Alpha Magnetic Spectrometer

Summary

Alpha Magnetic Spectrometer
Alpha Magnetic Spectrometer - 02.jpg
Rendering of AMS-02
Module statistics
Part ofInternational Space Station
Launch date16 May 2011 13:56:28 (2011-05-16UTC13:56:28) UTC[1][2][3]
Launch vehicleSpace Shuttle Endeavour
Berthed19 May 2011
Mass6,717 kg (14,808 lb)
AMS-02 logo

The Alpha Magnetic Spectrometer (AMS-02) is a particle physics experiment module that is mounted on the International Space Station (ISS).[4] The experiment is a recognized CERN experiment (RE1).[5][6] The module is a detector that measures antimatter in cosmic rays; this information is needed to understand the formation of the Universe and search for evidence of dark matter.

The principal investigator is Nobel laureate particle physicist Samuel Ting. The launch of Space Shuttle Endeavour flight STS-134 carrying AMS-02 took place on 16 May 2011, and the spectrometer was installed on 19 May 2011.[7][8] By April 15, 2015, AMS-02 had recorded over 60 billion cosmic ray events[9] and 90 billion after five years of operation since its installation in May 2011.[10]

In March 2013, Professor Ting reported initial results, saying that AMS had observed over 400,000 positrons, with the positron to electron fraction increasing from 10 GeV to 250 GeV. (Later results have shown a decrease in positron fraction at energies over about 275 GeV). There was "no significant variation over time, or any preferred incoming direction. These results are consistent with the positrons originating from the annihilation of dark matter particles in space, but not yet sufficiently conclusive to rule out other explanations." The results have been published in Physical Review Letters.[11] Additional data are still being collected.[11][12][13][14][15][16][17]

History

The alpha magnetic spectrometer was proposed in 1995 by the Antimatter Study Group,[18][4] led by MIT particle physicist Samuel Ting, not long after the cancellation of the Superconducting Super Collider. The original name for the instrument was Antimatter Spectrometer,[4][18][19] with the stated objective to search for primordial antimatter, with a target resolution of antimatter/matter ≈10−9.[18][19] The proposal was accepted and Ting became the principal investigator.[20]

AMS-01

AMS-01 flew in space in June 1998 aboard the Space Shuttle Discovery on STS-91. It is visible near the rear of the payload bay.
A detail view of the AMS-01 module (center) mounted in the shuttle payload bay for the STS-91 mission.

An AMS prototype designated AMS-01, a simplified version of the detector, was built by the international consortium under Ting's direction and flown into space aboard the Space Shuttle Discovery on STS-91 in June 1998. By not detecting any antihelium the AMS-01 established an upper limit of 1.1×10−6 for the antihelium to helium flux ratio[21] and proved that the detector concept worked in space. This shuttle mission was the last shuttle flight to the Mir Space Station.

AMS-02

AMS-02 during integration and testing at CERN near Geneva.

After the flight of the prototype, the group, now labelled the AMS Collaboration, began the development of a full research system designated AMS-02. This development effort involved the work of 500 scientists from 56 institutions and 16 countries organized under United States Department of Energy (DOE) sponsorship.

The instrument which eventually resulted from a long evolutionary process has been called "the most sophisticated particle detector ever sent into space", rivaling very large detectors used at major particle accelerators, and has cost four times as much as any of its ground-based counterparts. Its goals have also evolved and been refined over time. As built it is a more comprehensive detector which has a better chance of discovering evidence of dark matter along other goals.[22]

The power requirements for AMS-02 were thought to be too great for a practical independent spacecraft. So AMS-02 was designed to be installed as an external module on the International Space Station and use power from the ISS. The post-Space Shuttle Columbia plan was to deliver AMS-02 to the ISS by space shuttle in 2005 on station assembly mission UF4.1, but technical difficulties and shuttle scheduling issues added more delays.[23]

AMS-02 successfully completed final integration and operational testing at CERN in Geneva, Switzerland which included exposure to energetic proton beams generated by the CERN SPS particle accelerator.[24][25] AMS-02 was then shipped by specialist haulier to ESA's European Space Research and Technology Centre (ESTEC) facility in the Netherlands where it arrived 16 February 2010. Here it underwent thermal vacuum, electromagnetic compatibility and electromagnetic interference testing. AMS-02 was scheduled for delivery to the Kennedy Space Center in Florida, United States. in late May 2010.[7] This was however postponed to August 26, as AMS-02 underwent final alignment beam testing at CERN.[26][27]

AMS-02 during final alignment testing at CERN just days before being airlifted to Cape Canaveral.
Beamline from SPS feeding 20 GeV positrons to AMS for alignment testing at the time of the picture.

A cryogenic, superconducting magnet system was developed for the AMS-02. With Obama administration plans to extend International Space Station operations beyond 2015, the decision was made by AMS management to exchange the AMS-02 superconducting magnet for the non-superconducting magnet previously flown on AMS-01. Although the non-superconducting magnet has a weaker field strength, its on-orbit operational time at ISS is expected to be 10 to 18 years versus only three years for the superconducting version.[28] In December 2018 it was announced that funding for the ISS had been extended to 2030.[29]

In 1999, after the successful flight of AMS-01, the total cost of the AMS program was estimated to be $33 million, with AMS-02 planned for flight to the ISS in 2003.[30] After the Space Shuttle Columbia disaster in 2003, and after a number of technical difficulties with the construction of AMS-02, the cost of the program ballooned to an estimated $2 billion.[31][32]

Installation on the International Space Station

A computer generated image showing AMS-02 mounted to the ISS S3 Upper Inboard Payload Attach Site.
Location of the AMS on the International Space Station (upper left).
AMS-02 installed on the ISS.

For several years it was uncertain if AMS-02 would ever be launched because it was not manifested to fly on any of the remaining Space Shuttle flights.[33] After the 2003 Columbia disaster NASA decided to reduce shuttle flights and retire the remaining shuttles by 2010. A number of flights were removed from the remaining manifest including the flight for AMS-02.[20] In 2006 NASA studied alternative ways of delivering AMS-02 to the space station, but they all proved to be too expensive.[33]

In May 2008 a bill[34] was proposed to launch AMS-02 to ISS on an additional shuttle flight in 2010 or 2011.[35] The bill was passed by the full House of Representatives on 11 June 2008.[36] The bill then went before the Senate Commerce, Science and Transportation Committee where it also passed. It was then amended and passed by the full Senate on 25 September 2008, and was passed again by the House on 27 September 2008.[37] It was signed by President George W. Bush on 15 October 2008.[38][39] The bill authorized NASA to add another space shuttle flight to the schedule before the space shuttle program was discontinued. In January 2009 NASA restored AMS-02 to the shuttle manifest. On 26 August 2010, AMS-02 was delivered from CERN to the Kennedy Space Center by a Lockheed C-5 Galaxy.[40]

It was delivered to the International Space Station on May 19, 2011 as part of station assembly flight ULF6 on shuttle flight STS-134, commanded by Mark Kelly.[41] It was removed from the shuttle cargo bay using the shuttle's robotic arm and handed off to the station's robotic arm for installation. AMS-02 is mounted on top of the Integrated Truss Structure, on USS-02, the zenith side of the S3-element of the truss.[42]

Operations, condition and repairs

ESA astronaut Luca Parmitano, attached to the Canadarm2 robotic arm, carries the new thermal pump system for AMS

By April 2017 only one of the 4 redundant coolant pumps for the silicon trackers was fully working, and repairs were being planned, despite AMS-02 not being designed to be serviced in space.[43][44] By 2019, the last one was being operated intermittently.[44] In November 2019, after four years of planning,[44] special tools and equipment were sent to the ISS for in-situ repairs that may require four or five EVAs.[45] Liquid carbon dioxide coolant was also replenished.[44]

The repairs were conducted by the ISS crew of Expedition 61. The spacewalkers were the expedition commander and ESA astronaut Luca Parmitano, and NASA astronaut Andrew Morgan. Both of them were assisted by NASA astronauts Christina Koch and Jessica Meir who operated the Canadarm2 robotic arm from inside the Station. The spacewalks were described as the "most challenging since [the last] Hubble repairs".[46]

First spacewalk

The first spacewalk was conducted on November 15, 2019. The spacewalk began with the removal of the debris shield covering AMS and it was jettisoned to burn up in the atmosphere. The next task was the installation of three handrails in the vicinity of AMS to prepare for the next spacewalks and removed zip ties on the AMS' vertical support strut. This was followed by the "get ahead" tasks: Luca Parmitano removed the screws from a carbon-fibre cover under the insulation and passed the cover to Andrew Morgan to jettison. The spacewalkers also removed the vertical support beam cover. The duration of the spacewalk was 6 hours and 39 minutes.[47][48]

Second spacewalk

The second spacewalk was conducted on November 22, 2019. Parmitano and Morgan cut a total of eight stainless steel tubes, including one that vented the remaining carbon dioxide from the old cooling pump. The crew members also prepared a power cable and installed a mechanical attachment device in advance of installing the new cooling system. The duration of the spacewalk was 6 hours and 33 minutes.[49]

Third spacewalk

The third spacewalk was conducted on December 2, 2019. The crew completed the primary task of installing the upgraded cooling system, called the upgraded tracker thermal pump system (UTTPS), completed the power and data cable connections for the system, and connected all eight cooling lines from the AMS to the new system. The intricate connection work required making a clean cut for each existing stainless steel tube connected to the AMS, then connecting it to the new system through swaging.[50]

The astronauts also completed an additional task to install an insulating blanket on the nadir side of the AMS to replace the heat shield and blanket they removed during the first spacewalk to begin the repair work. The flight control team on Earth initiated power-up of the system and confirmed its reception of power and data.[50]

The duration of the spacewalk was 6 hours and 2 minutes.[50]

Fourth spacewalk

The final spacewalk was conducted on January 25, 2020. The astronauts conducted leak checks for the cooling system on the AMS and opened a valve to pressurize the system. Parmitano found a leak in one of the AMS's cooling lines. The leak was fixed during the spacewalk. Preliminary testing showed the AMS was responding as expected.[51][52]

Ground teams are working to fill the new AMS thermal control system with carbon dioxide, allow the system to stabilize, and power on the pumps to verify and optimize their performance. The tracker, one of several detectors on the AMS, began collecting science data again before the end of the week after the spacewalk.[51]

The astronauts also completed an additional task to remove degraded lens filters on two high-definition video cameras.[51]

The duration of the spacewalk was 6 hours and 16 minutes.[51]

Specifications

  • Mass: 7,500 kg
  • Structural material: Stainless steel
  • Power: 2,500 W
  • Internal data rate: 7 Gbit/s
  • Data rate to ground: 2 Mbit/s (typical, average)[53]
  • Primary mission duration: 10 to 18 years
  • Design life: 3 years.[44]
  • Magnetic field intensity: 0.15 teslas produced by a 1,200 kg permanent neodymium magnet[53]
  • Original superconducting magnet: 2 coils of niobium-titanium at 1.8 K producing a central field of 0.87 teslas[54] (Not used in the actual device)
  • AMS-02 flight magnet changed to non-superconducting AMS-01 version to extend experiment life and to solve reliability problems in the operation of the superconducting system

About 1,000 cosmic rays are recorded by the instrument per second, generating about one GB/sec of data. This data is filtered and compressed to about 300 kbit/s for download to the operation center POCC at CERN.

Design

The detector module consists of a series of detectors that are used to determine various characteristics of the radiation and particles as they pass through. Characteristics are determined only for particles that pass through from top to bottom. Particles that enter the detector at any other angles are rejected. From top to bottom the subsystems are identified as:[55]

  • Transition radiation detector measures the velocities of the highest energy particles;
  • Upper time of flight counter, along with the lower time of flight counter, measures the velocities of lower energy particles;
  • Star tracker determines the orientation of the module in space;
  • Silicon tracker (9 disks among 6 locations) measures the coordinates of charged particles in the magnetic field;
    • Has 4 redundant coolant pumps
  • Permanent magnet bends the path of charged particles so they can be identified;
  • Anti-coincidence counter rejects stray particles that enter through the sides;
  • Ring imaging Cherenkov detector measures velocity of fast particles with extreme accuracy;
  • Electromagnetic calorimeter measures the total energy of the particles.

Scientific goals

The AMS-02 will use the unique environment of space to advance knowledge of the Universe and lead to the understanding of its origin by searching for antimatter, dark matter and measuring cosmic rays.[42]

Antimatter

Experimental evidence indicates that our galaxy is made of matter; however, scientists believe there are about 100–200 billion galaxies in the observable Universe and some versions of the Big Bang theory of the origin of the Universe require equal amounts of matter and antimatter. Theories that explain this apparent asymmetry violate other measurements. Whether or not there is significant antimatter is one of the fundamental questions of the origin and nature of the Universe. Any observations of an antihelium nucleus would provide evidence for the existence of antimatter in space. In 1999, AMS-01 established a new upper limit of 10−6 for the antihelium/helium flux ratio in the Universe. AMS-02 was designed to search with a sensitivity of 10−9,[19] an improvement of three orders of magnitude over AMS-01, sufficient to reach the edge of the expanding Universe and resolve the issue definitively.

Dark matter

The visible matter in the Universe, such as stars, adds up to less than 5 percent of the total mass that is known to exist from many other observations. The other 95 percent is dark, either dark matter, which is estimated at 20 percent of the Universe by weight, or dark energy, which makes up the balance. The exact nature of both still is unknown. One of the leading candidates for dark matter is the neutralino. If neutralinos exist, they should be colliding with each other and giving off an excess of charged particles that can be detected by AMS-02. Any peaks in the background positron, antiproton, or gamma ray flux could signal the presence of neutralinos or other dark matter candidates, but would need to be distinguished from poorly known confounding astrophysical signals.

Strangelets

Six types of quarks (up, down, strange, charm, bottom and top) have been found experimentally; however, the majority of matter on Earth is made up of only up and down quarks. It is a fundamental question whether there exists stable matter made up of strange quarks in combination with up and down quarks. Particles of such matter are known as strangelets. Strangelets might have extremely large mass and very small charge-to-mass ratios. It would be a totally new form of matter. AMS-02 may determine whether this extraordinary matter exists in our local environment.

Space radiation environment

Cosmic radiation during transit is a significant obstacle to sending humans to Mars. Accurate measurements of the cosmic ray environment are needed to plan appropriate countermeasures. Most cosmic ray studies are done by balloon-borne instruments with flight times that are measured in days; these studies have shown significant variations. AMS-02 is operative on the ISS, gathering a large amount of accurate data and allowing measurements of the long term variation of the cosmic ray flux over a wide energy range, for nuclei from protons to iron. In addition to the understanding the radiation protection required for astronauts during interplanetary flight, this data will allow the interstellar propagation and origins of cosmic rays to be identified.

Results

In July 2012, it was reported that AMS-02 had observed over 18 billion cosmic rays.[56]

In February 2013, Samuel Ting reported that in its first 18 months of operation AMS had recorded 25 billion particle events including nearly eight billion fast electrons and positrons.[57] The AMS paper reported the positron-electron ratio in the mass range of 0.5 to 350 GeV, providing evidence about the weakly interacting massive particle (WIMP) model of dark matter.

On 30 March 2013, the first results from the AMS experiment were announced by the CERN press office.[11][12][13][14][15][16][58] The first physics results were published in Physical Review Letters on 3 April 2013.[11] A total of 6.8×106 positron and electron events were collected in the energy range from 0.5 to 350 GeV. The positron fraction (of the total electron plus positron events) steadily increased from energies of 10 to 250  GeV, but the slope decreased by an order of magnitude above 20 GeV, even though the fraction of positrons still increased. There was no fine structure in the positron fraction spectrum, and no anisotropies were observed. The accompanying Physics Viewpoint[59] said that "The first results from the space-borne Alpha Magnetic Spectrometer confirm an unexplained excess of high-energy positrons in Earth-bound cosmic rays." These results are consistent with the positrons originating from the annihilation of dark matter particles in space, but not yet sufficiently conclusive to rule out other explanations. Ting said "Over the coming months, AMS will be able to tell us conclusively whether these positrons are a signal for dark matter, or whether they have some other origin."[60]

On September 18, 2014, new results with almost twice as much data were presented in a talk at CERN and published in Physical Review Letters.[61][62][63] A new measurement of positron fraction up to 500 GeV was reported, showing that positron fraction peaks at a maximum of about 16% of total electron+positron events, around an energy of 275 ± 32 GeV. At higher energies, up to 500 GeV, the ratio of positrons to electrons begins to fall again.

AMS presented for 3 days at CERN in April 2015, covering new data on 300 million proton events and helium flux.[64] It revealed in December 2016 that it had discovered a few signals consistent with antihelium nuclei amidst several billion helium nuclei. The result remains to be verified, and the team is currently trying to rule out contamination.[65]

A study from 2019, using data from NASA's Fermi Gamma-ray Space Telescope discovered a halo around the nearby pulsar Geminga. The accelerated electrons and positrons collide with nearby starlight. The collision boosts the light up to much higher energies. Geminga alone could be responsible for as much as 20% of the high-energy positrons seen by the AMS-02 experiment.[66]

See also

References

 This article incorporates public domain material from the National Aeronautics and Space Administration document: "AMS project page".

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Further reading

  • AMS Collaboration (2011). "Isotopic Composition of Light Nuclei in Cosmic Rays: Results from AMS-01". Astrophys. J. 736 (2): 105. arXiv:1106.2269. Bibcode:2011ApJ...736..105A. doi:10.1088/0004-637X/736/2/105.
  • AMS Collaboration (2010). "Relative Composition and Energy Spectra of Light Nuclei in Cosmic Rays. Results from AMS-01". Astrophys. J. 724 (1): 329–340. arXiv:1008.5051. Bibcode:2010ApJ...724..329A. doi:10.1088/0004-637X/724/1/329.
  • AMS Collaboration (2007). "Cosmic-ray positron fraction measurement from 1 to 30-GeV with AMS-01". Phys. Lett. B. 646 (4): 145–154. arXiv:astro-ph/0703154. Bibcode:2007PhLB..646..145A. doi:10.1016/j.physletb.2007.01.024.
  • AMS Collaboration (2005). "A study of cosmic-ray secondaries induced by the MIR Space Station using AMS-01". Nuclear Instruments and Methods B. 234 (3): 321–332. arXiv:hep-ex/0406065. Bibcode:2005NIMPB.234..321A. doi:10.1016/j.nimb.2005.01.015.
  • AMS Collaboration (2002). "The AMS on the ISS. Part I - Results from the test flight on the Space Shuttle". Physics Reports. 366 (6): 331–405. Bibcode:2002PhR...366..331A. doi:10.1016/S0370-1573(02)00013-3.
  • AMS Collaboration (2000). "Helium in near Earth orbit". Phys. Lett. B. 494 (3–4): 193–202. Bibcode:2000PhLB..494..193A. doi:10.1016/S0370-2693(00)01193-X.
  • AMS Collaboration (2000). "Cosmic Protons". Phys. Lett. B. 490 (1–2): 27–35. Bibcode:2000PhLB..490...27A. doi:10.1016/S0370-2693(00)00970-9.
  • AMS Collaboration (2000). "Leptons in near earth orbit". Phys. Lett. B. 484 (1–2): 10–22. Bibcode:2000PhLB..484...10A. doi:10.1016/S0370-2693(00)00588-8.
  • AMS Collaboration (2000). "Protons in near earth orbit". Phys. Lett. B. 472 (1–2): 215–226. arXiv:hep-ex/0002049. Bibcode:2000PhLB..472..215A. doi:10.1016/S0370-2693(99)01427-6.
  • AMS Collaboration (1999). "Search for anti-helium in cosmic rays". Phys. Lett. B. 461 (4): 387–396. arXiv:hep-ex/0002048. Bibcode:1999PhLB..461..387A. doi:10.1016/S0370-2693(99)00874-6. S2CID 119401739.
  • Sandweiss, J. (2004). "Overview of strangelet searches and Alpha Magnetic Spectrometer: when will we stop searching?". Journal of Physics G: Nuclear and Particle Physics. 30 (1): S51–S59. Bibcode:2004JPhG...30S..51S. doi:10.1088/0954-3899/30/1/004.

External links

  • AMS Collaboration Homepage
  • AMS Homepage at CERN. Inc. construction diagrams.
  • AMS Homepage at the Johnson Space Center
  • NASA AMS-02 Project Fact Sheet
  • NASA AMS-02 Project Home Page with real-time cosmic ray count
  • An animated movie of the STS-134 mission showing the installation of AMS-02 (72MB)
  • Alpha Magnetic Spectrometer – image collection – AMS-02 on Facebook
  • A Costly Quest for the Dark Heart of the Cosmos (New York Times, 16 November 2010)
  • Route To Space Alliance - European Transport for The Space and Aeronautic Industries