Cosmic Rays: AMS Experiment Javier Berdugo (CIEMAT, Madrid) October - - PowerPoint PPT Presentation

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Cosmic Rays: AMS Experiment Javier Berdugo (CIEMAT, Madrid) October - - PowerPoint PPT Presentation

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Cosmic Rays: AMS Experiment Javier Berdugo (CIEMAT, Madrid) October 11 th 2018 Frontiers of Astroparticle Physics. La Palma Cosmic rays Cosmic rays are a sample of solar, galactic and extragalactic matter which includes all known nuclei and

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Cosmic Rays: AMS Experiment

Javier Berdugo (CIEMAT, Madrid)

Frontiers of Astroparticle Physics. La Palma October 11th 2018

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  • P. Mertsch arXiv: 1012.4239 [astro-ph.HE]

Cosmic rays are a sample of solar, galactic and extragalactic matter which includes all known nuclei and their isotopes, as well as electrons, positrons and antiprotons

Cosmic rays

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  • Sci. Amer. 276 (1997) 44
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p, He + ISM antiparticles + …  +   antiparticles + …

EARTH

        

p, He

antiparticles

ISM

The collision of cosmic rays with interstellar medium (ISM) produces antiparticles (e+, p, D, …) The collision of dark matter particles will produce additional antiparticles Antiparticles in Cosmic Rays and Dark Matter

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Positrons in Cosmic Rays

m=800 GeV

  • I. Cholis et al., arXiv:0810.5344

m=400 GeV e± energy [GeV]

e+ /(e+ + e-)

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  • M. S. Turner and F. Wilczek, Phys. Rev. D42 (1990) 1001;
  • J. Ellis, 26th ICRC Salt Lake City (1999) astro-ph/9911440;
  • H. Cheng, J. Feng and K. Matchev, Phys. Rev. Lett. 89 (2002) 211301;
  • S. Profumo and P. Ullio, J. Cosmology Astroparticle Phys. JCAP07 (2004) 006;
  • D. Hooper and J. Silk, Phys. Rev. D 71 (2005) 083503;
  • 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 0901 025 (2009) 0810.1527; B2

Y–Z. Fan et al., Int. J. Mod. Phys. D19 (2010) 2011;

  • M. Pato, M. Lattanzi and G. Bertone, JCAP 1012 (2010) 020.
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Precision measurements of antiparticles requires long exposure time with detectors with large acceptance and percent level precision.

Flux of antiparticles in cosmic rays

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Experiments operating outside the atmosphere and capable to measure simultaneously the spectra of the different cosmic ray components.

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  • O. Adriani et al. Nature 458 (2009)
  • M. Ackerman et al. Phys. Rev. Lett. 108 (2012) 011103

PAMELA: Launched on June 15th 2006

Image: http://wizard.roma2.infn.it/pamela/html/resurs.html

Baikonur Cosmodrome (Kazakhstan) FERMI Launched on June 11, 2008

Image credit: NASA/Jerry Cannon, Robert Murray

Space based cosmic ray experiments

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CALET, started August 2015 ISS CREAM, started August 2017 AMS, started May 2011 DAMPE, started December 2015

Space-born Cosmic Ray Experiments in operation

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5m x 4m x 3m 7.5 tons

TRD TOF 1, 2 TOF 3, 4 RICH ECAL Magnet and Veto Counters

Silicon layer 1 Silicon layers 2 - 8 Silicon layer 9

Acceptance: 0.5 m2 sr

08/07/2014 8

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USA MEXICO

UNAM

  • UNIV. OF TURKU

ASI IROE FLORENCE INFN & UNIV. OF BOLOGNA INFN & UNIV. OF MILANO-BICOCCA INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF TRENTO

NETHERLANDS

ESA-ESTEC NIKHEF

RUSSIA

ITEP KURCHATOV INST.

SPAIN

CIEMAT - MADRID I.A.C. CANARIAS. ETH-ZURICH

  • UNIV. OF GENEVA

CALT (Beijing) IEE (Beijing) IHEP (Beijing) NLAA (Beijing) BUAA(Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU (Jinan) EWHA KYUNGPOOK NAT.UNIV.

PORTUGAL

  • LAB. OF INSTRUM. LISBON
  • ACAD. SINICA (Taipei)

CSIST (Taipei) NCU (Chung Li) NCKU (Tainan)

TAIWAN TURKEY

METU, ANKARA

CER N= JSC DOE- NASA

LUPM MONTPELLIER LAPP ANNECY LPSC GRENOBLE

FRANCE 9 BRAZIL

IFSC – SÃO CARLOS INSTITUTE OF PHYSICS RWTH-I. Aachen KIT-KARLSRUHE

SWITZERLAND MIT KOREA GERMANY FINLAND ITALY CHINA

AMS is an international collaboration based at CERN

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It took 650 physicists and engineers 17 years to construct AMS

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Ground Tests and Calibrations

Space 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 bar Ambient temperature:

  • 90oC to 40oC

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Test Beam at CERN (Calibration)

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237<|R|<290 GV

Positron measurement with AMS

Signal identification from 2D template fit in (∧TRD - ∧CC ) plane

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Positron fraction in cosmic rays with AMS

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1 10 100 1000 Energy [GeV]

50 100 150 200 250 ]

2

GeV

  • 1

sr

  • 1

s

  • 2

[m

3

E

  • e

F 5 10 15 20 25 ]

2

GeV

  • 1

sr

  • 1

s

  • 2

[m

3

E

+

e

F

Latest AMS results on positron and electron fluxes 28.1 million electrons 1.9 million positrons

Energy range from 0.5 GeV to 1 TeV

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Astrophysical point sources like pulsars will imprint a higher anisotropy on the arrival directions of energetic positrons than a smooth dark matter halo.

positrons Isotropic Map

C1 is the dipole moment The anisotropy in galactic coordinates

Amplitude of the dipole anisotropy on positrons for 16 < E < 350 GeV δ < 0.019 (95% C.I.)

AMS Positron cosmic ray anisotropy

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Models based on very different assumptions describe observed trends of a single measurement.

Positron flux modeling

Many models proposed to explain the physics origin of the observed behavior

1) Particle origin: Dark Matter 2) Astrophysics origin: Pulsars, SNRs 3) Propagation of cosmic rays

Simultaneous description of several precision measurements is difficult in the framework of a single model

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⦁ 1.9 million positrons

1.2 TeV Dark Matter + Collision of Cosmic Rays The positron flux appears to be in agreement with predictions from a 1.2 TeV Dark Matter model (J. Kopp, Phys. Rev. D 88, 076013 (2013))

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(e+ + e–) AMS data: comparison with other detectors

Measuring (e++e–) is much less sensitive to detect the source term due to the large e– background

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(e+ + e–) AMS data: comparison with other detectors

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The Antiproton Flux is ~10-4 of the Proton Flux. A percentage precision experiment requires background rejection close to 1 in a million

Kinetic energy [GeV] Antiproton / proton ratio

Donato et al., PRL 102, 071301 (2009)

Dark matter

10-4 10-5 10-6 10-7 10-3 10-2 1 10 100 1000 Dark matter +

Collision of cosmic rays with ISM

Antiprotons in Cosmic rays

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p

e p 175<|R|<211 GV

χ2/d.f. = 138/154

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Antiproton measurement with AMS

Signal identification from 2D template fit in (∧TRD - ∧CC ) plane

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p 3.49105 events

  • AMS-02
  • PAMELA

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Antiproton-to-Proton Flux Ratio

  • M. Aguilar et al. Phys. Rev. Lett. 117 (2016) 091103

Show no rigidity dependence above 60 GV

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G.Giesen, et. al., JCAP 09 (2015) 023 C.Evoli et. al., JCAP 12 (2015) 039 R.Kappl, et. al., JACP 10(2015) 034

Collision of cosmic rays with interstellar medium:

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Primary and secondary cosmic ray

08/07/2014 23 PDG, Phys. Rev. D86, 010001 (2012)

  • A. Obermeier et al. Astrophys. J. 742 (2011) 14

Understanding the origin, acceleration and propagation of CR require the knowledge of the chemical composition over a wide energy range

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Primary and secondary Cosmic Rays

Comparison 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

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Secondary/Primary Flux Ratios = KRΔ

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

Δ[200-3300GV] – Δ[60-200GV] = 0.13±0.03

200 GV 200 GV

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[GV] R ~ Rigidity

3 4 5 10 20

2

10

2

10 ´ 2

3

10

3

10 ´ 2 ]

1.7

GV

  • 1

sr

  • 1

s

  • 2

[ m

2.7

R ´

N

F 5 10 15 20 25 a)

AMS

S N

F +

P N

F =

N

F

B

F ´ = 0.62

S N

F ;

O

F ´ = 0.09

P N

F

Primary Component Secondary Component

Nitrogen Cosmic Rays

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AMS

ΦN = ΦNP+ΦNS

ΦN = ΦNP+ΦNS = (0.090±0.002)×ΦO+(0.62±0.02)×ΦB

  • M. Aguilar et al. Phys. Rev. Lett. 121 (2018) 051103

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3He/4He abundancies

Preliminary data, refer to upcoming AMS PRL publication

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AMS continous measurement of the e+ and e- flux in the energy range 1 -50 GeV

  • ver 6 years with a time resolution of 27 days.
  • M. Aguilar et al. Phys. Rev. Lett. 121 (2018) 051102
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Anti Deuterons have been proposed as an almost background free channel for Dark Matter indirect detection

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Anti Deuterons in Cosmic rays

The Anti Deuterons Flux is < 10-4 of the Antiproton Flux. Additional background rejection

1 4 10 40 100 10-6 10-8 10-10

Rigidity [GV]

Flux [(m2 sr s GV)-1]

D from collisions of

  • rdinary cosmic rays

D from annihilation

  • f Dark Matter

 Dark Matter model:

  • F. Donato et al., Phys. Rev. D, 62 (2000) 043003

 Collisions of CR model

  • K. Blum et al., Phys. Rev. D 96 (2017) 103021)
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Anti-deuterons have never been observed in space

BESS results (COSPAR 2018)

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Anti-Deuteron Search with AMS

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Anti-Deuteron Search prospects

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Y Z X

First anti-Helium event in the cosmos:

Momentum = 33.1 ± 1.6 GeV/c Charge = -1.97 ± 0.05 Mass = 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

There are large uncertainties in models to ascertain the origin of 3He The rate of anti-helium is ~1 in 100 million helium. We have also observed two 4He candidates. More events are necessary to ensure that there are no backgrounds.

Kinetic Energy/nucleon

model variations factor of ~300

  • K. Blum et al., Phys. Rev. D 96, 103021 (2017)
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High precision measurements of cosmic rays open new windows to observe unexpected phenomena There are several large scale detectors in space to study high energy charged cosmic rays: AMS, CALET, DAMPE, ISS-CREAM exploring a new and exciting frontier in physics research

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