press_release_en
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| {{ :wiki:swgo_pressimages_sky_light.png?nolink |Gamma-ray sky image as seen by the (current) HAWC and (future) SWGO observatories}} | {{ :wiki:swgo_pressimages_sky_light.png?nolink |Gamma-ray sky image as seen by the (current) HAWC and (future) SWGO observatories}} | ||
| - | //Gamma-ray sky image as seen by the (current) HAWC and (future) SWGO observatories (Credit: Richard White ,MPIK)// | + | //Gamma-ray sky image as seen by the (current) HAWC and (future) SWGO observatories (Credit: Richard White, MPIK)// |
| The baseline for the new observatory will be the approach of the current ground-based gamma-ray detectors, namely HAWC in Mexico and LHAASO in China. In particular, water Cherenkov detectors will be used to sample the particle showers produced by gamma rays in the atmosphere, by recording the light produced when particles pass through tanks full of purified water. New layouts and technologies will however be explored in order to increase the sensitivity and lower the energy threshold of the observatory. | The baseline for the new observatory will be the approach of the current ground-based gamma-ray detectors, namely HAWC in Mexico and LHAASO in China. In particular, water Cherenkov detectors will be used to sample the particle showers produced by gamma rays in the atmosphere, by recording the light produced when particles pass through tanks full of purified water. New layouts and technologies will however be explored in order to increase the sensitivity and lower the energy threshold of the observatory. | ||
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| Direct detection of primary gamma-rays is only possible with satellite-based detectors, such as Fermi. However, the cost of space technology limits the size of satellite-borne detectors, and thus their sensitivity, as fluxes become too small at higher energies. In the atmosphere, gammas interact creating a shower of particles. These showers can be studied in observatories of two complementary types: imaging atmospheric Cherenkov telescopes, pointing instruments such as CTA, and high altitude air shower arrays, such as SWGO. Cherenkov telescopes are highly sensitive pointing detectors, with high precision but limited duty cycle and narrow field-of-view, benefiting from pointing alerts provided by complementary observatories. Wide field-of-view observations from the ground have the highest energy reach, and are ideal to search for transient sources and for emissions from very extended regions of the sky. | Direct detection of primary gamma-rays is only possible with satellite-based detectors, such as Fermi. However, the cost of space technology limits the size of satellite-borne detectors, and thus their sensitivity, as fluxes become too small at higher energies. In the atmosphere, gammas interact creating a shower of particles. These showers can be studied in observatories of two complementary types: imaging atmospheric Cherenkov telescopes, pointing instruments such as CTA, and high altitude air shower arrays, such as SWGO. Cherenkov telescopes are highly sensitive pointing detectors, with high precision but limited duty cycle and narrow field-of-view, benefiting from pointing alerts provided by complementary observatories. Wide field-of-view observations from the ground have the highest energy reach, and are ideal to search for transient sources and for emissions from very extended regions of the sky. | ||
| {{ :wiki:swgo_pressimages_detector_light_tank.png?nolink |Illustration of the complementary detection techniques of high-energy gamma rays on ground}} | {{ :wiki:swgo_pressimages_detector_light_tank.png?nolink |Illustration of the complementary detection techniques of high-energy gamma rays on ground}} | ||
| - | //Illustration of the complementary detection techniques of high-energy gamma rays on ground. (Credit: Richard White ,MPIK)// | + | //Illustration of the complementary detection techniques of high-energy gamma rays on ground. (Credit: Richard White, MPIK)// |
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| + | Contacts (PIs representing the scientific communities of the different countries) | ||
| + | * Argentina: Adrian Rovero, Instituto de Astronomía y Física del Espacio | ||
| + | * Brazil: Ronald Shellard, Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, | ||
| + | * Czech Republic: Jakub Vicha, Institute of Physics of the Czech Academy of Sciences in Prague | ||
| + | * Germany: Jim Hinton, Max Planck Institute for Nuclear Physics, Heidelberg, | ||
| + | * Italy: Alessandro De Angelis, University Udine/Padua and INFN Padua, +39 320 4366230 | ||
| + | * Mexico: Andre Sandoval, UNAM, Cidade do Mexico | ||
| + | * Portugal: Mário Pimenta, LIP/IST, Lisboa, +351 93 6992234 | ||
| + | * UK : Jon Lapington, Univ. Leicester | ||
| + | * USA: Petra Huentemeyer, Michigan Technological University | ||
press_release_en.txt · Last modified: 2019/07/01 16:19 by swgowikiadmin
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