The case for High energy neutrino astronomy

1
The case forHigh energy neutrino astronomy

• Eli Waxman
• Weizmann Institute, ISRAEL

2
High energy ns A new window

• MeV n detectors
• Solar SN1987A ns
• Stellar physics (Suns core, SNe core collapse)
• n physics
• gt0.1 TeV n detectors
• Extend n horizon to extra-Galactic scale
• MeV n detectors limited to local (Galactic)
  sources
• 10kt _at_ 1MeV?1Gton _at_ TeV , sTeV/sMeV106
• Study Cosmic accelerators pg, pp ? ps?ns
• n physics

3
The 1020eV challenge
v
R
B
/G
v
G2
G2
2R
l R/G
(dtRFR/Gc)
Waxman 95, 04, Norman et al. 95

• AGN (Steady) G 101 ? Lgt1014 LSun ? few
  brightest
• 1/100 Gpc3? d gtgt 100Mpc ? ?? AGN flares
• GRB (transient) G 102.5 ? Lgt1017 LSun
  Lg 1018LSun

Blandford 76 Lovelace 76
Farrar Gruzinov 08
Waxman 95, Vietri 95, Milgrom Usov 95
4
Source physics

• GRB 1020LSun, MBH1Msun, M1Msun/s,
  G102.5
• AGN 1014 LSun, MBH109Msun, M1Msun/yr,
  G101
• MQ 105 LSun, MBH1Msun,
  M10-8Msun/yr, G100.5

Jet acceleration
Energy extraction
Particle acceleration
Jet content (kinetic/Poynting)
Radiation mechanisms
5
Clues CR phenomenology
Galactic heavy (hypernovae ? Z10
to 1019eV)
log dJ/dE
Flattening, Near isotropy, Heavy? light (?)
E-2.7
Protons
E-3
X-Galactic, ?Light
Heavy Nuclei
1
1010
106
Cosmic-ray E GeV
Blandford Eichler, Phys. Rep. 87 Axford,
ApJS 94 Nagano Watson, Rev. Mod. Phys. 00
6
Constraints Flux Spectrum
Particle acc. SFR , AGN, GRB
Waxman 1995 Bahcall Waxman 03
Berezinsky et al. 08
DEsys/E20
Kashti Waxman 08
7
Clues Anisotropy
Biased (rsourcergal for rgalgtrgal )
CR intensity map (rsourcergal)
Galaxy density integrated to 75Mpc
Waxman, Fisher Piran 1997
Kashti Waxman 08

• Cross-correlation signal
• Anisotropy _at_ 98 CL Consistent with LSS
• Few fold increase ? gt99 CL, but not 99.9
  CL
• Correlation with AGN ?
• VCV catalogue 99 CL
• Swift catalogue 84 (98 a posteriori)
  CL
• ? low-luminosity AGN? Simply trace
  LSS!

Auger collaboration 07
George et al. 08
8
gt1019eV 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)?

9
HE n Astronomy

• p g ? N p
• p0 ? 2g p ? e ne nm nm
• ? Identify UHECR sources
• Study BH accretion/acceleration physics
• E2dn/dE1044erg/Mpc3yr tgplt1
• If X-G ps
• ? Identify primaries, determine f(z)

Waxman Bahcall 99 Bahcall Waxman 01
10
AGN n models??
BBR05
11
Experiments

• Optical Cerenkov
• - South Pole
• Amanda 660 OM, 0.05 km3
• IceCube 660/yr OM
• (05/06, 06/07)
• 4800 OM1 km3s
• - Mediterranean
• Antares 10 lines (Nov 07),
• 750 OM ? 0.05 km3
• Nestor (?) ? 0.1 km3
• km3Net RD ? 1 km3

• UHE Radio Air shower
• Aura, Ariana (in Ice)
  Auger (nt)
• ANITA (Balloon)
  EUSO (?)
• 
  LOFAR

12
Generic GRB fireball ns

• If Baryonic jet, internal shocks
• (Weak dependence on model
  parameters)
• Background free

Waxman Bahcall 97, 99 Rachen Meszaros 98
Alvarez-Muniz F. Halzen 99 Guetta et al. 04
Hooper, Alvarez-Muniz, Halzen E. Reuveni 04
13
The current limit
Achterberg et al. 07 (The IceCube collaboration)
14
n- physics astro-physics

• p decay ? nenmnt 120 (Osc.)? nenmnt
  111
• t appearance experiment
• GRBs n-g timing (10s over Hubble distance)
• LI to 11016 WEP to 1106
• EM energy loss of ms (and ps)
• nenmnt 111 (EgtE0)? 122
• GRBs E01015eV
• Combining EltE0, EgtE0 flavor measurements
• may constrain CPV SinQ13 Cosd

Waxman Bahcall 97
Waxman Bahcall 97 Amelino-Camelia,et al.98
Coleman .Glashow 99 Jacob Piran 07
Rachen Meszaros 98 Kashti Waxman 05
Blum, Nir Waxman 05
15
Outlook

• ParticleAstro-phys. Open Qs
• - gt1011GeV particles primaries, f(z), origin
  acceleration
• - Physics of relativistic sources (GRBs, AGN,
  MQ)
• Energy extraction from BH accretion
• Relativistic plasma physics
• - Conventional astrophysics (starburst ISM)
• - nm nt ? t appearance
• gn Timing ? LI to 11016 WEP to 1106
• Flavor ratios ? CPV
• New HE g, CR and n detectors
• gt103 km2 hybrid gt1019eV CR
  detectors
• 1 km3 (1Gton) 1-1000TeV n detectors
• gtgt1 km3 radio, gtgt1000TeV n detectors
• 10MeV10GeV g-ray satellite (AGILE,
  GLAST)
• gt0.1TeV (ground based) g-ray
  telescopes
• 
  (Milagro, HESS, MAGIC, VERITAS)

Identified point sources Diffuse
16
Composition clues
HiRes 2005
17
GRB proton/electron acceleration

• Electrons
• MeV gs
• tgglt1
• e- (g) spectrum
• e- (g) energy production

• Protons
• Acceleration/expansion
• Synchrotron losses
• Proton spectrum
• p energy production

Waxman 95, 04
18
The GRB GZK sphere
g

• LSS filaments
• D1Mpc, fV0.1, n10-6cm-3, T0.1keV
• eB(B2/8p)/nT0.01 (B0.01mG), lB10kpc
• Prediction

p
D
lB
Waxman 95 Miralda-Escude Waxman 96, Waxman
04
19
GRB Model Predictions
Miralda-Escude Waxman 96
20
(No Transcript)
21
AMANDA
IceCube
22
The Mediterranean effort

• ANTARES (NESTOR, NEMO) ? KM3NeT

23
M82 M81
Mark Westmoquette (University College London),
Jay Gallagher (University of Wisconsin-Madison),
Linda Smith (University College London),
WIYN//NSF, NASA/ESA
Robert Gendler
24
A lower bound Star bursts

• Star burst galaxies
• - Star Formation Rate
• 103Msun/yr gtgt 1 Msun/yr
  normal (MW)
• - Density 103/cc gtgt 1/cc
  normal
• - B 1 mG gtgt 1mG
  normal
• Most stars formed in (zgt1.5) star bursts
• High density B
• CR e-s lose all energy to synchrotron
  radiation
• CR ps lose all energy to p production

Quataert et al. 06
Loeb Waxman 06
25
Synchrotron radio
Fn
calibration
Loeb Waxman 06