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"The Astrophysics Source Code Library (ASCL) is a free online registry and repository for source codes of interest to astronomers and astrophysicists, including solar system astronomers, and lists codes that have been used in research that has appeared in, or been submitted to, peer-reviewed publications. The ASCL is indexed by the SAO/NASA Astrophysics Data System (ADS) and Web of Science and is citable by using the unique ascl ID assigned to each code. The ascl ID can be used to link to the code entry by prefacing the number with ascl.net (i.e., ascl.net/1201.001)."

"Relativistic image doubling (RID) can occur when an object or image outpaces its own emission. This can happen, for example, when a muon travels faster than light through water and when a laser spot is swept across an infinitely extended wall. It also occurs for a shadow produced at sunrise on an infinitely flat plane. This code shows how two shadow images are created and propagate in opposite directions. For an extended object, successively higher portions undergo RID at later times, so both shadow images develop from the base of the object toward its apex rather than appearing as instantaneous projections of the complete object. This code includes both exact calculations and those including small-angle approximations for both a 1-dimensional extended object and a 2-dimensional object with a circular cross-section."

"DMS (Debris disks around Main-sequence Stars) computes the spectral energy distribution, thermal emission maps, scattered-light images and linear-polarization images (Stokes Q, U, Q_phi, U_phi) of optically thin debris disks, together with the fractional luminosity and the optical depth. The user specifies the star, the dust and the geometry of up to ten belts, which may be eccentric. DMS calculates the grain temperatures and optical properties (Mie theory, coated spheres, a distribution of hollow spheres, and effective-medium mixtures), including ice sublimation and radiation-pressure blow-out, and integrates the emission along the line of sight on an adaptively refined grid for any inclination and position angle. The Fortran core is parallelized with OpenMP and runs from the command line or through a Python interface that supports batch parameter studies."

"Modern digital radio astronomy receivers produce increasingly wide-bandwidth, high bit-rate data streams that necessitate the development of flexible, scalable, and maintainable back-end processing and recording systems. Historically, such back-end instrumentation has been tightly coupled to telescope observing modes, limiting reuse between observatories and science cases. We present the Effelsberg Direct Digitisation (EDD) back-end framework, a software-defined architecture for constructing real-time radio astronomy back ends on commodity off-the-shelf computing infrastructure. We describe its design, implementation, supported observing modes, and operational deployments. EDD separates a common core framework from plug-in-provided observing capabilities. The core provides orchestration, telescope interfaces, pipeline lifecycle management, monitoring, and deployment tooling, while plug-ins implement processing pipelines for specific observing modes. The framework is designed to support both single-dish and interferometric instruments through site-specific configuration and plug-in selection. EDD currently supports spectroscopy and spectropolarimetry, pulsar timing and searching, baseband recording, very long baseline interferometry, correlation, and beam forming. Operational deployments include the Effelsberg 100-m telescope, the SKA-MPI prototype dish, the Thai National Radio Telescope, and the ARGOS interferometric prototype array. We show that when coupled with in-receiver digitisation, the EDD back end at Effelsberg provides $\sim30$\% improvement in pulsar time-of-arrival estimation compared with previous instruments, given the same observing bandwidth and integration time. EDD provides a reusable open-source framework for developing and operating real-time radio astronomy back ends. By separating common services, observing-mode plug-ins, and site-specific configuration, it allows back-end capabilities to be deployed across heterogeneous telescope environments and provides a community resource for broadband radio astronomy instrumentation."

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