The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After...
Transcript of The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After...
![Page 1: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/1.jpg)
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)
![Page 2: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/2.jpg)
Main point of this talk
Universe without SUSY
Universe with SUSY
We can improve inflation constraints by including dark matter constraints.
![Page 3: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/3.jpg)
SUSY and Hierarchies after LHC
No sign of SUSY yet.
SUSY can stabilize the Electroweak Hierarchy
![Page 4: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/4.jpg)
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
![Page 5: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/5.jpg)
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.)
![Page 6: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/6.jpg)
✓ 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)
![Page 7: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/7.jpg)
Which cosmological history results from this framework?
![Page 8: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/8.jpg)
Split SUSY and Top-Down approaches both seem to favor a Non-thermal History for Dark Matter
![Page 9: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/9.jpg)
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
![Page 10: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/10.jpg)
Planck has constrained models of inflation to an impressive level of accuracy
![Page 11: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/11.jpg)
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
![Page 12: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/12.jpg)
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
![Page 13: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/13.jpg)
✓ 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
![Page 14: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/14.jpg)
Planck has constrained models of inflation to an impressive level of accuracy
![Page 15: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/15.jpg)
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
![Page 16: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/16.jpg)
�N ' 10
This leads to some (well known) freedom in Model Constraints
![Page 17: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/17.jpg)
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 )
![Page 18: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/18.jpg)
Universe with SUSY Prior
![Page 19: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/19.jpg)
�Ntotal
' 20
Universe with SUSY Prior
![Page 20: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/20.jpg)
More freedom for inflationary constraints with SUSYArXiv:1307.2453 with R. Easther (Auckland), R. Galvez, and O. Ozsoy (Syracuse)
r
ns
![Page 21: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/21.jpg)
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
![Page 22: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/22.jpg)
Is a universe with SUSY less restrictive?
r
ns
![Page 23: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/23.jpg)
We must account for dark matter
![Page 24: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/24.jpg)
SUSY Wimps in Non-thermal Histories
Dark matter will be dominantly non-thermal:
2nd Reheating from Scalar decay
![Page 25: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/25.jpg)
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:
![Page 26: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/26.jpg)
Indirect Detection Constraints from FERMIArXiv:1307.2453 with R. Easther (Auckland), R. Galvez, and O. Ozsoy (Syracuse)
![Page 27: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/27.jpg)
Current and Future Constraints from XenonArXiv:1307.2453 with R. Easther (Auckland), R. Galvez, and O. Ozsoy (Syracuse)
![Page 28: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/28.jpg)
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)
![Page 29: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/29.jpg)
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
![Page 30: The Post-Inflationary Universe After Planck (and LHC) · The Post-Inflationary Universe After Planck ArXiv:1307.2453 with R. Easther (Auckland), R. Galvez (Syracuse), and O. Ozsoy](https://reader030.fdocuments.in/reader030/viewer/2022041113/5f2086470eefbe387035bd94/html5/thumbnails/30.jpg)
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?