International Celestial Reference System (ICRS)
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The International Celestial Reference System (ICRS) is the fundamental celestial reference system adopted by the International Astronomical Union (IAU) for high-precision positional astronomy. The ICRS, with its origin at the solar system barycenter and "space fixed" axis directions, is meant to represent the most appropriate coordinate system for expressing reference data on the positions and motions of celestial objects.

Background

stars with grid

The ICRS was established by a set of specifications agreed to by the international astronomical community from 1997 to 2006. The origin of the ICRS is at the barycenter of the solar system and the orientation of its axes is "space fixed" (kinematically non-rotating) with respect to distant objects in the universe. Other specifications include a metric tensor, a prescription for establishing and maintaining the axis directions, a list of benchmark objects with precise coordinates for each one, and standard models and algorithms that allow these coordinates to be transformed into observable quantities for any location and time.

In this context it is helpful to distinguish between a reference system and a reference frame as used in astronomy. A reference system is the complete specification of how a celestial coordinate system is to be formed. It defines the origin and fundamental planes (or axes) of the coordinate system. It also specifies all of the constants, models, and algorithms used to transform between observable quantities and reference data that conform to the system. A reference frame consists of a set of identifiable fiducial points on the sky (specific astronomical objects), along with their coordinates, that serves as the practical realization of a reference system.

For example, the fundamental plane of an astronomical reference system has conventionally been the extension of the Earth's equatorial plane, at some date, to infinity. The declination of a star or other object is its angular distance north or south of this plane. The right ascension of an object is its angular distance measured eastward along the equator from some defined reference point where the right ascension value is set to zero. This reference point, the origin of right ascension, has traditionally been the equinox: the point at which the Sun, in its yearly circuit of the celestial sphere, crosses the equatorial plane moving from south to north. The Sun's apparent yearly motion lies in the ecliptic, the plane of the Earth's orbit. The equinox, therefore, is a direction in space along the nodal line defined by the intersection of the ecliptic and equatorial planes; equivalently, on the celestial sphere, the equinox is at one of the two intersections of the great circles representing these planes. Because both of these planes are moving, the coordinate systems that they define must have a date associated with them; such a reference system must be therefore specified as "the equator and equinox of [some date]".

Of course, such a reference system is an idealization, because the theories of motion of the Earth that define how the two planes move are imperfect. In fact, the very definitions of these planes are problematic for high-precision work. Even if the fundamental planes are defined without any reference to the motions of the Earth, there is no way to magically paint them on the celestial sphere at any particular time. Therefore, in practice, we use a specific reference frame—a set of fiducial objects with assigned coordinates—as the practical representation of an astronomical reference system. The scheme is completely analogous to how terrestrial reference systems are established using survey control stations (geodetic reference points) on the Earth's surface.

equatorial system

Most commonly, a reference frame consists of a catalog of precise positions (and motions, if measurable) of stars or extragalactic objects as seen from the solar system barycenter at a specific epoch (now usually "J2000.0", which is 12h TT on 1 January 2000). Each object's instantaneous position, expressed as right ascension and declination, indicates the object's angular distance from the catalog's equator and origin of right ascension. (A catalog's right ascension origin was formerly referred to as the catalog equinox, a now-obsolete term.) Any two such objects in the catalog therefore uniquely orient a spherical coordinate system on the sky—a reference frame.

A modern astrometric catalog contains data on a large number of objects (N), so the coordinate system is vastly overdetermined. The quality of the reference frame defined by a catalog depends on the extent to which the coordinates of all possible pairs of objects (approx. N2/2) serve to define the identical equator and right ascension origin, within the expected random errors. Typically, every catalog contains systematic errors, that is, errors in position that are similar in direction and magnitude for objects that are in the same area of the sky, or are of the same magnitude (flux) or color (spectral index). Systematic errors mean that the reference frame is warped, or is effectively different for different classes of objects. Obviously, minimizing systematic errors when a catalog is constructed is as important (if not more so) than minimizing the random errors.

To be useful, a reference frame must be implemented at the time of actual observations, and this requires the computation of the geocentric coordinates of the catalog objects at arbitrary dates and times. The accuracy with which we know the motions of the objects (unless they are assumed zero) is an essential factor in this computation. Astrometric star catalogs list proper motions, which are the projection of each star's space motion onto the celestial sphere, expressed as an angular rate in right ascension and declination per unit time. Because the tabulated proper motions are never perfect (even if assumed zero), any celestial reference frame deteriorates with time. Moreover, systematic errors in the proper motions can produce time-dependent warpings and spurious rotations in the frame. Therefore, the accuracy and consistency of the proper motions are critical to the overall quality, utility, and longevity of reference frames defined by stars.

The positions of solar system objects can also be used to define a reference frame. For each solar system body involved, an ephemeris (pl. ephemerides) is used, which is simply a table or file of the celestial coordinates of the body as a function of time (or an algorithm that yields such a table). A reference frame defined by the ephemerides of one or more solar system bodies is called a dynamical reference frame. Because the ephemerides used incorporate the theories of motion of the Earth as well as that of the other solar system bodies, dynamical reference frames embody in a very fundamental way the moving equator and ecliptic, hence the equinox. They have, therefore, been used to align star catalog reference frames properly (the star positions were systematically adjusted) on the basis of simultaneous observations of stars and planets. However, dynamical reference frames are not very practical for establishing a coordinate system for day-to-day astronomical observations. The ICRS does not involve a dynamical reference frame.

Descriptions of reference frames and reference systems often refer to three coordinate axes, which are simply the set of right-handed Cartesian axes that correspond to the usual celestial spherical coordinate system. The xy-plane is the equator, the z-axis points toward the north celestial pole, and the x-axis points toward the origin of right ascension. Although in principle this allows us to specify the position of any celestial object in rectangular coordinates, the distance scale is not established to high precision beyond the solar system. What an astronomical reference system actually defines is the way in which the two conventional astronomical angular coordinates, right ascension and declination, overlay real observable points in the sky.

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Late 20th Century Developments

The establishment of celestial reference systems is coordinated by the International Astronomical Union (IAU). The previous astronomical reference system was based on the equator and equinox of J2000.0 determined from observations of planetary motions, together with the IAU (1976) System of Astronomical Constants and related algorithms (Kaplan 1982). The reference frame that embodied this system for practical purposes was the Fifth Fundamental Catalogue (FK5) (Fricke, et al. 1988). The FK5 is a catalog of 1535 bright stars (to magnitude 7.5), supplemented by a fainter extension of 3117 additional stars (to magnitude 9.5). The FK5 was the successor to the FK3 and FK4 catalogs, all compiled from catalogs of meridian observations taken in the visual band (many such observations were, in fact, taken by eye). The formal uncertainties in the star positions of the FK5 at the time of its publication in 1988 were about 30-40 milliarcseconds over most of the sky, but the errors are considerably worse when systematic trends are taken into account.

Beginning in the 1970s, the most precise wide-angle (all-sky) astrometry was conducted not in the optical regime but at radio wavelengths, involving the techniques of Very Long Baseline Interferometry (VLBI) and pulsar timing. Uncertainties of radio VLBI antenna source positions listed in all-sky VLBI catalogs are now typically less than one milliarcsecond (5 × 10–9 radian), and often a factor of ten better. Furthermore, because these radio sources are very distant extragalactic objects (mostly quasars) that are not expected to show measurable intrinsic motion, a reference frame defined by VLBI positions should be "more inertial" (less subject to spurious rotation) than a reference frame defined by galactic objects, such as stars or pulsars. The VLBI catalogs do have the disadvantage that their origin of right ascension is somewhat arbitrary; there is no real equinox in VLBI catalogs, since VLBI has little sensitivity to the ecliptic plane. The VLBI origin of right ascension has effectively been carried over from one catalog to the next; it was originally based on the right ascension of the radio source 3C 273B measured using lunar occultations.

Because of the accuracy and stability of radio reference frames, since the mid 1980s, astronomical measurements of the Earth's rotation—from which astronomical time is determined—have depended heavily on VLBI, with classical methods based on star transits phased out. Hence the situation evolved to where the definition of the fundamental astronomical reference frame (the FK5) became irrelevant to some of the most precise and important astrometric measurements. VLBI revealed, in addition, that the models of the Earth's precession and nutation that were part of the old system were inadequate for modern astrometric precision. In particular, the "constant of precession"—a measurement of the long-term rate of change of the orientation of the Earth's axis in space—had been overestimated by about 0.3 arcseconds per century. Moreover, the success of the European Space Agency Hipparcos astrometric satellite, launched in 1989, promised to provide a new, very accurate set of star coordinates in the optical regime.

Thus, beginning in 1988, a number of IAU working groups began considering the requirements for a new fundamental astronomical reference system (Lieske & Abalakin 1990, Hughes et al. 1991). The resulting series of IAU resolutions, passed in 1991, 1994, 1997, and 2000 (IAU 1992, 1996, 1999, 2001), effectively form the specifications for the ICRS. The axes of the ICRS are defined by the adopted positions of a specific set of extragalactic objects, which are assumed to have no measurable proper motions. The ICRS axes are consistent, to better than 0.1 arcsecond, with the equator and equinox of J2000.0 defined by the dynamics of the Earth. However, the ICRS axes are meant to be regarded as fixed directions in space that have an existence independent of the dynamics of the Earth or the particular set of objects used to define them at any given time.

The promotion, maintenance, extension, and use of the ICRS are the responsibilities of IAU Division A (Fundamental Astronomy), especially Commission A1 (Astrometry) and Commission A2 (Rotation of the Earth). The International Earth Rotation and Reference System Service (IERS), which was established by the IAU and International Union of Geodesy and Geophysics (IUGG), is also involved. The IERS generates VLBI-based science products for astrometry and geodesy, and the IAU entities provide a framework within the astronomical community for international collaboration, overall guidance for the work, and evaluation and endorsement of results.

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ICRS Implementation

The Defining Extragalactic Frame

Galaxies with Grid

The International Celestial Reference Frame (ICRF or ICRF1) is a catalog of adopted positions of 608 extragalactic radio sources observed with VLBI, all strong (greater than 0.1 Jy) at S and X bands (wavelengths 13 and 3.6 cm) (Ma & Feissel 1997). Most have faint optical counterparts (typically with visual magnitudes fainter than 18) and the majority are quasars. Of these objects, 212 are defining sources that establish the orientation of the ICRS axes, with origin at the solar system barycenter. Typical position uncertainties for the defining sources are of order 0.5 milliarcsecond; the orientation of the axes is defined from the ensemble to an accuracy of about 0.02 milliarcseconds. As described below, these axes correspond closely to what would conventionally be described as "the equator and equinox of J2000.0".

The International Earth Rotation Service (IERS) monitors the radio sources involved in the ICRF. This monitoring is necessary because, at some level, most of the sources are variable in both flux and structure, and the centers of emission can display spurious motions, which may not be linear on the sky or constant in rate; see the discussion in Ma et al. (1998), Section 8.

By 2006, it was recognized that a major update of the ICRF was needed to maintain the accuracy and fixed orientation of the overall frame, and an IAU working group was established to update the list of sources and coordinates. The working group presented a revised and extended list of sources and coordinates. The new list was adopted by the IAU in 2009 as the Second Realization of the International Celestial Reference Frame (ICRF2) (Ma et al. 2009), superseding the original in defining the spatial orientation of the ICRS at S and X bands. The ICRF2 has 295 defining sources, chosen from a solution for the positions of 3414 sources. Only 97 of the defining sources are also defining sources in ICRF1, reflecting the results of the ongoing analysis of source stability and the working group's goal of mitigating source position variations. The positional uncertainties have been reduced considerably and the new list is more evenly distributed across the sky, especially in the south. Typical ICRF2 defining source position errors, all things considered, are approximately 0.1 milliarcseconds. The overall orientation of the axes is estimated to be stable within 0.010 milliarcseconds and is consistent with that of ICRF1.

A third version of the ICRF, the ICRF3, is in preparation for proposed adoption by the IAU at its General Assembly in 2018 (Malkin et al. 2014). The ICRF3 will have better coverage of sources in the sky's southern hemisphere than the previous versions. The anticipated accuracy for all the sources is in the range 70-100 microarcseconds.

The Frame at Optical Wavelengths

The ICRS is currently realized at optical wavelengths by stars in the Hipparcos Catalogue of 118,218 stars, some as faint as visual magnitude 12 (ESA 1997). Only stars with uncomplicated and well-determined proper motions (e.g., no known binaries) are used for the ICRS realization. This subset, referred to as the Hipparcos Celestial Reference Frame (HCRF), comprises 85% of the stars in the Hipparcos catalog. Hipparcos star coordinates and proper motions are given within the ICRS coordinate system but are listed for epoch J1991.25. (That is, the catalog effectively represents a snapshot of the motion of the stars through space taken on 2 April 1991.) At the catalog epoch, Hipparcos uncertainties for stars brighter than 9th magnitude have median values somewhat better than 1 milliarcsecond in position and 1 milliarcsecond/year in proper motion (ESA 1997, Mignard 1997). The overall alignment to the ICRF at that epoch is estimated to be within 0.6 milliarcsecond, with any spurious rotations or distortions less than 0.25 milliarcsecond/year. Projected to epoch 2015, typical position errors for the brighter Hipparcos stars are approximately 25 milliarcseconds.

A major reanalysis of the original Hipparcos observations (van Leeuen 2007a, 2007b) resulted in a new Hipparcos catalog with substantially improved astrometric data. However, the IAU never took any action that officially replaced the original Hipparcos catalog as the basis for the HCRF.

Launched at the end of 2013, the European Space Agency Gaia mission is now taking astrometric observations, and the results will replace the Hipparcos data as the most accurate representation of the ICRS in the optical wavelengths. The spacecraft is in orbit at the L2 point, 1.5 million kilometers from Earth. A series of data releases started in September 2016. Gaia data will eventually be complete for 1 billion stars, down to magnitude 20, and for stars brighter than magnitude 15, the estimated final accuracies are expected to be better than 25 microarcseconds in position and parallax and 15 microarcseconds/year in proper motion. This is an unprecedented leap in astrometric accuracy over all previous observing programs.

Other representations of the ICRS are described in the section below titled Data in the ICRS.

Standard Algorithms

At its General Assembly in 2000, the IAU defined a system of space-time coordinates for (1) the solar system, and (2) the Earth, within the framework of General Relativity, by specifying the form of the metric tensors for each and the 4-dimensional space-time transformation between them (IAU 2001). The former is called the Barycentric Celestial Reference System (BCRS), and the latter, the Geocentric Celestial Reference System (GCRS). Since the IAU definitions of the BCRS and GCRS concern only relativity, they can be thought of as defining two families of reference systems; the 2000 resolutions did not specify an absolute orientation for either (although their relative orientation is described by the transformation between them). To remedy the situation, in 2006, the IAU passed a resolution (IAU 2008) that specified that the ICRS defines the orientation of the BCRS. Thus, the ICRS and BCRS are closely linked and the two terms are often used interchangeably. A simple way of understanding the connection is that BCRS coordinates are expressed with respect to the ICRS spatial axes and ICRS data are based on the BCRS metric.

Also in 2000 and 2006, the IAU adopted new models for the computation of the Earth's instantaneous orientation within the ICRS. The new models include new algorithms for precession and nutation, a new definition of the celestial pole, and two new reference points in the equatorial plane for measuring the rotational angle of the Earth around its instantaneous axis. These models are described in detail in the IERS Conventions (2010) (Petit & Luzum 2010), in USNO Circular 179 (Kaplan 2005), and in the 2012 edition of the Explanatory Supplement to the Astronomical Almanac (Urban & Seidelmann 2012). These models are important when the instantaneous coordinates of celestial objects are to be expressed with respect to the equator and equinox of date, or with respect to a local horizon-based system.

A collection of computer modules in Fortran and C that implement these IAU-recommended algorithms for Earth orientation is the Standards of Fundamental Astronomy (SOFA) library. The collection is managed by an international panel, the SOFA Reviewing Board, which works under the auspices of IAU Division A (Fundamental Astronomy). The board solicits code from the astrometric and geodetic community that implements the IAU models. Subroutines/functions are adapted to established coding standards and validated for accuracy before being added to the SOFA collection. The latest version of the U.S. Naval Observatory Vector Astrometry Software (NOVAS), available in Fortran, C, and Python, also implements the IAU models.

The new Earth orientation models are, of course, relevant only to fundamental observations made from the surface of the Earth. Astrometric observations taken from space platforms, or those that are differential in nature (based on reference objects that are all within a small field), are not affected by these models. However, there are other effects that must be taken into account in analyzing astrometric observations—e.g., proper motion, parallax, aberration, and gravitational light-bending—and algorithms for these may be found in Volumes 1 and 3 of the Hipparcos Catalogue documentation ESA (1997) and in the 2012 edition of the Explanatory Supplement to the Astronomical Almanac (Urban & Seidelmann 2012). For analysis of very high accuracy observations from space, see the development by Klioner (2003).

Finally, IAU-recommended models for the rotation of the planets, satellites, and asteroids, compiled by the IAU Working Group on Cartographic Coordinates and Rotational Elements, are given with respect to the ICRS (Archinal, et al. 2011).

Relationship to Other Systems

The orientation of the ICRS axes is consistent with the equator and equinox of J2000.0 represented by the FK5, within the errors of the latter. Since, at J2000.0, the errors of the FK5 are significantly worse than those of Hipparcos, the ICRS can be considered to be a refinement of the FK5 system at (or near) that epoch.

The ICRS can also be considered to be a good approximation (at least as good as the FK5) to the conventionally defined dynamical equator and equinox of J2000.0 (Feissel & Mignard 1998). In fact, the equator is well determined fundamentally from the VLBI observations that are the basis for the entire ICRS, and the ICRS pole is within 20 milliarcseconds of the dynamical pole. As previously mentioned, the zero point of VLBI-derived right ascensions is arbitrary, but traditionally has been set by assigning to the right ascension of source 3C 273B a value derived from lunar occultation timings—the Moon's ephemeris thus providing an indirect link to the dynamical equinox. The ICRS origin of right ascension was made to be consistent with that in a group of VLBI catalogs previously used by the IERS, aligned in this way. The difference between the ICRS origin of right ascension and the dynamical equinox has been independently measured by two groups that used different definitions of the equinox, but in both cases the difference found was less than 0.1 arcsecond.

Because of its consistency with previous reference systems, use of the ICRS would be transparent to any applications with accuracy requirements that are not more stringent than about 0.1 arcseconds. That is, for applications of this accuracy—which is good enough, for example, for telescope pointing—the distinctions between the ICRS, FK5, and dynamical equator and equinox of J2000.0 are not significant. However, as mentioned above, implementation of the latest IAU Earth orientation models (precession and nutation) is needed to express most accurately (and to avoid systematic errors in) the apparent positions of celestial objects with respect to the equator and equinox of date, regardless of which catalog or ephemeris is used for the source data.*

For a concise review of the ICRS adoption and its implications, see the paper by Feissel & Mignard (1998).


* FK5 data should not be used for current applications. The FK5 proper motions are based on the previous value for the rate of precession, and their use may cause a very small spurious rotation in the coordinate system defined by the computed star positions.

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Data in the ICRS

quasar

Although the ICRF2 and HCRF are currently its basic radio and optical realizations, the ICRS has been extended to fainter magnitudes and other wavelengths. An ever-increasing amount of fundamental astronomical data is being brought within the system. Some examples (not a complete list) are:

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Authorizing IAU Resolutions

The construction and implementation of the ICRS was authorized and supported by the IAU. Resolution B2, passed by the 23rd General Assembly of the IAU in August 1997 (IAU 1999), states that

The "1991 IAU Resolution on reference frames" referred to above was Resolution A4 passed by the 21st IAU General Assembly (IAU 1992). It recommended that "the space coordinate grids with origins at the solar system barycentre and at the centre of mass of the Earth show no global rotation with respect to a set of distant extragalactic objects" and that "the principal plane of the new conventional reference system be as near as possible to the mean equator of J2000.0 and that the origin in this principal plane be as near as possible to the dynamical equinox of J2000.0." It also recommended that an IAU working group establish a list of extragalactic radio sources that would be "candidates for primary sources defining the new conventional reference frame." Thus, the ICRS as established in 1997 was based on specifications defined by the IAU in 1991.

At the subsequent IAU General Assembly in 2000, Resolution B1.2 (IAU 2001) restricted the number of Hipparcos stars that would be considered part of the optical realization of the ICRS. The relevant part of this resolution states that

Effectively, this change eliminated about 15% of the stars in the Hipparcos catalog, leaving those with well determined linear proper motions. The flags referred to are given in Hipparcos data field H59.

Resolutions B1.3. B1.4, B1.5 of the 2000 General Assembly defined the Barycentric Celestial Reference System (BCRS), the Geocentric Celestial Reference System (GCRS), the transformation between them, and the time scales appropriate for each system. Resolutions B1.6, B1.7, and B1.8 of the same General Assembly defined the IAU 2000A precession-nutation model, the celestial pole, points on the celestial and terrestrial equators from which the rotational angle of the Earth is measured, and the expression for the Earth rotation angle as a function of Universal Time (UT1).

At the IAU General Assembly in 2006, Resolution 2 (IAU 2008) completed the definition of the Barycentric Celestial Reference System (BCRS) with the words

For all practical applications, unless otherwise stated, the BCRS is assumed to be oriented according to the ICRS axes.

So the fundamental celestial reference system is actually defined by both the BCRS (relativistic metric) and ICRS (orientation).

Texts of all IAU resolutions, listed by year of the General Assembly at which they were adopted, can be found at the IAU web site. Extended explanations of the resolutions mentioned here, as well as formulas for their practical implementation, can be found in USNO Circular 179 (Kaplan 2005).

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