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We study the entanglement entropy in lattice field theory using a simulation algorithm based on Jarzynski's theorem. We focus on the entropic c-function for the Ising model in two and in three dimensions: after validating our algorithm against known analytical results from conformal field theory in two dimensions, we present novel results for the three-dimensional case. We show that our algorithm, which is highly parallelized on graphics processing units, allows one to precisely determine the subleading corrections to the area law, which have been investigated in many recent works. Possible generalizations of this study to other strongly coupled theories are discussed., Comment: 1+33 pages; v2: typos corrected, matches published version

We report the Astrorivelatore Gamma ad Immagini LEggero (AGILE) observations of solar flares, detected by the on board anticoincidence system in the 80-200 keV energy range, from 2007 May 1st to 2022 August 31st. In more than 15 yr, AGILE detected 5003 X-ray, minute-lasting transients, compatible with a solar origin. A cross-correlation of these transients with the Geostationary Operational Environmental Satellites (GOES) official solar flare database allowed to associate an intensity class (i.e., B, C, M, or X) to 3572 of them, for which we investigated the main temporal and intensity parameters. The AGILE data clearly revealed the solar activity covering the last stages of the 23rd cycle, the whole 24th cycle, and the beginning of the current 25th cycle. In order to compare our results with other space missions operating in the high-energy range, we also analyzed the public lists of solar flares reported by RHESSI and Fermi Gamma-ray Burst Monitor. This catalog reports 1424 events not contained in the GOES official dataset, which, after statistical comparisons, are compatible with low-intensity, short-duration solar flares. Besides providing a further dataset of solar flares detected in the hard X-ray range, this study allowed to point out two main features: a longer persistence of the decay phase in the high-energy regime, with respect to the soft X-rays, and a tendency of the flare maximum to be reached earlier in the soft X-rays with respect to the hard X-rays. Both these aspects support a two-phase acceleration mechanism of electrons in the solar atmosphere., 22 pages, 10 figures

Gamma-Flash is an Italian project funded by the Italian Space Agency (ASI) and led by the National Institute for Astrophysics (INAF), devoted to the observation and study of high-energy phenomena, such as terrestrial gamma-ray flashes and gamma-ray glows produced in the Earth's atmosphere during thunderstorms. The project's detectors and the data acquisition and control system (DACS) are placed at the "O. Vittori" observatory on the top of Mt. Cimone (Italy). Another payload will be placed on an aircraft for observations of thunderstorms in the air. This work presents the architecture of the data acquisition and control system and the data flow., 4 pages, 1 figure, Astronomical Data Analysis Software and System XXXII (2022)

The scope of this document is to provide a detailed design description of the SAG Sub- system of the Array Control and Data Acquisition (ACADA) System that will be operating the instruments at both CTA-N and CTA-S installations. The main audience of this document is the development team that is expected to implement the sub-system. Motivations for the main design decisions taken are provided in connection with requirements and standards. This document describes writing SW design for the SAG sub-system in the context of the ACADA system. Throughout the document, UML is the preferred notation for depicting the component to be designed. The modelling tool used is Sparx Enterprise Architect. Throughout this document, the term “component” is used to refer to anything beyond the level of the system to be designed. A component usually consists of several sub-compo- nents. The main components of the SAG sub-system are: 1) SAG-SUP: Supervisors 2) SAG-RECO: Image Parameter Extractor and Low Level Reconstruction Pipeline 3) SAG-DQ: Data Quality 4) SAG-SCI: High-Level Analysis

This specification describes a plan to conduct requirements verification to assess for the de- sired performance, design, development, test and qualification requirements defined for the Science Alert Generation Pipeline (SAG) sub-system of the Array Control and Data Acqui- sition (ACADA) System of CTAO.

The GAMMA-FLASH Data Acquisition and Control System (DACS) is modular and is composed of one or more Data Acquisition Modules (DAMs) and one Main Control Computer (MCC). DAM units are based on Red Pitaya 125-14 boards running dedicated application software on Linux OS. Each DAM is in charge of collecting and processing the data from at least one gamma-ray or neutron detector and saving such data on-board or transferring it to the MCC. The aim of this document is to describe both the functional and the TC/TM interfaces implemented by the DAM and the MCC and to give a unique reference for the installation and configuration of the DACS SW. The DACS SW described in this document is designed to satisfy the requirements

All’interno dell’ Osservatorio di Astrofisica e Scienza dello Spazio di Bologna (OAS), da sempre abbiamo avuto la necessità di strumenti di calcolo potenti e condivisi su cui gli scienziati possano svolgere le elaborazioni sui dati scientifici di Progetti e Missioni. Il Cluster OAS nasce proprio per soddisfare questa esigenza ed è ospitato nel Centro di Calcolo del plesso OAS presso il CNR di Bologna. Tutti gli afferenti a OAS possono chiedere di essere registrati nel sistema di autenticazione LDAP del Cluster e in questo modo accedere via Internet ai nodi di login da dove possono sottomettere le loro elaborazioni. Ci sono due modalità di usare il cluster: quella interattiva e quella batch più classica per un Cluster. L’accesso interattivo consente di lanciare in tempo reale le elaborazioni anche in maniera grafica tramite opportuni programmi si console virtuale, questo tipo di elaborazione viene svolta direttamente nei nodi di login. La modalità batch sfrutta il meccanismo a code, slurm, per sottomettere i lavori in maniera organizzata ai più potenti nodi di calcolo che non sono direttamente utilizzabili dagli utenti. Il cluster inoltre fornisce spazio di archiviazione condiviso organizzato in HOME per i dati personali degli utenti, DATA per i risultati delle elaborazioni PROGRAMMI per la memorizzazione dei moduli di elaborazione e LUSTRE per il calcolo parallelo. I vantaggi di avere un Cluster sono che gli utenti trovano i programmi e compilatori di cui necessitano già installati nelle principali versioni e hanno a disposizione una buona potenza di calcolo e spazio di storage per poter lavorare molto più agevolmente rispetto ai propri computer personali. Il Cluster OAS non ha una potenza paragonabile ai grandi Cluster Commerciali e di Ricerca, ma essendo ritagliato sulle esigenze degli afferenti a OAS risponde bene alle esigenze dell'istituto e può servire come Nave Scuola per poter poi accedere a strutture più grandi qualora fosse necessario. Nel documento saranno illustrate nel dettaglio le caratteristiche Hardware e Software del Cluster, compresi tutti i principali Software scientifici installati di cui si spiega brevemente l’utilizzo.

AGILE is a space mission launched in 2007 devoted to high-energy astrophysics. The AGILE Team is involved in the multi-messenger campaigns to send and receive science alerts about transient events in the shortest time possible. For this reason, the AGILE Team developed several real-time analysis pipelines to analyse data and follow-up external science alerts. However, the results obtained by these pipelines are preliminary and must be validated with manual analyses that are the bottleneck of the workflow. To speed up the scientific analysis performed by scientists, the AGILE Team developed the AGILEScience mobile application (for iOS and Android devices) that offers to the AGILE Team a password-protected section used to visualise the results of automated pipelines. We present in this contribution an improved functionality of the AGILEScience application that aims to enable the AGILE Team to execute a full scientific analysis using their mobile devices. When the analysis is completed, the system sends an email to notify the user that can visualise the results (e.g. plots, tables, and HTML pages) through the application. The possibility to perform scientific analysis from a mobile device enables the AGILE researchers to perform fast scientific analyses remotely to validate the preliminary results obtained with the automated pipelines. This workflow reduces the overall reaction time of the AGILE Team for the follow-up of transient phenomena., Comment: 4 pages, 4 figures, Astronomical Data Analysis Software and System XXXI (24-28 Ottobre 2021)

The main purpose of this Note is to define a method and a template to collect Physical Science use cases from scientists and research engineers working on Physical Science projects in the context and within the scope of the OpenPOWER Foundation for Physical Science Workgroup. An effective method (shared between all stakeholders) could contribute to • understand the workflow, starting with user expectations; • help Physical Science projects maintain costs within a chosen envelope; • map the functionalities to the scientific requirements; • remove possible misunderstanding between the scientific community and ICT stakeholders.

The ASTRI Mini-Array (MA) is an INAF ground-based project to construct, deploy and operate a set of nine identical dual-mirror Cherenkov gamma-ray telescopes. The ASTRI Mini-Array will exploit the imaging atmospheric Cherenkov technique to measure the energy, direction and arrival time of gamma-ray photons arriving at the Earth from astrophysical sources. The ASTRI Mini-Array will also perform Stellar Hambury-Brown intensity interferometry and direct measurements of cosmic rays. The site selected for the installation and operation of the ASTRI Mini-Array is the Observatorio del Teide in Tenerife (Spain). This Statement of Work (SoW) describes the activities and the deliverables and work logic necessary for the provision of the “Central Control software system” required by INAF (referred to as “the Customer”) in the context of the ASTRI Mini-Array Project. This SoW will serve as an applicable document throughout the execution of the work by the Contractor to provide the core packages of the ASTRI Central Control software system design, development, integration, and on-site deployment, acceptance and maintenance during the warranty period.

The ASTRI Mini-Array is a project for the Cherenkov astronomy in the TeV energy range. ASTRI Mini-Array consists of nine Imaging Atmospheric Cherenkov telescopes located at the Teide Observatory (Canarias Islands). Large volumes of monitoring and logging data result from the operation of a large-scale astrophysical observatory. In the last few years, several "Big Data" technologies have been developed to deal with such volumes of data, especially in the Internet of Things (IoT) framework. We present the Monitoring, Logging, and Alarm (MLA) system for the ASTRI Mini-Array aimed at supporting the analysis of scientific data and improving the operational activities of the telescope facility. The MLA system was designed and built considering the latest software tools and concepts coming from Big Data and IoT to respond to the challenges posed by the operation of the array. A particular relevance has been given to satisfying the reliability, availability, and maintainability requirements towards all the array sub-systems and auxiliary devices. The system architecture has been designed to scale up with the number of devices to be monitored and with the number of software components to be considered in the distributed logging system.

The ASTRI Mini-Array (MA) is an INAF project aimed to observe astronomical sources emitting at very high-energy in the TeV spectral band. This document aims to define in detail the testing procedures that are implemented for the PMSC System.

The ASTRI Mini-Array (MA) is an INAF project aimed to observe astronomical sources emitting at very high-energy in the TeV spectral band. This document aims to define in detail the testing procedures that are implemented for the PMSC System.

The ASTRI Mini-Array (MA) is an INAF project aimed to observe astronomical sources emitting at very high-energy in the TeV spectral band. This document aims to define in detail the testing procedures that are implemented for the ICTSC System.

This document provides an overview of the data products of the ASTRI MA System, and their conceptual (and logical) data models. The goals are: - list the data products produced by the MA system and the related data product categories; - show the relationship between the data products; - define a short identifier for the data product; - refer to data streams in architectural diagrams without ambiguity; - define interfaces and data models.

This document provides a comprehensive architectural overview of the ASTRI Mini-Array Software system (a.k.a MA Software or MA Software System), which manages observing projects, observation handling, array control and monitoring, data acquisition, archiving, processing and simulations of the Cherenkov and Intensity Interferometry observations, including science tools for the scientific exploitation of the ASTRI MA data. This document, using a number of different views, depicts different aspects of the Mini-Array software and describes the significant architectural decisions.

Il CSN5, rispondendo alle esigenze di creare maggiori occasioni di dialogo e di networking e di mettere a fattor comune le esperienze maturate in settori strategici del nostro Ente, ha organizzato il primo “Forum della Ricerca Sperimentale e Tecnologica INAF” che si è svolto presso l’area di ricerca di Bologna nei giorni 22, 23 e 24 giugno 2022. L'evento aveva diversi obiettivi: - incrementare la reciproca conoscenza delle attività tecnologiche condotte nelle diverse strutture INAF; - favorire discussioni, scambi, sinergie; - promuovere il senso di appartenenza alla comunità INAF; - introdurre e coinvolgere il personale assunto negli ultimi anni, che non dispone di una visione di insieme di tutte le attività svolte dall’INAF; - stimolare le collaborazioni, anche al di fuori dei rapporti già esistenti; - far emergere eventuali problematiche, discuterne insieme ed individuare possibili soluzioni; - in generale, migliorare la capacità dell’Ente nel realizzare strumentazione sempre più sofisticata e complessa.

The ASTRI Mini-Array (MA) is an INAF project to construct and operate an experiment to study gamma-ray sources emitting at very high-energy in the TeV spectral band. This document defines the Use Cases of the ICT System Collector (ICTSC).

The ASTRI Mini-Array (MA) is an INAF ground-based project to construct, deploy and operate a set of nine identical dual-mirror Cherenkov gamma-ray telescopes, and several other auxiliary equipment and infrastructures. The ASTRI Mini-Array scientific objective is to exploit the imaging atmospheric Cherenkov technique to measure the energy, direction and arrival time of gamma-ray photons arriving at the Earth from astrophysical sources. This document lists acronyms and the glossary of the project

This document contains the ASTRI Mini-Array Software PBS. This document applies to all application- and domain-level software for the MA software project.

To capture the greatest possible number of points of view during the requirements-gathering phase, the observation-related use cases have been developed and presented in this document. The goal is to understand how to serve the users of the ASTRI Mini-Array System. The Observation-related use cases describe how to perform observations from the proposal to the scientific exploitation of the observation from a user’s point of view and the commonalities of all the science-related use cases. This category includes calibration and other technical-related use cases. his document defines the Top Level Use Cases of the ASTRI MA project. The use cases contained in this document are part of the functional requirements of the MA Software System to describe the workflow. These requirements complement the functional and quality requirements provided in the "ASTRI Mini-Array Top Level Software Architecture" document.

The ASTRI Mini-Array (MA) is an INAF project to construct and operate an experiment to study gamma-ray sources emitting at very high-energy in the TeV spectral band. This document defines the Use Cases of the Power Management System Collector (PMSC).

The Compton Spectrometer and Imager (COSI) is a 0.2-5 MeV Compton telescope capable of imaging, spectroscopy, and polarimetry of astrophysical sources. Such capabilities are made possible by COSI's germanium cross-strip detectors, which provide high efficiency, high resolution spectroscopy and precise 3D positioning of photon interactions. Science goals for COSI include studies of 0.511 MeV emission from antimatter annihilation in the Galaxy, mapping radioactive elements from nucleosynthesis, determining emission mechanisms and source geometries with polarization, and detecting and localizing multimessenger sources. The instantaneous field of view (FOV) for the germanium detectors is >25% of the sky, and they are surrounded on the sides and bottom by active shields, providing background rejection as well as allowing for detection of gamma-ray bursts or other gamma-ray flares over >50% of the sky. We have completed a Phase A concept study to consider COSI as a Small Explorer (SMEX) satellite mission, and here we discuss the advances COSI-SMEX provides for astrophysics in the MeV bandpass., 9 pages, 4 figures, 1 table, author affiliations provided on final page. arXiv admin note: substantial text overlap with arXiv:1908.04334

Several types of Galactic sources, like magnetars, microquasars, novae or pulsar wind nebulae flares, display transient emission in the X-ray band. Some of these sources have also shown emission at MeV--GeV energies. However, none of these Galactic transients have ever been detected in the very-high-energy (VHE; E$>$100 GeV) regime by any Imaging Air Cherenkov Telescope (IACT). The Galactic Transient task force is a part of the Transient Working group of the Cherenkov Telescope Array (CTA) Consortium. The task force investigates the prospects of detecting the VHE counterpart of such sources, as well as their study following Target of Opportunity (ToO) observations. In this contribution, we will show some of the results of exploring the capabilities of CTA to detect and observe Galactic transients; we assume different array configurations and observing strategies., 37th International Cosmic Ray Conference (ICRC2021)

The ASTRI Mini-Array is an international collaboration led by the Italian National Institute for Astrophysics (INAF), aiming to construct and operate an array of nine Imaging Atmospheric Cherenkov Telescopes (IACTs) to study gamma-ray sources at very high energy (TeV) and to perform stellar intensity interferometry observations. This contribution describes the design and the technologies used by the ASTRI team to implement the Online Observation Quality System (OOQS). The main objective of the OOQS is to perform data quality analyses in real-time during Cherenkov and intensity interferometry observations to provide feedback to both the Central Control System and the Operator. The OOQS performs the analysis of key data quality parameters and can generate alarms to other sub-systems for a fast reaction to solve critical conditions. The results from the data quality analyses are saved into the Quality Archive for further investigations. The Operator can visualise the OOQS results through the Operator Human Machine Interface as soon as they are produced. The main challenge addressed by the OOQS design is to perform online data quality checks on the data streams produced by nine telescopes, acquired by the Array Data Acquisition System and forwarded to the OOQS. In the current OOQS design, the Redis in-memory database manages the data throughput generated by the telescopes, and the Slurm workload scheduler executes in parallel the high number of data quality analyses., 8 pages, 3 figures, Proceedings of the 37th International Cosmic Ray Conference (ICRC 2021), Berlin, Germany

The Cherenkov Telescope Array (CTA) is an initiative that is currently building the largest gamma-ray ground Observatory that ever existed. A Science Alert Generation (SAG) system, part of the Array Control and Data Acquisition (ACADA) system of the CTA Observatory, analyses online the telescope data - arriving at an event rate of tens of kHz - to detect transient gamma-ray events. The SAG system also performs an online data quality analysis to assess the instruments' health during the data acquisition: this analysis is crucial to confirm good detections. A Python and a C++ software library to perform the online data quality analysis of CTA data, called rta-dq-lib, has been proposed for CTA. The Python version is dedicated to the rapid prototyping of data quality use cases. The C++ version is optimized for maximum performance. The library allows the user to define, through XML configuration files, the format of the input data and, for each data field, which quality checks must be performed and which types of aggregations and transformations must be applied. It internally translates the XML configuration into a direct acyclic computational graph that encodes the dependencies of the computational tasks to be performed. This model allows the library to easily take advantage of parallelization at the thread level and the overall flexibility allow us to develop generic data quality analysis pipelines that could also be reused in other applications.

The present document is aimed at providing a complete description of all the work and outcome done during the AREMBES Core Technology Program (CTP) project that has been kicked-off on March 21st, 2016. AREMBES is the acronym for “ATHENA Radiation Environment Models and X-ray Background Effects Simulators” which is a project carried out under the ESA Contract No. 4000116655/16/NL/BW [AD1] and successive CCN1 [AD2]. The reference space mission which is the bone of the present CTP project is Athena, the 2nd ESA Large Class mission to be launched on early 2030’s. The main tasks carried out have been: characterization of L2 particle environment; optimization of a new physics list for Athena aims; development of a user-friendly simulator framework to perform simulation of particle interaction with payload/detectors. During the development of the project, a CCN1 has been also put in place ([AD2], 16/05/2017) addressing the necessity in expanding the knowledge of the particle environment also at the L1 Lagrangian Point, beyond the baselined L2 one. The main outcomes of the AREMBES project have been: 1) the detailed study of L2 vs L1 particle environment (ESA – ASST have taken into account also this study to take in the close future a final decision about the Athena satellite orbit) 2) the creation of the Geant4 Space Physics List (ESA has endorsed this List as the reference to be used in Athena NXB Geant4 assessment study) 3) the creation of the “core” of the Simulator Framework 4) the creation of the mass models of the two focal plane instruments and the Athena optics and flight module 5) to contribute up to 23 publication on peer reviewed journals, conferences proceeding, citations from/to AREMBES, etc (see Annex 1 for details) The present report is structured as follows: §1 Comprehensive introduction of the context §2 Description of the programme of work §3 Description of the activities performed, and main results achieved §4 Open issues, bugs and recommendations for future work related to the ASF

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 in 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 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 based on the inspection of data 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., Proceedings of the 17th International Conference on Accelerator and Large Experimental Physics Control Systems, ICALEPCS2019, New York, NY, USA

The first direct detection of gravitational waves (GW) by Advanced LIGO detectors in September 2015 has drawn the attention of the astrophysical community that is now searching for the electromagnetic counterparts of the detected GW events. The AGILE (Astro-Rivelatore Gamma a Immagini Leggero) mission is primarily devoted to the high-energy astrophysical study of gamma-ray sources in the 30 MeV to 30 GeV energy range. The capability of the AGILE satellite for the discovery of transients is unique: the actual spinning configuration of the satellite, together with a large field of view and a good sensitivity of F =(1-2) ×10-8ergcm-2 s-1 for 100s integrations, provides a coverage of 80% of the sky, with each position exposed for 100 seconds, 200 times a day. The AGILE team signed a memorandum of understanding (MoU) with the LIGO/Virgo collaboration to follow the GW notices provided through the GCN network. In this paper we describe our automated pipeline that reacts to LIGO/Virgo GW notices and performs different kind of automated analysis to boost the search for of GW event counterparts.

In this paper is described the approach used to develop the software system of the AGILE γ-ray Observatory, from the definition phase to construction, verification and calibration activities of the satellite, until operations for scientific observations. Flexible software architectures, effective software management workflow, new algorithms (from payload simulators to reconstruction algorithms, from detection algorithms for Real-Time Analysis systems to the follow-up of science alerts in the multi-wavelenght and multi-messenger context) and team management approach are described. The approach followed by the AGILE Team in more than twenty years of work is a key element of the success of the AGILE Observatory, and the foundation for the involvement in new high-energy telescopes and observatories. Our legacy is not only in experience and tools but also in lesson learned, that are described in this work.

Consider $n$ independent measurements, with the additional information of the times at which measurements are performed. This paper deals with testing statistical hypotheses when $n$ is large and only a small amount of observations concentrated in short time intervals are relevant to the study. We define a testing procedure in terms of multiple likelihood ratio (LR) statistics obtained by splitting the observations into groups, and in accordance with the following principles: P1) each LR statistic is formed by gathering the data included in $G$ consecutive vectors of observations, where $G$ is a suitable time window defined a priori with respect to an arbitrary choice of the `origin of time'; P2) the null statistical hypothesis is rejected only if at least $k$ LR statistics are sufficiently small, for a suitable choice of $k$. We show that the application of the classical Wilks' theorem may be affected by the arbitrary choice of the "origin of time", in connection with P1). We then introduce a Wilks' theorem for grouped data which leads to a testing procedure that overcomes the problem of the arbitrary choice of the `origin of time', while fulfilling P1) and P2). Such a procedure is more powerful than the corresponding procedure based on Wilks' theorem., arXiv admin note: text overlap with arXiv:1411.0947

The Cherenkov Telescope Array (CTA) project is an international initiative to build a next generation ground-based observatory for very high energy gamma-rays. Three classes of telescopes with different mirror size will be located in the northern and southern hemispheres. The ASTRI mini-array of CTA preproduction is one of the small sized telescopes mini-arrays proposed to be installed at the CTA southern site. The ASTRI mini-array will consist of nine units based on the end-to-end ASTRI SST-2M prototype already installed on Mt. Etna (Italy). The mini-array software system (MASS) supports the end to end ASTRI SST-2M prototype and miniarray operations. The ASTRI software integration team defined the procedures to perform effectively the integration test and release activities. The developer has to properly use the repository tree and branches according to the development status. We require that the software includes also specific sections for automated tests and that the software is well tested (in simulated and real system) before any release. Here we present the method adopted to release the first MASS version to support the ASTRI SST-2M prototype test and operation activities., Proceedings of the 16th Int. Conf. on Accelerator and Large Experimental Control Systems, ICALEPCS2017, Barcelona, Spain

Low energy protons (< 300 keV) can enter the field of view of X-ray telescopes, scatter on their mirror surfaces at small incident angles, and deposit energy on the detector. This phenomenon can cause intense background flares at the focal plane decreasing the mission observing time (e.g. the XMM-Newton mission) or in the most extreme cases, damaging the X-ray detector. A correct modelization of the physics process responsible for the grazing angle scattering processes is mandatory to evaluate the impact of such events on the performance (e.g. observation time, sensitivity) of future X-ray telescopes as the ESA ATHENA mission. The Remizovich model describes particles reflected by solids at glancing angles in terms of the Boltzmann transport equation using the diffuse approximation and the model of continuous slowing down in energy. For the first time this solution, in the approximation of no energy losses, is implemented, verified, and qualitatively validated on top of the Geant4 release 10.2, with the possibility to add a constant energy loss to each interaction. This implementation is verified by comparing the simulated proton distribution to both the theoretical probability distribution and with independent ray-tracing simulations. Both the new scattering physics and the Coulomb scattering already built in the official Geant4 distribution are used to reproduce the latest experimental results on grazing angle proton scattering. At 250 keV multiple scattering delivers large proton angles and it is not consistent with the observation. Among the tested models, the single scattering seems to better reproduce the scattering efficiency at the three energies but energy loss obtained at small scattering angles is significantly lower than the experimental values. In general, the energy losses obtained in the experiment are higher than what obtained by the simulation. The experimental data are not completely representative of the soft proton scattering experienced by current X-ray telescopes because of the lack of measurements at low energies (< 200 keV) and small reflection angles, so we are not able to address any of the tested models as the one that can certainly reproduce the scattering behavior of low energy protons expected for the ATHENA mission. We can, however, discard multiple scattering as the model able to reproduce soft proton funnelling, and affirm that Coulomb single scattering can represent, until further measurements at lower energies are available, the best approximation of the proton scattered angular distribution at the exit of X-ray optics. Low energy protons (< 300 keV) can enter the field of view of X-ray space telescopes, scatter at small incident angles, and deposit energy on the detector, causing intense background flares at the focal plane or in the most extreme cases, damaging the X-ray detector. A correct modelization of the physics process responsible for the grazing angle scattering processes is mandatory to evaluate the impact of such events on the performance of future X-ray telescopes as the ESA ATHENA mission. For the first time the Remizovich model, in the approximation of no energy losses, is implemented top of the Geant4 release 10.2. Both the new scattering physics and the built-in Coulomb scattering are used to reproduce the latest experimental results on grazing angle proton scattering. At 250 keV multiple scattering delivers large proton angles and it is not consistent with the observation. Among the tested models, the single scattering seems to better reproduce the scattering efficiency at the three energies but energy loss obtained at small scattering angles is significantly lower than the experimental values. In general, the energy losses obtained in the experiment are higher than what obtained by the simulation. The experimental data are not completely representative of the soft proton scattering experienced by current X-ray telescopes because of the lack of measurements at low energies (< 200 keV) and small reflection angles, so we are not able to address any of the tested models as the one that can certainly reproduce the scattering behavior of low energy protons expected for the ATHENA mission. We can, however, discard multiple scattering as the model able to reproduce soft proton funneling, and affirm that Coulomb single scattering can represent, until further measurements, the best approximation of the proton scattered angular distribution at the exit of X-ray optics.

The Cherenkov Telescope Array (CTA) project is an international initiative to build the next generation of ground-based very high energy gamma-ray instrument . Three classes of telescopes with different mirror size will cover the full energy range from tens of GeV up to hundreds of TeV. The full sky coverage will be assured by two arrays, with one site located in each of the northern and southern hemispheres. In the current design scenario, the southern hemisphere array of CTA will include seventy small size telescopes (SST, 4m diameter) covering the highest energy region. Their implementation includes proposed intermediate steps with the development of mini-arrays of telescope precursors like the ASTRI mini-array, led by the Italian National Institute for Astrophysics (INAF) in synergy with the Universidade de Sao Paulo (Brazil) and the North-West University (South Africa). The ASTRI mini-array will be composed of nine telescope units (ASTRI SST-2M) based on double-mirror configuration whose end-to-end prototype has been installed on Mt. Etna (Italy) and is currently undergoing engineering tests. In the ASTRI SST-2M prototype, operating in single telescope configuration, the basic camera server software is being deployed and tested; it acquires the data sent by the camera back end electronics as a continuous stream of packets. In near real time, the bulk data of a given run are stored in one raw file. In parallel they are sorted by data type, converted to FITS format and stored in one file for data type. Upon closure, each file is transferred to the on-site archive. In addition, the quick look component allows the operator to display the camera data during the acquisition. This contribution presents how the camera server software of the prototype is being upgraded in order to fulfil the mini-array requirements, where it will be deployed on the camera server of each ASTRI SST-2M telescope. Particular emphasis will be devoted to the most challenging requirements that are related to the stereoscopy, when two or more telescopes have triggered simultaneously. To handle stereoscopy, each camera server has also to: (i) get the timestamp information from the clock distribution and trigger time stamping system, and associate it to the related camera event; (ii) get from the software array trigger the timestamp which passed the stereo trigger criteria; and (iii) forward to the array data acquisition system the stereo trigger events, according to the required data format and communication protocol.