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?