Next Generation Next Generation Particle Astrophysics Particle Astrophysics with GeV/TeV with GeV/TeV -Rays-Rays

D. KiedaD. KiedaUniversity of UtahUniversity of Utah

OutlineOutline

Quick VERITAS Update Quick VERITAS Update GeV/TeV GeV/TeV -rays and Dark Matter -rays and Dark Matter

searchessearches GRBs GeV/TeV emissionGRBs GeV/TeV emission Diffuse and point source angular/energy Diffuse and point source angular/energy

rangesranges Roadmap for future Roadmap for future -ray observatories-ray observatories

499 PMT camera

Steel OSS

Control Room

Davies-Cotton f/1.0 Optics. Total area=Davies-Cotton f/1.0 Optics. Total area=110m110m22

Operational at Whipple Basecamp at Mt. Hopkins (1275m) in Operational at Whipple Basecamp at Mt. Hopkins (1275m) in February 2006February 2006

VERITAS Telescopes-1 & 2

CameraCamera

1.8 m

3.5º FOV

•499 PMTs

•Photonis XP2970

•0.15º spacing

VERITAS:1-2VERITAS:1-2Stereo Observations of Mrk 421Stereo Observations of Mrk 421April-May , 2006April-May , 2006Wobble mode: ~10 sigma/30 Wobble mode: ~10 sigma/30 minutesminutes

VERITAS UpdateVERITAS Update 2 VERITAS telescopes operational at Mt. 2 VERITAS telescopes operational at Mt.

Hopkins (Feb 2006)Hopkins (Feb 2006) T3, T4 additional telescopes under construction T3, T4 additional telescopes under construction

now (First light T3: 9/2006; T4: 10/2006)now (First light T3: 9/2006; T4: 10/2006) Expect full 4 telescope array operation by end of Expect full 4 telescope array operation by end of

2006.2006.

T1 & T2 (Dec 2005) T3 assembly (June 9, 2006)

R. ONG 2005 ICRC

Santa Fe 2006

40

Updated ofR. ONG 2005 ICRC

Physics/Astrophysics with GeV/TeV Physics/Astrophysics with GeV/TeV -rays-rays

Active Galactic Nuclei

Extragalactic Background Light

Shell-type Supernova Remnants

Gamma-ray Pulsars

Plerions

Gamma Ray Bursts

Dark Matter (Neutralino)

Galactic Diffuse Emission

Unidentified Galactic EGRET Sources

Lorentz symmetry violation (Quantum Gravity)

SN Nucleosynthesis/Cosmic Ray Origin*

*

*

mSUSY Dark matter Search:mSUSY Dark matter Search:Neutralino-antiNeutralino annihilationNeutralino-antiNeutralino annihilation

Integrate annihilation cross sections

over Dark Matter Galactic Halo density/velocity profiles

to predict gamma ray energy spectrum

But: Galactic Halo density profile for r<1kpc mostly based upon N-body simulations

-> Only see strong signal if cusp in DM profile

->large variations in predicted GeV/TeV gamma ray production rate

->Galactic Mergers may reduce/eliminate cusps

-> Cusps may also form in Galactic Halo?

But: Galactic Halo density profile for r<1kpc mostly based upon N-body simulations

-> Only see strong signal if cusp in DM profile

->large variations in predicted GeV/TeV gamma ray production rate

->Galactic Mergers may reduce/eliminate cusps

-> Cusps may also form in Galactic Halo?

Variations in central Cusp with Variations in central Cusp with recent mergersrecent mergers

HESS Sag A* SpectrumHESS Sag A* Spectrum

Profumo-Dark Matter Conf. UCLA 2006

Diffuse Emission in the GC Diffuse Emission in the GC RegionRegion

(HESS 2006)

N-body simulations of N-body simulations of DM Cusp formation in HaloDM Cusp formation in Halo

Dieand,Kuhlen & Madan2006

•DM cusps form in Halo as well as Galactic Center

•Cups region may persist & be dark (except for DM annhilation)

•High Galactic Latitudes may be easier to observe DM annhilation than GC

•Need unbiased all-sky survey with large detection area (>104 m2) to detect.

•Unable to use optical, radio surveys to predict source regions

•DM cusps form in Halo as well as Galactic Center

•Cups region may persist & be dark (except for DM annhilation)

•High Galactic Latitudes may be easier to observe DM annhilation than GC

•Need unbiased all-sky survey with large detection area (>104 m2) to detect.

•Unable to use optical, radio surveys to predict source regions

359° 330°

The H.E.S.S. Survey Galactic PlaneThe H.E.S.S. Survey Galactic Plane

30° 0°

RX J1713.7-3946 HESS J1640-485HESS J1616-508

HESS J1614-518

G0.9+0.1 HESS J1813-178 HESS J1825-137

HESS J1834-087HESS J1804-216 Gal. Centre

HESS J1837-069

230 h in 2004, 500 pointings; sensitivity 2% of Crab above 200 GeV8 new sources @ > 6 post-trial (+3 known)

359° 330°

The H.E.S.S. Survey Galactic PlaneThe H.E.S.S. Survey Galactic Plane

30° 0°

RX J1713.7-3946 HESS J1640-485HESS J1616-508

HESS J1614-518

G0.9+0.1 HESS J1813-178 HESS J1825-137

HESS J1834-087HESS J1804-216 Gal. Centre

HESS J1837-069

230 h in 20048 new sources @ > 6 post-trial (+3 known)6 new sources @ > 4 post-trial

LS 5039

HESS J1745-303 HESS J1702-420HESS J1713-381 HESS J1632-478HESS J1708-410

HESS J1634-472

Aharonian et al, Science (2005)Aharonian et al, ApJ (2006)

359° 330°

Classes of Objects / Classes of Objects / CounterpartsCounterparts

30° 0°

SNRPWNX-ray binary

359° 330°

Classes of Objects / Classes of Objects / CounterpartsCounterparts

30° 0°

SNRPWNX-ray binary unknown

At least 3 objects in the scanwith no counterpart.

As for TeV J2032-4130 by HEGRA HESS J1303-631

New Unidentified HESS Objects:New Unidentified HESS Objects:

•In the Galactic Plane•Extended (Diffuse) emission•Are there More Sources at High Galactic Latitudes?

Dark accelerators?Dark accelerators?

TeV J2032+4130: Recent 50 ks Chandra obs. reveals no compelling counterpart (Butt et al. astro-ph/0509191)

GRB remnant ?? (Atoyan, Buckley & Krawcynski astro-ph/0509615) -TeV flux huge E budget, yet no synchrotron… relativistic shock accel. of p+ not a single power law.

HESS J1303-631: Chandra, XMM) reveal no obvious counterpart.

Archival ROSAT image, plus new Chandra image FOV (squares). Several pulsars - but none with sufficient spin-down flux for powering detectable TeV emission from a PWN.

~ 1 extent of HESS source.

Mukherjee & Halpern astro-ph/0505081€

Microquasar Detected!Microquasar Detected!

LS 5039

The only point-like source in the HESS Galactic Plan scan.

~1.4% Crab (>100 GeV)

AGN/MicroQuasar/GRB AGN/MicroQuasar/GRB GeV/TeV Unification?GeV/TeV Unification?

Next Generation Next Generation ObservationsObservations

Horan & Weeks 2003Horan & Weeks 2003

Next Generation ObservationsNext Generation Observations

All-sky GeV/TeV survey with good All-sky GeV/TeV survey with good sensitivity/ large areasensitivity/ large area

Deep follow-up with high angular Deep follow-up with high angular resolution/energy resolutionresolution/energy resolution

Ability to map large scale, diffuse Ability to map large scale, diffuse structuresstructures

Lower energy threshold/faster response Lower energy threshold/faster response times for GRBstimes for GRBs

GeV/TeV Observation TechniquesGeV/TeV Observation Techniques

GLASTDirect -ray detectionEnergy Range: 0.1-100 GeVAngular resolution: 0.1-30

Energy Resolution: 10%Field of View: 2.4 srDetection Area: 1 m2

On-time efficiency : > 90%$>100 M US

VERITAS/HESSCherenkov Light DetectorEnergy Range: 50 GeV-50 TeVAngular resolution: 0.050

Energy Resolution: 10%Field of View: 0.003 sr Detection Area: >104 m2

On-time efficiency : 10%$12 M US

MILAGROParticle DetectorEnergy Range: 0.1-100 TeVAngular resolution: 0.50

Energy Resolution: 50-100%Field of View: > 3 srDetection Area: >104 m2

On-time efficiency : >90%$3 M US

Energy RangesEnergy Ranges

10-100 GeV10-100 GeV 100 GeV-10 TeV100 GeV-10 TeV 10-100 TeV10-100 TeV

•Inaccessible to Particle detectors

•Cherenkov: low Cherenkv light density ->20-30 m diameter mirrors, high altitude?

•Satellite: only a few photons: difficult spectra

•Particle detectors ok

•Cherenkov: 10 m diameter mirrors; low gamma ray rate, 1 km2

array , larger f.o.v.

•Satellite: very few photons: no spectra

•Particle detectors good

•Cherenkov: 6 m diameter mirrors, very low gamma ray flux->>km2 array, large f.o.v

•Satellite: too small

Future Future -Ray Roadmap (2010+)-Ray Roadmap (2010+)

HAWC Particle detector

$40 M US

Wide FOV

>90% on time

All-sky survey at 10 mCrab/year

Moderate angular/energy resolution

Major IACT Array

$~100 M US

narrow FOV

10% on time

<1 mCrab point source/50 hours

High angular/energy resolution

30 + IACT telescopes?

few 1000 m

High-energy section~0.05% area coverage

Eth ~ 1-2 TeV

250 m

Medium-energy section~1% area coverage

Eth ~ 50-100 GeV

70 m

Low-energy section~10% area coverage

Eth ~ 10-20 GeV

Array layout: 2-3 ZonesArray layout: 2-3 Zones

FoV increasingto 8-10 degr.

in outer sections

Not to scale !

Option:Mix of telescope types

10-16

10-15

10-14

10-13

10-12

10-11

10 100 1000 104 105

E x

F(>

E)

[TeV

/cm

2s]

E [GeV]

Point Source Sensitivity of CTAPoint Source Sensitivity of CTA

Crab

10% Crab

1% Crab

GLAST

MAGIC

H.E.S.S.

Current Simulations

20 wide-angle10 m telescopesde la Calle Perez,Biller, astro-ph 0602284

30 m stereotelescopesKonopelkoAstropart.Phys. 24 (2005) 191

W. HofmannW. HofmannCTA Talk CTA Talk (2006)(2006)

High Density Camera Stack-UpHigh Density Camera Stack-Up

Need a to develop versitile, reliable, cheap camera/readout inOrder for IACT array to be feasible.

Active base• DC-DC converter 0-1500 V• Last 4 dynodes active• HV & current readout• Current limit

Analog Ring Sampler (ARS)• Samples PMT signal at 1 GHz• 128 samples ring buffer• Serves to delay signal until

trigger decision• High/low gain channels for large

dynamic range (> 2000 pe)Multiplexed ADC to digitize signal;FPGA• Controls conversion and

readout• Optionally sums signals over

readout window (16 ns)

Parallel bus for readout,token-passingscheme

Photonis PMT XP 29608 DynodesGain ~2 x 105

Particle Detector LayoutParticle Detector Layout

Milagro:450 PMT (25x18) shallow (1.4m) layer273 PMT (19x13) deep (5.5m) layer175 PMT outriggers

Instrumented Area: ~40,000m2

PMT spacing: 2.8mShallow Area: 3500m2

Deep Area: 2200m2

HAWC:5625 or 11250 PMTs (75x75x(1 or 2))Single layer at 4m depth or 2 layers atMilagro depths

Instrumented Area: 90,000m2

PMT spacing: 4.0mShallow Area: 90,000m2

Deep Area: 90,000m2

miniHAWC:841 PMTs (29x29)5.0m spacingSingle layer with 4m depth

Instrumented Area: 22,500m2

PMT spacing: 5.0mShallow Area: 22,500m2

Deep Area: 22,500m2

Andy Smith, Santa Fe Workshop 2006

Source DetectabilitySource Detectability

source

resolution

Source Size < Angular resolution

= Point Sources: CrabAGNM87

KA

A

F

FT

A

A

F

FTN

Speff

eff

resolutioncrpeff

eff

resolutioncr

141

),,,,,( crresolutionpeffeff FAATKfF

constant

Source DetectabilitySource Detectability

source resolution

'1

4

1K

A

A

F

FT

A

A

F

FTN

Speff

eff

sourcecrpeff

eff

sourcecr

Source Size > Angular Resolution

= Diffuse Sources: SNRTibet-Milagro UIDMolecular Cloud

sourceF

n.b. if Source has internal structure you will do better 1;' KNS

Diffuse SensitivityDiffuse Sensitivity

Extended Sources:Molecular cloudsSNR, PWNPoint Sources:AGNPulsar

Diffuse Sources:Galactic PlaneGalactic Arm

Next Gen is 1 km2 IACT, 5 deg f.o.v, 1 mCrab/50 hours

VHE Experimental World: 2010VHE Experimental World: 2010

SummarySummary

DM detection probably requires wide fov survey in DM detection probably requires wide fov survey in GeV/TeV energy band comnbined with pointed follow-GeV/TeV energy band comnbined with pointed follow-upup

New GeV/TeV sources at wide range of energies, New GeV/TeV sources at wide range of energies, angular scales. angular scales.

GeV/TeV GRB emission requires all-sky capabilityGeV/TeV GRB emission requires all-sky capability Next generation Instruments require balanced Next generation Instruments require balanced

combination of complementary techniquescombination of complementary techniques New Collaborations are being formed at the present New Collaborations are being formed at the present

time to develop/build next generation Instruments. time to develop/build next generation Instruments. Chinese participation is highly needed for these major Chinese participation is highly needed for these major new facilities.new facilities.

Source ResolvabilitySource Resolvability

source resolution

Source Size > Angular Resolution

Just need some factor >1 more S/Nto resolve internal source structure

KA

A

F

FT

A

A

F

FTN

Speff

eff

sourcecrpeff

eff

sourcecr

1

4

1

sourceF

Source ResolvabilitySource Resolvability

resolution

Source Size < Angular resolution

As F increases, tails of Gaussian become detectable->resolve source size

resolutiond

source

resolution

F

K

22

2

2

12

1source

resolution

r

sourcepeff

effeff

sourcecr

erdrA

A

F

FTK

2

2

2)( source

resolution

eKgF source

Possible Emission Possible Emission MechanismsMechanisms

Inverse Compton scattering• stellar photons• jet synchrotron photons• disk photons• “coronal” photons

high-mass companion low-mass companion

ORhadronicorigin

Hadron

Gamma ray

Muon Ring

Hadron

Point Source All-sky Survey Point Source All-sky Survey SensitivitySensitivity

Andy Smith, Santa Fe Workshop 2006