Results and perspectives from Alteino and Si-Rad experiments M. Casolino INFN Roma Tor Vergata JointNASA/ESA Inc13 Science Symposium Slide 2 Current and future detectors images with labels: Sileye-3/Alteino; Lazio; Altea; Pamela; Sirad Slide 3 Observations at the minimum of 23 degrees solar cycle graph of ISES Solar Cycel Sunspot Number Progression with labels: Sileye-1; Nina-1; Sileye-2; Sileye-3; Sileye-3; Pamela; Altea; Satellite; Mir; ISS; Nina-2; Lazio Slide 4 Altcriss Alteino Long Term cosmic ray measurements on board the ISS • In response to AO 2004 ESA (AO2004-067) • ESA opportunity to start operations in the framewol of the ESA LDM (Long Duration Mission) – 4/5/2005 • Replanned on increment 12 (Dic2005-Mar 2006) • Next operations on increment 13 (Apr 2006 - Oct 2006) Slide 5 ALTCRISS Collaboration Dr. Francis Cucinotta, NASA Prof. Marco Durante, University Napoli Dr. Christer Fuglesang, EAC Dr. Cesare Lobascio, Aleniaspazio Dr. Aiko Nagamatsu (JAXA) Prof. Livio Narici, University of Roma Tor Vergata Prof. Piergiorgio Picozza, University of Roma Tor Vergata Guenther Reitz (DLR) Prof. Lembit Sihver, University of Chalmers (SE) Prof. Piero Spillantini, University of Florence Dr. V. Bengin (IBMP) Slide 6 Sileye/Alteino institutions 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.Trukhanov91 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, Russia4 Dept. of Physics of Univ. and Sez. INFN of Trieste, Italy8 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, Italy7 IROE of CNR, Florence, Italy; 8 Royal Institute of Technology, Stockholm, Sweden; 9IMBP, Institute of BioMedical Problems, Moscow, Russia Slide 7 Scientific Objectives • Measure of cosmic ray abundances and radiation environmenton on board the ISS (p-Fe >50-100MeV/n) • Long term monitoring of solar modulation and solar particle events. • Study of the effectiveness of different shielding materials on board the ISS - in parallel to Montecarlo and Beam Test studies • Measures with passive dosimeters (JAXA, DLR, FedII, INFN) • Joint measures with Matroska, Pamela and Altea Slide 8 Earth's magnetosphere WhyShielding? • A vast number of studies have been devoted to the subject of radiation shielding • Different material have been proposed. Hydrogenous materials have the best characteristics. • Active (superconducting magnets) shielding has also been proposed (ESA TT 2002) • Needed for interplanetary or lunar missions outside the magnetosphere ESA Topical Team in Life Sciences Shielding from Comic Radiation for Interplanetary Missions: Active & Passive Methods Contributors: Dr.M.Casolino,Rome (I) Prof.M.Durante,Naples (I) Prof.R.Mueller-Mellin,Kiel(D) Dr.P.Nieminen,Noordwijk (NL) Dr.G.Reitz,Cologne (D) Prof.L.Rossi,Milan (I) Prof.V.Shurshakov,Moscow (RUS) Dr.M.Sorbi,Milan (I) Prof.P.Spillantini,Florence (I) Slide 9 Sileye-3 Alteino • Placed on ISS in 2002 (ISM-1):operational for 6 days • Reswitched on in 2005 (ISM-2): operational for4 days • Long term measurements (ALTCRISS): 3 months untill now Slide 10 Silicon detector: image of silicon detector with labels Silicon plane #1 (back side); Top Scintillator; Silicon Detector; Front-end electronics with description of: 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.) • 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 (E min=40MeV/n) • Geom Fact: 24 cm^2sr • Bidirectional • Max Field of view 39 degrees • 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. Slide 11 graphs of Single track (Ne) event (ADC Channels) with labels: X view; Y view; Strip number; Plane number graphs of Shower event (ADC Channels) with labels: X view; Y view; Strip number; Plane number Slide 12 Mission timeline . 24 Dec 2005 Begin measurements – PIRS module – no shield . 26 Dec 2005 Data sample received . 06 Gen 2006 Poliethilene shielding inserted . 08 Gen 2006 Data sample received . 26 Gen 2006 Moved in the Service Module–noshield . Feb 2006 Shielding in the Service Module . Mar 2006 Rotate Instrument . Apr 2006: End increment 12 Rientro dati e dosimetri con Soyuz 11S . Apr 2006: Launch new dosimeters with Progress 21P . New orientation in crew cabin . New position close to DB-8 (IBMP) detector . Command module? . Autumn 2006: Joint measurements within Matroshka-2 Slide 13 Shielding and radiation measurements with active and passive detectors image of Alteino TLD, CR39 to measure charged particle and neutron dose with images of detectors for Jaxa, DLR, Napoli Fed. II INFN-LNF Slide 14 Precursor measurements with Lazio-Sirad (ISM-2: April 2005) • Study of the effect of different shielding materials on the cosmic radiation • 4 different shielding materials (5g/cm^2): Air, Kevlar, Poliethilene, Nextel/Kapton In use in ALTCRISS with passive detectors images with no labels. Slide 15 Shielding bag Polietilene shielding: (5g/cm^2): (Same thickness of the US section of the station) image of shielding bag Slide 16 Dosimeter arrangement Each Package: 2 Napoli TLD 6 DLR TLD (diff. Material) 1 Napoli CR-39 2 DLR CR-39 1 JAXA Padles images for dosimeter arrangement with labels: SHIELD1; SHIELD2; CNTRL GROUND; ESCHILO (SPACE); CNTRL (SPACE) Slide 17 image of Brasilian As Marcos Pon 5/4/2006 Slide 18 INCR. 12 PIRS module - PANEL 302 image with labels: ALTEINO detector; Eschilo tile + dosimeters; Cards and Control dosimeter; Poliethilene Tiles with dosimeters; PIRS module: 401 To Progress 24/12/2005 Configuration Slide 19 6/1/2006 Configuration: same location - with shielding tiles image with no labels Slide 20 Service Module (Crew Cabin) image with diagram of spectrometer ast image with description: Ray Tracing Results - Shielding (pathlength in assigned material) along each of 5000 rays is color-coded to the total amount of shielding [g cm^-2]; thinnest shielding is white, thickist is blue M. Shavers et al, ASR 34 (2004) 1333 Slide 21 Incr. 12 preliminary data: Acquisition rate vs time, min (raw data) image of graph c1 with labels: rate, SAA, Entries 431114, Mean 1108, RMS 671.3 Slide 22 Acquisition rate vs time, min (raw data, zoom) image of graph c1 with labels: Poles, Equator, SAA, Entries 431114, Mean 1467, RMS 457.3, rate slide 23 All-Particle count world map SAA Slide 24 Heavy nuclei world (Z>6) world map image of c1 graph with labels: ratellhighz, Entries 2552, Mean x 181.3, Mean y 0.9411, RMS x 104, RMS y 42.54 Slide 25 Nuclear abundances image of c1 graph with labels: C, O, N, Mg, Ca, Fe, 26-12-2005 data sample PIRS Module (2gg) – No Shield, yse, Entries 2997, Mean 4.983e+004, RMS 7.488e+004 Slide 26 Comparison with/without shielding image of c1 graph with labels: C; O; N; Mg; Ca; Fe; Ne; Black – 26/12/2005 No shield O/C=0.9; Red–6/1/2006 5 g/cm^2 poliet; O/C=0.75; Data normalized to Carbon (preliminary analysis based only on sample data; xse; Entries 2672; Mean 2.511e+004; RMS 1.99e+004 Slide 27 Nuclear abundances 2002 Image of graph with labels: newene_angolo_h; C, O, B, N F, Ne, Na, Mg, Si, Ca, Fe, ADC ch, Ev.N., KeV/u Slide 28 Difference PIRS – Service Module image of c1 graph with labels: Nero – PIRS (2672 entries) – 40 hours; Red– Service module (Crew Cabin) – 4319 entries–45 ore; C; O; N; Mg; Ca; Fe; Ne; Higher flux in the crew (according to calculations); xse; Entires 2672; Mean 7.296e+004; RMS 9.78e+004 Slide 29 Pirs-Service Module rel. abundance image of c1 graph with labels: Nero –PIRS; Red– Service module(values normalized to carbon); Higher flux in the crew (according to calculations); C; O; N; Mg; Ca; Fe; Ne; xse; Entries 2672; Mean 7.296e+004; RMS 9.78e+004 Slide 30 Number of hits distribution image of scatter graph of c1 with labels: Time (2002); Number of hits; n. entries Slide 31 Particle Showers – multiple hits image of c1 graph with labels: Time (2002); Number of hits; zhitperc; In High cutoff regions the percentage of straight tracks is lower Slide 32 Showers vs straight tracks image of graph with labels: Percentage of Showers (>16 hits); Geomagnetic shell L; percL; Entries 47; Mean 3.003; RMS 1.476 Slide 33 Ground Segment • Usoc at Mars (NA) (Link with ESA, data reception, ISS orbital parametes) – special thanks to Dario Castagnolo and Raimondo Fortezza • Local Usoc in Tor Vergata (Built for ISM-2 mission, currently shared for Altea, Pamela and Altcriss) image of Usoc Slide 34 Lazio-Sirad Detector Built (in 6 months) In response to opportunity to flight in ISM-2 (April 2005) •Silicon detector •SI-PM •Magnetometer image of Lazio Detector assembly with labels: Magetomter; Pc104 Tower|8 Standared card Pc 104; SC3+SIPM; SC2; Ladders; SC1+SiPM; Magnetometer DAQ; Front-end Electronics; DC/DC converter; Case; Trigger power Supply; Backplane; 4 Standard VME (2TDR.TPSFE.TBS) slide 35 Figure 2b Alteino & Lazio detectors inside PIRS module of ISS To Soyuz Slide 36 Silicon Microstrip detector graphs with labels: Readout pitch is 110 µm for the p-side (640 channels) 208 µm for the n-side (384 ch) Slide 37 LAZIP-SiRad flight data graphs of LAZIO-SiRad Slide 38 graph of Particle rate with 2.5 hours data Energy release •Good linearity between channels •Proton peak evident graph with charge (truncated mean) with labels: n-side (arbitary units); p-side (arbitary units) Slide 39 SIRAD • Under construction • 16 double silicon planes • Trigger with scintillator • Self Trigger • Calorimeter on bottom graph of SIRAD Slide 40 CPU •Protototype integrated with FPGA and front-end •CPU 144 Mhz, 280 Mips •2 Mbyte flash 4 RAM •2 usb •1 bus esterno 16 bit indirizzamento esterno 14 bit •FPGA actel reprogrammable 80kGate 208 pin: •I/F frontend, alarms housekeeping image of CPU board slide 41 Front end Completed ingegnerization of the boards Low interplanar distance (5mm/2 piani vs a 3 cm/2 piani) Under intergration with power and distribution boards image of board Slide 42 schmitic with labels: A=26.7mm; A=26.7mm; A=26.7mm; power supply; Trig1; DPU, Driver Y; Driver X; Trig2; DPU, DPU; FPGA Slide 43 SiPM’s SiPM consist of thousands pixels . 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=10^6e Electrical inter-pixel cross-talk minimized by: - decoupling quenching resistor for each pixel - boundaries between pixels to decouple them results: reduction of sensitive area and geometrical efficiency Very fast Geiger discharge development < 500ps Pixel recovery time = (Cpixel Rpixel) ~ 20 ns - 1µs Dynamic range ~ number of pixels diagrams with labels: Resistor Rn=400 k Omega-20M Omega; Pixel; Ubias; Al; Depletion Region 2 µm; Substrate; 20µm; 42µm Slide 44 Scintillation detector based on SiPM for LAZIO-Sirad (1*1mm) The scintillator+ wave length sifter (WLS) + SiPM technology was used. image of Scintillation detector with labels: Scintillation detector with SiPM’s (each detector consist of 8 tiles ); Power distributor image of Single tile= scintillator+WLS+SiPM WLSused for: - The light collection from 30x30 cm2 scintillator to 1x1 mm2 sensitive aria of SiPM, - The shift of scintillation radiation spectrum to yellow-green field, where is maximum of SiPM PDE (Photon Detection Efficiency) Slide 45 Silicon-Photomultiplier data graph of Silicon-Photomultiplier data with labels: POLI; Equatore; Count rates of trigger system signals vs time; Time in sec; Count rate in Hz; S1T1S2; S1S2 Slide 46 3x3mm SiPM, 5625 pixels Sensitive area : 3x3 mm2 # of pixels: 5625 Depletion region: ~ 1 µm Pixel size: 30 µmx30 µm Working voltage: 20…25 V Gain: (1…2) x10**6 Dark rate.room temperature: 20 MHz SiPM noise(FWHM): room temperature 5-8 electrons -50 C 0.4 electrons Single pixel recovery time: 1us After pulsing probability: ~ 1% Optical crosstalk: ~ 30 - 50 % ENF: appr. 1.5-2.0 (overvoltage dependent) image SiPM Slide 47 SiPM’s long term stability graph of 20 tested SiPM’sworked during 1500 hours with labels: before tests ; after 500 hours; after 1500 hours; dark rate, kHz; SiPM number; efficiency of light registration, %; gain (*10^6); dark current, microAmper; Parameters under control: • Dark rate • Efficiency of light registration • One pixel gain • Dark current Slide 48 Some properties of 3x3 mm SiPM’s graph of 3x3 mm^2 (#35 delta U=U-U sub bd=2V) T=-500 degrees C with labels: Efficiency e, %; Wavelength gamma, nm slide 49 Cosmic Ray spectrum (3*3mm) graph with image and labels: Numero Eventi; Canali ADC; SiPM 2 (a+b); PMT; SIPM1; PMT; SIPM1; 1ph; 2ph; 3ph; 4ph; T ambiente Sipm + Scintillatore (no wlshifter) Slide 50 Pamela image of Pamela with labels: Magnetic Spectrometer Microstrip detector; Silicon Tungsten Tracking calorimeter; Shower Catcher Scintillator; Neutron Detector; Time of Flight; RESURS DK1 SATELLITE (4.5T) Slide 51 diagram back ground with labels: X View; Top View; Y View • 450 kg detector devoted to research of antimatter component in cr • Protons + nuclei up to O • Polar orbit • Currently integration in Baikonur, • Launch foreseen by Spring2006 slide 52 Integration in Baikonur cosmodrome, April 2006 Slide 53 Conclusions: need for joint operations • Joint Measurements with different detectors Active/Passive Different detector response, shielding ecc. Of crucial importance to determine particle flux variation in different points of the magnetosphere and ISS • Ground/Space comparison/crosscorrelation accelerator / shielding / calibration • Use of space data for operational applications • Models (trapped population, solar particle events, propagation in the magnetosphere) • Montecarlo Simulations (Benchmarking / ion interactions): Geant 3.21, Geant 4, Fluka, HZTRN, Phits More important than HE experiments Slide 54 Availability of PhD positions (post-graduate) in Roma Tor Vergata University: http://www.uniroma2.it/postgrad/inglese/applicazioni/instruction.htm And/or contact casolino@roma2.infn.it or picozza@roma2.infn.it Slide 55 Thank you! Slide 56 Energy acceptance Table 1 Left Minimum trigger energy of Sileye-3. Center Minimum energy for the data cut for various nuclear species. Right Minimum energy loss in silicon. Particle Trigger Threshold Cut threshold Energy loss MeV/n MeV/n (keV/µm) P 32 34 0.4 He 32 40 1.6 B 53 54 9.3 C 59 70 13.5 N 65 75 18.7 O 69 79 24.5 F 71 84 30.8 Ne 77 94 37.9 Na 79 95 47.2 Mg 86 104 54.4 Al 88 106 68.4 Si 94 110 75.3 Ca 114 136 152.6 Fe 126 150 254.4