Recent As γ results +History+Future

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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

description

Recent As γ results +History+Future. Introduction Brief history of the experiment Recent results γ ray observation Knee physics Future plan MUON dector “Shower” Core detector. CR spectrum. LHC E cm. LHC E lab. 3 PeV. Steepenning spectrum: Ground based Observation is necessary. - PowerPoint PPT Presentation

Transcript of Recent As γ results +History+Future

Page 1: Recent As γ  results +History+Future

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

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Steepenning spectrum:Ground basedObservation isnecessary

LHC Elab

LHC Ecm

CR spectrum

(Berezhko)

Emax~ Z

3PeV

3EeV

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Emax=βZBL

Solar flares:1011eV

SN1006: 1016eV

AGN: 1018-20eV

(Hillas plot)

Crab :1016eV

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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

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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)

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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

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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).

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History of ASγ development

BD(1996)

3TeV;1700Hz;0.87 o3TeV;115Hz;0.9 o;

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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

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Gamma ray emission from Crab (TibetII-HD : 5.5σ,ApJ 525,L93,1999)

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Mrk501 (TibetII HD)ApJ 532,302(2000)

Feb.1997-Aug.1997. Only observation from conventional air shower array.

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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。

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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。

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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

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Milagro limit

Preliminary

Flux Limit (1999.11-2004.10)

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Indirect search of DM

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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.)

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Two dimensional observation on large scale anisotropy of TeV Cosmic-ray using the Tibet Air Shower Array

(Preliminary)

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EC and BD Total EC area : 80 m2 ;

80 channels electronics + 600 channels from shower array

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KASCADEKASCADE

e/ Hadron

(~100K channels of electronics !!!)

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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)

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Tibet III + MUON

8,640 m2

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Number of μ in MUON detector

10TeV 100TeV (gamma)

0.4

( μ 数= 0  →  0.12  と表示)

10TeV 100TeV (gamma)

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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)

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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

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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

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Primary energy range

M. Shibata

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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