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1 Recent&results&from&the&Alpha&Magne4c& Spectrometer&(AMS)&Experiment&& on&the&interna4onal&space&sta4on Federico Pilo - INFN Pisa Vulcano, May 19 th 2014
2
3 3 Experimental Challenges Search for Dark Matter χ + χ e + +. Signal/background=e + /p< 1/10 4 background rejection > 10 6 P e - e + Cosmic Rays Flux Ref: B Beischer et al 2009 New J. Phys P
4 A Large Magnetic Spectrometer in Space : a game changing for the study of Cosmic Ray L. Baldini "
5 AMS International Collaboration 16 Countries, 60 Institutes and 600 Physicists USA MIT - CAMBRIDGE NASA JOHNSON SPACE CENTER TEXAS A&M UNIVERSITY UNIV. OF HAWAII 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 SWITZERLAND ETH-ZURICH UNIV. OF GENEVA 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 TRENTO GERMANY RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE RUSSIA I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. ROMANIA ISS UNIV. OF BUCHAREST TURKEY METU CHINA BISEE (Beijing) IEE (Beijing) IHEP (Beijing) NLAA (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) KOREA EWHA KYUNGPOOK NAT.UNIV. TAIWAN SDU (Jinan) ACAD. SINICA (Taiwan) AIDC (Taiwan) CSIST (Taiwan) NCU (Chung Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu) DOE sponsored experiment, NASA space operation 95% construction from Europe and Asia
6 AMS: A TeV precision, multipurpose spectrometer TRD Identify e +, e - TOF Z, β Silicon Tracker Z, P 1 TRD! TOF! Tracker! Magnet ±Z ECAL E of e +, e -, γ TOF! RICH! 9 ECAL! RICH Z, β
7 Sensitive Search for the origin of Dark Matter with p/e + >10 6 p Tracker Entry TRD! TRD: P e + rejection >10 2 TOF! e + p TOF! RICH! e + Tracker! 0.50 X 0 Tracker Total ECAL! ECAL: P e + rejection >10 4 Tracker Exit a) Minimal material in the TRD and TOF So that the detector does not become a source of e +. b) A magnet separates TRD and ECAL so that e + produced in TRD will be swept away and not enter ECAL In this way the rejection power of TRD and ECAL are independent c) Matching momentum of 9 tracker planes with ECAL energy measurements
8 AMS Flight Electronics for Data Acquisition (DAQ) TRD: 5248 Signals 300,000 channels at 2 KHz, 650 computers designed and built by AMS TOF & ACC: 88 Signals Silicon Tracker: 196,608 Signals 1 TRD! TOF! TOF! RICH! Tracker! Magnet ECAL: 2,916 Signals 9 ECAL! RICH: 10,800 * 2 Signals
9 TRD 24 Heaters 8 Pressure Sensors 482 Temperature Sensors AMS Flight Electronics for Thermal Control 1118 temperature sensors, 298 heaters 1 TOF & ACC 64 Temperature Sensors TRD! Silicon Tracker 4 -Pressure Sensors 32 Heaters 142 Temperature Sensors TOF! TOF! RICH! 9 ECAL! Tracker! Magnet 68 Temperature Sensors ECAL 80 Temperature Sensors RICH 96 Temperature Sensors
10 Proton rejection at 90% e + efficiency TRD performance on ISS Rigidity (GV)
11 Events Time of Flight System Measures Velocity and Charge of particles Data from ISS" x10 3 x10 " 3 Z=2 σ β =2%% σ Time =80ps% Events Z=6 σ β =1.2 % σ Time =48ps% Velocity [Rigidity>20GV] Velocity [Rigidity>20GV] H& He& Li& Be& B& C& Plane 4 N& O& F& Ne& Na& Mg& Al& Si& P& S& Cl& Ar& Ca& 3, K& 4 Ti& Sc& V& Mn& Fe& Cr& Ni& Zn&
12 Alignment"accuracy"of"the"9"Tracker"layers"over"18"months"
13 RICH - Detector performance on ISS Z&=&7&(N)& P&=&2.088&TeV/c&& Z&=&10&(Ne)& P&=&0.576&TeV/c&& Z&=&13&(Al)& P&=&9.148&TeV/c&& Z&=&14&(Si)& P&=&0.951&TeV/c&& Z&=&15&(P)& P&=&1.497&TeV/c&& Z&=&16&(S)& P&=&1.645&TeV/c&& Z&=&19&(K)& P&=&1.686&TeV/c&& Z&=&20&(Ca)& P&=&2.382&TeV/c&& Z&=&21&(Sc)& P&=&0.390&TeV/c&& Z&=&22&(Ti)& P&=&1.288&TeV/c&& Z&=&23&(V)& P&=&0.812&TeV/c&& Z&=&26&(Fe)& P&=&0.795&TeV/c&&
14 ECAL Performance σ(e)/e = 10.4/ E %
15 Data from ISS: Proton rejection using the ECAL 15
16 Intensive Beam Tests at CERN AMS Particle Momentum (GeV/c) Positions Purpose Protons ,650 Full Tracker alignment, TOF calibration, ECAL uniformity Electrons 100, 120, 180, each TRD, ECAL performance study Positrons 10, 20, 60, 80, 120, each TRD, ECAL performance study Pions 20, 60, 80, 100, 120, each TRD performance to 1.2 TeV
17 17 May 16 th,, 2011 May 16, 2011
18 AMS today
19 AMS Operations TDRS Satellites White Sands, NM 24 hours x 365 days x years Payload Operations Control Center at CERN
20 AMS Physics results
21 Physics results (ICRC 2013) 1. e + /(e +& +&e V &)&ra4o&and&anisotropy& 2. Proton&spectrum& 3. Helium&spectrum& 4. Electron&Spectrum& 5. Positron&Spectrum& 6. All&electron&spectrum& 7.&BoronVtoVCarbon&ra4o&
22 Physics of Positron Fraction: e + /(e + + e - ) M. Turner and F. Wilczek, Phys. Rev. D42 (1990) 1001; J. Ellis, 26th ICRC Salt Lake City (1999) astro-ph/ ; H. Cheng, J. Feng and K. Matchev, Phys. Rev. Lett. 89 (2002) ; S. Profumo and P. Ullio, J. Cosmology Astroparticle Phys. JCAP07 (2004) 006; D. Hooper and J. Silk, Phys. Rev. D 71 (2005) ; E. Ponton and L. Randall, JHEP 0904 (2009) 080; G. Kane, R. Lu and S. Watson, Phys. Lett. B681 (2009) 151; D. Hooper, P. Blasi and P. D. Serpico, JCAP (2009) ; B2 Y Z. Fan et al., Int. J. Mod. Phys. D19 (2010) 2011; M. Pato, M. Lattanzi and G. Bertone, JCAP 1012 (2010) 020. Positron"fracIon" 0.1" χ + χ e +. mχ=400 GeV mχ=800 GeV Collision&of&Cosmic&Rays& Dark"Ma<er"model"based"on"I."Cholis"et"al.,"arXiv: "" 10& 10 2& e ± Energy [GeV] "
23 front view In the first 1.5 years in space, AMS has collected over 25 billion events. 6.8 million are electrons or positrons. Electron&E=982&GeV& Positron&E=636&GeV& Run/Event / Run/Event / side view front view side view
24 TRD performance on ISS TRD estimator = -ln(p e /(P e +P p )) Probability electron proton Normalized probabilities P e and P p ISS: GeV TRD estimator
25 Separa4on&of&protons&and&electrons&with&ECAL&& Boosted Decision Tree, BDT: 19 variables describing 3D shower shape combined (B.Roe et al., NIM A543 (2005) 577) ISS data: GeV protons ε e = 90% electrons
26 Results of the fit: he TRD Estimator shows clear separation between protons and positrons with a small charge confusion background Events TRD Estimator ( GeV) positrons protons
27 First Result from the AMS on the ISS: Precision Measurement of the Positron Fraction in Primary Cosmic Rays of GeV Selected for a Viewpoint in Physics and an Editors Suggestion [Aguilar,M. et al (AMS Collaboration) Phys. Rev. Lett. 110, 1411xx (2013)]
28 AMS-02 (6.8 million e +, e events) The positron fraction is steadily increasing from 10 to ~250 GeV From 20 to 250 GeV, the slope decreases by an order of magnitude No structure in the spectrum Positron fraction
29 8% of total Data to 2028 Positron fraction A new phenomenon has occurred e ± energy [GeV]
30 Physics&Example:&Comparing&data&with&a&minimal&model.& Positron fraction Φ e + && =&C e + & Ε γ e+ &+&C s Ε γ s&e VE/E s&& & Φ e V & %=&C e V & Ε γ ev &+&C s Ε γ s&e VE/E s%! Data Fit to Data with Model χ 2 /d.f.%=&28.5/57 e ± energy [GeV] & The"agreement"between"the"data"and"the"model"shows"that"the" positron"fracion"spectrum"is"consistent"with"e ±!fluxes"each"of"which"is" the"sum"of"its"diffuse"spectrum"and"a"single"common"power"law"source.""
31 A&fit&to&the&data&in&the&energy&range&1&to&350&GeV&yields:& & γ ev % %γ e+ &=& 0.63&±&0.03,"i.e.,"the"diffuse"positron"spectrum"is"less" energeic"than"the"diffuse"electron"spectrum" $ γ& ev % &γ& S %%=&0.66±0.05,"i.e.,"the"source"spectrum"is"more"energeIc"than" the"diffuse"electron"spectrum" & C e+& /C ev& =&0.091&±%0.001,"i.e.,"the"weight"of"the"diffuse"positron"flux" amounts"to" 10%"of"that"of"the"diffuse"electron"flux" " C S& /C ev& %=&0.0078&±%0.0012,"i.e.,"the"weight"of"the"common"source" consitutes"only" 1%"of"that"of"the"diffuse"electron"flux" " 1/Ε s %=&0.0013&±%0.0007&GeV 1,"" """""""""""corresponding"to"a"cutoff"energy"of" % GeV." V280&
32 Bergstrom,Bringmann,Cholis,Hooper,Weniger 2013 Also : Ibarra,Lamperstorfer,Silk 2013
33 Positron fraction Cutoff energy = DM Mass 700 GeV DM model Pulsar model Background in 10 years from now e ± energy [GeV] What will the Positron Fraction look like at high energy? 33
34 34 Comparison of p/p with Models in 10 more years Ref:&Donato&et&al.,&PRL&102,&071301&(2009)&
35 We now understand the systematic errors to ~1%. Studies with 1% statistical error will take time to collect the data.
36 Physics analysis nearing completion 1. An4protons&(0.5V300&GeV)& 2. 8 &He&events)& & 3. Ion&fluxes& 4. Solar&physics&& 5..&
37 The Cosmos is the Ultimate Laboratory Cosmic rays can be observed at energies higher than any accelerator With AMS-02 on the ISS we have entered the era of precision Cosmic Ray physics to search for phenomena which exist in nature but we have not yet imagined nor had the tools to discover
38 SPARE SLIDES
39 Deviation from 1997 measurements in R-Phi coordinates, Z=0
40 AMS in SPS Test Beam, 2010 Particle Momentum (GeV/c) Positions Purpose Protons ,650 Full Tracker alignment, TOF calibration, ECAL uniformity Electrons 100, 120, 180, each TRD, ECAL performance study Positrons 10, 20, 60, 80, 120, each TRD, ECAL performance study Pions 20, 60, 80, 100, 120, each TRD performance to 1.2 TeV
41 May 16, 2011
42 Data analysis in AMS (2 years of data) AMS is a very precise particle physics detector. Precision physics results require attention to detail and a large analysis effort. The data are analysed by two independent AMS international teams. Group A Example: the positron fraction paper Group α B. Bertucci V. Choutko A. Kounine J. Berdugo S. Schael M. Incagli S. Rosier-Lees S. Haino, A. Oliva J. Casaus, P. Zuccon A. Contin
43 AMS Nuclei Measurement on ISS
44
45 " 45
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