AGILE is an ASI (Italian Space Agency) Small Scientific Mission dedicated to high-energy astrophysics which was launched on April 23 2007 from Satish Dawan Space Centre, India) on a PSLV-C8 rocket. The AGILE Payload is composed of three instruments: a Tungsten-Silicon Tracker designed to detect and image photons in the 30 MeV-50 GeV energy band, an X-ray imager called SuperAGILE that works in the 18-60 keV energy band, and a Minicalorimeter that detects gamma-rays or particle energy deposits between 300~keV and 200~MeV. The instrument is surrounded by an anti-coincidence (AC) system. We have developed a set of Quick Look software tools in the framework of the Test Equipment (TE) and the Electrical Ground Support Equipment (EGSE. This s/w is required in order to support all the assembly, integration and verification (AIV) activities to be carried out for the AGILE mission, from data handling unit level to payload integrated level, calibration campaign, launch campaign and in-orbit commissioning. These software tools have enabled us to test the engineering performance and to perform a health check of the Payload during the various phases. We have used an incremental development approach and a common framework to rapidly adapt our software to the different requirements of the various phases.

The AGILE Science Tools are written in C++ and are based on the ROOT (CERN) and CFITSIO (NASA) libraries. All the tools can be run from the command line. The Science Tools use the Parameter Interface Library (PIL), developed by the ISDC, for parameter input, allowing a variety of input methods: 1. the user can input all or some of the parameters on the command line, in the same order as the provided parameter file; 2. the user can start the tool, which then asks for the values of some parameters interactively on the console; 3. by adding ’mode=h’ on the command line, the user can accept all the defaults (the last values used) for parameter values not explicitly provided on the command line The input and output files are in FITS format. FITS files consist of a series of units, each containing a header and data. Each header contains a list of ’keywords’ and their values, which describe the format of the data. The first unit is the ’primary’ unit and may or may not contain data. The subsequent units are called ’extensions.’ FITS files can be read and modified by standard tools such as fv and the output maps generated by the tools can be displayed with the ds9 tool.

The Italian AGILE space mission, with its Gamma-Ray Imaging Detector (GRID) instrument sensitive in the 30 Me–50 GeV γray energy band, has been operating since 2007. Agilepy is an open-source Python package to analyse AGILE/GRID data. The package is built on top of the command-line version of the AGILE Science Tools, developed by the AGILE Team, publicly available and released by ASI/SSDC. The primary purpose of the package is to provide an easy to use high-level interface to analyse AGILE/GRID data by simplifying the configuration of the tasks and ensuring straightforward access to the data. The current features are the generation and display of sky maps and light curves, the access to \gray sources catalogues, the analysis to perform spectral model and position fitting, the wavelet analysis. Agilepy also includes an interface tool providing the time evolution of the AGILE off-axis viewing angle for a chosen sky region. The Flare Advocate team also uses the tool to analyse the data during the daily monitoring of the γray sky. Agilepy (and its dependencies) can be easily installed using Anaconda.

The Command-line Catalogue Cross-matching (C3) software efficiently performs the positional cross-match between massive catalogues from modern astronomical surveys, whose size have rapidly increased in the current data-driven science era. Based on a multi-core parallel processing paradigm, it is executed as a stand-alone command-line process or integrated within any generic data reduction/analysis pipeline. C3 provides its users with flexibility in portability, parameter configuration, catalogue formats, angular resolution, region shapes, coordinate units and cross-matching types.

The DAOSPEC Output Optimizer pipeline (DOOp) runs efficient and convenient equivalent widths measurements in batches of hundreds of spectra. It uses a series of BASH scripts to work as a wrapper for the FORTRAN code DAOSPEC (ascl:1011.002) and uses IRAF (ascl:9911.002) to automatically fix some of the parameters that are usually set by hand when using DAOSPEC. This allows batch-processing of quantities of spectra that would be impossible to deal with by hand. DOOp was originally built for the large quantity of UVES and GIRAFFE spectra produced by the Gaia-ESO Survey, but just like DAOSPEC, it can be used on any high resolution and high signal-to-noise ratio spectrum binned on a linear wavelength scale.

DPI is a FORTRAN77 library that supplies the symplectic mapping method for binary star systems for the Mercury N-Body software package (ascl:1201.008). The binary symplectic mapping is implemented as a hybrid symplectic method that allows close encounters and collisions between massive bodies and is therefore suitable for planetary accretion simulations. [Source code is in Astrophysics Source Code Library]

Questo software, basato su framework Django, è stato sviluppato per la gestione delle procedure di acquisto di INAF-Osservatorio Astronomico di Palermo, soddisfacendo l'esigenza di digitalizzare un processo multistep che richiede una sequenza di autorizzazioni e "firme". L'interfaccia utente è una web-app accessibile remotamente con autenticazione. Utilizza un database per raccogliere le informazioni sugli utenti abilitati e sulle procedure in atto e concluse. Ogni procedura consiste in una sequenza di sezioni, costituite da form, che possono essere compilate esclusivamente dai responsabili assegnati. E' possibile inserire allegati in ciascuna sezione. Le sezioni possono essere salvate per essere completate successivamente. Quando una sezione viene finalizzata (chiusa), il software invia una notifica email ai responsabili della successiva sezione aperta. Le sezioni possono essere chiuse in ordine sparso secondo esigenza, sebbene la sequenza rifletta il flusso ordinario di lavorazione. Una sezione chiusa può essere riaperta dal responsabile della sezione successiva. Le sezioni di una procedura vengono visualizzate in sequenza in una singola pagina web, con un menu di navigazione laterale che consente di avere una panoramica dello stato di chiusura delle sezioni e di saltare ad una sezione specifica. La struttura del software è flessibile, per consentire facili variazioni al flusso della procedura, alle sezioni e ai campi presenti nelle sezioni. In caso di aggiornamento del flusso di procedura viene assegnata una nuova versione e viene mantenuto il supporto a ordini ancora aperti con versione di procedura precedente. Determinati campi o intere sezioni possono essere mostrate o meno in funzione di valori selezionati in sezioni precedenti, in modo da consentire flussi alternativi, o l'inserimento di informazioni diverse, per differenti casistiche (es. gare piuttosto che affidamento diretto, oppure ordine tramite MEPA o meno). Il software è stato adottato stabilmente dalla struttura OAPA a partire da giugno 2015.

GOFIO is a DRS written for the GIANO-B infrared spectra. It is installed at the Telescopio Nazionale Galileo (TNG) and it is part of the online reduction pipeline running at the telescope, but it can work also as a standalone offline DRS without a graphical interface, which allows to reduce the ramp-processed raw files available in the TNG archive. GOFIO processes all the calibration and scientific images, observed both in the nodding and stare mode. The reduction process includes bad pixel and cosmic removal, flat-field and blaze correction, optimal extraction, wavelength calibration with U-Ne lamps, nodding or stare group processing. A logfile of the whole reduction process is created and stored in the reduction directory. In the offline mode, the reduction process can be completely customized, but it is suggested to use only the command line options, unless having a great familiarity with the instrument and its settings.

The model describes correctly all the aspects of the LFAA station beamformer. It is an useful tool to analyze variants of the proposed signal processing algorithms or to highlight possible problems. It can also be used to test different calibration strategies and to provide the CSP model with a realistic input signal.

LIRA (LInear Regression in Astronomy) performs Bayesian linear regression that accounts for heteroscedastic errors in both the independent and the dependent variables, intrinsic scatters (in both variables), time evolution of slopes, normalization and scatters, Malmquist and Eddington bias, and break of linearity. The posterior distribution of the regression parameters is sampled with a Gibbs method exploiting the JAGS (ascl:1209.002) library.

The Layer-Oriented Simulation Tool (LOST) is a code for simulating the performance of multiconjugate adaptive optics modules that uses a layer-oriented approach. It calculates atmospheric layers as phase screens, and then calculates the phase delays caused by these screens on the wave fronts of natural guide stars through geometrical optics approximations. This simulation considers the impact of wave-front sensors on measurement phase noise when combining wave fronts optically or numerically. The LOST code is explained in a dedicated publication. It was used for the estimation of the performance of the two layer-oriented modules MAD and NIRVANA, specifically the Multiconjugate Adaptive Optics Demonstrator for the Very Large Telescope and the Near-IR-Visible Adaptive Interferometer for Astronomy for the Large Binocular Telescope.

The ProcessorLib is a C++ library used to write processors for Test Equiments for AIV/AIT activities. The ProcessorLib has been used in the AIV/AIT activities of AGILE satellite and in the CIWS project

Every planetary exploration study faces a common challenge: integrating images from diverse sources, each with unique spatial and spectral resolutions, and often, georeferencing inaccuracies. This software suite is dedicated to facilitating the integration of surface images of planetary bodies through simplified co-registration procedures and reciprocal resolution enhancement using CS pansharpening techniques. The first validation study is currently being reviewed in Planetary and Space Science, and involves tests on the mutual implementation of ESA TGO CaSSIS and NASA MRO HiRISE images.

pyLCSIM simulates X-ray lightcurves from coherent signals and power spectrum models. Coherent signals can be specified as a sum of one or more sinusoids, each with its frequency, pulsed fraction and phase shift; or as a series of harmonics of a fundamental frequency (each with its pulsed fraction and phase shift). Power spectra can be simulated from a model of the power spectrum density (PSD) using as a template one or more of the built-in library functions. The user can also define his/her custom models. Models are additive.

QSFit performs automatic analysis of Active Galactic Nuclei (AGN) optical spectra. It provides estimates of: AGN continuum luminosities and slopes at several restframe wavelengths; luminosities, widths and velocity offsets of 20 emission lines; luminosities of iron blended lines at optical and UV wavelengths; host galaxy luminosities. The whole fitting process is customizable for specific needs, and can be extended to analyze spectra from other data sources. The ultimate purpose of QSFit is to allow astronomers to run standardized recipes to analyze the AGN data, in a simple, replicable and shareable way.

Sensitive detectors, as transition edge sensors, operating in X-ray instrumentation from space (or in laboratories) are susceptible to degradation due to photons at lower energies than X-rays. Although the detector does not trigger on individual low energy photons, the statistical fluctuation of the absorbed energy during the effective X-rays detection time, can introduce a degradation of the energy resolution of the detector known as Photon Shot Noise (PSN). Thermal filters are usually interposed between the optics and the detector to minimize the PSN due to out of band radiation from the instrument warm surfaces and from external light sources. The PSN strongly depends on the geometry of the system, since the photons rejected by a filter are mainly reflected, and after further reflections they can reach the filter again and again. Multiple reflections on the system surfaces have thus the effect of increasing the amount of unwanted energy that can reach the detector, raising the PSN. A careful design of the geometries and of their surface properties (reflectivity/emissivity) is necessary to guarantee the PSN levels needed for meeting the instrument requirements. This code, "ray3cer", has been developed to evaluate the PSN for a specified configuration, taking in account multiple reflections. A trivial Monte Carlo simulation is not apt, since the very high rejection given by the filters allows only for a small fraction of photons to reach the detector, and an unreasonable number of photons should be simulated to attain a passable statistic. The approach adopted is to calculate all the possible trajectories for each simulated photon, within a probability threshold limit, to evaluate the overall probability for the photon to reach the detector. This technique bypasses the limitation due to the filter rejection and allows for a simulation with a good statistic with a relatively small number of simulated photons.

REPS (REscaled Power Spectra) provides accurate, one-percent level, numerical simulations of the initial conditions for massive neutrino cosmologies, rescaling the late-time linear power spectra to the simulation initial redshift

SpectraPy is an Astropy affiliated package, which collects algorithms and methods for data reduction of astronomical spectra obtained by a through slits spectrograph. The library is designed to be spectrograph independent. It comes with a set of already configured spectrographs, but it can be easily configured to reduce data of other instruments. Current implementation of SpectraPy is focused on the extraction of 2D spectra: it produces wavelength calibrated spectra, rectified for instrument distortion. The library can be used on both longslit (LS) and multi object spectrograph (MOS) data.

Stingray is a spectral-timing software package for astrophysical X-ray (and more) data. The package merges existing efforts for a (spectral-)timing package in Python and is composed of a library of time series methods (including power spectra, cross spectra, covariance spectra, and lags); scripts to load FITS data files from different missions; a simulator of light curves and event lists that includes different kinds of variability and more complicated phenomena based on the impulse response of given physical events (e.g. reverberation); and a GUI to ease the learning curve for new users.