Ultra - High Energy Neutrino Astronomy Ultra - High Energy Neutrino Astronomy DmitrySemikoz UCLA, Los Angeles in collaboration with F.Aharonian, A.Dighe,

Ultra - High Energy Neutrino Ultra - High Energy Neutrino AstronomyAstronomy

Dmitry Dmitry

SemikozSemikozUCLA, Los Angeles UCLA, Los Angeles

in collaboration with in collaboration with

F.Aharonian, A.Dighe, O.Kalashev, F.Aharonian, A.Dighe, O.Kalashev, M.Kachelriess, V.Kuzmin, A.Neronov, M.Kachelriess, V.Kuzmin, A.Neronov,

G.Raffelt, G.Sigl , M.Tortola and G.Raffelt, G.Sigl , M.Tortola and R.TomasR.Tomas

Ultra High Energy \\ Cosmic Rays

Fermilab February 9, 2004

Overview: Introduction: high energy neutrinos Experimental detection of high energy

neutrinos:Under/ground/water/iceHorizontal air showersRadio detection Acoustic signals from neutrinos

Neutrinos from UHECR protons Neutrinos from AGN


Most probable neutrino sources Neutrinos from Galactic SN Neutrinos in exotic UHECR models Conclusion


INTRODUCTION


Extragalactic neutrino flux? Sanduleak –69 Sanduleak –69 202 202

Large Magellanic Cloud Large Magellanic Cloud Distance 50 kpcDistance 50 kpc (160.000 light years)(160.000 light years)

Tarantula NebulaTarantula Nebula

Supernova 1987A Supernova 1987A 23 February 198723 February 1987

Georg

Raff

elt

, M

ax-P

lan

ck-I

nst

itu

t fü

r Ph

ysi

k (M

ün

chen

)


Neutrino Signal from SN 1987A Kamiokande (Japan)Kamiokande (Japan) Water Cherenkov detectorWater Cherenkov detector Clock uncertainty Clock uncertainty 1 min1 min

Kamiokande (Japan)Kamiokande (Japan) Water Cherenkov detectorWater Cherenkov detector Clock uncertainty Clock uncertainty 1 min1 min

Irvine-Michigan-BrookhavenIrvine-Michigan-Brookhaven (USA)(USA) Water Cherenkov detectorWater Cherenkov detector Clock uncertainty Clock uncertainty 50 ms50 ms

Irvine-Michigan-BrookhavenIrvine-Michigan-Brookhaven (USA)(USA) Water Cherenkov detectorWater Cherenkov detector Clock uncertainty Clock uncertainty 50 ms50 ms

Baksan Scintillator TelescopeBaksan Scintillator Telescope (Soviet Union)(Soviet Union) Clock uncertainty +2/-54 sClock uncertainty +2/-54 s

Baksan Scintillator TelescopeBaksan Scintillator Telescope (Soviet Union)(Soviet Union) Clock uncertainty +2/-54 sClock uncertainty +2/-54 s

Within clock uncertainties,Within clock uncertainties, signals are contemporaneoussignals are contemporaneous Within clock uncertainties,Within clock uncertainties, signals are contemporaneoussignals are contemporaneous


Atmospheric 's in AMANDA-II neural network energy reconstruction regularized unfolding

spectrum up to 100 TeV compatible with Frejus data

In future, spectrum will be usedto study excess due to cosmic ‘s

PRELIMINARY

1 TeV


Why UHE neutrinos can exist?

Protons are attractive candidates to be accelerated in astrophysical objects up to highest energies E~1020 eV.

Neutrinos can be produced by protons in P+P pions or P+pions reactions inside of astrophysical objects or in intergalactic space.

Neutrinos can be produced directly in decays of heavy particles. Same particles can be responsible for UHECR events above GZK cutoff.


Pion production

ee

...

'

i

b

i

b

PP

NN

p

n

20

eepn

Conclusion: proton, photon and neutrino fluxes are connected in well-defined way. If we know one of them we can predict other ones: tottot EE ~


High energy neutrino

experiments


Neutrino – nucleon cross section

Proton density

np~ 1024/cm3

Distance R~104km Cross section

N=1/(Rnp)~10-33cm2

This happens at energy E~1015 eV.

~E0.4


Experimental detection of E<1017eV neutrinos

Neutrinos coming from above are secondary from cosmic rays

Neutrino coming from below are mixture of atmospheric neutrinos and HE neutrinos from space

Earth is not transparent for neutrinos E>1015eV

Experiments: MACRO, Baikal, AMANDA


Experimental detection of UHE (E>1017eV) neutrinos

Neutrinos are not primary UHECR

Horizontal or up-going air showers – easy way to detect neutrinos

Experiments: Fly’s Eye, AGASA, HiRes


Radio detection


e + n p + e-

e- ... cascade

relativist. pancake ~ 1cm thick, ~10cm

each particle emits Cherenkov radiation

C signal is resultant of overlapping Cherenkov cones

for >> 10 cm (radio) coherence

C-signal ~ E2

nsec

negative charge is sweeped into developing shower, which acquiresa negative net chargeQnet ~ 0.25 Ecascade (GeV).

Threshold > 1016 eVExperiments:

GLUE, RICE, FORTE


Acoustic detection


d

R

Particle cascade ionization heat pressure wave

P

t

s

Attenuation length of sea water at 15-30 kHz: a few km(light: a few tens of meters)

→ given a large initial signal, huge detection volumes can be achieved.

Threshold > 1016 eV

Maximum of emission at ~ 20 kHz


Renewed efforts along acoustic method for GZK neutrino detection

Greece: SADCO Mediterannean, NESTOR site, 3 strings with hydrophones

Russia: AGAM antennas near Kamchatka:existing sonar array for submarine detection

Russia: MG-10M antennas: withdrawn sonar array for submarine detection

AUTEC: US Navy array in Atlantic:existing sonar array for submarine detection

Antares: R&D for acoustic detection

IceCube: R&D for acoustic detection


Present limits on neutrino flux


MACRO


FORTE


4-string stage (1996)

First underwater telescopeFirst neutrinos underwater


AMANDA-II

depth AMANDA

Super-K

DUMANDAmanda-II:677 PMTsat 19 strings

(1996-2000)


AGASA

AGASA covers an area of about 100 km2 and consists of 111 detectors on the ground (surface detectors) and 27 detectors under absorbers (muon detectors). Each surface detector is placed with a nearest-neighbor separation of about 1 km.


High Resolution Fly’s Eye: HiRes

HiRes 1 and HiRes 2 sit on two small mountains in western Utah, with a separation of 13 km.

HiRes 1 has 21 three meter diameter mirrors which are arranged to view the sky between elevations of 3 and 16 degrees over the full azimuth range;

HiRes 2 has 42 mirrors which image the sky between elevations of 3 and 30 degrees over 360 degrees of azimuth.

At the focus of each mirror is a camera composed of 256 40-mm diameter hexagonal photomultiplier tubes, each tube viewing a 1 degree diameter section of the sky.


GLUE Goldstone Lunar Ultra-high Energy Neutrino Experiment

E2·dN/dE < 105 eV·cm-2·s-1·sr-1

Lunar Radio Emissions from Inter-actions of and CR with > 1019 eV

1 nsec

moon

Earth

Gorham et al. (1999), 30 hr NASA Goldstone70 m antenna + DSS 34 m antenna

at 1020 eV

Effective target volume~ antenna beam (0.3°) 10 m layer

105 km3


RICE Radio Ice Cherenkov Experiment

firn layer (to 120 m depth)

UHE NEUTRINO DIRECTION

300 METER DEPTH

E 2 · dN/dE < 10-4 GeV · cm-2 · s-1 · sr-1

20 receivers + transmitters

at 1017 eV


Future limits on neutrino flux


Mediterranean Projects

4100m

2400m

3400mANTARESNEMO NESTOR


NEMO 1999 - 2001 Site selection and R&D

2002 - 2004 Prototyping at Catania Test Site 2005 - ? Construction of km3 Detector

ANTARES 1996 - 2000 R&D, Site Evaluation 2000 Demonstrator line 2001 Start Construction

September 2002 Deploy prototype line December 2004 10 (14?) line detector complete 2005 - ? Construction of km3 Detector

NESTOR 1991 - 2000 R & D, Site Evaluation Summer 2002 Deployment 2 floors Winter 2003 Recovery & re-deployment with 4 floors Autumn 2003 Full Tower deployment 2004 Add 3 DUMAND strings around tower 2005 - ? Deployment of 7 NESTOR towers


Baikal km3 project: Gigaton Volume Detector GVD


IceCube

1400 m

2400 m

AMANDA

South Pole

IceTop

- 80 Strings- 4800 PMT - Instrumented

volume: 1 km3

- Installation: 2004-2010

~ 80.000 atm. per year


Pierre Auger observatory


Telescope Array


MOUNT


OWL/EUSO


ANITA Antarctic

Impulsive

Transient

Array

Flight in 2006


Natural Salt Domes

Potential PeV-EeV Neutrino Detectors

SalSA Salt Dome Shower Array


Renewed efforts along acoustic method for GZK neutrino detection

Greece: SADCO Mediterannean, NESTOR site, 3 strings with hydrophones

Russia: AGAM antennas near Kamchatka:existing sonar array for submarine detection

Russia: MG-10M antennas: withdrawn sonar array for submarine detection

AUTEC: US Navy array in Atlantic:existing sonar array for submarine detection

Antares: R&D for acoustic detection

IceCube: R&D for acoustic detection


RICE AGASA

Amanda, Baikal2002

2007

AUGER

Anita

AABN

2012

km3

EUSO,OWLAuger

Salsa

GLUE

2004

RICE

Amanda II


Neutrinos from UHECR protons


Why neutrinos from UHE protons?

All experiments agree (up to factor 2) on UHECR flux below cutoff. All experiments see events above cutoff!

Majority of the air-showers are hadronic-like

Simplest solution for energies 5x1018 eV < E < 5x1019 eV: protons from uniformly distributed sources like AGNs.


Active galactic nuclei can accelerate heavy nuclei/protons



Photo-pion production

ee

iNN '

p

n

20

eepn


Parameters which define diffuse neutrino flux

Proton spectrum from one source:

Distribution of sources:

Cosmological parameters:

E

AEF )(

maxmin EEE

3)1( mzD maxmin zzz

0H vac


Theoretical predictions of neutrino fluxes

WB bound: 1/E2 protons; distribution of sources – AGN; analytical calculation of one point near 1019 eV.

MPR bound: 1/E protons; distribution of sources – AGN; numerical calculation for dependence on Emax

The ray bound: EGRET


The high energy gamma ray detector on the Compton Gamma Ray Observatory (20 MeV - ~20 GeV)

EGRET: diffuse gamma-ray flux


Detection of neutrino fluxes: today


Future detection of neutrinos from UHECR protons

AGN,1/E

Old sources1/E^2

/ EUSO


Neutrinos from Active galactic

nuclei


Active Galactic Nuclei (AGN)

Active galaxies produce vast amounts of energy from a very compact central volume.

Prevailing idea: powered by accretion onto super-massive black holes (106 - 1010 solar masses). Different phenomenology primarily due to the orientation with respect to us.

Models include energetic (multi-TeV), highly-collimated, relativistic particle jets. High energy -rays emitted within a few degrees of jet axis. Mechanisms are speculative; -rays offer a direct probe.


Neutrinos from AGN core

/ EUSO


Photon background in core Energy scale

E= 0.1 – 10 eV Time variability

few days or

R = 1016cm Model: hot thermal

radiation.

T=1 eVT=10 eV


Photo-pion production

ee

iNN '

p

n

20

eepn


Neutrino spectrum for various proton spectra and backgrounds

1/E

1/E2

T=10 eV

1/E2

T=1 eV

E~1018eV

Atm.flux


Most probable neutrino sources


Optics: SDSS. Most powerful objects are AGNs

500 sq deg of the sky, 14 million objects, spectra for 50,000 galaxies and 5,000 quasars.

Distance record-holder

>13,000 quasars (26 of the 30 most distant known)


Low energy radiation from AGN is collimated

Typical gamma-factor is

Radiation is collimated in 1/ angle ~ 5o in forward direction.


EGRET 3rd Catalog: 271 sources

Most of identified MeV-GeV sources are blazars


Which sources ?

Blazars (angle – energy correlation)


High energy photons from pion decay cascade down in GeV region


EGRET 3rd Catalog: 271 sources

Only 22 sources from 66 are GeV - loud


Which sources ?

Blazars (angle – energy correlation) Blazars should be GeV loud (conservative model)


Which sources ?

Blazars (angle – energy correlation) Blazars should be GeV loud (conservative model) ‘Optical depth’ for protons should be large:

pnR


Bound on blazars which can be a neutrino sources


TeV blazars does not obey last condition

Indeed, in order TeV blazars be a neutrino sources:

pnR nR

p= 6x10-28cm2 while = 6.65 x 10-25cm2

CONTRADICTION!!!


Which sources ?

Blazars (angle – energy correlation) Blazars should be GeV loud (conservative model)

Optical depth for protons should be large:

pnR No 100 - kpc scale jet detected (model-dependent)


Neutrino production in AGN


Collimation of neutrino flux in compare to GeV flux


Neutrinos from Galactic

Supernova


Prompt neutrino signal in 1-50 MeV energies.Prompt neutrino signal in 1-50 MeV energies.

1-10 sec after SN burst/Strong signal in each optical 1-10 sec after SN burst/Strong signal in each optical

module / SN 1987A signalmodule / SN 1987A signal

Prompt neutrino signal in 1-50 MeV energies.Prompt neutrino signal in 1-50 MeV energies.

1-10 sec after SN burst/Strong signal in each optical 1-10 sec after SN burst/Strong signal in each optical

module / SN 1987A signalmodule / SN 1987A signal

50-200 events with E> 1TeV in 10-12 hours after burst. 50-200 events with E> 1TeV in 10-12 hours after burst. Shock front reached surface and became colisionless.Shock front reached surface and became colisionless. Duration t ~ 1 hour / Waxman & Loeb 2001Duration t ~ 1 hour / Waxman & Loeb 2001

50-200 events with E> 1TeV in 10-12 hours after burst. 50-200 events with E> 1TeV in 10-12 hours after burst. Shock front reached surface and became colisionless.Shock front reached surface and became colisionless. Duration t ~ 1 hour / Waxman & Loeb 2001Duration t ~ 1 hour / Waxman & Loeb 2001

SN shock interact with pre-SN wind and interstelar SN shock interact with pre-SN wind and interstelar medium. 1000-10000 events with E>1 TeV in km^3 medium. 1000-10000 events with E>1 TeV in km^3 detectordetectorFrom 10 days till 1 year /Berezinsky & Ptuskin 1989From 10 days till 1 year /Berezinsky & Ptuskin 1989

SN shock interact with pre-SN wind and interstelar SN shock interact with pre-SN wind and interstelar medium. 1000-10000 events with E>1 TeV in km^3 medium. 1000-10000 events with E>1 TeV in km^3 detectordetectorFrom 10 days till 1 year /Berezinsky & Ptuskin 1989From 10 days till 1 year /Berezinsky & Ptuskin 1989

Possible neutrino signals from Galactic SN in km^3 detector


Supernova MonitorAmanda-II

Amanda-B10

IceCube0 5 10 sec

Count rates

B10: 60% of Galaxy

A-II:95% of Galaxy

IceCube:up to LMC


Pointing to Galactic SN

AMANDA II will see 5-20 events with E> 1TeV. For angular resolution 2o of each event. Pointing to SN direction is possible with resolution ~0.5o

For ANTARES pointing is up to 0.1o . Compare to SuperKamiokande 8o now and 3.5o

with gadolinium. HyperKamiokande ~0.6o


Detection of Galactic SN from wrong side by km^3 detector

Atmospheric muons 5*1010/year or

300/hour/(1o)2

Signal 200 events, besides energy cut 1 TeV. Angular resolution 0.8o for each event or less

then 0.1o for SN signal !!!

(A.Digle, M.Kachelriess, G.Raffelt, D.S. and R.Tomas, hep-ph/0307050)


Neutrinos from exotic UHECR

models


Z-burst mechanism(T.Weiler, 1982)

Resonance energy E = 4 1021 (1 eV/m) eV

Works only if

meV

Mean free path of neutrino is

L = 150 000 Mpc >> Luniv


Cross sections for neutrino interactions with

relict background and


Pure neutrino sources


Sources of both and

Kalashev, Kuzmin, D.S. and Sigl, hep-ph/0112351


Gelmini-Kusenko model: X->


FORTE and WMAP practically exclude Z-burst model

D.S. and G.Sigl, hep-ph/0309328


Top-down models


New hadrons (Kachelriess, D.S. and Tortola, hep-ph/0302161)


Diffuse neutrino flux

Flux is unavoidably high due to

Shape depends on distribution of background photons and on proton spectrum

S

p

S

pUHE E

EFF


Conclusions Sensitivity of the neutrino telescopes will be

increased in 102-3 times during next 10 years. Now they just on the border of theoretically interesting region.

Secondary neutrino flux from UHECR protons can be detected by future UHECR experiments.

Neutrino flux from AGN’s can be detected by under-water/ice neutrino telescopes. GeV-loud blazars with high optical depth for protons are good candidates for neutrino sources.

Galactic SN can be detected with neutrinos at low and high energies.

Some of exotic UHECR models will be ruled out or confirmed in near future by neutrino data.


References:

Diffuse neutrino flux. O.Kalashev, V.Kuzmin, D.S. and G.Sigl, hep-ph/0205050; D.S. and G.Sigl, hep-ph/0309328

Extragalactic neutrino sources. A.Neronov & D.S., hep-ph/0208248

AGN jet model. A.Neronov, D.S., F.Aharonian and O.Kalashev, astro-ph/0201410

Z-burst model. O.Kalashev, V.Kuzmin, D.S. and G.Sigl, hep-ph/0112351

New hadrons as UHECR. M.Kachelriess, D.S. and M.Tortola, hep-ph/0302161

SN pointing with low and high energy neutrinos. R.Tomas, D.S., G.Raffelt, M.Kachelriess and A.Dighe, hep-ph/0307050

Documents

Ultra - High Energy Neutrino Astronomy Ultra - High Energy Neutrino Astronomy DmitrySemikoz UCLA, Los Angeles in collaboration with F.Aharonian, A.Dighe,