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A&A
Volume 509, January 2010
Article Number A37
Number of page(s) 8
Section Celestial mechanics and astrometry
DOI https://doi.org/10.1051/0004-6361/200912691
Published online 14 January 2010
A&A 509, A37 (2010)

Gaia relativistic astrometric models

I. Proper stellar direction and aberration

M. Crosta - A. Vecchiato

INAF - Astronomical Observatory of Torino, via Osservatorio 20, 10025 Pino Torinese (TO), Italy

Received 12 June 2009 / Accepted 5 October 2009

Abstract
The high accuracy achievable by modern space astrometry requires the use of General Relativity to model the stellar light propagation through the gravitational field encountered from a source to a given observer inside the Solar System. The general relativistic definition of an astrometric measurement needs an appropriate use of the concept of reference frame, which should then be linked to the conventions of the IAU resolutions. On the other hand, a definition of the astrometric observables in the context of General Relativity is also essential for finding the stellar coordinates and proper motion uniquely, this being the main physical task of the inverse ray-tracing problem. The aim of this work is to set the level of reciprocal consistency of two relativistic models, GREM and RAMOD (Gaia, ESA mission), in order to guarantee a physically correct definition of the light's local direction to a star and deduce the star coordinates and proper motions at the level of accuracy required by these models consistently with the IAU's adopted reference systems.

Key words: relativity - astrometry - gravitation - reference systems - methods: data analysis - techniques: high angular resolution

1 Introduction

The correct definition of a physical measurement requires identification of an appropriate reference frame. This also applies to determining the position and motion of a star from astrometric observations made from within our Solar System. Moreover, modern instruments housed in space-borne astrometric probes like Gaia (Turon et al. 2005) and SIM (Unwin et al. 2008) aim to be accurate at the micro-arcsecond level, or higher as in the case of bright stars observed by SIM (0.2 micro-arcsecond), thus requiring that any astrometric measurement be modeled in a way that both light propagation and detection should be conceived in a general relativistic framework. One needs, in fact, to solve the relativistic equations of the null geodesic that describe the trajectory of a photon emitted by a star and detected by an observer with an assigned state of motion. The whole process takes place in a geometrical environment generated by an N-body distribution such as for our Solar System. Essential to the solution of the above astrometric problem (inverse ray tracing from observational data) is the identification, as boundary conditions, of the local observer's line-of-sight defined in a suitable reference frame (Bini et al. 2003; de Felice & Preti 2006; de Felice et al. 2006).

Summarizing from the quoted references, the astrometric problem consists of determining the astrometric parameters of a star (its coordinates, parallax, and proper motion) from a prescribed set of observational data (hereafter observables). However, while these quantities are well defined in classical (non relativistic) astrometry, in General Relativity (GR) they must be interpreted consistently with the relativistic framework of the model. Similarly, the parameters describing the attitude and the center-of-mass motion of the satellite need to be defined consistently with the chosen relativistic model.

As far as Gaia is concerned, at present two conceptual frameworks are able to treat the astrometric problem at the micro-arcsecond level within a relativistic context. The first model, named GREM (Gaia RElativistic Model) and described in Klioner (2003), is an extension of a seminal study by Klioner & Kopeikin (1992) conducted in the framework of the post-Newtonian (pN) approximation of GR. GREM has been formulated according to a parametrized post-Newtonian scheme accurate to 1 micro-arcsecond. In this model finite dimensions and angular momentum of the bodies of the Solar System are included and linked to the motion of the observer in order to consider the effects of parallax, aberration, and proper motion, and the light path is solved using a matching technique that links the perturbed internal solution inside the near zone[*] of the Solar System with the (assumed) flat external one.

Basically, the pN approach (and post-Minkowskian one, pM, as in Kopeikin & Mashhoon 2002) solves the light trajectory as a straight line (Euclidean geometry) plus integrals, containing the perturbations encountered, from a gravitating source at an arbitrary distance from an observer located within the Solar System. This allows one to transform the observed light ray in a suitable coordinate direction and to read off the aberrational terms and light deflections effects, evaluated at the point of observation. This model is considered as baseline for the Gaia data reduction.

The second model, RAMOD, is an astrometric model conceived to solve the inverse ray-tracing problem in a general relativistic framework not constrained by a priori approximations. RAMOD is actually a family of models of increasing intrinsic accuracy, all based on the geometry of curved manifolds (de Felice et al. 2004,2006). As in Kopeikin & Mashhoon (2002), the full development to the micro-arcsecond level imposes consideration of the retarded distance effects by the motion of the bodies of the Solar System. At present, the RAMOD full solution requires numerical integration of a set of coupled nonlinear differential equations (also called ``master equations''[*]), which allows the light trajectory to be traced back to the initial position of the star and which naturally entangles the contributions by the aberration and those by the curvature of the background geometry. RAMOD is formulated with a completely different methodology. This makes its comparison with the former one a difficult task.

Despite its difficulty, this comparison is a necessity, beacuse GREM and RAMOD will be used for the Gaia data reduction with the purpose of creating a catalog of one billion positions and proper motions based on measurements of absolute astrometry, so any inconsistency in the relativistic model(s) would invalidate the quality and reliability of the estimates, hence all related scientific output.

In this paper we present the first step in the theoretical comparison, showing how it is possible to isolate the aberration terms from the global RAMOD construct (which are normally entangled together with other terms such as those of the deflection) and recasting them in a GREM-like formula.

In Sect. 2 we review all the building steps of the RAMOD astrometric set-up. In Sect. 3 we show the procedures used in RAMOD to define the observables and compare the quantities of GREM-like formulations by making the aberration part in the RAMOD framework explicit. Sect. 4 will comment on the results of the comparison and on what has to be addressed to proceed with the theoretical comparison of the two models. Finally, Appendix B reports the calculations of the pN/pM approaches recovering the stellar aberration.

Throughout the paper, regular bold indicates four-vector (e.g. ${\vec u}$) and italic bold indicates three-vector (e.g. ${\vec n}$); the components of vectorial quantities are indicated with indexes (no bold symbols), where the Latin index stands for 1, 2, 3 and the Greek ones for 0, 1, 2, 3. A repeated index means Einstein summation convention and indexes are raised and lowered with the metric $g_{\alpha\beta}$ (in particular, ni ni stands for the scalar product with respect to the Euclidean metric $\delta_{ij}$, whereas $l^{\alpha} l_{\alpha}$ with respect to the metric $g_{\alpha\beta}$). The speed of light is symbolized by c, notations like $\{ ... \}$ indicate a set of quantities (e.g. $ \{ {\bf\lambda}_{\hat{\alpha}} \}$), and $U_{\alpha\beta} \left (\vec{u}\right)$ or $P_{\alpha\beta} \left({\vec u} \right)$ an operator projecting with respect to the observer ${\vec u}$.

2 The RAMOD frames

In order to bring out the different methodologies and mathematical constructs applied in RAMOD, this section summarizes the set-up of RAMOD by focusing on the reference frames needed to define the measurements.

The set-up of any astrometric model primarily implies the identification of the gravitational sources and of the background geometry. Then one needs to label the space-time points with a coordinate system. These steps allow us to fix a reference frame with respect to which one describes the light trajectory, the motion of the stars, and that of the observer. The RAMOD framework is based on the weak-field requirement for the background geometry, which in turn have to be specialized to the particular case one wants to model. For example, keeping in mind a Gaia-like mission, we can assume the Solar System is the only source of gravity, i.e. a physical system gravitationally bound, in the weak field and slow motion regime. Then, only first-order terms in the metric perturbation h (or equivalently in the constant G as in the pM approximation) are retained. These terms already include all of the possible (v/c)n-order expansions of the pN approach, but just those up to (v/c)3 are needed to reach the micro-arcsecond accuracy required for the next generation astrometric missions, like e.g. Gaia and SIM. With these assumptions the background geometry is given by the following line element

$\displaystyle {\rm d}s^{2}\equiv g_{\alpha\beta}{\rm d}x^{\alpha}{\rm d}x^{\bet... ...ha\beta}+\mathcal{O}\left(h^{2}\right)\right){\rm d}x^{\alpha}{\rm d}x^{\beta},$    

where $\mathcal{O}(h^{2})$ collects all nonlinear terms in h, and the coordinates are x0=ct,x1=x,x2=y,x3=z, the origin being fixed at the barycenter of the Solar System, and $\eta_{\alpha\beta}$ is the Minkowskian metric. In the small curvature limit (Misner et al. 1973), the metric components used in RAMOD are
                      g00 = $\displaystyle -1+\mathop{h_{00}}\limits_{(2)}+\mathcal{O}\left(v^{4}/c^{4}\right)\qquad$  
g0i = $\displaystyle \optwo_{(3)}+\mathcal{O}\left(v^{5}/c^{5}\right)\qquad$ (1)
gij = $\displaystyle 1+\mathop{h_{00}}\limits_{(2)}\delta_{ij}+\mathcal{O}\left(v^{4}/c^{4}\right),$  

where $\mathop{h_{00}}\limits_{(2)}=2w/c^{2}$, $\optwo_{(3)}=w^{i}/c^{3}$, and w and wi are, respectively, the gravitational potential and the vector potential generated by all the sources inside the Solar System that can be chosen according to the IAU resolution B1.3 (Soffel et al. 2003). The metric of Eq. (1) is also adopted in GREM and the subscripts indicate the order of (v/c) (e.g. $\optwo_{(3)}\sim\mathcal{O}(v^{3}/c^{3})$).

2.1 The BCRS

In RAMOD, a Barycentric Celestial Reference System (BCRS, Soffel et al. 2003) is identified requiring that a smooth family of space-like hyper-surfaces exists with the equation $t\left(x,y,z\right)={\rm constant}$ (see de Felice et al. 2004). The function t can be taken as a time coordinate. On each of these $t\left(x,y,z\right)={\rm constant}$ hypersurfaces, one can choose a set of Cartesian-like coordinates centered at the barycenter of the Solar System (B) and running smoothly as parameters along space-like curves that point to distant cosmic sources. The latter are chosen to assure that the system is kinematically nonrotating, i.e. nonrotating with respect to the reference distant sources as recommended by the IAU (Soffel et al. 2003). The parameters x, y, z, together with the time coordinate t, provide a basic coordinate representation of the space-time according to the IAU resolutions[*].

Any tensorial quantity will be expressed in terms of coordinate components relative to coordinate bases induced by the BCRS.

2.2 The local BCRS

As shown in detail in (de Felice et al. 2004,2006), in RAMOD at any space-time point a unitary four-vector exists ${\vec u}$ that is tangent to the world line of a physical observer at rest with respect to the spatial grid of the BCRS defined as

$\displaystyle {u}^{\alpha}=\left(-g_{00}\right)^{-1/2} \delta^{\alpha}_{0}=\left(1+\frac{h_{00}}{2}\right) \delta^{\alpha}_{0}+\mathcal{O}\left(h^{2}\right).$   (2)

The totality of these four vectors over the space-time forms a vector field that is proportional to a time-like and asymptotically Killing vector field  $\vec{\eta}$. In fact, to the order of accuracy required for Gaia, the congruence of curves ${\vec u}$ does not admit a global family of orthogonal hyper-surfaces, i.e. a rest-space that covers the entire space-time. However, the rest-space of ${\vec u}$ can be locally identified by a spatial triad lying on a surface, which differs from the $t=\mbox{constant}$ one (see Fig. 1) in such a way that their spatial components point to the local coordinate directions as chosen by the BCRS. This frame works as a local BCRS.
\begin{figure} \par\includegraphics[width=7.5cm,clip]{12691fg1.eps} \end{figure} Figure 1:

The local observer ${\vec u}$ with respect to the BCRS coordinate system. The spatial axes of the BCRS point toward distant sources. The dashed lines are the curves that are orthogonal, say $\vec{\eta}$, to the $t=\mbox{constant}$ hyper-surfaces, asymptotically orthogonal to the time direction. The rest-space (green area) of ${\vec u}$ locally deviates from the space-like hyper-surface with equation $t(x,y,z)={\rm constant}$by terms of the order of a micro-arcsecond.

Open with DEXTER

The tetrad associated to the local BCRS has spatial axes (the triad) coinciding with the local coordinate axes, but its origin is the barycenter of the satellite. At the $\mathcal{O}\left(h^{2}\right)$, this triad is (Bini et al. 2003)

                         $\displaystyle \lambda_{\hat{a}}^{\alpha}$ = $\displaystyle h_{0a}\delta_{0}^{\alpha}+\left(1-\frac{h_{00}}{2}\right)\delta_{a}^{\alpha}+\mathcal{O}\left(h^{2}\right).$ (3)

Let us stress that ${\vec u}$ is an essential prerequisite of RAMOD, because at any space-time point and apart from a position-dependent rescaling of its time rate, it plays the role of a barycentric observer as the one located at the spatial coordinate fixed at the barycenter of the Solar System. In RAMOD any physical measurement refers to this local BCRS.

2.3 The proper reference frame for the satellite

The proper reference frame of a satellite consists of its rest-space and a clock that measures the satellite proper time. The tensorial quantity that expresses a proper reference frame of a given observer is a tetrad adapted to that observer, namely a set of four unitary, mutually orthogonal four-vectors $\vec{\lambda_{\hat{\alpha}}}$, one of which, i.e. $\vec{\lambda_{\hat{0} }}$, is the observer's four-velocity, while the other $\vec{\lambda_{\hat{a}}}$s form a spatial triad of space-like four-vectors (Misner et al. 1973). The physical measurements made by the observer (satellite) represented by such a tetrad are obtained by projecting the appropriate tensorial quantities on the tetrad axes.

The same measurements can also be defined by splitting the space-time into two subspaces, as sketched in Appendix A. Essentially, this last method is useful when we do not know the solution of a tetrad, which depends on the metric, and we only need to know the moduli of the physical quantities. As far as RAMOD is concerned, given the metric (1) and in the case of a Gaia-like mission, an explicit analytic expression for a tetrad adapted to the satellite four-velocity exists and can be found in Bini et al. (2003). The spatial axes of this tetrad, named $\left\{ \vec{E_{\hat{a}}}\right\}$, are used to model the attitude of the satellite.

2.3.1 Satellite proper reference frame and IAU conventions

In RAMOD the satellite reference frame is obtained by successive transformations of the local BCRS tetrad $\left\{ \vec{\lambda_{\hat{\alpha}}}\right\} $as defined in Eq. (3). In particular, the vectors of the triad $\left\{ \vec{\lambda_{\hat{a}}}\right\}$ are boosted to the satellite rest-frame by means of an instantaneous Lorentz transformation (Bini et al. 2003, and reference therein), which depends on the relative spatial velocity $\nu^{\alpha}$ of the satellite

$\displaystyle \nu^{\alpha}=\frac{1}{\gamma}\left(u_{s}^{\alpha}-\gamma u^{\alpha}\right),$   (4)

identified by the four-velocity ${\vec u_{s}}$ with respect to the local BCRS ${\vec u}$, whose Lorentz factor is given by $\gamma=-u_{s}^{\alpha}u_{\alpha}$ (Jantzen et al. 1992).

The boosted tetrad $\left\{\mathop{\lambda^{\alpha}}\limits_{bs}\right\}$ obtained in this way represents a CoMRS (Center-of-Mass Reference System, comoving with the satellite), similar to what is defined for Gaia (Klioner 2004; Bastian 2004). In addition to the definition in the cited works, one of the axes is Sun-locked, i.e. one axis points toward the Sun at any point of its Lissajous orbit around L2. The Gaia attitude frame is finally obtained by applying the following rotations to the Sun-locked frame: (i) by an angle $\omega_{p}t$ about the four-vector ${\mathop{\vec{\lambda_{\hat{\alpha}}}}\limits_{bs}}_{\hat{1}}$which constantly points towards the Sun (where $\omega_{p}$ is the angular velocity of precession); (ii) by a fixed angle $\alpha$ about the image of the four-vector ${\mathop{\vec{\lambda_{\hat{\alpha}}}}\limits_{bs}}_{\hat{2}}$after the previous rotation; and (iii) by an angle $\omega_{r}t$ about the image of the four-vector ${\mathop{\vec{\lambda_{\hat{\alpha}}}}\limits_{bs}}_{\hat{1}}$after the previous two rotations (where $\omega_{r}$ is now the spin angular velocity). The triad resulting from these transformations establishes the satellite attitude triad, given by

$\displaystyle {\vec E_{\hat{a}}}=\mathcal{R}_{1}\left(\omega_{r}t\right)\mathca... ...cal{R}_{1}\left(\omega_{p}t\right)\mathop{\vec{\lambda_{\hat{a}}}}\limits_{bs}.$    

The final triad $\left\{ \vec{E_{\hat{a}}}\right\}$ only depends on the attitude parameters of the satellite, and should be the RAMOD equivalent of the GREM Satellite Reference System (SRS) (Bastian 2004). This defines the spatial components of the reference system.

To complete the process one has to include the transformations between the observer's proper time and the barycentric coordinate time. This can be done using the subspace splitting technique cited in Appendix A. Let us consider the satellite's world-line in the space-time geometry as

$\displaystyle {\vec u_{s}}=u_{s}^{0}\left(\delta_{0}^{\alpha}+\beta^{i}\delta_{i}^{\alpha}\right),$   (5)

where $\beta^{i}=v^{i}/c$ are the BCRS coordinate components of the satellite velocity and $v^i={\rm d}x^i / {\rm d}t$ ( v2=vivi); us0 can be chosen as the normalization factor. Since the satellite is a physical observer, from the unitary condition $ u_{s\alpha}u_{s}^{\alpha}=-1 $, we deduce the expansion of us0in powers of (v/c) (once we use the pN potentials w and wi defined by IAU resolutions, Soffel et al. 2003):
                           us0 $\textstyle \approx$ $\displaystyle 1+c^{-2}\left(w+\frac{v^{2}}{2}\right)$ (6)
    $\displaystyle +c^{-4}\left(\frac{3}{8}v^{4}+\frac{5w}{2}v^{2}+\frac{w^{2}}{2}-4\delta_{ij}v^{i}w^{j}\right).$  

Then, by inserting the last expression (6) in Eq. (A.3), we obtain the formula which ties the running between the clock on board up to the order (v/c)4and that for the origin of the BCRS:
                          $\displaystyle {\rm d}T_{\vec{u_{s}}}$ = $\displaystyle -u_{s}^{0}\left[\left(g_{00}+\frac{v^{i}}{c}g_{i0}\right)+\frac{1}{c}g_{i0}{\rm d}x^{i}+g_{ij}\frac{v^{i}}{c}{\rm d}x^{j}\right]$ (7)
  $\textstyle \approx$ $\displaystyle {\rm d}t-c^{-2}\left[\left(\frac{v^{2}}{2}+w\right)+v^{i}{\rm d}R^{i}\right]$  
    $\displaystyle +c^{-4}\left[\left(\frac{w^{2}}{2}-\frac{v^{4}}{8}-\frac{3v^{2}w}{2}+4w^{i}v^{i}\right){\rm d}t\right.$  
    $\displaystyle \left.+4w^{i}{\rm d}R^{i}-\left(3w+\frac{v^{2}}{2}\right)v^{i}{\rm d}R^{i}\right],$  

where xi is any spatial location inside or in the neighborhood of the satellite and Rsi=xi - xsi. It is trivial to check that, when we make a first-order Taylor series expansion around the satellite barycenter location ${\vec x}_{s}$ of the potential (and the vector potential),
$\displaystyle w({\vec x})=w({\vec x}_{s})+\left(\frac{\partial w}{\partial x^{i}}\right)_{s}R_{s}^{i}+\mathcal{O}(R^{2}).$    

Equation (7) can be transformed (Crosta 2003) in the relationships between the proper time on board the satellite and the barycentric coordinate time interval as reported in IAU resolutions B1.5. This finally completes the definition of the proper reference frame for the Gaia-like satellite in the RAMOD framework and, moreover, gives proof of the compatibility of the RAMOD formalism with the IAU conventions (hence with a GREM-like approach).

3 Multi-step application of the observable e in RAMOD to the aberration

The classical (non relativistic) approach of astrometry has traditionally privileged a ``multi-step'' definition of the observable; i.e., the quantities that ultimately enter the ``final'' catalog and are referred to a global inertial reference system, are obtained taking into account effects such as aberration and parallax, one by one and independent from each other.

GREM reproduces this approach of classical astrometry in a relativistic framework. For this model the BCRS is the equivalent of the inertial reference system of the classical approach, while the final expression of the star direction in the BCRS is obtained after converting the observed direction into coordinate ones in several steps that divide the effects of the aberration, the gravitational deflection, the parallax, and proper motion (Klioner 2003) (see Appendix B). As is well known, stellar aberration arises from the motion of the observer relative to the BCRS origin, assumed to coincide with the center of mass of the Solar System.

In the previous section we mentioned that RAMOD relies on the tetrad formalism for the definition of the observable. In general, the three direction cosines that identify the local line-of-sight to the observed object are relative to a spatial triad $\left\{ \vec{E_{\hat{a}}}\right\}$associated with a given observer $\vec {u'}$; the direction cosines with respect to the axes of this triad are defined as

$\displaystyle \cos\psi_{\hat{a}}=\frac{P(\vec {u'})_{\alpha\beta}k^{\alpha}E_{\... ...(P(\vec {u'})_{\alpha\beta}k^{\alpha}k^{\beta}\right)^{1/2}}\equiv e_{\hat{a}},$   (8)

where the final $e_{\hat{a}}$ is a shorthand notation for $\cos\psi_{\hat{a}}$ and $k^{\alpha}$ the four-vector tangent to the null geodesic connecting the star to the observer, and all the quantities are obviously computed at the event of the observation[*]. As a consequence, given the solution of the null geodesic equation and the motion and the attitude of the observer, Eq. (8) expresses a relation between the unknowns, the position and motion of the star, and the observable quantities that include all of these effects mentioned for GREM. Once the procedure for defining Eq. (8) is complete, the final measurements will naturally entangle every GR ``effect'' in a single result. In other words, RAMOD does not need to disentangle each single effect, relativistic or not. The main purpose is to keep as long as possible the physical expressions of the quantities entering Eq. (8). Therefore, the natural way to ``extract'' any of those effects in a separate formula, as in GREM, is to express the observable with a specific tetrad that makes the aberration part evident.

3.1 Attitude-free tetrad for the aberration

Whatever tetrad we consider, the expression of Eq. (8) for the relativistic observable in the RAMOD model can also be written as (de Felice et al. 2006)

$\displaystyle e_{\hat{a}}=\frac{\left(\bar{l}_{\left(0 \right) \beta}-\nu_{\bet... ...}^{\beta}}{\gamma\left(1-\nu_{\alpha}\bar{l}_{\left(0\right)}^{\alpha}\right)},$   (9)

where $\vec{\nu}$ is the spatial four-velocity (see Eq. (4), also called as the ``physical velocity'') of the satellite ${\vec u_{s}}$ relative to the local barycentric observer ${\vec u}$. The quantity $\bar{l}_{\left(0\right)}^{\alpha}$was introduced in RAMOD and is a unitary four-vector that represents the local line-of-sight of the photon as seen by ${\vec u}$ at the moment of observation. In general, $\bar{l}^{\alpha} = P_{\beta}^{\alpha}({\vec u})k^{\beta}/ (- u^{\beta} k_{\beta})$ (de Felice et al. 2004,2006). Finally, $\gamma$ is the Lorentz factor of ${\vec u_{s}}$ with respect to ${\vec u}$; that is,
$\displaystyle -u_{s}^{\alpha}u_{\alpha}=\frac{1}{\sqrt{1-\nu^{2}/c^{2}}}\equiv\gamma,$   (10)

where $\nu^{2}=\nu^{\alpha}\nu_{\alpha}$.

To retrieve the aberration effect given by the motion of the satellite with respect to the BCRS in RAMOD, one needs to specialize Eq. (9) to the case of a tetrad $ \{ {\bf\tilde{\lambda}_{\hat{\alpha}}} \} $adapted to the center of mass of the satellite assumed with no attitude parameters. In this case, in fact, the observation equation will give a relation between the ``aberrated'' direction represented by the direction cosines ea, as measured by the satellite and the ``aberration-free'' direction given by the quantity $\bar{l}_{\left(0\right)}^{\alpha}$referring to the local BCRS frame $ \{ \bf {\lambda_{\hat{a}}} \}$. The vectors of the triad $ \{ {\bf\tilde{\lambda}_{\hat{a}}} \} $differ from the local BCRS's $ \{ \bf {\lambda_{\hat{a}}} \}$for a boost transformation with four-velocity ${\vec u_{s}}$. This means that it can be derived from Eq. (3) using the relation (Jantzen et al. 1992)

$\displaystyle \tilde{\lambda}_{\hat{a}}^{\alpha}=P\left(\vec{u_{s}}\right)_{\si... ...amma}{\gamma+1}\nu^{\sigma}\left(\nu^{\rho}\lambda_{\rho\hat{a}}\right)\right],$   (11)

where ${\vec u_{s}}$ and $\vec{\nu}$ are the above-mentioned four velocity of the satellite and its physical velocity relative to the local BCRS, and $P\left(\vec{u_{s}}\right)_{\sigma}^{\alpha}=\delta_{\sigma}^{\alpha}+u_{s}^{\alpha}u_{s\sigma}$.

3.2 Aberration at the $\left (\sf\textit v/\textit c\right )^{\sf 3}$ order as function of the local line-of-sight

To recover a GREM-like aberration relativistic effect in RAMOD, we have to expand Eq. (9) with respect to the (v/c) small pN parameter. From de Felice et al. (2006) and Bini et al. (2003) it is

$\displaystyle u_{s}^{\alpha}=\left(1+\frac{h_{00}}{2}+\frac{1}{2}\frac{v^{2}}{c... ...v^{i}}{c}\delta_{i}^{\alpha}\right)+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)$   (12)

where vi are the same as was defined in the previous sections. Now, when considering Eq. (4) one deduces that $\nu^{0}\sim\mathcal{O}\left(v^{4}/c^{4}\right)$and
$\displaystyle \nu^{i}=\left(1+\frac{h_{00}}{2}\right)\frac{v^{i}}{c}+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)\cdot$   (13)

Expanding Eq. (11) with relations (10) and (4), one gets
                           $\displaystyle \tilde{\lambda}_{\hat{a}}^{\alpha}$ = $\displaystyle \lambda_{\hat{a}}^{\alpha}+u_{{\rm s}}^{\alpha}\left(u_{{\rm s}}^... ...v^{2}}{c^{2}}\right)\nu^{\alpha}\left(\nu^{\beta}\lambda_{\hat{a} \beta}\right)$  
    $\displaystyle -u_{{\rm s}}^{\alpha}\left(\frac{1}{2}+\frac{1}{8}\frac{v^{2}}{c^... ...\lambda_{\hat{a} \beta}\right)+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)\cdot$ (14)

Then, using Eqs. (3), (12), and (13) and expanding the scalar products to the right order, we obtain
                 $\displaystyle \left(u_{{\rm s}}^{\beta} \lambda_{\hat{a} \beta}\right)$ = $\displaystyle \left(1+h_{00}+\frac{1}{2}\frac{v^{2}}{c^{2}}\right)\frac{v^{a}}{c}+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)$ (15)
$\displaystyle \left(\nu^{\beta} \lambda_{\hat{a} \beta}\right)$ = $\displaystyle \left(1+h_{00}\right)\frac{v^{a}}{c}+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)$ (16)
$\displaystyle \left(u_{{\rm s}}^{\beta} \nu_{\beta} \right)$ = $\displaystyle \frac{v^{2}}{c^{2}}+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)$ (17)

so that the expression for the boosted tetrad finally becomes
                     $\displaystyle \tilde{\lambda}_{\hat{a}}^{\alpha}$ = $\displaystyle \lambda_{\hat{a}}^{\alpha}+\left(1+\frac{3h_{00}}{2}+\frac{1}{2}\frac{v^{2}}{c^{2}}\right)\delta_{0}^{\alpha}\frac{v^{a}}{c}$  
    $\displaystyle +\frac{1}{2}\frac{v^{i}}{c}\delta_{i}^{\alpha}\frac{v^{a}}{c}+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)\cdot$ (18)

Given Eq. (18) one can consistently recast Eq. (9) as
                             $\displaystyle \tilde{e}_{\hat{a}}$ = $\displaystyle \frac{\left(\bar{l}-\nu\right)_{\beta}\lambda_{\hat{a}}^{\beta}}{... ...\left(1+\frac{3h_{00}}{2}+\frac{1}{2}\frac{v^{2}}{c^{2}}\right) \frac{v^{a}}{c}$  
    $\displaystyle +\frac{1}{2}\frac{\left(\bar{l}-\nu\right)_{\beta}\frac{v^{i}}{c}... ...l}^{\alpha}\right)}\frac{v^{a}}{c}+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right),$ (19)

where $\tilde{e}_{\hat{a}}$ are the cosines related to the tetrad $ \{ {\bf\tilde{\lambda}_{\hat{a}}} \} $, which, as said, does not contain the attitude parameters. Here and in the rest of the section, we replace $\left(\bar{l}_{\left(0 \right) \beta}-\nu_{\beta}\right)$ with $\left(\bar{l}_{\left(0 \right)}-\nu\right)_{\beta}$, and the symbol $\bar{l}_{\left(0\right)}^{\alpha}$ with $\bar{l}^{\alpha}$to ease the notation.

After long calculations and considering the IAU metric, the first term on the righthand-side of this formula can be written as

    $\displaystyle \frac{\left(\bar{l}-\nu\right)_{\beta}\lambda_{\hat{a}}^{\beta}}{... ...ac{1}{c}\left[-v^{a}+\left(\delta_{ij}v^{i}\bar{l}^{j}\right)\bar{l}^{a}\right]$ (20)
    $\displaystyle +\frac{1}{c^{2}}\left\{ w\bar{l}^{a}-\left(\delta_{ij}v^{i}\bar{l... ...elta_{ij}v^{i}\bar{l}^{j}\right)^{2}-\frac{1}{2}v^{2}\right]\bar{l}^{a}\right\}$  
    $\displaystyle + \frac{1}{c^{3}}\left\{ -2wv^{a}-\left[\left(\delta_{ij}v^{i}\ba... ...v^{a}+\bar{l}^{a}\left[3w\left(\delta_{ij}v^{i}\bar{l}^{j}\right)\right.\right.$  
    $\displaystyle \left.\left.+\left(\delta_{ij}v^{i}\bar{l}^{j}\right)^{3}-\frac{1... ...r{l}^{j}\right)\right]\right\}+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)\cdot$  

The second term is zero since both $\bar{l}_{0}$ and $\nu_{0}$ are zero, while the third one becomes
$\displaystyle \frac{1}{2}\frac{\left(\bar{l}-\nu\right)_{i}\left(v^{i}/c\right)... ...}{c^{2}}\right]\frac{v^{a}}{c}+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)\cdot$   (21)

Finally, collecting all terms, we get
                                         $\displaystyle \tilde{e}_{\hat{a}} = \bar{l}^{a}+\frac{1}{c}\left[-v^{a}+\left(\delta_{ij}v^{i}\bar{l}^{j}\right)\bar{l}^{a}\right]$  
    $\displaystyle +\frac{1}{c^{2}}\left\{ w\bar{l}^{a}-\frac{1}{2}\left(\delta_{ij}... ...elta_{ij}v^{i}\bar{l}^{j}\right)^{2}-\frac{1}{2}v^{2}\right]\bar{l}^{a}\right\}$  
    $\displaystyle +\frac{1}{c^{3}}\left\{ -2wv^{a}-\frac{1}{2}\left(\delta_{ij}v^{i}\bar{l}^{j}\right)^{2}v^{a}\right.$  
    $\displaystyle +\left.\bar{l}^{a}\left[3w\left(\delta_{ij}v^{i}\bar{l}^{j}\right... ...ght)^{3}-\frac{1}{2}v^{2}\left(\delta_{ij}v^{i}\bar{l}^{j}\right)\right.\right.$  
    $\displaystyle \left.\left.+w\left(\delta_{ij}v^{i}\bar{l}^{j}\right)\right]\right\} +\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)\cdot$ (22)

3.3 Recasting to the GREM-like aberration

Expression (22) relates the observed direction cosines with $\bar{l}^{a}$. The equivalent relation for the GREM observable is Eq. (B.6) where the aberration is expressed in terms of a vector ${\vec n}$. At first glance, it comes out that we cannot simply identify $\bar{l}^{a}$ with ${\vec n}$, since the last expression shows differences in terms up to the $\left(v/c\right)^{2}$ order! In particular, the appearance of the term $w ~ \bar{l}^{a}$ and of different factors at the $\left(v/c\right)^{3}$ order cannot allow a straightforward comparison, as expected, of Eq. (22) to the GREM vectorial one of Eq. (B.6). Therefore, to compare formula (22) with GREM's formula (B.6) and find a relationship between ${\vec n}$ and $\vec{\bar{l}}$, we need to reduce the $\bar{l}^{a}$s to their coordinate Euclidean expressions.

In GREM, ${\vec n}$ represents the ``aberration-free'' coordinate line of sight of the observed star at the position of the satellite momentarily at rest. In RAMOD, as said, $\vec{\bar{l}}$ represents the normalized local line-of-sight of the observed star as seen by the local barycentric observer ${\vec u}$. In other words, $\vec{\bar{l}}$ is a four-vector that fixes the line of sight of an object with respect to the local BCRS. Do ${\vec n}$ and $\vec{\bar{l}}$ have a similar role in the two approaches? From the physical point of view they have the same meaning, as the observed ``aberration free'' direction to the star. Let us start from the definition of ${\vec n}$ in GREM:

$\displaystyle n^{i}=\frac{p^{i}}{p},$  

where $p^{i}=c^{-1}{\rm d}x^{i}/{\rm d}t$ and pis the Euclidean norm of pi, so that $p^{-1}\simeq\left(1+h_{00}+h_{0i}p^{i}\right)+\mathcal{O}\left(h^{2}\right)$. This means that
$\displaystyle n^{i}=p^{i}\left(1+h_{00}+h_{0i}p^{i}\right)+\mathcal{O}\left(h^{2}\right).$   (23)

On the other hand, using the definition of $\vec{\bar{l}}$, it can be easily shown that its spatial components are
$\displaystyle \bar{l}^{i}=-\frac{k^{i}}{u_{\alpha}k^{\alpha}}=-\frac{k^{i}}{u^{0}k^{0}\left(-1+h_{00}+h_{0i}\frac{k^{i}}{k^{0}}\right)},$    

and, from $u^{0}=\left(-g_{00}\right)^{-1/2}$ and $k^{i}/k^{0}=c^{-1}{\rm d}x^{i}/{\rm d}t\equiv p^{i}$, we get
                       $\displaystyle \bar{l}^{i}$ = $\displaystyle p^{i}\left(-g_{00}\right)^{1/2}\left(1-h_{00}-h_{0i}p^{i}\right)^{-1}$  
  = $\displaystyle p^{i}\left(1+\frac{1}{2}h_{00}+h_{0i}p^{i}\right)+\mathcal{O}\left(h^{2}\right).$ (24)

Finally, from Eqs. (23) and (24) one has
                 $\displaystyle \bar{l}^{i}$ = $\displaystyle n^{i}\left(1-\frac{h_{00}}{2}\right)+\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right),$ (25)

namely, the spatial light direction, expressed in terms of its Euclidean counterpart at the satellite location in the gravitational field of the solar system. It is worth noticing that no terms of the order of $\mathcal{O}[(v/c)^{3}]$ appear in (25).

Combining Eq. (22) with (25) and setting $\delta_{ij}v^{i}n^{j} \equiv\vec{v}\cdot\vec{n}$to ease the notation, we obtained

                                   $\displaystyle \tilde{e}_{\hat{a}} = n^{a}+\frac{1}{c}\left[-v^{a}+\left(\vec{v}\cdot\vec{n}\right)n^{a}\right]$ (26)
    $\displaystyle +\frac{1}{c^{2}}\left\{ -\frac{1}{2}\left(\vec{v}\cdot\vec{n}\rig... ...eft[\left(\vec{v}\cdot\vec{n}\right)^{2}-\frac{1}{2}v^{2}\right]n^{a}\right\} +$  
    $\displaystyle \frac{1}{c^{3}}\left\{ -2wv^{a}-\frac{1}{2}\left(\vec{v}\cdot\vec{n}\right)^{2}v^{a} \right.$  
    $\displaystyle \left.+\left(\vec{v}\cdot\vec{n}\right)n^{a}\left[2w+\left(\vec{v... ...}-\frac{1}{2}v^{2}\right]\right\} +\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right),$  

i.e. the righthand side of the aberration expression of RAMOD rewritten as in GREM.

Now we have to be certain that the lefthand side of Eq. (26) can also be directly compared with GREM's formula (B.6). Let us apply the tetrad property $\lambda_{\alpha}^{\hat{\mu}}\lambda_{\hat{\mu}\beta}=g_{\alpha\beta}$to the definition of $\tilde{e}_{\hat{a}}$ and get

    $\displaystyle \tilde{e}_{\hat{a}}\equiv\frac{P(u)_{\alpha\beta}k^{\alpha}\tilde... ...}_{\hat{a}}^{\beta}}{\left(P(u)_{\alpha\beta}k^{\alpha}k^{\beta}\right)^{1/2}}=$  
    $\displaystyle \frac{k^{\alpha}\tilde{\lambda}_{\alpha}^{\hat{a}}}{\vert g_{\alp... ...beta}^{\hat{0}}}=\frac{{\rm d}\tilde{x}^{\hat{a}}}{{\rm d}\tilde{x}^{\hat{0}}}.$ (27)

Is there a relation between the direction cosines of this equation with the spatial components of the observed vector  ${\vec s}^{i}$ in GREM? The crucial point stands on the definition of the coordinate system. The tetrad components of the light ray can be directly associated to CoMRS coordinates, i.e. to a coordinate-induced tetrad (as in Klioner 2004), if the boosted local BCRS tetrad coordinates $\tilde{x}^{\hat{\alpha}}$are equivalent to the CoMRS ones $\mathcal{X}^{\alpha}$.

In RAMOD, at the milli-arcsecond level, i.e. at (v/c)2, the rest-space of the local barycentric observer coincides globally with the spatial hyper-surfaces that foliate the space-time and define the BCRS (de Felice et al. 2004). At micro-arcsecond accuracy, instead, the vorticity cannot be neglected and the geometry is affected by nondiagonal terms of the metric, meaning that the $t={\rm constant}$ hyper-surfaces do not coincide with the rest-space of the local barycentric observer (de Felice et al. 2006). Then, to be consistent, at each point of observation we can only define a spatial direction measured by the local barycentric observer and then associate it to the satellite measurements via the direction cosines relative to the boosted attitude frame.

The equivalence of the two coordinate systems thus holds if the origins of the two reference systems coincide and only locally, i.e. in a sufficiently small neighborhood, since the tetrads are not necessarily holonomic. Under these hypotheses and from (B.1), one can state that

$\displaystyle \frac{{\rm d}\tilde{x}^{\hat{a}}}{{\rm d}\tilde{x}^{\hat{0}}}=\frac{{\rm d}\mathcal{X}^{a}}{{\rm d}\mathcal{X}^{0}}\equiv-s^{a},$    

and it follows that
$\displaystyle \tilde{e}_{\hat{a}} =-s^{a}.$   (28)

Therefore, using the local validity of Eq. (28) and considering that $\vec{n} \cdot \vec {n} =1$ and $v^{2} = \delta_{ij} v^{i} v^{j} \equiv \vec{v} \cdot \vec{v}$, Eq. (26) can be written as
                                sa = $\displaystyle -n^{a}+\frac{1}{c}\left[v^{a}\left(\vec{n}\cdot\vec{n}\right)-n^{a}\left(\vec{v}\cdot\vec{n}\right)\right]+$  
    $\displaystyle \frac{1}{c^{2}}\left\{ \left(\vec{v}\cdot\vec{n}\right)\left[v^{a... ...vec{n}\cdot\vec{n}\right)-n^{a}\left(\vec{v}\cdot\vec{n}\right)\right]+ \right.$  
    $\displaystyle \left.\frac{1}{2}\left[n^{a}\left(\vec{v}\cdot\vec{v}\right)-v^{a}\left(\vec{v}\cdot\vec{n}\right)\right]\right\} +$  
    $\displaystyle \frac{1}{c^{3}}\left\{ 2w\left[v^{a}\left(\vec{n}\cdot\vec{n}\right)-n^{a}\left(\vec{v}\cdot\vec{n}\right)\right]+\right.$  
    $\displaystyle \left. \left(\vec{v}\cdot\vec{n}\right)^{2}\left[v^{a}\left(\vec{n}\cdot\vec{n}\right)-n^{a}\left(\vec{v}\cdot\vec{n}\right)\right]+\right.$  
    $\displaystyle \left.\frac{1}{2}\left(\vec{v}\cdot\vec{n}\right)\left[n^{a}\left... ...cdot\vec{n}\right)\right]\right\} +\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right).$ (29)

Finally, from the relation $\vec{a}\times\left(\vec{b}\times\vec{c}\right)=\vec{b}\left(\vec{a}\cdot\vec{c}\right)-\vec{c}\left(\vec{a}\cdot\vec{b}\right)$, it is
                                 $\displaystyle s^{a} = -n^{a}+\frac{1}{c}\left[\vec{n}\times\left(\vec{v}\times\... ...n}\right)\left[\vec{n}\times\left(\vec{v}\times\vec{n}\right)\right]^{a}\right.$  
    $\displaystyle \left.+\frac{1}{2}\left[\vec{v}\times\left(\vec{n}\times\vec{v}\r... ...w\right]\left[\vec{n}\times\left(\vec{v}\times\vec{n}\right)\right]^{a} \right.$  
    $\displaystyle \left.+\frac{1}{2}\left(\vec{v}\cdot\vec{n}\right)\left[\vec{v}\t... ...s\vec{v}\right)\right]^{a}\right\} +\mathcal{O}\left(\frac{v^{4}}{c^{4}}\right)$ (30)

which is formula (B.6) for the aberration in GREM-like model if we consider that $\vec{v}\equiv\dot{\vec{x}}_{{\rm o}}$, and $w\equiv w\left(\vec{x}_{{\rm o}}\right)$. This result states that, limited to the case of aberration and using the appropriate definitions of the IAU recommendations, RAMOD recovers GREM at the $\left(v/c\right)^{3}$ order.

4 Conclusions

This paper compares two approaches within the context of relativistic astrometry, GREM and RAMOD, both suitable for modeling modern astrometric observations at micro-arcsecond accuracy. Because of the structure of GREM, the earliest stage of a theoretical comparison starts with the evaluation of the aberration ``effect'' in RAMOD.

This work presents a first analysis between two different methods in applying general relativity, the only theory of gravitation up to now, to astrometry. Understanding any difference and/or equivalence represents a valuable help to exploit the Gaia observations to their full extent and to validate data analysis in the new era of relativistic astrometry.

Indeed, the different mathematical structures of GREM and RAMOD hinder a straightforward comparison and call for a more in-depth analysis of the two models. While GREM favors the direct application of the coordinate approach since the beginning, RAMOD prefers, instead, to keep the meaning of the physical quantity as far as possible, i.e. to move to the coordinates once the condition equations are solved (namely the equations linking the measurements and astrometric unknowns). This implies a certain number of differences between the two derivations that have to be taken into account to avoid misinterpretations of parallel but different quantities. Up to now, we can distinguish the following differences in how the two models use: (i) the boundary conditions; (ii) the astrometric measurements; (iii) the attitude implementation; (iv) and the definition of the proper light direction.

Of crucial importance is point (i). The light signal arriving at the local BCRS along the spatial direction $l^{\alpha}=P({\vec u})_{\beta}^{\alpha} k^{\beta}$satisfies the RAMOD master equations, a set of nonlinear coupled differential equations (de Felice et al. 2006). Therefore the cosines (i.e. the astrometric measurements) taken as a function of the local line of sight (the physical one), at the time of observation, allow fixing the boundary conditions needed to solve the master equations and determining the star coordinates uniquely. However, since the direction cosines are expressed in terms of the attitude, the mathematical characterization of the attitude frame is essential for completing the boundary value problem in the process of reconstructing the light trajectory. The vector ${\vec n}$ in GREM, i.e. the ``aberration-free'' counterpart of $\vec{\bar{l}}$ of RAMOD, is instead used to derive the aberration effect (in a coordinate language), and there is no need to connect it with a RAMOD-like boundary value problem.

In RAMOD the direction cosines link the attitude of the satellite to the measurements, combining several reference frames useful to determine, as final task, the stellar coordinates: the BCRS (kinematically non-rotating global reference frame), the CoMRS (a local reference frame comoving with the satellite centre of mass), and the SRS (the attitude triad of the satellite). The coordinate transformations between BCRS/CoMRS/SRS come out naturally once the IAU conventions are adopted. A proof of this is given when we apply proper time formula (A.3) to get the relationship between the running time on board and the barycentric coordinate time (7). This is inside the conceptual framework of RAMOD, where the astrometric set-up allows one to trace the light ray back to the emitting star in a curved geometry, and it is not natural to disentangle each single effect. As for the solution of the geodesic equation, RAMOD defines a complete procedure to derive the satellite attitude that as input depends only on the specific terms of the metric that describes the addressed physical problem. GREM, instead, embeds the definition of its main reference system (BCRS) within the metric, consequently each further step depends on this choice. This includes all the subsequent transformations among the reference systems that are essential for extracting the GREM observable as a function of the astrometric unknowns. On the other side, the RAMOD directly implements in the solution of the astrometric problem the relativistic algorithms of the attitude frame, assuring its consistency with GR, since by definition the origin of the tetrad system follows the observer's world-line (i.e. the center of mass of the satellite in this case). The last comment explains items (ii) and (iii) and introduces item (iv).

Because physical quantities do not depend on the coordinates, the direction cosines are a powerful tool for comparing the astrometric relativistic models: their physical meaning allows us to correctly interpret the astrometric parameters in terms of coordinate quantities. This justified the conversion of the physical stellar proper direction of RAMOD into its analogous Euclidean coordinate counterpart, which ultimately leads to the derivation of a GREM-style aberration formula. Another point arises when the observables of RAMOD have to be identified with si, i.e. the components of the observed vector of GREM. This matching is admitted only if the origins of the boosted local BCRS tetrad in RAMOD and of the CoMRS in GREM coincide.

In conclusion, to what extent, then, is the process of star coordinate ``reconstruction'' consistent with General Relativity&Theory of Measurements? Solving the astrometric problem in practice means to compile an astrometric catalog with the same order of accuracy as the measurements. This paper shows not only that the two models give the same results, but also that particular care is needed in the interpretation of the observables and of the quantities that constitute the final catalog in order to avoid differences that already exist at the level of the aberration effect.

Acknowledgements
The authors wish to thank Prof. Fernando de Felice and Dr. Mario G. Lattanzi for constant support and useful discussions. In particular, we thank the referee for his valuable comments and suggestions. This work is supported by the ASI grants COFIS and I/037/08/0.

Appendix A: Length and time measurements due to a space-time splitting

An observer $\vec {u'}$ carrying its laboratory is usually represented as a world tube; in the case of a non-extended body, the world tube can be restricted to a world line tracing the history of the observer's barycenter in the given space-time. At any point P along the world line of $\vec {u'}$, and within a sufficiently small neighborhood, it is possible to split the space-time into a one-dimensional space and a three-dimensional one (de Felice & Clarke 1990), each space being endowed with its own metric, respectively $U_{\alpha\beta}\left(\vec{u'}\right)=-u'_{\alpha}u'_{\beta}$and $P_{\alpha\beta}\left(\vec{u'}\right)=g_{\alpha\beta}+u'_{\alpha}u'_{\beta}$. Clearly,

$\displaystyle g_{\alpha\beta} = U_{\alpha\beta}\left({\vec u'}\right)+P_{\alpha\beta}\left({\vec u'}\right).$   (A.1)

The subspace with metric $P_{\alpha\beta}\left(\vec{u'}\right)$ is generated by lines (i.e. geodesics in a normal neighborhood) that are orthogonal to the world line of $\vec {u'}$ at P. This sub-space defines the rest-space of the observer $\vec {u'}$ at P and here one is allowed to measure proper lengths. The subspace with metric $U_{\alpha\beta}\left(\vec{u'}\right)$ is generated by lines that differ from that of $\vec {u'}$ by a new parameterization. In this subspace one measures the observer's proper time.

As a consequence of Eq. (A.1), the invariant interval between two events in space-time can be written as ${\rm d}s^{2}=P_{\alpha\beta}\left(\vec{u'}\right)~{\rm d}x^{\alpha}{\rm d}x^{\beta}+U_{\alpha\beta}\left(\vec{u'}\right)~{\rm d}x^{\alpha}{\rm d}x^{\beta}$, from which we are able to extract the measurements of infinitesimal spatial distances and time intervals taken by $\vec {u'}$ as, respectively,

$\displaystyle {\rm d}L_{\vec{u'}}=\sqrt{P_{\alpha\beta}\left(\vec{u'}\right){\rm d}x^{\alpha}{\rm d}x^{\beta}}$   (A.2)

and
$\displaystyle {\rm d}T_{\vec{u'}}=-c^{-1}u'_{\alpha}{\rm d}x^{\alpha}.$   (A.3)

Appendix B: Stellar observed direction and stellar aberration in GREM-like approaches

The pN/pM approaches (Klioner 2003; Kopeikin & Mashhoon 2002; Kopeikin & Schäfer 1999) transform the observed direction to the source ($\vec{s}$) into the BCRS spatial coordinate direction of the light ray at the point of observation with coordinates $x^{i}(t_{{\rm o}})\equiv x^{i}_{{\rm s}}$(see Fig. B.1). Now, paraphrasing Klioner (2003), the coordinate direction to the light source at $x^i_{{\rm s}}$is defined by the four-vector $p^{\alpha}=(1,p^{i})$, where $p^{i}=c^{-1}{\rm d}x^{i}/{\rm d}t$, xi, and t are the BCRS coordinates. But the coordinate components pi are not directly observable quantities; the observed vector towards the light source is the four-vector $s^{\alpha}=(1,s^{i})$, defined with respect to the local inertial frame of the observer. In the local frame:

$\displaystyle s^{i}=-\frac{{\rm d}\mathcal{X}^{i}}{{\rm d}\mathcal{X}^{0}}$ (B.1)

where $\mathcal{X}^{\alpha}$ are the coordinates in the CoMRS. Then to deduce the spatial direction pi from si an infinitesimal transformation $\mathcal{X}^{\alpha}(x^{\beta})$between CoMRS and BCRS is adopted, given by the formula
$\displaystyle {\rm d}\mathcal{X}^{\alpha}=\Lambda_{\beta}^{\alpha}{\rm d}x^{\beta}.$   (B.2)

\begin{figure} \par\includegraphics[width=8cm]{12691fg2} \end{figure} Figure B.1:

The vectors representing the light direction in the pM/pN approaches inside the near-zone of the solar system.

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From (B.2) the expression of si as a function of the spatial components pi is obtained:
$\displaystyle s^{i}=-\frac{\Lambda_{0}^{i}+\Lambda_{j}^{i}p^{j}}{\Lambda_{0}^{0}+\Lambda_{j}^{0}p^{j}}\cdot$   (B.3)

One can make Eq. (B.3) explicit by following the procedure reported in (Klioner & Kopeikin 1992) and adopting the IAU resolution B1.3 (Soffel et al. 2003). From the BCRS $\left(ct,x^{i}\right)$to the CoMRS ( $c\mathcal{T},\mathcal{X}^{i}$), the transformation between the time coordinates reads as
                          $\displaystyle \mathcal{T}$ = $\displaystyle t-c^{-2}[A(t)+\delta_{ij}v^{i}R_{{\rm s}}^{j}]$ (B.4)
    $\displaystyle +c^{-4}[B+\delta_{ij}B^{i}R_{{\rm s}}^{j}+\delta_{im}\delta_{jk}B^{ij}R_{{\rm s}}^{m}R_{{\rm s}}^{k}$  
    $\displaystyle +C(t,{\vec x})]+\mathcal{O}\left(c^{-5}\right),$  

and between the spatial coordinates as

                         $\displaystyle \mathcal{X}^{i}$ = $\displaystyle \left[\delta_{j}^{i}+c^{-2}\left(\frac{1}{2}v^{i}v_{j}+qF_{j}^{i}(t)+D_{j}^{i}(t)\right)\right]R_{{\rm s}}^{j}$  
    $\displaystyle +c^{-2}D_{jk}^{i}(t)R_{{\rm s}}^{j}R_{{\rm s}}^{k}+\mathcal{O}\left(c^{-4}\right).$ (B.5)

All the functions A,  B,  C,  D are defined in Klioner & Kopeikin (1992) or in IAU resolutions, and $ R_{{\rm s}}^{i}=x^{i}-x_{{\rm s}}^{i} $ are the coordinate displacements with respect to the center of mass of the satellite $x_{{\rm s}}^{i}$ in the BCRS, and finally $v^{i}={\rm d}x_{{\rm s}}^{i}/{\rm d}t $.

As reported in Klioner (2004), the attitude in GREM (SRS) is obtained by applying an orthogonal rotation matrix $\mathcal{R}_{i}^{a}$ to $\mathcal{X}^{i}$ in Eq. (B.5). At this stage the role of the SRS is equivalent to that of the $E_{\hat{a}}^{\beta}$s in Eq. (8).

If one keeps all the terms up to the order of 1 micro-arcsecond, the observed stellar direction si is transformed (in the CoMRS) into the unitary ``aberration-free'' direction ni=pi/p (where $p=\sqrt{p^{i}p_{i}}$):

                                   si = $\displaystyle -n^{i}+c^{-1}\left[\vec{n} \times \left(\vec{v} \times \vec{n}\right)\right]^{i}$  
    $\displaystyle +c^{-2}\left\{ (\vec{n}\cdot\vec{v})\left[\vec{n}\times\left(\vec... ...ac{1}{2}\left[\vec{v}\times\left(\vec{n}\times\vec{v}\right)\right]^{i}\right\}$  
    $\displaystyle +c^{-3}\left\{ \left[\left(\vec{v}\cdot\vec{n}\right)^{2}+ (2) w\... ...t)\right]\left[\vec{n}\times\left(\vec{v}\times\vec{n}\right)\right]^{i}\right.$  
    $\displaystyle \left.+\frac{1}{2}\left(\vec{n}\cdot\vec{v}\right)\left[\vec{v}\t... ...left(\vec{n}\times\vec{v}\right)\right]^{i}\right\} +\mathcal{O}\left(4\right).$ (6)

References

Footnotes

... zone[*]
The near zone of a system of bound sources, which generates no stationary gravitational field, is defined as the region of space with a size comparable to the wavelength of the gravitational radiation emitted by that system.
... equations''[*]
These equations derive from the null geodesic with the appropriate projection onto the rest-space of the local barycentric observer (de Felice et al. 2004,2006).
... resolutions[*]
These resolutions are based on the pN approximation, which is still compatible with RAMOD, since the perturbation $h_{\alpha\beta}$ to the Minkowskian metric in (1) can be calculated at any desired order of approximations in $\left(v/c\right)$ inside the Solar System.
... observation[*]
Also, each Eq. (8) is essential in RAMOD as it represents a boundary condition needed to uniquely solve the master equations.
Copyright ESO 2010

All Figures

  \begin{figure} \par\includegraphics[width=7.5cm,clip]{12691fg1.eps} \end{figure} Figure 1:

The local observer ${\vec u}$ with respect to the BCRS coordinate system. The spatial axes of the BCRS point toward distant sources. The dashed lines are the curves that are orthogonal, say $\vec{\eta}$, to the $t=\mbox{constant}$ hyper-surfaces, asymptotically orthogonal to the time direction. The rest-space (green area) of ${\vec u}$ locally deviates from the space-like hyper-surface with equation $t(x,y,z)={\rm constant}$by terms of the order of a micro-arcsecond.

Open with DEXTER
In the text

  \begin{figure} \par\includegraphics[width=8cm]{12691fg2} \end{figure} Figure B.1:

The vectors representing the light direction in the pM/pN approaches inside the near-zone of the solar system.

Open with DEXTER
In the text

Copyright ESO 2010

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