Application specific integrated circuits for ANTARES offshore front-end electronics

Lachartre, D.; Feinstein, F.

doi:10.1016/s0168-9002(99)01205-x

Cited by 25 publications

(14 citation statements)

References 3 publications

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“…The 900 PMTs foreseen for the ANTARES detector have been selected and fully characterized to work with a threshold below the single photo-electron level with a mean transit time spread (TTS) of σ ∼ 1.3 ns (FWHM ∼ 3.0 ns) [3]. The PMT signal is processed by the Analogue Ring Sampler (ARS) ASIC which measures the arrival time and charge of the pulse [7]. Only this information is sent to shore in the case where it is compatible with a single photo-electron (SPE) pulse, while the ARS can perform a full digitisation of the PMT signal for larger amplitudes.…”

Section: The Optical Module Datamentioning

confidence: 99%

First results of the Instrumentation Line for the deep-sea ANTARES neutrino telescope

Aguilar

Albert

Ameli

et al. 2006

Astroparticle Physics

105

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18 pages, 12 figures, submitted to Astroparticle PhysicsIn 2005, the ANTARES Collaboration deployed and operated at a depth of 2500 m a so-called Mini Instrumentation Line equipped with Optical Modules (MILOM) at the ANTARES site. The various data acquired during the continuous operation from April to December 2005 of the MILOM confirm the satisfactory performance of the Optical Modules, their front-end electronics and readout system, as well as the calibration devices of the detector. The in-situ measurement of the Optical Module time response yields a resolution better than 0.5 ns. The performance of the acoustic positioning system, which enables the spatial reconstruction of the ANTARES detector with a precision of about 10 cm, is verified. These results demonstrate that with the full ANTARES neutrino telescope the design angular resolution of better than $0.3^\circ$ can be realistically achieved

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Section: The Optical Module Datamentioning

confidence: 99%

First results of the Instrumentation Line for the deep-sea ANTARES neutrino telescope

Aguilar

Albert

Ameli

et al. 2006

Astroparticle Physics

105

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“…In order to meet the demands of next-generation IACT arrays for very-high-energy (VHE) gamma-ray astronomy, we draw upon this ASIC development experience to optimize the design of such highly integrated, cost-effective readout. The TARGET ASIC can be compared with the ARS (Analogue Ring Sampler) ASIC [12,13] used for ANTARES and H.E.S.S. I readout and the SAM (Swift Analogue Memory) ASIC [14] used for H.E.S.S.…”

Section: Introductionmentioning

confidence: 99%

TARGET: A multi-channel digitizer chip for very-high-energy gamma-ray telescopes

Bechtol

Funk

Okumura

et al. 2012

Astroparticle Physics

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The next-generation very-high-energy (VHE) gamma-ray observatory, the Cherenkov Telescope Array, will feature dozens of imaging atmospheric Cherenkov telescopes (IACTs), each with thousands of pixels of photo-sensors. To be affordable and reliable, reading out such an array of up to a million channels requires event recording technology that is highly integrated and modular, with a low cost per channel. We present the design and performance of a chip targeted to this application: the TeV Array Readout with GSa/s sampling and Event Trigger (TARGET). This application-specific integrated circuit (ASIC) has 16 parallel input channels, a 4096-sample buffer for each channel, adjustable input termination, self-trigger functionality, and tight window-selected readout. We report the performance of the first-generation version of this chip (TARGET 1) in terms of sampling frequency, power consumption, dynamic range, current-mode gain, analog bandwidth, and cross talk. The large number of channels per chip allows a low cost per channel ($10 to $20 including front-end and back-end electronics but not including photosensors) to be achieved with a TARGET-based IACT readout system. In addition to basic performance parameters of the TARGET 1 chip, we present a camera module prototype as well as a second-generation chip (TARGET 2), both of which have now been produced.

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“…5 shows the charge distribution obtained through the high gain channel when a PMT receives an amount of light which results in the occasional emission of one 14 photo-electron. 15 Analogue to Digital Converter. The input range is 0-2 V and the output digital is in the range ±2048 (decimal).…”

Section: Analogue Memory Boardsmentioning

confidence: 99%

The camera of the fifth H.E.S.S. telescope. Part I: System description

Bolmont

Corona

Gauron

et al. 2014

Nuclear Instruments and Methods in Physics Research Section A:

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In July 2012, as the four ground-based gamma-ray telescopes of the H.E.S.S. (High Energy Stereoscopic System) array reached their tenth year of operation in Khomas Highlands, Namibia, a fifth telescope took its first data as part of the system. This new Cherenkov detector, comprising a 614.5 m^2 reflector with a highly pixelized camera in its focal plane, improves the sensitivity of the current array by a factor two and extends its energy domain down to a few tens of GeV. The present part I of the paper gives a detailed description of the fifth H.E.S.S. telescope's camera, presenting the details of both the hardware and the software, emphasizing the main improvements as compared to previous H.E.S.S. camera technology.Comment: 16 pages, 13 figures, accepted for publication in NIM

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Application specific integrated circuits for ANTARES offshore front-end electronics

Cited by 25 publications

References 3 publications

First results of the Instrumentation Line for the deep-sea ANTARES neutrino telescope

First results of the Instrumentation Line for the deep-sea ANTARES neutrino telescope

TARGET: A multi-channel digitizer chip for very-high-energy gamma-ray telescopes

The camera of the fifth H.E.S.S. telescope. Part I: System description

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