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High energy neutrino astronomy: Challenges & Prospects. Eli Waxman Weizmann Institute, ISRAEL. High energy n ’ s: A new window. MeV n detectors: Solar & SN1987A n ’ s Stellar physics (Sun ’ s core, SNe core collapse) n physics >0.1 TeV n detectors: - PowerPoint PPT Presentation
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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)?