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IceCube and Multimessenger Astronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
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• 20% of the Universe is opaque to the EM spectrum
• non-thermal Universe powered by cosmic accelerators
• probed by gravity waves, neutrinos and cosmic rays
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radiationand dust
black hole
neutron star
p + p0
~ cosmic ray + gamma
NEUTRINO BEAMS: HEAVEN & EARTH
Neutrino Beams: Heaven & Earth
p + g n + p+
~ cosmic ray + neutrino
n and g beams : heaven and earthaccelerator is powered bylarge gravitational energy
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nm m+ n m-
m+
p+ p-
e+ ne
e+ e-
e+
g
p0
g
g e-
e+ g
nm
neutral pions
are observed as
gamma rays
charged pions
are observed as
neutrinos
ggnn mm
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active galaxy
particle flows near
supermassive
black hole
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IceCube and Multimessenger Astronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
![Page 7: IceCube and Multimessenger Astronomy francis halzen ... · Fermi gammas E-2.15 ... Universe is the same as that in gamma-rays • at some level common Fermi-IceCube sources? multimessenger](https://reader035.vdocument.in/reader035/viewer/2022070612/5b44fab27f8b9a05708b4bda/html5/thumbnails/7.jpg)
ultra-transparent ice below 1.5 km
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IceCube
5160 PMs
in 1 km3
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muon track: color is time; number of photons is energy
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muons detected per year:
• atmospheric* m ~ 1011
• atmospheric** n m ~ 105
• cosmic n m ~ 10-102
* 3000 per second ** 1 every 6 minutes
separating signal and “background”
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total energy measurement
all flavors, all sky
isolated neutrinos interacting
inside the detector (HESE)
up-going muon tracks
(UPMU)
astronomy: angular resolution
superior (<0.5o)
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IceCube and Multimessenger Astronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
![Page 13: IceCube and Multimessenger Astronomy francis halzen ... · Fermi gammas E-2.15 ... Universe is the same as that in gamma-rays • at some level common Fermi-IceCube sources? multimessenger](https://reader035.vdocument.in/reader035/viewer/2022070612/5b44fab27f8b9a05708b4bda/html5/thumbnails/13.jpg)
muon
• lattice of photomultipliersneutrino
interaction
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14
muon neutrinos through the Earth 6.4 sigma
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above 100 TeV
• cosmic
neutrinos
• atmospheric
background
disappears
atmospheric neutrino cosmic
100 TeV
dN /dE ~ E-2
10—100 events
per year for fully
efficient detector
Neutrino
2012
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~ 550 cosmic neutrinos in a background of ~340,000 atmospheric
atmospheric background: less than one event/deg2/year
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highest energy nm are cosmic:
astronomy with 0.2-0.4 degree resolution !
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18
after 7 years 6.4 sigma
2.16
0.97+.27-.25
0.11
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2.6 ± 0.3 PeV
inside detector
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IceCube and MultimessengerAstronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
![Page 22: IceCube and Multimessenger Astronomy francis halzen ... · Fermi gammas E-2.15 ... Universe is the same as that in gamma-rays • at some level common Fermi-IceCube sources? multimessenger](https://reader035.vdocument.in/reader035/viewer/2022070612/5b44fab27f8b9a05708b4bda/html5/thumbnails/22.jpg)
calorimetry: direct energy
measurement; all flavors
isolated neutrinos interacting
inside the detector
up-going muon tracks
astronomy: angular resolution
superior
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no light in the veto region
veto for atmospheric
neutrinos that are typically
accompanied by muons
energy measurement: to-
tal absorption calorimetry
all sky, all flavors
neutrinos starting inside the detector
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atmospheric neutrinos are
accompanied by muons from
the decay (and also shower) that
produced them
isolated events only
(no signals in IceTop)
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electron showers versus muon tracks
PeV ne and nt
showers:
• 10 m long
• volume ~ 5 m3
• isotropic after
25~50 m
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GZK neutrino search: two neutrinos with > 1,000 TeV
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• > 300 sensors
• > 100,000 pe reconstructed to 2 nsec
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starting events: now 6 years 8s
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Partially contained event with energy ~ 6 PeV
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30
two methods consistent above 100 TeV
nm astrophysical
flux
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et
moscillate over cosmic
distances to 1:1:1
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new physics ?
if not…
every model
ends up in
the triangle
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IceCube and Multimessenger Astronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
![Page 34: IceCube and Multimessenger Astronomy francis halzen ... · Fermi gammas E-2.15 ... Universe is the same as that in gamma-rays • at some level common Fermi-IceCube sources? multimessenger](https://reader035.vdocument.in/reader035/viewer/2022070612/5b44fab27f8b9a05708b4bda/html5/thumbnails/34.jpg)
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Galactic p0 gamma rays (Fermi) charged p neutrinos
extrapolation GeV TeV, PeV energy?
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at most ~10% of the events are Galactic in origin
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• we observe a diffuse flux of neutrinos from
extragalactic sources
• a subdominant Galactic component cannot be
excluded (no evidence reaches 3s level)
• where are the PeV gamma rays that accompany
PeV neutrinos?
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IceCube and Multimessenger Astronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
![Page 39: IceCube and Multimessenger Astronomy francis halzen ... · Fermi gammas E-2.15 ... Universe is the same as that in gamma-rays • at some level common Fermi-IceCube sources? multimessenger](https://reader035.vdocument.in/reader035/viewer/2022070612/5b44fab27f8b9a05708b4bda/html5/thumbnails/39.jpg)
g
p
n
gamma rays accompanying IceCube neutrinos interact
with interstellar photons and fragment into multiple lower
energy gamma rays that reach earth
e+
e-g
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cosmic
neutrinos
Fermi
gammas
E-2.15
p + = p - = p 0
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• energy density of neutrinos in the non-thermal
Universe is the same as that in gamma-rays
• at some level common Fermi-IceCube sources?
multimessenger campaign of telescope follow-
up of IceCube real-time neutrino alerts
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What are the sources of Fermi’s gamma rays?
• 50% identified blazars, non-blazar sources cannot exceed
15%?
• can be accommodated by starbursts galaxies that
accommodate at most 10% of IceCube (however
argument sensitive to spectral index)
• can be accommodated by radiogalaxies that
accommodate IceCube neutrinos
blazars? not the resolved Fermi blazars, but…
• neutrinos originate from a larger volume
• 50% of blazars not identified
• sources transparent to high energy gamma rays may not
have the target density to produce neutrinos (GRB?)
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radiogalaxiesTjus et al.
Hooper
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no resolved point sources… yet
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flux nearest source = (diffuse flux observed)(density of sources)1/3
Olbers paradox
density 10-7 Mpc-3
soon !
blazars, FSRQ…
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IceCube and Multimessenger Astronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
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flux < 1% of astrophysical neutrino flux observed
Nature 484 (2012) 351-353
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IceCube and Multimessenger Astronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
![Page 53: IceCube and Multimessenger Astronomy francis halzen ... · Fermi gammas E-2.15 ... Universe is the same as that in gamma-rays • at some level common Fermi-IceCube sources? multimessenger](https://reader035.vdocument.in/reader035/viewer/2022070612/5b44fab27f8b9a05708b4bda/html5/thumbnails/53.jpg)
• is there more ?
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cosmic
neutrinos
Fermi
gammas
E-2.15
p + = p - = p 0
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a “problem” ?
gamma rays cascade in the source to < GeV energy
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towards lower energies: a second component?
atmospheric C.R. muons cosmic n
PeV neutrinos
absorbed in the Earth
warning:• spectrum may not be a power law• slope depends on energy range fitted
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57
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low threshold starting event analysis; 7 years
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shower events only: cosmic flux dominates > 20 TeV
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• two component cosmic neutrino flux?
• cosmic accelerators do not follow a power-law
spectrum?
• note that the gammas rays accompanying
< 100 TeV neutrinos are not seen suggesting a
hidden source(s)
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• tracks cosmic ray flux in energy, isotropic in zenith, normalization unknown:
does not fit the data
• neutrino events are isolated
• incompatible with observes atmospheric electron neutrino spectrum
not background: prompt decay of charm particles produced in the atmosphere
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IceCube and Multimessenger Astronomy
francis halzen
• IceCube
• cosmic neutrinos: two independent
observations
muon neutrinos through the Earth
starting neutrinos: all flavors
• where do they come from?
• Fermi photons and IceCube neutrinos
• other multiwavelength observations
• cosmic neutrinos below 100 TeV?
• the Galaxy
IceCube.wisc.edu
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neutrinos
from
supernova
remnants :
molecular
clouds as
beam dumps
of
PeVatrons
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MGRO J1908+06: the first Pevatron? (2007!)
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2007 simulated sky map of IceCube in Galactic coordinates after
five years of operation of the completed detector. Two Milagro
sources are visible with four events for MGRO J1852+01 and three
events for MGRO J1908+06 with energy in excess of 40 TeV.
multiple sources
unidentified
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• most significant source in pre-defined list (p-value 0.003 pretrial)
• joined HAWC-IceCube analysis in progress using photon templates
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HAWC sky above 55 TeV
HAWC View of Gamma Ray Sky
E > 1 TeV 340 days
0°360°
Equatorial Coordinates
MGRO J1908+06
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Conclusions
• discovered cosmic neutrinos with an energy density similar to the one of gamma rays.
• neutrinos (cosmic rays) are essential in understanding the non-thermal universe.
• from discovery to astronomy: more events, more telescopes
• neutrinos are never boring!
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Related talks with more details:
• Nancy Wandkowski– starting events 6 years
• Nancy Wandkowski– low threshold starting events 7 years
• Hans Niederhausen– neutrino induced showers 4 years
• Lu Lu– All flavor very high energy analysis
• Joshua Wood-– joint HAWC-IceCube Galactic analysis
• Sarah Mancina– impoved starting muon neutrino analysis
• Donglian Xu– fast radio burst
• Carsten Rott– neutrinos from the sun
• Mike Richman– point source search 6 years
• Zach Griffith– high energy gamma ray search
• Tianlu Yuan– improved shower reconstruction
• Daan Van Eijk– ANTARES and KM3NeT
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overflow slides
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populate the
Universe
Pamela
AMS
HAWCIceTop
Cascade
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energy in the Universe in gamma rays, neutrinos and cosmic rays
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radiogalaxiesTjus et al.
Hooper
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81
after 7 years 6 sigma
2.16
0.97+.27-.25
0.11
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82
after 6 years: 3.7 6.0 sigma
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