The earliest and still most commonly used type of FITS data is an image header/data block. For example, it is possible to store x-ray and infrared exposures in the same file. A FITS file may contain several extensions, and each of these may contain a data object. The keyword/value pairs provide information such as size, origin, coordinates, binary data format, free-form comments, history of the data, and anything else the creator desires: while many keywords are reserved for FITS use, the standard allows arbitrary use of the rest of the name-space.įITS is also often used to store non-image data, such as spectra, photon lists, data cubes, or structured data such as multi-table databases. Each FITS file consists of one or more headers containing ASCII card images that carry keyword/value pairs, interleaved between data blocks. The information in this header is designed to calculate the byte offset of some information in the subsequent data unit to support direct access to the data cells. Image metadata is stored in a human-readable ASCII header. FITS was designed with an eye towards long-term archival storage, and the maxim once FITS, always FITS represents the requirement that developments to the format must be backward compatible. The FITS format was first standardized in 1981 it has evolved gradually since then, and the most recent version (4.0) was standardized in 2016. The FITS standard was designed specifically for astronomical data, and includes provisions such as describing photometric and spatial calibration information, together with image origin metadata. FITS is the most commonly used digital file format in astronomy. Flexible Image Transport System ( FITS) is an open standard defining a digital file format useful for storage, transmission and processing of data: formatted as multi-dimensional arrays (for example a 2D image), or tables.
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