galvez, and O. Ozsoy
✓ Unification
✓ Dark Matter
✓ No Flavor, CP problems
✓ No moduli problems
Moduli get masses:
m3/2 =⇤2SUSY
mp
m� ' m3/2 ' 100� 1000 TeV
Dark Matter
A SUSY Prior (post LHC)ArXiv:1307.2453 with R. Easther, R. Galvez, and O. Ozsoy
Planck has constrained models of inflation to an impressive level of accuracy
There is an uncertainty in matching observable modes today with a particular inflationary model during inflation(related to scale of inflation and how it ends)
Matching Equation
�N ' 10
This leads to some (well known) freedom in Model Constraints
Split SUSY and Top-down motivated approaches both seem to favor a Non-thermal History for Dark Matter
( Moduli evolve like a Matter dominated universe )
Universe with SUSY Prior
�Ntotal
' 20
Universe with SUSY Prior
More freedom for inflationary constraints with SUSYArXiv:1307.2453 with R. Easther (Auckland), R. Galvez, and O. Ozsoy (Syracuse)
r
ns
More freedom for inflationary constraints with SUSYArXiv:1307.2453 with R. Easther (Auckland), R. Galvez, and O. Ozsoy (Syracuse)
Inflation without scalars (using W. Kinney’s Flow Code 1.0)
r
ns
Is a universe with SUSY less restrictive?
r
ns
We must account for dark matter
SUSY Wimps in Non-thermal Histories
Dark matter will be dominantly non-thermal:
2nd Reheating from Scalar decay
Restrict Mass and Cross-section by dark matter experiments!
⌦
obs
h2 ' 0.12
Restrict Reheat temperature
Reduce freedom for Planck constraints
Dark matter will be of non-thermal origin:
Indirect Detection Constraints from FERMIArXiv:1307.2453 with R. Easther (Auckland), R. Galvez, and O. Ozsoy (Syracuse)
Current and Future Constraints from XenonArXiv:1307.2453 with R. Easther (Auckland), R. Galvez, and O. Ozsoy (Syracuse)
Summary of our Results
• For pure wino SUSY Dark Matter we find a lower bound on the reheat temperature of around 700 MeV, substantially reducing the theoretical prior.
• General SUSY WIMPs are also constrained, but a little more model dependence must be considered (e.g. tan beta, etc..)
• Lesson learned: Theory Priors (world with SUSY) + Cosmological constraints (Planck) + Dark Matter Detection (microscopic), allow us to begin to probe the “Dark Ages”.
• Additional data improves these bounds
ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez, and O. Ozsoy (Syracuse)
Recent results of Fan and ReeceSee also: Cohen, Lisanti, Pierce, and Slatyer 1307.4082Fan and Reece 1307.4400
Reheat temperature must be above 1 GeV for wino
Partial list of many things I did not mention
• Gravitino Problem (model dependent -- difficult issue)
• Baryogenesis?Affleck-Dine + moduli decay can address this more work should be done: e.g. Arxiv:1108.5178 with Kane, Shao, and Yu
• Dark Radiation / axion background / Neff (Conlon / Marsh / Cicoli)
• Gravity Waves / Preheating? (in progress with M. Amin, and Z. Zhou)
• Consequences for Matter Power Spectrum / mini-halos / Non-gaussianity (work in progress with O. Ozsoy)
• Effect on CMB last scattering and reionization (work in progress with Cora)
• In some models moduli can be lighter Large Volume Stabilization in Type IIB (work in progress with M. Cicoli)
• Behavior of moduli during inflation (work in progress with K. Sinha and D. Marsh)
• Life without SUSY?