Km3 neutrino detector workshop January 23 20.30-22.00 KM3 - - PowerPoint PPT Presentation

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Km3 neutrino detector workshop January 23 20.30-22.00 KM3 - - PowerPoint PPT Presentation

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1/60 Km3 neutrino detector workshop January 23 20.30-22.00 KM3 Cerenkov neutrino detector, the Cerenkov medium properties: ice, sea water, lake water. Their effect on Km3 neutrino detector workshop detector structure, effective area and

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Km3 neutrino detector workshop

January 23 20.30-22.00 KM3 Cerenkov neutrino detector, the Cerenkov medium properties: ice, sea water, lake water. Their effect on detector structure, effective area and angular resolution. Pascal Vernin & Chantal Racca – properties of the ANTARES site Giorgio Riccobene – evaluation of optical and oceanological properties for a Km3 detector close to Capo Passero (Sicily) Zhan Arys Dzhilkibaev - properties of Lake Baikal water Christian Spiering – properties of South Pole ice around AMANDA January 24 17.00-19.30 KM3 neutrino detectors – Cerenkov, radio, acoustic detections; effective area, energy range, energy and angular resolution, discovery capabilities. Present status and future techniques Luciano Moscoso – Cerenkov detection Christian Spiering – acoustic and radio detection Gianni Pavan (Centro Interdisciplinare di Bioacustica, Univ. Di Pavia)– The km3 neutrino detector: an example of deep underwater multidisciplinary laboratory Sandra Zavatarelli (INFN, Genova, Italy) – Present and future photon detectors for km3 neutrino telescope. Riccardo Papaleo (Lab. Naz. Del Sud, INFN, Catania, Italy)– study for a Km3 Cerenkov detector in Capo Passero site: mechanics, deployment, data transmission January 30 17.00-19.00 Gert-Jan Nooren – electronic equipment required for a Km3 neutrino detector Vincent Bertin – slow control for a Km3 neutrino detector Domenico Lo Presti (University of Catania, Italy) - development of a new electronics for the km3 neutrino detector.

Km3 neutrino detector workshop

Antonio Capone - February 1st 2002 - Les Houches - Summary of “Km3 neutrino detector workshop”

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ANTARES: site evaluation results (1)

  • P. Vernin

deep Sea Currents Fouling on optical modules

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ANTARES: site evaluation results (2)

  • P. Vernin
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ANTARES: site evaluation results (3)

Optical background by β- from 40K decay and by bioluminescent organism (1)

  • C. Racca
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ANTARES: site evaluation results (4)

Optical background by β- from 40K decay and by bioluminescent organism (2)

  • C. Racca
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  • KM2 36°10’ N 16°19’E, depth 3350m

(1: Jan ‘99)

  • KM3 36°30’ N 15°50’E, depth 3345m

(1: Feb ‘99, 1: Aug’99, 2: Dec ‘99)

  • KM4 36°19’N, 16°04’E, depth 3341m

(2: Dec ‘99, 2: March ’00, contiuing ) 100 km KM2

NEMO - Capo Passero site

KM3 KM4

  • G. Riccobene
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North 10 cm/sec

Lat:36°30’N Long:15°50’E Depth: 3350m current meter moored @ -3325m Average current intensity: 3.6 cm/sec RMS: 2.5 cm/sec Average angle: 8° NW Preliminary analysis

Tidal Effect Filtered out Raw Data

North 10 cm/sec

NEMO - Deep Sea Current Measurements (August 1998 - running)

  • G. Riccobene
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days

July 1st

Northern Ionian Sea(1997 data)

Flux (mg m-2 day-1)

Sediment rate measurements

  • G. Riccobene
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NEMO site bioluminescent bacteria

Bioluminescent bacteria on SWC

  • G. Riccobene
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NEMO- Seasonal dependences of La and Lc

Attenuation length [m]

  • G. Riccobene
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NEMO-BAIKAL joint measurement Absorption and Scattering in Lake Baikal (1000 m)

  • G. Riccobene
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NEMO-BAIKAL joint measurement Attenuation in Lake Baikal (1000 m)

  • G. Riccobene
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Summary of Labs and Latt meas. in NEMO & Baikal sites

  • G. Riccobene
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NEMO Measurement of scattering angle distribution in deep sea water: DEWAS Preliminary

  • G. Riccobene
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BAIKAL parameters

BAIKAL parameters

  • Z. Dzhilkibaev
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λscatt eff

10m 20m

AMANDA: effective scattering coefficient

  • C. Spiering
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Amanda scattering & absorption

100m 50m 20m 200m

length

  • C. Spiering
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Parameters for Cerenkov detectors

Optical parameters: (for blue light )

λabs λscatt

noise fouling

  • n optical

modules ~ 90m in ice, 50 ÷ 80m in sea water ~ 20m in lake water (Baikal) ~ 0.2 ÷ 25m in ice, > 100m in sea water ~ 50m in lake water (Baikal)

  • negligible on ice
  • relevant on sea water (40kHz minimum on 8”PMT in

ANTARES site)

  • absent in ice
  • relevant on up-looking surfaces in sea water (ANTARES)
  • negligible in NEMO site (long time measurement needed)
  • relevant in Baikal lake

>

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Workshop II

Km3 neutrino detector workshop

KM3 neutrino detectors – Cerenkov, radio, acoustic detections; effective area, energy range, energy and angular resolution, discovery capabilities. Present status and future techniques Luciano Moscoso – Cerenkov detection Christian Spiering – Acoustic and radio detection Gianni Pavan (Centro Interdisciplinare di Bioacustica, Univ. Di Pavia – The km3 neutrino detector: an example of deep underwater multidisciplinary laboratory Sandra Zavatarelli – Present and future photon detectors for km3 neutrino telescope. Riccardo Papaleo - Study for a Km3 Cerenkov detector in Capo Passero site: mechanics, deployment, data transmission Gert-Jan Nooren – Electronic equipment required for a Km3 neutrino detector Vincent Bertin – Slow control for a Km3 neutrino detector Domenico Lo Presti - Development of a new electronics for the km3 neutrino detector.

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Cerenkov-Radio-Acoustic

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Different techniques

Ice: Amanda ⇒ IceCube Lake water: Baikal Sea water:

  • Nestor ⇒ 7 towers in Pylos, Greece
  • Antares ⇒ KM3
  • Nemo ⇒ KM3 near Sicily, Italy
  • L. Moscoso
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Relevant parameters

Angular resolution (astronomy) Energy resolution

  • Induced muons
  • Contained events

Effective area or volume

  • L. Moscoso
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AMANDA

Presence of the two surface shower detectors, SPASE-1 & 2 allows to check the AMANDA pointing resolution and the efficiency estimations. σθ ≅ 2.5°

  • L. Moscoso
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Angular Resolution (Antares)

The angular resolution

  • f the detector

depends on – reconstruction algorithms – selection programs – timing accuracy (PMT timing error, positional error on OMs, timing calibration error)

  • At high energies the neutrino pointing accuracy is 0.4° or better including

light scattering effects

  • Note: at high energy error is dominated by reconstruction errors, at low

energy error by the angle between the muon and neutrino

(including scattering)

  • L. Moscoso
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AMANDA

  • L. Moscoso
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Effective area for Antares

trigger reconstruction selection

  • L. Moscoso
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Energy resolution in Antares

Energy estimation based on the quantity

  • f light detected by

the optical modules. Energy resolution is a factor of 4-5.

  • L. Moscoso
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Detection of νe

Muons induced by νµ: MT/MD ≈ (2.5km/D)ln(1.+Eν/(500GeV))

– 100-300 for the first gen. at 1 TeV – 50-100 (SuperK, Macro,…) – 10-20 for present projects – 2.5 for KM3

Energy determination: EMeas ∝ E1/2 at HE

– 1 TeV → 370 GeV – 1 PeV → 20 TeV – 1 EeV → 700 TeV

  • L. Moscoso

νµ I guess !!!

Tonino

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Detection of νe

Contained νe events: F. Bernard thesis (Antares) Worse angular resolution: σθ ≅ 2° Better energy reconstruction: ∆E/E ≅ 15%

  • L. Moscoso
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Amanda/Antares complementarity

Amanda Antares

  • L. Moscoso
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Acoustic1

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Acoustic2

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Acoustic3

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Acoustic4

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Acoustic5

  • Z. Dzhilkibaev

Baikal : Cerenkov and Acoustic set-up

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Acoustic6

  • C. Spiering
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Rice1

  • C. Spiering
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Rice2

  • C. Spiering
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Rice3

  • C. Spiering
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Rice4

  • C. Spiering
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IceCube

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Baikal upgrading

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Optical modules - Sandra Zavatarelli

  • reduction of TTS for QUASAR type PMT
  • position sensitive big diameter PMT ?? (see page 44)

DAQ in a km scale detector - Gert-Jan Nooren

  • 8000 PMT (all data to shore) on 100 strings (1or 2 fibres/string)
  • standard telecom items
  • 80 optical channels/fibre, 10 Gb/s per channel (see pages 45÷47)

Optical modules electronics - Domenico Lo Presti

  • low power (200mW/ch)
  • low Dead Time (<0.75% @ 50kHz 40K background)
  • fully configurable from shore
  • 0.35µm custom ASIC

Slow control system for a km3 neutrino detector - Vincent Bertin

  • extrapolate to large scale system adopted for 0.1km2

NEMO: R&D for a km3 in the Mediterranean - Riccardo Papaleo

  • cables, connectors, mechanics, deployment, electronics, site evaluation
  • the present project
  • the test site

R&D and Technology developments for the km3

200 MHz PM T&SPC Vi Start NSPE Dyn Anode Dynode 80ns R/W ACk R2 S SE1SE2 NSPE Start R1 RFf Dyn CkI TS PwD CkO SE CkW 3x250 channel SCA I1 I0 I2 CkR R/W R Cs Os Ot RAdc RTc CR SR Load 20 MHz
  • Est. Reset
16/ O I Read FIFO 16/ LIRA SE CkW I1 I0 I2 CkR R/W R Cs Os Ot LIRA SR 3x250 channel SCA 80ns PLL 10/ 5 Mbit/s ADC Ck PwD ADS 901 I O Control Unit Data Pack & Transfer U. Counter R16 Bit DPTU k j Q Ck Q R H H L k j Q Ck Q R Trh = 5SPE Comp2 Too long Too High More than one shot G1 TH TL TS NSPE Start Ck2 C2 Comp1 Trh = SPE/4 80ns Q Tr M1 Q T & SPC Vi C1 G2 Q Tr M1 Q Dyn Q Tr M1 Q 1 2 3 4 5 6 7 12 Low Power DAQ A/D; D/A Switch PLL DSP 2:1 Compression FIFO FPGA Manchester Codec Clock Recovery Hybrid Transformer DC Extraction DC/DC Conv data bus control 20 Mhz Clk Rx TX Line data bus control slow Control bus 2.5 Mhz Clk data bus control Test Port Optical Module 8 9 10 11 DC Power Hybrid Transformer DC Feeder FPGA 2.5:1 Compression FIFO Test Port x 10 10 Mhz Clk 10 Mbit/s Line Rx TX x 10 x 10 Control bus 100 m DSP Concentrator Module
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  • S. Zavatarelli

Studing & Improving Photomultipliers ....

... a change in the QUASAR PMT geometry could equalize the photoelectrons paths and reduce the TTS ...

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DAQ in km-scale (1)

G.-J. Nooren

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DAQ in km-scale (2)

G.-J. Nooren

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DAQ in km-scale (3)

G.-J. Nooren

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NEMO PROJECT NEMO PROJECT

SHORE SHORE STATION STATION ELECTRO OPTICAL ELECTRO OPTICAL CABLE CABLE

  • R. Papaleo

papaleo1

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MAIN CABLE MAIN CABLE

  • 64

64 STRINGS and/or TOWERS STRINGS and/or TOWERS

  • 8

8 ROWS ROWS

  • 8

8 COLUMNS COLUMNS

  • 200m

200m Distance between ROWS Distance between ROWS

  • 200m

200m Distance between COLUMNS Distance between COLUMNS

  • 1

1 MAIN JUNCTION BOX MAIN JUNCTION BOX

  • 8

8 SECONDARY JUNCTION BOXES SECONDARY JUNCTION BOXES

  • 100 km

100 km ELECTRO OPTICAL CABLE ELECTRO OPTICAL CABLE FROM FROM SHORE SHORE

  • 4096

4096 OPTICAL MODULES OPTICAL MODULES

The LAYOUT The LAYOUT

  • R. Papaleo
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Ti or composite Ti or composite Material Material 20 m 20 m Plane length Plane length 150 m 150 m Distance between the BSS and the first plane Distance between the BSS and the first plane 40 m 40 m Distance between planes Distance between planes 64 64 Optical modules in each tower Optical modules in each tower 4 4 Optical modules in each plane Optical modules in each plane 16 16 Number of planes Number of planes 750 m 750 m Total height Total height Optical Module Optical Module Electronic module Electronic module Electro optical cable Electro optical cable Beam Beam

750 m

TOWER a la NEMO TOWER a la NEMO

  • R. Papaleo
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ALCATEL ALCATEL

proposed a data transmission system according to NEMO specifications. Main characteristics :

  • Standard communication system;
  • Redundancy system;
  • High MTBF;
  • High transmission rate (8 output line @ 20 Gbps)
  • Low power consume (< 500 W each string and/or tower)

DATA TRANSMISSION SYSTEM DATA TRANSMISSION SYSTEM

One module for each plane

  • f the string.This Optical

Module (S-1.1) will be used as Electrical/Optical converter within the customer equipment in both sides, under sea and in the landing station.

ST STM M1 1+S1 +S1.1 .1 1660 SM 1660 SM

One module for each tower

  • f

the detector. Each 1660SM will collect all the data coming from the 16 STM 1 of the string. The module will be closed inside a small Junction Box at the base of the string.

  • R. Papaleo
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Main Spare 1660SM 1660SM 1686 W M 1686 W M 100 Km. STM-1 STM-1

SHORE

Ring S t ruc tu re

NE M O

TRANSMISSIOM SYSTEM TRANSMISSIOM SYSTEM General Scheme General Scheme

  • R. Papaleo
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Land ing S t a t i

  • n

From Sea

8x1686W M (

t hey a r e t he equ i va len t

  • f

t he 8 j unc t i

  • n

Boxes )

64x1660SM

( t hey ar e t he equ i va len t

  • f

t he 64 s t r i ngs and /o r t

  • we

rs

  • f

t he t e l escope )

1024xST1 . 1

N MS

TRANSMISSIOM SYSTEM TRANSMISSIOM SYSTEM LANDING station LANDING station

( t hey a re t he equ i va len t

  • f

t he 1024 p lanes

  • f

t he t e l escope )

  • R. Papaleo
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papaleo7

  • R. Papaleo
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Deployment of the Deployment of the towers towers

  • R. Papaleo
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LABORATORY LABORATORY UNDERWATER UNDERWATER STATION STATION

TEST SITE LAB TEST SITE LAB at Port of at Port of Catania Catania

Long term tests for: underwater connections, electronics, mechanical structures, optical and acoustic detectors. Multidisciplinary laboratory GEOSTAR – POSEIDON on line underwater seismic station

  • R. Papaleo
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Cable features: Cable features: 10 Optics Fiber standard ITU- T G- 652 6 Electrical Conductors Φ 4 mm2

TEST SITE CABLE TEST SITE CABLE LAYOUT LAYOUT

2.330 m of Double Armed Cable 20.595 m of Single Armed Cable J B B U J B JB

Drop cable 2 Drop cable 2 -

  • 5.220

5.220 m m Drop cable 1 Drop cable 1 -

  • 5.000

5.000 m m

  • R. Papaleo
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LABORATORY LABORATORY EO CABLE EO CABLE

  • Length – 25 km
  • 10 Optics Fiber ITU- T G-652
  • 6 Electrical Conductors Φ 4 mm2

UNDERWATER LABORATORY UNDERWATER LABORATORY

  • N.1 Main Junction Box
  • N.2 Secondary Junction Box
  • N.2 NEMO Tower

NEMO PROJECT NEMO PROJECT Phase 1 Phase 1

EO Cable EO Cable EO Cable EO Cable

  • R. Papaleo
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MAIN JUNCTION BOX MAIN JUNCTION BOX SECONDARY JB SECONDARY JB Base of a NEMO TOWER Base of a NEMO TOWER

UNDERWATER LABORATORY UNDERWATER LABORATORY

Base of a NEMO TOWER Base of a NEMO TOWER CABLE from SHORE CABLE from SHORE

  • R. Papaleo
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Cerenkov detectors on the way towards two km3 astrophysics neutrino detectors The improved BAIKAL could reach high sensitivity on νe Tecnology development in collaboration with leader companies is mandatory Radio and Acoustic detections are

  • promising. On-going test will

demonstrate the S/N separation, calibration, directionality, ... Radio and Ice-Cube Acoustic and km3 water detector ... future hybrid detectors ????

Summary