Sirad/Altcriss: misure a lungo termine a bordo della stazione

spaziale con il rivelatore Sileye3: risultati preliminari

M. Casolino

INFN Roma Tor Vergata

SileyeSileye//AlteinoAlteinoinstitutionsinstitutions

V. Bidoli1, M. Casolino1, M. P. De Pascale1, M. Minori1, A., L. Narici1, P. Picozza1, E. Reali1, R. Sparvoli1, V. Zaconte, A. Galper2, A. Popov2, S. Avdeev3, M. Boezio4, W.

Bonvicini4, A. Vacchi4, G. Zampa4, N. Zampa4, G. Mazzenga5, M. Ricci5, P. Spillantini6,G. Castellini7, P. Carlson8, C. Fuglesang8, V. Benghin9, V. P. Salnitskii9, O. I.

Shevchenko9, V. Shurshakov9, V. P. Petrov9, K.A.Trukhanov9

1 Dept. of Physics, Univ. of Rome "Tor Vergata" and INFN Sez. Rome2 , Italy; 2 Moscow State Engineering Physics Institute, Moscow, Russia;3 Russian Space Corporation "Energia" by name Korolev, Korolev, Moscow region, Russia 4

Dept. of Physics of Univ. and Sez. INFN of Trieste, Italy; 8 Dept. of Physics of Univ. and Sez. INFN of Perugia, Italy; 5

L.N.F. - INFN, Frascati (Rome), Italy; 6 Dept. of Physics of Univ. and Sez. INFN of Florence, Italy; 7 IROE of CNR, Florence, Italy; 8 Royal Institute of Technology, Stockholm, Sweden;

9IMBP, Institute of BioMedical Problems,Moscow, Russia

Dr. Francis Cucinotta, NASAProf. Marco Durante, University of NapoliDr. Christer Fuglesang, EACDr. Cesare Lobascio, AleniaspazioDr. Aiko Nagamatsu (JAXA)Prof. Livio Narici, University of Roma Tor VergataProf. Piergiorgio Picozza, University of Roma Tor VergataDr. Guenther Reitz (DLR) Prof. Lembit Sihver,University of Chalmers (SE)Prof. Piero Spillantini, University of FlorenceDr. V. Bengin (IBMP)

Collaborazione ALTCRISS

Sirad/Altcriss Alteino Long Term measurements inside the ISS

•In risposta all’AO 2004 ESA

•Valutazione “Excellent”, 29/3/2005.

• Proposta ESA di anticipare le attività nell’ambito della LDM (Long Duration Mission di Thomas Reiter – 6 mesi astronauta ESA sulla ISS) – 4/5/2005

•Ripianificato, a causa del ritardo dello Shuttle su Incremento 12 (Dic 2005-Mar 2006)

Piano della Missione

•Utilizzo Sileye-3/Alteino per misure a lungo termine sulla ISS

• Previsti tre anni di misure nella stazione (in preparazione missione con Incremento 13 – Progress 21P, Aprile 2006)

•Impegno finanziario Esa (upload, tempo astronauta, ground segment…) circa 700keuro/anno

Obiettivi scientifici

• Misura dei raggi cosmici e dell’ambiente radioattivo a bordo della ISS(p-Fe >50-100MeV/n)

•Studio dell’efficacia e dell’effetto di vari tipi di schermatura sui raggi cosmici a bordo della stazione (Misure con e senza schermatura in vari punti ed orientazioni della ISS, in parallelo a test su fascio e simulazioni Montecarlo)

•Misure con Dosimetri passivi (JAXA, DLR, Fed II)

•Misure congiunte con Matroska, Pamela ed Altea

•Monitor a lungo termine dell’attività solare ed eventi solari

Sileye-3 Alteino

•Posto sulla ISS nel 2002 (operativo per 6 giorni)

•Riacceso nel 2005 (operativo per 4 giorni) (Lazio-Sirad)

Left: AST detector tower open (without readout electronics): it is possible to see the stack of silicon detectors and the top scintillator (the detector is upside down). The bottom scintillator has been removed for clarity. Rigth: One of the 8 silicon detector boards (X view). It is possible to see the segmentation of the 32 strips of the detector. (Photos taken during assembly in the clean room facilities of Tor Vergata.)

Silicon detector:•8 silicon planes (4x,4y)•32 strips strip pitch 2.5 mm, 8x 8 cm2, thickness 380 µm•Total 256 Independent channels•Triggered by two scintillators (Emin=40MeV/n)••GeomGeom Fact: Fact: 24 cm24 cm2 2 srsr••Bidirectional Bidirectional ••MaxMax FieldField ofof viewview 3939oo

• The front-end is a developed version of two 16 channels CR1 chip with a peaking time of 2 µs; a sensitivity of 5 mV/MIP and a maximum counting rate of 30 kHz.

Shower event (ADC Channels)

X view

Y view

Strip number

Pla

ne n

umbe

r

Single track (Ne) event(ADC Channels)

Y view

Strip number

Pla

ne n

umbe

r

X view

X view

Y view

Strip number

Pla

ne n

umbe

r

X view

Y view

Strip number

Pla

ne n

umbe

r

Lancio Progress 20P– 22/12/05 h 00:38:18(cosmodromo di Baikonur)

Attracco Progress – 23 Dec 2005

Piano della Missione

!24 Dec 2005 Attivazione strumento – Modulo PIRS – no schermatura!26 Dec 2005 Ricezione campione di dati!06 Gen 2006 Inserimento schermatura polietilene!08 Gen 2006 Ricezione campione dati!26 Gen 2006 Spostamento nel modulo di Servizio – no schermatura

!Feb 2006 Inserimento schermatura!Mar 2006 Riorientazione strumento

!30 Mar 2006: Fine incremento 12. Rientro dati e dosimetri con Soyuz 11S

!Apr 2006: Lancio nuovi dosimetri con Progress 21P

Futuro missione

•Nuovo lancio dosimetri, card con Progress 21P (30/4/2006)(In preparazione materiale, card e documentazione)

•Misure congiunte nell’ambito di MatroskaII (Settembre 2006) ed Altea (lancio previsto con prossimo shuttle… Luglio 2006)

Misure di Schermatura Lazio-Sirad

•Precursor flight – Lazio/Sirad (Apr 2005)•Study of the effect of differentshielding materials on the cosmicradiation•4 different shielding materials(5g/cm^2):

Air, Kevlar, Poliethilene, Nextel/Kapton

Alteino & Lazio detectors inside PIRS module of ISS

To Soyuz

To ISS

Schermatura – Altcriss

Nuovo Schermo solo in Polietilene (5g/cm^2):(Stesso spessore della sezione americana della stazione)

ALTCRISS DOSIMETERSEach Package:2 Napoli TLD6 DLR TLD (diff. Material)1 Napoli CR-392 DLR CR-391 JAXA Padles

SHIELD1 SHIELD2

CNTRL GROUND

ESCHILO (SPACE)CNTRL (SPACE)

X

Z

YV

X

Z

YV

Misure nel modulo d’attracco (PIRS)

ALTEINO detector

Eschilo tile+ dosimeters

Cards and Controldosimeter

Poliethilene Tiles with dosimeters

PIRS module: PANEL 401To Progress (nadir)

24/12/2005 Configuration

PIRS module - PANEL 302

6/1/2006 Configuration: same location - with shielding tiles

Service Module (Crew Cabin)

Acquisizione dati

•Avviene in continuo su card PCMCIA da 512 Mbyte

•Sostituite ogni 13 giorni

•Ogni locazione e configurazione viene trasmesso a terra un campione di dati di 1-2 giorni per la verifica dello stato del sistema

Acquisition rate vs time, min (raw data)

SAA

PolesEquator

SAA

Acquisition rate vs time, min (raw data, zoom)

Conteggi particelle

SAA

Nuclei Pesanti (Z>6)

C

O

N

Mg Ca Fe

DATI 26-12-2005Campione PIRS Module (2gg) – No Shield

ABBONDANZE NUCLEARI

C

ON

Mg Ca FeNe

Nero – Dati 26/12/2005 No shield O/C=0.9Rosso – Dati 6/1/2006 5 g/cm^2 poliet O/C=0.75Dati normalizzati al Carbonio (analisi preliminare)

Confronto con/senza schermatura

ABBONDANZE NUCLEARI 2002

Differenze PIRS – Service Module

Nero – Modulo PIRS (2672 entries) – 40 oreRosso – Modulo di Servizio (Crew Cabin) – 4319 entries –45 ore

C

ON

Mg Ca FeNe

Confronto Pirs- Service Module

Nero – Modulo PIRS Rosso – Modulo di Servizio (valori normalizzati)

C

ON

Mg Ca FeNe

R 50ΩΩΩΩ

hνννν

Pixel

Ubias

Al

DepletionRegion

2 µµµµm

Substrate

20µµµµm

42µµµµm

" Pixel size ~(20-40) µm" Working point: VBias = VBreakDown + Vd (< ~70 V )

Vd ~ 3V above breakdown voltage"Each pixel behaves as a Geiger counter with

Qpixel = Vd * Cpixel ;

Cpixel~50fmF #Qpixel~150fmC=106e

Electrical inter-pixel cross-talk minimized by: - decoupling quenching resistor for each pixel - boundaries between pixels to decouple themresults: reduction of sensitive area

and geometrical efficiency

Very fast Geiger discharge development < 500 ps

Pixel recovery time = (Cpixel Rpixel) ~ 20 ns - 1µs

Dynamic range ~ number of pixels

ResistorRn=400 kΩΩΩΩ - 20M ΩΩΩΩ

SiPM’s

SiPM consist of thousands pixels

Scintillation detector based on SiPM for LAZIO-Sirad (1*1mm)

The scintillator + wave length sifter (WLS) + SiPM technology was used.

Power distributor

Single tile = scintillator+WLS+SiPM

WLS used for:

- The light collection from 30x30 cm2 scintillatorto 1x1 mm2 sensitive aria of SiPM,

- The shift of scintillation radiation spectrum to yellow-green field, where is maximum of SiPMPDE (Photon Detection Efficiency)

Scintillation detector with SiPM’s

(each detector consist of 8 tiles )

Silicon-Photomultiplier data

Count rates of trigger system signals vs time

0

5

10

15

20

25

30

35

40

0 1000 2000 3000 4000 5000 6000 7000 8000 9000Time in sec

Coun

t rate

in Hz

S1T1S2

S1S2

POLI

Equatore

Calibration of SIPM

Count rate of S1*T1*S2 vs count rate of S1*S2

y = 0,4943x - 0,0616

R2 = 0,9827

0

5

10

15

20

25

5 10 15 20 25 30 35 40

Count rate of triggers in Hz

Coun

t rate

of S1

*T1*S

2

Sensitive area : 3x3 mm2 # of pixels: 5625Depletion region: ~ 1 µm Pixel size: 30 µmx30 µmWorking voltage: 20…25 V Gain: (1…2)

x10**6Dark rate.room temperature: 20 MHz

SiPM noise(FWHM):room temperature 5-8 electrons-50 C 0.4 electrons

Single pixel recovery time: 1usAfter pulsing probability: ~ 1%

Optical crosstalk: ~ 30 - 50 %ENF: appr. 1.5-2.0 (overvoltage dependent)

3x3mm SiPM, 5625 pixels

Test camere pulite – Tor Vergata(D. Badoni, R. Messi, M. Marchetti)

Caratterizzazione I-V(misure in continua)

L=68muAHL=94muA(20.8V)

Invecchiamento – dark current

Amplificazione

A(V)=I(V)/I(0.5V)

SiPM’s long term stability

0 2 4 6 8 10 12 14 16 18 2010-2

10-1

100

101

102

103

before tests after 500 hours after 1500 hours

dark rate, kHzS

iPM

par

amet

ers

SiPM number

efficiency of light registration, %

gain (*106)

dark current, microAmper

Parameters under control:

•Dark rate

•Efficiency of light registration

•One pixel gain

•Dark current

20 tested SiPM’s worked during 1500 hours

Some properties of 3x3 mm SiPM’s

350 400 450 500 550 600 650 7000

5

10

15

20

25

E

ffici

ency

ε, %

Wavelength λ, nm

3x3 mm2 (#35 ∆U=U-Ubd

=2V) T=-500C

Caratterizzazione

Spettro rc (3*3mm)

0 50 100 150 2000

5

10

15

20

25

30

35

40

Num

ero

Eve

nti

Canali ADC

SiPM 2 (a+b)

PMT

SIPM1

PMT

SIPM1

1ph

2ph3ph

4ph

T ambienteSipm + Scintillatore (no wlshifter)