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]

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.

This application allows to visualize the thermonuclear fusion helium burning within a star: the user can grab the nucleons in the screen (with the help of a kinect sensor) and can make them interact reproducing the nuclear reactions of the star in details highlighting the result of the fusion, that is the new element produced and, for the most interested, the elementary particles and the photons emitted.

This software was developed to fit many-parameters IR/Vis/UV transmission curve models of multilayers to measured data. It implements a modified Forouhi2019 model for the complex refractive index of materials, with revised fitting parameters that improve the stability of the fitting and the manual search of initial values. A matrix calculation of the transmission takes in account the interference effects beteween the layers. The implemented GUI allows to easily explore the initial parameters and to fine-tune them, as well as adding model terms.

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.

This application allows the users to see a cosmic object (or more objects) at different frequencies so that he/she can "see" the differences between one band and another.

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.

This application, with the help of an Oculus device, allow the user to get into a room within the universe. At the center of the room there are the planets of the solar system placed in a disorderly manner: the users must rebuild the solar system putting the planet in the right orbit.

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.

This application displays the stability valley β, introducing the concepts of stability for an element and for an isotope. With the help of this representation, an astronomer can introduce the basic concepts like the decay process beta and the neutron capture process slow and fast in a very easy way.

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.