Astroparticle ResultsAstroparticle ResultsRene A Ong (UCLA)Rene A. Ong (UCLA)
Nobel Symposium on LHC Results, May 2013
Astroparticle Physics OverviewAstroparticle Physics encompasses a wide variety of topics:
1) N P ti l /I t ti (BSM)1) New Particles/Interactions (BSM)Dark Matter, Weakly Interacting Slim Particles (WISPs)Other relics (PBH’s, GUT particles, etc.)Lorentz Invariance ViolationLorentz Invariance Violationetc.
2) VHE Astrophysics (VHE = Very High Energy, E > 1012 eV)Point/diffuse sources of VHE γ-rays, CR’s and ν’s.Origin of cosmic raysIntergalactic radiation fieldsetc.
3) Particle PropertiesNeutrino properties (atm solar SN and relic ν)Neutrino properties (atm., solar, SN, and relic ν)Proton, photon and ν interactions at ultrahigh energies etc.
4) Cosmology (a field in its own right)
Outline
Selected set of topics in three general areas:
A. Very High Energy (VHE) Astrophysics• VHE sources of γ-rays (and possibly neutrinos and CR’s)
B. AP Topics Connected to LHC
γ y ( p y )
• Proton-Proton Cross Section at 70 TeV• WIMP DM – Direct and Indirect Detection Results & LHC
C. Other Topics (possibly connected to LHC)• Axions and axion like particles (ALPs)
Future Projects and Summary
(note: some overlap with talk by Lars Bergstrom)
Many Detectors, Many TechniquesCR
Balloon Satellite
CR, γ-ray
BalloonInstruments Instruments
Fermi, AMSPAMELA …
ANITA
AtmosphericCherenkov
PAMELA …
Telescopes Air Shower ArraysHESS, VERITAS
MAGIC
Ground or
Auger …MAGIC …
Ice/Water
Ground orUnderground
DetectorsIceCube …
CDMS Xenon
νCherenkovDetectors
CDMS, Xenon …ADMX, CAST …
Outline
A. Very High Energy (VHE) Astrophysics• VHE sources of γ rays (and possibly neutrinos and CR’s)• VHE sources of γ-rays (and possibly neutrinos and CR s)
VHE Multi-Messenger Astrophysics
EeVBlack Hole p Cosmic RaysHole
eπ
p
P VνActive Galactic
Jete
PeVNeutrinos
γNucleus (AGN)
GeV/TeVγ−rays
TeV γ-ray Sky c2013
~140 sources
tevcat.uchicago.edu
• Almost all discoveries made by atm. Cherenkov telescopes• Detailed information from spectra, images, variability, MWL …
VHE γ-ray Sky c2013 + HE γ-ray Sky
~140 sources ~2000 sources
tevcat.uchicago.edu
VHE/UHE ν Sky c2013
tevcat.uchicago.edu
• Neutrino detections should be coming soon !
The High Energy Milky WayThe High Energy Milky WayH E S S (TeV)
Extended sources, size typically few 0.1o
few 10 pcH.E.S.S. (TeV) few 10 pc
Fermi-LAT (GeV)Courtesy of W. Hofmann
The Many Faces of TeV Particle Acceleration
Pulsars
AGN Star Forming RegionsSupernovaRemnantsRemnants
NS dynamo
Jets powered by accretion or unipolarInduction UHECR’s ?
SNRs, cosmic rays,molecular clouds.
F i A l tiNS dynamo Induction. UHECR s ? Fermi Acceleration
Binary SystemsGamma-RayBursts Unidentifieds
VERITAS
Accretion jetsor stellar windsStar collapse
relativistic jets???
Latest IceCube ResultsSimple Search for Diffuse ν’s
Look at events all directions Look for upward (E>1 PeV) and downward (E>100 PeV) events
Find 2 events (0.08 exp. bkgnd)
C. Kopper, LLWI 2013
~1.1 PeV (“Bert”) ~1.2 PeV (“Ernie”)( )
Not consistent with atm. background norconsistent with expected cosmogenic ν.
… perhaps the “tip of the iceberg” ?!
Outline
B. AP Topics Connected to LHC• Proton-Proton Cross Section at 70 TeV• WIMP DM – Direct and Indirect Detection Results & LHC
P-P Cross-Section @ 60 TeV (Auger)Auger measures p-air collisions at Elab ~ 1018-1018.5eV
Cross-section scales with dn/dxmax, wherei t f h d l txmax = point of max shower development.
Glauber formalism to infer pp cross-section.
dn/dxmax distribution P. Abreu et al., arXiV: 1208.1520
Auger results consistent with smooth extrapolation from LHC.
Dark Matter
Postulated in the 1930’s, dark matter (DM) remains one of the deepest mysteries of science.p y
There is now overwhelming evidence for existence of DM.for existence of DM.
What we do know: Dark matter:
1E 0657-56
• is non-baryonic• is non-relativistic (cold or warm)• is stable on cosmological times
Planck
is stable on cosmological times• has v. weak interaction with SM matter• comprises ~85% of the matter in Universe
One of the clearest indications for physicsbeyond the standard model !
Planck
What is Dark Matter ?We don’t know … many candidates !
Candidate Mass Range “Bonus”
WIMP 1 – 104 GeV “WIMP miracle” (new physics ~WI scale)
Axion 1 μeV – 1 meV Strong CP problem (PQ symmetry)
Sterile ν various Accel /reactor ν experimentsSterile ν various Accel./reactor ν experiments
Many others various
C ld d k tt (CDM) i tt ti d fit h f thCold dark matter (CDM) is attractive and fits much of theastrophysical/cosmological data, but …
1 CDM h ll k bl ( i i t llit )1. CDM has well-known problems (e.g. missing satellites, cusps …)“warm” DM, “fuzzy” DM, self-interacting DM, …
2 DM i ht i t f lti l tit t i2. DM might consist of multiple constituents, i.e. “Dark Sector”, such as asymmetric DM
WIMP DM Complementary Approaches
Heavy particle prod.MET + jets
WIMP annihilationIn the cosmos MET + jets
Weak pair prod.MET + monojet
LHC P d ti
Indirect Detection
LHC ProductionWIMP-NucleonElastic scattering
Direct Detection
WIMP Direct Detection
Particle Physics Astrophysics
P ti l Ph iParticle Physics:Elastic scattering of WIMPs off nuclei
a) Spin-independent (coherent) ~ A2) p p ( )b) Spin-dependent (target has net spin)
Astrophysics:D. Bauer, LLWI 2013
p yIsothermal, spherical halo with MB velocity dist, f(v)dv, for vo ~ 230 km/s and ρχ ~ 0.3 GeV/cm3
Signals: Challenges:1) Counting (eliminate SM interactions) 1) Very low bkgnd required2) Annual modulation 2) Low E threshold (<25 keV)2) Annual modulation 2) Low E threshold (<25 keV)3) Diurnal modulation 3) Stable, large mass detectors
Underground Labs & Some Expts
PicassoCOUPP
LUXSuperCDMSCoGeNT
DAMA
XMASSEdelweiss
CoGeNT Xenon100CRESST
PANDAX
D Bauer LLWI 2013 Selected expts in red
There are ~20 operational (or soon to be operational) experiments !
D. Bauer, LLWI 2013 Selected expts in red
Detection Techniques by Experiment
P D ki A 2013
The use of two detection techniques allows for cleaner separation ofnuclear recoils from background
P. Decowski, Aspen 2013
nuclear recoils from background.
Also important is use of different targets – different A, properties.
WIMP Direct Detection Limits
Spin Independentpotential
Spin Dependent
signals
COUPPSuper KXenon100 MSSM
IceCube
Super-K
MSSM
(Potential signals: DAMA/LIBRA, CRESST, CoGeNT – see backup slides)
SuperCDMS Results (2013)SuperCDMSSi detectors, more sensitive below 15 GeV
P b f 3 t f b d 5 4% b t
R. Agnese et al.,arXiV:1304.4279
Prob for 3 evts from bgnd ~ 5.4%, butProb for measured energies ~0.19%.
Beforei itiming cut
After timing cut
Max. likelihood @ m = 8.6 GeV, σ = 1.9 x 10-41 cm2
Not yet statistically significant.
WIMP Indirect Detection
γγGeV Fermi, AGILE
(Satellite)WIMP Annihilation
γγZγ
γ (cont.)Gamma
rays TeV HESS, MAGICVERITAS
(Atm. Cherenkov)
G V T VνfromSun
NeutrinosGeV-TeVIceCube, AntaresSuper-KSun(Ice/Water Cherenkov)
Anti-matter e+,p, din CR
- - GeV-TeVPAMELA, Fermi, AMS(Satellite)Particle Physics (Satellite)y
(Uncertainty from mχ, decay modes, etc.)
WIMP Indirect Detection: γ-raysDM di t ib tiDM distributionLine-of-sight Integral
(Uncertainty from unknown DM profile)
Where to look:to look:
What to look for:
D. Hooper,Aspen 2013
WIMP Limits: γ-rays
Fermili li it
Fermi, HESS, VERITASGal. center, dwarf galaxies
γγ line limits
No evidence for a signal in gamma rays
A. Drlica-Wagner, APS 2013
No evidence for a signal in gamma rays,for standard thermal WIMP m > 10 GeV. But …
130 GeV WIMP Line in Fermi Data ?Line evidence: However:
A. Drlica-Wagner, APS 2013
Analysis done using public data & tools
Analysis done by Fermi-LAT team:• Re-processed data, includes
better calibration, reconstructionAnalysis done using public data & tools• Feature near 130 GeV• Near to (but displaced from) the
Galactic center
• 3.4-3.7σ (local), ~2σ (global)• “Peak” seen in Earth limb data,
largely at incident cos(θ) ~ 0.7.• 4.6σ (local), 3.2σ (global)
Systematic Effect ?
Anti-Protons
Secondaryanti-p
Future AMS-02 sensitivityy(note: p-bar/p is plotted)
O. Adriani et al., PRL 105, 121101 (2010)
No evidence in anti-protons
But … what about Positrons ?Clear rise in e+ fraction at high E:(including very recent results from AMS-02)( g y )
But, astrophysicalsources possible:
Local pulsar(Y k l Ki tl & St(Yuskel,Kistler, & Stanev, PRL 103, 051101 (2009)).
But … “leptophilic” models largely ruled out by γ-ray and ν resultsp p g y y γ y(see backup slides). Anti-deuteron signal would be much morecompelling.
WIMP Detection SummaryTrying to make sense of all the results:
Technique Experiment(s) Features Difficulties with DM hypothesisTechnique with “Signal” Features Difficulties with DM hypothesis
Direct DetectionSpin-independent
DAMA, CRESST,CoGeNT
Low EAnnual modulation
Possible unknown bkgnds & large modulation; seemingly ruled out by Xenon100, Super-CDMS.
Direct DetectionSpin-independent Super-CDMS Low E
Si detectors only Near threshold, not significant yet.
Di t D t tiDirect DetectionSpin-dependent No Signal
γ-raysDwarf galaxies
No Signal
γ-raysGalactic center
Fermi-LAT Line near 130 GeV Hard to account for strength of line signal; possible systematic? Not very significant.
Anti-Protons No Signalg
Positrons PAMELA, Fermi,AMS
Rising e+ fractionabove 10 GeV
Requires “leptophilic” models and large σ. Possible astrophysical source(s).DM hypothesis ruled out by γ-ray, ν results.
NeutrinosSun No Signal
Plus, more results not listed here !
WIMP Detection SummaryTrying to make sense of all the results:
Technique Experiment(s) Features Difficulties with DM hypothesisTechnique with “Signal” Features Difficulties with DM hypothesis
Direct DetectionSpin-independent
DAMA, CRESST,CoGeNT
Low EAnnual modulation
Possible unknown bkgnds & large modulation; seemingly ruled out by Xenon100, Super-CDMS.
Direct DetectionSpin-independent Super-CDMS Low E
Si detectors only Near threshold, not significant yet.
Di t D t tiDirect DetectionSpin-dependent No Signal
γ-raysDwarf galaxies
No Signal
γ-raysGalactic center
Fermi-LAT Line near 130 GeV Hard to account for strength of line signal; possible systematic? Not very significant.
Anti-Protons No Signalg
Positrons PAMELA, Fermi,AMS
Rising e+ fractionabove 10 GeV
Requires “leptophilic” models and large σ. Possible astrophysical source(s).DM hypothesis ruled out by γ-ray, ν results.
NeutrinosSun No Signal
Plus, more results not listed here !
WIMP Comparisons to LHC
Making comparisons between:Direct detection results• Direct detection results
• Indirect detection results• LHC results
is, of course, non-trivial; no generic prescriptions and many DOF.
Two general approaches:
1 C i t t f ifi d l1. Compare in context of specific models(e.g. MSSM)
2. Compare using generalized models(e.g. effective field theory models)
Operators for Dirac WIMP
Some LHC Results and Comparisonsi i d i dσscatt spin-ind σscatt spin-dep
<σanh v > ATLAS Collab., arXiV: 1210:4491v2.
• For some operators, LHC limits are quite constraining for mχ < 100 GeV.
• For others, direct or indirect detectorsare more constraining.
• Similar results for CMS• Similar results for CMS(see CMS PAS EXO-12-048,http://cds.cern.ch/record/1525585)
WIMPs: a More General FrameworkD B t l “D k M tt i th C i D d C l t P th
Gluon Interactions Quark Interactions Lepton Interactions
D. Bauer et al., “Dark Matter in the Coming Decade: Complementary Pathsto Discovery and Beyond,” White Paper for Snowmass 2013.
p
1.0 = expected thermal relic cross-section
preliminary preliminary preliminary
• For gluon/quark interactions, LHC competitive or dominatesat energies below ~few 100 GeV.
• For gluon and lepton interactions, direct expts. are important.
• For quark and lepton interactions, indirect expts are important.
Outline
C. Other Topics (possibly connected to LHC)• Axions and axion like particles (ALPs)Axions and axion like particles (ALPs)
Axions as Dark Matter• Axion motivated by strong CP problem (PQ symmetry).
• Constraints (astrophysics, accelerators) on the axion coupling (and mass).
• For a stable relic axion, and a DM candidate:
e.g. for na ~ 2 x1013 /cm3 and ma = 20 μeV, Ωa ~ 0.23.
• Axion: neutral psuedoscalar boson(light cousin of πo)
Produced/detected via Primakoff effect(Sikivie):
Extension to ALPsWISPs: ALPs, hidden photons, chameleons, etc. are components of a “hidden sector”, inspired by string theory extensions of SM.
ALPs = Axion-like-particlesA. Lindner, DPG 2013,
QCD AxionAxion
Coupling-mass diagram for axions and ALPs.
Axion/ALP Current/Future LimitsLaboratory Axions• “Light-shining-through A. Lindner, DPG 2013g g g
-walls”(OSQAR,LIPSS,ALPS …)
Solar Axions• Helioscopes
(C S )(CAST, Tokyo …)
Cosmic ALPs• γ-ray Telescopes(Fermi, VERITAS …)
DM Halo Axions• HaloscopesHaloscopes
(ADMX)
VHE γ-rays as Cosmological Probes
Extragalactic BackgroundExtragalactic BackgroundLight (EBL):
• Optical/IR diffuse backgroundproduced by all star-formationthroughout history of universe.
• γγ interaction probes EBLdensity & uniformity.
• Potential way to measure tiny extragalactic magnetic field (EGMF).
B ~ 10-9 - 10-18 G
Energy1 TeV 1 PeV
Is the Universe too Transparent ?
D. Horns & M. Meyer,JCAP 1202 033 (2012)JCAP 1202, 033 (2012)
Axion conversion ??Axion conversion ??Sanchez-Conde et al.,arXiv:0905.3270
(Some) Future ExperimentsCR
Balloon Satellite
CR, γ-ray
GAPSBalloon
Instruments InstrumentsFermi, AMSPAMELA …
GAPS
Dedicated searchfor anti-D’s.
Sensitivity:ANITA
AtmosphericCherenkov
PAMELA …Gamma-200DAMPE
Ch k T l A (CTA)
Sensitivity:~10-7 /m2/s/sr/GeVSi(Li)
Telescopes Air Shower ArraysHESS, VERITAS
MAGIC
Cherenkov Telescope Array (CTA)γ-rays, 30 GeV–300 TeV; factor 10 sensitivity improvement
Ground or
Auger …MAGIC …
JEM-EUSO
KM3NET
CTA
Ice/Water
Ground orUnderground
DetectorsIceCube …
CDMS Xenon
KM3NET
νCherenkovDetectors
CDMS, Xenon …ADMX, CAST …Many Discussed
SUMMARY
A tremendous amount of activity exists in astroparticle physics. There are new results from a wide variety of experiments.y
VHE γ-rays have opened a new window in astrophysics. TeV particle acceleration is ubiquitous in the cosmos and needs to be
d t d VHE t i t i lik l t f llunderstood. VHE neutrino astronomy is likely to follow soon.
WIMP dark matter is being increasingly constrained by LHC, direct and indirect measurements Interesting anomalies exist but noneand indirect measurements. Interesting anomalies exist, but none (as yet) provide convincing evidence for dark matter.
Numerous other dark matter candidates remain viable. Some (e.g. ( gaxions and ALPs) are being pursued by new projects with improved sensitivity. What other well-motivated candidates remain?
Th l b f f t i t b i l dThere are a large number of future experiments being planned or proposed. A common thread is the wish for “large scale” (> 40 M€) instruments. Not all of these will be realized.
QUESTIONS
1) What is required to eliminate the generic thermal WIMP pict re for dark matter? (or can the WIMP scenario bepicture for dark matter? (or, can the WIMP scenario be falsified?).
2) If LHC does not clearly see any new physics, are there other accelerator experiments that can shed light on d k tt ? (If h ?)dark matter? (If so, how?).
3) When can we say that we have determined the origin3) When can we say that we have determined the originof cosmic rays?
4) What is the appropriate balance of accelerator and non-accelerator projects in particle physics?
Some of the Topics Not Covered
Proton decaySterile neutrinosSterile neutrinosCosmic electronsDM astrophysics – local density, cusps, streams, etc.Th G l ti tThe Galactic centerFermi “bubbles”WMAP/Plank “haze”Fermi “haze”Primordial black holesUHE Cosmic RaysUHE Cosmic RaysGUT-scale particlesLorentz invariance violation (LIV)Relic neutrinos Extragalactic magnetic field (EGMF)Origin of cosmic rays (real progress made here !)Origin of cosmic rays (real progress made here !)…
BACKUP
Some of the Experiments
GeV and TeV γ-ray TelescopesSi Strip TrackerAnti-Coincidence
ShieldFermi-LAT
GeV
Calorimeter
• E = 30 MeV-300 GeV• A ~ 1 m2
• 2 5 sr FOV• 2.5 sr FOV• 0.3o-1.5o resolution
T4Atm. CherenkovTelescopes T2
T3
• E > 50 GeV• A ~ 1 x 105 m2
• ~4o FOV T1• < 0.1o resolution
VERITAS @ Mt. Hopkins AZ, USA
IceCube: ν Detector at South Pole
DetectorMuon
Neutrino
TeV muon-neutrino detection
km3 Neutrino Detector
Installing an IceCube string
km Neutrino DetectorIce-Cherenkov techniqueEnergy range: 1011-1017 eV86 strings x 60 optical modulesIceTop for air showersD C f l iDeep Core for low energies
Schematic of IceCube at South Pole
Auger Project for Ultrahigh Energies
Auger Project in Mendoza, Argentina
Surface array & fluorescence detection
3000 km2 air shower array17
g j g
E > 1017 eVSurface array of 1600 detectors24 fluoresence detectors 4 locations24 fluoresence detectors, 4 locations
A surface detector & fluorescence station
Super CDMS (LNGS)Ge or Si crystals: ionization and phonon signalsT < 50 mK(EDELWEISS II i il )(EDELWEISS II similar)
Interleaved ionization/photonionization/photonsensors
One detector
• Low energy threshold (< 10 keV)• Excellent energy resolution (<1%)• Proven event-by-event background discrimination• (Surface events mimic nuclear recoil)
Xenon100 (Gran Sasso)Dual phase Xe: Ionization and scintillation signals 3D track reconstruction (TPC)(LUX P d X i il )(LUX, PandaX similar)
XENON100 XENON1Ton
• Good self-shielding, pure and homogeneous material• Large A large rate, but less sensitive at lower E• Straightforward to scale to larger volumesStraightforward to scale to larger volumes• (Weaker detector discrimination, maintaining high purity LXe required)
Other Direct Detection ExperimentsSolid state ionization detectorsUltrapure Ge @ 77KCoGeNT
Scintillating CrystalsNaI (Tl)
CoGeNT DAMA/LIBRA, DM-ICE
• V. low E threshold • keV E threshold• Low intrinsic bkgnd• (Hard to distinguish NR from ER)• (Pulse shape to discriminate
• keV E threshold• Large mass large signal• (No event-by-event discrimination)• (Large residual bkgnds, annual
surface from bulk events)(Large residual bkgnds, annualmodulation required)
Evolution of DM Detectors
Year
Anti-Matter Space DetectorsA Drlica-Wagner APS 2013A. Drlica Wagner, APS 2013
e detected by shower shape and TRDe+ detected by magnet
e detected by shower shapee+ detected by magnet
Anti-Matter Space DetectorsA Drlica-Wagner APS 2013A. Drlica Wagner, APS 2013
e detected by shower shapee+ detected by magnet
e detected by shower shape and TRDe+ detected by magnet
Axions
Original motivation – to explain the “strong CP” problem
• QCD contains CP violating termfor non-zero θ
• Expect EDM(n) ~ 10-15 e-cm; current limit 1011 below this!
Peccei Quinn introduce dynamical field which produces an• Peccei-Quinn introduce dynamical field, which produces aneffective potential to drive θ to zero.
f f ( )• The quantum of the field is a particle, the axion (Weinberg-Wilczek).
Axion mass:
fa = decay constanta yInteractions scale as 1 / fa
Laboratory & Solar Axion ExptsCAST (CERN)ALPS (DESY)
LHERA MagnetLaser Magnet Detector
• Decomissioned LHC magnet
Wall
• HERA magnet g• Tracks Sun (3 hrs/day)• Search for conversion to X-rays• Future experiment IAXO (LLNL)
• ALPS-I search in 2010• Search for conversion to X-rays• Upgrade to laser, magnet and p ( )
cavity (ALPS-II).
DM Haloscope (ADMX)ADMX (U. Washington)
• Microwave cavity DM axion search• Phase II construction underway• Operation by 2015Operation by 2015• Cover ma = 2-40 μeV range
VHE γ-ray, CR and ν Astrophysics
TeV γ-ray Sky c1997
4 sources
tevcat.uchicago.edu
TeV γ-ray Sky c2005
13 sources
tevcat.uchicago.edu
The GeV Sky (c 2012)
Extragalactic SourcesExtragalactic Sources(AGN, galaxy clusters, dwarf galaxies, local group,UnIDs)
Galactic Center
Galactic Plane (pulsars, SNRs, binaries, UnIDs)
E t l ti DiffExtragalactic Diffuse
Three-year γ-ray sky seen by Fermi-LAT
Fermi Bubbles
M. Su et al. 2010
Complete Surprise !Very extended (10 kpc) with hard spectrum.Related to earlier history of Galactic center ?
SNRs: Origin of Cosmic Rays
General PictureRecent Data from Tycho’s SNR
Tycho, age = 440y, D = 2-5 kpc
Recent Data from Tycho’s SNRVERITAS Fermi-LAT
., 20
11
, 201
1
Gio
rdan
o et
al.
V. A
ccia
riet
al.
F.
Standard paradigm for CR’sGives luminosity, spectral shape.Several SNRs now provide evidence for hadron acceleration.but … more evidence needed.
Morlino & Caprioli, 2011
Latest Neutrino Results
Event displays of one PeV diffuse neutrino event
C. Spiering, “Gamma 2012”
IceCube neutrino sky map (probability)
No ν’s detected from point sources.Limits now well below initial estimates.
A. Ishihara, “N
Diffuse Search: 2 detected events0 14 expected from background
Neutrino 2012”0.14 expected from background
E > 1015 eVNumber of photoelectrons detected by IceCubefor two shower events, with models/bkgfn.
The 1019 eV Sky (c 2012)P. Abreu et al., 2010
AGN position(3.1° circle)
Event position
EeV sky seen by Auger (E > 55 EeV), 69 events.EeV sky seen by Auger (E > 55 EeV), 69 events.Additional 25 events from Telescope Array (E>57 EeV).
CR’s at the Highest Energies
Auger Telescope Array
S. Westerhoff, “COSPAR 2012”
O i i i till k
S. Westerhoff, “COSPAR 2012”
Origin is still unknownAuger and Telescope Array agree on spectrum – clear cutoff ~6x1019eV
Unclear if GZK effect or source acceleration limitWeakly correlated with nearby AGN/matter
WIMP Direct Detection
WIMP Evidence: Direct Detection
DAMA/LIBRAAnn Modulation is ~9σ effect
R. Bernabei et al., arXiv:1002.1028
Ann. Modulation is 9σ effectIs it due to DM ?
CoGeNT442 live daysLow E threshold & extensiveLow E threshold & extensiveBkgnd studies
2 8σ annual modulation2.8σ annual modulation(4-5 times expected amount)
Continuing to take data C E Aalseth et alContinuing to take data … C.E. Aalseth et al., PRL 107, 141301 (2011)
DM Indirect Detection
Fermi e+ Detection Technique
Neutrino WIMP Detection
• WIMPs scatter off nuclei in Sun and get captured (σSI or σSD).
• WIMP annihilation produces primary or secondary neutrinos.
• Neutrinos detected on Earth in water or ice Cherenkov detectorsNeutrinos detected on Earth in water or ice Cherenkov detectors.
Constraints on Leptophilic Scenario
CMB Constraints• CMB power spectrum sensitive to energy injected near recombination• Limit DM annihilation < σ v> from power spectrum
Some pMSSM Comparisons (Future)
WIMP Comparisons to LHC
T. Tait, Aspen 2013
Future Experiments
ADMX Target Sensitivity
Cherenkov Telescope Array (CTA)
CTA: artist’s conception
Key features of CTA:Factor of 10 more sensitive, better σang and σE than HESS/VERITAS.Wide E range: 25 GeV – 100 TeV.Wide field-of-view (>6o).( )Two sites: S (10 km2), N (1 km2)40-80 Cherenkov telescopes/site.Open observatory.
S. Funk, 2012p y
Complemented by HAWC (wide-field, high duty cycle) in N. CTA and Fermi dark matter sensitivity
Askaryan Radio Array (ARA)ARA:
Very large (~150 km2) radio neutrino detector at South Pole.Uses Askaryan effect to detect radio Cherenkov signal.Main science goal: GZK neutrinos, E > 1017 eV.
Possible layout for ARA at South Pole
ARA Projected Sensitivity
A. Karle, “Neutrino 2012”
ARA 3-year sensitivity to diffuse neutrino flux
JEM-EUSO: UHECRs in SpaceJEM-EUSO:
N fluorescence detector on ISSN2 fluorescence detector on ISS.Exposure/year is x10 Auger.Proposed launch in 2017.p
JEM-EUSO concept
JEM-EUSO on ISS (nadir).JEM-EUSO effective area in nadir & tilt modes.
JEM-EUSO Energy Reach
UHECR exposure versus time.
JEM-EUSO expected event numbers (5 years).