a glimpse on cosmology: mathematics meets the datapeople.na.infn.it/~semgr4/doc/091106.pdfcm 3...
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![Page 1: A glimpse on Cosmology: Mathematics meets the Datapeople.na.infn.it/~semgr4/doc/091106.pdfcm 3 •ρDE ≅1.3×10 −29 g cm 3 Part 2: The Known Unknowns 10 November 2009 Monica Capone](https://reader035.vdocuments.us/reader035/viewer/2022081623/614a3b8312c9616cbc69486b/html5/thumbnails/1.jpg)
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A glimpse on Cosmology: Mathematics meets the Data
A glimpse on Cosmology: Mathematics meets the Data
Naples ‘09 Seminar
by
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Toward a unified epistemology of SciencesToward a unified epistemology of Sciences
...As we know,There are known knowns.There are things we know we know.
We also know There are known unknowns.That is to sayWe know there are some thingsWe do not know.
But there are also unknown unknowns,The ones we do not knowWe do not know...
- D.H. Rumsfeld, Feb 12, 2002, Dept. Of Defense news briefing
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We live at the outskirts of a huge, disk-like collection of stars: the Milky Way galaxy
Part 1: The Known Knowns
What do we see out there?What do we see out there?
1924: Edwin Hubble showed that each galaxy is a collection of stars, just like the Milky Way
QuickTime™ and a decompressor
are needed to see this picture.
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Part 1: The Known Knowns
v = H0 d
1929: Hubble “finds” that the further away a galaxy is, the more rapidly it is moving away from us
It looks the same for every galaxy...
⇒ The universe is expanding!Relative distance at different times is measured by the scale factor a(t). Hubble parameter is related to a via
)(/)()( tatatH &≡
dHv 0=
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The wonderful gravityThe wonderful gravity
• It was Einstein that figured out that gravity is a manifestation of the spacetime curvature
• Using gravity we can detect everything in the universe, even those things that are invisible and transparent somehow (“dark”)
• Everything causes gravity, everything is affected by gravity
Part 1: The Known Knowns
⇒ A guess for the search of invisible matter...
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Gravitational LensingGravitational Lensing
The gravitational field of a galaxy (or a cluster of galaxies) deflects the source light. The more mass, the greater deflection
So we can infer the existence of matter even if we cannot see it!
Part 1: The Known Knowns
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Weighing matterWeighing matterPart 2: The Known Unknowns
So... Some matter in our universe is ordinary - i.e., made of the particles of the Standard Model
But much of it is dark! There is 5 times as much DM in the universe than ordinary matter
Whatever DM is, it is not made of particle(s) we know - it is something new CL0024+1654
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Weighing our universeWeighing our universePart 2: The Known Unknowns
Are ordinary and DM the whole stuff? Is there anything between galaxies (and clusters)?
To weigh the whole universe, measure its expansion rate. We expect it to slow down because of the mutual gravitational pull of all the matter
To track the expansion rate, use the type Ia Supernovae (SnaeIa)
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Part 2: The Known Unknowns
They are exploding white dwarf stars and can be considered as standardizable candles
As luminous as an entire galaxy!
SnaeIa and what you don’t expect
SnaeIa and what you don’t expect
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Part 2: The Known Unknowns
The universe is accelerating!
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What pushes the accelerator?What pushes the accelerator?Well, Dark Energy!
• A form of energy coming from the empty space
• Smoothly distributed through space: does not clump into galaxies and clusters
• Constant density (or changing very slowly) through cosmic time: not diluted by expansion
• Invisible to and not interacting with ordinary matter (only detected via gravity)
Part 2: The Known Unknowns
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No direct evidence for DENo direct evidence for DE
CMB H(z)CMBLSS
Curvature Matter Radiation Dark Energy
H 2 = H02 1− Ωtot( ) 1− z( )2 + Ωm 1+ z( )3 + Ωr 1+ z( )4 + Ωw 1+ z( )3(1+w )[ ]
Part 2: The Known Unknowns
As for DM, we only infer the existence of DE
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CMBr: from noise to Nobel(s)CMBr: from noise to Nobel(s)Part 2: The Known Unknowns
2009 Planck
The oldest light in universe
Discovered the remnant afterglow from the Big Bang . 2.7 K
Blackbody radiation ,Discovered the patterns (anisotropy ) in the afterglow. angular scale ~ 7° at a level ∆T/T of 10-5
(Wilkinson Microwave Anisotropy Probe): angular scale ~ 15’
angular scale ~ 5’,∆T/T ~ 2x10-6, 30~867 Hz
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CMB with PlanckCMB with PlanckPart 2: The Known Unknowns
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Consistency checksConsistency checksPart 2: The Known Unknowns
ρcr ≅1.9 ×10−29 g
cm3
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Join the Dark Side!Join the Dark Side!
Dark side of the Universe: > 95% !!!Dark side of the Universe: > 95% !!!
• ρb ≅ 8.7 ×10−31 g
cm3
• ρDM ≅ 4.75 ×10−30 gcm3
• ρr ≅ 5 ×10−34 g
cm3
• ρν ≅10−32 gcm3
• ρDE ≅1.3 ×10−29 g
cm3
Part 2: The Known Unknowns
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The universe identikitThe universe identikit
Part 2: The Known Unknowns
Quite a “simple” picture but... so many open issues!
++−
−= 2222222
2222 sin1
1)( ϕϑϑ drdrdr
krtadtcds
• (Nearly) spatially homogeneous and isotropic (Cosmological Principle)
• Spatially flat
• Dominated by dark stuff
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Shadows on the Sun: old and new problems in standard cosmology
Shadows on the Sun: old and new problems in standard cosmology
• Flatness problem
• Large-scale smoothness(horizon problem)
• Monopoles
Standard cosmology: standard model of particle physics + FRW
• Galaxies rotation curves
• Large Scale Structure
INFLATION
• Spatially flat universe
• Missing matter/energy
• Accelerating universe
Part 2: The Known Unknowns
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The vacuum is not empty!The vacuum is not empty!
Part 2: The Known Unknowns
Vacuum is not a boring place: it is “full” of the fluctuations of every field in the universe. We know they are there because they affect other forces beside gravity. They also affect gravity because they carry energy
How much energy? ..... Well, ∞!
ρth ∝ 10120 ρexp Renormalize and suitably cut-off and then... !!!
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Gravity
CL0024+1654
The universe promThe universe promPart 2: The Known Unknowns
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The universe promThe universe promPart 2: The Known Unknowns
Weak force (WIMPs)?Anomalies (Axions)?
Scattering?Annihilation?
Evolution?Perturbations?Fifth force?
Variation of constants?
Variable-mass particles?Chaplygin gas?
Gravity
CL0024+1654
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The Known UnknownsThe Known Unknowns
Not to mention:• What came before the Big Bang?
Part 2: The Known Unknowns
•••••••
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Was Einstein wrong?Was Einstein wrong?
Part 2: The Known Unknowns
One possibility could surely be a problem with GR
BUTTo have a successful field theory alternative to GR, one should
Add or subtract degrees of freedom;
Propagation through space (long-range/massless; short-range/massive);
Interactions (coupling to other fields and themselves)
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Part 2: The Known Unknowns
For GR we have gravitons which are massless, spin-2 and coupled to energy
A scalar (spin-0) graviton would look different. It would distort the metric away from GR predictions, e.g. the curvature of the Solar System in a detectable way
Experiments and tests constrain the Brans-Dicke(linked to the coupling of the new dof) parameter to be ω > 40x103
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Example: MONDExample: MONDPart 3: Maths and Data
1984: Milgrom noticed that DM was only needed in galaxy when the acceleration due to gravity falls below a0 ≅ 10-8 cm/s2. He proposed a phenomenological force law in which gravity falls off more slowly when it is weaker, i.e.
1/r2 a > a0
F ∝1/r a < a0
2004: Bekenstein introduced TeVeS, relativistic version of MOND, featuring the metric, a fixed-norm vector Uµ, a scalar field φ, and Lagrange multipliers ηand λ
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TeVeS vs GRTeVeS vs GR
( )12
1 ++= νµµν
µνµν λ UUgFKFLU
( )∫ ++= φπLLRxd
GS U
4
16
1
[ ] ( )ηφφηµ νµνµµν
φ VUUgL −∂∂−−= 0
where
Part 3: Maths and Data
( )[ ])1(ln2424128
3)( 232
20 −++−+= ηηηηη
πµη
BlV
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In classical field ths. symmetries and conserved quantities are essential
Conserved quantities are the integral counterparts of the Lagrangian symmetries
They are related to many fundamental quantities (energy, angular momentum, electric charge, etc.) The Noether’s Th. provides
an explicit and algorithmic correspondence between Lagrangian symmetries and conserved quantities
Variational ApproachVariational Approach
Part 3: Maths and Data
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The Bullet Cluster and Popper’s spiritThe Bullet Cluster and Popper’s spirit
Part 3: Maths and Data
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The Bullet Cluster and Popper’s spiritThe Bullet Cluster and Popper’s spirit
Part 3: Maths and Data
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The Bullet Cluster and Popper’s spiritThe Bullet Cluster and Popper’s spirit
Part 3: Maths and Data
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The Bullet Cluster and Popper’s spiritThe Bullet Cluster and Popper’s spirit
Part 3: Maths and Data
No escape: DM exists!
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Getting rid of DEGetting rid of DE
Part 3: Maths and Data
Beware: Big Bang Nucleosynthesis (BBN) gives stringent constraints: 75% H, 25% He, traces of Li and D
BBN occurred when the universe was 1 minute old and its size was 10-9 its current size. This theory of light elements production in the early universe yields precise quantitative predictions for the mixture of these elements, that is, the primordial abundances
⇒ Deviation from GR must turn on rather late!
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Possible CandidatesPossible Candidates
• Alternative theories of gravitation• Vector Theories• Generalized MOND (TeVeS)
• Branes-Walls• Cosmic strings• .....
• Cosmological constant Λ• Quintessence φ(t, xi) ≈ φ(t) • K-essence• Chaplygin• Cardiassians
Part 3: Maths and Data
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Science is a collaborative effort between us and the universe. We propose ideas, the universe smacks down them...or occasionally agrees...
It’s a good system!
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Facing the FutureFacing the Future
• We can describe the constituents and patterns of our universe. But the description is at least weird. The next challenge is to move from inventory to understanding
• A new generation of experiments will provide crucial clues: satellites, laboratory experiments, large particle accelerators
• One century ago, Physics seemed almost settled, with only a few loose ends to figure out. What followed was a revolutionary upheaval. What is next for us?