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Neutrino AstronomyNeutrino AstronomyStatus and PerspectivesStatus and Perspectives

Christian SpieringChristian Spiering

DESYDESY

Gamma-2008, Heidelberg 2008Gamma-2008, Heidelberg 2008

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The unified spectrum of neutrinosThe unified spectrum of neutrinos

under-ground

optical:- deep water- deep ice

- air showers- radio- acoustics

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In this talk: In this talk: only optical underwater/ice only optical underwater/ice

detection @ TeV/PeVdetection @ TeV/PeV

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Underwater/Ice: optical telescopesUnderwater/Ice: optical telescopes

muon tracks cascades

angle water < 0.3° water 3-6° (at 10 TeV)

ice 0.5-1° ice ~25° (at 10 TeV)

energy 0.3 in log E 30% in E (at 10 TeV)

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The Baikal Neutrino TelescopeThe Baikal Neutrino Telescope

NT200

3600 m

1366

m

140 m NT200+- upgrade 2005/06- 4 times better sensitivity than NT200 for PeV cascades- basic cell for km3 scale detector

construction 1993-1998

192 optical modules at 8 strings

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677 optical modulesat 19 strings

AMANDA

construction 1996-2000

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ANTARESANTARES

Installation:Junct.Box - Dec 2002Line 1 - March 2006Line 5-10 - Dec 2007Line 11-12 - May 2008

900 optical modules

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5 years Baikal NT200

396 candidates

Preliminary

Atmospheric NeutrinosAtmospheric Neutrinos

down

up

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Atmospheric NeutrinosAtmospheric Neutrinos

4 years Amanda

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Multi string condition

Atmospheric NeutrinosAtmospheric Neutrinos

Preliminary

5-string Antares 2007

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Amanda: energy spectrum of Amanda: energy spectrum of atmospheric neutrinos (4-year data)atmospheric neutrinos (4-year data)

Spectrum upto >100 TeV !

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NESTOR NESTOR & NEMO& NEMO

4100m

2400m

3400m

ANTARES

NEMO NESTOR

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IceCubeIceCube Baikal-GVDBaikal-GVD KM3NeTKM3NeT

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IceTop

IceCube

Air shower detector

80 pairs of ice

Cherenkov tanks

Threshold ~ 300 TeV

Goal of 80 strings of 60

optical modules each

17 m between modules

125 m string separation

2004-2005 : 1 string

2005-2006: 8 strings

AMANDA-II

19 strings

677 modules

2006-2007:

13 strings deployed

Current configuration- 22 strings- 52 surface tanks

Completion by 2011.

1450m

2450m

2007-2008: 18 strings

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IceCube 50% installed IceCube 50% installed and and ..taking datataking data

Will have 1 km³Will have 1 km³year by 2009year by 2009

Entering cubic kilometer eraEntering cubic kilometer era

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Amanda as a low-energy subdetector Amanda as a low-energy subdetector of IceCube of IceCube

MC for livetime: IC22 281 days, 142 days together with AMANDA

See poster ofGross & Bazo Alba

only IC22

IC22 +Amanda

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DeepCore: a new low energy DeepCore: a new low energy subdetector for IceCubesubdetector for IceCube

6 strings each with 60 PM, 6 strings each with 60 PM, spaced by ~10 mspaced by ~10 m

better veto from topbetter veto from top located in best ice located in best ice

(below 2100 m (below 2100 m exceptionally clear!)exceptionally clear!)

uses IceCube technologyuses IceCube technology considerably better considerably better

performance at low energyperformance at low energy

Can look upward !!Can look upward !!

AMANDA

DeepCore

See poster of O. Scholz

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Gigaton Volume Detector, Gigaton Volume Detector, GVDGVD

624m

280m

70m

70m120m

208m

Sparse instrumentation:

91 – 100 strings with 12 – 16 OMs (1300 – 1700 OMs)

Effective volume for 100 TeV cascades: ~ 0.5 -1.0 km³

Muon threshold 10 – 30 TeV

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Presentlyunder test:

GVD prototype

string

Gigaton Volume Detector, GVDGigaton Volume Detector, GVD

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KM3NeTKM3NeT

European priority project of HE European priority project of HE astronomy astronomy – ESFRI listESFRI list– FP6 design studyFP6 design study– recently started a FP7 Preparatory Phaserecently started a FP7 Preparatory Phase– One of the priority entries in ASTRONET roadmap.One of the priority entries in ASTRONET roadmap.

Resources for a Mediterranean detector Resources for a Mediterranean detector should be pooled in a single optimized should be pooled in a single optimized design for a large research infrastructuredesign for a large research infrastructure . .

The sensitivity of KM3NeT must The sensitivity of KM3NeT must substantially exceed that of all existing substantially exceed that of all existing neutrino detectors including IceCube.neutrino detectors including IceCube. This has This has to be achieved within the present budget estimateto be achieved within the present budget estimate..

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Time schedule

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a b

c d

Configuration ?Site ?Technology ?

Challenge for the next 1.5 years (TDR) ! Challenge for the next 1.5 years (TDR) !

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Effective Effective area @ 100 TeV: area @ 100 TeV: ~ 4 m² ~ 4 m² Amanda/Antares classAmanda/Antares class ~100 m² ~100 m² km² classkm² class

Point source sensitivity (5Point source sensitivity (5):): AMANDA, ANTARES:AMANDA, ANTARES: ~ 3~ 31010-10-10 / (cm² s) above 1 / (cm² s) above 1

TeVTeV IceCubeIceCube, KM3NeT , KM3NeT < 10 < 10-11-11 / (cm² s) above 1 TeV / (cm² s) above 1 TeV

Angular resolution:Angular resolution: ~ 4° Baikal NT200~ 4° Baikal NT200 ~ 2° Amanda~ 2° Amanda < 1° IceCube< 1° IceCube ~ 0.3° Antares (KM3NeT)~ 0.3° Antares (KM3NeT)

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High energy astrophysical sourcesHigh energy astrophysical sources (Supernova burst)(Supernova burst)

Nothing on particle physics, dark Nothing on particle physics, dark matter, charged cosmic rays, …matter, charged cosmic rays, …

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Skymap AMANDA and BaikalSkymap AMANDA and Baikal

galactic coordinates

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δ=90º

24h 0h

3 yr max significance3.73σ → 1.5σ

5 yr max significance3.74σ → 2.8σ

Max Significance3.38σ

7 years Amanda (6595 events)7 years Amanda (6595 events)

Preliminary

No significant excess

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Amanda Flux Limits for Amanda Flux Limits for EE--22 Point sources Point sources

Preliminary

Energy Range (90%): 1 TeV – 3 PeV

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Stacking of AGN (Amanda)Stacking of AGN (Amanda)

Assumes „identical“ objects with a given class

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IceCube 22 strings, 2007IceCube 22 strings, 2007

Equatorial sky map (scrambled in RA!) for 281 days of IC22, from a binned analysis optimized for E-2 – E-3.

Note: there are 2 analyses, 1 binned, 1 unbinned. Limits/fluxes will be published for the more sensitive one. Unblinding soon.

See poster of Bazo Alba & Gross

Preliminary

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Flux limits for point sourcesFlux limits for point sources

Preliminary

20122012

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Signal predictions: galactic sourcesSignal predictions: galactic sources

Predictions on firmer ground than for extragalactic Predictions on firmer ground than for extragalactic sourcessources– Shell-type SNRShell-type SNR– Pulsar Wind NebulaPulsar Wind Nebula– Micro-quasarsMicro-quasars– Compact Binary SystemsCompact Binary Systems

Many papers in the last 2 years, e.g.:Many papers in the last 2 years, e.g.:– Vissani 2006Vissani 2006– DiStefano 2006DiStefano 2006– Lipari 2006Lipari 2006– Kappes, Hinton, Stegmann, Aharonian 2007Kappes, Hinton, Stegmann, Aharonian 2007– Gabici, Aharonian 2007Gabici, Aharonian 2007– Torres, Halzen 2007Torres, Halzen 2007– Halzen, Kappes, Murchadha 2008Halzen, Kappes, Murchadha 2008– Taylor et al., 2008Taylor et al., 2008

Conclusion: Conclusion: Cubic kilometer detectors will likely Cubic kilometer detectors will likely just scrape the detection regionjust scrape the detection region

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from molecular Clouds: smoking gun for from molecular Clouds: smoking gun for hadronic acceleration ?hadronic acceleration ?

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Expected Expected flux from galactic point sources, flux from galactic point sources, example: RXJ 1713-3946example: RXJ 1713-3946

Assume 0 and calculate related ±

C. Stegmann ICRC 2007

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MGRO J2019+37

MGRO J2032+37

MGRO J2031+41 MGRO J1852+01

MGRO J1908+06

MGRO J2043+36

Milagro, Galactic plane

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MGRO J1908+06: the first PevatronMGRO J1908+06: the first Pevatron ? ?

Neutrino spectra for all sourcesSpectra for MGRO J1908+06

Assumed Assumed EE-2-2 with Milagro normalization with Milagro normalization

(MGRO J1908+06 index= 2.1)(MGRO J1908+06 index= 2.1)

spectrum cutoff @ 300 TeVspectrum cutoff @ 300 TeVHalzen, Kappes, O’Murchadha: arXiv:0803.0314

neutrino flux

gamma flux

MGRO J1852+01MGRO J2019+37MGRO J1908+06MGRO J2031+41MGRO J2043+36MGRO J2032+37

1 10Ethresh (TeV)

1000100 1 10Ethresh (TeV)

100010010-13

10-12

10-11

10-10

E2

flu

x (T

eV s

-1 c

m-2)

E2

flu

x (T

eV s

-1 c

m-2)

10-13

10-12

10-11

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Simulated Neutrino Skymaps IC80 (5 years)Simulated Neutrino Skymaps IC80 (5 years)

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Stacking all 6 Milagro sources, 5 yearsStacking all 6 Milagro sources, 5 years

p-value close to 10-4 after 5

years

Optimal threshold @ 30 TeV

(determined by loss of signal

events)

Halzen, Kappes, O’Murchadha: arXiv:0803.0314

Assumption: cut-off at 300 TeV

p-value close to 10-4 after 5 years

Optimal threshold @ 30 TeV (determined by loss of signal events)

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Stacking all 6 Milagro sources, 5 yearsStacking all 6 Milagro sources, 5 years

Halzen, Kappes, O’Murchadha: arXiv:0803.0314

Assumption: cut-off at 800 TeV

5

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Conclusions for galactic sourcesConclusions for galactic sources

Optimum threshold for typical analyses Optimum threshold for typical analyses with a km³ detector 5-30 TeVwith a km³ detector 5-30 TeV

Desirable sensitivity > 5 Desirable sensitivity > 5 IceCube IceCube

But: don‘t forget SN shells in first But: don‘t forget SN shells in first months after explosion !months after explosion !

Always to the rescue: hidden sources Always to the rescue: hidden sources

(but they also eventually should be visible at low (but they also eventually should be visible at low photon energies !)photon energies !)

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Search forSearch fordiffuse diffuse extraterrestrialextraterrestrialfluxflux

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Toy model

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exclusion limit for this model

Toy model

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MPR bound, neutrons escape (CR bound)

Factor 4 below MPR bound for sources transparent to neutrons

MPR and WB boundMPR and WB bound

Waxman-Bahcall

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Limit on diffuse extraterrestrial fluxesLimit on diffuse extraterrestrial fluxes

AMANDA HE analysis

Baikal

IceCube muons, 1 year

Icecube, muons & cascades4 years

GRB (WB)

2003

2006

2009

2013

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A. Silvestri, thesis, 2007

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2/3int

~po

sourcediffuses C

LKN

Number of observable point sources

Limit on diffuse flux

Flux sensitivityfor point sources

Typical sourceluminosity

Isotropically distributed sources Similar luminosity for all sources dN/dE ~ E-2 for all sources and cut-off only at >100 Tev Euclidian Universe, uniform source density

Assumptions:

Connecting diffuse and point source fluxesConnecting diffuse and point source fluxes

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2/3int

~po

sourcediffuses C

LKN

Number of observable point sources

Limit on diffuse flux

Flux sensitivityfor point sources

Typical sourceluminosity

Connecting diffuse and point source fluxesConnecting diffuse and point source fluxes

Amanda present

Amanda

Ns < 0.01- 0.1

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2/3int

~po

sourcediffuses C

LKN

Number of observable point sources

Limit on diffuse flux

Flux sensitivityfor point sources

Typical sourceluminosity

Connecting diffuse and point source fluxesConnecting diffuse and point source fluxes

Amanda present

IceCube

Ns < 1- 10

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Simple arguments suggest that 1 km³ has a Simple arguments suggest that 1 km³ has a fair – but not too large! – discovery chance fair – but not too large! – discovery chance for single sources.for single sources.

Increase point source sensitivityIncrease point source sensitivity– by area > 1 km²by area > 1 km²– by better pointingby better pointing– by reducing the BG of atmospheric neutrinosby reducing the BG of atmospheric neutrinos

Not excluded that first a Not excluded that first a diffuse excessdiffuse excess will will be discovered.be discovered.

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Multi-Messenger AnalysesMulti-Messenger Analyses

Steady sourcesSteady sources– Reducing trial factors by source selection Reducing trial factors by source selection

based on X-ray/gamma information based on X-ray/gamma information Transient sourcesTransient sources

– Being triggered by GRB satellite data Being triggered by GRB satellite data – Optical follow-up of neutrinos doubletsOptical follow-up of neutrinos doublets– Target of Opportunity programs Target of Opportunity programs

(like AMANDA/MAGIC) (like AMANDA/MAGIC)– Compile continuous gamma time series Compile continuous gamma time series – Identify flare states Identify flare states – SN burst trigger to optical astronomersSN burst trigger to optical astronomers

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Limit on diffuse extraterrestrial fluxesLimit on diffuse extraterrestrial fluxes

AMANDA HE analysis

Baikal

IceCube muons, 1 year

Icecube, muons & cascades4 years

GRB (WB)

2003

2006

2009

2013

GRB:multi-messenger

to the rescue

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AMANDA limit from 408 bursts

1997-2003

Waxman-BahcallGRB prediction

10-10

10-7

10-8

10-9

104 106105 107 108

neutrino energy E (GeV)

E2

flu

x (G

eVc

m-2s

-1s

r-1)

Check for coincidences with BATSE, IPN, SWIFT

close to WB within < factor 2 with IceCube: test WB within a few months

Coincidences with GRBCoincidences with GRB

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Optical follow-up for GRB/SNOptical follow-up for GRB/SN

Ando & Beacom Ando & Beacom PRL2005PRL2005

Sensitivity doubled by optical follow-up!

Principle: turn robotic opticaltelescopes to directions of doubletsin nu-telescopes.

M.Kowalski, A. Mohr, astro-ph/0701618

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Flares of AGN: ES 1959+650 ?Flares of AGN: ES 1959+650 ?

Year2000 2001 2002 2003

May June July

Flux ofTeV photons

(arb. units)

0

1

2

3

WHIPPL

E

Arrival time of neutrinos from the direction of the AGN ES1959+650

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Neutrino Target of Opportunity (NToO)*Neutrino Target of Opportunity (NToO)*

H.E.S.S.CANGAROO

small overlap in the visible sky

MAGICNToO – follow-up neutrino alerts plus long term observ.

VERITASLong-term gamma-ray observations used for light-curves studies

27th September to 27th November 2006Five alerts sent

Result: 3 observationsNo coincidence …

* M. Ackermann, E. Bernardini

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Understanding transient gamma signalsUnderstanding transient gamma signals

Compiling gamma time series, e.g.M. Tluczykont et al., JoP 60 (2007) 318

Defining flare periodse.g. E.Resconi et al., JoP 60 (2007) 223

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Supernova in IceCubeSupernova in IceCube

Signal for SN in GC

Detection byenhancednoise rates

0 5 10 sec

Count rates

Dark noise inIceCubeOptical Modulesis only ~ 320 Hz !

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Supernova in IceCubeSupernova in IceCube

5 signal for SN of 1987A strength

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tremendous technological progress over last tremendous technological progress over last decadedecade

no positive detection yet, but already testing no positive detection yet, but already testing (optimistic) bounds(optimistic) bounds

IceCube reaches 1 kmIceCube reaches 1 km33 year by early 2009 year by early 2009

entering region with fair discovery potential. entering region with fair discovery potential. Most interesting period 2009-2013 !Most interesting period 2009-2013 !

KM3NeT should be substantially more KM3NeT should be substantially more sensitive than IceCubesensitive than IceCube

IceCube is ready for the next SupernovaIceCube is ready for the next Supernova

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Discovery potential for neutrino point Discovery potential for neutrino point sourcessources

2006 2008 2010 2012 2014 2016 year

Steady sourcesIceCube

Transient sources

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Discovery potential neutrino point Discovery potential neutrino point sourcessources

2006 2008 2010 2012 2014 2016 year

Steady sources

Steady sources

IceCube

KM3NeT / GVD (assume substantially better point source sensitivity than IceCube)

Transient sources

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