neutrino “astronomy” · • introduction • we built a km3 neutrino detector 3 challenges: •...
TRANSCRIPT
francis halzen university of wisconsin
http://icecube.wisc.edu
neutrino “astronomy”
• introduction
• we built a km3 neutrino detector 3 challenges:
• drilling
• optics of ice
• atmospheric muons
• search for the sources of the Galactic cosmic rays
• search for the extragalactic cosmic rays
• gamma ray bursts
• active galaxies
dark matter
IceCube.wisc.edu
TeV sources
cosmic rays
Rad
io
CM
B
Vis
ible
GeV
g-r
ay
s
energy (eV)
flu
x
n
particle flux
In the Universe
Pacini 1910
1911
neutrino sky
requires a km2
neutrino telescope
cosmic rays interact with the
microwave background
0g pandnp
TeV102E 6
cosmic rays disappear, neutrinos appear
{e e}
~1 event per cubed kilometer per year
M. Markov
1960
B. Pontecorvo
M.Markov :
we propose to install detectors
deep in a lake or in the sea and
to determine the direction of
charged particles with the help
of Cherenkov radiation.
• lattice of photomultipliers
• shielded and optically
transparent medium
n
n
n
n
RnP
energy measurement ( > 1 TeV )
e+e-
g pair-creation
bremsstrahlung
photo-nuclear
convert the amount of light emitted
to measurement of the muon
energy (number of optical modules,
number of photons, dE/dx, …)
muon track
main board
LED flasher board
HV board
architecture of independent DOMs
10 inch pmt
improving angular and energy resolution
why did it take so long ?
IceCube / Deep Core
Digital Optical Module (DOM)
• 5320 optical modules on 86 strings ( + IceTop)
• detects ~220 neutrinos and 3x108 muons per day
• threshold 10 GeV
• angular resolution
< 1 degree
completed December 18, 2010
IC-1
04-05 Season
IC-9
05-06 Season
IC-22
06-07 Season
IC-40
07-08 Season
IC-59
08-09 Season
IC-79
09-10 Season
IC-86
10-11 Season
each DOM is
independent:
continuously
sends time-
stamped
wave forms
each DOM is
independent:
continuously
sends time-
stamped
wave forms
n
27
89 TeV
• introduction
•we built a km3 neutrino detector 3 challenges:
• drilling
• optics of ice
• atmospheric muons
• search for the sources of the Galactic cosmic rays
• search for the extragalactic cosmic rays
• gamma ray bursts
• active galaxies
dark matter
IceCube.wisc.edu
… you looked at 10msec of data !
muons detected per year:
• atmospheric* ~ 1011
• atmospheric** n ~ 105
• cosmic n ~ 10
* 3000 per second ** 1 every 6 minutes
moon shadow
> 16
~ 0.1 deg
… on to IceCube science
we measure the flux of atmospheric muons and
neutrinos at higher energies and with better
statistics than previous experiments. Any deviations
from what is expected is new neutrino physics or
new astrophysics. We just look for surprises.
cosmic
neutrinos:
energy:
>> 100 TeV
atmospheric neutrino spectrum to >100 TeV
zenith angle
two analyses
matter effect
of eV sterile n’s ?
3
3+1
zenith angle distribution
not even preliminary
59 strings
… on to IceCube science
we measure the flux of atmospheric muons and
neutrinos at higher energies and with better
statistics than previous experiments. Any deviations
from what is expected is new neutrino physics or
new astrophysics. We just look for surprises.
• introduction
• we built a km3 neutrino detector 3 challenges:
• drilling
• optics of ice
• atmospheric muons
• search for the sources of the cosmic rays
• search for the extragalactic cosmic rays
• gamma ray bursts
• active galaxies
dark matter
IceCube.wisc.edu
cassiopeia A supernova remnant in X-rays
gravitational energy
released is trans-
formed into
acceleration
E-2 spectrum
acceleration when
particles cross
high B-fields
and if the star collapses to a black hole …
collapse of massive
star produces a
gamma ray
burst
shocks produced
in the outflow of
the spinning
black hole:
electrons (and
protons ?)
spinning black hole
and if the star collapses to a black hole …
happens in seconds not thousands of years
beamed not spherical
simulation not image
Hillas formula :
qBRvE
RvqB
ERgyro
)(
• dimensional analysis, difficult to satisfy
• accelerator must contain the particles
Cosmic Rays & SNRs
supernova remnants:
1050 ergs every 30 years
~10-12 erg/cm3
for steady state of CR
with lifetime ~106 years
SNRs provide the environment and energy
to explain the galactic cosmic rays!
observed energy
density of galactic CR:
~ 10-12 erg/cm3
galactic
Cosmic Rays & GRBs
Extragalactic
Gamma-Ray Bursts:
1052 ergs x 300/Gpc3
x 1010 yr
~ 10-19 erg / cm3
GRBs provide environment and energy
to explain the extragalactic cosmic rays!
observed energy
density of
extragalactic CR:
~ 10-19 erg / cm3
directions of ~ 600 neutrinos
early
astronomy
AMANDA
2000
IceCube 40 strings
operated 375.5 days northern sky: 14139 neutrinos
southern sky: 23151 muons
search for
• clustering
• high energy (>> 100 TeV)
• nothing seen
• nothing expected
next?
neutrinos
•about to unblind one year of data for 79 strings
•one year of data with completed detector on tape
• introduction
• we built a km3 neutrino detector 3 challenges:
• drilling
• optics of ice
• atmospheric muons
• search for the sources of the Galactic cosmic rays
• search for the extragalactic cosmic rays
• gamma ray bursts
• active galaxies
dark matter
IceCube.wisc.edu
Galactic
cosmic rays :
must produce
pionic g-rays
in interactions
with hydrogen
in Galactic plane
(1 proton cm-3)
cr + p pions
0 gg
trace cosmic
rays
Galactic extragalactic
produce 100 TeV
gamma rays
Galactic plane in 10 TeV gamma rays : supernova remnants in star forming regions
Southern
Hemisphere
Sky
Sta
ndard
Devia
tions
30°
210°
90° 65°
milagro
neutrinos
from
supernova
remnants :
molecular
clouds as
beam
dumps
n + n -
+
+ -
e+ ne
e+ e-
e+
g
0
g
g e-
e+ g
n
neutral pions
are observed as
gamma rays
charged pions
are observed as
neutrinos
nn = g g
Cygnus region : Milagro
translation of
TeV gamma rays
into
TeV neutrinos :
3 ± 1 n per year in IceCube per source
5 in 5 years of IceCube …
IceCube image of our Galaxy > 10 TeV
first surprise
cosmic rays
in IceCube 10 TeV
to several
100 TeV
10 TeV
2 KHz
3 deg resolution
• we map the highest
energy Galactic
cosmic rays, but…
• their gyroradius is
< 1 pc in microgauss
magnetic field
• closest sources
> 100 pc
should not point! that’s why we
detect neutrinos!
32 billion cosmic ray muons/ 59 strings
Smoothing scan results
Abbasi et al., ApJ, 740, 16, 2011 arxiv/1105.2326
Skymap energy dependence summary
40 TeV
40 TeV
Skymap energy dependence summary
100 TeV
100 TeV
Skymap energy dependence summary
126 TeV
126 TeV
Skymap energy dependence summary
200 TeV
200 TeV
Skymap energy dependence summary
316 TeV
316 TeV
Skymap energy dependence summary
400 TeV
400 TeV
Skymap energy dependence summary
630 TeV
630 TeV
Skymap energy dependence summary
1 PeV
1 PeV
Skymap energy dependence summary
5 PeV
5 PeV
Skymap energy dependence summary
10 PeV
10 PeV
Wolfendale – Erlykin
Single Source Model
-- a recent, nearby Supernova IIa --
single source: more IceTop data required
• introduction
• we built a km3 neutrino detector 3 challenges:
• drilling
• optics of ice
• atmospheric muons
• search for the sources of the Galactic cosmic rays
• search for the extragalactic cosmic rays
• gamma ray bursts
• active galaxies
dark matter
IceCube.wisc.edu
… often wrong, but never in doubt …
Galactic:
supernova
remnants?
extragalactic:
gamma ray
bursts?
active
galaxies?
solar cosmic
rays
collapse of massive
star produces a
gamma ray
burst
neutrinos are
produced in the
interactions of
fireball protons
(cosmic rays)
with synchrotron
photons
spinning black hole
decays to neutrino
decays to cosmic ray
GRB: one neutrino per cosmic ray observed
Search for GRB in coincidence with FERMI and SWIFT alerts
collide cosmic rays of
GRB
origin with fireball and
microwave photons
0g pandnp
cosmic rays from n-decay
GRB origin of cosmic
rays challenged
0 gamma rays after
cascading in the
microwave background + neutrinos
active galaxy
particle flows near
supermassive
black hole
cosmic rays interact with the
microwave background
0g pandnp
TeV102E 6
cosmic rays disappear, neutrinos appear
{e e}
~1 GZK event per cubed kilometer per year
• introduction
• we built a km3 neutrino detector 3 challenges:
• drilling
• optics of ice
• atmospheric muons
• search for the sources of the Galactic cosmic rays
• search for the extragalactic cosmic rays
• gamma ray bursts
• active galaxies
dark matter
IceCube.wisc.edu
c
WIMP Capture and Annihilation
DETECTOR
n
n
c + c W + W n + n
b + b n + n
Galactic Center
in
neutrinos and
muons
~20σ
without
oscillations
with
oscillations
3+1 neutrinos?
IceCube science
conclusions
• Hess 1912…. and still no conclusion
• the instrumentation is in place …
• … supernova remnants,GZK neutrinos
and GRB are in close range !
• unblinding 59, 79 data by Neutrino 2012
Overflow slides
CLatmsstart
samplingmwithevents
%953:
sec7.1106
supernova
quantized space: matter where the geometry is activated
cm3310E1~
n
quantized space: matter where the geometry is activated
Lorentz violation from Planck scale
violation of Lorentz invariance may be a tool to study
Planck scale physics
interaction with Planck mass particles distort
spacetime
Planck scale vacuum fluctuations probed by
high energy neutrinos
modification to dispersion relation leads to an energy
dependent speed of light.
...)(2222 n
PlanckM
EEmpE
violation of Lorentz invariance because of Planck scale
physics can be detected through time delays of high
energy neutrinos relative to low energy photons
from a source at a distance d; for instance a GRB.
n
PlanckM
E
c
dnt
n
2
1
sensitivity to Planck scale !
Lorentz violation: E vs t
violation of Lorentz invariance because of Planck scale
physics can be detected through time delays of high
energy neutrinos relative to low energy photons
from a source at a distance d; for instance a GRB.
n
PlanckM
E
c
dnt
n
2
1
Lorentz violation: E vs t
violation of Lorentz invariance because of Planck scale
physics can be detected through time delays of high
energy neutrinos relative to low energy photons
from a source at a distance d; for instance a GRB.
PlanckMt
E
c
dscaleenergy
tests
• equivalence
principle
and
• Lorentz
invariance
…general
relativity
will not last
200 years…
M. Turner
IceCube
radiation and dust
black hole
p + 0
~ cosmic ray + gamma
NEUTRINO BEAMS: HEAVEN & EARTH Neutrino Beams: Heaven & Earth
p + g n + +
~ cosmic ray + neutrino
n and g beams : heaven and earth
1~1.5 events/yr
59 strings
• crash program in calibration and systematics
• check against 59 strings data
The Italian Navy Cacciatorpediniere “Fulmine” used
by Pacini in 1910-1911
Moon shadow observed in muons – IceCube points in the right direction!
Center of moon is spot on
to a precision of <0.1 degrees.
Statistical significance with
IC 59: > 10 sigma
145
One benchmark analysis as performance measure: Point source searches, E^-2 flux limits and sensitivities
original IC80
est. in 2004
paper
Example: Energy resolution Muon energy: rms of log(E) ~
0.15
Muon neutrino: 0.3 (inevitable
physics fluctuations from
neutrino energy to muon
energy at detector)
Electron neutrino cascades:
rms of log(E): ~ 0.175
sigma of peak: 0.07
Muon energy resolution