The Cherenkov Telescope Array Observatory (CTAO) is the next generation ground-based observatory for gamma-ray astronomy at very-high energies. The CTAO will combine telescopes of different designs plus a large number of scientific instruments to achieve unprecedented performance and energy coverage. The Array Control and Data Acquisition (ACADA) system provides the means to execute observations and to handle the acquisition of scientific data in CTAO. The Resource Manager (RM) and Central Control (CC) subsystems are core components of the ACADA system. The RM subsystem provides infrastructure services concerning the administration of various resources to all ACADA subsystems. The CC subsystem implements the execution of observation requests received from the scheduler subsystem. CC interprets the received requests and sends appropriate commands to telescopes and other controllable array elements, supervises ongoing operations and coordinates the dynamic allocation and management of concurrent operations of telescopes to subarrays, which are logical groupings of individual CTAO telescopes performing coordinated scientific operations. This contribution provides a summary of the main design features, current status and future implementation plans for the ACADA RM and CC subsystems.
The Cherenkov Telescope Array Observatory (CTAO) is the next-generation atmospheric Cherenkov gamma-ray project. CTAO will be deployed at two sites, one in the Northern and the other in the Southern Hemisphere, containing telescopes of three different sizes for covering different energy domains. The commissioning of the first CTAO Large-sized Telescope (LST-1) is being finalized at the CTAO Northern site. Additional calibration and environmental monitoring instruments such as laser imaging detection and ranging (LIDAR) instruments and weather stations will support the telescope operations. The Array Control and Data Acquisition (ACADA) system is the central element for onsite CTAO operations. ACADA controls, supervises, and handles the data generated by the telescopes and the auxiliary instruments. It will drive the efficient planning and execution of observations while handling the several Gb/s camera data generated by each CTAO telescope. The ACADA system contains the CTAO Science Alert Generation Pipeline – a real-time data processing and 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 instruments, will be managed by the Transients Handler (TH) component. The TH informs the Short-term Scheduler of ACADA about interesting science alerts, enabling the modification of ongoing observations at sub-minute timescales. The capacity for such fast reactions – together with the fast movement of CTAO telescopes – makes CTAO an excellent instrument for studying high-impact astronomical transient phenomena. The ACADA software is based on the Alma Common Software (ACS) framework, and written in C++, Java, Python, and Javascript. The first release of the ACADA software, ACADA REL1, was finalized in July 2023, and integrated after a testing campaign with the LST-1 finalized in October 2023. This contribution describes the design and status of the ACADA software system.
The Cherenkov Telescope Array Observatory (CTAO) is the next-generation atmospheric Cherenkov gammaray Observatory. CTAO will be constructed on two sites, one array in the Northern and the other in the Southern hemisphere, containing telescopes of three different sizes, for covering different energy domains. To combine and orchestrate the different telescopes and auxiliary instruments (array elements), the Array Control and Data Acquisition (ACADA) system is the central element for the Observatory on-site operations: it controls, supervises, and handles the data generated by the array elements. Considering the criticality of the ACADA system for future Observatory operations, corresponding quality assurance provisions have been made at the different steps of the software development lifecycle, with focus on continuous integration and testing at all levels. To enable higher-level tests of the software deployed on a distributed system, an ACADA test cluster has been set up to facilitate testing and debugging of issues in a more realistic environment. Furthermore, a separate software integration and test cluster has also been established that allows for the off-site testing of the integrated software packages of ACADA and of the corresponding array elements. Here the software integration can be prepared, interfaces and interactions can be tested, and on-site procedures that are required later in the process can be checked beforehand, only limited by the simulation capabilities that are delivered as part of the software packages. Once preparations and testing with the off-site test cluster are completed, the integrated software can be deployed at the target site. The software packages and setup parameters are kept under configuration control at all stages, and deployment steps are documented to ensure that installations are reproducible. This methodology has been applied for the first time in the context of the integration of ACADA with the first CTAO Large-sized Telescope (LST-1) in October 2023.
The Cherenkov Telescope Array (CTA) will be the next-generation ground-based detector for gamma rays with very high energies. Telescopes will be located at one site each in both the northern and southern hemisphere. The arrays will comprise, in total, more than 100 telescopes of different sizes and designs. The sensitivity of CTA in its central energy range, i.e. between approximately 100 GeV and 1 TeV, will be driven by the performance of the Medium-Sized Telescopes (MSTs). This performance crucially depends on an exact alignment of the facets of the tessellated mirror surface of each telescope. In this contribution, an automated mirror alignment procedure for MSTs is presented. This procedure consists of two steps. First a rough mirror alignment is achieved with the socalled Bokeh method, which is based on the non-focused imaging of an artificial light source onto the Cherenkov camera plane. Afterwards, an optimal mirror alignment is achieved with an alignment procedure based on the focused imaging of stars. Here, the Bokeh method will be described in detail, including the hardware and software setups, devised technologies and pattern recognition with classical and neural network-based methods. Also results from star alignment procedures are given and compared to results from the Bokeh method. The performance of the presented approach is demonstrated with results obtained from measurements at the MST prototype installation in Berlin, Germany.
KEYWORDS: Software development, Atmospheric Cherenkov telescopes, Telescopes, System integration, Process modeling, Java, Control systems, Data storage, Computer architecture, Lead
The Cherenkov Telescope Array (CTA) will be the next-generation ground-based instrument for detecting veryhigh energy gamma rays. It will consist of roughly 100 telescopes of different sizes and designs. In addition, a variety of auxiliary instrumentation will be part of the array. The Observation Execution System (OES) is the software system in charge of operating and monitoring all telescopes and devices, applying short-term observation schedules depending on the hardware status and environmental conditions and handling the data. Motivated by the wealth of tasks to accomplish and requirements to fulfil, a software development procedure is conceived for the development of OES. Part of this development process is the application of software testing procedures. These procedures range from unit tests up to system tests and stress tests. In this contribution, the software development process and the application of static and dynamic code analysis tools are described.
The Cherenkov Telescope Array (CTA) will be the next generation ground-based observatory for gamma-ray astronomy at very-high energies. CTA will consist of two large arrays with 118 Cherenkov telescopes in total, deployed in the northern and southern hemispheres. The Observation Execution System (OES) provides the means to execute observations and to handle the acquisition of scientific data in CTA. The Manager and Central Control (MCC) system is a core element in the OES system that implements the execution of observation requests received from the scheduler sub-system. This contribution provides a summary of the main MCC design features and of the plans for prototyping.
KEYWORDS: Atmospheric Cherenkov telescopes, Telescopes, Control systems, Observatories, Data acquisition, Imaging systems, Observatories, Control systems, Cameras, Prototyping, Systems modeling, Software development
The Cherenkov Telescope Array (CTA) will be the next-generation ground-based observatory using the atmospheric Cherenkov technique. The CTA instrument will allow researchers to explore the gamma-ray sky in the energy range from 20 GeV to 300 TeV. CTA will comprise two arrays of telescopes, one with about 100 telescopes in the Southern hemisphere and another smaller array of telescopes in the North. CTA poses novel challenges in the field of ground-based Cherenkov astronomy, due to the demands of operating an observatory composed of a large and distributed system with the needed robustness and reliability that characterize an observatory. The array control and data acquisition system of CTA (ACTL) provides the means to control, readout and monitor the telescopes and equipment of the CTA arrays. The ACTL system must be flexible and reliable enough to permit the simultaneous and automatic control of multiple sub-arrays of telescopes with a minimum effort of the personnel on-site. In addition, the system must be able to react to external factors such as changing weather conditions and loss of telescopes and, on short timescales, to incoming scientific alerts from time-critical transient phenomena. The ACTL system provides the means to time-stamp, readout, filter and store the scientific data at aggregated rates of a few GB/s. Monitoring information from tens of thousands of hardware elements need to be channeled to high performance database systems and will be used to identify potential problems in the instrumentation. This contribution provides an overview of the ACTL system and a status report of the ACTL project within CTA.
KEYWORDS: Atmospheric Cherenkov telescopes, Telescopes, Systems modeling, Chemical elements, Computer architecture, Data acquisition, Control systems, Data modeling, Calibration, Software development
The Cherenkov Telescope Array (CTA) project is an initiative to build two large arrays of Cherenkov gamma- ray telescopes. CTA will be deployed as two installations, one in the northern and the other in the southern hemisphere, containing dozens of telescopes of different sizes. CTA is a big step forward in the field of ground- based gamma-ray astronomy, not only because of the expected scientific return, but also due to the order-of- magnitude larger scale of the instrument to be controlled. The performance requirements associated with such a large and distributed astronomical installation require a thoughtful analysis to determine the best software solutions. The array control and data acquisition (ACTL) work-package within the CTA initiative will deliver the software to control and acquire the data from the CTA instrumentation. In this contribution we present the current status of the formal ACTL system decomposition into software building blocks and the relationships among them. The system is modelled via the Systems Modelling Language (SysML) formalism. To cope with the complexity of the system, this architecture model is sub-divided into different perspectives. The relationships with the stakeholders and external systems are used to create the first perspective, the context of the ACTL software system. Use cases are employed to describe the interaction of those external elements with the ACTL system and are traced to a hierarchy of functionalities (abstract system functions) describing the internal structure of the ACTL system. These functions are then traced to fully specified logical elements (software components), the deployment of which as technical elements, is also described. This modelling approach allows us to decompose the ACTL software in elements to be created and the ow of information within the system, providing us with a clear way to identify sub-system interdependencies. This architectural approach allows us to build the ACTL system model and trace requirements to deliverables (source code, documentation, etc.), and permits the implementation of a flexible use-case driven software development approach thanks to the traceability from use cases to the logical software elements. The Alma Common Software (ACS) container/component framework, used for the control of the Atacama Large Millimeter/submillimeter Array (ALMA) is the basis for the ACTL software and as such it is considered as an integral part of the software architecture.
The Cherenkov Telescope Array (CTA) is an international initiative to build the next generation ground-based gamma-ray instrument. CTA will allow studying the Universe in the very-high-energy gamma-ray domain with energies ranging from a few tens of GeV to more than a hundred TeV. It will extend the currently accessible energy band, while increasing the sensitivity by a factor of 10 with respect to existing Cherenkov facilities. Furthermore, CTA will enhance other important aspects like angular and energy resolution. CTA will comprise two arrays, one in the Northern hemisphere and one in the Southern hemisphere, of in total more than one hundred of telescopes of three different sizes. The CTA performance requirements and the increased complexity in operation, control and monitoring of such a large distributed multi-telescope array leads to new challenges in designing and developing the CTA control software system. Indeed, the control software system must be flexible enough to allow for the simultaneous operation of multiple sub-arrays of different types of telescopes, to be ready to react in short timescales to changing weather conditions or to automatic alarms for transient phenomena, to be able to operate the observatory with a minimum personal effort on site, to cope with the malfunctioning of single telescopes or sub-arrays of telescopes, and to readout and control a large and heterogeneous set of devices. This report describes the preliminary architectural design concept for the CTA control software system that will be responsible to manage all the functionality of the CTA array, thereby enabling CTA to reach its scientific goals.
KEYWORDS: Prototyping, Optical proximity correction, Telescopes, Atmospheric Cherenkov telescopes, Control systems, Java, CCD cameras, Cameras, Databases, OLE for process control
The Cherenkov Telescope Array (CTA) will be the next generation ground-based very-high energy -ray observatory. CTA will consist of two arrays: one in the Northern hemisphere composed of about 20 telescopes, and the other one in the Southern hemisphere composed of about 100 telescopes, both arrays containing telescopes of different sizes and types and in addition numerous auxiliary devices. In order to provide a test-ground for the CTA array control, the steering software of the 12-m medium size telescope (MST) prototype deployed in Berlin has been implemented using the tools and design concepts under consideration to be used for the control of the CTA array. The prototype control system is implemented based on the Atacama Large Millimeter/submillimeter Array (ALMA) Common Software (ACS) control middleware, with components implemented in Java, C++ and Python. The interfacing to the hardware is standardized via the Object Linking and Embedding for Process Control Unified Architecture (OPC UA). In order to access the OPC UA servers from the ACS framework in a common way, a library has been developed that allows to tie the OPC UA server nodes, methods and events to the equivalents in ACS components. The front-end of the archive system is able to identify the deployed components and to perform the sampling of the monitoring points of each component following time and value change triggers according to the selected configurations. The back-end of the archive system of the prototype is composed by two different databases: MySQL and MongoDB. MySQL has been selected as storage of the system configurations, while MongoDB is used to have an efficient storage of device monitoring data, CCD images, logging and alarm information. In this contribution, the details and conclusions on the implementation of the control software of the MST prototype are presented.
The Cherenkov Telescope Array (CTA) is the next generation Very High Energy (VHE, defined as > 50GeV to several
100TeV) telescope facility, currently in the design and prototyping phase, and expected to come on-line around 2016. The
array would have both a Northern and Southern hemisphere site, together delivering nearly complete sky coverage. The
CTA array is planned to have ~100 telescopes of several different sizes to fulfill the sensitivity and energy coverage needs.
Each telescope has a number of subsystems with varied hardware and control mechanisms; a drive system that gets
commands and inputs via OPC UA (OPC Unified Architecture), mirror alignment systems based on XBee/ZigBee protocol
and/or CAN bus, weather monitor accessed via serial/Ethernet ports, CCD cameras for calibration, Cherenkov camera, and
the data read out electronics, etc. Integrating the control and data-acquisitions of such a distributed heterogeneous system
calls for a framework that can handle such a multi-platform, multi-protocol scenario. The CORBA based ALMA Common
software satisfies these needs very well and is currently being evaluated as the base software for developing the control
system for CTA.
A prototype for a Medium Size Telescope (MST, ~12m) is being developed and will be deployed in Berlin, by end of
2012. We present the development being carried out to integrate and control the various hardware subsystems of this MST
prototype using ACS.
The Cherenkov Telescope Array (CTA) is designed to make a major improvement in the sensitivity of ground based
VHE (Very High Energy, defined as > 20GeV to 100s of TeV) gamma-ray telescopes. Not only will the differential-flux
sensitivity be an order of magnitude better than those of the currently operating Cherenkov telescopes, but there will also be
significant improvements in the energy, spectral and angular resolution. Delivering these features cost-effectively requires
several telescope sizes and designs - a few large size telescopes (23m diameter) are designed for the lowest energies, a
large number of small size telescopes (4-7m diameter) to increase the overall collection area which helps at the highest
energies and a number of Medium Size Telescopes (MST, 9.5m or 12m diameter, depending on the mirror design) to
provide the greatest sensitivity at ∼ 1 TeV. To provide complete sky coverage, CTA will have both a Northern Hemisphere
and a Southern Hemisphere site.
A prototype for an MST design (currently under development) will be build in Berlin by 2012. This MST prototype
has a modified Davies-Cotton design with a tessellated mirror, with individual facets of ∼ 1.2m in diameter. The facets are
three-point mounted on the optical support structure, having two powered actuators for alignment adjustments. In addition
a number of CCD cameras will be mounted at various positions on the dis and will be used for calibration. Here we present
the various optical calibration tasks - optimization of the optical point-spread-function (PSF) and the pointing of this MST
prototype, along with initial results.
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