High Energy Particle Astrophysics

PRC-US Collaboration

Summary Report

Gus SinnisDavid KiedaGus SinnisHu Hongbo Jordan Goodman Min Zha

What Do We Want to Learn?• What are the origins of cosmic rays?

– Are the accelerators of hadrons different from electrons?– How high in energy can galactic sources produce particles?– What are the sources of the UHECRs?

• How do astrophysical sources accelerate particles?– What is the role of the extreme gravitational an magnetic

fields surrounding black holes and neutron stars?– How are particles accelerated within relativistic jets?

• Are there new classes of objects in the universe?• Fundamental physics & cosmology

– What is the EBL and how did it evolve?– What is the dark matter?– Does the speed of light depend on photon energy?– Are there primordial black holes?

What Measurements Required?

• Build a large observational database of the quiescent sky– Different source classes– Many objects from each class

• Build a database of transient phenomena– Active galactic nuclei– Gamma ray bursts

• Perform a complete sky survey– Point sources– Extended sources– Large-scale structure

• Perform detailed studies of individual objects – Morphology– Energy spectra

• Compare -ray images with spectra & images with:– X-ray and optical images– Neutrino measurements

Active Galactic Nuclei

Rotating ~108 Msun black hole Accretion powered ~1048 ergs/sec TeV emission is along jet

Hadrons or leptons accelerated? Bulk Lorentz factor in jet (>30) B-field in shock?

GeV/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%Field of View: > 2 srDetection Area: >104 m2

On-time efficiency : >95%$3 M US

Santa Fe 2006

40

Updated ofR. ONG 2005 ICRC

359° 330°

HESS Galactic Plane Survey

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

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€

Milagro Sky Survey

Crab Nebula ~14

Galactic Ridge clearly visible

Cygnus Region discovery ~12

Prelim

inary

Milagro Cygnus Region

Prelim

inary EGRET diffuse model

EGRET sources

A new TeV gamma-ray source

Diffuse Gamma Ray Emission

Milagro

preliminary

Inner Galaxy (40-100) Cygnus Region (65-85)

EGRET

From A. Strong

Milagro

Two dimensional observation on large scale anisotropy of TeV Cosmic-ray

using the Tibet Air Shower Array(Preliminary)

Tibet III + MUON

8,640 m2

ARGO Project

astronomy （ Sub-TeV ， 0.3ICrab）

• Diffused γsources （ Sub-TeV）

• GRB （ 10GeV）• Knee Physics• Anti-p/p （ 300GeV）• Primary Proton Spectrum

（ 10TeV）• Solar Physics• 120/154 clusters complete

90o31’50” E, 30o6’38” N 4300m a. s. l., 606g/cm2

RPCDAQ

ARGO

Smooth window radius = 1.5°

miniHAWC and HAWC

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

miniHAWC Construction

• Prefabricated steel building 900k$• Building installation ~500 k$• Pond excavation ~800 k$• Liner cost ~700 k$

Total facility cost ~3.4M$

170m 170m

170m

150m

4.5-5.0 m 6m

GRB Sensitivity

Fluence Sensitivity to 100s GRB.

Both Milagro and miniHAWC can “self trigger” and generate alerts in real time.

GRB rate in FOV ~100 GRB/year (BATSE rate)

MilagrominiHAWC

Potential miniHAWC Sites

Sierra Negra, Mexico

4010m asl Chacaltaya, Bolivia4800m

Yangbajing, China4300m

Geomagnetic Cutoff

Milagro:3.5 GV

Tibet- 13.1 GVLa Paz: 12.0 GV

Sierra Negra: 7.7 GV

Singles rates at sites under consideration are reduced by ~20-30% due to improved geomagnetic cutoff.

Requirements on Observation SiteRequirements on Observation Site

high quality operation, low cost and long life-span:• Altitude 4300m a.s.l. • Topography flat and wide, plenty of space.

• Climate easy for construction, operation & living.

• Traffic accessible to highway, airport or railway station.

• Power existed electric power line network.

• Logistics not far from local town/modern city.

• Neighborhood 1000s of residents: clinic, post office, school …

• Communication Telephone, mobile phone, high speed optical fibre network (155Mbps today).

Detector Sensitivity (Single Location)

miniHAWCHAWC

GLAST

EGRET

Crab Nebula

WhippleVERITAS/HESS

Current synoptic instruments

Survey Sensitivity

4 m

in/fo

v

7 m

in/fo

v1500 hrs/fov1500 hrs/fov

Summary

• Gamma Ray astrophysics has entered a period of discovery– Dark sources, Galactic diffuse emission, extended sources

• Cherenkov telescopes and particle detection arrays offer complimentary views of the sky

• New instruments are coming online and planned which promise large increases in sensitivity

• YBJ is an excellent location for the next generation water Cherenkov detector

• Discussions continuing and we hope for collaboration in this endeavor

• Thank you for an excellent workshop!