The time structure of Cherenkov images generated by TeV γ-rays and by cosmic rays

Heß, M.; Bernlöhr, K.; Daum, A.; Hemberger, M.; Hermann, G.; Hofmann, W.; Lampeitl, H.; Aharonian, F.; Akhperjanian, A. G.; Barrio, J. A.; Beteta, J. J. G.; Contreras, J. L.; Cortina, J.; Deckers, T.; Fernández, J.; Fonseca, V.; Gonzalez, J.; Heinzelmann, G.; Heusler, Andréas; Hohl, H.; Holl, I.; Horns, D.; Kankanyan, R.; Kestel, M.; Kirstein, O.; Köhler, Christian; Konopelko, A.; Kornmayer, H.; Kranich, D.; Krawczynski, H.; Lindner, A.; Lorenz, E.; Magnussen, N.; Meyer, H.; Mirzoyan, R.; Moralejo, A.; Padilla, L.; Panter, M.; Petry, D.; Plaga, R.; Prahl, J.; Prosch, C.; Pühlhofer, G.; Rauterberg, Matthias; Rhode, W.; Röhring, A.; Samorski, M.; Sánchez, J.; Schmele, D.; Schröder, Frank G.; Stamm, W.; Völk, H. J.; Wiebel-Sooth, B.; Wiedner, C. A.; Willmer, M.

doi:10.1016/s0927-6505(99)00003-1

Cited by 16 publications

(8 citation statements)

References 10 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The arrival time of Cherenkov photons, however, does improve discrimination somewhat -an aspect of the analysis that becomes more important with the development of very large isochronous reflectors, and very fast (≥ 1 GHz) sampling electronics. [51][52][53]…”

Section: Alternative Analysis Methodsmentioning

confidence: 99%

Atmospheric Cherenkov Gamma-ray Telescopes

Holder¹

2015

Preprint

View full text Add to dashboard Cite

The stereoscopic imaging atmospheric Cherenkov technique, developed in the 1980s and 1990s, is now used by a number of existing and planned gamma-ray observatories around the world. It provides the most sensitive view of the very high energy gamma-ray sky (above 30 GeV), coupled with relatively good angular and spectral resolution over a wide field-of-view. This Chapter summarizes the details of the technique, including descriptions of the telescope optical systems and cameras, as well as the most common approaches to data analysis and gammaray reconstruction.

show abstract

Section: Alternative Analysis Methodsmentioning

confidence: 99%

Atmospheric Cherenkov Gamma-ray Telescopes

Holder¹

2015

Preprint

View full text Add to dashboard Cite

show abstract

“…The anticipated size and weight are about 50 Â 20 Â 20 cm 3 and roughly 11 kg, respectively. All boards are powered by the 24 V that are also used for supplying the 7-pixel clusters.…”

Section: The L2 Cratementioning

confidence: 99%

“…CTA will cover the energy range from few tens of GeV up to hundreds of TeV with a sensitivity at 1 TeV that is a factor of 10 better than achieved by the current-generation experiments H.E.S.S., 1 MAGIC, 2 and VERITAS. 3 It will also provide a good energy (about 10-15%) and angular resolution (on the arcmin scale) for reconstructed photons. Currently considered array designs (see, for example, [2]) deploy a mixture of large-size telescopes (LSTs), medium-size telescopes (MSTs), and small-size telescopes (SSTs), with typical reflector diameters of 23 m, 12 m, and 4 m, respectively, on an area of roughly 1-10 km 2 in order to ensure good performance over four orders of magnitude in photon energy.…”

Section: Introductionmentioning

confidence: 99%

“…Typical γ-rays generate a Cherenkov light-flash of a few nanosecond duration in spatially neighbouring pixels, but at high energies ð c 1 TeVÞ and large impact distances of the shower with respect to the telescope the camera image acquires a substantial time-gradient [3] and can last several 10 ns. The background is dominated by the diffuse night-sky background (NSB) light from natural and artificial light sources, resulting in pixel count rates of O(100 MHz) at single photoelectron (p.e.)…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A versatile digital camera trigger for telescopes in the Cherenkov Telescope Array

Schwanke

Shayduk²,

Sulanke³

et al. 2015

Nuclear Instruments and Methods in Physics Research Section A:

View full text Add to dashboard Cite

a b s t r a c tThis paper describes the concept of an FPGA-based digital camera trigger for imaging atmospheric Cherenkov telescopes, developed for the future Cherenkov Telescope Array (CTA). The proposed camera trigger is designed to select images initiated by the Cherenkov emission of extended air showers from very-high energy (VHE, E 420 GeV) photons and charged particles while suppressing signatures from background light. The trigger comprises three stages. A first stage employs programmable discriminators to digitize the signals arriving from the camera channels (pixels). At the second stage, a grid of low-cost FPGAs is used to process the digitized signals for camera regions with 37 pixels. At the third stage, trigger conditions found independently in any of the overlapping 37-pixel regions are combined into a global camera trigger by few central FPGAs. Trigger prototype boards based on Xilinx FPGAs have been designed, built and tested and were shown to function properly. Using these components a full camera trigger with a power consumption and price per channel of about 0.5 W and 19 €, respectively, can be built. With the described design the camera trigger algorithm can take advantage of pixel information in both the space and the time domain allowing, for example, the creation of triggers sensitive to the timegradient of a shower image; the time information could also be exploited to online adjust the time window of the acquisition system for pixel data. Combining the results of the parallel execution of different trigger algorithms (optimized, for example, for the lowest and highest energies, respectively) on each FPGA can result in a better response over all photons energies (as demonstrated by Monte Carlo simulation in this work).

show abstract

“…The detection of Very High Energy (VHE) gamma photons is possible by observing the Cherenkov light produced by the relativistic secondary particles in the air shower generated by the interaction with the Earth atmosphere. This light, emitted in the ultraviolet band within a cone of about 1.3 • , reaches the ground in a " pool " having a radius of ∼120 m. It is very faint and lasts only a few ns with a duration that depends mainly on the distance between the shower core and the telescope axis [4].…”

Section: Introductionmentioning

confidence: 99%

Characterization of EASIROC as front-end for the readout of the SiPM at the focal plane of the Cherenkov telescope ASTRI

Impiombato¹,

Giarrusso²,

Mineo³

et al. 2013

Nuclear Instruments and Methods in Physics Research Section A:

View full text Add to dashboard Cite

The Extended Analogue Silicon Photo-multiplier Integrated Read Out Chip, EASIROC, is a chip proposed as front-end of the camera at the focal plane of the imaging Cherenkov ASTRI SST-2M telescope prototype. This paper presents the results of the measurements performed to characterize EASIROC in order to evaluate its compliance with the ASTRI SST-2M focal plane requirements.In particular, we investigated the trigger time walk and the jitter effects as a function of the pulse amplitude. The EASIROC output signal is found to vary linearly as a function of the input pulse amplitude with very low level of electronic noise and cross-talk (<1%). Our results show that it is suitable as front-end chip for the camera prototype, although, specific modifications are necessary to adopt the device in the final version of the telescope.

show abstract

The time structure of Cherenkov images generated by TeV γ-rays and by cosmic rays

Cited by 16 publications

References 10 publications

Atmospheric Cherenkov Gamma-ray Telescopes

Atmospheric Cherenkov Gamma-ray Telescopes

A versatile digital camera trigger for telescopes in the Cherenkov Telescope Array

Characterization of EASIROC as front-end for the readout of the SiPM at the focal plane of the Cherenkov telescope ASTRI

Contact Info

Product

Resources

About