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Biermann - Quarks and the Cosmos
1. 2009 Biermann Lectures:
“Quarks and the Cosmos”
I. Cosmic Acceleration and Dark Energy (8 July)
I. Inflation and Beyond (23 July)
I. Future Opportunities and Challenges (28 July)
July 2009
MPA-Garching
Michael S. Turner
Kavli Institute for Cosmological Physics
The University of Chicago
2. CCoossmmoollooggyy
iiss aa
yyoouunngg sscciieennccee
… its story only begins 60 years
after Darwin, 300 years after the
invention of the telescope
Michael S Turner
3. Progress driven by
powerful ideas and
instruments
(especially last 25 years)
Michael S Turner
6. TTwwoo RReeaallllyy IImmppoorrttaanntt IIddeeaass
TThhaatt CChhaannggeedd CCoossmmoollooggyy
with deep connections between quarks and the cosmos
IInnffllaattiioonn:: brief period of rapid
(accelerated) expansion accounts for
smoothness, flatness; heat of the big
bang; and seed inhomogeneities
PPaarrttiiccllee ddaarrkk mmaatttteerr:: bulk of the dark
matter that holds the Universe together
resides in a sea of elementary particles
left over from the big bang
Michael S Turner
7. Cold Dark Matter Transformed
“Astrophysical Cosmology”
… and this Institute!
Michael S Turner
9. TThhee ““CCoonnsseennssuuss CCoossmmoollooggyy””
based upon precision measurements
• From quark soup to nuclei and atoms to
galaxies and large-scale structure
• Flat, accelerating Universe; ΛCDM structure
formation
• Atoms, exotic dark matter & dark energy
• Consistent with inflation
• Precision parameters
–Ω0 = 1.005 ± 0.006 (uncurved)
–ΩM = 0.280 ± 0.013
–ΩB = 0.045 ± 0.0015
–ΩDE = 0.72 ± 0.015
–H0 = 70 ± 1.3 km/s/Mpc
–t0 = 13.73 ± 0.12 Gyr
–Nν = 4.4 ± 1.5
Michael S Turner
10. IInnffllaattiioonn::
TTiimmee ffoorr CCeelleebbrraattiioonn
oorr TTiimmee ffoorr aa CChhaannggee??
See, M.S. Turner, Nature Physics 4, 89 (2008)
Michael S Turner
11. Successes ooff SSttaannddaarrdd HHoott
BBiigg BBaanngg CCoossmmoollooggyy
circa 1980
• Expansion of the Universe
• Big-bang nucleosynthesis (BBN)
• Cosmic Microwave Background (CMB)
• Structure formation by gravitational
instability
“Reliable account of the Universe from
10-5 seconds until today”
12. BBiigg UUnnaannsswweerreedd QQuueessttiioonnss
circa 1980
• Origin of baryons
• Cosmological constant problem
• Before the big bang/initial singularity
• Nature of dark matter
• Dynamite behind the big bang
• Heat of the big bang
• Isotropy, homogeneity and flatness (not generic
initial conditions)
• Origin of seed inhomogeneity Addressed by Inflation
15. ““TTwwoo HHoorriizzoonn PPrroobblleemmss””
SSaaiidd AAnnootthheerr WWaayy
• Horizon at last scattering subtends only 1
degree on the sky; what mechanism causes the
temperature to be so uniform on scales » 1
degree?
• Galactic-sized masses entered the horizon
about 1 year after the big bang; what causal
physics created density perturbations that late in
the history of Universe?
16. CCoossmmiicc IInnffllaattiioonn
• Addresses isotropy, homogeneity &
inhomogeneity, flatness, dynamite, and
heat of the BB
• Lessens (does not eliminate) dependence
upon initial data
• Paradigm, not a model
17. TThhee 22 EElleemmeennttss ooff IInnffllaattiioonn
1. Period of exponential expansion (constant
Hubble Constant and horizon size)
“superluminal expansion’
1. Tremendous entropy production (called
reheating)
23. Homogeneous SSccaallaarr--ffiieelldd iiss
JJuusstt LLiikkee aa FFlluuiidd
≈ -1
• Slow roll (flat part of potential): w ≈ -1
• Rapid oscillation: particle production and
conversion of potential energy to particles
(heat) aka decay of φ particles
24. Given scalar
potential V(φ),
can compute
observables in
terms of V, V’
and V’’
• S = square of CMB
quadrupole due to
density perturbations
≈ 10-10
• T = square of CMB
quadrupole due to
density perturbations
≈ ??
• r = T/S
29. Important FFaaccttss AAbboouutt IInnffllaattiioonn
1. Paradigm, no standard model, many
viable models (new, chaotic, …)
2. Key predictions
• Flat Universe: Ω0 = 1.000
• Almost scale-invariant adiabatic, almost
power-law, nearly Gaussian adiabatic
fluctuations
• |n-1| ~ O(0.1), |dn/dlnk| ~ O(10-3)
• Almost scale-invariant spectrum of
gravitational waves
• nT ~ 0 to -0.1 (i.e., negative)
3. Consistency relation: T/S = -5nT
• Unfortunately, T/S not directly related to n
30. IImmppoorrttaanntt FFaaccttss AAbboouutt
IInnffllaattiioonn,, ccoonntt’’dd
1. Measuring GWs immediately gives
scale of inflation!
1. But, no robust prediction for T/S (=r)
2. Inflationary perturbations + Cold
Dark Matter + “Λ” = ΛCDM scenario
for structure formation (another test)
31. T/S > 0.001 if n > 0.9?
Hoffman/Turner, PRD 64, 02350 (2001)
32. Important FFaaccttss AAbboouutt IInnffllaattiioonn,,
ccoonntt’’dd
7. Inflaton is described by a very
weakly coupled scalar field, weak
coupling makes reheating inefficient
1. Conditions for successful inflation
1. δρ/ρ ≈ 10-5 (hardest)
2. > 60 e-folds of inflation (easy)
3. Reheating to > 10 MeV (BBN), xx GeV
(baryogenesis)
4. No unwanted debris (e.g., gravitinos,
moduli fields, …)
41. SSeerriioouuss tteessttiinngg ooff
IInnffllaattiioonn hhaass bbeegguunn
KKeeyy PPrreeddiiccttiioonnss
• Flat Universe
• Almost scale-invariant, Gaussian perturbations:
|(n-1)| ~ 0.1 and |dn/dlnk| ~ 0.001
• Gravity waves: spectrum, but not amplitude
• Cold Dark Matter Scenario
KKeeyy RReessuullttss
• Ω0 = 1.0 ± 0.006
• (n-1) = -0.04 ± 0.014*; dn/dlnk = -0.032 ± 0.02; no
evidence for nonGaussianity
• r < 0.2 (95% cl)*
*Depends significantly upon the priors assumed
42. Michael S Turner
CCoolldd DDaarrkk MMaatttteerr
SScceennaarriioo
= Particle DM + Inflation
Structure Forms From the
Bottom Up:
First Stars (z ~ 10 -20)
Galaxies (z ~ 2 – 5), Clusters
(z ~ 0 - 2), and Superclusters
(z ~ 0)
43. Tracing the history from a slightly lumpy
Universe to galaxies ablaze
Michael S Turner
56. CMBPol / Astro2010
Science Objectives for a Space Mission
8 yrs
1.2 yrs
4 yrs
CMB Community Reports
Probing Inflation with CMB Polarization, Baumann et al. 2008, ArXiv 0811.3919
Gravitational Lensing, Smith et al. 2008, ArXiv 0811.3916
Reionization Science with the CMB, Zaldarriaga et al. 2008, ArXiv 0811.3918
Prospects for Polarized Foreground Removal, Dunkley et al. 2008, ArXiv 0811.3915
Foreground Science Knowledge and Prospects, Fraisse et al. 2008, ArXiv 0811.3920
57. How Sub-Orbital Program Benefits a Satellite Mission
100 mK 1 mK 100 nK few nK
COBE
1989
Historical Interplay: Suborbital Experiments serve to
- Shape scientific objective of a space mission - Develop experimental methodologies
- Train leaders of future orbital missions - Develop technologies at systems level
CMBPol / Astro2010
WMAP
2001
Planck
2009
Sensitivity
60x
Sensitivity
20x
Sensitivity
>20x
CMBPOL
2022
Woody-Richards Archeops, Boomerang, Maxima
U2-DMR
QMAP, SK, TOCO
Sub-Orbital Precursor Satellite Mission
Multiple
Ground-based
&
Balloon-borne
58. FFoouunnddaattiioonnaall
• Fundamental theory of inflation: Who is φ?
– Many, many models, no compelling theory
– “Landau-Ginzburg” theory of inflation
• Laboratory test of inflation to close the circle
(e.g., produce a φ)
– Recall, “believe in BBN” because of laboratory
measurements (nuclei, nuclear physics cross
sections, etc)
– NB: dark matter is on the same path.
60. GGrreeaatt tthheeoorryy,, bbuutt ……
• No fundamental theory (still at Landau
Ginzburg stage – is there a BCS theory?)
• Does not address initial singularity
– geodesically incomplete
• Like “duct tape”, very useful but …
– Only postpones appearance of inhomogeneity
– not all initial conditions inflate
• Quantum unpredictability
• No laboratory signature/test
61. TTiimmee ttoo bbee bboolldd aaggaaiinn!!
some ideas
• Ekpyrotic (brane-collisions, s l o w
c o l l a p s e rather than rapid expansion
NB: solve horizon problem by d2a/dt2 and da/dt having same
sign, positive or negative
• Cyclic (multiple brane collisions)
• Variable speed of light??
• Pre big bang
No well developed competitor for inflation yet
Potential signatures: nonGaussianity, detection of
gravity waves (anti-signature)
62. SSuummmmaarryy
• Inflation addresses important shortcomings of the
standard model and has been the driving force in
cosmology for 3 decades
• First significant evidence for inflation (flat
Universe, nearly scale-invariant, Gaussian density
perturbations)
• Precision tests of inflation coming soon!
• GWs are smokin’ gun signature (but only
detectable if r > 0.001?)
• Foundational challenges: compelling model &
laboratory tests
• Time for a new bolder idea?
63. Time for Celebration
or a New Idea?
Time will tell
In any case
a most exciting time,
maybe even
a Golden Age
Michael S Turner
Theorists needed!
64. Question is now within
the realm of science
Three ideas – all probably
wrong!
65. neat & tidy!
… but Einstein’s
theory does not
incorporate
quantum
mechanics.
… and the
conditions at
the beginning
are precisely
where quantum
effects should
be critical!
66. Einstein got
the right
answer for
the wrong
reason!
= Emergence of
space and time
70. WWee CCaann TTeesstt WWhheetthheerr oorr
NNoott ““OOuurr PPiieeccee ooff tthhee
MMuullttiivveerrssee”” OOrriiggiinnaatteedd
FFrroomm IInnffllaattiioonn
… well on our way to doing so