the dark universe: dark matter and dark energy · 2018. 11. 15. · particle relic from the...
TRANSCRIPT
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CERN Academic Training Lectures January 2008Rocky Kolb The University of Chicago
The Dark Universe:The Dark Universe:Dark Matter and Dark EnergyDark Matter and Dark Energy
Rocky I:Rocky II:Rocky III:Rocky IV:
The Universe ObservedInflationDark MatterDark Energy
MondayTuesdayWednesdayThursday
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ν
ν
ν
Cold Dark Matter: (CDM) 25%
Dark Energy (Λ): 70%
Stars:0.8%
H & He:gas 4%
Chemical Elements: (other than H & He) 0.025%
Neutrinos: 0.17%
ΛCDMΛΛCDMCDM
+ inflationary perturbations+ baryo/lepto genesis
Radiation: 0.005%
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105
50expectedfrom stars
observed
R (kpc)
100
v (k
m/s
)Vera Rubin
M33 rotation curve
The Dark UniverseThe Dark Universe
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Sofue & Rubin
Rotation CurvesRotation CurvesRotation CurvesCO – central regionsOptical – disksHI – outer disk & halo
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Source
Lens
Observer
Einstein Ring
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Abel 2218 HST
The Dark UniverseThe Dark Universe
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Navarro, et al.
The Dark UniverseThe Dark Universe
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We only see the tip of the iceberg—most of the matter is dark!
Some of the dark matter is ahot gas of hydrogen & helium
But most of it doesn’t seem to be “normal” matter.
Dark MatterDark Matter
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cmb
dynamics x-ray gaslensing
simulations
power spectrum
ΩM ~ 0.3
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Power spectrum for CDMPower spectrum for CDMPower spectrum for CDMmatter-radiation equality
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QSO 1937-1009
Ly−α
Burles et al.Tytler
Baryons ΩB h2 ∼ 0.02BaryonsBaryons ΩΩB B hh2 2 ∼ 0.02∼ 0.02
2BWMAP: 0.0229 0.00073hΩ = ±
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Dissipative ProcessesDissipative ProcessesDissipative Processes
Collisional damping – Silk dampingAs baryons decouple from photons, the photon mean-free path becomes large. As photons escape from dense regions, they can drag baryons along, erasing baryon perturbations on small scales.Baryon-photon fluid suffers damped oscillations.
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Eisenstein
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Eisenstein
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The Evolved SpectrumThe Evolved SpectrumThe Evolved Spectrum
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• MOND (Modified Newtonian Dynamics)
Dark Matter
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Dark Matter
• MOND (Modified Newtonian Dynamics)The Bullet Cluster
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• Size challenged stars• Dwarf starsbrown red white
• MOND (Modified Newtonian Dynamics)
• Particle relic from the bang
• Black holes
• Planets
MACHOS
Microlensing
Dark Matter
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Particle Relic From The BangParticle Relic From The Bang
• neutrinos (hot dark matter)• sterile neutrinos, gravitinos (warm dark matter)
• axions, axion clusters• LKP (lightest Kaluza-Klein particle)
• supermassive wimpzillas• solitons (Q-balls; B-balls; Odd-balls, ….)
• LSP (neutralino, axino, …) (cold dark matter)
axionsaxion clusters
6 40
8 25
10 eV (10 g)10 M (10 g)
− −
−
Mass range
Noninteracting: wimpzillasStrongly interacting: B balls
Interaction strength range
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NeutrinosNeutrinosNeutrinos• Neutrinos exist:
• Neutrinos have mass:Atmospheric (10−2 eV)Solar (10−3 eV)
• Not most of dark mattertoo light!too hot!
2
93 eVmh ν
ννΩ
• Contribute to Ω hot thermal relic:
three active + sterile?
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Dissipative ProcessesDissipative ProcessesDissipative Processes
Collisionless phase mixing – free streamingIf dark matter is relativistic or semi-relativistic particles can stream out of overdense regions and smooth out inhomogeneities. The faster the particle the longer its free-streaming length.Quintessential example: eV-range neutrinos
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Eisenstein
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Eisenstein
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Collisionless dampingCollisionlessCollisionless dampingdamping
CDM
HDM
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WMAP + LSSWMAP + LSSWMAP + LSS
Tegmark et al., SDSS
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WMAP + LSSWMAP + LSSWMAP + LSS
Lesgourgues & Pastor
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Particle Relic From The BangParticle Relic From The Bang
• neutrinos (hot dark matter)• sterile neutrinos, gravitinos (warm dark matter)
• axions, axion clusters• LKP (lightest Kaluza-Klein particle)
• supermassive wimpzillas• solitons (Q-balls; B-balls; Odd-balls, ….)
• LSP (neutralino, axino, …) (cold dark matter)
axionsaxion clusters
6 40
8 25
10 eV (10 g)10 M (10 g)
− −
−
Mass range
Noninteracting: wimpzillasStrongly interacting: B balls
Interaction strength range
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Sterile Neutrinos & GravitinosSterile Neutrinos & Sterile Neutrinos & GravitinosGravitinos
• weaker interactions• decouple earlier• diluted more• can have larger mass• smaller velocity• “warm”• satellite & cusp problem?
Particle models with sterile neutrinos or gravitinosin desired mass range are “unfashionable.”
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Small-Scale Structure SmallSmall--Scale Structure Scale Structure
Moore et al.
14Cluster 5 10
2 Mpc
M×
12Galaxy 2 10
300 kpc
M×
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Small-Scale StructureSmallSmall--Scale StructureScale Structure
Moore et al.
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Particle Relic From The BangParticle Relic From The Bang
• neutrinos (hot dark matter)• sterile neutrinos, gravitinos (warm dark matter)
• axions, axion clusters• LKP (lightest Kaluza-Klein particle)
• supermassive wimpzillas• solitons (Q-balls; B-balls; Odd-balls, ….)
• LSP (neutralino, axino, …) (cold dark matter)
axionsaxion clusters
6 40
8 25
10 eV (10 g)10 M (10 g)
− −
−
Mass range
Noninteracting: wimpzillasStrongly interacting: B balls
Interaction strength range
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• Particle is stable (or at least has a lifetime greater than t0) • There is no associated chemical potential (no asymmetry)• Particle is in LTE at temperatures greater than its mass• Particle remains in LTE until M < T (cold)• Particle annihilates with thermal-average cross section
⟨σ v⟩ = σ0 (T/M)n
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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freeze outactual
equilibrium
XΩ1010−
Rel
ativ
e ab
unda
nce
1510−
2010−
510−
010
1 2 31 10 10 10− − −
/e M T−
T/MX
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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• Particle is stable (or at least has a lifetime greater than t0) • There is no associated chemical potential (no asymmetry)• Particle is in LTE at temperatures greater than its mass• Particle remains in LTE until M < T (cold)• Particle annihilates with thermal-average cross section
⟨σ v⟩ = σ0 (T/M)n
• Freeze-out at
• Freeze-out abundance relative to entropy density (or γ density)
• Contributing
( ) ( )01 lnF PlM T n MM σ+
( ) 1
0
nFX
Pl
M Tns MM σ
+
10
XnMs
σ −Ω ∝ ∝
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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freeze out
actual
equilibrium
XΩ
T/MX
1010−R
elat
ive
abun
danc
e
1510−
2010−
510−
010
1 2 31 10 10 10− − −
/e M T−
• s-wave or p-wave?• annihilation or scattering cross section?• co-annihilation?• sub-leading dependence on mass, g*, etc.
Not quite so clean:
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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X AσΩ ⇒
X X q q+ → +
X
X
q
q
X SσΩ ⇒
X q X q+ → +
X
q q
X
X PσΩ ⇒
q q X X+ → +Xq
q X
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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• Direct detection (σS)More than a dozen experiments
• Indirect detection (σA)Annihilation in sun, Earth, galaxy. . .
neutrinos, positrons, antiprotons, γ rays, . . .
• Accelerator production (σP)Tevatron, LHC, …
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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Indirect DetectionIndirect DetectionIndirect Detection
• Neutrinos from the sun or Earth
• Anomalous cosmic rays and γ rays from galactic halo(s)
• Neutrinos, γ rays , radio waves fromour galactic center
• Role of halo substructure [rate ∝ (density)2]
Galactic center: spike cusp, ???Black hole in the galactic center
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Small-Scale Structure SmallSmall--Scale Structure Scale Structure
![Page 41: The Dark Universe: Dark Matter and Dark Energy · 2018. 11. 15. · Particle Relic From The BangParticle Relic From The Bang • neutrinos ... Strongly interacting: ... Dissipative](https://reader035.vdocuments.mx/reader035/viewer/2022071404/60f81b6985efec077257f1f4/html5/thumbnails/41.jpg)
Favorite cold thermal relic: the neutralino• Study “constrained” MSSM models
• Typical SUSY models consistent w/ collider data have too• small annihilation cross section → too large Ω
• Need chicanery to increase annihilation cross section– s-channel resonance through light H and Z poles– co-annihilation with or– large tanβ (s-channel annihilation via broad A resonance)– high values of m0–LSP Higgsino-like &– annihilates into W & Z pairs (focus point)– …– or, unconstrained
tτ
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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Favorite cold thermal relic: the neutralino• Direct detectors, indirect detectors, & colliders race for discovery
• Suppose by 2010 have credible signals from all three???
How will we know we all seeing the same phenomenon?
• Lots of opinions (papers)– Will learn enough from LHC (Arnowitt & Dutta)– Need ILC (Baltz, Battaglia, Peskin, Wizansky)– Depends where in SUSY space (Chung, Everett, Kong, Matchev)– …
• Let’s hope for this problem!!!!
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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Favorite cold thermal relic: the neutralino
“a simple, elegant, compelling explanation for a complex physical phenomenon”
“For every complex natural phenomenon there is a simple, elegant, compelling, wrong explanation.”
- Tommy Gold
Cold Thermal Relics*Cold Thermal Relics*Cold Thermal Relics*
* An object of particular veneration.
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( )10 WIMPlog GeVM
log 1
0(σ/
pico
barn
s)
Particle Dark Matter CandidatesParticle Dark Matter CandidatesParticle Dark Matter CandidatesSUSYM GUTM PLANCKMPQf IH
coldthermalrelics w
impzilla
gravitino
ν
axion
QCDΛ
STERILEM
STRINGM
Other Scales::
TECHNICOLORM
EXTRA DIMENSIONSM
EWKM
WEAK" "σ
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Kaluza-Klein ParticlesKaluzaKaluza--Klein ParticlesKlein ParticlesKolb & Slansky (84); Servant & Tait (02); Cheng, Feng & Matchev (02)
2 2 2 2 2 25 5
2 2 2 2 2
n n
E p p p n R
p M M n R
= + =
= + =
Quantized Kaluza-Klein excitations
Conservation of momentum conservation of KK mode number
First excited mode (n=1) stable, mass R-1
First excited mode (n=1) stable, mass R-1
needchiral
fermions
KK quantum numberKK parity
X
X1 12S S Z→
R1 4S M×
3 space dimensions
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Kaluza-Klein ParticlesKaluzaKaluza--Klein ParticlesKlein Particles
• LKP = KK photon
• Looks like SUSY
• Beware KK graviton
• Direct detection
• Indirect detection
Kolb, Servant & Tait
Bertrone, Servant, Sigl
Servant & TaitCheng, Feng & Matchev
Cheng, Matchev & Schmaltz
Cheng, Matchev & Schmaltz
1 500 GeVR− =
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Axion Dark MatterAxion Dark MatterAxion Dark Matter. . . about to be ruled out or closing in on detection
•• Pseudo-Nambu-Goldstone boson
• Axion mass:
• Pseudoscalar• Couples to two photons through the anomaly• Very weakly interacting with matter• Origin of axions
phase transitiondecay of axion strings
2 710 GeV1 eV aPQ PQ
mf fΛ
= =
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BallsBallsBalls• Q-balls (non-topological solitons): S. Coleman; T.D. Lee
Scalar field withconserved global charge “Q”
Ground state is a Q-ball, lump of coherentscalar condensate
3 4 :E Q∝ can’t decay to Q free particles
• Q-ball production and evolution:Solitogenesis Frieman, Gelmini, Gleiser & Kolb
Solitosynthesis Frieman, Olinto, Gleiser & Alcock; Greist & Kolb
Statistical fluctuations Greist, Kolb & Masssarotti
Condensate fragmentation Kusenko & Shaposhnikov
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BallsBallsBalls• Q-balls exist in MSSMscalars = squarks & sleptons
• Fragmentation of Affleck-Dine condensate
• Relates ΩDM to ΩB
Kusenko, Shapashnikov & Tinyakov
( )3 4 12(1 TeV) stable for 10BM B B× ≥∼Kusenko & Shapashnikov
( )3 2410 g 10BM B−∼
Affleck-Dine condensate
related!
Baryon asymmetry B-ball dark matter
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Nonthermal Dark Matter(Supermassive Relics)
NonthermalNonthermal Dark MatterDark Matter((SupermassiveSupermassive Relics)Relics)
Production Mechanisms:
• Bubble collisions Chung, Kolb, Riotto
• Preheating Chung
• Reheating Chung, Kolb, Riotto
• Gravitational Chung, Kolb, Riotto; Kuzmin & Tkachev
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First application: density perturbations, gravitational waves from inflation
Expanding Universe Particle CreationExpanding Universe Particle CreationExpanding Universe Particle Creation
1983—present: It’s a feature!
It’s a bug!
Discovery: Schrödinger (1939) The Proper vibrations of the expanding universe“the alarming phenomenon”
New application: dark matter(Chung, Kolb, & Riotto; Kuzmin & Tkachev)
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Chung, Kolb& Riotto; Kuzmin & Tkachev)
GeV10 to101for1 1510INFLATON ≈⇒≈≈Ω XXX MMM
INFLATONMM X
chaoticinflation
Particle ProductionParticle ProductionParticle Production
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Inflaton mass (in principle measurable from gravitational wave background, guess ) may signal a new mass scale in nature.
Other particles may exist with mass comparable to the inflaton mass.
Conserved quantum numbers may render the particle stable.
GeV1012
Superheavy ParticlesSuperheavySuperheavy ParticlesParticles
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• supermassive: 109 − 1019 GeV (~ 1012 GeV ?)• abundance may depend only on mass
• abundance may be independent of interactions
– sterile?
– electrically charged?
– strong interactions?
– weak interactions?• lifetime age of the universe
Wimpzilla CharacteristicsWimpzillaWimpzilla CharacteristicsCharacteristics
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WimpzillasWimpzillasWimpzillas
• Origin of inflationary perturbations from creation of particles inthe expanding universe
• Beautiful ideas often have other applicationsNature uses only the longest threads to weave her patterns…
–– Feynman
• Perhaps origin of dark matter also from creation of particles inthe expanding universe (it’s a long thread!)
• Dark matter may have only gravitational interactions—no accelerator production, no direct detection, no indirect detection(an inconvenient truth)
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WIMPZILLAWIMP
SIZEDOESMATTER
SIZESIZEDOESDOESMATTER
MATTER
Dark Matter
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ν
ν
ν
Cold Dark Matter: (CDM) 25%
Dark Energy (Λ): 70%
Stars:0.8%
H & He:gas 4%
Chemical Elements: (other than H & He) 0.025%
Neutrinos: 0.17%
ΛCDMΛΛCDMCDM
+ inflationary perturbations+ baryo/lepto genesis
Radiation: 0.005%
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Suggested reading:
Origin of (particle) speciesThe Early Universe, Kolb & Turner
Neutrinos in cosmologyJulien Lesgourgues & Sergio Pastor Phys.Rept.429,2006.
Dark Matter Direct & Indirect DetectionGianfranco Bertone, Dan Hooper, Joseph SilkPhys.Rept.405:279,2005.
Other referencesCosmology and the Unexpected.Edward W. Kolb. e-Print: arXiv:0709.3102
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CERN Academic Training Lectures January 2008Rocky Kolb The University of Chicago
The Dark Universe:The Dark Universe:Dark Matter and Dark EnergyDark Matter and Dark Energy
Rocky I:Rocky II:Rocky III:Rocky IV:
The Universe ObservedInflationDark MatterDark Energy
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