Download - The case for High energy neutrino astronomy
The case forHigh energy neutrino astronomy
Eli WaxmanWeizmann Institute, ISRAEL
High energy’s: A new windowMeV 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
The 1020eV challengeR
B eBRBRRBR
ccV p c
vcv
v/1~1 2
cec
BRL p22
2
v/21v
84
v
v
sun122
20,
2
L10/v
pcL
2R
tRF=R/c)
l =R/
2 2
[Waxman 95, 04, Norman et al. 95]
• AGN (Steady): ~ 101 L>1014 LSun few brightest ~1/100 Gpc3 d >> 100Mpc ?? AGN flares
• GRB (transient): ~ 102.5 L>1017 LSun L~ 1018LSun
[Farrar & Gruzinov 08]
[Blandford 76; Lovelace 76]
[Waxman 95, Vietri 95, Milgrom & Usov 95]
• 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
Energy extraction
Jet acceleration
Jet content (kinetic/Poynting)
Particle acceleration
Radiation mechanisms
Clues: CR phenomenology
Cosmic-ray E [GeV]
log [dJ/dE]
1 106 1010
E-2.7
E-3
Heavy Nuclei
Protons
Flattening,Near isotropy,Heavy light (?)
Galactic heavy(“hypernovae” Z~10 to 1019eV)
X-Galactic, ?Light
[Blandford & Eichler, Phys. Rep. 87; Axford, ApJS 94; Nagano & Watson, Rev. Mod. Phys. 00]
%23.
sysEE
Constraints: Flux & Spectrum
[Waxman 1995;
Bahcall & Waxman 03]
[Kashti & Waxman 08]
Esys/E~20%
3344
5.192
)1()(,0,yrerg/Mpc10)3.0(7.0
)(0,eV10
zzfx
zfEzdEndE x
Particle acc.; SFR , AGN, GRB
1)(,eV)10cutoff(7.0,yrerg/Mpc103.1 18344
zfx
[Berezinsky et al. 08]
Clues: AnisotropyGalaxy 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 Few fold increase >99% 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]
>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)?
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
srscmGeV10
zzf
ddj
[Waxman & Bahcall 99; Bahcall & Waxman 01]
srscmGeV10)eV10( 2
8192
ddj
AGN models??
BBR05
Experiments• Optical Cerenkov - South Pole Amanda: 660 OM, 0.05 km3
IceCube: +660/yr OM (05/06, 06/07) 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
Generic GRB fireball ’s• If: Baryonic jet, internal shocks
(Weak dependence on model parameters)
• 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
TeV1005.2TeV1007.1
EE
The current limit[Achterberg et al. 07 (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…) Energy extraction from BH accretion Relativistic plasma physics - “Conventional” astrophysics (starburst ISM) - 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)
Identified point so
urces
Diffuse
Composition cluesHiRes 2005
GRB proton/electron accelerationElectrons
• MeV ’s:
• <1:
• e- () spectrum:
• e- ()energy production
erg/s1052L
5.210
2/ eee ddn
yrMpcerg10erg10
yrGpc5.0
3445.53
32
e
ee dnd
[Waxman 95, 04]
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
yrMpcerg10)3.0(6.0 3
442 p
pp dnd
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
fDdcd
fDd
2220
3
2
2
2052
2/120
2/10
10~)eV10(
yrGpc/5.0~
eV10/Mpc100/yr10~~~
eV10/Mpc100/3.0
GRB Model Predictions
[Miralda-Escude & Waxman 96]
AMANDA &IceCube
The Mediterranean effort• ANTARES (NESTOR, NEMO) KM3NeT
Mark Westmoquette (University College London), Jay Gallagher (University of Wisconsin-Madison), Linda Smith (University College London), WIYN//NSF, NASA/ESA
Robert Gendler
M82 M81
A lower bound: Star bursts• 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]
eepnpp ,
Synchrotron radio calibration
[Loeb & Waxman 06]