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Dark Matter: Evidenze, Candidati, Esperimenti. Gianpiero Mangano INFN, Sezione di Napoli Italy. Summary. A short tour of cosmology Observational evidences: baryons vs matter Relic abundance: baryogenesis vs freezing Candidates Experiments. A basic list of References. - PowerPoint PPT Presentation
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G. ManganoG. Mangano 11
Dark Matter: Evidenze, Dark Matter: Evidenze, Candidati, EsperimentiCandidati, Esperimenti
Gianpiero ManganoGianpiero Mangano
INFN, Sezione di NapoliINFN, Sezione di Napoli
ItalyItaly
22G. ManganoG. Mangano
SummarySummary
A short tour of cosmologyA short tour of cosmology
Observational evidences: baryons vs matterObservational evidences: baryons vs matter
Relic abundance: baryogenesis vs freezingRelic abundance: baryogenesis vs freezing
CandidatesCandidates
ExperimentsExperiments
33G. ManganoG. Mangano
A basic list of ReferencesA basic list of ReferencesC. Jungman, M. Kamionkowski and K. Griest, Phys. Rept. C. Jungman, M. Kamionkowski and K. Griest, Phys. Rept. 267 (1996) 195267 (1996) 195G. Bertone, D. Hooper and J. Silk, Phys. Rept. G. Bertone, D. Hooper and J. Silk, Phys. Rept. 405 (2005) 279405 (2005) 279S. Dodelson, Modern S. Dodelson, Modern Cosmology, Academic Press 2003Cosmology, Academic Press 2003J. Peacock, Cosmological J. Peacock, Cosmological Physics, Cambridge University Press 1999Physics, Cambridge University Press 1999L. Bergstrom, Rept. Prog. L. Bergstrom, Rept. Prog. Phys. 63 (2000) 793Phys. 63 (2000) 793J. Edsjo,J. Edsjo,
Ph.D Thesis, hep-ph/9704384Ph.D Thesis, hep-ph/9704384
44G. ManganoG. Mangano
Talks at ISAPP 2006, SorrentoTalks at ISAPP 2006, Sorrento
F. Donato, Dark Matter Particle PhysicsF. Donato, Dark Matter Particle Physics
C. Galbiati, Direct Dark Matter searchesC. Galbiati, Direct Dark Matter searches
R. Battiston, Searching for Dark MatterR. Battiston, Searching for Dark Matter
http://isapp06na.na.infn.it/http://isapp06na.na.infn.it/
55G. ManganoG. Mangano
A short tour of cosmologyA short tour of cosmology
66G. ManganoG. Mangano
Main pillars IMain pillars I Cosmic Microwave Background (CMB) Cosmic Microwave Background (CMB)
anisotropiesanisotropies
The Universe is spatially flat
Primordial perturbations are order 10-5
1
77G. ManganoG. Mangano
Main pillars IIMain pillars II
Big Bang Nucleosynthesis (BBN)Big Bang Nucleosynthesis (BBN)
Baryons contribute for a very tiny fraction of the total energy 002.0023.02 hb
88G. ManganoG. Mangano
Main pillars IIIMain pillars III Large Scale Large Scale
Structures (LSS) Structures (LSS) SDSS
Primordial perturbations are of the order of 10-5 and grow by gravitational instability
ikxkk e
tPk
k
dkkdttx
2
32
3
3
2
)(
)2(),0( ),(
Main pillars IIIMain pillars III Large Scale Structures (LSS)Large Scale Structures (LSS)
99G. ManganoG. Mangano
Main pillars IVMain pillars IV
The Hubble lawThe Hubble law
The Universe is presently accelerating
7/3/ m
Main pillars IVMain pillars IV The Hubble lawThe Hubble law
1010G. ManganoG. Mangano
Cosmology:
Einstein Equation (dynamics)
Metric (symmetries)
Equation of state
gTGRgR 82
1
22
2
2222
1)( dr
kr
drtadtds
00 ,)( TPPT i
i
1111G. ManganoG. Mangano
Friedmann equation: equation for expansion rate H
2
22
3
8
a
kG
a
aH
Critical density and energy density fraction
G
Hc
8
3 20
7.0
Mpc s Km 100 -1-10
h
hH
c
ii
Hubble parameter versus redshift z=obs/source-1=1/a-1
23420
2 )1()1()1()( zzzHzH Kmr
3-25
-3229
cm GeV 10
cm g 10 9.1
h
hc
1212G. ManganoG. Mangano
Observational evidences: Observational evidences: baryons vs matterbaryons vs matter
1313G. ManganoG. Mangano
Baryon density• spectra of high redshift quasars
• CMB temperature anisotropies
• primordial nucleosynthesis
b 0.05
1414G. ManganoG. Mangano
Matter density I: mass to light ratio
L
MLM
1515G. ManganoG. Mangano
From galaxy redshift survey the total luminosity density L 108 h L Mpc-3
Stellar population of galaxies 1 - 10
For a critical Universe, =1
M/L 1400 h
For a purely baryonic Universe
M/L 20
A lot of dark matter!
1616G. ManganoG. Mangano
Matter density II: the galactic scale
Rotation curves of (spiral) galaxies
Observation of 21 cm hyperfine line in HI clouds
Flat behavior, well beyond the visible disk
Halo with M r
r
rGMrv
)()(
1717G. ManganoG. Mangano
inner part: cuspy or shallow?
N - body numerical simulation predict a steep profile
observations suggest a universal density profile with an exponential thin stellar disk and a flat core with density 4.5 10-2 (r0/Kpc)-2/3 M pc-3
1818G. ManganoG. Mangano
Elliptic galaxies: debated!
Some show evidence via strong lensing
X-ray emission support the idea of hot gas clouds whose hydrostatic suggest the presence of DM
Other observations on sub/inter galactic scale
•Weak gravitational lensing of distant galaxies by foreground structure
•Velocity dispersion of dwarf spheroidal galaxies: high M/L ratio
•Velocity dispersion of spiral galaxy satellites
1919G. ManganoG. Mangano
Matter density III: the Milky way and the
Oort discrepancy
Comparison of mass density of stars and gas ( = 0.1 M pc-3)
with its dynamical determination via gravitational potential
hydrostatic equilibrium
Unclear result: at most a factor 2 larger than observed density
4)(1 2
diskvz
diskz
P
2020G. ManganoG. Mangano
Matter density IV: the galaxy cluster scale
Measures of cluster mass using virial theorem to the observed velocity of galaxies (Zwicky, 1933 first suggestion observing the COMA cluster)
High M/L = 400 suggesting 0.2 – 0.3
Measures of X-ray emission tracing hot gas clouds in rich clusters
kTm
P
rradr
dP
p
)()(
r
Mpc
M
rMKeVkT
1
10
)()8.13.1(
14
2121G. ManganoG. Mangano
Check via gravitational lensing (measure total mass)
and Sunyaev-Zeldovich effect
2222G. ManganoG. Mangano
Matter density V: the cosmological scale
Two main observables:
CMB temperature fluctuation
Power spectrum of structures on large scales
2||
),(),(
lml
lmlmlm
aC
YaT
T
2
3)(
2
)()(
kkP
ek
dkyx yxik
2323G. ManganoG. Mangano
WMAP
=1
b=0.05
m=0.25
2424G. ManganoG. Mangano
2525G. ManganoG. Mangano
2626G. ManganoG. Mangano
Matter density VI: the local density
Crucial for direct and indirect measurements of DM
Observation of rotation curves of the Milky Way
Typical estimated velocity
<v2>1/2 270 Km s-1
2727G. ManganoG. Mangano
Relic abundance: Relic abundance: baryogenesis vs freezingbaryogenesis vs freezing
2828G. ManganoG. Mangano
The effect of DM on structure formation depends upon its mass
For collisionless DM•Hot DM (relativistic during a large fraction of structure formation) like neutrinos erase perturbations on small scales and produces a top-down scenario (large structure form first, small structure form via fragmentation)
•Cold DM (massive particles > KeV) falls in the initial overdensity gravitational well and produce a bottom–up structure formation scheme (small scale structures form first, large scale via clustering)
CDM scenario is preferred by data: •our galaxy appear to be older than the Local Group
•galaxies are observed at redshift as high as z=4
2929G. ManganoG. Mangano
How massive particles can have a large abundance today?
thermodynamical equilibrium
two possibilities
• some particle – antiparticle asymmetry (baryons): works for CDM
• chemical equilibrium is lost for expansion rate is faster than scattering rate at some stage early stage: scenario for both HDM and CDM
eVTT
emT
n
n TmEQCDM 4
3
/2/3
10 ,1)(
3030G. ManganoG. Mangano
more popular scenario: relic DM via freezing of interactions
3131G. ManganoG. Mangano
Which annihilation rate is required to produce 0.3 ?
Departure from equilibrium: Boltzmann equation
d/dt nDM = collisions
leading to
Weak Interacting Massive Particle (WIMP)
)(3 22 EQCDMCDMCDM
CDM nnvHnt
n
v
scmhDM
103.4 13272
3232G. ManganoG. Mangano
CandidatesCandidates
3333G. ManganoG. Mangano
• Standard Model neutrinos
• sterile neutrinos• axions• wimpzillas
•SUSY particles: neutralino,
gravitino
•Kaluza Klein states
•light scalar DM•mirror particles
•self-interacting DM•light scalar DM•………………….
3434G. ManganoG. Mangano
Cosmological limits on neutrino massOverdensity for a wide range of mass
Neutrinos
From 3H decay and oscillation experiments h2 = 0.07
From WMAP and LSS h2 0.007
Only a very small fraction of can be ascribed to massive neutrinos
Neutrinos are HDM
eV
m
1.93
3535G. ManganoG. Mangano
Neutralino: the best SUSY candidate
The Standard Model: electroweak and strong interactions•Quarks and leptons (fermions)
•Intermediate bosons: 1 massless (photon) + 3 massive (W and Z)+ gluons
•Higgs field: spontaneous symmetry breaking mechanism as a mass generating mechanism
3636G. ManganoG. Mangano
Motivations
1) Hierarchy problem
2) Unification problem
3737G. ManganoG. Mangano
General structure
How to embed the Poincarè and internal symmetries into a larger non trivial symmetry group? Coleman-Mandula-‘O Rafertaigh
Graded Lie algebra
fermionbosonQbosonfermionQ || ||
Superspace
and superfield
,,x
),,( x
3838G. ManganoG. Mangano
The Minimal Supersymmetric Standard Model (MSSM)
R parity The lightest SUSY neutral particle is stable
under decay
3939G. ManganoG. Mangano
Constraints from colliders
Present….
….and future
4040G. ManganoG. Mangano
ExperimentsExperiments
4141G. ManganoG. Mangano
Direct detection: look for scattering of DM off matter
elastic scattering: with <v> = 270 Km/s typical energies
of tens of KeV
inelastic scattering: excitation or ionization after
scattering with electrons: recoil + photon emission in ns
Spin independent: grows with mass of the target
Spin dependent: grows with J(J+1) of the target
Indirect detection: products of DM annihilation in the halo, galaxy, Sun
gamma-ray experiments
neutrino telescopes
positron and antiproton experiments
radio-experiments (syncrhrotron radiation emitted by
electrons and protons propagating in the galactic
magnetic field
4242G. ManganoG. Mangano
Direct detection
mass DM
densityenergy DM
mass Atomic
massDetector
Many experiments:
scintillation (DAMA, ZEPLIN-I, NAIAD, LIBRA)
photons (CREST, DRIFT)
ionization (HDMS; GENIUS, IGEX; MAJORANA, DRIFT)
mixed tecniques (CDMS, Edelweiss, WARP, ZEPLIN-II,
ZEPLIN-III, ZEPLIN-MAX)
4343G. ManganoG. Mangano
4444G. ManganoG. Mangano
4545G. ManganoG. Mangano
Genius
CRESST-II
CDMS-Soudan
Edelweiss-II
WARP
Zeplin-max
CDMS
Zeplin-I
Edelweiss-I
4646G. ManganoG. Mangano
v
cmhDM
2392 103.4
4747G. ManganoG. Mangano
Indirect detection I: Gamma-ray experiments
Space-based: in the GeV-TeV range photons interact with matter via pair production (interaction length 38 g cm-2)
EGRET, GLAST
Ground-based: look for e.m. cascade via Cerenkov light. Large background due to ordinary isotropic Cosmic Rays. MC simulation
4848G. ManganoG. Mangano
4949G. ManganoG. Mangano
5050G. ManganoG. Mangano
Indirect detection II: Neutrino Telescopes: Km3 experiments looking for Cerenkov light of muon tracks after v interaction
under ice under water
Amanda, ICECUBE Antares, Nemo, Nestor
5151G. ManganoG. Mangano
5252G. ManganoG. Mangano
5353G. ManganoG. Mangano
Indirect detection III:Positron and antiproton experiments
PAMELA: antiproton 80 GeV<E<180 GeV
positron 50 MeV <E<270 GeV