observation of gamma-ray emission above 10 tev from the ... · observation of gamma-ray emission...
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ObservationofGamma-rayEmissionAbove10TeVfromtheSuperNovaRemnantG106.3+2.7
withtheTibetAirShowerArrayandtheMuonDetectorArray
T.K.SakofortheTibetASγ Collaboration26July,2019@ICRC2019
GAI4b 1
M.Amenomori(1),Y.-W.Bao(2),X.J.Bi(3),D.Chen(4),T.L.Chen(5),W.Y.Chen(3),XuChen(3),Y.Chen(2),Cirennima(5),S.W.Cui(7),Danzengluobu(5),L.K.Ding(3),J.H.Fang(3,6),K.Fang(3),C.F.Feng(8),ZhaoyangFeng(3),Z.Y.Feng(9),QiGao(5),Q.B.Gou(3),Y.Y.Guo(3),Y.Q.Guo(3),H.H.He(3),Z.T.He(7),K.Hibino(10),N.Hotta(11),HaibingHu(5),H.B.Hu(3),J.Huang(3),H.Y.Jia(9),L.Jiang(3),H.-B.Jin(4),F.Kajino(12),K.Kasahara(13),Y.Katayose(14),C.Kato(15)
S.Kato(16),K.Kawata(16),W.Kihara(15),Y.Ko(15),M.Kozai(17),Labaciren(5),G.M.Le(18),A.F.Li(19,8,3),H.J.Li(5),W.J.Li(3,9),Y.-H.Lin(3,6),B.Liu(2),C.Liu(3),J.S.Liu(3),M.Y.Liu(5),W.Liu(3),Y.-Q.Lou(20),H.Lu(3),X.R.Meng(5),H.Mitsui(14),K.Munakata(15),H.Nakada(14),Y.Nakamura(3),H.Nanjo(1),M.Nishizawa(21),
M.Ohnishi(16),T.Ohura(14),S.Ozawa(22),X.L.Qian(23),X.B.Qu(24),T.Saito(25),M.Sakata(12),T.K.Sako(16),Y.Sengoku(14),J.Shao(3,8),M.Shibata(14),A.Shiomi(26),H.Sugimoto(27),W.Takano(10),M.Takita(16),Y.H.Tan(3),
N.Tateyama(10),S.Torii(28),H.Tsuchiya(29),S.Udo(10),H.Wang(3),H.R.Wu(3),L.Xue(8),K.Yagisawa(14),Y.Yamamoto(12),Z.Yang(3),Y.Yokoe(16),A.F.Yuan(5),L.M.Zhai(4),H.M.Zhang(3),J.L.Zhang(3),X.Zhang(2),
X.Y.Zhang(8),Y.Zhang(3),YiZhang(3),YingZhang(3),S.P.Zhao(3),Zhaxisangzhu(5)andX.X.Zhou(9)
TheTibetASγCollaboration
Correlation Between Solar Activity and the Sun’s Shadow Observed by the Tibet Air Shower Array
Kazumasa Kawata
ICRR, University of Tokyo, Japan
For the Tibet ASJ Collaboration
32nd ICRC, Aug.ust 17, Beijing 1
(1)DepartmentofPhysics,HirosakiUniversity,Hirosaki036-8561,Japan(2)SchoolofAstronomyandSpaceScience,NanjingUniversity,Nanjing210093,China(3)KeyLaboratoryofParticleAstrophysics,InstituteofHighEnergyPhysics,ChineseAcademyofSciences,Beijing100049,China(4)NationalAstronomicalObservatories,ChineseAcademyofSciences,Beijing100012,China(5)PhysicsDepartmentofScienceSchool,TibetUniversity,Lhasa850000,China(6)UniversityofChineseAcademyofSciences,Beijing100049,China(7)DepartmentofPhysics,HebeiNormalUniversity,Shijiazhuang050016,China(8)DepartmentofPhysics,ShandongUniversity,Jinan250100,China(9)InstituteofModernPhysics,SouthWestJiaotongUniversity,Chengdu610031,China(10)FacultyofEngineering,KanagawaUniversity,Yokohama221-8686,Japan(11)UtsunomiyaUniversity,Utsunomiya321-8505,Japan(12)DepartmentofPhysics,KonanUniversity,Kobe658-8501,Japan(13)ShibauraInstituteofTechnology,Saitama337-8570,Japan(14)FacultyofEngineering,YokohamaNationalUniversity,Yokohama240-8501,Japan(15)DepartmentofPhysics,ShinshuUniversity,Matsumoto390-8621,Japan(16)InstituteforCosmicRayResearch,UniversityofTokyo,Kashiwa277-8582,Japan(17)InstituteofSpaceandAstronauticalScience,JapanAerospaceExplorationAgency(ISAS/JAXA),Sagamihara252-5210,Japan(18)NationalCenterforSpaceWeather,ChinaMeteorologicalAdministration,Beijing100081,China(19)SchoolofInformationScienceandEngineering,ShandongAgricultureUniversity,Taian271018,China(20)PhysicsDepartment,AstronomyDepartmentandTsinghuaCenterforAstrophysics,Tsinghua-NationalAstronomicalObservatoriesofChinajointResearchCenterforAstrophysics,TsinghuaUniversity,Beijing100084,China(21)NationalInstituteofInformatics,Tokyo101-8430,Japan(22)AdvancedICTResearchInstitute,NationalInstituteofInformationandCommunicationTechnology,Koganei184-8795,Japan(23)DepartmentofMechanicalandElectricalEngineering,ShandongManagementUniversity,Jinan250357,China(24)CollegeofScience,ChinaUniversityofPetroleum,Qingdao,266555,China(25)TokyoMetropolitanCollegeofIndustrialTechnology,Tokyo116-8523,Japan(26)CollegeofIndustrialTechnology,NihonUniversity,Narashino275-8576,Japan(27)ShonanInstituteofTechnology,Fujisawa251-8511,Japan(28)ResearchInstituteforScienceandEngineering,WasedaUniversity,Tokyo169-8555,Japan(29)JapanAtomicEnergyAgency,Tokai-mura319-1195,Japan
2
Tibet Air Shower Array
3
p Tibet, China (90.522oE, 30.102oN) 4,300 m a.s.l. p scintillation counters 0.5 m2 x 597 p area ~65,700 m2 p angular resolution ~0.5°@10TeV ~0.2°@100TeV
p energy resolution ~40%@10TeV ~20%@100TeV
2nd particles timing ➡︎ arrival direction 2nd particles energy deposit ➡︎ primary energy
Water Cherenkov Muon Detector Array
MD ~3400m2
4
ü 2.4m underground (515g/cm2 ~19X0) ü 7.35m x 7.35m x 1.5m-deep water cell x 64 ü 20”ΦPMT (HAMAMATSU R3600) ü Concrete pools + Tyvek sheets
Soil & Rocks 2.6m
Waterproof & reflective materialsReinforced concrete
eγµ
1.0m
PMT
7.3m
Water 1.5m
Cherenkov lights
20 inchAir 0.9m
Measurement of number of muons in air showers ➡︎ γ/CR discrimination
)��log(1.5 2 2.5 3 3.5 4
)�
N�
log(
-0.5
0
0.5
1
1.5
2
2.5
3
3.5
4
-310
-210
-110
1
10
210
�=0�N�
(a) Photons MC
)��log(1.5 2 2.5 3 3.5 4
)�
N�
log(
-0.5
0
0.5
1
1.5
2
2.5
3
3.5
4
-110
1
10
210
310
�=0�N�
(b) CRs Data
)��log(1.5 2 2.5 3 3.5 4
)�
N�
log(
-0.5
0
0.5
1
1.5
2
2.5
3
3.5
4
-310
-210
-110
1
10
210
�=0�N�
(a) Photons MC
)��log(1.5 2 2.5 3 3.5 4
)�
N�
log(
-0.5
0
0.5
1
1.5
2
2.5
3
3.5
4
-110
1
10
210
310
�=0�N�
(b) CRs Data
Event selection by MD
5
100TeV10TeV
log(Σρ)fromAS
log(ΣΝ
µ)fromM
D
Survivalra
tio ΣNµ=0
Optimization of muon cut γ : MC sample (Crab orbit & Crab flux) CR:Data (excluding Crab & Galactic Plane)
Σρ(Sum of particle densities by all AS counters)
~99.9% CR rejection ~90% γ efficiency @ 100 TeV
ΣNµ=0log(Σρ)fromAS
log(ΣΝ
µ)fromM
D
γMC
CRMCData
M.Amenomorietal.,arXiv:1906.05521(2019),AcceptedbyPRL
Σρ (fromASarray):3256ΣΝµ (MD):2.3zenithangle:29.8°Erec:251TeV
+46-43
Kawata+,ExperimentalAstronomy,44,1(2017)
Crab: γ-like event display
circlesize∝log(#ofdetectedparticles)circlecolor∝relativetiming[ns]
Distance from the shower axis [ m ]1 10 210 310
] 2
Part
icle
den
sity
[ pa
rtic
les/
m
-210
-110
1
10
210
310Relative position [m]
-150 -100 -50 0 50 100 150
Rel
ativ
e po
sitio
n [m
]
-150
-100
-50
0
50
100
150
Rel
ativ
e tim
ing
[ns]
-200
-150
-100
-50
0
50
100
150
(a)
(b)
fittingwithNKGfunction➡︎Erec(S50,θ)
Distance from the shower axis [ m ]1 10 210 310
] 2
Part
icle
den
sity
[ pa
rtic
les/
m
-210
-110
1
10
210
310Relative position [m]
-150 -100 -50 0 50 100 150
Rel
ativ
e po
sitio
n [m
]
-150
-100
-50
0
50
100
150
Rel
ativ
e tim
ing
[ns]
-200
-150
-100
-50
0
50
100
150
(a)
(b)lateraldistribution
S50
6
M.Amenomorietal.,arXiv:1906.05521(2019),AcceptedbyPRL
Ø Data: Feb. 2014 ー May 2017
Ø Equi-Zenith-Angle Method — Search window radius ⎯ : number of events observed in ON-source window ⎯ : average of numbers of events in 20 OFF sources ⎯ Excess =
7
(∼0.7°tolowerlimit0.5°,variableas)RSW = 6.9�/p
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Ø Standard event selection conditions for AS analysis & muon cut by MDLive time: 720 days
Excess count estimation
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NON � hNOFFi<latexit sha1_base64="IipMXTpc6vMEsB2xrh469fVhkOg=">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</latexit>
hNOFFi<latexit sha1_base64="ZsJmi8+RZpYIfXFTepVscppFrn0=">AAACkXicSyrIySwuMTC4ycjEzMLKxs7BycXNw8vHLyAoFFacX1qUnBqanJ+TXxSRlFicmpOZlxpaklmSkxpRUJSamJuUkxqelO0Mkg8vSy0qzszPCympLEiNzU1Mz8tMy0xOLAEKxQvoxOSkppUoxOQk5qXnpCr4xVfH5CaWZBTlVvu7udXWKsQUZaZnlMQUgaXjBZQN9AzAQAGTYQhlKDNAQUC+wHKGGIYUhnyGZIZShlyGVIY8hhIgO4chkaEYCKMZDBkMGAqAYrEM1UCxIiArEyyfylDLwAXUWwpUlQpUkQgUzQaS6UBeNFQ0D8gHmVkM1p0MtCUHiIuAOhUYVA2uGqw0+GxwwmC1wUuDPzjNqgabAXJLJZBOguhNLYjn75II/k5QVy6QLmHIQOjC6+YShjQGC7BbM4FuLwCLgHyRDNFfVjX9c7BVkGq1msEig9dA9y80uGlwGOiDvLIvyUsDU4NmM3ABI8AQPbgxGWFGeobGekaBJsoOTtCo4GCQZlBi0ACGtzmDA4MHQwBDKNDeSQw7GA4yHGISZrJkcmCCqmVihOoRZkABTN4A5CqbRg==</latexit>
ONsourceOFFsource
0 0.5 1 1.5 2 2.5 3
Num
ber o
f eve
nts
050
100150200250300350400
MC Data>10 TeVE(a)
)2 (deg2φ0 0.5 1 1.5 2 2.5 3
Num
ber o
f eve
nts
02
4
68
1012
14>100 TeVE(b)
φ2 distributions: consistent with point source
>10TeV
>100TeV
DatavsMCγ-ray emission from Crab
E>10TeV
E>100TeV
Data
MC
8M.Amenomorietal.,arXiv:1906.05521(2019),AcceptedbyPRL
significancemap
9
Relative number of muons > 100 TeV
Ø FirstDetectionofsub-PeV γ
✓Rµ =
observed ⌃Nµ
cut value of ⌃Nµ
◆
<latexit sha1_base64="H/pXcCPqpLthueTHb7TOZyChFKA=">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</latexit>
ERec(TeV)aftermuoncut
NON/<NOFF> σ
>10.0 1691/1031 18.3
>15.8 915/472.7 17.5
>25.1 417/159.1 16.4
>39.8 169/46.9 13.2
>63.1 69/14.6 9.8
>100 24/5.5 5.6
>251 4/0.8 2.4
Number of events (integral)
DataBG
γMC
DataON
muoncut
M.Amenomorietal.,arXiv:1906.05521(2019),AcceptedbyPRL
Ø Highest-energyphoton∼450TeV(Seeposter:PS1-75)
Crab
Relativenumberofmuons
10
γ-ray energy spectrum from Crab
M.Amenomorietal.,arXiv:1906.05521AcceptedbyPRL(Seeposter:PS1-75)
ICmodelnormalizedtoHEGRA
E>100TeV:5.6σ
A.U.Abeysekaraetal.,arXiv:1905.12518SubmittedtoApJ
E>100TeV:3.3σ
Aharonian+, ApJ, 614, 897 (2004)
TibetAS+MD HAWC
spectrumconsistentwithHAWCrecentresults
11
SNR G106.3+2.7Excesscountmap>0.63TeVbyVERITAS
BoomerangPWN
PSRJ2229+6114
Ø age10kyr,distance0.8kpc,size14pcx6pc, ifSNRisassociatedwithBoomerangPWNØ AtTeVenergies,firstobservedbyMilagro(MGROJ2228+61)andthenbyVERITAS(VERJ2227+608)Ø γ-rayemissioncentroidcoincidentwithamolecularcloudØ spectrumseemstoextendtoward35TeVwithoutcutoff
Kothesetal,ApJ,560,236(2001)
A.A.Abdoetal.,ApJL,700,L127(2009)V.A.Acciarietal.,ApJL,703,L6(2009)
VERITAS
Milagro
R.A. (deg.)
60
61D
ec. (
deg.
)
1−
0
1
2
3
4
5
6
7
8
9
336338340
>40TeV>10TeV
>10TeV
PSFsmoothing
PSF
Declination(deg.)
(68%containment)
12
Ø TibetemissioncentroidcoincidentwithmolecularcloudindicatedbyCOemissioncontours※consistentwithVERITASØ spectrumunderanalysis
PSRJ2229+6114
significance map by Tibet AS+MD
VERJ2227+608
SNR G106.3+2.7
13
Ø MuoncutbyMD:∼99.9%CRrejection,∼90%γefficiency@100TeVØ CrabNebula
⎯ FirstDetectionofSub-PeVγ(5.6σabove100TeV)⎯ Highestenergyphoton∼450TeV(Seeposter:PS1-75)⎯ spectrumconsistentwithICmodel⎯ spectrumconsistentwithHAWCresults(3.3σabove100TeV)
Ø SNRG106.3+2.7
⎯ emissioncentroid>10TeVcoincidentwithmolecularcloudconsistentwithVERITAS
⎯ spectrumunderanalysis
Summary
CrabNebula&SNRG106.3+2.7observedbyTibetAS+MD
Energyresolutionenergydeterminedasafunctionofθ andS50 (particledensityat50mawayfromshoweraxis)
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secθ =1.1➡︎θ=24.6°secθ =1.2➡︎θ=33.6°secθ =1.3➡︎θ=39.7°
M.Amenomorietal.,arXiv:1906.05521(2019),AcceptedbyPRL
Kothesetal.,ApJ560,236(2001) Kothesetal,ApJ,638,225(2006)Ifleptonic,whereisthesourceofelectrons?
Densematerial Boomerang
PWN
SNRG106.3+2.7
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