Measuring the total neutrino cross section using the IceCube detector
Neutrino source search with Four year IceCube neutrino …...Neutrino source search with Four year...
Transcript of Neutrino source search with Four year IceCube neutrino …...Neutrino source search with Four year...
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Neutrino source search with Four yearIceCube neutrino events.
Reetanjali Moharana
&
Soebur Razzaque
[University of Johannesburg]
TeVPA 2015, Kashiwa2015, Oct. 29
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IceCube results
ICRC proceeding, 2015, M.G. Aartsen et. al., 2014, Aya Ishihara,TeVPA2015
Total 54 events, adding 6 tracks,and 11 cascades.
Background expectation nearly21.6. Rejecting only backgroundwith 6.5σ.
And
ICRC proceeding, 2015
Deposited energy 2.6 ± 0.3 PeV.Direction: 11.48◦ dec, 110.34◦ RA.
ICRC presentation by Claudio Kopper
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Cross-correlation Method R. Moharana & S. Razzaque (in Prep.)
P. G. Tinyakov & I.I. Tkachev 2001
γ = cos−1(x̂neutrino · x̂source),
Calculating the number N idata for which γ < bin, where bin are ringsof 0.1σ, 0.2σ.... till 1σ.
We repeat the same procedure for a large number (typically 105) ofrandomly generated sets of IceCube neutrino events for two nulldistributions, giving mean Monte-Carlo counts N iMC and variance σi
σ2i =1
105
105∑i=1
(NMCi − N ip
)2,
The relative excess (N idata − N iMC )/σi and minima of p with respectto each ring show the scales at which correlation is most significant.
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175 TeVCat sources, AGNs, Starburst galaxies, PWN, UNID, Binary,SNR/Molec. Cloud.
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-2
0
2
4
6
8
0 2 4 6 8 10
(Nd
ata
-NM
C)/
σ
bin
10-6
10-5
10-4
10-3
10-2
10-1
100
0 2 4 6 8 10
p-v
alu
e
bin
-2
0
2
4
6
8
0 2 4 6 8 10
(Nd
ata
-NM
C)/
σ
bin
10-6
10-5
10-4
10-3
10-2
10-1
100
0 2 4 6 8 10
p-v
alu
e
bin
45 HBL 53.
RandomizingIceCubeneutrino eventsRA withinrange 0 to 360
Randomizingboth RA andCos(dec) from-1 to +1.
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2FHL catalog sources
(M. Ackermann et., al, arXiv: 1508.04449)
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-2
0
2
4
6
8
0 2 4 6 8 10
(Nd
ata
-NM
C)/
σ
bin
10-7
10-6
10-5
10-4
10-3
10-2
10-1
100
0 2 4 6 8 10
p-v
alu
e
bin
-2
0
2
4
6
8
0 2 4 6 8 10
(Nd
ata
-NM
C)/
σ
bin
10-7
10-6
10-5
10-4
10-3
10-2
10-1
100
0 2 4 6 8 10
p-v
alu
e
bin
34 2FHLgalacticsources.
RandomizingIceCubeneutrino eventsRA withinrange 0 to 360
Randomizingboth RA andCos(dec) from-1 to +1.
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-2
0
2
4
6
8
0 2 4 6 8 10
(Nd
ata-
NM
C)/
σ
bin
10-7
10-6
10-5
10-4
10-3
10-2
10-1
100
0 2 4 6 8 10
p-v
alu
e
bin
13 2FHL supenovaeremnants (SNRs)
15 2FHLPulsar windnebulae (PWNs)
-2
0
2
4
6
8
0 2 4 6 8 10(N
da
ta-N
MC
)/σ
bin
10-7
10-6
10-5
10-4
10-3
10-2
10-1
100
0 2 4 6 8 10
p-v
alu
e
bin
-2
0
2
4
6
8
0 2 4 6 8 10
(Nd
ata
-NM
C)/
σ
bin
10-7
10-6
10-5
10-4
10-3
10-2
10-1
100
0 2 4 6 8 10
p-v
alu
e
bin
6 SNRs/PWNs from 2FHLsource catalog.
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Star Burst galaxies and Super bubbles
(K. Emig, C. Lunardini & R. Windhorst arXiv: 1507.05711) R. Moharana & S.Razzaque, JCAP 2015
TeV SBG (2)Fermi SBG (2)100µm IRAS
SBG(3)
TeV (Super-bubbles) (3)TeV SBG (2)Fermi SBG (2)
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Sources
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To see further realistic view of these correlation study we need to seea fit of high energy gamma-rays as well with the neutrino eventsfrom pp channel.
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High energy gamma rays and neutrinos from pp channel
10-15
10-14
10-13
10-12
10-11
10-10
10-9
10-2
10-1
100
101
102
103
104
105
106
α=2.59E0=10
3 [TeV]
F0=1.995e+5 [cm-2
sec-1
/TeV]
HESS
E2(d
N/d
E)
[erg
cm
-2 s
ec
-1]
E [GeV]
Star forming region 30 Dor C
Eν=71.5 TeV
10-14
10-13
10-12
10-11
10-10
10-9
10-2
10-1
100
101
102
103
104
105
α=2.26
E0=102 [GeV]
F0=1.584E+6 [cm-2
sec-1
/TeV]
FermiARGO-YBJ
E2(d
N/d
E)
[erg
cm
-2 s
ec
-1]
E [GeV]
Star forming region Cygnus Cacoon
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10-15
10-14
10-13
10-12
10-11
10-10
10-9
10-2
10-1
100
101
102
103
104
105
106
α=2.7E0=500 [TeV]
F0=9.901e+5 [cm-2
sec-1
/TeV]
α=2.77E0=100 [TeV]
F0=9.901e+5 [cm-2
sec-1
/TeV]
Fermi-LAT
Eν=385 TeV
H.E.S.S
E2(d
N/d
E)
[erg c
m-2
sec
-1]
E [GeV]
Star forming region W 49A
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Starburst Galaxy
3.6 MPc
Gamma-rays detected by Fermi-LAT,H.E.S.S
10-15
10-14
10-13
10-12
10-11
10-2
10-1
100
101
102
103
104
105
106
107
α=2.39999
E0=108 [GeV]
F0=1.901E4 [cm-2
sec-1
/TeV]
Fermi-LAT
H.E.S.S
E2(d
N/d
E)
[erg
cm
-2 s
ec
-1]
E [GeV]
Star Burst galaxy NGC 253
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10-14
10-13
10-12
10-11
10-10
10-9
10-2
10-1
100
101
102
103
104
105
106
α=2.366
E0=105 [GeV]
F0=2.0417E+4 [cm-2
sec-1
/TeV]
Fermi-LAT
Eν=2 PeV
E2(d
N/d
E)
[erg
cm
-2 s
ec
-1]
E [GeV]
Star Burst galaxy NGC 4945
Eν=46 TeV
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Summary
Cross correlation method is used to find a correlation betweendifferent sources from catalog and the 4 yrs of IceCube neutrinoevents.
Two randomization methods used for IceCube neutrino events.
We found more than 4σ correlation result for 2FHL ”spp” sourcesand Starburst galaxies and Superbubbles.
A multimessenger study is done for the SBG and superbubble.
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Thank you
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