Neutrino-Driven
Multi-Messenger
Astronomy(and some updated I3 results)
Shigeru Yoshida
ICEHAP
Chiba University1

The recently published resultsfrom IceCube
EHE analysis updated
Cosmic n in Ultra-high energy region (10PeV – 10 EeV)2

UHE eventsin the 7 years of IceCube data(April 2008 – May 2015)(2012)

808 TeV(2014)

2.6 PeV (deposited energy)

They are astrophysical (3.6 s)
But they are not EeV-energies  Not originated in UHE Cosmic rays
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No Radio-loud AGNs
No GRBs
for UHE cosmic-ray sourcesnModel

GZKY&T

GZK
AhlersGZKAhlersGZK
KoteraGZK
Aloisio

AGN
Murasem=4,zmax=4

Best Fit
10EeVBest Fit
1EeV

SFR

SFR

g=2.3
Load.fac
100Young
Pulsar

Ke+SFR

Expect.
# ofevents

7.0

5.3

2.8

3.6

4.8

7.4

5.5

Model
Rejection
Factor

0.37

0.48

1.17

1.44

1.09

0.96

1.34

p-value

1.0x10-3

7.0x10-3

9.5x10-2

2.2x10-1

7.8x10-2

2.2x10-3

7.8x10-2

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No Radio-loud AGNs
No GRBs
for UHE cosmic-ray sources

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No Radio-loud AGNs
No GRBs
for UHE cosmic-ray sources

E2 f < 3x10-9 GeV/cm2 sec sr

6The recently published resultsfrom IceCube
No neutrinos associated from GRBs

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The recently published resultsfrom IceCube
No neutrinos associated from GRBs
Based on 807 GRBs

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The recently published resultsfrom IceCube
100TeV– PeV energy up-going nm measurement
using 6 year data (2009-2015)

Astrophysical Journal 833 (2016) 39

The recently published resultsfrom IceCube
100TeV– PeV energy up-going nm measurement
using 6 year data (2009-2014)

E 2 f (E)  8 10 9 GeV/cm 2sec sr

10The recently published resultsfrom IceCube
Sterile Neutrinos? May be better to forget it12

Multi-Messenger
South Pole

< 3 minutes time lag

Northern Hemisphere
GCN-TAN13

IceCube Realtime Analysis
Chainmuon multiplet for Gamma-ray/Optical follow-up
TeV
PeV

veto-based
HESE

muon neutrino sensitive
good angular resolutions
large background chance

TeVHigh cosmic n purity samples.
Launched in 2016!

EeV

PeV

EeV

all neutrino flavor sensitivehigh chance of real cosmic neutrino signals
angular resolutions so-so

EHE (Ultra-High Energies)
TeV

PeVEeVall neutrino flavor sensitivehigh chance of real cosmic neutrino signals
good angular resolutions
signal flux highly uncertain
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HESE channel

Cosmic n ~ 1.09 event/year
Atmospheric BG ~3.73 event/year
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HESE channel
Additional cut to only pick up track-like eventsA HESE track event

A HESE cascade (shower) event

angular error 0.6~1.6 deg (median)16

First GCN event from HESE
~ 150 TeV
April 27, 2016 at 5:52 UTC~0.6 deg uncert.

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EHE channel
Selects energetic (i.e., bright) events
cosmic n signalness mapin the plane of cos(zenith) and # of Cherenkov photons

events above
the black curve
retains

Cosmic n ~ 2.5 event/year
Atmospheric BG ~1.91 event/year

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EHE channel
Selects energetic (i.e., bright) events
effective area : most efficient channel for energies above PeV
same as the standard EHE/UHE selections
For realtime alerts

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EHE channel
Selects energetic (i.e., bright) events
This is THE event in EHE channel – detected in 2014 sample

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EHE channel
Selects energetic (i.e., bright) events
Detected last Sunday morning (in JST)21

IceCube alerts are foundin GCN-AMON notice
http://gcn.gsfc.nasa.gov/amon.html

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Referencesfor IceCube follow-up observers
IceCube HESE channel
http://gcn.gsfc.nasa.gov/amon_hese_events.html
public document
http://gcn.gsfc.nasa.gov/doc/Public_Doc_AMON_IceCube_GCN_Alerts_Oct2016_v7.pdf

IceCube EHE channel
http://gcn.gsfc.nasa.gov/amon_ehe_events.html
public document
http://gcn.gsfc.nasa.gov/doc/AMON_IceCube_EHE_alerts_Oct31_2016.pdf

We will also publish a paper on “IceCube Realtime Alert system”(to be submitted to Astroparticle Physics)
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