The fundamental definition of "radial velocity'' Lindegren, Lennart; Dravins, Dainis Published in: Astronomy & Astrophysics DOI: 10.1051/0004-6361:20030181 2003 Link to publication Citation for published version (APA): Lindegren, L., & Dravins, D. (2003). The fundamental definition of "radial velocity''. Astronomy & Astrophysics, 401(3), 1185-1201. https://doi.org/10.1051/0004-6361:20030181 Total number of authors: 2 General rights Unless other specific re-use rights are stated the following general rights apply: Copyright and moral rights for the publications made accessible in the public portal are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. • Users may download and print one copy of any publication from the public portal for the purpose of private study or research. • You may not further distribute the material or use it for any profit-making activity or commercial gain • You may freely distribute the URL identifying the publication in the public portal Read more about Creative commons licenses: https://creativecommons.org/licenses/ Take down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. LUND UNIVERSITY PO Box 117 221 00 Lund +46 46-222 00 00 A&A 401, 1185–1201 (2003) Astronomy DOI: 10.1051/0004-6361:20030181 & c ESO 2003 Astrophysics The fundamental definition of “radial velocity” Lennart Lindegren and Dainis Dravins Lund Observatory, Box 43, 22100 Lund, Sweden e-mail: [email protected]; [email protected] Received 4 September 2002 / Accepted 31 January 2003 Abstract. Accuracy levels of metres per second require the fundamental concept of “radial velocity” for stars and other distant objects to be examined, both as a physical velocity, and as measured by spectroscopic and astrometric techniques. Already in a classical (non-relativistic) framework the line-of-sight velocity component is an ambiguous concept, depending on whether, e.g., the time of light emission (at the object) or that of light detection (by the observer) is used for recording the time coordi- nate. Relativistic velocity effects and spectroscopic measurements made inside gravitational fields add further complications, causing wavelength shifts to depend, e.g., on the transverse velocity of the object and the gravitational potential at the source. 1 Aiming at definitions that are unambiguous at accuracy levels of 1 m s− , we analyse different concepts of radial velocity and their interrelations. At this accuracy level, a strict separation must be made between the purely geometric concepts on one hand, and the spectroscopic measurement on the other. Among the geometric concepts we define kinematic radial velocity,which corresponds most closely to the “textbook definition” of radial velocity as the line-of-sight component of space velocity; and astrometric radial velocity, which can be derived from astrometric observations. Consistent with these definitions, we propose strict definitions also of the complementary kinematic and astrometric quantities, namely transverse velocity and proper mo- tion. The kinematic and astrometric radial velocities depend on the chosen spacetime metric, and are accurately related by simple coordinate transformations. On the other hand, the observational quantity that should result from accurate spectroscopic measurements is the barycentric radial-velocity measure. This is independent of the metric, and to first order equals the line-of- sight velocity. However, it is not a physical velocity, and cannot be accurately transformed to a kinematic or astrometric radial velocity without additional assumptions and data in modelling the process of light emission from the source, the transmission of the signal through space, and its recording by the observer. For historic and practical reasons, the spectroscopic radial-velocity measure is expressed in velocity units as czB,wherec is the speed of light and zB is the observed relative wavelength shift reduced to the solar-system barycentre, at an epoch equal to the barycentric time of light arrival. The barycentric radial-velocity measure and the astrometric radial velocity are defined by recent resolutions adopted by the International Astronomical Union (IAU), the motives and consequences of which are explained in this paper. Key words. techniques: radial velocities – techniques: spectroscopic – astrometry – reference systems – stars: kinematics – methods: data analysis 1. The need for stringent definitions their background, the need for such definitions, and to elabo- rate on their consequences for future work. Thus, the paper is Radial velocity is an omnipresent concept in astronomy, and not about the detailed interpretation of observed spectral-line a quantity whose precision of determination has improved displacements in terms of radial motion, nor about the actual significantly in recent years. Its meaning is generally under- techniques for making such measurements; rather, it is the def- stood as the object’s motion along the line of sight, a quantity inition of “radial velocity” itself, as a geometric and spectro- normally deduced from observed spectral-line displacements, scopic concept, that is discussed. interpreted as Doppler shifts. However, despite its ubiquity, The need for a strict definition has become urgent in re- there has not existed any physically stringent definition of “ra- cent years as a consequence of important developments in the dial velocity” with an accuracy to match currently attainable techniques for measuring stellar radial velocities, as well as the measuring precisions. Two first such definitions – one for the improved understanding of the many effects that complicate result of spectroscopic observations, and one for the geomet- their interpretation. We note in particular the following circum- ric (astrometric) concept of radial velocity – were adopted at stances: the General Assembly of the International Astronomical Union (IAU), held in 2000. The purpose of this paper is to explain Precision and accuracy of spectroscopic measurements: spectroscopic measurement precisions are now reaching (and Send offprint requests to: L. Lindegren, surpassing) levels of metres per second. In some applications, e-mail: [email protected] such as the search for (short-period) extrasolar planets or stellar 1186 Lennart Lindegren and Dainis Dravins: The fundamental definition of “radial velocity” oscillations, it may be sufficient to obtain differential measure- The role of standard stars: practical radial-velocity mea- ments of wavelength shifts, in which case internal precision is surements have traditionally relied on the use of standard stars adequate and there is no need for an accurate definition of the to define the zero point of the velocity scale. While these have 1 zero point. However, other applications might require the com- aimed at accuracies of the order 100 m s− , it has in reality bination of data from different observatories, recorded over ex- been difficult to achieve consistency even at this level due to tended periods of time, and thus the use of a common reference poorly understood systematic differences depending on spec- point. Examples could be the study of long-term variations due tral type, stellar rotation, instrumental resolution, correlation to stellar activity cycles and searches for long-period stellar masks used, and so on. Standard stars will probably continue to companions. Such applications call for data that are not only play a role as a practical way of eliminating, to first order, such precise, but also accurate, i.e., referring to some “absolute” differences in radial-velocity surveys aiming at moderate ac- scale of measurements. However, the transfer of high-precision curacy. However, their relation to high-accuracy measurements measurements to absolute values was previously not possible, needs to be clearly defined. partly because there has been no agreement on how to make Gravitational redshifts: the gravitational potential at the such a transfer, or even on which physical quantity to transfer. stellar surface causes all escaping photons to be redshifted by an amount that varies from 30 m s 1 for supergiants, In the past, a classical accuracy achieved for measuring ∼ − 1 30 km s 1 for white dwarfs, and much greater values for neu- stellar radial velocities has been perhaps 1 km s− ,atwhich ∼ − level most of these issues did not arise, or could be solved tron stars and other compact objects. Even for a given star, the by the simple use of “standard stars”. With current methods precise shift varies depending on the height at which the spec- and instrumentation, the accuracy by which measured stel- tral lines are formed. The observed shift also depends on the lar wavelengths can be related to absolute numbers is largely gravitational potential at the observer, and therefore on the ob- set by the laboratory sources used for spectrometer calibra- server’s distance from the Sun. tion (lines from iodine cells, lasers, etc.). An accuracy level Astrometric determination of radial motion: current and 1 expected advances in astrometry enable the accurate deter- of about 10 m s− now seems reachable. Since any fundamen- tal definition should be at least some order of magnitude better mination of stellar radial motions without using spectroscopy than current performance, the accuracy goal for the definition