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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