Post on 07-Jan-2016
description
Recent Asγ results+History+Future
• Introduction– Brief history of the experiment
• Recent results – γ ray observation– Knee physics
• Future plan– MUON dector– “Shower” Core detector
Steepenning spectrum:Ground basedObservation isnecessary
LHC Elab
LHC Ecm
CR spectrum
(Berezhko)
Emax~ Z
3PeV
3EeV
Emax=βZBL
Solar flares:1011eV
SN1006: 1016eV
AGN: 1018-20eV
(Hillas plot)
Crab :1016eV
宇宙线在地球大气层中引发广延大气簇射(Extensive Air
Shower)
的原理示意图
Advantage of YangBaJing altitude (4300M)
–Number of secondary reach maximum, in favor of knee physics, including composition and spectrum measurement.
–Low energy threshold, in favor of γ ray astronomy
–Better angular,energy resolution
γ ray astronomy
knee
(Ong)
90km NW from Lhasa
~1º slope; 4300 m a.s.l.
90º53’E, 30º11’N
Shigatse
YBJ Satisfy all the requirementsYBJ Satisfy all the requirements
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).
History of ASγ development
BD(1996)
3TeV;1700Hz;0.87 o3TeV;115Hz;0.9 o;
中意合作 ARGO 实验 RPC 大厅
中日合作 AS γ 实验区闪烁体探测器阵列
ARGO hall, floored by RPC. Half installed.
Asγ,ARGO (High Duty cycle,Large F.O.V)
~TeV ~100GeV
MILAGRO,Jemez （ 2630M ）
e
AS γ scintillation counter
Gamma ray emission from Crab (TibetII-HD : 5.5σ,ApJ 525,L93,1999)
Mrk501 (TibetII HD)ApJ 532,302(2000)
Feb.1997-Aug.1997. Only observation from conventional air shower array.
Mrk421 (6.9σ)AS γ 比切伦可夫望远镜更长时间地观测了 2000-2001 年间Mrk421 的爆发。
太阳宇宙线 1) 最先观测到宇宙线太阳阴影；
2 ）寻找与太阳耀斑， GLE 事件相伴随的高能宇宙线发射。
NO. R.A.(˚) DEC(˚) Sig.(σ) NO. R.A.(˚) DEC(˚) Sig(σ)1 62.7 51.1 4.2 9 254.8 5.8 4.1
2 83.7 21.8 5.6 10 263.6 21.4 4.1
3 129.3 13.5 4.1 11 286.8 6.0 4.4
4 131.8 33.9 4.3 12 316.5 13.0 4.0
5 137.5 41.8 4.1 13 318.2 40.9 4.1
6 165.7 38.3 5.4 14 331.6 52.5 4.4
7 175.8 2.1 4.4 15 353.3 24.6 4.1
8 221.3 13.6 4.6
Allsky Survey (1999.11-2004.10)PRELIMINARY
Milagro limit
Preliminary
Flux Limit (1999.11-2004.10)
Indirect search of DM
γ>100MeV （ EGRET ）
Diffuse TEV gamma ray from the Galactic Plane
Effective Area
９９％ C.
L.
９９％ C.
L.
９９％ C.
L.
Tibet-III (22,050m2) 1041.3 days (1999 Nov.~2004 Oct.)
Two dimensional observation on large scale anisotropy of TeV Cosmic-ray using the Tibet Air Shower Array
(Preliminary)
EC and BD Total EC area : 80 m2 ;
80 channels electronics + 600 channels from shower array
KASCADEKASCADE
e/ Hadron
(~100K channels of electronics ！！！）
J. Huang Primary proton
spectrum(analyses based on
Corsika_QGSJET
and SIBYLL )
(KASCADE data: astro-ph/0312295)
PreliminaryAll
ProtonKASCADE (P)
Present Results -3.11-3.13
PreliminaryAll
Proton
Present Results
KASCADE (P)
Tibet III + MUON
8,640 m2
Number of μ in MUON detector
10TeV 100TeV (gamma)
0.4
（ μ 数＝ 0 → 0.12 と表示）
10TeV 100TeV (gamma)
MAGIC
VERITAS
HESS
Tibet-III
Tibet-III+WC
Detection Sensitivity of Tibet-III+WC (3 years 5σ)
Tibet-III Scintillation Counters 37,000m2
+Underground
Water Cherenkov Detector 8,640m2
Crab orbit
Flat region (> 200TeV)Background << 1 event15 photon sensitivity(Poisson 5σ)
Energy Spectrum of HESS sources
Indices are harder
Aharonian et al, ApJ, 636, 777 (2006)
(If it is constructed in the southern hemisphere)
Most of HESS sources detectable byTibet III+WC!
Extrapolation
Consistent withpower low
Design of detector
3.75m
3.75m
20 detectors
20 d
etec
tors
YAC array
Tibet III
YAC
AS
Pb
Iron
Scint.
Box
7cu
ConclusionPb=7cu, Spacing=3.75m, Nb>100
Primary energy range
M. Shibata
Summary
• YangBaJing is an unparalleled observatory
• AS γ has been very successful
• Looking forward to seeing TIBET-III/MUON, HAWC & other projects will get going in YBJ