introduction to inflation non...
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![Page 1: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/1.jpg)
Daniel Green
CITA
Introduction to Inflation:
Non-gaussianity
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Outline : Lecture 2
Non-gaussanity in Single-field
!
Single-Field Consistency Conditions
!
Multifield inflation
!
Cosmology after Planck
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References : Lecture 1
The Effective Field Theory of Inflation
Cheung, Creminelli, Fitzpatrick, Kaplan, & Senatore
arXiv : 0709.0293
!Equilateral Non-Gaussanity and
New Physics on the Horizon
Baumann & DG
arXiv: 1102.5343
!
See Baumann’s TASI lectures for more background
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References : Lecture 2
Consistency Conditions:
!
Non-gaussian features of primordial fluctuations
Maldacena
astro-ph/0210603
!
Single-Field Consistency Condition for the 3pt func.
Creminelli & Zaldarriaga
astro-ph/0407059
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References : Lecture 2
Conventional Multifield:
!
The Effective Field Theory of Multifield Inflation
Senatore & Zaldarriaga
arXiv : 1009.2093
!
NG in models with a varying inflaton decay rate
Zaldarriaga
astro-ph/0306006
!
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References : Lecture 2
Quasi-Single Field Inflation
!
Quasi-Single Field Inflation & NG
Chen & Wang
arXiv : 0911:3380
!
Signatures of Supersymmetry of the Early Universe
Baumann & DG
arXiv : 1109.0292
!
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References : Lecture 2
Fun Applications
!
Planck Suppressed Operators
Assassi, Baumann, DG & McAllister
arXiv : 1304.5226
!
Cosmological Collider Physics
Arkani-Hamed & Maldacena
arXiv : 1503.08043
!
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Lightning Review of Lecture 1
Inflation is a period of quasi-de Sitter expansion
!
!
!
!
We can pick some general as long as
!
!
We also needed a clock to end this period
!
!
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Lightning Review of Lecture 1
During inflation, quantum fluctuations produced
!
!
!
!
!
!
!
Flat space intuition applies when
!
Modes free outside the horizon
!
!
expansion
H�1H�1
time evolution
|⌃x� ⌃y| ⇥ a(t) = eHt
|⇤x� ⇤y|
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Lightning Review of Lecture 1
Variations in length of inflation = density fluctuations
!
!
!
!
!
EFT of Inflation = EFT of clock the controls length
!
Single-field = no spectators, just a clock
!
!
!
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Lightning Review of Lecture 1
EFT described by
!
!
!
!!Keeping up to
!
!
!
Define breaking scale
!
!
!
L =M2plH@µU@µU �M2
pl(H2 + H)
+X
n�2
M4n(U)(@µU@µU + 1)n +O(rµr⌫U)
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Energy2
H2
|H|
M2pl
f2⇡ = (58H)2
f2⇡ =
p2⇡�⇣H
2
Energy Scales
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Non-Gaussanity
in Single-Field Inflation
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EFTs include operators of all dimensions
!
The irrelevant operators show where theory breaks
!
!
!
!
Scale hints at the UV origin of our EFT
!
Constraints on from precision measurements
!
!
!
Strong Coupling Scale
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Action contains irrelevant operators
!
!
!
!
Canonically normalize and rescale
!
!
!
!
Guess that strong coupling at !
!
Strong Coupling Scale
L3 =M2
pl|H|(1� c2s)
c2s[⇡@i⇡@
i⇡ � ⇡3]
x = csx
L3 =1
⇤2
h⇡@i⇡@
i⇡ � c2s⇡2i
⇤4 = 2M2pl|H| c5s
(1� c2s)2
! > ⇤
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A more precise measure is perturbative unitarity
!
!
!
!
!
!
Unitarity requires partial wave amplitude
!!
Violated for
Strong Coupling Scale
|a`| 1
2
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Energy Scales
Energy2
⇤2?
f2⇡
H2
|H|
M2pl
Freeze-out
Symmetry breaking
Strong Coupling
Gravity
non-dS evolution
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Non-Gaussanity
Quadratic action leads to gaussian statistics
(i.e. 2-pt function determines everything)
!
We saw that interactions are allowed
!
!
!
At horizon crossing, size of interaction
!
This effect is naturally small (irrelevant) !
!
!
L3 =1
⇤2
h⇡@i⇡@
i⇡ � c2s⇡2i
!2 ⇠ H2
⇤2
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Non-Gaussanity
Using perturbation theory, we compute bispectrum
!
!
!
The precise function is called the “shape” !
The amplitude is typically given in terms of !
!
!
Order one non-gaussian means
!
!
h⇣k1⇣k2⇣k3i = (2⇡)3B(k1, k2, k3)�(~k1 + ~k2 + ~k3)
fNL =5
18
B(k, k, k)
P 2⇣ (k)
fNL ⇠ 105
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Non-Gaussanity
Intuitively, we should expect !
!
!
!
!
!
For the speed of sound term, we get !
!
!
!
fNL�⇣ ⇠ H2
⇤2
f equilateralNL = � 85
325
H2
⇤2(2⇡�⇣)
�1 = � 85
325
f2⇡
⇤2
⇣~k1
⇣~k2
⇣~k3
L3 =M2
plH(1�c2sc2s
⇡(@⇡)2
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Planck looks for this shape in the data
!
!
(68% C.I.)
Courtesy of Fergusson & Shellard
Equilateral
Peaked at:k1 = k2 = k3
Non-Gaussanity
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Energy2
H2
|H|
⇤2 > (4.2H)2
f2⇡ = (58H)2
Strong coupling consistent with
Planck
Non-Gaussanity
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Non-Gaussanity
What would we expect from slow-roll?
!
!
!
Control of background requires
!
Expand in fluctuations to find bispectrum
!
!
!
!
!
L = �1
2@µ�@
µ�� V (�)� 1
⇤4(@µ�@
µ�)2
⇤2 > �
L3 ⇠ �
⇤4��(@��)2 fNL ⇠ f2
⇡�
⇤4=
�2
⇤4⌧ 1
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Energy2
H2
|H|
Strong coupling
Non-Gaussanity
Slow-roll
linear description using
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Energy2
H2
|H|
⇤2 > (4.2H)2
f2⇡ = (58H)2
Not possible in slow roll
Non-Gaussanity
Non-slow roll
EFT of Inflation is still valid
Non-trivial UV Completion
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Non-Gaussanity
General take-aways:
NG is like precision EW tests of the Standard model !
NG is an IR probe of higher dim. effective operators
!
Current constraints are
!
Current tests are not sensitive enough to suggest inflation is weakly coupled (i.e. slow-roll) !
!
!
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Summary
These few assumptions explain:
!
• Gaussianity of fluctuations (irrelevant interactions)
!
• Small amplitude of fluctuations (hierarchy of scales)
!
• Near scale invariance (near de Sitter background)
!
• Small tensor amplitude (scale of inflation)
!
These features are generic (but can be violated with work)
!
!
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Single-Field
Consistency Conditions
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For scalar fluctuations, the metric we use is
!!
!
Last time, we used our gauge freedom to write
!
!
This is a good idea inside the horizon
!
Outside the horizon, need to make predictions
!
!
!
Adiabatic modes
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For scalar fluctuations, the metric we use is
!!
!
Now lets focus on directly
!
Outside the horizon, has important properties:
• Conserved outside the horizon
• Relations between N and N+1 correlation functions
!
!
!
Adiabatic modes
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It all boils down to a simple observation
!
!
This metric has a symmetry
!
!
This is a diffemorphism (it is not physical) !
But we have already “fixed the gauge” !
This is a “large” diffeomorphism
!
!
Adiabatic modes
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But these are connected to physical solutions
!
!
!
But we can’t tell them apart until we take derivatives
!
These solutions must exist: is THE solution when:
• There is only 1 degree of freedom (single-field)
• Thermal equilibrium (controlled by 1 parameter T)
!
!
Adiabatic modes
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Why is this true physically?
Time evolution is determined locally
Since metric is only degree of freedom, must be
!
!
We can’t measure locally because it is pure gauge
Conservation of
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Big picture:
In FRW, is non-linearly realized
(isometries of dS, 3d conformal group)
The “goldstone” is
E.g. it acts like a dilaton
Just like any goldstone - it has interesting
(1) Soft limits
(2) Ward identities relating N and N+1 correlations
!
Adiabatic modes
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Big picture:
Extra degrees of freedom much less constrained
E.g. Conservation no longer required
!
!
!
!
Robust to astrophysics / Easiest to detect !
!
Forbidden by symmetry Sensible possibility
Adiabatic modes
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Squeezed limit :
!
!
!
Squeezed-limit
x�L(x)
�s(x1)
�s(x2)
⇥k1
⇥k2
⇥k3Momentum
conservation
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Squeezed-limit
The canonical example is local NG
!
Long-short coupling from
!
which gives the squeezed bispectrum
!
!
Generally arise from local mode coupling
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Squeezed limit :
!
!
!
Bispectrum determined at horizon crossing
Means we have to wait for
Long mode has long since crossed the horizon
Squeezed-limit
⇥k1
⇥k2
⇥k3Momentum
conservation
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Measures small-scale power coupling to
!
!
Measures short power in the presence of long mode
But long mode is just a diffeomorphism
Squeezed-limit
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In fact, even the is just a coordinate artifact
The long mode cannot be measured locally
But, physical units are different
!
In a physical measurement
!
I.e. there is no “local” non-gaussanity
Squeezed-limit
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Multi-field Inflation
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All particles with are produced
!
!
!
!
!
Energy could be as high as
!
We observe the “decays” to
Why Multifield?
�
�
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Particle spectra during inflation
Types of Multi-field models
mass2
Single-Field Quasi Single-Field Multi-Field
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Particle spectra during inflation
Types of Multi-field models
mass2
Single-Field Quasi Single-Field Multi-Field
Consistency conditions apply
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Particle spectra during inflation
Types of Multi-field models
mass2
Single-Field Quasi Single-Field Multi-Field
May violate consistency conditions
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Basic geometry of multi-field
Conventional Multi-field
Classical Trajectory
Goldstone fluctuates along trajectory
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Basic geometry of multi-field
Conventional Multi-field
isocurvature fluctuates
perpendicular to trajectory
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Curvature perturbation is still length of inflation
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!
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Reheating / ending inflation is a local process
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!
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If we force then it must reproduce single-field
Conventional Multi-field
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Orthogonal directions are not constrained
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!!where
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Small scale power is modulated
!
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Leads to conventional local non-gaussianity
!!!
!
Conventional Multi-field
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This is the “local model” of non-gaussianity
!
(68% C.I.)
Courtesy of Fergusson & Shellard
Local
Peaked at:k1 ⌧ k2 ⇠ k3
Conventional Multi-field
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What makes these orthogonal directions different?
!
!
!
Conventional Multi-field
Constant shift changes
geometry of reheating surface
Constant shift is just a time diffeomorphism
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What makes these orthogonal directions different?
!
!
!
Conventional Multi-field
Short modes experience a new
history around the
background of a long mode
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The picture as drawn is simple:
Assumed instantaneous conversation to adiabatic
Instead, isocurvature modes can exist after inflation
E.g. extra light scalar field with independent fluctuations
Isocurvature may slowly evolve into adiabatic
But, essential physics is always local
!
!
!
Complications
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Inflation and
Particle Detection
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Particle spectra during inflation
Quasi-Single Field Inflation
mass2
Single-Field Quasi Single-Field Multi-Field
Conventional Multifield effects
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Particle spectra during inflationmass2
Single-Field Quasi Single-Field Multi-Field
Can massive fields matter?
Quasi-Single Field Inflation
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It is easy to solve for free massive field
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!
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Mode decays outside the horizon
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!
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Has no “conventional” effect at the end of inflation
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Massive fields in de Sitter
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Does this make sense intuitively?
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At late times
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Using
!
!
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Has no “conventional” effect at the end of inflation
!
Massive fields in de Sitter
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Just like single-field inflation
!
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This alone isn’t equivalent to consistency conditions
!
!
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Goldstone evolution is influenced by isocurvature
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System has memory of the past (after horizon crossing)
Quasi-Single Field Inflation
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Consider a simple model
Quasi-Single Field Inflation
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Consider a simple model
Quasi-Single Field Inflation
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Consider a simple model
Quasi-Single Field Inflation
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Consider a simple model
Quasi-Single Field Inflation
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Consider a simple model !
!
!
!
!
!
Intermediate shape - local : - equil. : !
Amplitude can be large :
Quasi-Single Field Inflation
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Locality + mode coupling would suggest !
!
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It matters when the mode coupling happens
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Freeze-in means short modes cross-horizon
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But remember long mode decays
Squeezed limit
?
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Keeping track of time
!
!
but because of the decay outside the horizon
!
!
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Time dependence that suppressed local shape
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Squeezed limit
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Amplitude can naturally be quite large
!
!
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Weak coupling means
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Perturbative suppression is intuitive
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Scalar is non-gaussian when
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Non-gaussianity of only suppressed by mixing
Amplitude
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But what do we know about these parameters
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SUSY makes natural !
Mixing in the UV should be irrelevant !
!
!
Amplitude
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Squeezed limit important in case of detection
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Current bounds from equilateral shape
!
!
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Hubble scale is determine by tensors
!
!
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Sensitive to Planck supposed couplings
!
!
Amplitude
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Energy2
M2pl
f2⇡
H2 =�
r0.1
� �5.7⇥ 1013 GeV
�2
Amplitude
![Page 71: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/71.jpg)
Massive fields can impact inflationary observables
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Can produce significant non-gaussian signal !
Squeezed limit depends on mass
!
!
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Effect is measurable (we can determine the mass)
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Not degenerate with other effects
!
!
QSFI Summary
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Inflation and
Observations
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We probe initial conditions (inflation) through
!
1. The cosmic microwave background (CMB)
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2. The large scale structure of the universe
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Measure density fluctuations + GR after inflation
!
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Pros / Cons are then just about the details
!
!
Future Directions
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We are still trying to figure out the basic picture
!
!
!
!
Energy2
H2
f2⇡ = (58H)2
Future Directions
??
??
M2pl
![Page 75: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/75.jpg)
We are still trying to figure out the basic picture
!
!
!
!
Energy2f2⇡ = (58H)2
Future Directions
M2pl
H2 =�
r0.1
� �5.7⇥ 1013 GeV
�2
Future CMB
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We are still trying to figure out the basic picture
!
!
!
!
Energy2f2⇡ = (58H)2
Future Directions
M2pl
Future LSSH2
![Page 77: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/77.jpg)
The CMB
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CMB Polarization
Compton scattering polarizes light
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Polarization vector must be transverse to motion
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No polarization if incoming light is uniform
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!
!
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Polarized light requires a non-zero quadrupole
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CMB Polarization
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The polarization pattern depends on the source
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Courtesy of Bicep
CMB Polarization
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Polarization is split into E and B modes
E-modes : measure the scalar density fluctuations
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!
!
!
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More sensitive to cosmological parameters than T
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CMB Polarization
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Polarization is split into E and B modes
B-modes : directs of gravitational waves
!
!
!
!
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Constrains the Hubble parameter during inflation
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CMB Polarization
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Tensor amplitude fixes all the scales in inflation
!
!
!
!
!
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Already a strong constraint on many popular ideas
CMB Polarization
![Page 84: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/84.jpg)
Name of the game is number of detectors
Today (Stage 2): 1000 detectors
ACTpol, BICEP, Keck, Spider, SPT, …
Next few years (Stage 3): 10000 detectors
Advanced ACT, SPT3G, Keck-array,…
Stage 4: 100 000 - 1 000 000 detectors
Strongly endorsed by DOE/NSF
Currently in planning stage
Status of CMB
![Page 85: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/85.jpg)
For raw statistical power we need LSS
!
!
!
!
!
!
!
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Large Scale Structure
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One goal is to test the full non-slow-roll region
!
!
!
Energy
Hubble scale
Non-linear region
Can we exclude this region ??
Large Scale Structure
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One goal is to test the full non-slow-roll region
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In terms of measurable parameters we need
!
!
!
Best limit today is
!
WMAP to Planck(2015) was a factor of 4 improvement
Large Scale Structure
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The brute force approach is to find more “modes” !
When each bin is cosmic variance limited
!
!
!
E.g. From Planck we get roughly
!
!!To improve by we will need modes!
Large Scale Structure
![Page 89: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/89.jpg)
There aren’t many more modes in the CMB
!
!
!
!
!
!
!
!
!
Small scales (high ) dominated by foregrounds
Large Scale Structure
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For raw statistical power we need LSS
Basic advantage: a lot more linear fourier modes
!
Reason 1 : LSS is 3d versus 2d CMB
!!!
Reason 2 : Larger range of scales
!
!
!
!
Large Scale Structure
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Linear regime of LSS
CMB
Large Scale Structure
Figure from Hlozek et al.
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Capable of improving tests of gaussianity
!
Idea: Constraint higher point statistics of galaxies
!
!
!
!
!
!
!
This is the only way to beat current limits from CMB
Large Scale Structure
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Non-gaussanity measurements will be difficult
To take advantage of 3d modes we need:
• Very accurate redshifts
• Good model for galaxy formation
• Control of many many new systematics
!
For these (and other) reasons, no one has actually
performed the analysis that will be needed
!
!
Large Scale Structure
![Page 94: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/94.jpg)
Some problems can be avoided for local NG
!
E.g. galaxy formation depends on
!
Not possible from astrophysics / Newtonian gravity
!
Systematics are still a big problem
!
SPHEREx is best designed approach:
!
!
!
!
Local NG and LSS
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Status of LSS
Taken from Alvarez et al.
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Status of LSS
Taken from Alvarez et al.
Funded
![Page 97: Introduction to Inflation Non gaussianityparticle.physics.ucdavis.edu/seminars/lib/exe/fetch.php?media=2015:… · Quadratic action leads to gaussian statistics (i.e. 2-pt function](https://reader033.vdocuments.us/reader033/viewer/2022053101/60609e01b833dc01cc56a065/html5/thumbnails/97.jpg)
Summary
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Summary
Inflation is more than a scalar field on a flat potential !
In single-field, strongly coupled models still allowed
(i.e. analogue of technicolor still possible)
!
We are also sensitive to full spectrum of particles
(interesting possibilities in weakly coupled models)
!
Probes of physics at (possibly) very high energies
!
Significant experimental progress expected
!
!