Cosmic rays as seen from Space with AMS

Transcription

1 Cosmic rays as seen from Space with AMS Javier Berdugo / CIEMAT Madrid Società Italiana di Fisica XCVIII Congresso Nazionale Naples, 17 September 2012

2 V. Hess: 7th balloon flight (August 7th, 1912) Also Theodor Wulf, Domenico Pacini

3 Carl David Anderson working at Caltech with the electromagnet and a Wilson cloud chamber (~1932)

4 Discovery of Muons Discovery of Pions e Discovery of Kaons and Lambdas

5 The highest energy particles are produced in the cosmos LHC CERN Prevessin CERN Meyrin Largest Accelerator on Earth (LHC) will produce particles of 7 TeV Cosmic Rays with energies about 100 Million TeV have been detected.

6 Fundamental Science on the International Space Station (ISS) There are two kinds of cosmic rays traveling through space 1- Neutral cosmic rays (light rays and neutrinos): Light rays have been measured (e.g., Hubble) for over 50 years. Fundamental discoveries have been made. 2- Charged cosmic rays: Following the pioneering experiments with balloons and small satellites, using a magnetic spectrometer (AMS) on ISS is a unique way to provide precision long term (10-20 years) measurements of high energy charged cosmic rays.

7 The scientific goals of AMS on the ISS Search for primordial antimatter Search for Dark Matter Chemical composition and energy spectra of cosmic rays

8 6 ACC 0.45 m2 sr Exposure time: ISS live time 300,000 electronic channels 650 computers 5m x 4m x 3m 7.5 tons

9 AMS-02 Collaboration USA FLORIDA A&M UNIV. FLORIDA STATE UNIVERSITY MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER TEXAS A&M UNIVERSITY UNIV. OF MARYLAND - DEPT OF PHYSICS YALE UNIVERSITY - NEW HAVEN MEXICO UNAM NETHERLANDS ESA-ESTEC NIKHEF NLR FRANCE GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE SPAIN CIEMAT - MADRID I.A.C. CANARIAS. PORTUGAL LAB. OF INSTRUM. LISBON DENMARK UNIV. OF AARHUS FINLAND HELSINKI UNIV. UNIV. OF TURKU ITALY ASI CARSO TRIESTE IROE FLORENCE INFN & UNIV. OF BOLOGNA INFN & UNIV. OF MILANO INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF SIENA GERMANY RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE ROMANIA ISS UNIV. OF BUCHAREST SWITZERLAND ETH-ZURICH UNIV. OF GENEVA RUSSIA I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. KOREA EWHA KYUNGPOOK NAT.UNIV. CHINA BISEE (Beijing) IEE (Beijing) IHEP (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) TAIWAN SDU (Jinan) ACAD. SINICA (Taiwan) AIDC (Taiwan) CSIST (Taiwan) NCU (Chung Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu) 16 countries, 60 institutes, 600 physicists, 17 years

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11 AMS Group at INFN and University of Perugia

12 Italy in AMS M ilano Pisa LN L Bologna Perugia Terni Italian Roma 60 Scientists and Engineers 6 U niversities 5 I N FN Sections 2 I N FN N ational Laboratories 16 years of collaboration among I N FN and ASI LN S

13 Italian Industries in AMS CGS FBK - irst CARSO RI-Ba Composites CAEN Galli e M orelli G& A Engineering Euromec Space Companies

14 Tracker AMS: A TeV precision, multipurpose spectrometer TRD Identify e +, e - Particles and nuclei are defined by their charge (Z) and energy (E ~ P) TOF Z, E Silicon Tracker Z, P 1 Magnet ±Z ECAL E of e +, e -, γ RICH Z, E Z, P are measured independently by the Tracker, RICH, TOF and ECAL

15 The Magnet The detailed 3D field map (120k locations) was measured in May 2010 Z=0 Field 2010 Deviation from 1997 measurement In 12 years the field has remained the same to <1%

16 nuclear charge Z Time of Flight System Measures Velocity and Charge of particles Provide trigger for charged particles TOF 1 and Resolution = 160ps TOF 3 and , time of flight (ns) PMTs Scintillator PMTs Light Guides Light Guides He C O Al Ca Plane 4 3, 4

17 Anti-Coincidence Counters Efficieny >99.99% 17

18 The AMS Silicon-Tracker To use the bending power of the magnet, we have built a state of the art Tracking Detector based on 9 thin layers of Silicon Detectors Matter Antimatter

19 Silicon Tracker: 9 planes, 200,000 channels The coordinate resolution is 10 microns K side 0.11 mm pitch Construction: Mechanical: 50 engineers 3 yrs Electronics: 10 yrs at CSIST

20 MAGNET 1 Tracker: coordinate resolution 10 m de/dx: identify nuclei 2 Test Beam TRD TOF Test Beam TOF RICH ECAL S

21 Tracker Alignment System accuracy: 3 m with 20 UV lasers 1080 nm 21

22 Transition Radiation Detector (TRD)

23 Transition Radiation Detector: identifies Positrons and Electrons 9,000 Straw Tubes Manufactured 5,248 tubes selected from 9,000, 2 m length centered to 100 m, verified by CAT scanner Life time: ~20 years in Space p/e + rejection: Test Beam (400GeV): >10 2 In Space: > de/dx: identifies nuclei (He.)

24 Ring Imaging Cherenkov (RICH) Cherenkov radiation Particle Charge Velocity Velocity Cherenkov Radiator Conical Reflector Photodetectors Electric Charge 24

25 160 GV He Li C 10,880 photosensors to identify nuclei and their energy 25 O Ca

26 On the ISS, AMS will measure the composition of high energy Cosmic Rays with extraordinary accuracy Test results from accelerator Charge of Nuclei 26

27 Calorimeter (ECAL) A precision, 17 X 0, 3-dimensional measurement of the directions and energies of light rays and electrons Lead foil (1mm) e Fibers (f1mm) σ(e) 10.6±0.1 = E E +(1.25±0.03)% Test Beam Results fibers, f = 1 mm distributed uniformly Inside 600 kg of lead

28 AMS electronics 650 computers, 300,000 channels, up to 400% redundancy Fast: 10 x the commercial space electronics Accurate: measure coordinate to 10 microns Linear: 1 in 10 5, 10 MeV to 1 TeV Electronics fabricated in Taiwan, under NASA supervision MIT

29 AMS-02: Subdetector Qualification Test CSIST, NSPO (Taiwan): Electronics modules AACHEN (Germany): TRD and electronics crates INTA (Spain): RICH and electronics crates SERMS (Italy): TOF, TRK, ECAL and electronics crates Aachen (Germany) INTA (Spain) SERMS (Italy) CSIST / NSPO (Taiwan) 29

30 lectromagnetic Dedicated Space Qualification Facilities have been developed for AMS in Italy Vibration Radiation Radiation Thermal Thermal- Vacuum

31 Vibration tests of Flight Model Time of Flight

32 2009: AFTER 9000 hrs of TVT THE END OF SUB-SYSTEMs SYSTEMs TESTS

33 AMS in the ESA Electromagnetic Interference (EMI) Chamber, March 2010, ESTEC, Noordwijk, Netherlands

34 AMS in the ESA TVT Chamber, April 2010, ESTEC Duration 330hours P < 10-6 mbar Ambient temperature from -90 o C to +40 o C

35 Test at CERN AMS in accelerator test beam Feb 4-8 and Aug 8-20, 2010 AMS 7 km 27 km CERN Accelerator Complex

36 AMS in Test Beam 8-20 Aug 2010, CERN

37 N Test Beam Results 8-20 Aug 2010, CERN N Velocity measured to an accuracy of 1/1000 for 400 GeV protons N Bending Plane Residual (cm) e ± Energy Resolution: 2.5-3% Reconstructed Velocity/c Energy TRD: 400 GeV protons

38 Arrival of the AMS C5 at Geneva 25 Aug 2010

39 AMS mated with the Payload Attach System simulator during Space Station interface verification test KSC, October 22, 2010

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41 Transport of Space Shuttle to the Vehicle Assembly Building Installation of Space Shuttle onto External Tank and Solid Rocket Boosters

42 Transfer of STS-134 to the launch pad

43 AMS in the Payload Bay of Endeavour ready for launch

44 Closing Endeavour s Payload Bay Doors at the Launch Pad

45 May 16, 2011, 08:56 AM Total weight: AMS weight: 2008 t 7.5 t

46 After 123 seconds, 1,000 tons of fuel is spent.

47 Endeavour approaching the Space Station, May 18, 2011

48 AMS is grappled by the Shuttle Arm May 19, 2011

49 May 19: AMS installation completed at 5:15 AM. Data taking started at 9:35 AM

50 AMS Payload Operation and Control Center, JSC

51 AMS AMS Operations Astronaut at ISS AMS Laptop TDRS Satellites Flight Operations Ground Operations Ku-Band High Rate (down): Events <10Mbit/s> S-Band Low Rate (up & down): Commanding: 1 Kbit/s Monitoring: 30 Kbit/s AMS Payload Operations Control and Science Operations Centers (POCC, SOC) at CERN AMS Computers at MSFC, AL White Sands Ground Terminal, NM

52 Thermal Control is the most challenging task in the operation of AMS 52

53 TRD Pump temperature Thermal variables: ISS Radiator positions ISS attitude changes (primarily for visiting vehicles) Visiting Vehicles (Soyuz or Progress) STBD Main Radiator parked at -8 o 3 Sep STBD Main Radiator moved from -8 o to +25 o 4 Sep, 2011

54 Thermal variables: Solar Array positions Solar Array

55 Tracker AMS Flight Electronics for Thermal Control Over 1,100 temperature sensors and 298 heaters are monitored in the AMS POCC to assure components stay within thermal limits and avoid permanent damage. TRD 24 Heaters 8 Pressure Sensors 482 Temperature Sensors 1 TOF & ACC 64 Temperature Sensors Silicon Tracker 4 -Pressure Sensors 32 Heaters 142 Temperature Sensors Magnet 68 Temperature Sensors 9 ECAL 80 Temperature Sensors 30 o 20 o ECAL Temperature RICH 96 Temperature Sensors 10 o 0 o C -10 o

56 Temperature/ o C AMS Tracker on ISS Stability of the temperature of Tracker planes 5 and 6 over 4 months /08/ /10/ /11/ /12/ /02/2012

57 Alignment (μm) N AMS Tracker on ISS The alignment stability (3 microns) of the uppermost Tracker plane L1 L1 Over 150 days. Alignment stability (3 (μ) Day (2011) L2 L3,4 L5,6 L7,8 Alignment (μm) L9

58 AMS TRD on ISS Due to temperature variations the TRD is moving on top of the inner tracker by up to 1 mm. We use protons for alignment to an accuracy of 0.04 mm for each straw module. before Alignment TRD after Alignment 58

59 AMS TRD on ISS Due to temperatue, pressure, gas composition and HV changes the TRD detector response is changing We use cosmic ray protons to calibrate the detector response to 3% accurary. before calibration before Calibration after calibration after Calibration 59

60 Orbital DAQ parameters Acquisition rate [Hz] Time at location [s] DAQ efficiency Particle rates vary from 200 to 2000 Hz per orbit On average: DAQ efficiency 85% DAQ rate ~700Hz

61 AMS SOC: Data Processing Reconstructed data are available in average less than 3 hrs after flight data arrived at POCC

62 The INFN Computing center Master Copy of the AMS Raw Data Data reprocessing Montecarlo Production 62

63 AMS collected over 20 billion events Events collected Events reconstructed First year of AMS operations

64 e + /( e + + e ) The physics of AMS include: The Origin of Dark Matter The leading candidate for Dark Matter is a neutralino ( 0 ) Collisions of 0 will produce excess in the spectra of e + different from collisions of cosmic rays AMS data on ISS e + Energy [GeV] 1 TeV

65 e + /(e + + e - ) Detection of High Mass Dark Matter from ISS AMS-02 m =800 GeV m =200 GeV m =400 GeV e+ Energy (GeV) AMS data on ISS

66 AMS data on high energy e ± : 1.03 TeV electron front view side view TRD: identifies electron Tracker and Magnet: measure momentum RICH charge of electron ECAL: identifies electron and measures its energy 66

67 AMS TRD on ISS

68 Rejection AMS ECAL on ISS ECAL rejection (E/P>0.5)

69 front view AMS data: High energy e ± 369 GeV Positron 205 GeV Positron front view front view 388 GeV Positron front view 424 GeV Positron

70 Experimental work on Antimatter in the Universe Direct search Search for Baryogenesis New CP BELLE BaBar (sin 2β= 0.672±0.023 consistent with SM) FNAL KTeV (Re(ε / ε) = (19.2±2.1)*10-4 ) CERN NA-48 CDF, D0 Proton decay Super K (τ p > 6.6 * years ) AMS Increase in sensitivity: x Increase in energy to ~TeV LHC-b ATLAS CMS y06k299a

71 Geomagnetic AMS data field on ISS: He rate Earth magnetic field bends charged particles in 1st approx. dipolar B si n 2 λ cos 6 λ (G) (at 370 Km) λ geomag polar angle wrt magn equator Geomagnetic Cutoff minimal particle Rigidity (R = Pc )to reach ze anearearthpoint Polar region Solar Flare, 24/1/2012 Quiet period R c = 60 GV 1+ h R E 2 cos 4 λ (1 + cosα cos 3 λ) 1/ East-West assymetry maximal in magnetic equator IDPASC (Sesimbra), 18 December 2010 F.Barao (27) 10 3

72 AMS data: He rate and Solar Flare Polar region Solar Flare, 24/1/2012 Quiet period Equatorial region

73 Φ (m -2 sr -1 GeV -1 ) Physics of AMS: Nuclear Abundances Measurements For energies from 100 MeV to 1 TeV with 1% accuracy over the 11-year solar cycle. These spectra will provide experimental data that go into calculating the background in the Search for Dark Matter, i.e., p + C e +,

74 AMS RICH on ISS: Z = 7 (N) P = TeV/c Z = 10 (Ne) P = TeV/c Nuclei in the TeV range Z = 13 (Al) P = TeV/c Z = 14 (Si) P = TeV/c Z = 15 (P) P = TeV/c Z = 16 (S) P = TeV/c Z = 19 (K) P = TeV/c Z = 20 (Ca) P = TeV/c Z = 21 (Sc) P = TeV/c Z = 22 (Ti) P = TeV/c Z = 23 (V) P = TeV/c Z = 26 (Fe) P = TeV/c

75 AMS Data from RICH, Tracker and TOF on ISS TOF Z Z Si Al Mg Na Ne F O N C B Be Li Z He AMS de/dx data from Tracker, TOF, TRD and ECAL together with photon counting from RICH will provide more accurate separation

76 First Year Data from AMS and detector performance The detectors function exactly as designed, we have collected over 20 billion events. Every year, we will collect 16*10 9 events and in years we will collect *10 9 events. This will provide unprecedented sensitivity to search for new physics.

77 During 100 years of Cosmic rays studies

78 The Cosmos is the Ultimate Laboratory. Cosmic rays can be observed at energies higher than any accelerator. The most exciting objective of AMS is to probe the unknown; to search for phenomena which exist in nature that we have not yet imagined nor had the tools to discover.