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Abdellaoui, G., Fuglesang, C., Zuccaro Marchi, A. & et al, . (2018). EUSO-TA - First results from a ground-based EUSO telescope. Astroparticle physics, 102, 98-111
Open this publication in new window or tab >>EUSO-TA - First results from a ground-based EUSO telescope
2018 (English)In: Astroparticle physics, ISSN 0927-6505, E-ISSN 1873-2852, Vol. 102, p. 98-111Article in journal (Refereed) Published
Abstract [en]

EUSO-TA is a ground-based telescope, installed at the Telescope Array (TA) site in Black Rock Mesa, Utah, USA. This is the first detector to successfully use a Fresnel lens based optical system and multi-anode photomultipliers (64 channels per tube, 2304 channels encompassing a 10.6° × 10.6° field of view) for detection of Ultra High Energy Cosmic Rays (UHECR). The telescope is located in front of one of the fluorescence detectors of the TA experiment. Since its installation in 2013, the detector has observed several ultra-high energy cosmic ray events and, in addition, meteors. The limiting magnitude of 5.5 on summed frames (∼ 3 ms) has been established. Measurements of the UV night sky emission in different conditions and moon phases and positions have been completed. The performed observations serve as a proof of concept for the future application of this detector technology.

Place, publisher, year, edition, pages
Elsevier, 2018
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-233182 (URN)10.1016/j.astropartphys.2018.05.007 (DOI)000439677800012 ()2-s2.0-85048819892 (Scopus ID)
Note

QC 20180813

Available from: 2018-08-13 Created: 2018-08-13 Last updated: 2018-11-13Bibliographically approved
Abdellaoui, G., Abe, S., Adams, J. H., Ahriche, A., Allard, D., Allen, L., . . . Marchi, A. Z. (2018). First observations of speed of light tracks by a fluorescence detector looking down on the atmosphere. Journal of Instrumentation, 13, Article ID P05023.
Open this publication in new window or tab >>First observations of speed of light tracks by a fluorescence detector looking down on the atmosphere
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2018 (English)In: Journal of Instrumentation, ISSN 1748-0221, E-ISSN 1748-0221, Vol. 13, article id P05023Article in journal (Refereed) Published
Abstract [en]

EUSO-Balloon is a pathfinder mission for the Extreme Universe Space Observatory onboard the Japanese Experiment Module (JEM-EUSO). It was launched on the moonless night of the 25(th) of August 2014 from Timmins, Canada. The flight ended successfully after maintaining the target altitude of 38 km for five hours. One part of the mission was a 2.5 hour underflight using a helicopter equipped with three UV light sources (LED, xenon flasher and laser) to perform an inflight calibration and examine the detectors capability to measure tracks moving at the speed of light. We describe the helicopter laser system and details of the underflight as well as how the laser tracks were recorded and found in the data. These are the first recorded laser tracks measured from a fluorescence detector looking down on the atmosphere. Finally, we present a first reconstruction of the direction of the laser tracks relative to the detector.

Place, publisher, year, edition, pages
IOP PUBLISHING LTD, 2018
Keywords
Detectors for UV, visible and IR photons, Lasers, Balloon instrumentation, Space instrumentation
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-231633 (URN)10.1088/1748-0221/13/05/P05023 (DOI)000432931100003 ()2-s2.0-85048075268 (Scopus ID)
Note

QC 20180903

Available from: 2018-09-03 Created: 2018-09-03 Last updated: 2018-09-03Bibliographically approved
Abdellaoui, G., Capel, F., Carlson, P., Fuglesang, C., Larsson, O., Zuccaro Marchi, A. & et.al., . (2017). Cosmic ray oriented performance studies for the JEM-EUSO first level trigger. Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 150-163
Open this publication in new window or tab >>Cosmic ray oriented performance studies for the JEM-EUSO first level trigger
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2017 (English)In: Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, ISSN 0168-9002, E-ISSN 1872-9576, p. 150-163Article in journal (Refereed) Published
Abstract [en]

JEM-EUSO is a space mission designed to investigate Ultra-High Energy Cosmic Rays and Neutrinos (E > 5.10(19) eV) from the International Space Station (ISS). Looking down from above its wide angle telescope is able to observe their air showers and collect such data from a very wide area. Highly specific trigger algorithms are needed to drastically reduce the data load in the presence of both atmospheric and human activity related background light, yet retain the rare cosmic ray events recorded in the telescope. We report the performance in offline testing of the first level trigger algorithm on data from JEM-EUSO prototypes and laboratory measurements observing different light sources: data taken during a high altitude balloon flight over Canada, laser pulses observed from the ground traversing the real atmosphere, and model landscapes reproducing realistic aspect ratios and light conditions as would be seen from the ISS itself. The first level trigger logic successfully kept the trigger rate within the permissible bounds when challenged with artificially produced as well as naturally encountered night sky background fluctuations and while retaining events with general air-shower characteristics.

Place, publisher, year, edition, pages
Elsevier, 2017
Keywords
JEM-EUSO; Trigger system; FPGA; Nightglow background
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-214415 (URN)10.1016/j.nima.2017.05.043 (DOI)000407863700020 ()2-s2.0-85021224738 (Scopus ID)
Note

QC 20170913

Available from: 2017-09-13 Created: 2017-09-13 Last updated: 2017-09-13Bibliographically approved
Capel, F., Fuglesang, C., Casolino, M., Piotrowski, L. & Collaboration, J.-E. E. (2017). Mini-EUSO flight software and operations on ISS. In: Proceedings of Science: . Paper presented at 35th International Cosmic Ray Conference, ICRC 2017, 10 July 2017 through 20 July 2017. Sissa Medialab Srl
Open this publication in new window or tab >>Mini-EUSO flight software and operations on ISS
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2017 (English)In: Proceedings of Science, Sissa Medialab Srl , 2017Conference paper, Published paper (Refereed)
Abstract [en]

The Mini-EUSO instrument is designed by the JEM-EUSO collaboration to pave the way for space-based observations of Extreme Energy Cosmic Rays (EECRs). To be placed inside the International Space Station (ISS) in early 2018, it is a small UV (300-400 nm) telescope which will observe the Earth's atmosphere with a spatial resolution of 6.11 km. Mini-EUSO is capable of detecting a wide variety of UV events such as cosmic ray signals, transient luminous events and meteors with a minimum time resolution of 2.5 μs. It will also be possible to detect space debris during twilight periods. The flight software is fully automated and takes advantage of the frequent day/night cycles of the ISS orbit and ancillary instruments with which Mini-EUSO is equipped in order to optimise the mission's scientific output. The flight operations of Mini-EUSO are presented including the data acquisition, storage and transfer, astronaut interaction and predicted instrument duty cycle. 

Place, publisher, year, edition, pages
Sissa Medialab Srl, 2017
Keywords
Cosmology, Data acquisition, Digital storage, Earth atmosphere, Orbits, Space debris, Space stations, Extreme energy cosmic rays, Flight operation, Flight Software, International Space stations, Scientific output, Space-based observations, Spatial resolution, Transient luminous events, Cosmic rays
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-236846 (URN)2-s2.0-85046054225 (Scopus ID)
Conference
35th International Cosmic Ray Conference, ICRC 2017, 10 July 2017 through 20 July 2017
Funder
Stiftelsen Olle Engkvist Byggmästare
Note

QC 20181214

Available from: 2018-12-14 Created: 2018-12-14 Last updated: 2018-12-14Bibliographically approved
Fuglesang, C., Zetterling, C.-M. & Wilson, C. F. (2017). Venus long-life surface package (VL2SP). In: Proceedings of the International Astronautical Congress, IAC: . Paper presented at 68th International Astronautical Congress: Unlocking Imagination, Fostering Innovation and Strengthening Security, IAC 2017, 25 September 2017 through 29 September 2017 (pp. 3035-3043). International Astronautical Federation, IAF
Open this publication in new window or tab >>Venus long-life surface package (VL2SP)
2017 (English)In: Proceedings of the International Astronautical Congress, IAC, International Astronautical Federation, IAF , 2017, p. 3035-3043Conference paper, Published paper (Refereed)
Abstract [en]

Measurements in the atmosphere and at the surface of Venus are required to understand fundamental processes of how terrestrial planets evolve and how they work today. While the European Venus community is unified in its support of the EnVision orbiter proposal as the next step in European Venus exploration, many scientific questions also require in situ Venus exploration. We suggest a long-duration lander at Venus, which would be capable of undertaking a seismometry mission, operating in the 460°C surface conditions of Venus. Radar maps have shown Venus to be covered with volcanic and tectonic features, and mounting evidence, including observations from Venus Express, suggests that some of these volcanoes are active today. Assessing Venus' current seismicity, and measuring its interior structure, is essential if we are to establish the geological history of our twin planet, for example to establish whether it ever had a habitable phase with liquid water oceans. Although some constraints on seismic activity can be obtained from orbit, using radar or ionospheric observation, the most productive way to study planetary interiors is through seismometry. Seismometry requires a mission duration of months or (preferably) years. Previous landers have used passive cooling, relying on thermal insulation and the lander's thermal inertia to provide a brief window of time in which to conduct science operations - but this allows mission durations of hours, not months. Proposals relying on silicon electronics require an electronics enclosure cooled to < 200 °C; the insulation, cooling and power system requirements escalate rapidly to require a > 1 ton, > €1bn class mission, such as those studied in the context of NASA flagship missions. However, there are alternatives to silicon electronics: in particular, there have been promising advances in silicon carbide (SiC) electronics capable of operating at temperatures of 500°C. Within the coming decade it will be possible to assemble at least simple circuits using SiC components, sufficient to run a seismometry lander. We are proposing a Venus Long-Lived Surface Package (VL2SP) consisting of power source (RTG), science payload (seismometer and meteorology sensors), and ambient temperature electronics including a telecommunications system weighing < 100 kg. We do not specify how this VL2SP gets to the surface of Venus, but we estimate that an orbiter providing data relay would be essential. This presentation is based on a response sumitted to ESA's Call for New Scientific Ideas in September 2016. 

Place, publisher, year, edition, pages
International Astronautical Federation, IAF, 2017
Keywords
High-temperature, Lander, Planetary probe, Seismometry, Venus, C (programming language), Electronic cooling, NASA, Orbits, Planetary landers, Radar, Seismology, Silicon carbide, Space flight, Thermal insulation, Volcanoes, High temperature, Planetary probes, Planets
National Category
Other Electrical Engineering, Electronic Engineering, Information Engineering Aerospace Engineering
Identifiers
urn:nbn:se:kth:diva-236788 (URN)2-s2.0-85051414171 (Scopus ID)9781510855373 (ISBN)
Conference
68th International Astronautical Congress: Unlocking Imagination, Fostering Innovation and Strengthening Security, IAC 2017, 25 September 2017 through 29 September 2017
Note

QC 20181213

Available from: 2018-12-13 Created: 2018-12-13 Last updated: 2018-12-13Bibliographically approved
Fuglesang, C., Zetterling, C.-M. & Östling, M. (2017). Working on venus and beyond - SiC electronics for extreme environments. In: Proceedings of the International Astronautical Congress, IAC: . Paper presented at 68th International Astronautical Congress: Unlocking Imagination, Fostering Innovation and Strengthening Security, IAC 2017, 25 September 2017 through 29 September 2017 (pp. 10393-10398). International Astronautical Federation, IAF
Open this publication in new window or tab >>Working on venus and beyond - SiC electronics for extreme environments
2017 (English)In: Proceedings of the International Astronautical Congress, IAC, International Astronautical Federation, IAF , 2017, p. 10393-10398Conference paper, Published paper (Refereed)
Abstract [en]

Venus is our closest planet, but we know much less about it than about Mars. The main reason for this is the extreme conditions, with a dense atmosphere of mainly CO2 at 92 bar atmosphere and 460 °C temperature at the surface. Only six spacecraft have succeeded to land on Venus and transmit data back to Earth; however none survived for long due to the high temperature. Venera-13 has the record, with 127 minutes at the surface of Venus in 1982. There are many compelling reasons to learn more about the sister planet of Earth, which requires measurements over months rather than minutes on the surface of Venus. Perhaps the single-most challenging task for long-term data taking on the surface of Venus is to build electronics that can operate at temperatures up to 500 °C without cooling. It seems that such technology must be based on wide bandgap semiconductors, such as GaN, SiC or diamond. At KTH, research with SiC devices and integrated circuits has been done for more than 20 years, demonstrating high voltage devices and digital integrated circuit operation at 600 °C. In 2014 the project Working On Venus launched, with funding from Knut and Alice Wallenberg Foundation. The goal is to demonstrate all the electronics for a complete working lander, with all electronics from sensors through amplifiers and analog-to-digital converters to microcontroller with memory and radio, including power supply. The particular sensors the project has in mind are seismic, gas and image sensors. So far, a 200 device level integration has been demonstrated at 500 °C and a 5000+ device level 4 bit microcontroller is being fabricated in an in-house bipolar technology. As for all devices for space, radiation is another concern. SiC integrated circuits have survived exposure to 3 MeV protons with fluences of 1013 cm-2 and gamma rays with doses of 332 Mrad. The dedicated project SUPERHARD IC will study manufacture methods for radiation hardened instrument components that could go beyond Venus, for example for Jovian system exploration. Members of Working on Venus are discussing with scientists seeking opportunities for a Venus Long-Life Surface Package (lander). In 2016 a response was submitted to ESA's Call for New Scientific Ideas. 

Place, publisher, year, edition, pages
International Astronautical Federation, IAF, 2017
Keywords
High-temperature, Lander, Planetary probe, Silicon carbide, Venus, Analog to digital conversion, Atmospheric temperature, Digital devices, Digital integrated circuits, Digital radio, Electronic cooling, Gamma rays, III-V semiconductors, Microcontrollers, Petroleum prospecting, Planetary landers, Planets, Semiconducting gallium compounds, Semiconducting silicon compounds, Space flight, Spacecraft power supplies, Analog to digital converters, Extreme conditions, Extreme environment, High temperature, High voltage devices, Planetary probes, Wide band gap semiconductors
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-236802 (URN)2-s2.0-85051506191 (Scopus ID)9781510855373 (ISBN)
Conference
68th International Astronautical Congress: Unlocking Imagination, Fostering Innovation and Strengthening Security, IAC 2017, 25 September 2017 through 29 September 2017
Note

QC 20181214

Available from: 2018-12-14 Created: 2018-12-14 Last updated: 2018-12-14Bibliographically approved
Fuglesang, C. (2015). Increasing impact of astronaut visits to schools by early preparation, exemplified by "community days" of the ase planetary congress inspired by space. In: Proceedings of the International Astronautical Congress, IAC: . Paper presented at 66th International Astronautical Congress 2015: Space - The Gateway for Mankind's Future, IAC 2015, 12 October 2015 through 16 October 2015 (pp. 10239-10242). International Astronautical Federation
Open this publication in new window or tab >>Increasing impact of astronaut visits to schools by early preparation, exemplified by "community days" of the ase planetary congress inspired by space
2015 (English)In: Proceedings of the International Astronautical Congress, IAC, International Astronautical Federation, 2015, p. 10239-10242Conference paper, Published paper (Refereed)
Abstract [en]

The Association of Space Explorers (ASE) organizes the annual "ASE Planetary Congress". This year (2015) between 20-27 September, the congress took place in Sweden, with the theme name Inspired by Space. In addition to give astronauts and cosmonauts from all over the world a forum to meet and discuss, there are several open technical sessions with a mixture of speakers by ASE members and distinguished guests. However, the most important part of the Planetary Congresses are the "Community Days", when the participating astronauts and cosmonauts split in small groups and visit schools, universities, and other public places. In Sweden about one hundred astronauts were expected to participate and during two half-days around close to hundred schools would get visits by space fliers who share their experiences and enthusiasm with many thousands of pupils and students. The schools prepare many months in advance for the visits, e.g. by "challenges" that are published on websites. Teachers are invited to special briefings. This talk will present the preparations for the ASE congress Inspired by Space Community Days that were done in order to optimize the impact of visiting astronauts and cosmonauts, and detail the outcome, which took place only a few weeks before IAC2015. The presenter is the head responsible for the Inspired by Space congress.

Place, publisher, year, edition, pages
International Astronautical Federation, 2015
Keywords
Manned space flight, Reconfigurable hardware, Societies and institutions, Public places, Space community, Space explorers, Teaching
National Category
Aerospace Engineering
Identifiers
urn:nbn:se:kth:diva-202906 (URN)2-s2.0-84991706354 (Scopus ID)9781510818934 (ISBN)
Conference
66th International Astronautical Congress 2015: Space - The Gateway for Mankind's Future, IAC 2015, 12 October 2015 through 16 October 2015
Note

QC 20170307

Available from: 2017-03-07 Created: 2017-03-07 Last updated: 2017-03-07Bibliographically approved
Larsson, O., Benghin, V. V., Berger, T., Casolino, M., Di Fino, L., Fuglesang, C., . . . Zaconte, V. (2015). Measurements of heavy-ion anisotropy and dose rates in the Russian section of the International Space Station with the Sileye-3/Alteino detector. Journal of Physics G: Nuclear and Particle Physics, 42(2), 025002
Open this publication in new window or tab >>Measurements of heavy-ion anisotropy and dose rates in the Russian section of the International Space Station with the Sileye-3/Alteino detector
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2015 (English)In: Journal of Physics G: Nuclear and Particle Physics, ISSN 0954-3899, E-ISSN 1361-6471, Vol. 42, no 2, p. 025002-Article in journal (Refereed) Published
Abstract [en]

In this work we present data on linear energy transfer (LET), dose and dose equivalent rates from different locations of the Russian part of the International Space Station (ISS) measured by the Sileye-3/Alteino detector. Data were taken as part of the ESA ALTCRISS project from late 2005 through 2007. The LET rate data shows a heavy-ion (LET > 50 keV/mu m) anisotropy. From the heavy-ion LET rate in the Zvezda service module we find ISS (y) over cap (Starboard) and (z) over cap (Nadir) to be about 10-15 times higher than in (x) over cap (Forward). The situation is similar for dose and dose equivalent rates, ranging from 25-40 mu Gy d(-1) in (x) over cap to about 75 mu Gy d(-1) in (z) over cap, whereas for the dose equivalent the rate peaks in (y) over cap with around 470 mu Sv d(-1). The heavy-ion anisotropy confirms what has been reported by the ALTEA collaboration. Measurements using two sets of passive detectors, DLR-TLDs and PADLES (TLD+CR-39), have also been performed in conjunction with Alteino measurements, both shielded and unshielded. The passive detectors register a dose rate about 3-5 times as high as Alteino, 260-280 mu Gy d(-1) for PADLES and 200-260 mu Gy d(-1) for DLR-TLDs. For the dose equivalent PADLES measurements ranges from 560-740 mu Sv d(-1).

Keywords
Alteino, ISS, dose, dose equivalent, LET, heavy ion
National Category
Subatomic Physics
Identifiers
urn:nbn:se:kth:diva-160376 (URN)10.1088/0954-3899/42/2/025002 (DOI)000348130400003 ()2-s2.0-84921444424 (Scopus ID)
Funder
Swedish National Space Board
Note

QC 20150226

Available from: 2015-02-26 Created: 2015-02-19 Last updated: 2017-12-04Bibliographically approved
Fuglesang, C., Capel, F., Casolino, M., Klimov, P., Larsson, O. & Ricci, M. (2015). Mini-euso inside iss to prepare for studying ultra-high energy particles from the outside. In: Proceedings of the International Astronautical Congress, IAC: . Paper presented at 66th International Astronautical Congress 2015: Space - The Gateway for Mankind's Future, IAC 2015, 12 October 2015 through 16 October 2015 (pp. 3998-4002). International Astronautical Federation
Open this publication in new window or tab >>Mini-euso inside iss to prepare for studying ultra-high energy particles from the outside
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2015 (English)In: Proceedings of the International Astronautical Congress, IAC, International Astronautical Federation, 2015, p. 3998-4002Conference paper, Published paper (Refereed)
Abstract [en]

The Mini-EUSO (Extreme Universe Space Observatory) is a small UV telescope to be placed inside the Zvezda module of ISS in 2017, as a part of the work of the JEM-EUSO collaboration. The Mini-EUSO instrument will be equipped with one full original JEM-EUSO Photo-Detector-Module (PDM), an optical system made of two Fresnel lenses (25 cm in diameter) and a data acquisition system. The Mini-EUSO instrument serves as a pathfinder towards the goals of the full JEM-EUSO mission: to place a large instrument on the outside of ISS to study Ultra-High Energy Cosmic Rays (UHECR) with energies of E &gt; 3×1019 eV. This can be achieved by measuring the light in the UV range from the Extensive Air Showers (EAS) that these particles trigger in the atmosphere [1]. By using the ISS altitude to monitor a target volume far greater than is possible from the ground, unprecedented statistical accuracy of the primary energy, arrival direction and composition of UHECRs will be obtained. Such data will shed light on the origin of the UHECRs, on the sources that are producing them, on the propagation environment from the source to the Earth and, possibly, on the particle physics mechanisms at energies well beyond those achievable in man-made accelerators. Moreover, there are exploratory objectives such as constraining the galactic and extragalactic magnetic fields, the detection of extreme energy neutrinos and gamma rays, the verification of special relativity at extremely large Lorentz factors, the examination of possible quantum gravity effects at extreme energies and the systematic surveillance of atmospheric phenomena. The Mini-EUSO instrument will have 2, 304 pixels from 36 multi-anode PMTs with each pixel viewing an equivalent area of 5.4 × 5.4 km2 on ground. The full field of view is ±19° and the instrument has a time resolution of 2.5 μs. The Mini-EUSO mission has at least four different objectives: (1) to raise the technical readiness level of JEM-EUSO to the highest grade, (2) to perform an absolute calibration of the multi-anode photomultipliers in flight (crucial for JEM-EUSO), (3) to take advantage of being at ISS altitude, like JEM-EUSO, and study in a precise way the UV background coming from Earth in all the different reflective conditions (water, earth, vegetation, snow, etc.) and (4) to study atmospheric phenomena, such as lightning, and related light, as well as meteors.

Place, publisher, year, edition, pages
International Astronautical Federation, 2015
Keywords
Anodes, Cosmology, Data acquisition, Electrodes, Gamma rays, Gravitation, Lenses, Optical systems, Pixels, Reconfigurable hardware, Relativity, Absolute calibration, Atmospheric phenomena, Data acquisition system, Extensive air showers, Extragalactic magnetic fields, Multi-anode photomultipliers, Propagation environment, Ultrahigh-energy cosmic rays, Cosmic rays
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-202898 (URN)2-s2.0-84991746969 (Scopus ID)9781510818934 (ISBN)
Conference
66th International Astronautical Congress 2015: Space - The Gateway for Mankind's Future, IAC 2015, 12 October 2015 through 16 October 2015
Note

QC 20170308

Available from: 2017-03-08 Created: 2017-03-08 Last updated: 2017-03-08Bibliographically approved
Topchiev, N. P., Galper, A. M., Bonvicini, V., Adriani, O., Aptekar, R. L., Arkhangelskaja, I. V., . . . Yurkin, Y. T. (2015). The GAMMA-400 experiment: Status and prospects. Bulletin of the Russian Academy of Sciences: Physics, 79(3), 417-420
Open this publication in new window or tab >>The GAMMA-400 experiment: Status and prospects
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2015 (English)In: Bulletin of the Russian Academy of Sciences: Physics, ISSN 1062-8738, Vol. 79, no 3, p. 417-420Article in journal (Refereed) Published
Abstract [en]

The development of the GAMMA-400 γ-ray telescope continues. The GAMMA-400 is designed to measure fluxes of γ-rays and the electron-positron cosmic-ray component possibly associated with annihilation or decay of dark matter particles; and to search for and study in detail discrete γ-ray sources, to measure the energy spectra of Galactic and extragalactic diffuse γ-rays, and to study γ-ray bursts and γ-rays from the active Sun. The energy range for measuring γ-rays and electrons (positrons) is from 100 MeV to 3000 GeV. For 100-GeV γ-rays, the γ-ray telescope has an angular resolution of ∼0.01°, an energy resolution of ∼1%, and a proton rejection factor of ∼5 × 105. The GAMMA-400 will be installed onboard the Russian Space Observatory.

National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-167000 (URN)10.3103/S1062873815030429 (DOI)2-s2.0-84928111559 (Scopus ID)
Note

QC 20150609

Available from: 2015-06-09 Created: 2015-05-21 Last updated: 2015-06-09Bibliographically approved
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Identifiers
ORCID iD: ORCID iD iconorcid.org/0000-0002-0406-0962

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