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MIRIAD
MIRIAD is a software package and data-reduction system widely used for interferometric radio-astronomy data, developed to support synthesis-imaging observations and calibration from arrays and millimetre facilities. It provides tools for visibility manipulation, imaging, deconvolution, calibration, and analysis, and has been applied to data from a range of telescopes and observatories to produce maps, spectra, and derived astrophysical products. The package is notable for its role in processing data from several prominent facilities and for influencing later software such as CASA and AIPS++.
MIRIAD originated as an integrated collection of programs for handling interferometric data, offering tasks that perform flagging, Fourier inversion, CLEAN deconvolution, self-calibration, and image restoration. It has been used in conjunction with arrays and instruments including the Australia Telescope Compact Array, the Submillimetre Array, and the Combined Array for Research in Millimeter-wave Astronomy, enabling users to convert raw visibilities into calibrated images and spectral-line cubes. The package provided command-line utilities, scripting interfaces, and task libraries suitable for astronomers working with continuum, spectral-line, and polarimetric observations.
MIRIAD was developed in the late 20th century by teams at institutions such as the Australia Telescope National Facility and related groups to address limitations of existing packages like AIPS for millimetre and compact-array interferometry. Early contributors included engineers and scientists associated with facilities and projects at institutions such as the Commonwealth Scientific and Industrial Research Organisation, the University of Sydney, and collaborating observatories. Over time, MIRIAD evolved through community-driven enhancements, patches, and ports across UNIX-like systems, reflecting developments at observatories including the Australia Telescope Compact Array, the James Clerk Maxwell Telescope, and other radio facilities.
Although MIRIAD itself is software, its capabilities were tailored to the characteristics of instrumentation such as interferometric baselines, correlator configurations, and receiver setups observed at arrays like the Australia Telescope Compact Array, the Submillimeter Array, and the Nobeyama Radio Observatory. Tasks support calibration strategies for complex gains, bandpass, and polarisation products arising from feeds and receivers designed by groups at institutions like the Max Planck Institute for Radio Astronomy and the National Radio Astronomy Observatory. The software handles multi-channel spectral datasets produced by correlators comparable to those at the Very Large Array, the Atacama Large Millimeter/submillimeter Array, and the Plateau de Bure Interferometer.
MIRIAD includes utilities for visibility-format conversion, baseline-based editing, time-dependent calibration, imaging with FFT inversion, and deconvolution via CLEAN algorithms and variants. The package interfaces with system libraries and compilers common at research centers such as the University of Manchester, the California Institute of Technology, and the Harvard–Smithsonian Center for Astrophysics. Users have often integrated MIRIAD workflows with scripting environments and pipeline frameworks developed at observatories like the European Southern Observatory, the National Astronomical Observatory of Japan, and the Leibniz Institute for Astrophysics Potsdam to automate reduction for surveys and target-of-opportunity projects.
MIRIAD has been used to produce scientific results across topics including star formation studies in regions observed by teams working at institutions like the Max Planck Institute for Astronomy, molecular-line surveys by research groups at the Smithsonian Astrophysical Observatory, and imaging of active galactic nuclei investigated by collaborations involving the University of Cambridge and the International Centre for Radio Astronomy Research. The software enabled mapping of molecular clouds, kinematic analyses in protoplanetary discs, and continuum imaging of radio galaxies studied by researchers at the University of Oxford and the California Institute of Technology. Results processed with MIRIAD have been published in journals and presented at meetings organized by the American Astronomical Society, the International Astronomical Union, and the Astronomical Society of Australia.
Compared to packages such as AIPS, CASA, and GILDAS, MIRIAD offered a simpler, lightweight toolset optimized for compact-array and millimetre data workflows used by observatories including the Australia Telescope Compact Array, the James Clerk Maxwell Telescope, and the Submillimeter Array. While AIPS from the National Radio Astronomy Observatory emphasized legacy VLA-era processing and CASA from the National Radio Astronomy Observatory and partners provided modern Python-driven pipelines for ALMA and VLA, MIRIAD retained popularity within user communities at institutions like the University of Sydney and CSIRO for its direct handling of certain correlator formats and its established task set. GILDAS, developed by IRAM and associated European institutes, focuses on single-dish and interferometer data with strengths in spectral analysis; MIRIAD complemented these tools in multi-instrument campaigns and joint-reduction efforts.
Future work historically discussed for MIRIAD communities included porting more functionality to contemporary platforms, integrating with Python ecosystems popular at institutions such as the Massachusetts Institute of Technology, enabling interoperability with CASA measurement sets used by ALMA and the Very Large Array, and updating algorithms to support wideband imaging and advanced deconvolution techniques pioneered by teams at the National Radio Astronomy Observatory and the European Southern Observatory. Collaborative initiatives among universities, national laboratories, and observatories—such as those involving the Max Planck Society and the Australian research community—have explored pathways to preserve legacy MIRIAD workflows while migrating to unified, scalable reduction environments suitable for next-generation arrays and survey projects.
Category:Radio astronomy software