PRE-SUSY Karlsruhe July 2007 Rocky Kolb The University of Chicago Cosmology 101 Rocky I : The...
Transcript of PRE-SUSY Karlsruhe July 2007 Rocky Kolb The University of Chicago Cosmology 101 Rocky I : The...
PRE-SUSY Karlsruhe July 2007Rocky Kolb
The University of Chicago
Cosmology 101Cosmology 101
Rocky I: The Universe Observed
Rocky II: Dark Matter
Rocky III: Dark Energy
Dark Matter: 25%
Dark Energy (): 70%
Stars:0.5%
Free H & He:4%
Chemical Elements: (other than H & He)0.025%
Neutrinos: 0.47%
CDMCDM
Radiation: 0.005%
cmb
dynamics x-ray gaslensing
simulations
power spectrum
TOTAL (CMB) M B
MM
If We Could “See” Dark MatterIf We Could “See” Dark Matter
Navarro, et al.
Matter?Matter?
• Black holes
• Planets
• Dwarf starsbrown red white
• MOND (Modified Newtonian Dynamics)
• Fossil relic from the big bang (WIMP)
MOND Takes a BulletMOND Takes a Bullet
Dark Matter?Dark Matter?• 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, Screw-balls….)
• LSP (neutralino, axino, …) (cold dark matter)
axions
axion clusters
6 40
8 25
10 eV (10 g)
10 M (10 g)
Mass range
Noninteracting: wimpzillas
Strongly interacting: B balls
Interaction strength range
10 WIMPlog GeVM
log 10
(/p
icob
arns
)
Particle Dark Matter CandidatesParticle Dark Matter CandidatesSUSYM GUTM PLANCKMPQf IH
coldthermalrelics w
imp
zilla
gravitino
axion
QCD
STERILEM
STRINGM
Other Scales::
TECHNICOLORM
EXTRA DIMENSIONSM
EWKM
WEAK" "
NeutrinosNeutrinos
• Neutrinos exist:
three active + sterile?
• Neutrinos have mass: Atmospheric ( eV) Solar ( eV)
• Not most of dark mattertoo hot!too light!
45 eVm
• Contribute to hot thermal relic:
Growth of small perturbationsGrowth of small perturbations
Today (13.78 Gyr AB)
• radiation and matter decoupled
•
•
5~ 10T T 6~ 10G G
Before recombination (380 kyr AB)
• radiation and matter coupled
•
•
5~ 10T T 5~ 10G G
AndreyKravtsov
The growth of cosmic seedsThe growth of cosmic seeds
100
My
r
1 G
yr
5 G
yr
tod
ay
The growth of cosmic seedsThe growth of cosmic seeds
Dissipative processesDissipative processes
1. 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
Collisionless dampingCollisionless damping
CDM
HDM
Melchiorri, Dodelson, Serra, Slosar, 2006
meVAll: m eVWMAP: m eV
Collisional dampingCollisional damping
Dissipative processesDissipative processes
1. 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
1. 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.
The evolved spectrumThe evolved spectrum
Cold Thermal Relics*Cold Thermal Relics*
• Particle is stable (or at least has a lifetime greater than age of universe)
• 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 v
* An object of particular veneration.
Cold Thermal RelicsCold Thermal Relics
freeze out
actual
equilibrium
X
T/MX
1010
Rel
ativ
e ab
un
dan
ce
1510
2010
510
010
1 2 31 10 10 10
/e M T
Cold Thermal RelicsCold Thermal Relics
• Particle is stable (or at least has a lifetime greater than age of universe)
• 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 v (TM)n
• Freeze-out at
• Freeze-out abundance relative to entropy density (or photon density)
• Contributing to
01 lnF PlM T n MM
1
0
n
FX X
Pl
M Tn nM
s MM s
10
Cold Thermal RelicsCold Thermal Relics
freeze out
actual
equilibrium
X
T/MX
1010
Rel
ativ
e ab
un
dan
ce
1510
2010
510
010
1 2 31 10 10 10
/e M T
X A(independent of mass)
Cold Thermal RelicsCold Thermal Relics X X AA
X A
X X q q
X
X
q
q
X S
X q X q
X
q q
X
X P
q q X X Xq
q X
• Direct detection (S)
More than a dozen experiments
• Indirect detection (A)
Annihilation in sun, Earth, galaxy. . .
neutrinos, positrons,
antiprotons, rays, . . .
• Accelerator production (P)
Tevatron, LHC, ILC
Cold thermal relics (neutralino)Cold thermal relics (neutralino)
freeze out
actual
equilibrium
X
T/MX
1010R
elat
ive
abu
nd
ance
1510
2010
510
010
1 2 31 10 10 10
/e M T
Cold Thermal RelicsCold Thermal Relics
• s-wave or p-wave?• annihilation or scattering cross section?• co-annihilation?• sub-leading dependence on mass, g*, etc.
Not quite so clean:
Indirect DetectionIndirect Detection
• Neutrinos from the sun or Earth
• Anomalous cosmic rays and rays from galactic halo(s)
• Neutrinos, rays , radio waves from our galactic center
• Role of halo substructure [rate (density)2]
Galactic center: spike cusp, ???Black hole in the galactic center
Small-Scale StructureSmall-Scale Structure
Moore et al.
Small-Scale Structure Small-Scale Structure
Moore et al.
14Cluster 5 10
2 Mpc
M
12Galaxy 2 10
300 kpc
M
Nonbaryonic Dark MatterNonbaryonic Dark Matter
Familiar candidate: a 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
Kaluza-Klein ParticlesKaluza-Klein 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 number KK parity
X
X1 12S S Z
R 1 4S M3 space dimensions
Kaluza-Klein ParticlesKaluza-Klein 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
Sterile Neutrinos & GravitinosSterile Neutrinos & Gravitinos
• weaker interactions• decouple earlier• diluted more• can have larger mass• smaller velocity• “warm”• satellite & cusp problem?
Particle models with sterile neutrinos or gravitinos in desired mass range are “unfashionable.”
Warm Dark Matter
Axion 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 transition
decay of axion strings
2 710 GeV1 eV a
PQ PQ
mf f
BallsBalls
• 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
BallsBalls
• Q-balls exist in MSSM scalars = squarks & sleptons
• Fragmentation of Affleck-Dine condensate
• Relates DM to B
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
Nonthermal Dark MatterNonthermal Dark Matter(Supermassive Relics)(Supermassive Relics)
Production Mechanisms:
• Bubble collisions Chung, Kolb, Riotto
• Preheating Chung
• Reheating Chung, Kolb, Riotto
• Gravitational Chung, Kolb, Riotto; Kuzmin & Tkachev
new application: dark matter(Chung, Kolb, & Riotto; Kuzmin & Tkachev)
• require (super)massive particle “X”
• stable (or at least long lived)• initial inflationary era followed by radiation/matter
Arnowit, Birrell, Bunch, Davies, Deser, Ford, Fulling, Grib, Hu, Kofman, Lukash, Mostepanenko, Page, Parker, Starobinski, Unruh, Vilenkin, Wald, Zel’dovich,…
first application:
(Guth & Pi; Starobinski; Bardeen, Steinhardt, & Turner; Hawking; Rubakov; Fabbi & Pollack; Allen)
Expanding Universe Particle CreationExpanding Universe Particle Creation
density perturbations from inflation
gravitational waves from inflation
It’s not a bug, it’s a feature!
Chung, Kolb& Riotto; Kuzmin & Tkachev)
GeV10 to101for1 1510INFLATON XXX MMM
INFLATONMM X
chaoticinflation
Particle ProductionParticle Production
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.
GeV10 12
Superheavy ParticlesSuperheavy Particles
• supermassive: GeV (~ 1012 GeV ?)
• abundance may depend only on mass
• abundance may be independent of interactions
– sterile?
– electrically charged?
– strong interactions?
– weak interactions?
• unstable (lifetime > age of the universe)?
Wimpzilla Characteristics:Wimpzilla Characteristics:
WIMPZILLA footprints:WIMPZILLA footprints:
Isocurvature modes: CMB, Large-scale structure
Decay: Ultra High Energy Cosmic Rays
Annihilate: Galactic Center, Sun
Direct Detection: Bulk, Underground Searches
Cold Dark Matter: 25%
Dark Energy (): 70%
Stars:0.5%
Free H & He:4%
Chemical Elements: (other than H & He)0.025%
Neutrinos: 0.47%
CDMCDM
Radiation: 0.005%
PRE-SUSY Karlsruhe July 2007Rocky Kolb
The University of Chicago
Cosmology 101Cosmology 101
Rocky I: The Universe Observed
Rocky II: Dark Matter
Rocky III: Dark Energy