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Dark Matter direct and indirect detection
Martti Raidal
NICPB, Tallinn, Estonia
07.01.2015 NORDITA Winer School 2015
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07.01.2015 NORDITA Winer School 2015 2
We are experiencing very interesting period in fundamental physics
–
there are paradigm shifts in several fields
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Instead of introduction:
A lesson from the LHC
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LHC discovered the Higgs boson
17.12.2014 Frascati, 2014 4
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All LHC + Tevatron data - 10σ signal
17.12.2014 Frascati, 2014 5
P. Giardino, K. Kannike, I. Masina, M. Raidal, A. Strumia,arXiv:1303.3570
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Tests of Higgs couplings
17.12.2014 Frascati, 2014 6
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New physics enters only in loops
17.12.2014 Frascati, 2014 7
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At the same time ….
• LHC:– No SUSY discovered yet – No signals of compositness, no new resonances – No extra dimensions– No unexpected results
• Precision physics and flavour physics:– No new sources of flavour and CP violation– No higher dim. operators below 10-100 TeV
17.12.2014 Frascati, 2014 8
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This is exactly opposite to the expectations by naturalness:
• All scalar masses must be at cutoff scale …
• … unless there exists a stabilizing mechanism at EW scale
• … or Nature is fine tuned
17.12.2014 Frascati, 2014 9
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17.12.2014 Frascati, 2014 10
The hierarchy problem is properly named: it is not the "quadratic divergence problem”
It concerns the physical hierarchy of physical particles
Naturalness is a real, physical principle for NP
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The lesson
Physics is experimental science!
• No SUSY seems to be around the corner
• Higgs indicates no GUTs
• Community is polarized in rethinking naturalness
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Dark Matter comes to rescue!
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Outline of my lectures
• Dark Matter – the evidence
• Dark Matter candidates
• Ways to detect Dark Matter – direct, indirect, colliders, dark matter self-interactions
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History of DM Jan Oort (1932) Fritz Zwicky (1933)
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Movement of starsin the Galaxy
Movement of galaxiesin clusters
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Evidences for DM
• Small scale (galactic sizes/distances)
• Medium scale (galaxy clusters)
• Large scale (observable Universe)
• DM is dark because it is seen only through its gravitational interaction. No interaction with SM seen so far!
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Small scale - rotation curves of galaxies
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Medium scale – galaxy clusters• Velocity dispersion of galaxies in clusters• Gravitational lensing
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Medium scale – bullet clusters
• Kills MOND, constrains DM self-interactions07.01.2015 NORDITA Winer School 2015 18
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Large scale
• Cosmic Microwave Background (CMB) anisotropies
• Large Scale Structure (LSS)
• Baryon Acoustic Oscillations (BAO)
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The history of Universe
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Anisotropies in the Cosmic Microwave Background
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The ESA Planck satellite
Fluctuations 10-5
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CMB tells the content of the Universe
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• The first peak – overall mass-energy content Ω• The second peak – baryonic matter Ωb
• The third peak – cold Dark Matter ΩDM
• The Universe can be described with ΛCDM
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Energy budget of the Universe
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Also SN observations confirm the accelerated expansion of the Universe
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CMB polarization
• Induced by Thomson scattering at the end of recombination – very small effect
• Consistency check for inflation
• Planck Mission polarization data must come out these days!
• The rumor is …..
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Two types of polarization – E-modes and B-modes!
• BICEP2 claims to measure primordial B-modes– Fluctuations of gravity– Gravitational lensing (excluded)
• Can also be induced by dust• Assuming the first, the measured tensor-to-
scalar ratio r=0.2 implies the scale of inflation to be 1016GeV
• This is our only realistic exp. test of quantum nature of gravity
17.12.2014 Frascati, 2014 25
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Tension with Planck data
17.12.2014 Frascati, 2014 26
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Implications for inflation and gravity?
• V=(1016)4 GeV4 is sub-Planckian – particle physics is under control
• But Lyth bound implies trans-Planckian field excursions
• What about operators likeϕ6, ϕ48, ϕ234567 which all must be there according to standard paradigm?• Inflation data shows no trans-Planckian operators!
17.12.2014 Frascati, 2014 27
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Planck published first dust data
17.12.2014 Frascati, 2014 28
The BICEP2 signal strength can be explained with• r=0.2 and no dust• R=0 and dust only
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One needs to study correlations between the BICEP2 and dust maps
17.12.2014 Frascati, 2014 29
• Done by theorists• Small but significant correlation found
• r=0.1±0.04
This analyses must be repeated by experiments
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Large scale - BAO
Matter distributionhas a preferred scale
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Acoustic peak dependson DM and baryon content
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Large Scale Structure
• Primordial fluctuations are seeds of structure
• Structure formation happens dimension by dimension
• Structure has fractal properties – it repeats itself in different scales
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DM in galaxies - where is it?• DM halos are believed to
be spherical (cannot loose energy)
• N-body simulations suggest rich sub-halo content (satellite and dwarf galaxies observed)
• Detection of DM depends on mass distribution and minimal mass of subhalos
• Detection of DM depends on DM halo properties around Sun
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DM density profiles in galaxies
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Non-relativistic DM velocity distribution
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Problems/challenges/future work
• Core vs. cusp problem - N-body simulations prefer cuspy profiles (NFW, Einasto)
• “Missing” satellites compared to N-body sim.• “Too big to fail” – satellites less massive than sim.
• DM self-interactions?
• Planes of satellites in the Galaxy• Bulge-less disc galaxies • Voids too empty?
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Example – core vs cusp problem• Density profile in dwarfs seems to have a core• Problem of physics or obs./sim.?• Baryonic matter dominatesin the Galactic centre• DM self-interactions, warm DM?
• Solutions:• GAIA satellite will measure movement of stars in our
Galaxy and in dwarf satellite galaxies!• N-body simulations become realistic (baryons, DM self)
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What is the Dark Matter?
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What is the DM mass scale?
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• The SM does not haveviable cold DM candidate!• The SM neutrinos with Σ mi=0.1 eV contribute 0.2% of DM• The SM neutrinos arewarm DM
Whatever is DM, it couples to gravity via Tμν
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Supermassive objects - MACHOs
07.01.2015 NORDITA Winer School 2015 39
Dead stars, planets etc., must be non-baryonic or created before BBN
Microlensing: MACHO fraction <20% for M=M
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Primordial Black Holes (PBH)
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Not predicted by standard cosmology because of small primordial perturbations
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DM as elementary particles
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DM as a thermal relic
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The WIMP miracle
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This mass scale has nothing to do with EWSB
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Warning – many alternatives possible
• DM stabilized by Z3 not Z2
semi-annihilations
• Freeze-in of very weakly coupled particle
very heavy DM possible
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Asymmetric DM
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• DM may be like proton
• The asymmetries in the baryon and DM sectors may be related
Scenarios contain dark forces and selfinteractions
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Paradigm shift in WIMP DM physics
• Instead of Z2-stabilized one thermal relic (SUSY)– Dark sector can be as complicated as visible sector– Multi-component DM– Dark sector can contain dark forces• Dark photons• Dark Yukawa sector• Strong interactions in the dark sector – Dark Techicolor
– Dark Matter can form dark discs (10% of DM in our Galaxy) and/or affect large scale structure
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DM mass scale
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Ultralight scalars: axion-like particles (ALPs)
• If scalar is light, its phase space density is high
Such a DM should be described as a field• To be viable DM, particles must be created at rest
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Initial misalignment mechanism
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The QCD axion Pseudo-Goldstone boson of axial symmetry
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Invented to explain the absence of strong CP violation
Axions solve the strong CP problem
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QCD axion couplingsCouples to gluons and photons due to mixing with the pion
where
Other possible interactions
1 MHz ≈ 4×10-9 eV
nucleon dipole moment d = gda
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Detection principle
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Look for axion-photon conversion• From cosmological sources• Create your own - laser
CAST
ADMXRes. microwave cavity
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Experiments: light-through a wall
• Photons „tunnel“ through a barrier via conversion to axions in a strong magnetic field
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Nucleon electric dipole moment• Given that
– DM is a classical field a– that couples to nucleons as
• then all (local) nucleons will have a time dependent EDM (current bound |dn| < 2.9×10−26 e·cm)
• In the case of the QCD axion
(Molecular EDMs are about 28 orders of magnitude larger.)
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Expected CASPER sensitivity
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The message
New experiments are being planned to test light dark sector properties (APLs, dark photons etc.)
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