Latest AMS Results - DSU 2019 - Buenos Aires, ArgentinaAMS-02 Collaboration CIEMAT, Madrid (Spain)...
Transcript of Latest AMS Results - DSU 2019 - Buenos Aires, ArgentinaAMS-02 Collaboration CIEMAT, Madrid (Spain)...
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Latest AMS Results
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J. BerdugoOn behalf of the
AMS-02 Collaboration
CIEMAT, Madrid (Spain)
Buenos Aires, Argentina
15-19 July 2019
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The physics of AMS on the Space Station:Long term precision measurement of Charged Cosmic Rays
Charged cosmic rays have mass. They are absorbed by the Earth’s atmosphere
To measure their charge and momentum requires
a magnetic spectrometer in space.
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Tra
cke
r
1
2
7-8
3-4
9
5-6
Particles and nuclei are defined by their charge (Z) and energy (E ~ p)
Z, P are measured independently by the Tracker, RICH, TOF and ECAL
AMS: A TeV precision, multipurpose spectrometer in space
TRD (e /p)Rej.Fact = 10-2 - 10-3
Silicon Tracker (Z, P) = 5-10 µm
Calorimeter (Ee,g)
(E) = 2-3 %
Time of Flight (Z, b)(t) = 160 ps
Magnet(Q sign)B= .15 T
RICH(b, Z)
(b) ~ 0.1 %
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Ground Tests and CalibrationsSpace Qualification(EMI and TV at ESTEC)
1,762 positions and angles with p, e+, e−, pion beams
from 10 to 400 GeV/c
TVT Chamber: P < 10-9 barAmbient temperature: -90oC to 40oC
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Test Beam at CERN(Calibration)
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D(1/R) [GV-1]
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In 8 years,over 140 billion
charged cosmic rays have been measured by AMS
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AMS Results:
Positrons and electrons fluxes
Nuclei fluxes
Solar physics
AMS installed on the ISSand taking data since9:35 CDT on May 19, 2011
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Positronsfrom Dark Matter
Dark Matter
Dark MatterElectrons
Interstellar Medium
Protons, Helium, …
Supernovae
AMS ResultsCosmic Ray Positrons
Positronsfrom Collisions
Positronsfrom Pulsars
New Astrophysical Sources: Pulsars, …
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TRD(radiation shape)
ECAL(shower shape)
ECAL/Tracker(E/p matching)
e/p Identification
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Positron identification in AMS
Rej.Fact (e /p) = 10-5 - 10-6
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Charge Confusion e±
Simulation
Data
Positron Analysis: Background identification
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Flux of Cosmic Ray Positrons
M. Aguilar et al. Phys. Rev. Lett. 122 (2019) 041102
First 6.5 years of AMS operation
1.9 million positrons up to 1 TeV
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model based on positrons from cosmic ray collisions. Astrophysical Journal 729, 106 (2011)
AMS-02 Data 1.9 million positrons up to 1 TeV
Collisions
M. Aguilar et al. Phys. Rev. Lett. 122 (2019) 041102
Flux of Cosmic Ray PositronsLow energy positrons mostly come from cosmic ray collisions
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Collisions
Source Term
Collisions Source Term
AMS positrons
The positron flux is the sum of low-energy part from cosmic ray collisions
plus a new source at high-energy.
The cutoff energy Es = 810+310 GeV is established
with a confidence of more than 0.9999. –180
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Flux of Cosmic Ray Electrons
First 6.5 years of AMS operation
28.1 million electronsup to 1.4 TeV
M. Aguilar et al. Phys. Rev. Lett. 122 (2019) 101101
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Flux of Cosmic Ray Electrons
First 6.5 years of AMS operation
e+/(e++e-) e++e-
M. Aguilar et al. Phys. Rev. Lett. 122 (2019) 101101
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Electrons from cosmic ray collisions
Flux of Cosmic Ray Electrons
The contribution from cosmic ray collisions is negligible
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Double power law
Electron flux characterization
1. Change of the spectral index with more than 7 sigma significance
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2. At the 5 sigma level the electron flux does not have an Energy Cutoff below 1.9 TeV
E0 = 42.1 GeV
Dg = 0.094 ± 0.014
+5.4- 5.2
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Power law b
Power
law a
and 68% CL
Minimal number of power-law like contributions
Electron flux characterization
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New sources of high energy positrons may also produce
an equal amount of high energy electrons
The electron flux data are consistent both with the existence of a high energy electron source term identical to that of positrons and also with the absence of such a term
Power law+ Positron source term
Power law
c2/d.o.f. = 15.5 / 24
c2/d.o.f. = 15.2 / 24
The Origin of Cosmic Ray Electrons
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Positrons: • Low energy from CR Collisions + New source at high energy• Es = 810 GeV
+310- 180
Electrons: • 2 power law contributions• Es <1.9 TeV excluded at 5
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The Origin of Cosmic Ray Positrons Dark Matter Models
DM self-annihilation would lead to a sharp cutoff in the flux (“kinematic edge”)
(Mass = 1.2 TeV)
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The Origin of Cosmic Ray Positrons
HAWC Coll. Science 17 Nov 2017. Vol. 358, Issue 6365, pp. 911-914 D. Hooper et al. Phys. Rev. D 96, 103013 (Nov 2017)
Pulsars produce and accelerate positrons to high energies.
Astrophysical sources: Pulsar
1. Pulsars may induce an anisotropy in the arrival direction of the particles
2. Pulsars do not produce antiprotons.
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Analysis of the arrival directions of the positrons ingalactic coordinates
The positron flux is found to be consistent with isotropy
AMS Positron cosmic ray anisotropy
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The Origin of Cosmic Ray Positrons
positrons Isotropic Map
C1 is the dipole moment
Amplitude of the dipole anisotropy on positrons for 16 < E < 350 GeVδ < 0.019 (95% C.I.)
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Antiproton data show a similar trend as positrons.
The Origin of Cosmic Ray Positrons
Energy [GeV]
e+
e+
p
p
AMS Antiproton
AMS Positron 2018
Please refer to the forthcoming
AMS publication
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Positrons and electrons by 2024
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Secondary cosmic nuclei (Li, Be, B, …) are produced by the collision of primary cosmic rays and interstellar medium
AMS ResultsPrecision Study of Cosmic Nuclei through the lifetime of ISS
Primary elements (H, He, C, ..., Fe) are produced during the lifetime of stars. They are accelerated by the explosion of stars (supernovae).
Traditionally, there are two prominent classes of cosmic rays
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Cosmic ray propagation is commonly modeled as a diffusion process due to the turbulent magnetic field:
Primary ~ source (R-a ) x propagation (R-d ) ~ R-(a+d)
Secondary ~ source (R-(a+d)) x propagation (R-d ) ~ R -(a+2d)
Secondary/Primary ~ R-d
With the Kolmogorov turbulence model δ = -1/3
Precise measurements of primaries and secondaries rigidity dependence provide key information on propagation and source processes
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Redundant measurement of
the Charge of the particles
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H
He
LiBe
BC
NO
F
NeNa
Mg
Al Si
P SCl Ar
KCa
ScTi
V CrFe
Ni
Mn
Tracker Plane 1
TRD
Upper TOF
Tracker Plane 2-8
Lower TOF
RICH
Tracker Plane 9
Analysed
In progress
Precision Study of Cosmic Nuclei through the lifetime of ISS
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Alignment validation on ISSMeasurement above test beam rigidity
Precision measurements of Cosmic Nuclei fluxes
Tracker alignment at 400 GV test beam
RL1-8
RL2-9
D(1/R) [GV-1]
Main systematic error is due to the uncertainty in the energy scale
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Comparison of the rigidity R measured by the tracker, with the energy E,
measured by the electromagnetic calorimeter, for positron and electron events.
The accuracy of the rigidity scale is found to be 0.033 TV−1,
limited mostly by available positron statistics
Absolute Rigidity Scale
e+ e-
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Measurement of proton spectrum with AMS
×10³ ⦁ AMS300 million protons
) [GeV]K
Kinetic Energy (E
1 10210
310 410
]1
.7G
eV
-1s
ec
-1s
r-2
[m
2.7
K E
´F
lux
0
2
4
6
8
10
12
14
310´
ATIC-02
BESS
CREAM
PAMELA
AMS
CALET
ProtonsATIC-02
BESS
CREAM
PAMELA
AMS
CALET
AMS 2011-2018
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Please refer to the forthcoming
AMS publication
1 billion protons
Proton flux shows a deviation from a single power law above few hundred GV
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Use right-to-left nuclei to measure the nuclear interactions in the TRD+TOF
Use left-to-right nuclei to measure the nuclear interactions in the TOF+RICH
We measured the nuclei survival probability using data acquired when ISS attitude was rotated so that AMS was pointing in a horizontal direction.
Define beams of nuclei: He, C, O, …
TRDTOF
TOFRICH
Unique properties of AMS:
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Atomic Number A
5 10 15 20 25 30 35
Nucle
us +
Ca
rbo
n [
mb
]In
El
s
0.2
0.4
0.6
0.8
1
1.2
1.4
1.6
1.83
10´
AMS
Jaros(1978) 5.8 GV
AMS Nucleus + C Inelastic Cross Section Measurements (5-100 GV Rigidity)
He
C
O
NeMg
S
30
Si
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Primary and secondary Cosmic RaysComparison with earlier measurements
M. Aguilar et al. Phys. Rev. Lett. 120 (2018) 021101 M. Aguilar et al. Phys. Rev. Lett. 119 (2017) 251101
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Primary and secondary Cosmic Rays with AMS
- Above 60 GV, the primary cosmic rays have similar rigidity dependence.
- Secondary cosmic rays Li, Be, and B also have identical rigidity dependence but they are different from primaries
Both deviate from a tradicional single power law above 200 GeV
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Secondary/Primary Flux Ratios = KRΔ
Δ[200-3300GV] – Δ[60-200GV] = 0.13±0.03
20
0 G
V
20
0 G
V
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Support the interpretation of the hardening in terms of a change in the propagation properties in the Galaxy.
Combining the six ratios, the secondary over primary flux ratio (B/C, …),deviates from single power law above 200 GV by 0.13±0.03
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p
C
Fe
He
Cosmic ray production and propagation
Effective propagation distance
∝ R −Δ/2 A−1/3
Effective distance is shown for ~1 GV.
i. Determine Δ from secondary-to -primary ratios
ii. Different nuclei A (1 - 60) probe different distances.
iii.Different rigidities R (1 – 3000 GV) probe different distances
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Understanding the origin, acceleration and propagation of Cosmic rays require the knowledge of the chemical composition over a wide energy range
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[GV]R~
Rigidity
2 3 4 5 10 20 210 210´23
103
10´2
] 1
.7 (
GV
)-1
sr
-1s
-2 [
m2
.7R~
´
Flu
x
50
100
150Oxygen
6.2´Neon5.3´Magnesium
5.8´Silicon30.0´Sulfur
O, Ne, Mg, Si and S Fluxes
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Please refer to the forthcoming
AMS publication
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Please refer to the forthcoming
AMS publication
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Rigidity [GV]
10 2103
10
Flu
x R
ati
o
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
1.3
1.4
0.032´He/O
C/O
The latest AMS Result on the He/O and C/O Flux Ratios
· He/O×0.032
· C/O
(2011-2018)
(2011-2018)
[GV]R~
Rigidity
70 210 210´23
103
10´2
] 1
.7 (
GV
)-1
sr
-1s
-2 [
m2
.7R~
´
Flu
x
1
2
3
43
10´
Helium
30´Carbon
28´Oxygen
Above ~60 GV, the He, C and O spectra have identical rigidity dependence
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Flux Ratio to Oxygen (Ne/O, Mg/O, Si/O, and S/O)
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RΔ1
RΔ2
Ne, Mg, Si
S
O
Δ2≈ Δ1≈-0.035
Please refer to the forthcoming
AMS publication
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AMS 3He/4He flux ratioData collected from May 2011 to Nov 2017 (6.5 y)
Ek: 0.5 GeV/n – 10 GeV/n
100 Million 4He18 Million 3He
Please refer to the forthcoming
AMS publication
Helium are the second most abundant nuclei in cosmic rays. They consist of two isotopes, 4He and 3He.
The 4He is thought to be mainly produced and accelerated in astrophysical sources, while 3He is mostly
produced by the collisions of 4He with the interstellar medium.
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Time (year)
AMS 3He and 4He fluxesMeasurements in 21 time periods of 4 Bartels rotations (108 days) each
Time (year)
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Below 4 GV the 3He/4He flux ratio shows a long-term time dependence in the lowest rigidity bin. Above 4 GV the 3He/4He flux ratio was found to be time independent
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AMS 3He/4He flux ratio
Above 4 GV the 3He/4He flux ratio rigidity dependence is well described by single power law (C RD) with D = -0.294 ± 0.004.
Different from B/0 ratio, which shows a maximum around 4 GV, the 3He/4He flux ratio was found being always decreasing with rigidity below 4 GV as Rd with <d>= 0.21 ± 0.02 and a time dependence of ± 0.05.
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Solar Physics over an 11-year Solar Cycle: 2011 - 2024
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AMS continous measurement of the e+ and e- fluxin the energy range 1 -50 GeV
over 6 years with a time resolution of 27 days.
M. Aguilar et al. Phys. Rev. Lett. 121 (2018) 051102
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The maximum and minimum differ by a factor of ~3.
400
600
800
40
60
80
100 2.15 GV-1.92
300
400
500
600
40
60
80 2.67 GV-2.40
2012 2013 2014 2015 2016 2017
he
liu
m f
lux
[m
sr
sG
V]-1
pro
ton
flu
x [
m s
rs
GV
]-1
•proton •helium
AMS Results on the Identical monthly time variation of the proton and helium fluxes over 6 years
M. Aguilar et al. Phys. Rev. Lett. 121 (2018) 051101
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Solar physics over a complete 11-year solar cycle
AMS will cover a complete solar cycle
reve
rsa
l
reve
rsa
l
•positron
•electron
So
lar
ma
gn
eti
c f
ield
po
lari
ty r
eve
rsa
l
reve
rsa
l
•proton
•helium
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Date
]-1
GV
-1s
-1s
r-2
Flu
x [
m
[1.92 - 2.15] GV
Carbon
Oxygen
1
2
3
4
5
1
2
3
4
5Carbon Oxygen
2012 2014 2016 2018 2020 2022 2024
Solar physics over a complete 11-year solar cycle
Carbon and Oxygen
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Please refer to the forthcoming
AMS publication
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Y
Z
X
anti-Helium event candidate
Momentum = 33.1 ± 1.6 GeV/cCharge = -1.97 ± 0.05Mass = 2.93 ± 0.36 GeV/c2
Mass (3He) = 2.83 GeV/c 2
Date: 2011-269:11:19:32
Anti-Helium Search with AMS
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3He flux models from collisions of cosmic rays
We have also observed two 4He candidates.More events are necessary to ensure that there are no backgrounds.
Kinetic Energy/nucleon
model variationsfactor of ~300
K. Blum et al., Phys. Rev. D 96, 103021 (2017)
There are large uncertainties in models to ascertain the origin of 3HeThe rate of anti-helium is ~1 in 100 million helium.
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Space is the ultimate laboratory. It provides the highest energy particles.
The AMS results contradict current cosmic ray models and require the development of a comprehensive theoretical scheme.
AMS will continue to collect and analyze data for the lifetime of the Space Station.
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