ANTARES Status Report - INFN Sezione di Roma

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ANTARES Status Report - INFN Sezione di Roma

Antonio Capone - INFN - Roma

on behalf of the

ANTARES Collaboration

http://antares.in2p3.fr/

ANTARES Status Report

-Scientific Aims

-R&D and Site properties studies

-The ANTARES detector design

-Deployment & operation of a demonstrator

-Construction plans

Neutrinos and Subterranean Science - NeSS02

Washington, DC - USA - 19÷21 September 2002

20/09/02 Antonio Capone - Neutrinos and Subterranean Science - Washington, DC - USA 1


ANTARES Collaboration

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ANTARES scientific program

H i g h E n e r g y

M e d i u m E n e r g y

L o w E n e r g y

> 1 0 T e V

< 1 T e V

< 1 0 0 G e V

ν f

r o m ( e x t r a - )

g a l a c t i c s o u r c e s

N e u t r a l i n o s e a r c h :

χ χ → ν + X

A t m o s p h e r i c ν o s c i l l a t i o n s

O b s e r v a t i o n o f fi r s t

S N r e m n a n t s ,

i n t h e c e n t e r o f E a r t h ,

S u n a n d i n g a l a c t i c

o s c i l l a t i o n m i n i m u m

A G N , G R B , . . .

c e n t e r

GRB cannonballs,

micro-quasar

20/09/02 Antonio Capone - Neutrinos and Subterranean Science - Washington, DC - USA 3


DETECTION PRINCIPLE

p

µ

Detector

ν

light cone detected by

array of PMTs

Muons produce Cerenkov light

µ

ν

µ

High energy ν interact in the medium

surrounding the detector

θνµ ≈ 0.7 o / E 0.6 (TeV)

20/09/02 Antonio Capone - Neutrinos and Subterranean Science - Washington, DC - USA 4


The ANTARES Site

• 2400m sea depth

• short path to the shore (40 Km)

42°50 N, 6°10 E

2400 m depth

• infrastructures (IFREMER,..)

•3.5 π sr coverage of the sky

•0.5 π sr overlap with Amanda

•Galactic center surveyed

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ANTARES site properties evaluation

Deep sea currents

Optical noise

Current speed [cm/sec]

Time [days]

Water optical properties

Arrival time distribution

from a point-like

source (pulsed LED)

Current speed [cm/sec]

Water

transparency:

Blue light (470nm)

λabs

λeff scatt

Λe f f s c a t t

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=

~ 5 5 m

~ 3 0 0 m

UV light (370 nm)

λabs

λeff scatt

Sea current

~5 cm/s

~ 2 5 m

~ 1 2 0 m

λ scatt

1 - < c o s

θ >

15

10

0

Oct 1996 Apr 1998

5

Counting rate [kHz]

Events per bin

From Decay of 40 K

and bioluminescence

Mean ~60 kHz for 10” PM

10 2 10 3

Counting rate distribution [kHz]

time [s]

Optical noise

→ 5% dead time


Biofouling and transparency of Glass Spheres

3% / 2

< 1,5% per year

(then saturates)

“Sedimentation and Fouling

of Optical Surfaces at the

ANTARES Site” June, 2002

Submitted to Astroparticle

Physics. - astro-ph/0206454 -

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ANTARES detector

0.1 km 2 effective area, 10 strings, 900 PMTs

Deployment of first two strings in 2003

shore station

time calibration

LED beacon

~300 m

float

~60 m

electronic

container

2400 m

electro-optic

submarine cable

~ 40 Km

hydrophone

Optical

modules

~100 m

Acoustic beacon

anchor

Junction box

An 11 th string dedicated to environmental properties measurements will implement the optical detector

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The first ANTARES storey

fully integrated at CPPM

August ‘02: storeys assembly

goes on for the construction

of the first ANTARES string

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A string dedicated to environmental

parameter measurements, to calibrations

and controls of the detector

Mechanical

Cable

ADCP

Sound

Velocimeter

Electro Mechanical Cable

3 fibers for DAQ

Acoustic Positioning

Modules (receivers)

100m

Optical

Beacon

CTD

CSTAR

Electro Mechanical Cable

2 fibers for DAQ, 1 for clock

100m

JB

2 fibers for DAQ

1 for clock

LASER

Beacon

Acoustic

Positioning

Modules

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ANTARES demonstrator line

•Deployed at 1200 m depth on Dec. 1999

•Retrieved July 2000

•PMTs, CTDs, tilt-meter, positioning system

•Linked to shore by electro-optical cable

• 50.000 events with

7-fold coincidences

•1350 events/day

reconstructed

•Data – MC agree

PMT Positioning

Accuracy

(σ) ≤ 6 cm

7

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ANTARES 0,1 km 2 expected performances:

energy and angular resolutions

Energy resolution

For E >10 TeV σ E /E ≈ 2

Dominated by

interaction

For E < 100 GeV energy

estimation via muon range

measurement.

Dominated by

reconstruction

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ANTARES 0,1 km 2 expected performances:

Effective areas for the 10 strings detector.

- no quality cuts

- θ ν,µ rec < 1º

geometrical

instrum. surface

Search for known sources (i.e. GRB),

almost background free, quality

reconstr. cuts replaced by angular cuts

after strict

reconstruction

quality cuts

Isotropically simulated events. Search for

point like sources (not necessarily

associated to any known object). Strict

quality cuts applied to the reconstruction.

20/09/02 Antonio Capone - Neutrinos and Subterranean Science - Washington, DC - USA 13


ANTARES 0,1 km 2 expected rates

Neutrinos from point-like sources:

an example

from GALACTIC MICRO QUASARS*

expected per year in a 1º cone:

GX339-4 → 6.5 events

SS433 → 4.3 events

Integrated rates (events/year for E>E µ ) of

predicted (solid lines) and reconstructed

(dashed lines) vs. simulated and reconstr. E µ

Flux

Atm. ν (Bartol)

ν W-B 1999

ν M.P.R. 2000

events/yr

E reco >10 (100) TeV

44 (1.3)

5 (1.7)

106 (20)

events/yr

E>10 (100) TeV

12 (0.15)

5 (1.4)

102 (11)

with 0.3 backg. events

*C. Di Stefano et al. astro-ph/0202200 (2002)

Neutrino associated to GRB

~0.5 events/year for E ν >10 TeV

Adding all possible sources

Angular cut = 1.5°

Expected background ~ 5 x 10 -3 y -1

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ANTARES 0,1 km 2 sensitivity to WIMPS

S e a r c h f o r N e u t r a l i n o s i g n a l f r o m t h e

χ χ → W

W →

S U N

ν + X

E

ν > 5 G e V

S e n s i t i v i t y ( 9 0 % C . L . ) f o r A N T A R E S

3 y r

σ Si

lim

= limit on the spin-independent

cross-section that can be set by EdelweissII

detector after ~3yr data taking

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Planning

Autumn 2002

Deployment of a prototype string made by 5 storeys (a “sector” of

the ANTARES string) and of the “instrumentation string”.

December 2002

Connection to the “junction box” and beginning of data taking.

June 2003

Deployment, and operation, of the first two (full size) ANTARES

strings

December 2004

The 10 strings and the “instrumentation line” deployed and in data

taking

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Summary

ANTARES site selection

Good knowledge of environmental data: deep sea currents, fouling,

light transmission in water, optical background, deep sea bottom. Data

collected since 1996)

ANTARES demonstrator

Deployed (Nov. 1999), operated and retrieved successfully (June 2000).

Good control of detector position.

Test of down going muons reconstruction: data and MC agree

Construction of the 0.1 KM 2

The main electro-optical cable (~40 km) deployed Oct. 2001: O.K.

Mechanical test of a prototype string deployment Nov. 2001: O.K.

Electronics, DAQ well defined continuously in progress

Industrial production of the 900 Optical Modules started April 2002

“String sector” and part of instrumentation string deployed by Autumn 2002

10 string detector completed by 2004

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