high energy particle astrophysics prc-us collaboration summary report gus sinnis david kieda gus...
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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%$3 M US
359° 330°
HESS Galactic Plane Survey
30° 0°
SNRPWNX-ray binary unknown
At least 3 objects in the scanwith no counterpart.
As for TeV J2032-4130 by HEGRA HESS J1303-631
Dark accelerators?
TeV J2032+4130: Recent 50 ks Chandra obs. reveals no compelling counterpart (Butt et al. astro-ph/0509191)
GRB remnant ?? (Atoyan, Buckley & Krawcynski astro-ph/0509615) -TeV flux huge E budget, yet no synchrotron… relativistic shock accel. of p+ not a single power law.
HESS J1303-631: Chandra, XMM) reveal no obvious counterpart.
Archival ROSAT image, plus new Chandra image FOV (squares). Several pulsars - but none with sufficient spin-down flux for powering detectable TeV emission from a PWN.
~ 1 extent of HESS source.
Mukherjee & Halpern astro-ph/0505081€
Milagro Sky Survey
Crab Nebula ~14
Galactic Ridge clearly visible
Cygnus Region discovery ~12
Prelim
inary
Diffuse Gamma Ray Emission
Milagro
preliminary
Inner Galaxy (40-100) Cygnus Region (65-85)
EGRET
From A. Strong
Milagro
Two dimensional observation on large scale anisotropy of TeV Cosmic-ray
using the Tibet Air Shower Array(Preliminary)
ARGO Project
astronomy ( Sub-TeV , 0.3ICrab)
• Diffused γsources ( Sub-TeV)
• GRB ( 10GeV)• Knee Physics• Anti-p/p ( 300GeV)• Primary Proton Spectrum
( 10TeV)• Solar Physics• 120/154 clusters complete
90o31’50” E, 30o6’38” N 4300m a. s. l., 606g/cm2
miniHAWC and HAWC
Milagro:450 PMT (25x18) shallow (1.4m) layer273 PMT (19x13) deep (5.5m) layer175 PMT outriggers
Instrumented Area: ~40,000m2
PMT spacing: 2.8mShallow Area: 3500m2
Deep Area: 2200m2
HAWC:5625 or 11250 PMTs (75x75x(1 or 2))Single layer at 4m depth or 2 layers atMilagro depths
Instrumented Area: 90,000m2
PMT spacing: 4.0mShallow Area: 90,000m2
Deep Area: 90,000m2
miniHAWC:841 PMTs (29x29)5.0m spacingSingle layer with 4m depth
Instrumented Area: 22,500m2
PMT spacing: 5.0mShallow Area: 22,500m2
Deep Area: 22,500m2
miniHAWC Construction
• Prefabricated steel building 900k$• 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
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!