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AMS-02 Experiment (Alpha Magnetic Espectrometer). Detector and Expectations. Diago UniverseNet School ‘09 IAC (Spain) October 2, 2009. AMS-01. AMS-01 was launched on the Shuttle Discovery on 2th June 1998. 180 hours of data: 10 8 events.
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AMS-02 Experiment(Alpha Magnetic Espectrometer) Detector and Expectations • Diago UniverseNet School ‘09 • IAC (Spain) October 2, 2009
AMS-01 • AMS-01 was launched on the Shuttle Discovery on 2th June 1998. • 180 hours of data: 108 events. Discovery with AMS-01 seen from MIR
AMS-02 AMS-01: Results • Feasible proyect • Measures of fluxes p, He3, He4, e+, antiprotons. • Secondary spectrums near earth orbit under the geomagnetic cutoff: • Protons • Leptons • Helium • New limits to the existence of antihelium AntiHe/He<1.1x10-6 AntiHe/He<0.9x10-4 (Buffington)
Detector’s Features AMS-02 • Second part of the AMS Experiment. • Developed with international cooperation. • It will be on ISS in autumn 2010. • General points: active 3 years at minimum + acceptance of 0.5 m2.sr 1010 nuclei
Detector’s Features Size: 3m x 3m x 3m Weight: 7 tons Subdetectors: TRD TOF TRACKER Anticounter RICH ECAL
Studies ready to be done • Cosmic rays composition (TRD, TRACKER, RICH) • Photon detection up to 1 TeV (TRACKER, ECAL) • Propagation (TRACKER, RICH) He3/He4 B/C Be10/Be9 • Antimatter searching Z>1 (TRACKER, RICH) • Dark matter searching (TRD, TRACKER, RICH) Size: 3m x 3m x 3m Weight: 7 tons
Transition Radiation e/p separation e- Discrimination e/p
e- Transition Radiation e/p separation p
Transition Radiation e/p separation e- Discrimination e/p e/p~102-103 x 20 AMS Collaboration
Time of Flight LV1, dir, β, Z LV1: Trigger
Time of Flight LV1, dir, β, Z LV1: Trigger selection
Time of Flight LV1, dir, β, Z LV1: Trigger selection ttravel= 1 ns 130 ps precision downwards-upwards
Time of Flight LV1, dir, β, Z e-
Time of Flight LV1, dir, β, Z e- e-
Time of Flight LV1, dir, β, Z e- e- e+
Time of Flight LV1, dir, β, Z LV1: Trigger selection Dir: downwards-upwards e-/antiP e+/p
Time of Flight LV1, dir, β, Z LV1: Trigger selection Dir: downwards-upwards e-/antiP e+/p Charge Z separation (up to 1 GeV)
Time of Flight LV1, dir, β, Z AMS Collaboration
Time of Flight LV1, dir, β, Z LV1: Trigger selection Dir: downwards-upwards e-/antiP e+/p Charge Z separation Mesure of b with few % precision
Superconducting Magnet AMS-01 Nd-Fe-B BL2= 0.14 T·m2 AMS-02 Superconducting BL2=0.86 T·m2 R=2.5 TV
Silicon Tracker Z,R Measure of rigidity Measure of charge
Silicon Tracker Z,R AMS Collaboration Combined Z measurements for 4 or more ladders on the K and S sides
Anticounter Acceptance
RICH β, Z n(NaF)=1,335 n(aerogel)=1,05
RICH β, Z AMS Collaboration Charge Z Speed b AMS Collaboration
Electromagnetic calorimeter e/p separación, E Discrimination e/p Measure of energy AMS Collaboration
Separation e/p Speed Charge Z Rigidity R Energy E Direction dir Mass m
Separation e/p: 106 Speed Charge Z Rigidity R Energy E Direction dir Mass m
Separation e/p Speed : s(b)/b=10-3 Charge Z Rigidity R Energy E Direction dir Mass m
Separation e/p Speed Charge Z:s(Z)/Z=0.2 Rigidity R Energy E Direction dir Mass m
Separation e/p Speed Charge Z Rigidity R: 2.5 TV Energy E Direction dir Mass m
Separation e/p Speed Charge Z Rigidity R Energy E: Direction dir Mass m
Separation e/p Speed Charge Z Rigidity R Energy E Direction dir: Distinction power: 10-9 Mass m
Separation e/p Speed Charge Z Rigidity R Energy E Direction dir Mass m: 2%(<1GeV)
What can be done with all this information? • What kind of particle is it? • Lepton, hadron, gamma
What can be done with all this information? • What kind of particle is it? • Lepton, hadron, gamma • Flux of the different particles
Composition: Fluxes C (10 days) e- (3 years) Fe (1 year) He (1 month) P (1 week) PAMELA PAMELA PAMELA AMS Collaboration
PAMELA PAMELA Composition: Fluxes AMS Collaboration PAMELA Collaboration
What can be done with all this information? • What kind of particle is it? • Lepton, hadron, gamma • Flux of the different particles • Ratios
Composition: ratios (1 day) Interestelar medium density Diffusion parameter AMS Collaboration
What can be done with all this information? • What kind of particle is it? • Lepton, hadron, gamma • Flux of the different particles • Ratios • Isotopic separation
Compostion: isotopic separation He3 He4 Be9 Be10 p D Rui Pereira, 2006 AMS Collaboration
What can be done with all this information? Is AMS-02 better than PAMELA? Of course!
AMS-01 (expected) PAMELA What can be done with all this information? AntiHe/He
What can be done with all this information? Is AMS-02 better than FERMI? We will try it with photons
AMS-02: Models constrains An anomalous positron abundance in cosmic rays with energies 1.5-100 GeV. O. Adriani etal 2009 Why this anomaly?
MDM=10 TeV DM+DM W+W- sannv=6·10-22 cm3/sec M. Cirelli, A. Strumia 0903.3381v2 e-+e+ antip/p AMS-02 e+/(e++e-) e-+e+ Posible answers: Dark matter contribution?