High energy neutrino astronomy with Cherenkov telescopes L. Moscoso CEA/Irfu/SPP & APC – Paris...

High energy neutrino High energy neutrino astronomy with Cherenkov astronomy with Cherenkov

telescopestelescopes L. MoscosoL. Moscoso

CEA/Irfu/SPP & APC – Paris Rive GaucheCEA/Irfu/SPP & APC – Paris Rive GaucheXI ICATPP ConferenceXI ICATPP Conference

Villa Olmo, Como, Italy, 5-9/10/2009Villa Olmo, Como, Italy, 5-9/10/2009

i r f u

yalcas

i r f u

yalcas

i r f u

yalcas

5-9 Oct. 20095-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, L. Moscoso, ICATPP, Villa Olmo, Como, ItalyComo, Italy

22

The history of the sky The history of the sky surveysurvey

The light since the origins

Extension to the non visible since tens of years (Radio, IR, UV, X and gamma)

Satellites tens of GeV

Large arrays tens of TeV

Multi-wavelenth astronomy


33

Cosmic ray spectrumCosmic ray spectrum

50 J


44

The GZK effectThe GZK effectInteraction withInteraction withIR, CMBR, Radio IR, CMBR, Radio absorption of HEabsorption of HEphotons andphotons anddegradation of thedegradation of theproton energyproton energy

Region aboveRegion above100Mpc cannot be100Mpc cannot beexplored withexplored withphotons abovephotons above10TeV10TeV

Protons:Protons:UsefulUsefulaboveabove10102020eV only.eV only.

Galaxy

Local cluster


55

High energy neutrinosHigh energy neutrinos

The neutrino as an alternative solutionThe neutrino as an alternative solution

• Multi-wavelength and multi-messenger studies Multi-wavelength and multi-messenger studies

• Exploration of the most remote regions of the Exploration of the most remote regions of the UniverseUniverse– Not absorbed (weak cross section)Not absorbed (weak cross section)– Electrically neutral: not deflected by magnetic Electrically neutral: not deflected by magnetic

fieldsfields

But at least a kmBut at least a km33 is necessary! is necessary!


66

Synchrotron radiation followed by inverse Compton

The mechanismThe mechanism

HE electron LE

HE electron

HE


77

Synchrotron radiation followed by photo-production


HE electron LE

HE proton

HE °

HE

nucleonHE

HE


88

Synchrotron radiation followed by ± photo-production


LCR L L

HE electron LE

HE proton

HE

±

HE

nucleon H

E m

uon

HE

HE electron

HE

HE

e


99

Scientific issuesScientific issues

Particle physics and CosmologyParticle physics and Cosmology–DM indirect searchDM indirect search

–Neutrino oscillationsNeutrino oscillations

AstrophysicsAstrophysics–QuasarsQuasars–Gamma ray bursts (GRB)Gamma ray bursts (GRB)–MicroquasarsMicroquasars–PulsarsPulsars–SNRSNR–Topological defects + other exoticsTopological defects + other exotics


1010

Difficult detectionDifficult detection

•Very weak cross section Very weak cross section Huge detectorHuge detector

kmkm33

•Very high cosmic ray flux Very high cosmic ray flux shielded detectorshielded detector

Underground or submarineUnderground or submarine


1111

Detection techniquesDetection techniques

• HE induced muon produced in the HE induced muon produced in the surrounding medium by HE neutrinosurrounding medium by HE neutrino– Upward-going neutrinos only (2Upward-going neutrinos only (2))– Mass = RMass = RS (RS (R2.5 km we @ 1 TeV; 10 km 2.5 km we @ 1 TeV; 10 km

@10 TeV)@10 TeV)• HE muons produced inside the detector by HE muons produced inside the detector by

HE neutrino interactions (4HE neutrino interactions (4))– Requires a very large detector (IceCube or Requires a very large detector (IceCube or

KM3NeT)KM3NeT)• VHE VHE e e interaction inside the detector (4interaction inside the detector (4))

– Detection of cascadesDetection of cascades


1212

Induced muonsInduced muons

detectordetectorThe cherenkov light is detected by the PMTs

The neutrinos interactWith the surrounding

matter

The muon generates the Cherenkov light

p

c=43°

Correlation time-position direction of the muon

Precision on the position: 10cm

Precision on time: 1ns


1313

The advantagesThe advantages

• Target mass Target mass R R increasesincreases with the with the neutrino energyneutrino energy

• Interaction cross sectionInteraction cross section increasesincreases with with the neutrino energythe neutrino energy

• Detection efficiencyDetection efficiency increasesincreases with the with the muon energy and therefore with the muon energy and therefore with the neutrino energyneutrino energy

Enrichment of the high energy neutrinosEnrichment of the high energy neutrinos


1414

PhysicPhysicss background background

Atm. muons

Atm.

106

d

/d

cm

-2 s

-1 s

r-1

cos

2400 m depth, E > 1 TeV

Atmospheric showersatmospheric muons 109 events/yearAtmospheric neutrinos 3000/year


1515

The neutrino telescopesThe neutrino telescopes

NESTOR : Pylos, Greece

ANTARES La-Seyne-sur-Mer, FranceBAIKAL: Baikal lake, Siberia

DUMAND, Hawaii (cancelled 1995)

AMANDA, IceCubeSouth Pole

NEMO Catania, Italy


1616

The Mini Tower for NEMO The Mini Tower for NEMO Phase-1Phase-1

Optical modules

Floor control module

Mechanical stresses are applied only to the tensioning ropesTower Base

Module

Floor 1

Floor 2

Floor 3

Floor 4

Backbone e.o. cable

Tensioning ropes

Tensioning ropes

e.o. Jumper cableTower base - JB

Break-out


1717

Nemo Phase 1Nemo Phase 1Shore station

2.5 km e.o. Cable with double steel shield

21 km e.o. Cable with single steel shield

J BUJ

J

5 km e.o. cable

Geoseismic station SN-1 (INGV)

5 km e.o. cable

10 optical fibres standard ITU- T G-652 6 electrical conductors 4 mm2


1818

The Antares stationThe Antares station

Submarine cable

-2475m

La Seyne sur Mer

Michel Pacha institute

On shore On shore stationstation


1919

The ANTARES detectorThe ANTARES detector

vincenzo flaminio

~60 m

100 m

350 m

14.5 m

Link cable

JunctionBox

Cable toshore

2500m depth

Storey

45°


2020

Number of TriggersNumber of Triggers

CABLEREPAIR

5 lines (2007)5 lines (2007)

19.1019.1066 μ μ10 or more lines (2008)10 or more lines (2008)

65.1065.1066 μ μ

Total : 240 days = 80% of calendarTotal : 240 days = 80% of calendarSelected :167d = 70% of totalSelected :167d = 70% of total

Total : 243 days = 83% of calendarTotal : 243 days = 83% of calendarSelected :173d = 71% of totalSelected :173d = 71% of total


2121

Zenith angular distributionZenith angular distribution

neutrinos

June 2007 – Dec 2008

5+10+12 lines

341 active days

1062 upward neutrino candidates

upgoing downgoing

Good agreement with “standard” neutrino oscillationsGood agreement with “standard” neutrino oscillations:: sinsin22 2 2θθ = 1; = 1; ΔΔmm22 = 2.4 = 2.4 ·· 10 10-3-3 eV eV22


2222

Search for point-like Search for point-like sourcessources

Upper limits obtained with Upper limits obtained with 2007 data (5 lines, 140 day 2007 data (5 lines, 140 day lifetime), compared with 1 lifetime), compared with 1 year of complete detector year of complete detector (12 lines) and other (12 lines) and other experimentsexperiments

Analysis of 12-line data is Analysis of 12-line data is ongoingongoing

For further information see talks given by M. Vecchi (INFN-Roma1) & U. Fritsh (ECAP Univ. Erlangen)


2323

5 lines (2007): Depth vs. 5 lines (2007): Depth vs. IntensityIntensity

Preliminary

Preliminary

Work on reducing systematics is ongoing

2,5km6km


2424

Transients with ANTARESTransients with ANTARES

•Triggered searches (alerts from satellites: Integral, Triggered searches (alerts from satellites: Integral, Swift, Fermi) Swift, Fermi)

•Low backgrounds due to direction and time coincidencesLow backgrounds due to direction and time coincidences•Dump all L0 data in 2min window around trigger (i.e. no trigger Dump all L0 data in 2min window around trigger (i.e. no trigger losses)losses)•Special track reconstruction using known directionSpecial track reconstruction using known direction

•Neutrino multiplets in time optical follow-up (Tarot in Neutrino multiplets in time optical follow-up (Tarot in France and at La Silla)France and at La Silla)

•Full sky 24h/24 searchFull sky 24h/24 search•Sliding time window around eventsSliding time window around events•Fast online reconstruction Fast online reconstruction optical follow up to identify source optical follow up to identify source

•Gravitational waves and neutrinos (Virgo + Ligo + Gravitational waves and neutrinos (Virgo + Ligo + Antares)Antares)

•Drafting a MoU in progressDrafting a MoU in progress


2525

IceCubeIceCube

• Full project: 80 60-floors detectorFull project: 80 60-floors detector

• First analysis results on 22 stringsFirst analysis results on 22 strings

• 40 strings now installed: will allow a 40 strings now installed: will allow a 44surveysurvey

• Installation of a deep dense core (7 Installation of a deep dense core (7 strings) foreseenstrings) foreseen


2626


2727

Flux upper limits vs Flux upper limits vs declinationdeclination

2009.09.26 Chad Finley 27


2828

See T. Montaruli, ICRC09


2929

Solar wimp Solar wimp limitslimits

Phys.Rev.Lett.102:201302,2009,C. Rott, ICRC 09


3030

KM3NeTKM3NeT

+ + +…

A research facility in the Mediterranean A research facility in the Mediterranean SeaSea

A next generation neutrino telescope (at the km-scale)A next generation neutrino telescope (at the km-scale)

Cabled observatory for Earth and Marine sciencesCabled observatory for Earth and Marine sciences

38 institutes from 10 38 institutes from 10 European countriesEuropean countries


3131

Design goalsDesign goals

Substantially competitive with IceCubeSubstantially competitive with IceCube Volume > 1 kmVolume > 1 km33

Optimized for energy range 1 TeV – 1 PeVOptimized for energy range 1 TeV – 1 PeV Angular resolution < 0.1Angular resolution < 0.1oo

Zenith angle:Zenith angle: Full acceptance for neutrinos originating from Full acceptance for neutrinos originating from

directions up to at least 10° above the horizondirections up to at least 10° above the horizon For energies > 100 TeV angular acceptance For energies > 100 TeV angular acceptance

limited only by the absorption of the Earth limited only by the absorption of the Earth

See the talk given by G. De Bonis (INFN-Pisa)


3232

KM3NeT Design StudyKM3NeT Design StudyDesign study Design study funded by EU FP6 in February 2006funded by EU FP6 in February 2006

Development of a cost-effective design for a cubic km sizedDevelopment of a cost-effective design for a cubic km sizeddeep-sea infrastructure housing a neutrino telescope….deep-sea infrastructure housing a neutrino telescope….

Conceptual Design ReportConceptual Design Report released in April 2008released in April 2008

(www.km3net.org)(www.km3net.org)

Includes:Includes:

Science caseScience case

Site studiesSite studies

Design goalsDesign goals

Technical implementationTechnical implementation


3333

Km3Net Design StudyKm3Net Design Study


3434

Funded by the EU FP7 framework in March 2008

Primary objective pave the path to political and scientific convergence on the legal, governance, financial engineering and siting aspects of the infrastructure…..

Km3Net Preparatory PhaseKm3Net Preparatory Phase

Km3net timeline


3535

ConclusionsConclusions• Since many years the neutrino has been considered Since many years the neutrino has been considered

as an alternative way to observe the Universeas an alternative way to observe the Universe• It was a long way to achieves some very large It was a long way to achieves some very large

volume neutrino telescopesvolume neutrino telescopes• Now two devices are operatingNow two devices are operating• 50% of the km50% of the km33 detector at the South Pole is detector at the South Pole is

achieved and the full detector will be completed in achieved and the full detector will be completed in 20112011

• The first neutrino telescope in the Mediterranean The first neutrino telescope in the Mediterranean has been achieved too and is operatinghas been achieved too and is operating

• The study for a kmThe study for a km33 detector in the Mediterranean detector in the Mediterranean is reaching the final phase (TDR editing). The is reaching the final phase (TDR editing). The construction will probably start at the end of the construction will probably start at the end of the preparatory phase (2011)preparatory phase (2011)

Date post:	31-Dec-2015
Category:	Documents
Upload:	mercy-harmon
View:	215 times
Download:	0 times

High energy neutrino astronomy with Cherenkov telescopes L. Moscoso CEA/Irfu/SPP & APC – Paris...

Documents