High energy neutrino astronomy:Challenges & Prospects

Eli WaxmanWeizmann Institute, ISRAEL

High energy’s: A new window

MeV detectors:• Solar & SN1987A ’s

• Stellar physics (Sun’s core, SNe core collapse) physics

>0.1 TeV detectors:

• Extend horizon to extra-Galactic scale

MeV detectors limited to local (Galactic)

sources

[10kt @ 1MeV1Gton @ TeV , TeV/MeV~106 ]

• Study “Cosmic accelerators” [p, pp ’s’s] physics

HEN detector motivation:Cosmic accelerators

Cosmic-ray E [GeV]

log [dJ/dE]

1 106 1010

E-2.7

E-3

Heavy Nuclei

Protons

Light Nuclei?

Galactic

X-Galactic)?(

[Blandford & Eichler, Phys. Rep. 87; Axford, ApJS 94; Nagano & Watson, Rev. Mod. Phys. 00]

Source: Supernovae)?(

Source?

Source?Lighter

UHE, >1010GeV, CRs

3,000 km2

J(>1011GeV)~1 / 100 km2 year 2 sr

Ground array

Fluorescence detector

Auger:3000 km2

Composition clues

HiRes 2005 Auger 2009

[Waxman 1995; Bahcall & Waxman 03]

[Katz & Waxman 09]

• E2(dN/dE)=E2(dQ/dE) teff. (teff. : p + CMB N +

Assume: p, dQ/dE~(1+z)mE-

• >1019.3eV: consistent with protons, E2(dQ/dE) ~1043.7 erg/Mpc3 yr + GZK

• E2(dQ/dE) ~Const.: Consistent with shock acceleration [Krimsky 77; Bednarz & Ostrowski 98; Keshet & Waxman 05

cf. Lemoine & Revenu 06]

Flux & Spectrum

cteff [Mpc]GZK (CMB) suppression

log(E2dQ/dE) [erg/Mpc2 yr]

Anisotropy clues

Galaxy density integrated to 75MpcCR intensity map (source~gal)

[Waxman, Fisher & Piran 1997]

Biased (source~gal for gal>gal )

[Kashti & Waxman 08]

• Cross-correlation signal: Anisotropy @ 98% CL; Consistent with LSS

• Correlation with AGN ? VCV catalogue: Anisotropy @ 99% CL low-luminosity AGN? Simply trace LSS! (& VCV non-uniform, incomplete…)

[Auger collaboration 07]

Composition-Anisotropy connection

• Plausible assumptions: Acceleration of Z(>>1) to E ~ Acceleration of p to

E/Z Jp(E/Z)>=JZ(E/Z)

+ Note: p(E/Z) propagation = Z(E) propagation

Anisotropy of Z at 1019.7eV implies Stronger aniso. signal (due to p) at (1019.7/Z) eV

! Not observed![:Lemoine & Waxman 09]

The 1020eV challenge

RB eBRBR

R

BR

ccV p c

v

c

v

v/

1~

1 2

cec

BRL p

222

v/2

1v

84

v

v

sun122

20,

2

46

2

20

2

L10

erg/s10eV10/v

p

p

cL

2R

tRF=R/c)

l =R/

2 2

[Waxman 95, 04, Norman et al. 95]

Suspects - L>1012 (2/) Lsun: * Extra-Galactic * Non at d<dGZK Transient - E2(dQ/dE) ~1043.7 erg/Mpc3 yr

Gamma-ray Bursts (GRBs) ~ 102.5, L~ 1019LSun L/2 >1012 Lsun

(dn/dVdt)*E~10-9.5 /Mpc3 yr *1053.5erg ~1044 erg/Mpc3 yr Transient: T~10s << Tp~105 yr

Active Galactic Nuclei (AGN, Steady): ~ 101 L>1014 LSun= few brightest

!! Non at d<dGZK Invoke:

“Dark” (proton only) AGN L~ 1014 LSun , t~1month flares from

stellar disruptions

[Blandford 76; Lovelace 76]

[Waxman 95, Vietri 95, Milgrom & Usov 95]

[Waxman 95]

[Boldt & Loewenstein 00]

[Farrar & Gruzinov 08]

• GRB: 1020LSun, MBH~1Msun, M~1Msun/s, ~102.5

• AGN: 1014 LSun, MBH~109Msun, M~1Msun/yr, ~101

• MQ: 105 LSun, MBH~1Msun, M~10-8Msun/yr, ~100.5

Source physics challenges

Energy extraction

Jet acceleration

Jet content (kinetic/Poynting)

Particle acceleration

Radiation mechanisms

[Reviws: GRBs Kouveliotou 94; Piran 05 AGN Begelman, Blandford & Rees 84 MQ HE: Aharonian et al 2005; Khangulyan et al 2007]

Cosmic accelerators: clues & open Q’s

• X-Galactic, (?)protons “Conventional” accelerators

Ep2dN/dEp~ 0.6x1044 erg/Mpc3 yr

• Open Q’s: Primaries Source identity Acceleration process Cosmic-accelerators physics (BH accretion jets, Baryonic/EM…)

HE Astronomy• p + N + 0 2 ; + e+ + e + +

Identify UHECR sources Study BH accretion/acceleration physics

• E2dn/dE=1044erg/Mpc3yr & p<1:

• If X-G p’s:

Identify primaries, determine f(z)

3

282

)1(,1)(for5,1

srscm

GeV10

zzf

d

dj

[Waxman & Bahcall 99; Bahcall & Waxman 01]

srscm

GeV10)eV10(

28192

d

dj[Berezinsky & Zatsepin 69]

HE experimentsOptical Cerenkov

- South Pole Amanda: 660 OM, 0.05

km3

IceCube: +660/yr OM (05/06…) 4800 OM=1 km3s - Mediterranean Antares: 10 lines (Nov 07), 750 OM 0.05 km3

Nestor: (?) 0.1 km3

km3Net: R&D 1 km3

•UHE: Radio Air shower Aura, Ariana (in Ice) Auger ()

ANITA (Balloon) EUSO (?) LOFAR

Single flavor Multi flavor

[Anchordoqui & Montaruli 09]

Star bursts: A lower bound?

• Star burst galaxies: - Star Formation Rate ~103Msun/yr >> 1 Msun/yr “normal”

(MW) - Density ~103/cc >> 1/cc “normal” - B ~1 mG >> 1G “normal”

• Most stars formed in (z>1.5) star bursts

• High density + B: CR e-’s lose all energy to synchrotron radiation CR p’s lose all energy to production

[Loeb & Waxman 06]

[Quataert et al. 06]

Mark Westmoquette (University College London), Jay Gallagher (University of Wisconsin-Madison), Linda Smith (University College London), WIYN//NSF, NASA/ESA

Robert Gendler

M82 M81

eepnpp ,

Synchrotron radio calibration

[Loeb & Waxman 06]

M82, NGC253: Hess, VERITAS 09

Fermi 09 dN/dE~1/Ep, p<~2.2

Starbursts

GRB ’s

• If: Baryonic jet

• Background free:

2GeV3.0// peV10,eV1010,MeV1 5.14165.2 p

yrkm/20

eV10,srscm

GeV102.0

2

5.142

82

J

WB

2.0pf

[Waxman & Bahcall 97, 99; Rachen & Meszaros 98; Alvarez-Muniz & F. Halzen 99; Guetta et al. 04; Hooper, Alvarez-Muniz, Halzen & E. Reuveni 04]

;yrkm/TeV1005.0

104~ 22

3

EJ

oA

TeV1005.2

TeV1007.1

E

E

The current limit

[Achterberg et al. 08 (The IceCube collaboration)]

- physics & astro-physics

• decay e:: = 1:2:0 (Osc.) e:: = 1:1:1

appearance experiment

• GRBs: - timing (10s over Hubble distance) LI to 1:1016; WEP to 1:106

• EM energy loss of ’s (and ’s) e:: = 1:1:1 (E>E0) 1:2:2

GRBs: E0~1015eV

• Combining E<E0, E>E0 flavor measurements

may constrain CPV [Sin13 Cos]

[Waxman & Bahcall 97]

[Rachen & Meszaros 98; Kashti & Waxman 05]

[Waxman & Bahcall 97; Amelino-Camelia,et al.98; Coleman &.Glashow 99; Jacob & Piran 07]

[Blum, Nir & Waxman 05]

Outlook• Particle+Astro-phys. Open Q’s - >1011GeV particles: primaries, f(z), origin & acceleration - Physics of relativistic sources (GRBs, AGN, MQ…) - <1011GeV particles: sources, acceleration, propagation (SNRs, starbursts, …) - appearance

Timing LI to 1:1016; WEP to 1:106

Flavor ratios CPV

• New HE , CR and detectors >103 km2 hybrid >1019eV CR detectors~1 km3 (=1Gton) 1-1000TeV detectors>>1 km3 [radio,…] >>1000TeV detectors

10MeV—10GeV -ray satellite (AGILE, GLAST) >0.1TeV (ground based) -ray telescopes (Milagro, HESS, MAGIC, VERITAS)

Point source

s

AMANDA &IceCube

The Mediterranean effort

• ANTARES (NESTOR, NEMO) KM3NeT

Back up slides

GRB proton/electron acceleration

Electrons• MeV ’s:

• <1:

• e- () spectrum:

• e- ()energy production

erg/s1051L

5.210

2/ eee ddn

yrMpc

erg10erg10

yrGpc

10~

34452

32

e

ee d

nd

yrMpc

erg10erg10

yrGpc

5.03

445.533

[Waxman 95, 04] Afterglow, RGRB~SFR

Protons• Acceleration/expansion:

• Synchrotron losses:

• Proton spectrum:

• p energy production:

erg/s10/1025.22

20,5.50 pL

4/14/320,

2 ms10/10 tp

2/ ppp ddn

yrMpc

erg10

34422

e

ee

p

pp d

nd

d

nd

52

The GRB “GZK sphere”

• LSS filaments: D~1Mpc, fV~0.1, n~10-6cm-3, T~0.1keV

B=(B2/8nT~0.01 (B~0.01G), B~10kpc

• Prediction:

p

D

B

few~)eV103( 20GRBsN[Waxman 95; Miralda-Escude &

Waxman 96, Waxman 04]

BBVGRBs

GRB

BBVp

DelaySpread

BBVp

fDN

R

fDd

c

d

fDd

2220

3

2

2

2052

2/1

20

2/10

10~)eV10(

yrGpc/5.0~

eV10/

Mpc100/yr10~~~

eV10/

Mpc100/3.0

GRB Model Predictions

[Miralda-Escude & Waxman 96]

AGN models??

BBR05

>1019eV cosmic rays: Clue summary

• Spectrum (+Xmax)

likely X-Galactic protons• Anisotropy + Spectrum likely “Conventional” sources• L constraint likely Transient sources

• Ep2dN/dEp~ 0.7x1044 erg/Mpc3 yr

• What next for Auger?

Identify (narrow spectrum) point source(s)?