Search for point sources of gamma radiation above 15 TeV with the HEGRA AIROBICC array

Aharonian, F.; Akhperjanian, A. G.; Barrio, J. A.; Bernlöhr, K.; Börst, H.; Bojahr, H.; Bolz, O.; Contreras, J. L.; Cortina, J.; Denninghoff, S.; Fonseca, V.; Gebauer, H. J.; Gonzalez, J.; Götting, N.; Heinzelmann, G.; Hermann, G.; Heusler, Andréas; Hofmann, W.; Horns, D.; Jung, I.; Kankanyan, R.; Kestel, M.; Kettler, J.; Kohnle, Antje; Konopelko, A.; Kornmayer, H.; Kranich, D.; Krawczynski, H.; Lampeitl, H.; López, M.; Lorenz, E.; Lucarelli, F.; Magnussen, N.; Mang, O.; Meyer, H.; Mirzoyan, R.; Moralejo, A.; Oña, E.; Padilla, L.; Panter, M.; Plaga, R.; Plyasheshnikov, A.; Prahl, J.; Pühlhofer, G.; Rauterberg, Matthias; Röhring, A.; Rhode, W.; Rowell, G.; Sahakian, V.; Samorski, M.; Schilling, M.; Schmele, D.; Schröder, Frank G.; Sevilla-Noarbe, I.; Siems, M.; Stamm, W.; Tluczykont, M.; Völk, H. J.; Wiedner, C. A.; Wittek, W.

doi:10.1051/0004-6361:20020686

Cited by 29 publications

(15 citation statements)

References 25 publications

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“…An IACT can only spend up to ∼200 hours per year observing a single interesting source due The CTA-South sensitivity to sky survey [19,20] is also shown. Upper limits to ultra high-energy gamma-ray emission set by different experiments in the Northern hemisphere are also reported [21,22,23,24].…”

Section: Motivation For a Multi-tev (>10 Tev) γ-Ray Tele-mentioning

confidence: 96%

The LHAASO experiment: From Gamma-Ray Astronomy to Cosmic Rays

Sciascio

2016

Nuclear and Particle Physics Proceedings

113

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LHAASO is expected to be the most sensitive project to face the open problems in Galactic cosmic ray physics through a combined study of photon-and charged particle-induced extensive air showers in the energy range 10 11 -10 17 eV. This new generation multi-component experiment will be able of continuously surveying the gamma-ray sky for steady and transient sources from about 100 GeV to PeV energies, thus opening for the first time the 10 2 -10 3 TeV range to the direct observations of the high energy cosmic ray sources.In addition, the different observables (electronic, muonic and Cherenkov components) that will be measured in LHAASO will allow the study of the origin, acceleration and propagation of the radiation through a measurement of energy spectrum, elemental composition and anisotropy with unprecedented resolution. The installation of the experiment started at very high altitude in China (Daocheng site, Sichuan province, 4410 m a.s.l.). The commissioning of one fourth of the detector will be implemented in 2018. The completion of the installation is expected by the end of 2021.

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Section: Motivation For a Multi-tev (>10 Tev) γ-Ray Tele-mentioning

confidence: 96%

The LHAASO experiment: From Gamma-Ray Astronomy to Cosmic Rays

Sciascio

2016

Nuclear and Particle Physics Proceedings

113

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“…Since an IACT can only spend up to ∼200 hours per year observing a single source due to solar [38,39] is also shown. Upper limits to ultra high-energy gamma-ray emission set by different experiments in the Northern hemisphere are also reported [40,41,42,43]. and lunar constraints, this means that even with the maximum exposure, an IACT still wouldn't be able to match LHAASO sensitivity above a few tens TeV.…”

Section: The Lhaaso Experimentsmentioning

confidence: 97%

“…The reduced observation time causes an increase of the minimum detectable flux, as shown in the blue band of Fig.4, where the lower limit of the band refers to a Galactic plane survey and the upper limit to an all sky survey of π sr [38,39]. In Fig.4 the upper limits set by different experiments to high energy gamma-ray emission in the Northern hemisphere are reported [40,41,42,43]. In five years of observations, the CASA-MIA experiment sets the lowest upper limits to the flux from the Crab Nebula around and above 100 TeV [43].…”

Section: The Lhaaso Experimentsmentioning

confidence: 99%

Future Ground-based Wide Field of View Air Shower Detectors

Sciascio¹

2018

Proceedings of XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF2017)

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Extensive air shower (EAS) arrays directly sample the shower particles that reach the observation altitude. They are wide field of view (FoV) detectors able to view the whole sky simultaneously and continuously. In fact, EAS arrays have an effective FoV of about 2 sr and operate with a duty cycle of ∼100%. This capability makes them well suited to study extended sources, such as the Galactic diffuse emission and measure the spectra of Galactic sources at the highest energies (near or beyond 100 TeV). Their sensitivity in the sub-TeV/TeV energy domain cannot compete with that of Cherenkov telescopes, but the wide FoV is ideal to perform unbiased sky surveys, discover transients or explosive events (GRBs) and monitor variable or flaring sources such as Active Galactic Nuclei (AGN). An EAS array is able to detect at the same time events induced by photons and charged cosmic rays, thus studying the connection between these two messengers of the nonthermal Universe. Therefore, these detectors are, by definition, multi-messenger instruments. Wide FoV telescopes are crucial for a multi-messenger study of the Gravitational Wave events due to their capability to survey simultaneously all the large sky regions identified by LIGO and VIRGO, looking for a possible correlated γ-ray emission. In this contribution we summarize the scientific motivations which push the construction of new wide FoV air shower detectors and introduce the future instruments currently under installation. Finally, we emphasize the need of an EAS array in the Southern hemisphere to monitor the Inner Galaxy and face a number of important open problems.

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“…Many experiments have already looked for an excessive intensity of CR from this region and found nothing. [37][38][39][40][41][42][43][44][45][46] Nevertheless the situation is controversial, since recently the Moscow University 47 and Tien-Shan 48 groups revealed weak EAS excesses in the Monogem Ring area. If there are indeed CR excesses at sub-PeV and PeV energies from the Monogem Ring region they can evidence for the activity of the pulsar B0656+14 which emitted high energy CR soon after its birth and which were confined within the SNR for a long time of about 80 kyear.…”

Section: Status Of the Single Source Modelmentioning

confidence: 99%

Models and Phenomenology

Erlykin¹

2005

Int. J. Mod. Phys. A

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It is evident that models of the knee should match the observational phenomenology. In this talk I discuss a few aspects of phenomenology, which are important not only for the understanding of the knee origin, but also for the general problem of the origin of cosmic rays. Among them are the shape of the energy spectrum, its irregularity, the sharpness of the knee and its fine structure. The classification of models is given and some examples of the most recent models are discussed. The most probable conclusion deduced from this examination is that the knee has an astrophysical origin and the so called 'source' models of the knee are most likely among them.

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Search for point sources of gamma radiation above 15 TeV with the HEGRA AIROBICC array

Cited by 29 publications

References 25 publications

The LHAASO experiment: From Gamma-Ray Astronomy to Cosmic Rays

The LHAASO experiment: From Gamma-Ray Astronomy to Cosmic Rays

Future Ground-based Wide Field of View Air Shower Detectors

Models and Phenomenology

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