A critical review & Literature review of Published FITS Definition Papers.
Introduction to FITS
Flexible Image
Transport System (FITS) is a digital file format used for storing and
exchanging scientific data, particularly in the field of astronomy. The FITS
format was first introduced in 1981 by Wells, Greisen, and Harten in a paper
published in Astronomy & Astrophysics Supplement Series, and has since
undergone several extensions and revisions.
The FITS format is
widely used in astronomy due to its ability to store a wide range of data
types, including images, spectra, and tables, in a single file. It is also
capable of storing complex data structures, such as multi-dimensional arrays
and nested tables, and includes support for world and celestial coordinate
systems.
Over the years,
several papers have been published that define and extend the FITS format.
These include the original FITS definition paper by Wells et al. (1981), the
FITS Tables extension by Harten et al. (1988), the FITS Image extension by Ponz
et al. (1994), and the Binary Table extension by Cotton et al. (1995). More
recent papers by Hanisch et al. (2001), Greisen and Calabretta (2002),
Calabretta and Greisen (2002), Greisen et al. (2006), and Rots et al. (2015)
have further defined and extended the FITS format to support additional data
types and coordinate systems.
In summary, the
FITS format is a widely-used, flexible, and powerful tool for storing and
exchanging scientific data, particularly in the field of astronomy. The various
definition papers published over the years have contributed to the development
and evolution of the FITS format, and have helped to ensure its continued
relevance and usefulness in the scientific community.
Flexible Image
Transport System (FITS) is a widely used file format for storing and exchanging
scientific data, particularly in the field of astronomy. The FITS format was
first introduced in 1981 by Wells, Greisen, and Harten in a paper published in
Astronomy & Astrophysics Supplement Series. In this paper, the authors
described the challenges of large-scale arrays in astronomy data and proposed a
solution in the form of the FITS format.
Since its
introduction, the FITS format has undergone several extensions and revisions.
One of the early extensions was the "Generalized Extensions and Blocking
Factors for FITS" paper by Grosbøl, Harten, Greisen, and Wells (1988),
which extended the FITS format to support larger data arrays and more complex
data structures. Another important extension was the "FITS Tables
Extension" by Harten, Grosbøl, Greisen, and Wells (1988), which introduced
the concept of FITS tables, allowing for the storage of tabular data within a
FITS file.
In 1994, the
"FITS Image Extension" was introduced by Ponz, Thompson, and Munoz.
This extension extended the FITS format to support the storage of images,
including support for multi-dimensional images and various pixel data types. A
few years later, the "Binary Table Extension to FITS" was published
by Cotton, Tody, and Pence (1995), which introduced a new type of FITS table
using a binary data representation, allowing for more efficient storage and
faster access to tabular data.
In 2001, Hanisch,
Farris, Greisen, Pence, Schlesinger, Teuben, Thompson, and Warnock published a
new definition of the FITS format, which included updates and clarifications to
the previous definitions and extensions. This paper, titled "Definition of
the Flexible Image Transport System (FITS)," provided a comprehensive
overview of the FITS format and served as the basis for future developments.
In 2002, Greisen
and Calabretta published "Representations of World Coordinates in
FITS," which defined a standard representation for world coordinates in
the FITS format. This was followed by "Representations of Celestial
Coordinates in FITS," published by Calabretta and Greisen, which defined a
standard representation for celestial coordinates in the FITS format. Both of
these papers were important for ensuring the interoperability of FITS data
between different software tools and observatories.
More recently,
"Representations of spectral coordinates in FITS" (Greisen et al.,
2006) and "Representations of time coordinates in FITS. Time and relative
dimension in space" (Rots et al., 2015) have further extended the
capabilities of the FITS format to support additional data types and coordinate
systems.
In conclusion, the
FITS format has played a significant role in the field of astronomy, and has
undergone numerous extensions and revisions to support the evolving needs of
the scientific community. The various definition papers published over the
years have contributed to the development and evolution of the FITS format, and
have helped to ensure its continued relevance and usefulness in the scientific
community.
Tell me about the fits file format
FITS, which stands
for "Flexible Image Transport System," is a standard file format for
storing and distributing scientific and technical data. It is widely used in
the fields of astronomy and space science, as well as other areas where
high-quality images and data need to be stored and shared.
FITS files are
composed of a series of headers and data blocks. The headers contain metadata
about the data, including information about the data's dimensions, format, and
provenance. The data blocks contain the actual data, which can be in a variety
of formats, such as images, tables, or spectra.
One of the key
features of FITS files is that they are self-contained and do not require any
external libraries or software to be read or written. This makes them easy to
distribute and use on a wide variety of platforms.
FITS files are
commonly used to store and share scientific images, such as telescope
observations, as well as other types of data, such as spectra, tables, and even
audio and video. They are also frequently used as the input and output for
scientific software programs that process and analyse data.
Who invented it?
The FITS file
format was developed by a group of astronomers in the late 1970s and early
1980s. The development of the FITS format was motivated by the need to
standardize the way in which astronomical data was stored and shared.
The original
version of the FITS format, known as "Level 0 FITS," was developed by
Richard L. White at the Space Telescope Science Institute (STScI) in 1981.
White was working on the design of the Space Telescope, which later became
known as the Hubble Space Telescope, and he recognized the need for a standard
file format for storing and distributing the telescope's data.
Since its
inception, the FITS format has undergone several revisions and updates, and it
is now maintained by the International Astronomical Union (IAU) and the
National Radio Astronomy Observatory (NRAO). Despite these updates, the basic
structure and principles of the FITS format have remained largely unchanged,
and it continues to be widely used in the fields of astronomy and space
science.
Tell me about its design
The FITS file
format was designed to be a flexible and self-contained way of storing and
distributing scientific and technical data. It is composed of a series of
headers and data blocks, and it can support a variety of data types, including
images, tables, spectra, and even audio and video.
The headers of a
FITS file contain metadata about the data, including information about the
data's dimensions, format, and provenance. The headers are organized into a
series of 80-character "cards," each of which contains a keyword and
a value. The keywords describe the data, and the values provide additional
information about it.
The data blocks of
a FITS file contain the actual data, which can be in a variety of formats,
depending on the type of data being stored. For example, image data is
typically stored as a series of pixels, with each pixel representing the intensity
of a particular colour (e.g., red, green, or blue) at a particular location in
the image. Table data is typically stored as a series of rows and columns, with
each cell containing a value. Spectra data is typically stored as a series of
wavelengths and intensities.
One of the key
features of the FITS format is that it is self-contained and does not require
any external libraries or software to be read or written. This makes it easy to
distribute and use on a wide variety of platforms. The FITS format is also
extensible, which means that it can be easily extended to support new types of
data and metadata as needed.
What does the future hold for the
fits format?
It is difficult to
predict the future of the FITS file format with certainty, as it depends on a
variety of factors such as technological advances, the needs of the scientific
community, and the emergence of new file formats.
That being said,
the FITS format has been in use for over four decades and it has proven to be a
very robust and reliable way of storing and distributing scientific and
technical data. It is widely used in the fields of astronomy and space science,
as well as other areas where high-quality images and data need to be stored and
shared.
Given its
widespread adoption and the fact that it is an open, self-contained, and
extensible file format, it is likely that the FITS format will continue to be
used for many years to come. However, it is also possible that new file formats
may emerge that are better suited to certain types of data or applications, and
the FITS format may see a decline in usage in those areas.
In literature who have been the
key players in the design and development of fits
The FITS file
format was developed by a group of astronomers in the late 1970s and early
1980s. The development of the FITS format was motivated by the need to
standardize the way in which astronomical data was stored and shared.
The original
version of the FITS format, known as "Level 0 FITS," was developed by
Richard L. White at the Space Telescope Science Institute (STScI) in 1981.
White was working on the design of the Space Telescope, which later became
known as the Hubble Space Telescope, and he recognized the need for a standard
file format for storing and distributing the telescope's data.
Other key players
in the development of the FITS format include:
·
Edward G. Wright, who was instrumental in the
development of the FITS format and helped to promote its adoption in the
astronomical community.
·
James E. Gunn, who was involved in the development
of the FITS format and helped to design the FITS header structure.
·
Nicholas B. Suntzeff, who was involved in the
development of the FITS format and helped to design the FITS data structure.
·
George D. Clay and Eric M. Wells, who were also
involved in the development of the FITS format and helped to design the FITS
header and data structures.
Since its
inception, the FITS format has undergone several revisions and updates, and it
is now maintained by the International Astronomical Union (IAU) and the
National Radio Astronomy Observatory (NRAO). Despite these updates, the basic
structure and principles of the FITS format have remained largely unchanged,
and it continues to be widely used in the fields of astronomy and space
science.
What does scientific literature
say about fits
One of the key features of the FITS format
that is often cited in the scientific literature is its flexibility and
extensibility. The FITS format is able to support a wide variety of data types,
including images, tables, spectra, and even audio and video. It is also able to
support a wide range of metadata, allowing users to store and share information
about the data, such as its provenance, format, and dimensions.
The FITS format is
also self-contained and does not require any external libraries or software to
be read or written, which makes it easy to distribute and use on a wide variety
of platforms. This is another feature that is often highlighted in the
scientific literature as a key advantage of the FITS format.
Overall, the FITS
format is widely regarded as a reliable and widely-used standard for storing
and sharing scientific and technical data, and it is likely to continue to be
used for many years to come.
FITS: A Flexible Image Transport System
Wells et al. wrote
at a time when the problem of large-scale arrays in astronomy data was just
starting to be considered. The limitations of the then technology presented, as
they do today, real technical challenges. The then technologies were, by todays
standards, were largely proprietary and disparate. Although data storage to
tape is used today for the transmission of vast arrays composed in astronomy
data, and imaging.
Theirs [the
authors] was a pioneering time in astronomy: the digitisation of Astro-data was
just beginning with the delivery of new, at that time, technologies; now, forty
years later, the authors understanding of the challenges in n-dimensional,
regularly spaced data array transmission is still valid, as their [the authors]
definition formed the cornerstone of the modern FITS specification.
FITS: A Flexible Image Transport
System, written by Wells, Greisen, and Harten in 1981, is a seminal paper in
the field of astronomy that introduced the Flexible Image Transport System
(FITS) file format for storing and exchanging digital images and data. The
FITS format has become the standard for storing and exchanging scientific data
in astronomy and other fields, and is used by many major observatories and
research institutions worldwide.
One of the key strengths of the FITS format is its
flexibility. The format is designed to support a wide range of data types and
data structures, including images, tables, and multi-dimensional arrays. This
flexibility allows the FITS format to handle a wide variety of scientific data,
from simple images to complex data sets. The format is also designed to be
efficient, with support for compression and data compression algorithms to
reduce file sizes and improve data transfer speeds.
Another strength of the FITS format is its ease of use. The
format is well-documented and has a large user base, making it easy for
researchers and developers to adopt and use. In addition, the FITS format has a
number of tools and libraries available for reading, writing, and manipulating
FITS files, which has contributed to its widespread adoption.
Despite these strengths, the FITS format is not without its
limitations. One potential drawback is that the format is not particularly
well-suited for handling large volumes of data. While the format can handle
large data sets, it may not be as efficient as other formats in terms of data
storage and transfer. In addition, the FITS format is not as widely supported
as other formats, such as JPEG or PNG, which may limit its use in some
applications.
Overall, FITS: A Flexible Image Transport System is a
valuable contribution to the field of astronomy and has had a significant
impact on the way scientific data is stored and exchanged. The FITS format is
widely used and has proven to be a flexible, efficient, and easy-to-use
solution for storing and exchanging digital images and data. While the format
has its limitations, it remains an important standard in the scientific
community and is likely to continue to be used for many years to come.
FITS (Flexible Image Transport System) is a file format
designed for storing and exchanging scientific and other images, as well as
data tables and other related information. The FITS format was developed by
D.C. Wells, E.W. Greisen, and R.H. Harten in 1981, and has since become a
widely-used standard in the field of astronomy and other scientific
disciplines.
One of the key features of the FITS format is its
flexibility. It is designed to support a wide range of data types, including 2D
and 3D images, data tables, and multi-dimensional arrays. FITS files can also
include metadata and other ancillary information, such as image calibration
data and information about the instruments used to collect the data.
One of the main advantages of the FITS format is its ability
to preserve the integrity of the original data. FITS files are self-contained
and include all the necessary information to accurately interpret and analyse
the data they contain. This makes FITS an ideal format for long-term data storage
and archiving.
Another strength of the FITS format is its wide adoption by
the scientific community. Many different software tools and libraries support
the FITS format, making it easy for researchers to work with FITS data and
share their results with others.
However, there are also some limitations to the FITS format.
One potential drawback is that FITS files can be quite large, especially for
images with high resolution or large data sets. This can be an issue for
researchers working with large data sets or limited storage space.
Additionally, the complexity of the FITS format can make it challenging for
non-experts to work with FITS data.
Overall, FITS is a widely used and well-respected file
format that has proven its value over time. Its ability to support a wide range
of data types, preserve the integrity of the original data, and be widely
adopted by the scientific community make it a valuable tool for researchers in
many fields.
The Flexible Image Transport System (FITS) file format,
introduced in the 1981 paper FITS: A Flexible Image Transport System by Wells,
Greisen, and Harten, has become a widely used standard for storing and
exchanging scientific data in astronomy and other fields. In this literature
review, we will explore the key features and capabilities of the FITS format,
as well as its strengths, limitations, and impact on the scientific community.
Another key feature of the FITS format is its support for
metadata, which allows for the inclusion of important information about the
data, such as the type of data, the units of measurement, and the observation
conditions. This metadata is essential for the proper interpretation and
analysis of the data, and the FITS format provides a standardized way to store
and exchange this information.
In terms of its strengths, the FITS format has proven to be
a reliable and effective solution for storing and exchanging scientific data.
The format is well-documented and has a large user base, making it easy for
researchers and developers to adopt and use. In addition, the FITS format has a
number of tools and libraries available for reading, writing, and manipulating
FITS files, which has contributed to its widespread adoption.
Despite these strengths, the FITS format is not without its
limitations. One potential drawback is that the format is not particularly
well-suited for handling large volumes of data. While the format can handle
large data sets, it may not be as efficient as other formats in terms of data
storage and transfer. In addition, the FITS format is not as widely supported
as other formats, such as JPEG or PNG, which may limit its use in some
applications.
Overall, the FITS format has had a
significant impact on the way scientific data is stored and exchanged. The
format is widely used in the scientific community and is likely to continue to
be used for many years to come. However, as technology and data storage needs
continue to evolve, it is possible that other formats may emerge that offer
greater efficiency and flexibility for handling scientific data.
An Extension of FITS for Groups of Small Arrays of Data
One of the key features of the BINTABLE extension is its
support for a wide range of data types, including integer, floating-point, and
string data. This allows the BINTABLE extension to handle a wide variety of
scientific data, including numerical data, text data, and data with mixed
types. The extension also allows for the inclusion of metadata, such as units
of measurement and data description, which is essential for the proper
interpretation and analysis of the data.
One strength of the BINTABLE extension is its ability to
handle small arrays of data efficiently. The extension is designed to store and
exchange data in a compact and efficient manner, which is particularly useful
for data sets with a large number of small arrays. This can reduce file sizes
and improve data transfer speeds, making the BINTABLE extension a useful tool
for handling scientific data.
Despite these strengths, the BINTABLE extension is not
without its limitations. One potential drawback is that the extension is not as
widely supported as the original FITS format, which may limit its use in some
applications. In addition, the BINTABLE extension is not as flexible as the
original FITS format in terms of data types and data structures, which may make
it less suitable for certain types of data.
Overall, An Extension of FITS for Groups of Small Arrays of
Data is a valuable contribution to the field of astronomy and has had a
significant impact on the way scientific data is stored and exchanged. The
BINTABLE extension has proven to be a useful tool for handling small arrays of
data efficiently, and it has become a widely used standard in the scientific
community. While the extension has its limitations, it remains an important
part of the FITS format and is likely to continue to be used for many years to
come.
An Extension of FITS for Groups of Small Arrays of Data,
written by Greisen and Harten in 1981, describes an extension to the Flexible
Image Transport System (FITS) file format that allows for the storage and
exchange of groups of small arrays of data. This extension, known as the Binary
Table Extension (BINTABLE), is designed to address the limitations of the
original FITS format in handling small arrays of data and is intended to
complement the capabilities of the original FITS format.
The BINTABLE extension has a number of strengths that make
it a useful tool for handling scientific data. One of the main strengths of the
extension is its ability to handle small arrays of data efficiently. The
extension is designed to store and exchange data in a compact and efficient
manner, which is particularly useful for data sets with a large number of small
arrays. This can reduce file sizes and improve data transfer speeds, making the
BINTABLE extension a useful tool for handling scientific data.
In addition to its efficiency, the BINTABLE extension is
also easy to use. The extension is well-documented and has a large user base,
making it easy for researchers and developers to adopt and use. The extension
is also supported by a number of tools and libraries, which makes it easy to
read, write, and manipulate BINTABLE data.
Despite these strengths, the BINTABLE extension is not
without its limitations. One potential drawback is that the extension is not as
widely supported as the original FITS format, which may limit its use in some
applications. In addition, the BINTABLE extension is not as flexible as the
original FITS format in terms of data types and data structures, which may make
it less suitable for certain types of data.
Generalized Extensions and Blocking Factors for FITS
Generalized Extensions and Blocking Factors for FITS,
written by Grosbøl, Harten, Greisen, and Wells in 1988, is a paper that
describes further developments to the Flexible Image Transport System (FITS)
file format. In this paper, the authors describe the addition of generalized
extensions and blocking factors to the FITS format, which are designed to
improve the efficiency and flexibility of the format.
One of the main features of the generalized extensions is
their ability to support a wide range of data types and data structures. These
extensions allow the FITS format to handle a wider variety of scientific data,
including images, tables, and multi-dimensional arrays. The generalized
extensions also allow for the inclusion of metadata, such as units of
measurement and data description, which is essential for the proper
interpretation and analysis of the data.
The blocking factors introduced in this paper are designed
to improve the efficiency of the FITS format by optimizing the way data is
stored and transferred. By dividing the data into blocks and adding padding to
the blocks, the blocking factors can improve the performance of the FITS format
in terms of data storage and transfer speeds.
One strength of the generalized extensions and blocking
factors is their ability to improve the efficiency and flexibility of the FITS
format. These improvements make the FITS format a more useful tool for handling
scientific data, particularly large data sets. The generalized extensions and
blocking factors also have a large user base and are supported by a number of
tools and libraries, which makes them easy to use and adopt.
Despite these strengths, the generalized extensions and
blocking factors are not without their limitations. One potential drawback is
that the extensions and factors may not be as widely supported as the original
FITS format, which may limit their use in some applications. In addition, the
generalized extensions and blocking factors may not be suitable for all types of
data, and may not provide significant improvements for certain types of data
sets.
Overall, Generalized Extensions and Blocking Factors for
FITS is a valuable contribution to the field of astronomy and has had a
significant impact on the way scientific data is stored and exchanged. The
generalized extensions and blocking factors have proven to be useful tools for
improving the efficiency and flexibility of the FITS format, and they have
become widely used standards in the scientific community. While the extensions
and factors have their limitations, they remain an important part of the FITS
format and are likely to continue to be used for many years to come.
One of the main features of the generalized extensions is
their ability to support a wide range of data types and data structures. These
extensions allow the FITS format to handle a wider variety of scientific data, including
images, tables, and multi-dimensional arrays. The generalized extensions also
allow for the inclusion of metadata, such as units of measurement and data
description, which is essential for the proper interpretation and analysis of
the data.
The blocking factors introduced in this paper are designed
to improve the efficiency of the FITS format by optimizing the way data is
stored and transferred. By dividing the data into blocks and adding padding to
the blocks, the blocking factors can improve the performance of the FITS format
in terms of data storage and transfer speeds.
The generalized extensions and blocking factors have a
number of strengths that make them useful tools for handling scientific data.
One of the main strengths of these developments is their ability to improve the
efficiency and flexibility of the FITS format. These improvements make the FITS
format a more useful tool for handling scientific data, particularly large data
sets. The generalized extensions and blocking factors also have a large user
base and are supported by a number of tools and libraries, which makes them
easy to use and adopt.
Despite these strengths, the generalized extensions and
blocking factors are not without their limitations. One potential drawback is
that the extensions and factors may not be as widely supported as the original
FITS format, which may limit their use in some applications. In addition, the
generalized extensions and blocking factors may not be suitable for all types
of data, and may not provide significant improvements for certain types of data
sets.
The FITS Tables Extension
The FITS Tables Extension, written by Harten, Grosbøl,
Greisen, and Wells in 1988, is a paper that describes further developments to
the Flexible Image Transport System (FITS) file format. In this paper, the
authors describe the FITS Tables Extension (TABLE), which is designed to
improve the handling and processing of tabular data in the FITS format.
One of the main features of the TABLE extension is its
support for a wide range of data types, including integer, floating-point, and
string data. This allows the TABLE extension to handle a wide variety of
scientific data, including numerical data, text data, and data with mixed
types. The extension also allows for the inclusion of metadata, such as units
of measurement and data description, which is essential for the proper
interpretation and analysis of the data.
One strength of the TABLE extension is its ability to handle
tabular data efficiently. The extension is designed to store and exchange data
in a compact and efficient manner, which is particularly useful for data sets
with a large number of small arrays. This can reduce file sizes and improve
data transfer speeds, making the TABLE extension a useful tool for handling
scientific data.
Another strength of the TABLE extension is its ease of use.
The extension is well-documented and has a large user base, making it easy for
researchers and developers to adopt and use. The extension is also supported by
a number of tools and libraries, which makes it easy to read, write, and
manipulate TABLE data.
Despite these strengths, the TABLE extension is not without
its limitations. One potential drawback is that the extension is not as widely
supported as the original FITS format, which may limit its use in some
applications. In addition, the TABLE extension may not be as flexible as other
file formats in terms of data types and data structures, which may make it less
suitable for certain types of data.
One of the main features of the
TABLE extension is its support for a wide range of data types, including
integer, floating-point, and string data. This allows the TABLE extension to
handle a wide variety of scientific data, including numerical data, text data,
and data with mixed types. The extension also allows for the inclusion of
metadata, such as units of measurement and data description, which is essential
for the proper interpretation and analysis of the data.
The TABLE extension has a number of strengths that make it a
useful tool for handling scientific data. One of the main strengths of the
extension is its ability to handle tabular data efficiently. The extension is
designed to store and exchange data in a compact and efficient manner, which is
particularly useful for data sets with a large number of small arrays. This can
reduce file sizes and improve data transfer speeds, making the TABLE extension
a useful tool for handling scientific data.
In addition to its efficiency, the TABLE extension is also
easy to use. The extension is well-documented and has a large user base, making
it easy for researchers and developers to adopt and use. The extension is also
supported by a number of tools and libraries, which makes it easy to read,
write, and manipulate TABLE data.
Despite these strengths, the TABLE extension is not without
its limitations. One potential drawback is that the extension is not as widely
supported as the original FITS format, which may limit its use in some
applications. In addition, the TABLE extension may not be as flexible as other
file formats in terms of data types and data structures, which may make it less
suitable for certain types of data.
Overall, the TABLE extension has had a significant impact on
the way scientific data is stored and exchanged. The extension is widely used
in the scientific community and is likely to continue to be used for many years
to come. However, as technology and data storage needs continue to evolve, it
is possible that other extensions or file formats.
The FITS Image Extension
The FITS Image Extension, written by Ponz, Thompson, and
Munoz in 1994, is a paper that describes further developments to the Flexible
Image Transport System (FITS) file format. In this paper, the authors describe
the FITS Image Extension (IMAGE), which is designed to improve the handling and
processing of image data in the FITS format.
One of the main features of the IMAGE extension is its
support for a wide range of data types, including integer, floating-point, and
string data. This allows the IMAGE extension to handle a wide variety of
scientific data, including numerical data, text data, and data with mixed
types. The extension also allows for the inclusion of metadata, such as units
of measurement and data description, which is essential for the proper
interpretation and analysis of the data.
One strength of the IMAGE extension is its ability to handle
image data efficiently. The extension is designed to store and exchange data in
a compact and efficient manner, which is particularly useful for large image
data sets. This can reduce file sizes and improve data transfer speeds, making
the IMAGE extension a useful tool for handling scientific data.
Another strength of the IMAGE extension is its ease of use.
The extension is well-documented and has a large user base, making it easy for
researchers and developers to adopt and use. The extension is also supported by
a number of tools and libraries, which makes it easy to read, write, and
manipulate IMAGE data.
Despite these strengths, the IMAGE extension is not without
its limitations. One potential drawback is that the extension is not as widely
supported as the original FITS format, which may limit its use in some
applications. In addition, the IMAGE extension may not be as flexible as other
file formats in terms of data types and data structures, which may make it less
suitable for certain types of data.
The FITS format was originally designed to store and
exchange images and has become a widely used standard in the field of
astronomy. However, the original FITS format had some limitations when it came
to handling certain types of image data, such as data with a large number of
pixels or data with multiple planes. The IMAGE extension was introduced to
address these limitations and improve the handling of image data in the FITS
format.
One of the main features of the
IMAGE extension is its support for a wide range of data types, including
integer, floating-point, and string data. This allows the IMAGE extension to
handle a wide variety of scientific data, including numerical data, text data,
and data with mixed types. The extension also allows for the inclusion of
metadata, such as units of measurement and data description, which is essential
for the proper interpretation and analysis of the data.
One strength of the IMAGE extension is its ability to handle
image data efficiently. The extension is designed to store and exchange data in
a compact and efficient manner, which is particularly useful for large image
data sets. This can reduce file sizes and improve data transfer speeds, making
the IMAGE extension a useful tool for handling scientific data.
In addition to its efficiency, the IMAGE extension is also
easy to use. The extension is well-documented and has a large user base, making
it easy for researchers and developers to adopt and use. The extension is also
supported by a number of tools and libraries, which makes it easy to read,
write, and manipulate IMAGE data.
Despite these strengths, the IMAGE extension is not without
its limitations. One potential drawback is that the extension is not as widely.
Binary Table Extension to FITS
Binary Table Extension to FITS, written by Cotton, Tody, and
Pence in 1995, is a paper that describes further developments to the Flexible
Image Transport System (FITS) file format. In this paper, the authors describe
the Binary Table Extension (BINTABLE), which is designed to improve the
handling and processing of tabular data in the FITS format.
One of the main features of the BINTABLE extension is its
support for a wide range of data types, including integer, floating-point, and
string data. This allows the BINTABLE extension to handle a wide variety of
scientific data, including numerical data, text data, and data with mixed
types. The extension also allows for the inclusion of metadata, such as units
of measurement and data description, which is essential for the proper
interpretation and analysis of the data.
One strength of the BINTABLE extension is its ability to
handle tabular data efficiently. The extension is designed to store and
exchange data in a compact and efficient manner, which is particularly useful
for data sets with a large number of small arrays. This can reduce file sizes
and improve data transfer speeds, making the BINTABLE extension a useful tool for
handling scientific data.
Another strength of the BINTABLE extension is its
flexibility. The extension allows for the use of variable-length arrays and the
inclusion of null values, which can be useful for handling data with missing or
incomplete values. The extension also allows for the use of multi-dimensional
arrays, which can be useful for handling data with more than two dimensions.
Despite these strengths, the BINTABLE extension is not
without its limitations. One potential drawback is that the extension is not as
widely supported as the original FITS format, which may limit its use in some
applications. In addition, the BINTABLE extension may not be as efficient as
other file formats in terms of data storage and transfer speeds, which may make
it less suitable for certain types of data sets.
Overall, Binary Table Extension to FITS is a valuable
contribution to the field of astronomy and has had a significant impact on the
way scientific data is stored and exchanged. The BINTABLE extension has proven
to be a useful tool for handling tabular data efficiently, and it has become a
widely used standard in the
In the paper "Binary Table Extension to FITS" by
Cotton, Tody, and Pence, published in the Astronomy & Astrophysics
Supplement Series in 1995, the authors describe the design and implementation
of the BINTABLE extension. They begin by outlining the need for a binary table
extension in the FITS format, citing the increasing use of computers in
astronomical data analysis and the need to store and access large amounts of
tabular data efficiently.
The authors then describe the structure of the BINTABLE
extension, which consists of a header containing metadata and a binary data
array. The header includes information about the table such as the number of
rows and columns, the data type of each column, and any units or scaling factors
associated with the data. The data array stores the actual data values in a
compact binary format, with each row of the table represented as a contiguous
block of memory.
The authors also discuss the use of variable-length arrays
in the BINTABLE extension, which allow for the storage of arrays of varying
lengths in a single column. This is useful for storing data such as spectra or
time series, which may have different lengths for different rows in the table.
In addition to describing the design and implementation of
the BINTABLE extension, the authors also present several examples of its use in
real-world astronomical data analysis. They demonstrate how the BINTABLE
extension can be used to efficiently store and access large amounts of tabular
data, and how it can be integrated with other software tools and programming
languages.
Definition of the Flexible Image Transport System (FITS
The authors begin by reviewing the history of the FITS
format, which was first introduced in the late 1970s as a way to store and
exchange images from the then-new field of CCD astronomy. They describe how the
format has evolved over the years to support a wider range of data types,
including images, spectra, and time series, as well as tabular data through the
Binary Table Extension (BINTABLE).
The authors then provide a detailed description of the
structure of the FITS format, which consists of a series of Header Data Units
(HDUs) containing a header and a data array. The header includes metadata about
the data, such as the data type, size, and any relevant units or scaling
factors. The data array stores the actual data values in a variety of formats
including integers, floating-point numbers, and characters.
One of the key features of the FITS format is its
flexibility, as it allows for the storage of a wide range of data types and
formats. The authors discuss the various data types and formats supported by
the FITS format and how they can be encoded in the data array. They also
describe how null values, which are used to represent missing or undefined
data, can be encoded in the data array.
The authors also discuss the use of extensions in the FITS
format, which allow for the storage of additional data types or formats beyond
the standard header and data array structure. They describe the various
extensions available, including the BINTABLE extension for storing tabular
data, and how they can be used in practice.
Overall, the "Definition of the Flexible Image
Transport System (FITS)" paper provides a comprehensive overview of the
FITS format and its capabilities. It is an important reference for anyone
working with FITS data and is widely cited in the literature.
However, it is worth noting that the FITS format has
continued to evolve since the publication of this paper, and newer versions of
the format have been developed to address limitations and add new features. As
such, it is important to be aware of the version of the FITS format being used
and to refer to the most up-to-date documentation for the most current
definition of the format.
The Flexible Image Transport System (FITS) is a standard
file format used in astronomy to store and exchange data. In the paper
"Definition of the Flexible Image Transport System (FITS)" by
Hanisch, Farris, Greisen, Pence, Schlesinger, Teuben, Thompson, and Warnock,
published in Astronomy & Astrophysics in 2001, the authors provide an
updated definition of the FITS format and describe its capabilities and
features.
The authors begin by reviewing the history of the FITS
format, which was first introduced in the late 1970s as a way to store and
exchange images from the then-new field of CCD astronomy. They describe how the
format has evolved over the years to support a wider range of data types,
including images, spectra, and time series, as well as tabular data through the
Binary Table Extension (BINTABLE).
The authors then provide a detailed description of the
structure of the FITS format, which consists of a series of Header Data Units
(HDUs) containing a header and a data array. The header includes metadata about
the data, such as the data type, size, and any relevant units or scaling
factors. The data array stores the actual data values in a variety of formats
including integers, floating-point numbers, and characters.
One of the key features of the FITS format is its
flexibility, as it allows for the storage of a wide range of data types and
formats. The authors discuss the various data types and formats supported by
the FITS format and how they can be encoded in the data array. They also
describe how null values, which are used to represent missing or undefined
data, can be encoded in the data array.
The authors conclude by discussing the advantages of the
FITS format, including its widespread use in the astronomical community, its
flexibility and ability to store a wide range of data types and formats, and
its support for data compression and data integrity checks.
Representations of World Coordinates in FITS
"Representations of World Coordinates in FITS" is
a paper written by E. W. Greisen and M. R. Calabretta and published in the
journal Astronomy & Astrophysics in 2002. The paper discusses the use of
the Flexible Image Transport System (FITS) to represent celestial coordinates
and other spatial information in astronomical images.
The paper begins with a brief overview of the FITS format,
which is a widely used standard for storing and exchanging scientific data,
particularly in the field of astronomy. The authors then go on to describe the
use of the World Coordinate System (WCS) in FITS, which is a set of conventions
for representing celestial coordinates and other spatial information in a
standardized way.
One of the main contributions of the paper is the
introduction of the concept of a "linear representation" of celestial
coordinates, which allows for more accurate representation of celestial coordinates
in FITS images. The authors demonstrate that this representation is more
accurate than previous methods, and discuss the implications of this for the
use of FITS in astronomy.
The paper also discusses the limitations of the WCS in FITS,
including the fact that it is limited to a particular set of coordinate systems
and cannot accurately represent all possible celestial coordinate systems. The
authors suggest ways in which the WCS could be improved in the future to
address these limitations.
Overall, "Representations of World Coordinates in
FITS" is a valuable contribution to the field of astronomy, providing a
detailed analysis of the use of the WCS in FITS and proposing ways in which the
system could be improved. The paper is well-written and clearly presents the
authors' ideas, making it accessible to a wide audience of astronomers and
other scientists.
In the paper, the authors begin by providing a brief
overview of the FITS format, which is a widely used standard for storing and
exchanging scientific data, particularly in the field of astronomy. They then
go on to describe the use of the World Coordinate System (WCS) in FITS, which
is a set of conventions for representing celestial coordinates and other
spatial information in a standardized way.
The paper also discusses the limitations of the WCS in FITS,
including the fact that it is limited to a particular set of coordinate systems
and cannot accurately represent all possible celestial coordinate systems. The
authors suggest ways in which the WCS could be improved in the future to
address these limitations.
Overall, "Representations of World Coordinates in
FITS" is a valuable contribution to the field of astronomy, providing a
detailed analysis of the use of the WCS in FITS and proposing ways in which the
system could be improved. The paper is well-written and clearly presents the
authors' ideas, making it accessible to a wide audience of astronomers and
other scientists.
Representations of Celestial Coordinates in FITS
"Representations of Celestial Coordinates in FITS"
is a paper published in the journal Astronomy & Astrophysics in 2002 that
discusses the representation of celestial coordinates in the Flexible Image
Transport System (FITS), a widely used standard for storing and exchanging
scientific data, particularly in the field of astronomy. The paper was written
by M. R. Calabretta and E. W. Greisen.
In the paper, the authors provide a detailed overview of the
World Coordinate System (WCS) in FITS, which is a set of conventions for
representing celestial coordinates and other spatial information in a
standardized way. They describe the various coordinate systems that can be used
in the WCS, and discuss the challenges and limitations of using these systems
to accurately represent celestial coordinates.
One of the main contributions of the paper is the
introduction of the concept of a "linear representation" of celestial
coordinates, which allows for more accurate representation of celestial
coordinates in FITS images. The authors demonstrate that this representation is
more accurate than previous methods, and discuss the implications of this for
the use of FITS in astronomy.
The paper also discusses the limitations of the WCS in FITS,
including the fact that it is limited to a particular set of coordinate systems
and cannot accurately represent all possible celestial coordinate systems. The
authors suggest ways in which the WCS could be improved in the future to
address these limitations.
Overall, "Representations of Celestial Coordinates in
FITS" is a comprehensive and detailed analysis of the use of the WCS in
FITS and its limitations. The paper is well-written and clearly presents the
authors' ideas, making it accessible to a wide audience of astronomers and other
scientists. The introduction of the linear representation of celestial
coordinates is a valuable contribution to the field, and the suggestions for
improving the WCS in the future are useful for researchers working in this
area.
In the paper, the authors provide a detailed overview of the
World Coordinate System (WCS) in FITS, which is a set of conventions for
representing celestial coordinates and other spatial information in a
standardized way. They describe the various coordinate systems that can be used
in the WCS, and discuss the challenges and limitations of using these systems
to accurately represent celestial coordinates.
The paper also discusses the limitations of the WCS in FITS,
including the fact that it is limited to a particular set of coordinate systems
and cannot accurately represent all possible celestial coordinate systems. The
authors suggest ways in which the WCS could be improved in the future to
address these limitations.
Overall, "Representations of Celestial Coordinates in
FITS" is a comprehensive and detailed analysis of the use of the WCS in
FITS and its limitations. The paper is well-written and clearly presents the
authors' ideas, making it accessible to a wide audience of astronomers and
other scientists. The introduction of the linear representation of celestial
coordinates is a valuable contribution to the field, and the suggestions for
improving the WCS in the future are useful for researchers working in this
area.
Representations of spectral coordinates in FITS
"Representations of spectral coordinates in FITS"
is a paper published in the journal Astronomy & Astrophysics in 2006 that
discusses the representation of spectral coordinates in the Flexible Image Transport
System (FITS), a widely used standard for storing and exchanging scientific
data, particularly in the field of astronomy. The paper was written by E. W.
Greisen, M. R. Calabretta, F. G. Valdes, and S. L. Allen.
In the paper, the authors provide a detailed overview of the
representation of spectral coordinates in FITS, including the various
coordinate systems that can be used and the challenges and limitations of using
these systems. They also introduce the concept of a "linear representation"
of spectral coordinates, which allows for more accurate representation of
spectral information in FITS images.
One of the main contributions of the paper is the
development of a new standard for the representation of spectral coordinates in
FITS, known as the Spectral Coordinate Representation (SCR). The authors
describe the SCR in detail and demonstrate its superiority to previous methods
for representing spectral coordinates in FITS. They also discuss the
implications of the SCR for the use of FITS in astronomy.
The paper also discusses the limitations of the SCR,
including the fact that it is limited to a particular set of coordinate systems
and cannot accurately represent all possible spectral coordinate systems. The
authors suggest ways in which the SCR could be improved in the future to
address these limitations.
Overall, "Representations of spectral coordinates in
FITS" is a comprehensive and detailed analysis of the representation of
spectral coordinates in FITS and the challenges and limitations of current
systems. The introduction of the SCR is a valuable contribution to the field,
and the suggestions for improving the system in the future are useful for
researchers working in this area. The paper is well-written and clearly
presents the authors' ideas, making it accessible to a wide audience of
astronomers and other scientists.
In the paper, the authors provide a detailed overview of the
representation of spectral coordinates in FITS, including the various
coordinate systems that can be used and the challenges and limitations of using
these systems. They also introduce the concept of a "linear
representation" of spectral coordinates, which allows for more accurate
representation of spectral information in FITS images.
The paper also discusses the limitations of the SCR,
including the fact that it is limited to a particular set of coordinate systems
and cannot accurately represent all possible spectral coordinate systems. The
authors suggest ways in which the SCR could be improved in the future to
address these limitations.
In terms of its
place within the broader literature on spectral coordinates and the use of
FITS, the paper builds upon earlier work on the representation of spectral
information in FITS and proposes a new standard for representing this
information. It also highlights the importance of standardized representation
of spectral coordinates in astronomical data, and the challenges and
limitations of current systems in this regard. As such, the paper is a valuable
resource for researchers and practitioners working in the field of astronomy
and related disciplines.
Representations of time coordinates in FITS. Time and relative dimension
in space.
"Representations of time coordinates in FITS" is a
paper published in the journal Astronomy & Astrophysics in 2015 that
discusses the representation of time coordinates in the Flexible Image
Transport System (FITS), a widely used standard for storing and exchanging
scientific data, particularly in the field of astronomy. The paper was written
by A. H. Rots, P. S. Bunclark, M. R. Calabretta, S. L. Allen, R. N. Manchester,
and W. T. Thompson.
In the paper, the authors provide a detailed overview of the
representation of time coordinates in FITS, including the various coordinate
systems that can be used and the challenges and limitations of using these
systems. They also introduce the concept of a "linear representation"
of time coordinates, which allows for more accurate representation of temporal
information in FITS images.
One of the main contributions of the paper is the
development of a new standard for the representation of time coordinates in
FITS, known as the Time Coordinate Representation (TCR). The authors describe
the TCR in detail and demonstrate its superiority to previous methods for
representing time coordinates in FITS. They also discuss the implications of
the TCR for the use of FITS in astronomy.
The paper also discusses the limitations of the TCR,
including the fact that it is limited to a particular set of coordinate systems
and cannot accurately represent all possible time coordinate systems. The
authors suggest ways in which the TCR could be improved in the future to
address these limitations.
Overall, "Representations of time coordinates in
FITS" is a comprehensive and detailed analysis of the representation of
time coordinates in FITS and the challenges and limitations of current systems.
The introduction of the TCR is a valuable contribution to the field, and the
suggestions for improving the system in the future are useful for researchers
working in this area. The paper is well-written and clearly presents the
authors' ideas, making it accessible to a wide audience of astronomers and
other scientists.
In the paper, the authors provide a detailed overview of the
representation of time coordinates in FITS, including the various coordinate
systems that can be used and the challenges and limitations of using these
systems. They also introduce the concept of a "linear representation"
of time coordinates, which allows for more accurate representation of temporal
information in FITS images.
The paper also discusses the limitations of the TCR,
including the fact that it is limited to a particular set of coordinate systems
and cannot accurately represent all possible time coordinate systems. The
authors suggest ways in which the TCR could be improved in the future to
address these limitations.
In terms of its
place within the broader literature on time coordinates and the use of FITS,
the paper builds upon earlier work on the representation of temporal
information in FITS and proposes a new standard for representing this
information. It also highlights the importance of standardized representation
of time coordinates in astronomical data, and the challenges and limitations of
current systems in this regard.
There have been
several developments and enhancements to the FITS (Flexible Image Transport
System) format since it was first introduced in 1981. Some of these include:
1.
Enhanced
data types: The FITS format has been expanded to support a wider range of data
types, including complex numbers, unsigned integers, and 64-bit integers.
2.
Improved
metadata support: FITS now supports more metadata fields and allows for the
inclusion of metadata in multiple languages.
3.
Better
compression: FITS now includes support for data compression, which can help
reduce the size of FITS files and make them easier to transmit and store.
4.
Extension
blocks: FITS now includes support for extension blocks, which allow for the
inclusion of additional data in a single file. This can be useful for storing
large data sets or multiple data types in a single file.
5.
Improved
error handling: FITS now includes improved error handling and error reporting
capabilities to help identify and resolve problems with FITS files.
6.
Better
support for large data sets: FITS now includes support for large data sets and
has been optimized for efficient storage and access to data.
7.
Improved
interoperability: FITS now includes support for improved interoperability with
other file formats, making it easier to exchange data with other scientific
applications and tools.
Overall, these
developments have helped to make the FITS format more flexible, efficient, and
easy to use for researchers in a wide range of scientific fields.
One of the key features of the FITS format
is its flexibility, as it is designed to support a wide range of data types and
includes support for metadata and other ancillary information. FITS files are
self-contained and include all the necessary information to accurately
interpret and analyze the data they contain, making them ideal for long-term
data storage and archiving.
Despite some limitations, such as the
potential for large file sizes and the complexity of the format, the FITS data
format has proven to be a valuable tool for researchers in many fields. Its
wide adoption by the scientific community, combined with the development of
tools and libraries to support the FITS format, make it a reliable and
effective way to store and exchange scientific data.
Flexible Image Transport System (FITS) is a file format for
storing and exchanging digital images and scientific data. It was developed by
Wells, Greisen, and Harten in 1981 as a solution to the limitations of existing
file formats in handling and processing scientific data. The FITS format is
designed to be flexible, supporting a wide range of data types and structures,
including images, tables, and multi-dimensional arrays. It is also designed to
be efficient, with support for compression and data compression algorithms to
reduce file sizes and improve data transfer speeds. The FITS format is
well-documented and easy to use, with a large user base and a range of tools
and libraries available for reading, writing, and manipulating FITS files.
However, it is not well-suited for handling large volumes of data and is not as
widely supported as other formats such as JPEG or PNG. Despite these
limitations, the FITS format has become a widely-used standard in the
scientific community and is likely to continue to be used for many years to
come.
Flexible Image Transport System (FITS) is a file format for
storing and exchanging digital images and scientific data. It was developed by
D.C. Wells, E.W. Greisen, and R.H. Harten in 1981 as a solution to the
limitations of existing file formats in handling and processing scientific
data. The authors wrote at a time when the problem of large-scale arrays in
astronomy data was just starting to be considered, and the then available
technologies were largely proprietary and disparate.
The main goal of the FITS format was to provide a way to
store and exchange digital images and data that was flexible, efficient, and
easy to use. To achieve this, the FITS format was designed to support a wide
range of data types and data structures, including images, tables, and
multi-dimensional arrays. This flexibility allows the FITS format to handle a
wide variety of scientific data, from simple images to complex data sets. The
format is also designed to be efficient, with support for compression and data
compression algorithms to reduce file sizes and improve data transfer speeds.
In addition to its flexibility and efficiency, the FITS
format is also easy to use. It is well-documented and has a large user base,
making it easy for researchers and developers to adopt and use. There are also
a number of tools and libraries available for reading, writing, and
manipulating FITS files, which has contributed to its widespread adoption.
Despite its strengths, the FITS format is not without its
limitations. One potential drawback is that it is not particularly well-suited
for handling large volumes of data. While the format can handle large data
sets, it may not be as efficient as other formats in terms of data storage and
transfer. In addition, the FITS format is not as widely supported as other
formats such as JPEG or PNG, which may limit its use in some applications.
Overall, FITS: A Flexible Image Transport System is a
valuable contribution to the field of astronomy and has had a significant
impact on the way scientific data is stored and exchanged. The FITS format is
widely used and has proven to be a flexible, efficient, and easy-to-use
solution for storing and exchanging digital images and data. While the format
has its limitations, it remains an important standard in the scientific
community and is likely to continue to be used for many years to come.
FITS Documentation
https://fits.gsfc.nasa.gov/fits_documentation.html
QFitsView
https://www.mpe.mpg.de/~ott/dpuser/qfitsview.html
FITS++: An Object-Oriented Set of C++
Classes to Support FITS
https://www.adass.org/adass/proceedings/adass96/farrisa.html
How to read and process .fits files
https://stackoverflow.com/questions/24970946/how-to-read-and-process-fits-files
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