Primary Cosmic Rays : what are we learning from AMS
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1 Primary Cosmic Rays : what are we learning from AMS Roberto Battiston University and INFN-TIFPA of Trento HERD Workshop IHEP-Beijing December
2 Agile Fermi PAMELA AMS Direct study of the HESS MAGIC ARGO cosmic Borexino ICARUS LVD AUGER TA radiation ICECube ANTARES KM3net
3 Space experiments reach outstanding accuracy using primary radiation 3
4 AMS today
5 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 Tracker ECAL E of e +, e -, γ 9 RICH Z, E Z, P are measured independently by the Tracker, RICH, TOF and ECAL
6 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
7 Data from ISS Nuclei in the TeV range Z = 7 (N) P = TeV/c Z = 10 (Ne) P = TeV/c 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
8 front view Boron Rigidity=3.7 GV Z TRK_L1 =5.3 Rigidity 3 GV Carbon Rigidity=3.3 GV Run/Event / Run/Event / side view front view Z TRK_L1 =6.4 side view Z TRD =5.1 Z TOF_UP =5.1 Z TRD =5.9 Z TOF_UP =6.1 Z TRK_L2-L8 =4.9 Z TRK_L2-L8 =6.1 Z TOF_LOW =4.9 Z TOF_LOW =6.1 Z RICH =5.1 Z RICH =5.9 Z TRK_L9 =5.0 Z TRK_L9 =6.5
9 Boron Rigidity=24 GV Rigidity 20 GV Carbon Rigidity=24 GV Run/Event / Run/Event / front view Z TRK_L1 =4.7 side view front view Z TRK_L1 =6.0 side view Z TRD =4.9 Z TRD =5.9 Z TOF_UP =5.1 Z TOF_UP =6.0 Z TRK_L2-L8 =4.9 Z TRK_L2-L8 =5.9 Z TOF_LOW =5.0 Z TOF_LOW =6.0 Z RICH =4.8 Z RICH =6.2
10 Boron Rigidity=187 GV Rigidity 200 GV Carbon Rigidity=215 GV front view Run/Event / Run/Event / Z TRK_L1 =4.9 Z TRD =4.5 side view front view Z TRK_L1 =6.1 Z TRD =5.9 side view Z TOF_UP =5.0 Z TOF_UP =5.9 Z TRK_L2-L8 =4.9 Z TRK_L2-L8 =5.8 Z TOF_LOW =5.1 Z TOF_LOW =5.8 Z RICH =5.2 Z RICH =6.1
11 Boron Rigidity=680 GV Rigidity 700 GV Carbon Rigidity=666 GV Run/Event / Run/Event / front view Z TRK_L1 =5. 2 side view front view Z TRK_L1 =5.8 side view Z TRD =5.2 Z TRD =6.0 Z TOF_UP =5.5 Z TOF_UP =6.1 Z TRK_L2-L8 =5.0 Z TRK_L2-L8 =6.0 Z TOF_LOW =5.4 Z TOF_LOW =6.5 Z RICH =4.8 Z RICH =6.1 Z TRK_L9 =5.1 Z TRK_L9 =6.1
12 Carbon Fragmentation to Boron in Upper TOF Rigidity 10.6 GV Z TRK_L1 =6.1 Z TRD =6.0 Z 0 =9.9 Z 1 =5.3 Z TRK_IN =4.8 Z TOF_LOW =5.2 Z RICH =5.1
13 Electron E=1.1 GeV Positron E=1.1 GeV Run/Event / Run/Event / front view side view front view side view
14 Electron E=10.1 GeV Positron E=9.5 GeV Run/Event / Run/Event / front view side view front view side view
15 front view Electron E=99 GeV Positron E=100 GeV Run/Event / Run/Event / side view front view side view
16 Electron E=982 GeV Positron E=636 GeV Run/Event / Run/Event / front view side view front view side view
17 8% of total Data to 2028 Positron fraction A new phenomena has occurred e ± energy [GeV]
18 Interpretation of the AMS e+ fraction: - DM - Pulsars - Something else 18
19 Physics Example: Comparing data with a minimal model. Positron fraction Φ e + = C e + Ε γ e+ + C s Ε γ s e -E/E s Φ e - = C e - Ε γ e- + C s Ε γ s e -E/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 fraction spectrum is consistent with e ± fluxes each of which is the sum of its diffuse spectrum and a single common power law source.
20 A fit to the data in the energy range 1 to 350 GeV yields: γ e- γ e+ = 0.63 ± 0.03, i.e., the diffuse positron spectrum is less energetic than the diffuse electron spectrum; γ e- γ S = 0.66±0.05, i.e., the source spectrum is more energetic than the diffuse electron spectrum; C e+ /C e- = ± 0.001, i.e., the weight of the diffuse positron flux amounts to 10% of that of the diffuse electron flux; C S /C e- = ± , i.e., the weight of the common source constitutes only 1% of that of the diffuse electron flux; 1/Ε s = ± GeV 1, corresponding to a cutoff energy of GeV.
21 Bergstrom,Bringmann,Cholis,Hooper,Weniger 2013 Also : Ibarra,Lamperstorfer,Silk 2013
22
23 Sensitivity of minimal model to cutoff E s E s (GeV)
24 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? 24
25 25 Comparison of p/p with Models in 10 more years Ref: Donato et al., PRL 102, (2009)
26 26
27 Selected events are grouped into 5 cumulative energy bins: , , , and GeV. Their arrival directions are used to build sky maps in galactic coordinates, (b,l), containing the number of observed positrons and electrons North Galactic Pole (90 lat.) Solar System South Galactic Pole (-90 lat.) North-South direction East-West direction Forward-Backward direction Galactic C
28 The relative fluctuations of the positron ratio, e + /e -, across the observed sky map show no evident pattern Significance ( )
29 The amplitudes of spherical harmonic contributions at fixed angular scale,, are fit to data for dipole ( =1), quadrupole ( =2) and octopole ( =3) The fit amplitudes,, are found to be consistent with the hypothesis of isotropy at all energies and angular scales
30 AMS upper limits on at the 95% CL <0.030 for 16<E<350GeV No seasonal excess is observed and same results are obtained using solar ecliptic coordinates
31 AMS Electron Spectrum
32 AMS Positron Spectrum
33 16% E pulsar E e+e- conversion efficiency Cholis,Hooper 2013
34 The Vela supernova remnant The Vela pulsar The Crab pulsar Sources of very high energy cosmic-ray electrons? 38
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40 AMS Electron plus Positron Spectrum
41 (Electron plus Positron) Spectrum comparison with recent measurements
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44 Open issues: the electron + positron spectrum above 100 GeV AMS O(1 TeV ) AMS (2013)
45
46 Cholis,Hooper 2013
47 Cholis,Hooper 2013
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49 54
50 Beware changing energy scale AND detector technique?
51 Anti-matter & Exotic sources (DM?) The electron bump? No bump in Fermi, AMS, PAMELA No fresh source of anti-p up to 100 GeV Positron excess reaching maximum 56
52 A structure around 135 GeV? Fermi data on a possible gamma line 57
53 15 years of space astroparticle physics, leave us with a number of hot issues : Electron/positrons ratio vs spectra Gamma rays line? CR spectral change? B/C spectral change? Pbar at higher energy 58
54 Scientific Objectives of future e/γ missions in space High energy particle detection in space Search for Dark Matter signatures Study of cosmic ray spectrum and composition High energy gamma astronomy Follow-up mission to both Agile Fermi/LAT and Pamela AMS-02 Extend the energy reach to the TeV region, providing better resolution Overlap with CTA on gamma ray astronomy Run in parallel for some time 59
55 What Nature gives us What From L. Baldini, SpacePart 2012
56 Expected rates detection tools/limitations ELECTRON AND POSITRON 5 sqm sr yr 5 m2 sr 3,14E+07 s/y ACCESSIBLE EXCLUDED EXCLUDED ev 10^8 10^9 10^10 10^11 10^12 10^13 10^14 10^15 scale 100MeV GV TV PV Integral. 1/y.@ 0,1-1.@ 1-10.@ @ @ >.@ >.@ >.@ > e- 4,99E+10 3,11E+09 1,56E+08 9,33E+05 7,78E+03 7,78E+01 7,78E-01 7,78E-03 e+ 2,50E+09 1,56E+08 1,56E+07 1,40E+05 1,17E+03 1,17E+01 1,17E-01 1,17E-03 Detectors tracker, TOF, TRD, ECAL tracker, TOF, TRD, ECAL Tracker, TRD, ECAL Tracker, TRD, ECAL Tracker,SRD,ECAL Tracker,SRD,ECAL Variables R, beta, gamma, energy R, beta, gamma, energy R, gamma, energy R, gamma, energy R,Energy, Syncrotron Radiation R, Energy, Synchroton Radiation Physics Van Allen, solar, subcutoff solar, geomagnetic, galactic DM, galactic, asymmetries DM, galactic, asymmetries DM, galactic DM, galactic, moon shadow, sun shadow DM, galactic DM, extragalactic, knee acceptance vs R, live time, efficiency, MC, inner tracker, alignement, TOF calibration, TRD acceptance vs R, live time, efficiency, MC, inner tracker, alignement, TOF calibration, TRD acceptance vs R, live time, efficiency, MC, inner tracker, alignement, TOF calibration, TRD acceptance vs R, live time, efficiency, MC, inner/outer tracker, TRD, alignement, acceptance vs R, live time, efficiency, MC, outer tracker, alignement, SRD calibration, ECAL acceptance vs R, live time, efficiency, MC, tracker, alignement, SRD calibration, ECAL calibration, backtracing calibration, backtracing calibration, backtracing backtracing (Earth- calibration, backtracing calibration, backtracing Tools (near Earth) (near Earth) (near Earth) Moon, Earth- Sun) Earth-Moon, Earth-Sun Earth-Moon, Earth-Sun Background e p p p p p Background e+ p p p p p p p p Limitations multiple, scattering, acceptance,ams02 magnetic field - SRD Acceptance, MDR Tracker, ECAL must be in accceptance 61 SRD acceptance, MDR Tracker, ECAL must be in accceptance no statistics no statistics
57 Expected rates and detection tools/limitations PROTON and HELIUM 5 sqm sr yr 5 m2 sr 3,14E+07 s/y ACCESSIBLE ACCESSIBLE ACCESSIBLE 10^8 10^9 10^10 10^11 10^12 10^13 10^14 10^15 100MeV GV TV PV Integral. 1/y.@ 0,1-1.@ 1-10.@ @ @ >.@ >.@ >.@ > p 4,99E+10 9,96E+10 1,99E+10 3,97E+08 7,19E+06 1,44E+05 2,86E+03 5,71E+01 He 1,80E+09 1,79E+10 3,58E+09 7,14E+07 1,29E+06 2,58E+04 5,15E+02 1,03E+01 Detectors tracker, TOF, RICH Tracker, (RICH) Tracker Tracker Tracker Tracker+ HCAL Tracker+ HCAL Tracker+ HCAL Variables R, beta R R R R R, Energy Energy Energy Physics Van Allen, solar, subcutoff solar, geomagnetic, galactic galactic galactic galactic, moon shadow, sun shadow galactic, moon shadow, sun shadow galactic extragalactic, knee acceptance vs R, live time, efficiency, MC, inner tracker, alignement, TOF calibration, RICH acceptance vs R, live time, efficiency, MC, inner tracker, alignement,, RICH acceptance vs R, live time, efficiency, MC, inner tracker, alignement, TOF calibration, RICH acceptance vs R, live time, efficiency, MC, inner/outer tracker, acceptance vs R, live time, efficiency, MC, outer tracker, alignement,, ECAL acceptance vs R, live time, efficiency, MC, tracker, alignement, HCAL calibration, calibration, calibration, backtracing calibration, backtracing alignement, backtracing calibration, backtracing backtracing Earth- Tools backtracing(near Earth) (near Earth) near Earth) Earth-Moon, Earth- Sun) Earth-Moon, Earth-Sun Moon, Earth- Sun Background p Background He He3/He4 He3/He4 He3/He4 He3/He acceptance vs R, live time, efficiency, MC, tracker, alignement, HCAL calibration, backtracing Earth-Moon, Earth- Sun HCAL calibration, backtracing Earth-Moon, Earth- Sun Limitations multiple, scattering, acceptance,ams02 magnetic field - - different tracker acceptances, alignement MDR MDR+ HCAL HCAL HCAL 62
58 Interesting spectra fall with E -3 Increasing one decade (e.g constant statistics would require O(100) time more collection power Cp = S * Ω * t O(100) times this explain AMS-02/Pamela 400 Fermi/ (Agile or EGRET) 20
59 while maintaining Particle Identification and Charge sign and Energy resolution
60 How to reach O(100) higher Cp? S from O(1) m 2 to O(10)m 2 10 Ω from 1 sr to 10 sr 10 t from 5 to 20 years 4 Cp = S * Ω * t 400 times all the parameters should be increased at the same time
61 Need for redundant, accurate measurement in space
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64 Future e/hadron/γ experiments CALET ISS-CREAM DAMPE (INFN participation) GAMMA-400 (INFN participation) HERD (INFN interest and preliminary discussions) + JEM-EUSO (INFN participation to prepartory phase) + possible next generation large acceptance, precision magnetic spectrometer
65 Conclusions Direct measurements of Cosmic Radiation in the 100 GeVmulti TeV scale could reveal fundamental phenomena which cannot be accessed by ground based accelerator physics It is a challenging but rewarding field, requiring large, accurate, experiments, operating for long period in space Accurate measurement of charge and energy are needed INFN will continue to work in this field, exploiting the large investments which have been made, with the goal of maximizing the science return followoing a strategy which, in the medium to long term, could lead to second generation experiments which would be able to fully address CR physics at the multi TeV scale
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