PAMELA detector

PAMELA (Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics) was a cosmic ray research module attached to an Earth orbiting satellite. PAMELA was launched on 15 June 2006 and was the first satellite-based experiment dedicated to the detection of cosmic rays, with a particular focus on their antimatter component, in the form of positrons and antiprotons. Other objectives included long-term monitoring of the solar modulation of cosmic rays, measurements of energetic particles from the Sun, high-energy particles in Earth's magnetosphere and Jovian electrons. It was also hoped that it may detect evidence of dark matter annihilation.[1] PAMELA operations were terminated in 2016,[2] as were the operations of the host-satellite Resurs-DK1. The experiment was a recognized CERN experiment (RE2B).[3][4]

For other uses, see PAMELA (disambiguation).

PAMELA
Organization PAMELA group
Mission Type Cosmic Ray
Host Satellite Resurs DK1
Launch 15 June 2006
Launch vehicle Soyuz-FG
Launch site Baikonur Cosmodrome
Mission duration 3 years (planned), over 9 years achieved
Mission end 7 February 2016
Mass 470 kg
Max length 1300 mm
Power consumption 335 Watts
Webpage PAMELA homepage
Orbital elements (Resurs DK1)
Inclination 70 degrees
Orbit quasi-polar elliptical
Min altitude 360 km
Max altitude 604 km
Period 94.02 min

Development and launch

PAMELA was the largest device up to the time built by the Wizard collaboration, which includes Russia, Italy, Germany and Sweden and has been involved in many satellite and balloon-based cosmic ray experiments such as Fermi-GLAST. The 470 kg, US$32 million (EU€24.8 million, UK£16.8 million) instrument was originally projected to have a three-year mission. However, this durable module remained operational and made significant scientific contributions until 2016.

PAMELA is mounted on the upward-facing side of the Resurs-DK1 Russian satellite.[1] It was launched by a Soyuz rocket from Baikonur Cosmodrome on 15 June 2006. PAMELA has been put in a polar elliptical orbit at an altitude between 350 and 610 km, with an inclination of 70°.

Design

The apparatus is 1.3 m high, has a total mass of 470 kg and a power consumption of 335 W. The instrument is built around a permanent magnet spectrometer with a silicon microstrip tracker that provides rigidity and dE/dx information. At its bottom is a silicon-tungsten imaging calorimeter, a neutron detector and a shower tail scintillator to perform lepton/hadron discrimination. A Time of Flight (ToF), made of three layers of plastic scintillators, is used to measure the velocity and charge of the particle. An anticounter system made of scintillators surrounding the apparatus is used to reject false triggers and albedo particles during off-line analysis.[5]

Sensitivity[1]
Particle Energy Range
Antiproton flux 80 MeV – 190 GeV
Positron flux 50 MeV – 270 GeV
Electron flux up to 400 GeV
Proton flux up to 700 GeV
Electron/positron flux up to 2 TeV
Light nuclei (up to Z=6) up to 200 GeV/n
Light isotopes (D, 3He) up to 1 GeV/n
Antinuclei search sensitivity better than 10−7 antiHe/He

Results

Preliminary data (released August 2008, ICHEP Philadelphia) indicate an excess of positrons in the range 10–60 GeV. This is thought to be a possible sign of dark matter annihilation:[6][7] hypothetical WIMPs colliding with and annihilating each other to form gamma rays, matter and antimatter particles. Another explanation considered for the indication mentioned above is the production of electron-positron pairs on pulsars with subsequent acceleration in the vicinity of the pulsar.

The first two years of data were released in October 2008 in three publications.[8][9] The positron excess was confirmed and found to persist up to 90 GeV. Surprisingly, no excess of antiprotons was found. This is inconsistent with predictions from most models of dark matter sources, in which the positron and antiproton excesses are correlated.

A paper, published on 15 July 2011, confirmed earlier speculation that the Van Allen belt could confine a significant flux of antiprotons produced by the interaction of the Earth's upper atmosphere with cosmic rays.[10] The energy of the antiprotons has been measured in the range of 60–750 MeV. Cosmic rays collide with atoms in the upper atmosphere creating antineutrons, which in turn decay to produce the antiprotons. They were discovered in a part of the Van Allen belt closest to Earth.[11] When an antiproton interacts with a normal particle, both are annihilated. Data from PAMELA indicated that these annihilation events occurred a thousand times more often than would be expected in the absence of antimatter. The data that contained evidence of antimatter were gathered between July 2006 and December 2008.[12][13]

Boron and carbon flux measurements were published in July 2014,[14] important to explaining trends in cosmic ray positron fraction.[15]

The summary document of the operations of PAMELA was published in 2017.[2]

Sources of error

Between 1 and 100 GeV, PAMELA is exposed to one hundred times as many electrons as antiprotons. At 1 GeV there are one thousand times as many protons as positrons and at 100 GeV ten thousand times as many. Therefore, to correctly determine the antimatter abundances, it is critical that PAMELA is able to reject the matter background. The PAMELA collaboration claimed in "The electron hadron separation performance of the PAMELA electromagnetic calorimeter" that less than one proton in 100,000 is able to pass the calorimeter selection and be misidentified as a positron when the energy is less than 200 GeV.

The ratio of matter to antimatter in cosmic rays of energy less than 10 GeV that reach PAMELA from outside the Solar System depends on solar activity and in particular on the point in the 11 year solar cycle. The PAMELA team has invoked this effect to explain the discrepancy between their low energy results and those obtained by CAPRICE, HEAT and AMS-01, which were collected during that half of the cycle when the solar magnetic field had the opposite polarity. It is important to note that these results are consistent with the series of positron / electron measurements obtain by AESOP, which has spanned coverage over both polarities. Also the PAMELA experiment has contradicted an earlier claim by the HEAT experiment of anomalous positrons in the 6 GeV to 10 GeV range.

See also
  • AMS-02 is a high energy physics experiment mounted to the exterior of the International Space Station featuring advanced particle identification and large acceptance of 0.3m2sr. AMS-02 has been in operation since May 2011. More than 100 billion charged cosmic ray events were recorded by AMS so far.

References
  1. Vincenzo Buttaro (ed.). "The Space Mission PAMELA". Retrieved 4 September 2009.
  2. Adriani, O; et al. (PAMELA Collaboration) (2018). "Ten Years of PAMELA in Space". Rivista del Nuovo Cimento. 10 (2017): 473–522. arXiv:1801.10310. Bibcode:2018arXiv180110310A. doi:10.1393/ncr/i2017-10140-x. S2CID 119078426.
  3. "Recognized Experiments at CERN". The CERN Scientific Committees. CERN. Retrieved 20 January 2020.
  4. "RE2B/PAMELA : A Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics". CERN. Retrieved 20 January 2020.
  5. Casolino, M; et al. (2008). "Launch of the Space experiment PAMELA". Advances in Space Research. 42 (3): 455–466. arXiv:0708.1808. Bibcode:2008AdSpR..42..455C. doi:10.1016/j.asr.2007.07.023. S2CID 119608020.
  6. Brumfiel, Geoff (14 August 2008). "Physicists await dark-matter confirmation". Nature. 454 (7206): 808–809. doi:10.1038/454808b. PMID 18704050.
  7. Cholis, Ilias; Finkbeiner, Douglas P; Goodenough, Lisa; Weiner, Neal (2009). "The PAMELA Positron Excess from Annihilations into a Light Boson". Journal of Cosmology and Astroparticle Physics. 2009 (12): 007. arXiv:0810.5344. Bibcode:2009JCAP...12..007C. doi:10.1088/1475-7516/2009/12/007. S2CID 73574983.
  8. Casolino, M; et al. (2008). "Two years of flight of the Pamela experiment: Results and perspectives". Journal of the Physical Society of Japan. 78: 35–40. arXiv:0810.4980. Bibcode:2009JPSJ...78S..35C. doi:10.1143/JPSJS.78SA.35. S2CID 119187767.
  9. Adriani, O; et al. (2009). "Observation of an anomalous positron abundance in the cosmic radiation". Nature. 458 (7238): 607–609. arXiv:0810.4995. Bibcode:2009Natur.458..607A. doi:10.1038/nature07942. PMID 19340076. S2CID 11675154.
  10. Adriani, O.; et al. (2011). "The Discovery of Geomagnetically Trapped Cosmic-Ray Antiprotons". The Astrophysical Journal Letters. 737 (2): L29. arXiv:1107.4882. Bibcode:2011ApJ...737L..29A. doi:10.1088/2041-8205/737/2/L29.
  11. Than, Ker (10 August 2011). "Antimatter Found Orbiting Earth—A First". National Geographic Society. Retrieved 12 August 2011.
  12. Cowen, Ron (9 August 2011). "Antimatter Belt Found Circling Earth". Science. Archived from the original on 24 October 2011. Retrieved 12 August 2011.
  13. Chung, Emily (8 August 2011). "Antimatter belt surrounds Earth". CBC News. Retrieved 12 August 2011.
  14. Adriani, O; et al. (31 July 2014). "Measurement of Boron and Carbon Fluxes in Cosmic Rays with the Pamela Experiment". Astrophysical Journal. 791 (2): 93. arXiv:1407.1657. Bibcode:2014ApJ...791...93A. doi:10.1088/0004-637X/791/2/93. S2CID 53002540.
  15. Cholis, Ilias; Hooper, Dan (24 February 2014). "Constraining the origin of the rising cosmic ray positron fraction with the boron-to-carbon ratio". Physical Review D. 89 (4): 043013. arXiv:1312.2952. Bibcode:2014PhRvD..89d3013C. doi:10.1103/PhysRevD.89.043013. S2CID 96470471.
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