The Central Calibration Facilities workpackage of the Cherenkov Telescope Array (CTA) observatory for very high energy gamma ray astronomy defines the overall calibration strategy of the array, develops dedicated hardware and software for the overall array calibration and coordinates the calibration efforts of the different telescopes. The latter include LED-based light pulsers, and various methods and instruments to achieve a calibration of the overall optical throughput. On the array level, methods for the inter-telescope calibration and the absolute calibration of the entire observatory are being developed. Additionally, the atmosphere above the telescopes, used as a calorimeter, will be monitored constantly with state-of-the-art instruments to obtain a full molecular and aerosol profile up to the stratosphere. The aim is to provide a maximal uncertainty of 10% on the reconstructed energy-scale, obtained through various independent methods. Different types of LIDAR in combination with all-sky-cameras will provide the observatory with an online, intelligent scheduling system, which, if the sky is partially covered by clouds, gives preference to sources observable under good atmospheric conditions. Wide-field optical telescopes and Raman Lidars will provide online information about the height-resolved atmospheric extinction, throughout the field-of-view of the cameras, allowing for the correction of the reconstructed energy of each gamma-ray event. The aim is to maximize the duty cycle of the observatory, in terms of usable data, while reducing the dead time introduced by calibration activities to an absolute minimum.

Calibration strategies for the Cherenkov Telescope Array

The Cherenkov Telescope Array (CTA) project is the initiative to build the next-generation gamma-ray observatory. With more than 100 telescopes planned to be deployed at two sites, CTA is one of the largest astronomical facilities under construction. The Array Control and Data Acquisition (ACADA) system will be the central element of on-site CTA Observatory operations. The mission of the ACADA system is to manage and optimize the telescope array operations at each of the CTA sites. To that end, ACADA will provide all necessary means for the efficient execution of observations, and for the handling of the several Gb/s of data generated by each individual CTA telescope. The ACADA system will contain a real-time analysis pipeline, dedicated to the automatic generation of science alert candidates as data are being acquired. These science alerts, together with external alerts arriving from other scientific installations, will permit ACADA to modify ongoing observations at sub-minute timescales in order to study high-impact scientific transient phenomena. This contribution describes the challenges, architecture, design principles, and development status of the ACADA system.

The Array Control and Data Acquisition System of the Cherenkov Telescope Array

1DESY, Zeuthen, Germany, 2Fraunhofer IESE, Kaiserslauten, Germany , 3UTFSM, Valparaíso, Chile, 4CAMK, Torun, Poland, 5I.A.S.F. di Bologna, Italy, 6IEECCSIC, Spain, 7DESY, Hamburg, Germany, 8University of Geneva Departement d'Astronomie, Switzerland, 9Humboldt-Universität zu Berlin, Germany, 10INAF – Osservatorio Astronomico di Brera, Italy, 11University of Perugia, Italy 12See www.cta-observatory.org

Designing and prototyping the control system for the Cherenkov Telescope Array

Summary
In this work, a signal-extraction algorithm pertaining to the Cherenkov Telescope Array's real-time-analysis pipeline has been parallelised using SSE, POSIX Threads and CUDA. Because of the observatory's constraints, the online analysis has to be conducted on site, on hardware located at the telescopes, and compels a search for efficient computing solutions to handle the huge amount of measured data. This work is framed in a series of studies which benchmark several algorithms of the real-time-analysis pipeline on different architectures to gain an insight into the suitability and performance of each platform.

Performance study of a signal‐extraction algorithm using different parallelisation strategies for the Cherenkov Telescope Array's real‐time‐analysis software

The Liverpool Telescope is one of the world’s premier facilities for time domain astronomy. The time domain landscape is set to radically change in the coming decade, with synoptic all-sky surveys such as LSST providing huge numbers of transient detections on a nightly basis; transient detections across the electromagnetic spectrum from other major facilities such as SVOM, SKA and CTA; and the era of ‘multi-messenger astronomy’, wherein astrophysical events are detected via non-electromagnetic means, such as neutrino or gravitational wave emission. We describe here our plans for the Liverpool Telescope 2: a new robotic telescope designed to capitalise on this new era of time domain astronomy. LT2 will be a 4-metre class facility co-located with the Liverpool Telescope at the Observatorio del Roque de Los Muchachos on the Canary island of La Palma. The telescope will be designed for extremely rapid response: the aim is that the telescope will take data within 30 seconds of the receipt of a trigger from another facility. The motivation for this is twofold: firstly it will make it a world-leading facility for the study of fast fading transients and explosive phenomena discovered at early times. Secondly, it will enable large-scale programmes of low-to-intermediate resolution spectral classification of transients to be performed with great efficiency. In the target-rich environment of the LSST era, minimising acquisition overheads will be key to maximising the science gains from any follow-up programme. The telescope will have a diverse instrument suite which is simultaneously mounted for automatic changes, but it is envisaged that the primary instrument will be an intermediate resolution, optical/infrared spectrograph for scientific exploitation of transients discovered with the next generation of synoptic survey facilities. In this paper we outline the core science drivers for the telescope, and the requirements for the optical and mechanical design.

/pdf/liverpool-telescope-2-a-new-robotic-facility-for-rapid-1mojxkxvo9.pdf

Liverpool telescope 2: a new robotic facility for rapid transient follow-up

The Cherenkov Telescope Array (CTA) observatory will be one of the biggest ground-based very-high-energy (VHE) gamma-ray observatory. CTA will achieve a factor of 10 improvement in sensitivity from some tens of GeV to beyond 100 TeV with respect to existing telescopes. The CTA observatory will be capable of issuing alerts on variable and transient sources to maximize the scientific return. To capture these phenomena during their evolution and for effective communication to the astrophysical community, speed is crucial. This requires a system with a reliable automated trigger that can issue alerts immediately upon detection of gamma-ray flares. This will be accomplished by means of a Real-Time Analysis (RTA) pipeline, a key system of the CTA observatory. The latency and sensitivity requirements of the alarm system impose a challenge because of the anticipated large data rate, between 0.5 and 8 GB/s. As a consequence, substantial efforts toward the optimization of high-throughput computing service are envisioned. For these reasons our working group has started the development of a prototype of the Real-Time Analysis pipeline. The main goals of this prototype are to test: (i) a set of frameworks and design patterns useful for the inter-process communication between software processes running on memory; (ii) the sustainability of the foreseen CTA data rate in terms of data throughput with different hardware (e.g. accelerators) and software configurations, (iii) the reuse of non-real-time algorithms or how much we need to simplify algorithms to be compliant with CTA requirements, (iv) interface issues between the different CTA systems. In this work we focus on goals (i) and (ii).

/pdf/a-prototype-for-the-real-time-analysis-of-the-cherenkov-3fakxka6r0.pdf

A prototype for the Real-Time analysis of the Cherenkov Telescope Array

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A prototype for the Real-Time analysis of the Cherenkov Telescope Array