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The ANTARES Underwater Neutrino Telescope The ANTARES Underwater Neutrino Telescope

The ANTARES Underwater Neutrino Telescope - PowerPoint Presentation

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The ANTARES Underwater Neutrino Telescope - PPT Presentation

CW James ECAP University of Erlangen on behalf of the ANTARES collaboration Cosmic rays and neutrinos What produces this spectrum Standard model acceleration at relativistic astrophysical shocks ID: 429279

antares data neutrinos search data antares search neutrinos neutrino muon flux univ gev 2007 matter limits dark magnetic background

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Slide1

The ANTARES Underwater Neutrino Telescope

C.W. James,

ECAP, University of Erlangen,

on behalf of the ANTARES collaboration.Slide2

Cosmic rays and neutrinos

What produces this spectrum?

Standard model: acceleration at relativistic astrophysical shocks

R.

Shellard

, Braz. J. Phys 31 (2001) Slide3

Why

look for neutrinos?

Flux

unattenuated

over cosmological distances

Image courtesy of NRAO/AUI

Nature 432 (2004) 75

Image courtesy of NRAO/AUI

Travel in straight lines (unlike cosmic rays)

Signatures of

hadronic

processes in the high-energy universe

SNR

AGN jets and lobes

GRB

NASA/Swift/Stefan

ImmlerSlide4

Quick note: these are not Solar neutrinos!

Production via cosmic-ray (~proton) interactions with:

Much rarer than solar neutrinos – but more energetic (

GeV-PeV

: not MeV)νμ and ντ CC interactions possible

l

ow E proton

Hadronic

matter

(interstellar

gas)

Photon fields (CMB)Slide5

m

42°

interaction

Earth’s crust

(sea floor; Antarctic continent)

Cherenkov light

from

m

3D PMT

array

n

m

Main detection channel:

CC interactions

(



NC, and 

e and 

 also

).Detection Principle

n

m

p

n

m

n

m

m

p,

a

5

Optically transparent material

(water; deep ice)Slide6

Let’s build it!Slide7

7

CPPM,

Marseille

DSM/IRFU/CEA,

Saclay

APC, Paris

LPC, Clermont-Ferrand

IPHC,

Strasbourg

Univ. de H.-A.,

Mulhouse

LAM,

Marseille

COM,

Marseille

GeoAzur

Villefranche

INSU-

Division

Technique

Univ./INFN

of Bari

Univ./INFN

of

Bologna

Univ./INFN

of Catania

LNS–Catania

Univ./INFN

of Pisa

Univ./INFN

of Rome

Univ./INFN

of

Genova

IFIC, Valencia

UPV, Valencia

UPC, Barcelona

NIKHEF,

Amsterdam

Utrecht

KVI

Groningen

NIOZ

Texel

ITEP,Moscow

Moscow

State

Univ

University

of

Erlangen

Bamberg

Observatory

Univ. of

Wurzeburg

ISS,

Bucarest

8

countries

31

institutes

~150

scientists

+

engineers

LPRM,

Oujda

The ANTARES CollaborationSlide8

ANTARES: Location

40km off the coast of ToulonSlide9

V. Bertin - CPPM - ARENA'08 @ Roma

The ANTARES detector

70 m

4

50 m

Junction

BoxInterlink cables

40 km to

shore

2500m

12

lines

25

storeys

/line

3 PMTs /

storey

885 10-inch

PMTs

10-20 Mton volume

Slide10

Sample events

Maximum-likelihood fit to recorded photon hit times

http://www.pi1.physik.uni-erlangen.de/

antares

/online-display/online-display.phpSlide11

ANTARES ‘visibility’

ANTARES at 43

o

NSensitive to the Southern skyIncludes the Galactic Centre

Mkn 501

RX J1713.7-39

GX339-4

SS433

CRAB

VELA

Galactic

Centre

Visible

Invisible

ANTARES: 43

o

N

Never visible

Always visible

Increasing sensitivitySlide12

n

m

ANTARES performance: angular resolution

~50% events reconstruct to better than 0.5

o

~99% reconstruct to better than 10oEnergy reconstruction is much harder (most is not ‘seen’)Slide13

Muon

and neutrino backgrounds

Remove atmospheric

muon background with quality cutsCR neutrino background irreducible

1%

misreconstructionfrom belowfrom above

p

n

m

m

p,

a

Muon

flux at 2500m depth

Look for an excess here!Slide14

Science with ANTARES

High-energy Neutrino Astrophysics

Galactic sources: SN & SNR, micro-quasars, CR in molecular clouds

Extra-galactic sources: AGN, GRB, GZK processesSearch for new physics:Dark matter annihilation, nuclearites, monopolesEarth sciences:

Oceanography, marine biology, seismology, environment monitoring…

GeV-100

GeV

GeV-TeV

TeV-PeV

PeV-EeV

>

EeV

Oscillations

DM

SNR,

μQSO

AGN

Exotics, GZK

Marine biology

GUT???Slide15

Results!Slide16

All-sky point-source search

Sky map in equatorial coordinates

:

2007-2010 data (813 days livetime)3058 candidates after cuts: expect 14% down-going muon contamination

Most significant cluster: 2.2σ

No strong evidence for a point-source excessSlide17

Search from suspected sources

51 pre-defined ‘suspect’ sources (mostly based on gamma-ray flux and visibility)

Top 11 sources: most significant first

WR20a & b: hot, massive stars

HESS, Astronomy & Astrophysics 467 (2007) 1075Slide18

Neutrinos from gamma-ray bursts

‘Fireball’ model for GRBs:

Explains long-duration bursts

Predicts neutrinos!

Search criteria:Direction (2o from source)Time (~1 minute)Upcoming events onlyResults from 2007 data (40 GRBs): no detectionSlide19

Neutrino Oscillations

Two-

flavour

mixing approximation:Measureable: ‘Unknown’: World data: 1st minimum at , (120 m max muon

range)Expectations for 863 days’ data:

Events seen with two lines

Events seen with one line

No oscillations

Best world dataSlide20

Oscillation analysis: results

After a Chi

2

minimisation to and two systematic variables:

1st measurement of its typeAccepted July 2nd by Physics Letters BPromising for next-generation larger detectors

DataNo oscillationsBest fitCombined single and multi-line data

ANTARESK2KMINOS

Super-K68% C.L.

90% C.L.Slide21

Search for Dark Matter Annihilation in the Sun

Muon

Flux Limits 90%CL (2007-2008)

21

PRELIMINARY

Angular distance from sun

Lack of excess: => model limits

(apologies: I do not have these plots here!)

A search for an excess from the galactic

centre

is ongoingSlide22

Search for magnetic monopoles

Relativistic monopoles emit VC radiation

8550 times brighter than a

muon

Look for extremely bright events!ANTARES search spaceRelativistic ‘intermediate mass’ (< 1014 GeV)

Search performed on data from 2008:

1 event

0.13 bkgd

1.5

σ

significanceSlide23

Multi-Messenger

astronomy

Alerts

Strategy:

Increase discovery potential (different probes)

Increase significance via coincidence

Ligo

/Virgo (

grav

. waves)

Dedicated analysis chain

GW trigger

GCN (GRB)

Global burst network

GRB burst alert

ANTARES trigger and coincident analysis

TAROT (optical)

Follow-up search for SN

10s repositioningSlide24

Summary

ANTARES underwater neutrino telescope:

Largest neutrino telescope in the Northern

HemisphereProven ability to detect neutrino-induced muonsGood performance in bread & butter science: neutrino astrophysicsSensitivity optimised for the galactic

centre regionDiverse physics program:Dark matterNeutrino oscillationsExotics (magnetic monopoles, nuclearites)Entering ‘mature’ phase:

First round of results published (~1 year’s data)Analyses on 3+ years of 12-line data in progressMore results on their way!Slide25

Extra Slides

(in case of tricky questions)Slide26

Background and diffuse flux sensitivity

High energies

favour

source spectraBackground from atmospheric neutrinos: Enu-3.7Sources: order Enu-2Look for a high-energy excess!

E2

F(E)90%= 5.3×10-8 GeV cm-2 s-1 sr-1 20 TeV<E<2.5 PeVEnergy estimation: the ‘R’ parameterLimits on an E-2 fluxSlide27

Standard data pipeline

‘hit’: send PMT data to shore when one or more photons are observed

Raw data rate: too high to record

Trigger: Record data to disk if it looks `interesting’.Standard trigger requirements:Large ( ) hits OR hits on

neighbouring PMTs (600 Hz)Clusters of >=5 hitsTrigger hits must be causally connectedMany other triggers (GRB alert, monitoring info, GC etc)

Threshold: 0.3

V

photon

PMT voltage

25 ns integration

Shore triggering and data acquisitionSlide28

Candidate List Search – 90%CL Flux Limits

28

Assumes E

-2

flux for a possible signalANTARES 2007-2010 813 daysANTARES has the most stringent limits for the Southern SkySlide29

Bioluminescence: large seasonal fluctuations

Bacteria

Vertebrates

Optical Background

Potassium 40 decay: constant background

Image courtesyWolfram Alpha

Spring 2006

Spring 2007Slide30

Trigger effective area

(preliminary plot: officially updated version will be out shortly)Slide31

Data reduction for point-source search

Cut on angular-error estimate, and on fit qualitySlide32

Resolution: use the Moon’s shadow

The Moon blocks CR: expect reduction in the upcoming-event rate

884 days’

livetime

2.7 sigma defecitAgrees with Monte Carlo expectationsSlide33

Sea currents

and

a

coustic positioning

Storey 1

Storey 8Storey 14Storey 20Storey 25Radial displacement

Measure every 2 min:

Distance line bases

to 5 storeys/line

and also storey

headings and tilts

Precision

~ few

cmsSlide34

2006 – 2008: Building phase of the Detector

Junction box 2001

Main cable 2002

Line

1, 2 2006Line 3, 4, 5

01 / 2007Line 6, 7, 8, 9, 10 12 / 2007Line 11, 12 05 / 2008

~70 mSlide35

Search for Neutrinos from Fermi Bubbles

For 100%

hadronic

models

:F ~1/2.5 F (Vissani)E2dF/dE=1.2*10-7 GeV cm-2s-1sr -1E cutoff

protons: 1PeV-10 PeV (Croker&Aharonian)

E cutoff neutrinos = 1/20 cutoff protons

Good

visibility

for ANTARES

Background

estimated

from

average

of three ‘OFF’ regions (time shifted in local coordinates)

galactic

coords

d

etector

coordsSlide36

Dark

Matter

Simulation

M

A

I

N

A

N

N

I

H

I

L

A

T

ION

C

H

A

N

NEL

S

36

M

WIMP

= 350

GeV

τ

leptons

regeneration

in the Sun

mUED

particular

case…Slide37

Dark matter – detector performance

ANTARES effective area to

muon

neutrinos incident on EarthMost neutrinos do not produce detectable muonsMost muons are very low in energySlide38

Magnetic Monopoles: data reduction

Magnetic monopoles…

Theoretical prediction (

quantisation of charge, guage theories…)Have not been observed (various limits exist)Have a magnetic charge g: will emit Vavilov-Cherenkov radiation

VC radiation: 8550 times brighter than that of a muon with similar velocityAcceleration in cosmic magnetic fieldsSlide39

Search for Dark Matter Annihilation in the Sun

Muon

Flux Limits 90%CL (2007-2008)

39

PRELIMINARY

Angular distance from sun

PRELIMINARY