General definitions of astronomy or statistical terms are included on this page.
The International Astronomical Union is constructing a glossary of common astronomy terms (see https://astro4edu.org/resources/glossary/search/). Here we plan to build up a similar dictionary, focusing on both statistics and astronomy jargon.
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In astronomy, calibration is the process by which the electrical signals output from an instrument are converted into physically meaningful quantities. You may point your telescope at an object and collect 1000 photons from it, but how does that translate to a physically meaningful flux (energy unit time per unit area passing through the telescope aperture)? Answering such questions requires calibration of the detector. Calibration seeps into every aspect of the measurement process, even to establish when you can say you have detected a photon in a sensor (like a CCD – a charge coupled device imaging semiconductor circuit).
In astronomy, color is the difference between two magnitudes (a standardized measure of ranked brightness of an astronomical object such as a star). Magnitudes are defined as scaled logarithmic intensities relative to some standard value, and colors are thus scaled logarithmic ratios of intensities or counts from a source measured in different passbands. Colors are often used as proxies for properties of the source; e.g., B-V in the Johnson filter system tracks the surface temperatures of stars.
In astronomy, cstat (aka C-stat or Cash statistics) is a measure of the ln(Poisson likelihood). It is a drop-in replacement for χ², and is a convenient statistic used by high-energy astronomers to find maximum likelihood estimates in a non-linear regression of Poisson binned counts data (see, e.g., Kaastra 2017, A&A 605, A51). It is written in a form that can be derived either from the Stirling approximation to the factorial, or as a likelihood ratio of two models where the model of interest is compared to a “perfect” model which matches the observed counts exactly, cstat=–2∑K(modelk–countsK)+countsK⋅(ln(countsK)–ln(modelK))), and the summation is carried out over all bins K. In this form it is asymptotically distributed as χ². There is another statistic called wstat, which is sometimes also called cstat, which includes a term describing a marginalized background.
In astronomy, the sensitivity of a telescope and detector system varies strongly with photon energy. The cross-section that the system presents to the sky is a fraction of the geometric area, and is called the effective area (often abbreviated EA). It is regularly reevaluated over the lifetime of a telescope, and is a critical part of instrument calibration. In optical and IR astronomy, this is often called sensitivity or response, and variations in the transmissions of different filters are often used to obtain color information. In high-energy astronomy, the effective area is first measured at ground-based facilities and adjusted in-flight by observations of objects with well-understood spectra. These effective areas are usually available as Ancillary Response Files (ARFs) with the data.