NectarCAM, a camera for the medium sized telescopes of the Cherenkov telescope array

Glicenstein, J. F.; Shayduk, M.

doi:10.1063/1.4969030

Cited by 13 publications

(11 citation statements)

References 5 publications

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“…due to maintenance activities). The east-west pair of telescopes represents the best option for a two LST stage-1 9 , and therefore the chosen telescope separation is close to optimal for a two-telescope system (as shown in Sec.…”

Section: Mst and Sst Patternsmentioning

confidence: 91%

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Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout

Acharyya

Agudo

Angüner

et al. 2019

Astroparticle Physics

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The Cherenkov Telescope Array (CTA) is the major next-generation observa-7 tory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possible by using tens of imaging Cherenkov telescopes of three successive sizes. They will be arranged into two arrays, one per hemisphere, located on the La Palma island (Spain) and in Paranal (Chile). We present here the optimised and final telescope arrays for both CTA sites, as well as their foreseen performance, resulting from the analysis of three different large-scale Monte Carlo productions.

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Section: Mst and Sst Patternsmentioning

confidence: 91%

“…The DC-MST is a 12m-diameter single-mirror IACT built with modified Davies-Cotton optics and a mirror area of ∼ 88 m 2 . Two different cameras have been prototyped for this telescope: NectarCam and FlashCam [9,10]. The SC-MST features a two-mirror optical design with a 9.7 m diameter primary mirror and an area of ∼ 41m 2 .…”

Section: Introductionmentioning

confidence: 99%

Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout

Acharyya

Agudo

Angüner

et al. 2019

Astroparticle Physics

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“…However, the SiPM choice was also adopted for the SST-DC that makes use of the non-commercial Hamamatsu S10943-2832(X) (Heller et al 2017). The MST telescopes will instead host PMT-based cameras (Glicenstein & Shayduk 2017), using the R12992-100 PMT from Hamamatsu 21 , and for the proposed Schwarzschild-Couder MST (Meagher 2014) at CTA-S. The case of LST is peculiar: its baseline design will make use of the PMT Hamamatsu R19200-100 (Okumura et al 2015), with the four LSTs planned for the CTA-N already being built with PMT cameras.…”

Section: Lgs Induced Light On Cta Pixelsmentioning

confidence: 99%

Impact of Laser Guide Star facilities on neighbouring telescopes: the case of GTC, TMT, VLT, and ELT lasers and the Cherenkov Telescope Array

Gaug

Doro

2018

Monthly Notices of the Royal Astronomical Society

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Powerful Laser Guide Star (LGS) systems are standard for the next-generation of extremely large telescopes. However, modern earth-based astronomy has gone through a process of concentration on few sites with exceptional sky quality, resulting in those becoming more and more crowded. The future LGS systems encounter hence an environment of surrounding astronomical installations, some of which observing with large fields-of-view. We derive formulae to calculate the impact of LGS light on the camera of a neighbouring telescope and the probabilities for a laser crossing the camera field-of-view to occur, and apply these to the specific case of the next very-high-energy gamma-ray observatory "Cherenkov Telescope Array" (CTA). Its southern part shall be constructed in a valley of the Cerro Armazones, Chile, close to the "Very Large Telescope" (VLT) and the "European Extremely Large Telescope" (ELT), while its northern part will be located at the "Observatorio del Roque de los Muchachos", on the Canary Island of La Palma, which also hosts the "Gran Telescopio de Canarias" (GTC) and serves as an optional site for the "Thirty Meter Telescope" (TMT), both employing LGS systems. Although finding the artificial star in the field-of-view of a CTA telescope will not disturb observations considerably, the laser beam crossing the field-of-view of a CTA telescope may be critical. We find no conflict expected for the ELT lasers, however, 1% (3%) of extra-galactic and 1% (5%) of galactic observations with the CTA may be affected by the GTC (TMT) LGS lasers, unless an enhanced version of a laser tracking control system gets implemented.creation of several guide stars is also possible, to achieve asterism with a radial distance from science target ranging from 0.5 to 6 on the sky. The LGS will likely be operated regularly during observations, and their scattered light (Rayleigh and Mie) will then be seen by other telescopes until distances of several kilometers from the location of their host observatory. Assuming the close-by installation observes in a wavelength range enclosing that of the LGS lasers, the scattered laser light may then leave spurious light tracks on the cameras and affect operation in several ways: a) by generating false triggers (for installations which trigger image readout e.g. from Cherenkov light pulses) the star guider camera and the precision pointing of the telescopes, and ultimately, d) by affecting the duty cycle, if active laser avoidance is chosen. Several of the enumerated problems can be often overcome with the use of Notch-filters (Schallenberg et al. 2010) or band-pass filters (Ahnen et al. 2017;Archambault et al. 2017), however this is not always possible at a reasonable cost, particularly not in the case of the CTA, where every camera pixel would need to be covered by such a filter. Light losses at smaller wavelengths, particularly in the sensitive region from 300 nm to 500 nm need to be strictly controlled in order to ensure that sensitivity losses remain acceptable, particularly around the energ...

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“…Such structure is shown in Figure 1, where the different subsystems and the signals exchanged with the TIB are presented. Further details of the subsystems can be found in [1] and [2].…”

Section: Tib Interfacesmentioning

confidence: 99%

“…Three different kinds of telescopes will be placed in the observatories according to their mirror diameters: Large-Sized Telescopes (LSTs), Medium-Sized Telescopes (MSTs) and Small-Sized Telescopes (SSTs). The LST camera [1] and NectarCAM [2], which is one of two MST camera designs, have been designed in a similar way, in terms of functionality and hardware implementation. However, they have a number of differences, since their designs are optimized for their corresponding target energy ranges.…”

Section: Introductionmentioning

confidence: 99%

A Trigger Interface Board to manage trigger and timing signals in CTA Large-Sized Telescope and Medium-Sized Telescope camera

Moya¹,

Peñil²,

Tejedor³

et al. 2017

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

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NectarCAM, a camera for the medium sized telescopes of the Cherenkov telescope array

Cited by 13 publications

References 5 publications

Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout

Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout

Impact of Laser Guide Star facilities on neighbouring telescopes: the case of GTC, TMT, VLT, and ELT lasers and the Cherenkov Telescope Array

A Trigger Interface Board to manage trigger and timing signals in CTA Large-Sized Telescope and Medium-Sized Telescope camera

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