dorsal/arxiv
View SchemaUV Light Shower Simulator for Fluorescence and Cerenkov Radiation Studies
| Authors | P. Gorodetzky, J. Dolbeau, T. Patzak, J. Waisbard, C. Boutonnet |
|---|---|
| Categories | |
| ArXiv ID | physics/0507138 |
| URL | https://arxiv.org/abs/physics/0507138 |
| Journal | Dans Proceedings of the 29th International Cosmic Ray Conference. - ICRC 2005 29th International Cosmic Ray Conference, Pune : Inde (2005) |
Abstract
All experiments observing showers light use telescopes equipped with pixellised photodetectors. Monte-Carlo (MC) simulations of the apparatus operation in various situations (background light, shower energy, proximity of tracks...) are mandatory, but never enter into detector details like pulse shape, dead-time, or charge space effects which are finally responsible for the data quality. An apparatus where each pixel receives light from individual 370 nm UV LEDs through silica fibers is being built. The LEDs receive voltage through DACs, which get their input (which pixel, at what time, which amplitude) from a shower plus noise generator code. The typical time constant of a shower being one $/mu$s (300 m for light), the pulses are one $/mu$s wide. This is rather long compared to the intrinsic time constant (around 10 ns) of the light detectors, hence, these see "constant light" changing every $/mu$s. This is where important loading effects which are not included in MC code can be observed. The fibers illuminate the pixels through a diffuser, and each fiber illuminates only one pixel. The number of equipped pixels is such that it englobes a full shower (much less than the full focal surface). Finally, this equipment can be used also to calibrate the pixels.
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"abstract": "All experiments observing showers light use telescopes equipped with\npixellised photodetectors. Monte-Carlo (MC) simulations of the apparatus\noperation in various situations (background light, shower energy, proximity of\ntracks...) are mandatory, but never enter into detector details like pulse\nshape, dead-time, or charge space effects which are finally responsible for the\ndata quality. An apparatus where each pixel receives light from individual 370\nnm UV LEDs through silica fibers is being built. The LEDs receive voltage\nthrough DACs, which get their input (which pixel, at what time, which\namplitude) from a shower plus noise generator code. The typical time constant\nof a shower being one $/mu$s (300 m for light), the pulses are one $/mu$s wide.\nThis is rather long compared to the intrinsic time constant (around 10 ns) of\nthe light detectors, hence, these see \"constant light\" changing every $/mu$s.\nThis is where important loading effects which are not included in MC code can\nbe observed. The fibers illuminate the pixels through a diffuser, and each\nfiber illuminates only one pixel. The number of equipped pixels is such that it\nenglobes a full shower (much less than the full focal surface). Finally, this\nequipment can be used also to calibrate the pixels.",
"arxiv_id": "physics/0507138",
"authors": [
"P. Gorodetzky",
"J. Dolbeau",
"T. Patzak",
"J. Waisbard",
"C. Boutonnet"
],
"categories": [
"physics.ins-det",
"astro-ph"
],
"journal_ref": "Dans Proceedings of the 29th International Cosmic Ray Conference.\n - ICRC 2005 29th International Cosmic Ray Conference, Pune : Inde (2005)",
"title": "UV Light Shower Simulator for Fluorescence and Cerenkov Radiation Studies",
"url": "https://arxiv.org/abs/physics/0507138"
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