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Radio Detection of the Highest Energy
Astrophysical Neutrinos
David Saltzberg University of California, Los Angeles (UCLA)
Neutrino 2006, Santa FeJune 19, 2006
---A tale taking us---
from the South Pole to the Moon,
from the Bahamas to low-Earth orbit
from120,000 ft above Antarctica
to 1500 ft below Louisiana
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Astrophysical Neutrino Sources “Batting 1000”
weak eigenstates ≠ mass eigenstates mass
Every source has:1. has had major impact on particle physics
2. Looks deeper into the source than otherwise possible
lack of
dispersion mass limits
SN1987A
Kamiokande
Homestake
Super-K
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The range of photon astronomy
Atmospheric Cherenkov >1012 eV photons
.
Radio Astronomy <10-7 eV photons
…and everything in between
Karl Jansky, Holmdel NJ Hess Telescope, Namibia
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The end of extra-galactic photon
astronomy
.
But no cutoffs for neutrinos!
G. Sigl
Distance to M32
Pho
ton
atte
nuat
ion
Leng
th (
MP
c)+ (IR,CMB,URB) ! e+ e-
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Motivation for an Astrophysicist:Neutrinos point back
GZK with protons:
GZK with nuclei:
neutrinos
+
(NOT a typo)~1019 eV
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Neutrinos Point Back
~ 10Mpc/1000Mpc ~ 30 arcminutes
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One Motivation for a Particle Physicist
Exotic Physics: UHECR would result from decays of super-heavy particles. Example: Grand Unified Supersymmetric Theories:
Is its lifetime comparable to age of universe or is it ~10-40 sec?
Loophole—produce them continuously by “topological defects” (TD)
MX ~ 1025 eV
`EM’
`weak’
strong
1013 1019 1025 (eV)
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More Particle Physics:z=1 is a VERY long baseline
One experimental parameter: (L/E)|experiment / ~tproper
Determines (largely) the sensitivity to
m2, decays (eg majoron emission) decoherence …
available
?
Decays alter flavor ratios: Beacom,Bell,Hooper,Pakvasa,Weiler, PRL 90,181301 (2003)Recent review: Pakvasa, Phys. Atom. Nucl., 67, 1154 (2004)
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The UHE Beam
GZK p ~1 /km2/yr above 1017 eV
TD
GZK p
GZK Fe
GZK p : Engel, Seckel, Stanev, PRD 64,093010 GZK Fe: Ave, Busca, Olinto, Watson,Yamamoto, Astropart. Phys., 23, 19 TD: Yoshida, Dai Jui, Sommers, Ap. J. 479, 547
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These are not your typical neutrinos
Linteraction ~ only 500 km of rock at 1019 eV
Earth attenuation is significant
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Quantifying Detection
[A ] t vs. energy (& background) for each neutrino flavor describes experiment For example: [A ] for a flat,black paddle=A£2 [V ]=[A ]£ Lint accounting for neutrino cross section vs. energy
(Discovery potential also depends on background)
Optical techniques have Latten~100 m Instrument up to ~km3
Need many km3 of material to detect GZK> 1015 eVNeed longer attenuation lengths
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km3 and Beyond?Two Good Ideas by Gurgen Askaryan
(I)(1962)
UHE event will induce an e/ shower:
In electron-gamma shower in matter, there will be ~20% more electrons than positrons.
Compton scattering: + e-(at rest) + e-
Positron annihilation: e+ + e-(at rest) +
lead
e-
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Two Good Ideas by Gurgen Askaryan (II)
Excess charge moving faster than c/n in matter emit Cherenkov Radiation
In dense material RMoliere~ 10cm.
<<RMoliere (optical case), random phases P N
>>RMoliere (microwaves), coherent P N2
dddPCR
Confirmed with Modern simulations + Maxwell’s equations: (Halzen, Zas, Stanev, Alvarez-Muniz, Seckel, Razzaque, Buniy, Ralston, McKay …)
Each charge emits field |E| eik•r
and Power |Etot|2
Optical viewing ~ 100m, Radio viewing ~ 1km
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South Pole Ice properties:RF attenuation
Deeper ice is, on average, even colder – So will have an even longer attenuation length
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The SLAC ``Kitty Litter’’ box4 tons sand
Amplitude expected 100% linearly polarizedCherenkov angle
SLAC FFTB
PRF/ E2
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RICE Experiment
“Radio in Ice Experiment”
Dipoles (250-1000 MHz) on AMANDA strings @ S Pole
200 x 200 x 200 meter array E>~1017 eV [V]» 10 km3-sr
Candidate event
I. NEW 7 year result Kravchenko, et al., PRD73,082002
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First results (1996)
12 hrs using single Parkes 64m dish in Australia.
Limitted by R.F.I.
T. Hankins et al., MNRAS 283, 1027 (1996)
Zheleznyk and Dagkesamanskii (1988)
1020 eV produces ~1000 Jy at 2GHz
(1Jy = 10-26 W/m2/Hz)
brightest quasars ~25 Jy at this frequency band
Moon as blackbody: ~200 Jy
no need to go to the moon
use radiotelescopes
Using the Moon as a 200,000 km3 Target
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Goldstone Lunar UHE Neutrino Search (GLUE)P. Gorham et al., PRL 93, 041101 (2004)
Two antennas at JPL’s Goldstone, Calif. Tracking Station
limits on >1020 eV ’s
regolith atten. len. ~20 m
~123 hours livetime
[V]eff~600 km3-sr
New experiment planned using Westerbork (NL) Antennas
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A more detailed view of GLUE(since common to most radio
detection)
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FORTE satellite(Fast On-orbit Recording of Transient
Events)
Main mission: synaptic lightning observation
Viewed Greenland ice with appropriate trigger (1997-99) 1.9 MILLION km3
38 days £ 6% Can self-trigger on transient events in
22MHz band in VHF band (from 30 to 300 MHz)
Event characterization polarization ionospheric group delay and
birefringence timing
Log-periodic antennas
N. Lehtinen et al., PRD 69, 013008 (2004)
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Example Forte Event
Ethresh » 1022 eV
[V] ~ 100,000 km3 sr, but threshold extremely high.
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>1 million cubic km!
60 days in 3 flights
E>1017 eV
[V]~20,000 km3-sr
ANITA
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ANITA Schedule
December: 2003-04 Anita-lite (completed)
June 2005 Test run at Ft. Sumner, NM (completed)
June 2006 Full ANITA assembled (completed)
June 2006 Testbeam with Ice target @SLAC (now)
July 2006 Flight-ready test before shipment to Antarctica
Dec 2006 full-ANITA flight Future seasons Anticipate 2
more flights
photo: Jeff Kowalski
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18 day flight, Dec. 03 - Jan. 04 Experience assembling the payload
on the ice Calibration studies: ground pulse
and Sun Analysis of Anita-lite data
Backgrounds Timing resolution Angular resolution No events seen
Anita-LITE
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Amanda
RICE
ANITA-LITE
GLUE
FORTE
Approaching GZK sensitivity:Limits as of 2006
limits are for energy bin with Ehi/Elo=e
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SALSA:A possible salt detector
~25km3 in upper 3km of dome (75 km3 water-equiv.) >2£ denser than ice easier to deploy than S.Pole
Calorimetric; large V,; Cherenkov polarization usable for tracking
Good candidates in Texas and Louisiana, maybe Utah
Dutch investigating sites as well
diapir action pushes out water~1km3 w.e.
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Salt Dome DetectorNoise and attenuation length
measurements
Fully contained events: Expect good flavor ID for charged-current events.
RF quiet
New data just taken in Cote Blanche, LA
Hockley Dome measurements
Attenuation >250m (>500 m w.e.)
No evidence of birefringence or scattering
P. Gorham et al., NIMA 490, 476 (2002)
Salt mine at Avery Island, Louisiana, USA
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ARIANNA
Ice shelf
Reflected Ray
Direct Ray
Ice shelf
Reflected Ray
Direct Ray
Increase solid angle with downgoing eventsSee reflected radio off of salt water
~500m
Antarctic Ross Ice shelf Antenna Neutrino Array
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ARIANNA: 100 £ 100 station Array
Ross Ice Shelf, Antarctica
antennas
R&D Funding established from NSF (SGER) and DOE (ADRP)NSF to provide helicopter & basecamp to make measurements this Novemer
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Expanding Ice-CubeHybrid Acoustic & Radio Technique
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Reaching GZK sensitivity & Lowering the Theshold
full ANITA
ARIANNA/
SALSA
TD
GZK-p
GZK-Fe
Events! even if UHECR are Iron limits are for energy bin with Ehi/Elo=e
I will add HYBRID-ICE-CUBE to the proceedings
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Another Good Idea from Askaryan (III):Acoustic Detection
(1957)
@1km perp.
sim
Verified in beamtests at Brookhaven (J. Learned)
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SAUND(Study of Acoustic Underwater Neutrino Detection)
7 Hyrdophones, subset U.S. Navy array (AUTEC)
Detection 7kHz to 50 kHz
Noise floor -1.7, sets threshold ~ 1023 eV
Physics run 195 days
Bahamas“Tongue of
the Ocean”
J. Vandenbrouke et al.,Ap. J. 621, 301
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SAUND Calibration
~1021 eV !
Attenuation length >500-1000m
E ~ 1022 eV: too high for now.
but salt domes may prove 10£ more signal and much less background
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Other Developing Ideas
Drone flights over deepest Antarctic Iceuse the best ice: 4km deepcloser lower threshold instrument can be maintained
ANITA-IIPhased array of balloon-borne deployable antennas
Europa orbiter
There are more ideas than people to work on them
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•Conclusion-II (for an astronomer):
from Nat. Research council
Domain of radio & acoustic
Conclusion-I (for a particle physicist):UHE may provide a unique high-energy lab
- Probe total cross section & new physics at highest Ecm
- The longest baseline available neutrinos– by far
- May detect super-heavy decaying particles
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BACKUP SLIDES
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n p
e
e
n p
W
Extremely Low-x: (~10-8) calculations e.g. above 1017 eV, more likely to scatter off of bottom sea, than u,d valence
Neutrino interactionsGhandhi et al., Astropart. Phys. 5, 81 (1996):
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Particle Physics at the Energy Frontier:
the UHE Neutrino Cross Section
SM
micro BH productionAlvarez-Muniz et al., PRD65, 124015 (2002)
Cross section can be measured by looking at zenith angle distributions
Ec.m. = 150 TeV Not accessible by LHC; UHECR not useful
TeV scale quantum gravity(compilation by D. Hooper)