theoretical bounds and current experimental limits on the diffuse neutrino flux

17.05.200417.05.2004 Reso ShanidzeReso Shanidze 11

Theoretical Bounds and Current Theoretical Bounds and Current Experimental Limits Experimental Limits

on the Diffuse Neutrino Fluxon the Diffuse Neutrino Flux

Rezo ShanidzeRezo Shanidze17/06/200417/06/2004

Seminar zu aktuellen Fragen der Seminar zu aktuellen Fragen der AstroteilchenphysikAstroteilchenphysik


LayoutLayout The sources of high energy The sources of high energy - Bottom-up models: pp(- Bottom-up models: pp() ) + X + Xeeee

- Top-down models: Decays of WIMPs - Top-down models: Decays of WIMPs (Dark matter, SUSY, Topolocical defects) (Dark matter, SUSY, Topolocical defects) Models and bounds:Models and bounds: - Atmospheric - Atmospheric , WB-bound, HE-, WB-bound, HE- from the Sun from the Sun - Fluxes from AGN, GRB, …- Fluxes from AGN, GRB, … Current experimental limitsCurrent experimental limits Future prospectsFuture prospects SummarySummary


The Sources of High EnergyThe Sources of High Energy

Weak decays: Weak decays: , K, …, charm hadrons:, K, …, charm hadrons:

(99.99 %)(99.99 %)

KK (63.4 %) (63.4 %)

e e 4.9 %, 38.8%) - K4.9 %, 38.8%) - Ke3e3 decay (K, K decay (K, Koo))

4.9 %, 27.2%) - K4.9 %, 27.2%) - K33 decay decay

c c l l ll + X , + X , l l =e, =e, ( 10 %) ( 10 %)

ee ee

cc,K, K,K, Koo)= 7.8 , 3.7 , 15.5 m, )= 7.8 , 3.7 , 15.5 m, L=L=cc =E/m=E/m cc( charm ) ~ 100 ( charm ) ~ 100 mm


Neutrino Flux from pp and pNeutrino Flux from pp and p

Learned, Mannheim, Annu.Rev.Nucl.Part.Sci. 50(2000), 679-749Learned, Mannheim, Annu.Rev.Nucl.Part.Sci. 50(2000), 679-749 The volume emissivity of produced The volume emissivity of produced

QQ(pp)(pp) = =∫∫nnt t c c NN ( (ddpppp(E(E,E)/dE,E)/dE)()(dN/dE) dEdN/dE) dE

ddpppp(E(EE) /dEE) /dEdiff. Inclusive cross-sectiondiff. Inclusive cross-section dN/dEdN/dE = = N N 00EE–s–s dEdE - - diff. energy spectra of p(CR)diff. energy spectra of p(CR) QQ

(pp)(pp)(E)(E) – – practically same energy spectrapractically same energy spectra

QQ(pp)(pp) ~ ~ QQ

(pp)(pp) (4E (4E)) ~ ~ EE-s-s

dd//dEdE= = ∫∫Q Q dr dr over spatial extent of the sourceover spatial extent of the source


Atmospheric Atmospheric flux flux

CR spectra: CR spectra: dN/dE = a EdN/dE = a E-- =2.7 (knee ~10=2.7 (knee ~101515-10-101616eV)eV) Hydrogen(0,9) He(0.08), …Hydrogen(0,9) He(0.08), …

p(He) + A p(He) + A +X +X exp(-exp(-h/h/

hh00))hh00=8.4km=8.4km Earth atmosphereEarth atmosphere: 1030 g/cm: 1030 g/cm-2-2

AA((KAKA116 (138) gm/116 (138) gm/cmcm-2-2

Int./decay(GeV): 115(850)Int./decay(GeV): 115(850)

change of change of 2.7 2.7 3.7 3.7 Secant theta effectSecant theta effect


Atmospheric Atmospheric flux flux

CR interaction and propagation:CR interaction and propagation:

MC codes: AIRES, COSMOS, MOCCA, MC codes: AIRES, COSMOS, MOCCA, HEMAS, CORSIKAHEMAS, CORSIKA

CORSICA physics models: CORSICA physics models: VENUS, QGSJET, DPMJET, VENUS, QGSJET, DPMJET, SYBILL, HDPM.SYBILL, HDPM.

Experimental Data:Experimental Data: - Underground experiments:- Underground experiments: MACRO, Frejus, L3C, …MACRO, Frejus, L3C, … - NT data:- NT data: Baikal, AMANDABaikal, AMANDA


Waxman-Bahcal Bound:Waxman-Bahcal Bound: High energy High energy from astrophysical from astrophysical sourcessources

• E.Waxman,J.Bahcall PRD, v59(1998), 023003E.Waxman,J.Bahcall PRD, v59(1998), 023003• Based on observations of Fly‘s Eye and AGASABased on observations of Fly‘s Eye and AGASA• Cosmological origin of CR above 10Cosmological origin of CR above 101919 GeV GeV ((E.Waxman, astro-ph/9508037E.Waxman, astro-ph/9508037))• Cosmological distribution of CR sources:Cosmological distribution of CR sources:• dN/dE ~ dN/dE ~ EE--22• Energy production rate ~ 5x10 Energy production rate ~ 5x10 4444 erg Mpc erg Mpc-3-3yr yr -1-1

•EE22< 2 x 10< 2 x 10-8-8 GeV/cm GeV/cm22 s sr s sr


Cosmogenic (GZK) Cosmogenic (GZK) Flux Flux Photopion production by Photopion production by

UHECR (E>10UHECR (E>101919 GeV) : GeV) : + p + p N N nn CMB : 2.7K , ~400 CMB : 2.7K , ~400 /cm /cm33, E , E

~ meV. ~ meV. IR: 1-2 IR: 1-2 cm cm33, E ~ eV. , E ~ eV.

(T.Stanev, astro-ph/0404535(T.Stanev, astro-ph/0404535))


High Energy High Energy from the Sun from the Sun Sun as a standard Sun as a standard - candle ? - candle ?

G. Ingelman, M. Thunman Phys. Rev. G. Ingelman, M. Thunman Phys. Rev.

D 54(1996), 4385D 54(1996), 4385

Calculations with LUND MC: Calculations with LUND MC: PYTHIA(v5.7) /JETSET(7.4)PYTHIA(v5.7) /JETSET(7.4)CR flux: (aECR flux: (aE--interactioninteractionWith the Sun atmosphereWith the Sun atmosphere

Rate of Rate of events integrated over events integrated over the Sun solid angle. the Sun solid angle. for NT (Efor NT (E > 100 GeV): > 100 GeV):

1 event /yr ~6x101 event /yr ~6x1044mm22


High Energy High Energy Detectors Detectors


The Baikal NTThe Baikal NT

First First telescope telescope 1.1 km depth 1.1 km depth NT-36, 96, 192NT-36, 96, 192

140 m


Results from BAIKALResults from BAIKAL

34 events of upward 34 events of upward

astro-ph/0404096astro-ph/0404096 Search for bright cascadesSearch for bright cascades EE-2-2, , ee=1:1:1=1:1:1 90% C.L. limit 90% C.L. limit EE22::

1.3x101.3x10-6-6 cm cm-2-2ss-1-1srsr-1-1GeVGeV


AMANDA AMANDA Detector Detector

AAntarcticntarctic MMuonuon AAndnd NNeutrinoeutrino DDetectoretector AArrayrray

AMANDA (ice):AMANDA (ice):1150-2350m1150-2350m

B10 (97-99): B10 (97-99): 10 strings,10 strings,302 OM302 OM

II (2000):II (2000):19 strings19 strings677 OM677 OM


AMANDA ResultsAMANDA Results ( ( flux) flux)

AMANDA B10: 1977AMANDA B10: 1977 measurement:measurement: Coverage - 2Coverage - 2 ang. ~ 2ang. ~ 2oo -2.5 -2.5oo

logE ~ 0.3-0.4logE ~ 0.3-0.4 6 < E < 1000 TeV6 < E < 1000 TeV PRL 90(2003) 2151101-1PRL 90(2003) 2151101-1

EE-2-2, , ee=1:1:1=1:1:1 EE22(E) <(E) <

8.4x108.4x10-7-7GeV /cmGeV /cm2 2 s srs sr


AMANDA ResultsAMANDA Results (cascades)(cascades)

cascades:cascades: Coverage - 4Coverage - 4 ang. ~ 30ang. ~ 30oo -40 -40oo

logE ~ 0.1-0.2logE ~ 0.1-0.2 Astro-ph/0405218 Astro-ph/0405218 197 d, MC: 920 d197 d, MC: 920 d 50 TeV<E<5 PeV50 TeV<E<5 PeV EE-2-2, , ee=1:1:1=1:1:1 EE22(E) <(E) <

8.6x108.6x10-7-7GeV /cmGeV /cm2 2 s srs sr


Acoustic Detection of UHE Acoustic Detection of UHE

Astro-ph/0406105Astro-ph/0406105 SAUND detector: ~ 250 SAUND detector: ~ 250

km2 (US Navy array) - km2 (US Navy array) - only 7 used.only 7 used.

~1600 m undersea~1600 m undersea 147 days of running 147 days of running

(2002)(2002) Calibration, analysisCalibration, analysis

-Energy, position -Energy, position

- Rates, reconstraction - Rates, reconstraction


IceCubeIceCube

1400 m

2400 m

AMANDA

South Pole

IceTop

- 80 Strings- 80 Strings- 4800 PMT - 4800 PMT - Instrumented Instrumented

volume: 1 km volume: 1 km3 3

- Installation:Installation: 2004-2010 2004-2010

~ 80.000 atm. per year

10/7/200310/7/2003 C.Spiering, VLVNT WorkshopC.Spiering, VLVNT Workshop

Search for diffuse excess of extra-terrestrial Search for diffuse excess of extra-terrestrial high energy muon neutrinos high energy muon neutrinos

bound

WB bound

DUMAND

FREJUSMACRO

Muons in Amanda-B10 (1997)

Expectation Amanda-II, 3 years

Expectation IceCube, 3 years


RICE AGASA

Amanda, Baikal2002

2004

2007

AUGER

Anita

AABN

2012

km3

EUSOAugerSalsa

GLUE


Sumary and OutlookSumary and Outlook High energy High energy astronomy: astronomy: Data from Baika(lake), AMANDA(ice)Data from Baika(lake), AMANDA(ice)

New undersea NT: ANTARES, NESTORNew undersea NT: ANTARES, NESTOR

Sensitivity to the cosmicSensitivity to the cosmic diffuse flux diffuse flux NT on km3 scale: IceCube, KM3NeTNT on km3 scale: IceCube, KM3NeT

Acoustic and other technique (RICE, ANITA, EUSO, GLUE) for UHE Acoustic and other technique (RICE, ANITA, EUSO, GLUE) for UHE ..

theoretical bounds and current experimental limits on the diffuse neutrino flux

Documents

g p g d g n p np

g e nm ne

q n dr

standard n candle

reso shanidze neutrino

reso shanidze results

cr flux

km3 decay c g