Dark Matter - ICTP
Transcript of Dark Matter - ICTP
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Dark MatterAlejandro Ibarra
Technische Universität München
Summer School on Particle PhysicsICTP, TriesteJune 2013
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Outline
Lecture 1: Evidence for dark matter.
Lecture 2: Dark matter production.
Lecture 3: Indirect dark matter detection.
Lecture 4: Direct dark matter detection. Collider searches.
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Main results from the previous lecture
SM
SM
DM
DM
annihilation
production
scat
teri
ng
WIMP dark matter
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Main results from the previous lecture
SM
SM
DM
DM
annihilation
production
scat
teri
ng
WIMP dark matter
~ weak interaction
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Main results from the previous lecture
WIMP dark matter
SM
SM
DM
DM
annihilation
scat
teri
ng
Relic abundance of DM particles
Correct relic density if
production
~ weak interaction
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Main results from the previous lecture
SM
SM
DM
DM
annihilation
scat
teri
ng
Relic abundance of DM particles
Correct relic density if
(provided )
WIMP dark matter
production
~ weak interaction
DM
DM
Z0SM
SM
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Fifteen years ago...Cosmic antiprotons Collider experiments
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TodayCosmic antiprotons Collider experiments
Beam energy: 4000 GeVIntegrated luminosity: 23.26 fb-1
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End of this decadeCosmic antiprotons Collider experiments
Beam energy: 6500 GeVIntegrated luminosity: 500 fb-1
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Dark matter distribution
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The universe at T~1 GeV
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200 million years after the Big Bang
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Distance Sun to Earth ~ 8.5 kpc
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Density distribution of dark matter particles:
Assume spherical symmetry (in a first approximation).
Radial distribution:
NFW
Isothermal
Moore
Einasto
Normalized such that the local DM density is r(r=8.5 kpc) = 0.38 GeV/cm3
NFW, Isothermal, Moore
Einasto
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General idea:1) Dark matter particles annihilate or decay producing a flux of stable particles: photons, electrons, protons, positrons, antiprotons or (anti-)neutrinos.
DM
DM
DM
Indirect dark matter searches
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Indirect dark matter searchesGeneral idea:1) Dark matter particles annihilate or decay producing a flux of stable particles: photons, electrons, protons, positrons, antiprotons or (anti-)neutrinos.
2) These particles propagate through the galaxy and through theSolar System. Some of them will reach the Earth.
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General idea:1) Dark matter particles annihilate or decay producing a flux of stable particles: photons, electrons, protons, positrons, antiprotons or (anti-)neutrinos.
3) The products of the dark matter annihilations or decays are detectedtogether with other particles produced in astrophysical processes (for example, cosmic ray collisions with nuclei of the interstellar medium).The existence of dark matter can then be inferred if there is a significant excess in the fluxes compared to the expected astrophysical backgrounds.
Indirect dark matter searches
2) These particles propagate through the galaxy and through theSolar System. Some of them will reach the Earth.
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General idea:1) Dark matter particles annihilate or decay producing a flux of stable particles: photons, electrons, protons, positrons, antiprotons or (anti-)neutrinos.
3) The products of the dark matter annihilations or decays are detectedtogether with other particles produced in astrophysical processes (for example, cosmic ray collisions with nuclei of the interstellar medium).The existence of dark matter can then be inferred if there is a significant excess in the fluxes compared to the expected astrophysical backgrounds.
Indirect dark matter searches
2) These particles propagate through the galaxy and through theSolar System. Some of them will reach the Earth.
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Indirect dark matter searchesAntimatter
Gamma-rays
Neutrinos
Production
Propagation
Detection
of
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AntimatterAntimatter
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The production is described by the source function: number of particles produced at a given position per unit volume, unit time and unit energy.
ProductionProduction
DM
DM
DM
Annihilationrate r2
Decayrate r
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PropagationPropagation
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PropagationPropagation
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Propagation
h=100 pc
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Propagation
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PropagationR = 20 kpc
L=1-15 kpc
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Propagation
xy
zR = 20 kpc
L=1-15 kpc
f : number density of antiparticles per unit kinetic energy
interstellar antimatter flux:
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Propagation
xy
zR = 20 kpc
L=1-15 kpc
Source term
dark matter annihilation
dark matter decay
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Propagation
xy
zR = 20 kpc
L=1-15 kpc
Source term
dark matter annihilation
dark matter decay
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Propagation
xy
zR = 20 kpc
L=1-15 kpc
Source term
dark matter annihilation
dark matter decay
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Negligible for positrons. For antiprotons,
Propagation
xy
z
Annihilation term
Tan, Ng
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Propagation
xy
z
Convection term ● Due to the Milky Way galactic wind. ● It drifts particles away from the Galactic disk. ● Difficult to model. Assume:
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● Due to inverse Compton scattering on the interstellar radiation field (starlight, thermal radiation of dust, CMB)and synchrotron radiation.● Negligible for antiprotons and antideuterons● Can be modelled
Propagation
xy
z
Energy loss term
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● Energy loss due to Inverse Compton scattering: e+g e+g
Porter et al.
ge= Ee/me Lorentz factor.
Ge=4 ge e/me
q=Eg/G(Ee-Eg)
sT=0.67 barn Compton scattering cross section in the Thomson limit.
Number density of photons in ISRF
● Energy loss due to synchrotron radiation:
Approximately
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● Energy loss due to Inverse Compton scattering: e+g e+g
Porter et al.
ge= Ee/me Lorentz factor.
Ge=4 ge e/me
q=Eg/G(Ee-Eg)
sT=0.67 barn Compton scattering cross section in the Thomson limit.
Number density of photons in ISRF
● Energy loss due to synchrotron radiation:
Approximately
Not very well known,though...
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xy
z
Diffusion term● Due to the tangled magnetic field of the Galaxy.● Difficult to model. Assume
b = velocity = rigidity
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Maurin, Donato, Taillet, Salati '01
K0, , Vc
(as well as L) must be determined with measurementsof other cosmic ray species (mainly B/C ratio).
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Propagation inside the Solar System
solar modulation parameter
F=500 MV 1.3 GV
In the “force field approximation”,the flux at the top of the atmosphere (TOA)is related to the interstellar flux (IS) by
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Gast, Schael '09
Cosmic ray proton spectrum as measured by BESS, AMS-01 and PAMELA
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PAMELA collaborationarXiv:1007.0821
Experimental results: antiprotons
Fairly good agreement between the measurements and the theoretical predictions from collisions of cosmic rays on the interstellar medium p p → p X
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Expectations from theory
A concrete example in the minimal supersymmetric standard model.TeV 10-26 cm3s-1
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Expectations from theory
A concrete example in the minimal supersymmetric standard model.TeV 10-26 cm3s-1
sv = 3 10-26 cm3s-1
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Expectations from theory
A concrete example in the minimal supersymmetric standard model.TeV 10-26 cm3s-1
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Expectations from theory
A concrete example in the minimal supersymmetric standard model.TeV 10-26 cm3s-1
Annihilation rate “boosted”!
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Experimental results: positrons
Expected from “secondary production”,namely collisions of cosmic rays on theinterstellar medium (p p → e+ X).
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Experimental results: positrons
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Experimental results: positrons
PAMELA coll.arXiv:0810.4995
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Experimental results: positrons
AMS-02 coll.Phys.Rev.Lett. 110 (2013) 14, 141102
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More puzzles: the electron+positron flux
Abdo et al.ArXiv:0905.0025
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Present situation:
Evidence for a primary component of positrons (possibly accompanied by electrons)
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Cholis et al.arXiv:0811.3641
An electron/positron excess could arise from dark matter annihilations ...
Dark matter interpretation
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… or dark matter decays
“Democratic” decay n
Ibarra, Tran, Weniger
mDM=2500 GeV
mDM=600 GeV
AI, Tran, WenigerarXiv:0906.1571
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sv = 3 10-26 cm3s-1
Is this the first non-gravitational evidence of dark matter?
“Extraordinary claims require extraordinary evidence” Carl Sagan
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Beware of backgrounds!
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Pulsars Pulsars areare sources sources of high energy of high energy electrons electrons && positrons positrons
Atoyan, Aharonian, Völk;Chi, Cheng, Young;Grimani
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Pulsar explanation I: Geminga + Monogem
Monogem (B0656+14)Geminga
T=370 000 yearsD=157 pc
T=110 000 yearsD=290 pc
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Nice agreement. However, it is not a prediction!● dN
e/dE
e E
e
-1.7 exp(-Ee/1100 GeV)
● Energy output in e+e- pairs: 40% of the spin-down rate
Pulsar explanation I: Geminga + Monogem Grasso et al.
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● dNe/dE
e E
e
-a exp(-Ee/E
0), 1.5 < a < 1.9, 800 GeV < E
0 < 1400 GeV
● Energy output in e+e- pairs: between 10-30% of the spin-down rate
Pulsar explanation II: Multiple pulsars Grasso et al.
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The origin of the positron excess is still unclear:
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The origin of the positron excess is still unclear:
Dark matter? Probably not.
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The origin of the positron excess is still unclear:
Dark matter? Probably not.
Pulsars? Perhaps yes.
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The origin of the positron excess is still unclear:
Dark matter? Probably not.
Pulsars? Perhaps yes.
Something else? Perhaps yes.