Performance and applications of the UVscope instrument

Maccarone, M. C.; Catalano, O.; Giarrusso, S.; Rosa, G. La; Segreto, A.; Agnetta, G.; Biondo, B.; Mangano, A.; Russo, F.; Billotta, S.

doi:10.1016/j.nima.2011.08.004

Cited by 23 publications

(21 citation statements)

References 5 publications

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“…Maria Concetta Maccarone 5 measure, in single photon counting mode, light flux with spectral acceptance matching the ones of the ASTRI camera [27]. Placed onto the primary mirror support and co-axial to the telescope receiving the light from the Illuminator, the UVscope will monitor the flux reaching the ASTRI aperture; this allows to completely eliminate the uncertainty due to the atmospheric transmission and propagation, so reaching an absolute telescope calibration.…”

Section: Astri For the Cherenkov Telescope Arraymentioning

confidence: 99%

“…Using different illumination features (wavelength, intensity, pulse length) as well as changing the telescope pointing towards the Illuminator, several calibration purposes can be accomplished [26]. UVscope is a well-tested stand-alone NIST-calibrated multi-pixels photon detector, remotely controlled, designed to measure, in single photon counting mode, light flux with spectral acceptance matching the ones of the ASTRI camera [27]. Placed onto the primary mirror support and co-axial to the telescope receiving the light from the Illuminator, the UVscope will monitor the flux reaching the ASTRI aperture; this allows to completely eliminate the uncertainty due to the atmospheric transmission and propagation, so reaching an absolute telescope calibration.…”

Section: 1mentioning

confidence: 99%

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ASTRI for the Cherenkov Telescope Array

Maccarone¹

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The Cherenkov Telescope Array (CTA) will be the largest ground-based observatory operating in the very-high-energy gamma-ray (20 GeV -300 TeV) range. It will be based on more than one hundred telescopes, located at two sites (in the northern and southern hemispheres). The energy coverage, in the southern CTA array, will extend up to hundreds of TeV thanks to 70 small size telescopes (SST), with their primary mirrors of about 4 meters in diameter and large field of view of the order of 9 degrees. It is proposed that one of the first sets of precursors for the CTA SSTs array will be represented by (at least) nine ASTRI telescopes. The prototype of such telescopes, named ASTRI SST-2M, is installed in Italy. It is currently completing the overall commissioning before entering the science verification phase that will performed observing bright TeV sources as Crab Nebula, Mrk421 and Mrk 501. This science verification phase will cross-check the prototype performance with the predictions of detailed Monte Carlo simulations.ASTRI telescopes are characterized by a dual-mirror optical design based on the SchwarzschildCouder (SC) configuration. The focal-plane camera is curved in order to fit the ideal prescription for the SC design and the sensors are small size silicon photomultipliers read-out by a fast front-end electronics. The telescope prototype installed in Italy, has been developed by the Italian National Institute for Astrophysics, INAF, following an end-to-end approach that comprises all aspects from the design, construction and implementation of the entire hardware and software system to the final scientific products. In this respect, the internal and external calibration systems, control/acquisition hardware and software, data reduction and analysis software, and data archiving system are being realized in addition to the telescope structure and camera. All parts of the system have been designed to comply with the CTA requirements. A collaborative effort, addressed to the implementation of the first ASTRI telescopes for the CTA southern site, is now on-going led by INAF with the Universidade de Sao Paulo (Brazil), the North-West University (South Africa) and the Italian National Institute for Nuclear Physics, INFN. In this contribution we will describe the main features of the ASTRI telescopes, the latest news from their prototype, its performance and the expectations of the first set of ASTRI telescopes proposed for CTA. [1,2] is the next generation ground-based observatory for gamma-ray astronomy at very high energies. With more than one hundred Cherenkov telescopes located in two sites, one for each hemisphere, assuring full sky coverage, CTA will detect very high energy radiation with unprecedented accuracy and sensitivity better than current Image Atmospheric Cherenkov Technique (IACT) experiments. Three different classes of telescopes (LST, MST, SST, that is large, medium and small, so defined with respect to their collecting mirror size) will have different field-of-views and are designed to access diff...

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Section: Astri For the Cherenkov Telescope Arraymentioning

confidence: 99%

Section: 1mentioning

confidence: 99%

ASTRI for the Cherenkov Telescope Array

Maccarone¹

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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“…Moreover, as in the ASTRI SST-2M prototype absolute calibration strategy [14] for which purpose the first Illuminator has been developed, this instrument can be accompanied by a small device used as a further reference. Details of such a device, named UVscope, are given in [15]. In brief, UVscope is a well-tested stand-alone portable NIST-calibrated multi-pixels photon detector, remotely controlled, designed to measure, in single photon counting mode, light flux with spectral acceptance matching the ones of the CTA cameras.…”

Section: Calibration Equipmentmentioning

confidence: 99%

Tools and Procedures for the CTA Array Calibration

Maccarone¹,

Parsons²,

Gaug³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The Cherenkov Telescope Array (CTA) is an international initiative to build the next generation ground-based very-high-energy gamma-ray observatory. Full sky coverage will be assured by two arrays, one located on each of the northern and southern hemispheres. Three different sizes of telescopes will cover a wide energy range from tens of GeV up to hundreds of TeV. These telescopes, of which prototypes are currently under construction or completion, will have different mirror sizes and fields-of-view designed to access different energy regimes. Additionally, there will be groups of telescopes with different optics system, camera and electronics design. Given this diversity of instruments, an overall coherent calibration of the full array is a challenging task. Moreover, the CTA's requirements on calibration accuracy are much more stringent than those achieved with current Imaging Atmospheric Cherenkov Telescopes, like for instance: the systematic errors in the energy scale must not exceed 10%. In this contribution we present both the methods that, applied directly to the acquired observational CTA data, will ensure that the calibration is correctly performed to the stringent required precision, and the calibration equipment that, external to the telescopes, is currently under development and testing. Moreover, some notes about the operative procedure to be followed with both methods and instruments, will be described. The methods applied to the observational CTA data include the analysis of muon ring images, of carefully selected cosmic-ray air shower images, of the reconstructed electron spectrum and that of known gamma-ray sources and the possible use of stereo techniques hardware-independent. These methods will be complemented with the use of calibrated light sources located on ground or on board unmanned aerial vehicles.

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“…UVSiPM has been designed as support instrumentation of the ASTRI prototype. Both of them use the 2 http://www.iasf-palermo.inaf.it/cgibin/INAF/pub.cgi?href=facilities/electronic/instruments/delphin/index.html The design and implementation of UVSiPM derive from the well-tested UVscope instrument [3], developed at IASF-Palermo, whose sensor is a calibrated Multi-Anode PMT (MAPMT) working in SPC mode. The simultaneous usage of the two instruments on field, both provided with a calibrated John-B-25 Johnson/Bessel filter and equipped with collimators of proper length, will allow us to test the performance of UVSiPM under real observing conditions.…”

Section: Uvsipm and Astri: Main Applicationsmentioning

confidence: 99%

UVSiPM: A light detector instrument based on a SiPM sensor working in single photon counting

Sottile

Russo

Agnetta

et al. 2013

Nuclear Physics B - Proceedings Supplements

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UVSiPM is a light detector designed to measure the intensity of electromagnetic radiation in the 320-900 nm wavelength range. It has been developed in the framework of the ASTRI project whose main goal is the design and construction of an end-to-end Small Size class Telescope prototype for the Cherenkov Telescope Array. The UVSiPM instrument is composed by a multipixel Silicon Photo-Multiplier detector unit coupled to an electronic chain working in single photon counting mode with 10 nanosecond double pulse resolution, and by a disk emulator interface card for computer connection. The detector unit of UVSiPM is of the same kind as the ones forming the camera at the focal plane of the ASTRI prototype. Eventually, the UVSiPM instrument can be equipped with a collimator to regulate its angular aperture. UVSiPM, with its peculiar characteristics, will permit to perform several measurements both in lab and on field, allowing the absolute calibration of the ASTRI prototype.

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Performance and applications of the UVscope instrument

Cited by 23 publications

References 5 publications

ASTRI for the Cherenkov Telescope Array

ASTRI for the Cherenkov Telescope Array

Tools and Procedures for the CTA Array Calibration

UVSiPM: A light detector instrument based on a SiPM sensor working in single photon counting

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