Transcript Neutrino Astrophysics - Vanderbilt University

Neutrino Astrophysics: PeV to ZeV
(with some whacky particle physics)
For the viewing pleasure of Alan,
the only person to make me regret
that I don’t play (cough) golf!
Tom Weiler
-- Vanderbilt University & CERN*
* thanks Alan, and Francis
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Neutrinos versus Cosmic-Rays and Photons
ns come from central engines
- near Rs of massive BHs
- even from dense “hidden” sources
cf. ns vs. gs from the sun
ns not affected by cosmic radiation
(except for annihilation resonance)
ns not bent by magnetic fields
- enables neutrino astronomy
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Cosmic Photo- Proto-Spectra
SN87a sun
Neutrino
Incognito
hadron wall?
no wall a’tall
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Extreme Energy (EE) Neutrino Sources:
Bottom-Up “Zevatrons”
- givens
Cosmogenics
~1019 eV
·
AGNs
·
GRBs
·
Hidden vs. Transparent (the thick/thin debate)
·
·
·
·
·
Top-Down “EE-trons”
- ??
Topological Defects
Wimpzillas, M ~H(post-inflation) ~1022 eV
Msee-saw
MGUT
And even MPlanck
Other:
Mirror-Matter mixing
Multiverse Leakage
AlanFest, 23July2004
~ 1023 eV
~ 1025 eV
~ 1028 eV
- ????
Tom Weiler, Vanderbilt & CERN
HiRes vs. AGASA UHE spectrum
FlysEye event goes here
discovery
opportunity
GZK recovery ?
Z-burst discovery ?
EUSO reach x 103
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
n HAS event rate
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Size matters
EUSO ~ 300 x AGASA ~ 10 x Auger
EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger
Exposure
10000
Exposure
1000
AGASA
HiRes
Auger
EUSO
100
10
1
90 92 94 96 98 00 02 04 06 08 10 12 14
19 19 19 19 19 20 20 20 20 20 20 20 20
Year
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
“clear moonless nights”
Blackout_14aug03.jpeg
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
“Essentially Guaranteed”
Xgal Cosmogenic n Flux
n
Cosmogenic ’s:
Fn(Ep/5/4) = Fp(E>5 1019) x 20
graphs from Semikoz and Sigl
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
for comparison,
AGN and Z-burst fluxes
an AGN prediction
AlanFest, 23July2004
and Z-burst fit
Tom Weiler, Vanderbilt & CERN
Present and Imminent Limits
on Neutrino Flux
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Model Neutrino Fluxes and Future Limits
Eberle,
Ringwald,
Song,
TJW
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
EE Neutrinos are young
Consider a 1020 eV neutrino.
Lorentz factor = 1021 for mn = 0.1 eV.
Age of Uni is 1018 sec,
But age of n is 1018/1021 sec = 1 millsec !
And it doesn’t even see the stream of radiation
rushing past it – untouched !
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Resonant Neutrino Annihilation Mean-Free-Path
From Fargion, Mele, Salis
l=(nn sn)-1 = 40 DH/h70
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Escher’s Angels and Devils”
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Z-bursts
TJW, 1982;
Revival – 1997
~ 50 Mpc
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Neutrino mass-spectroscopy: absorption and emission
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
What we think we know about neutrino mass
It “probably” looks
something like this
Log m2
m3
Dm223 ~ 2.5 x 10-3 eV2
m2
Dm212 ~ 7 x 10-5 eV2
m1
ne
AlanFest, 23July2004
nm
nt
Tom Weiler, Vanderbilt & CERN
n-mass spectroscopy
AlanFest, 23July2004
zmax=2, 5, 20 (top to bottom), n-a=2
(bottom-up acceleration)
Eberle, Ringwald, Song, TJW, 2004
Tom Weiler, Vanderbilt & CERN
Dips & sobering realism
hidden MX=4 1014 and 1016 GeV,
to explain >GZK w/ Z-bursts;
n mass = 0.2 (0.4) eV - dashed (solid);
Error bars – per energy decade, by 2013,
for flux saturating present limits
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Fitted Z-burst (Emission) Flux
Gelmini,
Varieschi,
TJW
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Nu-mass limit for Z-burst fitted to EECRs
Gelmini,
Varieschi,
TJW
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Neutrino Mass tomography
in the Local Super-galactic Cluster
(Fodor, Katz, Ringwald)
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Upward and Horizontal Air-shower Rates
Versus Neutrino Cross-section
Kusenko, TJW
HAS
UAS
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Earth Absorption versus
Neutrino Cross-Section
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Can’t Lose Thm
Whatever the weak cross-section,
get robust event rate from HAS or UAS!
and
Get measurement of
neutrino cross-section
(peak angle also gives snN)
Kusenko, TJW
hep-ph/
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
The “Learned Plot”
Oscillation phase is
. ( L dm2 / 4 En )
Figure
parameterized
by dm2 / (eV)2
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Neutrino Decay -Models, Signatures, and Reach
P(survive)= e –t/t = e –(L/E)(m/t0)
Beacom, Bell, Hooper, Pakvasa, TJW
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
PMNS neutrino-mixing matrix
Weak-interaction and mass “vectors” point differently:
|nk>=Uki |ni>, or Uki = <ni | nk> = <nk | ni>*
0
0  1 0
0   c13 0 s13 
 U e1 U e 2 U e 3   c12 s12 0   1

 
 
 
 

U li =  U μ1 U μ 2 U μ3  =  - s12 c12 0    0 c23 s23    0 1
0  0 1 0 
U
 
0 1   0 - s23 c23   0 0 e - iδ   - s13 0 c13 
 τ1 Uτ 2 Uτ 3   0
where cij = cos ij , and sij = sin  ij
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
The cosmic n flavor-mixing thm
If theta32 is maximal (it is),
And if Re(Ue3) is minimal (it is),
Then nm and nt equilibrate;
Further, if initial ne flux is 1/3
(as from pion-muon decay chain),
Then all three flavors equilibrate.
ne:nm:nt = 1 : 1 : 1
AlanFest, 23July2004
at Earth
Tom Weiler, Vanderbilt & CERN
AMANDA/IceCube nm event
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Flavor ratio  Topology ratio Map
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Sensitivity of n1 flavor-projection
to MNS parameters
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Final “remark”:
Is anyone driving to/by
Nottingham East Midlands airport
tomorrow morning?
I could use a ride.
Thank you.
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
1991
Fly’s Eye reports 3x1020 eV, with proton-like profile;
Akeno/AGASA Xpt begins
1993
Baikal sees underwater neutrinos
mid-90sDUMAND taken off life-support
90s
SuperK neutrinos from the sun (directional astro)
1996
AGASA reports event clustering within 2.50 ang. res’n
and: F(E  1020 eV) ~ 1/km2/century,
with shower diameter ~ 5km, N(e) ~ 1011
2000
20 events at and above 1020 eV
2001
HiRes withdraws 7 events; AGASA adds 6 (from z > 45o);
And the controversy has begun!
Importantly, Auger gets first “light”
2002
AMANDA pushes to 1014 eV thru-Earth neutrinos
2005
Auger expected to go public
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
CR Spectrum above a TeV
from Tom Gaisser
VLHC
(100 TeV)2
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Hillas Plot -- coherence length= B x L
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Orbiting Wide-angle Lens (OWL)
3000 events/year
above 1020eV
and UHE Neutrinos!
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
WINDOWS on the UNIVERSE
Crab Nebula
Stars & Galaxies
Big Bang
Galaxy Clusters
Planets
Black Holes
Neutron Stars
Distant
Galaxies
Gamma Ray Bursts
10-
103
1
106
109
1012
3
ELECTROMAGNETIC
Radio m-wave
IR /Visible/ UV
N E U T
3
Big Bang
R I
103
1
VHE g-rays
Vision
Accelerators
Reactors,
Nuclear Decays
10-
SPECTRUM
g-rays
X-rays
Limited
N O
106
S P E
109
Sun
1012
C T
R U M
1015
Crab Nebula
Atmospheric
Neutrinos
Stars
Dark Matter
Neutron Stars
1018
1021 eV
Produced by
New Particles
Produced by
Supermassive Black Holes
Supernovae
Ultra-High-Energy
Cosmic Rays
Gamma Ray Bursts
From Turner & Olinto
AlanFest, 23July2004
Underground Lab
IceCube
Auger
EUSO
radio
Tom Weiler,
Vanderbilt
& CERN
EUSO
2012 Hundredth anniversary of V. Hess
– EUSO finishes three-year data-taking
FOV = 2 105 km2,
Aperture = 106 km2 sr,
and 2 teratons of visible mass
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
“Essentially Guaranteed” High-Energy
Galactic Neutrino Flux
ctn = 10 kpc (En / EeV)
and
En / En ~ Q / mn ~ 0.8 x 10-3
 En ~ PeV, for En ~ EeV
Anchordoqui, Goldberg, Halzen, TJW;
hep-ph/0311002
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher !
“More Guaranteed”
a signal in a km3.
So, atmos background in 1o circle is just 1.5events/yr,
 3.5 events offers 95% CL detection in 1 yr;
Calculated signal is 4 nm /yr and 16 ne+nt showers/yr.
Conclude that in a few years, IceCube attains 5s
discovery sensitivity for Fe  n  ne  nm,
Providing “smoking ice” for GP neutron hypothesis.
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Schematic: AGN Unified Source Model
annotated by M. Voit
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
The TeV g-ray -- PeV n connection
A handful of TeV g-ray emitters have been identified,
all of the BL-Lac class, with a relativistic jet slightly
off-set from the line of sight.
Two principle production mechanisms:
Electrons: synchrotron on magnetic field,
or inverse Compton on gamma’s;
Hadrons: pion production off g’s and nucleons,
with p0  g g (and p+/-  2 nm + ne + e )
Only the latter accommodates production of observed CRs !
In the Unified Source Model, BL-Lacs, FR-I’s, …
are all Accreting Super-Massive Black Holes
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Nearest are Cen-A (3.4 Mpc) in South
and M87 (16 Mpc) in North
Ergo, may be the best candidate Xgal neutrino sources
The n-mixing thm predicts a nearly equal flux for each flavor
“j”, normalized to the g-ray flux as
(factor 2 from scaling energy bin)
The resulting n flux on Earth from Cen-A during a bursting
phase (~ yr, Narrabri 4.5s, 1970s) is

AlanFest, 23July2004
Prediction:
Tom Weiler, Vanderbilt & CERN
And for M87:
• From HEGRA, 4.1s, 98-99
• Consistent with Cen-A and 1/r2
• ~ 2 events/yr in IceCube, similar to atmospheric background
The diffuse flux on Earth then follows:
leading
to:
between bursts.
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Auger neutrons form Cen-A
Since ctn = 0.9 Mpc E20,
Neutron survival probability from Cen-A
= e –3.8/E20
= 2% at
1020 eV
= 15% at 2 1020 eV
= 1/e at 3.8 1020 eV
Maybe 2 evts/yr at Auger, more at EUSO,
with Glennys’ flux (Farrar-Piran)
Anchordoqui, Goldberg, TJW;
hep-ph/01
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Or maybe
…
It looks like this
Log m2
m3
m2
m1
m2
m1
m3
ne
AlanFest, 23July2004
nm
nt
Tom Weiler, Vanderbilt & CERN
Dirac neutrino vs Majorana neutrino
Dirac
n 
n 
 
n 
n 
 
L
C
R
P
T
L
Majorana
Lorentz
Boost,
E, B
n 
n 
 
L
R
C
P
T
R
AlanFest, 23July2004
So is a Dirac just two Majoranas?
Yes, iff the two Majoranas are
mass-degenerate and
have opposite CP parity
Tom Weiler, Vanderbilt & CERN
Pseudo-Dirac Mass Spectrum
Beacom, Bell, Hooper, Learned, Pakvasa, TJW
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
View (Japanese) of Earth-Moon System
n
AlanFest, 23July2004
radio
Cherenkov
Tom Weiler, Vanderbilt & CERN
Absorption Dips on Relic Nu’s
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Spectra: pi  2 gamma vs. nucleon
Xptl spectra in Z rest-frame
AlanFest, 23July2004
Boosted spectra in relic nu frame
(from Fodor, Katz, Ringwald)
Tom Weiler, Vanderbilt & CERN
The finger of god
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Does this look natural?
Or a firefly with
a lit-up butt?
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Model n fluxes
(Protheroe review)
atmosphere
AGN
GRB
GeV
pgIsm
GZK
SMPs
TDs
AlanFest, 23July2004
MGUT
Tom Weiler, Vanderbilt & CERN
Protheroe Summary Fluxes
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Galaxy Distribution 7-21 Mpc
Visible from the southern site
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Galaxy Distribution 7-21 Mpc
Visible from the northern site
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Auger neutrons form Cen-A
Since ctn = 0.9 Mpc E20,
Neutron survival probability from Cen-A
= e –3.8/E20
= 2% at
1020 eV
= 15% at 2 1020 eV
= 1/e at 3.8 1020 eV
Maybe 2 evts/yr at Auger, more at EUSO,
with Glennys’ flux (Farrar-Piran)
Anchordoqui, Goldberg, TJW;
hep-ph/01
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Important to ask
1. Can flavor ratios be measured ?
2. What would NOT 1:1:1 mean ?
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
AMANDA/IceCube nm event
To be contrasted with
localized “shower event”
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Flavor ratio  Topology ratio Map
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN
Neutrino Decay -Models, Signatures, and Reach
P(survive)= e –t/t = e –(L/E)(m/t0)
Beacom, Bell, Hooper, Pakvasa, TJW
AlanFest, 23July2004
Tom Weiler, Vanderbilt & CERN