1 / 15

Detector Sub-Systems: Transition Radiation Detector Time of Flight scintillator counters

Mass : 7 t Size: ~ 3.2 x 2.7 m Power consumption: 2 kW Acceleration take off: 9 g Operation Temperature: -180 o + 50 o C Outgasing limit : <10 - 12 g/s/cm 2

gilles
Download Presentation

Detector Sub-Systems: Transition Radiation Detector Time of Flight scintillator counters

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. Mass : 7 t Size: ~ 3.2 x 2.7 m Power consumption: 2 kW Acceleration take off: 9 g Operation Temperature:-180o + 50oC Outgasing limit : <10- 12 g/s/cm2 Trigger rate: ~ 200 Hz Data rate: ~ 3 Mb/s • Detector Sub-Systems: • Transition Radiation Detector • Time of Flight scintillator counters • 8 layers of Si strip tracker planes in a superconducting magnet • Rich Imaging Cerenkov detector • Electromagnetic calorimeter

  2. AMS02 Detector: basic spectrometer Tracker : 8 planes of double sided Silicon (6 m2). 110 and 208 m pitch Resolution = 10 m in bending plane and 25 m non bend. Rigidity pc/Ze measurements up to ~3TeV dE/dx ~ Z2 measurement. Time of Flight: 2x2 planes of scintillator hodoscope Resolution T=110 ps @ Z=1 . Used in Trigger Velocity measurement =L/ct1-ct2/~3.5% dE/dx measurements Anticoincidence: veto plastic scintillators used in Trigger Superconducting Magnet: Bdipol =0.87 Tesla I~459A Size: d=1.2m l=0.8 m; Mass 2.3 t cooled to 1.8K by superfluid He II (3000 l)

  3. AMS02 Detector: particle identification Transition Radiation Detector:20 layers of 6mm straw tubes (Ntot=5248) filled with Xe/Co2 (44 kg Xe+3.7kg Co2) interposed with fleece radiator (22 mm). dE/dx measurements . Separation e/h ~10 3 - 10 2 p=1-250 GeV Ring Image Cherenkov Detector: radiators (NaF n=1.336 and Aerogel n=1.035) +PMT's velocity measurements  (up to 20 GeV /~ 0.1%) Absolute charge measurements Nphotons~Z 2 (=0.2) up to Z=26 Electromagnetic Calorimeter: Pb + scintillating fibers readout by 324 PMT's (2x2cm readout granularity) Overall 18 x-y planes. Size 65x65 cm2 . Weight 640 kg. Thickness ~16 Xo and ~ 0.5 nucl. . Energy measurements for leptons dE/E=0.03+0.13/E[GeV] Used in gamma trigger e,g / h separation ~10 3 E=1-1000 GeV

  4. Energy and Rigidity Measurements • Rigidity R=cp/Ze in the tracker • 8 3D high precision (±15 mm bend., 25 mm not bend. plane, 10 mm z) coord. for track fit • Expected MDR ~3 TV for He • Elm energy in the ECAL • measured in a test beam

  5. Velocity Measurements (b) RICH b=1/ncosq TOF b=DL/Dt A 96 PMTs proto was tested db/b=0.07% @ Z=1 Test Beam with with ions st= 180 ps @ Z=1, db/b=2-3% ToF

  6. The Magnet Mass = 2.3 tons It will be first superconducting magnet which will be flown in space

  7. The AMS SC Magnet

  8. PAMELA Spectrometer • GF 20.5 cm2sr for HE particles • Angular aperture of 19°x16° • Spatial res.: 4 mm (B. V.), 15 mm (N. B. V.) • Maximum Detectable Rigidity (MDR): 740 GV • TOF accuracy <100 ps • e/p discrim. better than 2x105 Launch date june 2006

  9. PAMELA • GF 20.5 cm2sr for HE particles • Angular aperture of 19°x16° • Spatial res.: 4 mm (B. V.), 15 mm (N. B. V.) • Maximum Detectable Rigidity (MDR): 740 GV • TOF accuracy <100 ps • e/p discrim. better than 2x105 Antiproton flux 80 MeV - 190 GeV Positron flux 50 MeV – 270 GeV Electron flux up to 400 GeV Proton flux up to 700 GeV Electron + positron flux up to 2 TeV Light nuclei (up to Z=6) up to 200 GeV/n Antinuclei search (sensitivity ~ 10-8 in antiHe/He) LAUNCHED JUNE 15, 2006!

  10. WIMP detection Methods of WIMP CDM detection: Discovery at accelerators (fermilab, LHC) Direct detection of halo particles in terrestrial detectors Indirect detection of 's,  rays, radio waves, anti-p,e+ in earth, balloon borne and space based experiments Observe the recoil nucleus by different tecniques using large mass detectors ( not suitable for space based searches...) The basic process for indirect detection is annihilation in the halo, e.g. 's Neutralinos are Majorana fermions KK particles are bosons ann=n2DMv /2DMv/m2DM Enhanced for clumpy halo near the galactic center and in Sun & Earth Indirect detection

  11. c c M  100 GeV E ER ~ 10-100 keV ~ 50 GeV e+, p, ,  N background signal 0 50 100 E ( GeV) Methods to find Dark Matter Direct Indirect WIMPs scattering on target nuclei Measure nuclei recoils WIMPs annihilate in halo or in massive bodies Measure flux of annihilation products (,, e+,anti-p,anti-D) c c M  100 GeV + accelerator searches • Energy spectrum of recoils is featureless exponential with <E> ~ 50 keV • Energy spectrum is continuum, features possible signal N background 0 50 100 E ( keV)

  12. AMS02 status TRD Magnet Coils ready 2 Vacuum He cases ready: one in England (flight model), one at CERN (pre-integr. model) All the sub-detectors ready Magnet ready by Feb 08 Magnet • Pre-integration in progress at CERN • Tracker planes on support structure, being inserted in magnet vacuum case these days at Cern • Half November Upper Tof and TRD mounted (shipping to Cern half October) Tracker • Parallel separate integration of LTOF, RICH and ECAL which will not pre-integrated • Final integration will begin March 2008 UTOF • Thermovacuum test at ESTEC of the entire detector in June 2008 • Beam test at Cern in September 2008 (maybe) • End of 2008 shipping to Kennedy Space Center ready for flight • Within 2009 launch for installation of ISS RICH LTOF ECAL

  13. (m2 sr)

  14. What Nature has to Offer What we hope for! D.S. Akerib

More Related