All Tables

Table 1: Estimated numerical error in longitude in INPOP06 (step size 0.055 day) for all planets i (i=3 stands for the Earth-Moon Barycenter, and i=10 for the Moon). The error $\varepsilon _i$ is given in microarcseconds ( $\mu$ as) or micrometers ( $\mu$ m) over 100 years and over 10 000 years.
Table 2: Maximum difference between DE405 and INPOP05 (with the same initial conditions) in range (r), latitude ( $\phi$ ) and longitude ( $\lambda$ ). If (x,y,z) are the heliocentric (geocentric for the Moon) coordinates of the planet in the equatorial reference frame of the ICRF, then $r=\sqrt {(x^2+y^2+z^2)}$ , $\phi = \arcsin (z/r)$ and $\lambda = \arctan(y/x)$ . EMB is the Earth-Moon Barycenter. For the librations of the Moon, $\phi$ , $\theta$ and $\psi$ are the usual Euler's angles (see Newhall et al. 1983, Sect. II.D). Comparisons are made over the whole time interval of DE405 (-400 yr to 200 yr with origin at J2000); Col. 1: from -30 yr to +30 yr; Col. 2: from -100 yr to +100 yr; Col. 3: from -400 yr to 200 yr.
Table 3: INPOP05 (Col. 5) residuals for each type of observations. Column 3 gives the time interval of observations and Col. 4 the number N of observations used in the fit and in the residual computations. For optical observations, the residuals are given respectively in right ascension and declination ( $\alpha$ ; $\delta$ ). The given uncertainties are at 1-sigma.
Table 4: Maximum difference between DE405 and INPOP06 in range (r), latitude ( $\phi$ ) and longitude ( $\lambda$ ). (x,y,z) are the heliocentric (geocentric for the Moon) coordinates of the planet in the equatorial reference frame of the ICRF, and $r=\sqrt {(x2+y2+z2)}$ , $\phi = \arcsin (z/r)$ and $\lambda = \arctan(y/x)$ . EMB is the Earth-Moon Barycenter. For the librations of the Moon, $\phi$ , $\theta$ and $\psi$ are the usual Euler's angles (see Newhall et al., section II.D). Comparisons are made over the whole time interval of DE405 (-400 yr to 200 yr with origin at J2000); Col. 1: from -30 yr to +30 yr; Col. 2: from -100 yr to +100 yr; Col. 3: from -400 yr to 200 yr.
Table 5: Parameters used in DE405 (and INPOP05) (Col. 2), and in INPOP06 (Col. 3), to compute the tidal effects (see Sects. 2.3.3 and 2.3.5) and the Earth orientation. $\tau _{E21}$ and $\tau _{E22}$ are respectively the Earth's time delays for harmonics (2, 1) and (2, 2), and $\tau _{\rm M}$ is the time delays for the Moon. They are expressed in days and rounded to 10^-10. C, M and R are respectively the maximum moment of inertia, the mass and the mean equatorial radius of the Earth.
Table 6: INPOP06 (Col. 5) residuals for each type of observation. Column 3 gives the observational time interval and Col. 4 the number of observations N used in the fit and in the residual computations. For optical observations, the residuals are given respectively in right ascension and declination ( $\alpha$ ; $\delta$ ). The uncertainties are at 1-sigma.
Table 7: Physical parameters fitted in INPOP06. Other values deduced from planetary ephemerides are presented for comparisons.The given uncertainties are given at 1-sigma.
Table 8: Solar oblateness and the PPN parameter $\beta$ determinations based on INPOP06 fit to observations. In the first column, the publications from where the values are extracted and the methods used to estimate the Sun J2 and the PPN parameters $\beta$ are given. In Cols. 2, 3 and 4, computed values of these parameters can be found.