venice “ telescopes”, feb 22-25 tom weiler, vanderbilt university high-energy cosmic ray/...
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Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
High-Energy
Cosmic Ray/ Observatories,
and What They Can Do for Us
Tom Weiler
Vanderbilt University
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Cosmic Photon- Proton-Spectra
Rad
io
CM
B
Vis
ible
-ra
ys
CERN/Fermilab
x-ra
ysUV
IRCosmic-rays
TeV
-w
all
(after Ressell & Turner ‘90)
hadron wall?
no wall a’tall
sunSN87a
NeutrinoIncognito
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
The Sun thru SuperK eyes:
No dark glasses required
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
1991 Fly’s Eye reports 3x1020 eV, with proton-like profile;
Akeno/AGASA Xpt begins
mid-90sDUMAND prototype ended; Baikal continues
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 IceCube sees first muon
2005 Auger Observatory data expected
2008 Extreme Universe Space Observatory (EUSO) ?
Timeline
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
2012, a hundred years since Victor Hess
Auger data digested
IceCube data digested(neutrinos are calorie-free)
Anita data on cosmogenics
Nestor/Antares 100 GeV point sources
EUSO extends Auger
GZK are history!Neutrino sky-maps are available in textbooks;
But, there is no consensus theory in sight for neutrino mass and mixing
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
CR Spectrum above a TeV
from Tom Gaisser
VLHC(100 TeV)2
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Highest Energy Event
The CR record energy is 3x1020 eV (0.3 ZeV). Found by Fly’s Eye a decade ago (they got lucky!). This is truly a macroscopic energy: 3x1020 eV = 50 Joules
equivalent to a Roger Clemens fastball,a Tiger Woods tee shot,a Pete Sampras tennis serve,Or a speeding bullet.
(Also to 12 Calories, which heats a gram of water by 12oC)
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
3 x1020 eV = macroscopic 50 Joules
Clemens does this with 1027 nucleons;Nature does this with one nucleon, 1027 times better pitcher !
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Fly’s Eye 3x1020 eV event (1992)
100 billion e+e- pairs at xmax ~ 800 g/cm2
This longitudinal profile is consistent with a primary proton, but less so with a primary photon; Disfavors “local” top-down sources such as massive Particle DK, topo-defects,Z-bursts, etc.
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
AGASA Spectrum: EeV to ZeV
AGASA, July 2002
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
UHECR Mysteries-- acceleration mechanism above 10^18 eV
-- bottom-up: few nearby candidates for p&A (50Mpc horizon)
-- top-downgammas (5Mpc horizon) and neutrinos (no horizon)
-- is there a GZK suppression? (AGASA vs HiRes)
-- is there directional clustering of events? (AGASA vs HiRes)
-- is the crossover to Xgal at 2nd knee (10^18eV), or ankle (~10^19eV) ?
Neurtrino co-emission an important tool !!
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Greisen-Zatsepin-Kuzmin and the Cosmic-Ray Wall
-resonance
multi-pions
Photo-pion production off CMB
p+cmb p/n+
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
HiRes vs. AGASA UHE spectrum
discovery
opportunity
GZK recovery ?Z-burst uncovery ?
FlysEye event goes here
Auger (EUSO) reach 70 (103) better
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Auger update – February05
-- 12 of 24 FD’s operational (50%)
-- 650 (of 1600) tank’s operational (40%)
-- 100,000 events within 60deg vertical
-- data set Jan04-Mar05 to publish at ICRC Aug05,
with AGASA-equivalent exposure
-- site inaugural celebration Nov05
-- all 24 FDs end of 05
-- all 1600 SDs July06
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Auger Rates
Auger Events/yr:
spectrum above 10^19 eV above 10^20 above 3 10^20 above 5 10^20 above 10^21
E -̂2 2000 200 70 40 20
E -̂2.7 2000 40 7 2 to 3 0.7
E -̂3 2000 20 2 0.8 0.2
EUSO comparison:
EUSO FOV ~ (230 km)2 ~ 70 (instantaneous)Auger FOV (30 km)2
x 15% EUSO duty cycle ~ 10 (averaged)
But EUSO energy threshold ~ n x 1019 eV, versus Auger threshold ~ 1018 eV.
No GZK
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
AGASA hot-spots -- Data
red: E > 4 1019 eVgreen: E > 1020 eV
Cluster Component~ E -1.8±0.5
Neutrinos will point better
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
AGASA hot-spots -- numbersWithin 2.5 degree circles,AGASA identifies six doublet, one triplet,Out of 57 events;
Opening the angle to just 2.6 degrees,AGASA identifies seven doublets, two triplets;
Haverah Park contributes two more paired events in AGASA directions.
NOT corroborated by HiRes.
Source number ~ N12/2N2 ~ 270 to 50%,
weighting with GZK suppression, ~ 10-5 /Mpc3for source density
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
“Essentially Guaranteed” High-Energy Galactic Neutrino Flux
cn = 10 kpc (En / EeV)and
E/ En ~ Q / mn ~ 0.8 x 10-3
E ~ PeV, for En ~ EeV
AGHW2004
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
AMANDA, RICE, Anita, and IceCube:neutrinos as ice-art
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
AMANDA/IceCube event
and coming in the Mediterranean: Nestor, Antares
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
“More Guaranteed”
Icecube atmos background in 1o circle is just 1.5events/yr, 3.5 events offers 95% CL detection in 1 yr;
Calculated signal is 4 /yr and 16 e+ showers/yr.
Conclude that in a few years, IceCube attains 5discovery sensitivity for Fe n e providing “smoking ice” for GP neutron hypothesis.
Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher !
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Galactic Plane -beam, pure anti-e at source
Serpico and kachelreiss, 2005
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Xgal proton flux – Berezinsky et alMass-composition data (HiRes 2002)
Xgal proton dominance begins at 1018 eV, not 1019 eV !F ~ 50 x Waxman-Bahcall AMANDA/RICE/EAS-sensitive !!
(AGHW, 2004)
Theory threshold for p2.7Kpe+e- and data (knee) are at 1017.6 eV.
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Xgal proton fit huge flux
is pion energy/CR energy at source (1 for WB “limit”);z is cosmic evolution factor, 0.6 (no) to 3.0 (SFR)
WB fluxes
low Xgal dominance flux,with no evolution
AGHW, hep-ph/04010003,And in prog, w/ A. Ringwald
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Galaxy Distribution 7-21 Mpc
Visible from the northern site
Auger Skies
Galaxy Distribution 7-21 MpcVisible from the southern site
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Auger neutrons form Cen-A
Since cn = 0.9 Mpc E20,
Neutron survival probability from Cen-A = e –3.8/E
20
= 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;PRL2001
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Size mattersEUSO ~ 300 x AGASA ~ 15 x AugerEUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger
Exposure
1
10
100
1000
10000
Year
Expo
sure AGASA
HiResAugerEUSO
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Extreme Universe Space Observatory
2009 EUSO onboard the ISS (Or Not!)
2012 Hundredth anniversary of Hess
– EUSO finishes three-year data-taking
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
“clear moonless nights”
Blackout_14aug03.jpeg
Or New York State power blackout
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Orbiting Wide-angle Lens (OWL)
3000 events/year above 1020eV
and UHE Neutrinos!
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Neutrinos versus Cosmic-Rays and Photons
s come from central engines
- near Rs of massive BHs
- even from dense “hidden” sources
cf. s vs. s from the sun
s not affected by cosmic radiation(except for annihilation resonance)
s not bent by magnetic fields- enables neutrino astronomy
Also, besides Energy and Direction, ’s carry flavor
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
The “Learned Plot” – merits of cosmic L/E
Oscillation phase is ( Lm2 / 4 E
Figureparameterizedby m2 / (eV)2
Nature’s miracles:L/E, m, nmatter
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
The cosmic flavor-mixing theorem
If theta32 is maximal (it is),And if Re(Ue3) is minimal (it is),
Then and equilibrate;
Further, if initial e flux is 1/3
(as from pion-muon decay chain),Then all three flavors equilibrate.
e:: = 1 : 1 : 1 at Earth
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Democracy Broken:
1. Galactic -beam
2. Source dynamics
3. decay (15 minutes of fame)
4. Vacuum resonance(MaVaNs, LIV vector)
5. Pseudo-Dirac oscillations
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
decay (via majoron emission)P(survive)= e –t/ = e –(L/E)(m/
0)
Beacom, Bell, Hooper, Pakvasa, TJW, PRL2003
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
diagnostic of astro-engines:pp vs. p
The process e+e-- W-- is resonant at 6.4 PeV;
IceCube will have flavor ID, and E/E of 25%,and so can measure On-Res/Off-Res ratio.
pp make nearly equal , with P/Pp ~ 0.6 ::e:e = 2:2:1:1 flavor democracy, e = 1/6 total
p via + make +, with P/Pp ~ 0.25 e = 1:1:1 (no e) e = 1/15 total
IceCube can resolve this (AGHW, hep-ph/0410003)
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Sources:
Bottom-Up “Zevatrons” - givens Cosmogenics ~1019 eV· AGNs· GRBs· Hidden vs. Transparent (the thick/thin debate) Top-Down “EE-trons” - pure speculation· Topological Defects· Wimpzillas, M ~H(post-inflation) ~1022 eV· Msee-saw ~ 1023 eV
· MGUT ~ 1025 eV
· And even MPlanck ~ 1028 eV
Other: - impure thoughts Mirror-Matter mixing Multiverse Leakage (Brane-bridges)
Extreme Energy (EE) Neutrinos
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Model fluxes (Protheroe review 199X)
atmosphere
AGN
GRB GZK
pIsm
SMPs
TDs MGUT
GeV
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
EE Neutrinos are young
Liberated at T=Mev, t= 1 sec;But age depends on energy (Lorentz boost)
(Peter Minkowski)
Consider a 1020 eV neutrino.
Lorentz factor = 1021 for m = 0.1 eV.
Age of Uni is 1018 sec,
But age of is 1018/1021 sec = 1 millisecond !
And it doesn’t even see the stream of radiation rushing past it – untouched !
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Earth Absorption versus Neutrino Cross-Section
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Can’t Lose Thm for Space-based
Whatever the weak cross-section, get robust event rate from HAS or UAS!
and
Get measurement of neutrino cross-section(peak angle also gives )
A. Kusenko, TJWPRL2002
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Upward and Horizontal Air-shower Rates Versus Neutrino Cross-section
HAS
UAS
Kusenko, TJW, PRL2002
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Space-based HAS/UAS
with cirrus (12km) or high cumulus (4km) cloudsNo clouds
Sergio Palomares-Ruiz, TJW
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
HAS event rate is small
e.g. FCR at 1020 eV implies 10-2 events/yr;
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
View (Japanese) of Earth-Moon System – Radio Cherenkov
radio Cherenkov
This is literally GLUE Xpt,
is related to RICE and FORTE,and eventually, to SalSa
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Model Neutrino Fluxes and Future Limits
GLUE, RICE, Forte
,Auger, Anita, EUSO
From Eberle, AR, Song, TJW;Semikoz and Sigl
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Z-burst integrated rate (EUSO/yr) toward Virgo
Red = photonsBlue = protonsGreen = Gal bkgd
Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University
Whether you like protons or nuclei or gammas or neutrinos,this is an exceptional time to be a cosmic-ray physicist !
Hadron-rays:Auger and maybe EUSO should answer the mysteries
raised by AGASA.
Neutrino-rays:– now in the hands of theorists (speculation) and engineers (construction)-- soon in the hands of experimenters (real data)
Promise to reveal -- neutrino physics (cross-section, lifetime, pseudoDirac)-- extreme astrophysics (source dynamics, source environment)-- cosmology (CB, Omega‘s)
Next ten years will be critical, and, the deities/gods willing, most fruitful !
Summary: