The First Five Years of the Alpha Magne5c Spectrometer on
the Interna5onal Space Sta5on

William Creus
Academia Sinica (Taiwan)/CERN (Switzerland)
AMS collabora5on
Seminar at ICRRJanuary 10th 2017

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AMS Collabora5on

AMS is an interna,onal collabora,on of 16 countries in 4 con,nents.
Data are received by NASA in Houston, and then relayed to the AMS
AMS is an interna,onal collabora,on of 16 countries in 3 con,nents
Payload Opera,ons Control Centre (POCC) at CERN for analysis.
56 ins,tu,ons and 600 physicists

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The Alpha Magne5c Spectrometer (AMS)A TeV precision, mul5purpose spectrometer3

Transi5on Radia5on Detector

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Time of Flight System

5Tracker
AMS is an interna,onal
9 planes,
channelscollabora,onof 16200.000
countries
in 3
The coordinate resolu5on iscon,nents
10 μm
56 ins,tu,ons and 600
physicists

6Ring Imaging Cherenkov

7Electromagne5c Calorimeter8

Beam Tests at CERN

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Launch of AMS-02
ØMay/16/2011ØLast Endeavour ﬂightØTotal weight 2008 tØAMS 7.5 t
ASer 123 seconds,
1,000 t of fuel was spent

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Opera5on and Data link

Ku-Band (down):
Events <10Mbit/s>
S-Band (up & down):
Commanding: 1 Kbit/s
Monitoring: 30 Kbit/s

2011 年White Sands, NMAMS (ISS)

Payload Operations Control
Center (POCC) in Taiwan

TDRS

Payload Operations Control
Center (POCC) at CERN
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AMS in Space

Installed in ISS on 19/May/2011
Star,ng taking data only 4 hours later

In ﬁve years of opera,on on the ISS
AMS has collected more than 90 billions charged cosmic rays

New Physics Results

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Elementary par5cles in Space
There are hundreds of diﬀerent kindsof charged elementary par,cles.
Only four of them,electrons, protons, positrons, and an,protons,
have inﬁnite life,me,so they travel in the Galaxy.
Electrons and positrons have much smaller mass than protons andan,protons, so they lose much more energy in the galac,cmagne,c ﬁeld due to synchrotron radia,on.
AMS

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Before AMS : Electron and Positron spectraØ Large errors and inconsistentØ Create many theore,cal specula,ons

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Physics Results 1: The Electron and Positron ﬂuxes
The electron ﬂux and the positron ﬂux are diﬀerent
in their magnitude and energy dependence

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Physics Results 1: The Electron and Positron spectral indicesØ The electron and positron spectral indices are not constant.
Ø They are diﬀerent in their magnitude and energy dependence16

Search Dark Maaer

17Search Dark Maaer: Strategies
Indirect Detec,on by Annihila,onAMS, Fermi, CALET … (Detectors in Space)
Direct Detec,on by Sca]ering(Detectors in Underground)

XMASS
LUX
DARKSIDEXENON 100
CDMS II…

(Detectors in Colliders)
Detec,on by Produc,on18

Physics Results 2: The origin of the AMS positron spectrum
Ø Collision of Cosmic Rays with the Interstellar Media produce e+Ø Unexpectedly, star,ng from ~8GeV, the AMS e+ data show anexcess above ordinary Cosmic Ray collisions.
Ø Annihila,on of Dark Ma]er produces addi,onal e+ which are characterized
by a sharp drop oﬀ at the mass of dark ma]er.

DM model based on
J. Kopp, Phys. Rev. D 88 (2013) 076013

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Physics Results 3: The origin of the AMS positron frac5on
The excess of the Positron frac,on e+/(e+ + e−) isan alterna,ve way to search for signal of Dark Ma]er

DM model based on
J. Kopp, Phys. Rev. D 88 (2013) 076013

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Alterna5ve Models to explain the AMS positron ﬂux and positron
frac5on21

Alterna5ve Models to explain the AMS positron ﬂux and positron
frac5on22

Alterna5ve Models to explain the AMS positron ﬂux and positron
frac5onExcess of Positron ﬂux and Positron frac,on can be also explainedby Pulsar sources

AMS also observes excess on An,proton/Proton ra,o andthis is cannot be explained by Pulsars
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The AMS positron spectrum and frac5on expected by 2024

By 2024, AMS will dis,nguish
Dark Ma]er from Pulsars

24Physics Results 4: Measurement of Anisotropy

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Physics Results 5: The (e+ + e-) ﬂux
The precision AMS measurement of the (e+ + e-) ﬂux
contradicts all previous measurements and previous models

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The (e+ + e-) ﬂux projected in 2024
AMS will be able to dis,nguish the (e+ + e-) ﬂux behavior above 1 TeV

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CALET: Exploring the TeV region

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Installed at Japanese module, Kibo on 26/Aug/2015

Before AMS: Proton Flux Measurement
Ø Protons are the most abundant cosmic rays.
Ø Before AMS there have been many measurements of the proton spectrum.
Ø In cosmic rays models, the proton spectral func,on was assumed to be a singlepower law

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Physics Results 6: Precision measurement of proton ﬂux
to an accuracy of 1%

M. Aguilar et al., Phys. Rev. Lea. 114, 171103 (2015)30

New informa5on on AMS Proton ﬂux
The proton ﬂux cannot be described by a single power law =as has been assumed for decades

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Proton spectral index changing with momentum

32Understanding of the Solar Magne5c ﬁeld

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Spectra of elementary par5clese- and e+ have much smaller mass than p and p̄ , so they lose much more energy
in the galac,c magne,c ﬁeld due to synchrotron radia,on.

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Dark Maaer: An5proton channel

35Signal Selec5on36

Physics Results 7: The an5proton ﬂux and proper5es of
elementary par5cle ﬂuxes

M. Aguilar et al., Phys. Rev. Lea. 117, 091103(2016)37

An5proton-to-proton ra5o
Ø Excess of an,proton is observed by AMS!!!
Ø Cannot be explained by Pulsars
Ø Can be explained by Dark Ma]er Annihila,on orby new astrophysics phenomena

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Cosmic Rays Interac5on39AMS Nuclei Fluxes Measurements
7 instruments to iden,fy
independently the diﬀerent elements

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Measuring the interac5on of nuclei within AMS: Method
AMS in horizontal posi,on41

Before AMS : Helium Flux Measurement
Ø 2nd most abundant cosmic rays
Ø He produced by Supernovas
Ø As for Protons He spectral func,on was assumed to be a single power ( = 2.7)

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Physics Results 8: Precision measurement on the Helium ﬂux

M. Aguilar et al., Phys. Rev. Lea. 115, 211101 (2015)43

New informa5on on AMS Helium ﬂux
The Helium ﬂux cannot be described by a single power law

44Helium spectral index
Unexpectedly the Helium index change with the rigidity in the similar
way as for the Proton spectral index but the values are diﬀerent!!

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Physics Results 9: The AMS proton/helium ﬂux ra5o
Proton and Helium are “Primary” Cosmic Rays.
Since Proton and Helium are assumed to be produced by the same
Astrophysical sources, their ra,o should be ﬂat.

Ra,o not ﬂat in AMS!!!

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Proton-Helium ra5o: independent of the solar ac5vity

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Physics Results 10: The Lithium ﬂux
New AMS results on Secondary Cosmic Rays => Lithium
Similar as Proton and Helium ﬂuxes, Lithium ﬂux cannot be explain by a single power law.

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Physics Results 11: The Beryllium ﬂux
New AMS results on Secondary Cosmic Rays => Beryllium

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Physics Results 12: The Boron ﬂux
New AMS results on Secondary Cosmic Rays =>Boron

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Beryllium to Boron ﬂuxes ra5o and age of Cosmic Rays

Be/B ra,o increases with energy due to rela,vis,c ,me dila,on and provides
informa,on about the age of Cosmic Rays in the Galaxy51

Before AMS: Beryllium to Boron ﬂux ra5o measurement

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Physics Results 13: Berylllium to Boron ﬂux ra5o
Age of the cosmic rays in the galaxy ~ 12 millions years

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Ra5o between primaries (C) and secondaries (B)Provides informa,on on the cosmic propaga,on and ISM.
In general cosmic rays propaga,on is modeled as a fast moving gas
diﬀusing through magne,zed plasma.

For high rigidi,es, the magne,zed plasma model shows diﬀerent behavior.
=> Kolmogorov turbulence model=> Kraichnan theory
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Physics Results 14: Boron to Carbon ﬂux ra5oAbove 65 GeV, the B/C is well described by the single power law.
In agreement with the Kolmogorov turbulence model of magne,zed plasma

M. Aguilar et al., Phys. Rev. Lea. 117, 231101 (2016)55

Physics Results 15: The Carbon ﬂux (primary)56

Physics Results 16: The Oxygen ﬂux (primary)57

Physics Results 17: Diﬀerent momentum dependence for primaries
and secondaries cosmic rays

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Physics Results 18: The AMS Carbon/Helium ﬂux ra5o59

Physics Results 19: Iden5cal momentum dependence forprimary cosmic rays Carbon and Oxygen

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The Carbon/Oxygen ﬂux ra5o61

Physics Results 20: Iron rate

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Physics Results 21: Search for complex an5maaer
in cosmic rays (status report)

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Search for Baryogenesis
Two requirements for the Baryogenesis:
Strong Symmetry Breaking

Proton has a ﬁnite life,me

BELLE, BaBar
FNAL: KTeV, CDF, D0, NOvACERN NA-48
T2K,
LHC: LHC-b, ATLAS,CMS

underground experiments
Super Kamiokande

No evidence for strong symmetry breaking
nor proton decay have been found so far!!!
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Searching an5helium65Iden5ﬁca5on of an5helium66

An5helium Candidates
AMS observed few events with z = -2 and with mass around 3He!!!
At a signal to background ra,o of 1/109, a detailed understanding ofthe instrument is required.
Example: Precision measurement of Positron Frac,on requires e and p
separa,on of 1/106
Positron frac,on analysis with TRD+ECAL compared with TRD Only67

An5helium and AMS68

Summary1) Precise measurement on the Electron and Positron ﬂux => Spectral indexes not constant2) Excess on Positron ﬂux and Positron frac,on => Our dat ﬁts with the DM model3) Measurement of the Anisotropy
4) Measurement on the e+ + e- ﬂux
5) Proton and Helium ﬂuxes described by a double power law func,on => Spectral indexes
not constant6) Proton/Helium ra,o not constant7) Positron ﬂux has the same energy dependence as the An,proton and Proton ﬂuxes8) Excess on An,proton/Proton ra,o9) Age of the Cosmic rays (Be/B) => ~ 12 million years
69Summary10) Measurement on B/C in agreement with the Kolmogorov turbulence model of a magne,zedplasma
11) Diﬀerent momentum dependence between primaries and secondaries cosmic rays12) Iden,cal momentum dependence for primary cosmic rays Carbon and Oxygen13) Iron rate14) Search for complex an,ma]er (status report)

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Thank you for your a]en,on

Akemashite Omedetou Gozaimasu!!!

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Back up Slides

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Coming experiments

Table by S. Torii
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Can we explain AMS-02 an5proton and positron excesses
simultaneously by nearby supernovae without pulsars
or dark maaer? (Kohri et al. Prog. Theor. Exp. Phys. 2016 , 021)

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Can we explain AMS-02 an5proton and positron excesses
simultaneously by nearby supernovae without pulsars
or dark maaer? (Kohri et al. Prog. Theor. Exp. Phys. 2016 , 021)

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ANOMALOUS GALACTIC COSMIC RAYS IN THE FRAMEWORKOF AMS-02(Khiali et al.)In this paper “ we argued that a transi5on from diﬀuse shock accelera5on (DSA) to Superdiﬀuse
Shock accelera5on (SSA) in SNRs is an acceptable explana5on for the recent results of AMS-02,
especially the proton and helium hardenings at 300 GV. We proposed that the observed breakin proton and helium spectra originates from the source due to diﬀerent accelera5onmechanisms and ﬁnally with diﬀerent injec5on forms.”“the He/p ra5o decreases with a single power law and indicates that solar modula5on andinterac5on of He nuclei with ISM reduces the ﬂux at lower energies. Furthermore, this ﬁgureshows that the abundances of the CR helium are larger than the solar abundance (see Lodders2003).”“In addi5on, this model can be used for recent observed carbon spectrum by the AMS-02
experiment which is similar to that of helium, and for heavier nuclei, which will be provided in thenear future.”76Cosmic-ray hardenings in light of AMS-02 data
(Ohira et al.)77