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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).