# 4.3.3 Astrometric source model

Author(s): Lennart Lindegren

The astrometric model is a recipe for calculating the proper direction ${\bm{u}}_{i}(t)$ to a source ($i$) at an arbitrary time of observation ($t$) in terms of its astrometric parameters ${\bm{s}}_{i}$ and various auxiliary data, assumed to be known with sufficient accuracy. The auxiliary data include an accurate barycentric ephemeris of the Gaia satellite, ${\bm{b}}_{\text{G}}(t)$, including its coordinate velocity $\text{d}{\bm{b}}_{\text{G}}/\text{d}t$, and ephemerides of all other relevant solar-system bodies. The details of the model have been outlined in Section 3.2 of Lindegren et al. (2012) or Section 4.1.4 and only a short introduction is given here.

As explained in Section 4.1.3, the astrometric parameters refer to the ICRS and the time coordinate used is TCB. The reference epoch ${t}_{\text{ep}}$ is preferably chosen to be near the mid-time of the mission in order to minimize statistical correlations between the position and proper motion parameters.

The transformation between the kinematic and the astrometric parameters is non-trivial (Klioner 2003a), mainly as a consequence of the practical need to neglect most of the light-propagation time $t-{t}_{*}$ between the emission of the light at the source (${t}_{*}$) and its reception at Gaia ($t$). This interval is typically many years and its value, and rate of change (which depends on the radial velocity of the source), will in general not be known with sufficient accuracy to allow modelling of the motion of the source directly in terms of its kinematic parameters according to Equation 4.1. The proper motion components ${\mu}_{\alpha *i}$, ${\mu}_{\delta i}$ and radial velocity ${v}_{ri}$ correspond to the ‘apparent’ quantities discussed by in Sect. 8 of Klioner (2003a).

The coordinate direction to the source at time $t$ is calculated with the same ‘standard model’ as was used for the reduction of the Hipparcos observations (ESA (1997), Vol. 1, Sect. 1.2.8), namely

$${\overline{\bm{u}}}_{i}(t)=\u27e8{\bm{r}}_{i}+({t}_{\text{B}}-{t}_{\text{ep}})({\bm{p}}_{i}{\mu}_{\alpha *i}+{\bm{q}}_{i}{\mu}_{\delta i}+{\bm{r}}_{i}{\mu}_{ri})-{\varpi}_{i}{\bm{b}}_{\text{G}}(t)/{A}_{\text{u}}\u27e9$$ | (4.100) |

where the angular brackets signify vector length normalization, and $[{\bm{p}}_{i}{\bm{q}}_{i}{\bm{r}}_{i}]$ is the ‘normal triad’ of the source with respect to the ICRS (Murray 1983). In this triad, ${\bm{r}}_{i}$ is the barycentric coordinate direction to the source at time ${t}_{\text{ep}}$, ${\bm{p}}_{i}=\u27e8\bm{Z}\times {\bm{r}}_{i}\u27e9$, and ${\bm{q}}_{i}={\bm{r}}_{i}\times {\bm{p}}_{i}$. The components of these unit vectors in the ICRS are given by the columns of the matrix

$${\U0001d5a2}^{\prime}[{\bm{p}}_{i}{\bm{q}}_{i}{\bm{r}}_{i}]=\left[\begin{array}{ccc}\hfill -\mathrm{sin}{\alpha}_{i}\hfill & \hfill -\mathrm{sin}{\delta}_{i}\mathrm{cos}{\alpha}_{i}\hfill & \hfill \mathrm{cos}{\delta}_{i}\mathrm{cos}{\alpha}_{i}\hfill \\ \hfill \mathrm{cos}{\alpha}_{i}\hfill & \hfill -\mathrm{sin}{\delta}_{i}\mathrm{sin}{\alpha}_{i}\hfill & \hfill \mathrm{cos}{\delta}_{i}\mathrm{sin}{\alpha}_{i}\hfill \\ \hfill 0\hfill & \hfill \mathrm{cos}{\delta}_{i}\hfill & \hfill \mathrm{sin}{\delta}_{i}\hfill \end{array}\right].$$ | (4.101) |

${\bm{b}}_{\text{G}}(t)$ is the barycentric position of Gaia at the time of observation, and ${A}_{\text{u}}$ the astronomical unit. ${t}_{\text{B}}$ is the barycentric time obtained by correcting the time of observation for the Römer delay; to sufficient accuracy it is given by

$${t}_{\text{B}}=t+{\bm{r}}_{i}^{\prime}{\bm{b}}_{\text{G}}(t)/c,$$ | (4.102) |

where $c$ is the speed of light. See Section 3.2 of Lindegren et al. (2012) for further details.

The iterative updating of the sources is described in Section 5.1 of Lindegren et al. (2012). There the method of identifying potential outliers and estimating the excess source noise ${\u03f5}_{i}$ is also outlined together with the calculation of the partial derivatives of the coordinate direction with respect to the source parameters.

The perspective acceleration modelled by ${\mu}_{r}={v}_{r}\varpi /{A}_{\text{u}}$ in Equation 4.100 is totally negligible for the vast majority of sources, and ${\mu}_{r}=0$ (at the reference epoch) is therefore normally assumed, equivalent ${v}_{r}=0$. For Gaia DR3 we used the radial velocity from the RVS instrument (as given in Gaia DR2), complemented by values from the literature for the 38 sources listed in Table 4.3. The accumulated effect over a time interval $T$ is $\mathrm{\Delta}=|{v}_{r}|\mu \varpi {T}^{2}/{A}_{\text{u}}$, where $\mu ={({\mu}_{\alpha *}^{2}+{\mu}_{\delta}^{2})}^{1/2}$ is the total proper motion and ${A}_{\text{u}}=977792221.680789$ mas yr km s${}^{-1}$ is the astronomical unit. The largest effect, $\mathrm{\Delta}\simeq 4.9$ mas (for $T=2.76$ yr), is obtained for Barnard’s star (Gaia DR3 4472832130942575872).

Source identifier | HIP | ${v}_{r}$ |

[km s${}^{-1}$] | ||

Gaia DR3 222749343414443648 | 16209 | $-$173.0 |

Gaia DR3 470826482637310080 | 21088 | 27.9 |

Gaia DR3 762815470562110464 | 54035 | $-$84.69 |

Gaia DR3 778947814402602752 | 54211 | 68.89 |

Gaia DR3 1129149723913123456 | 57544 | $-$111.65 |

Gaia DR3 1364668825433435776 | 84140 | $-$30.1 |

Gaia DR3 1364668825433448704 | 84140 | $-$30.1 |

Gaia DR3 1364668825433454848 | 84140 | $-$30.1 |

Gaia DR3 1364668825435187840 | 84140 | $-$30.1 |

Gaia DR3 1637645127018395776 | 86162 | $-$28.58 |

Gaia DR3 1872046609345556480 | 104214 | $-$65.74 |

Gaia DR3 2007876324466455040 | 110893 | $-$33.94 |

Gaia DR3 2007876324472098432 | 110893 | $-$33.94 |

Gaia DR3 2261614264931057664 | 96100 | 26.78 |

Gaia DR3 2306965202564744064 | 439 | 25.38 |

Gaia DR3 2358524597030794112 | 5643 | 28.09 |

Gaia DR3 2452378776434477184 | 8102 | $-$16.68 |

Gaia DR3 2552928187080872832 | 3829 | 263.0 |

Gaia DR3 3139847906307949696 | 36208 | 18.22 |

Gaia DR3 3195919528989223040 | 19849 | $-$42.32 |

Gaia DR3 3340477717172813568 | 26857 | 105.83 |

Gaia DR3 3796072592206250624 | 57548 | $-$31.09 |

Gaia DR3 4268226078065241600 | 94349 | $-$42.4 |

Gaia DR3 4472832130942575872 | 87937 | $-$110.51 |

Gaia DR3 4810594479418041856 | 24186 | 245.19 |

Gaia DR3 4847957293278177024 | 15510 | 87.4 |

Gaia DR3 4937000898856156288 | 10138 | 57.0 |

Gaia DR3 5339892367684811520 | 55042 | $-$35.0 |

Gaia DR3 5690980582306104448 | 48336 | 61.6 |

Gaia DR3 5853498713190525696 | 70890 | $-$22.4 |

Gaia DR3 5918660719983560192 | 86990 | $-$115.0 |

Gaia DR3 5955305209191546112 | 86214 | $-$60.0 |

Gaia DR3 6228695270698475392 | 72511 | $-$39.6 |

Gaia DR3 6232511675556408320 | 73182 | 35.63 |

Gaia DR3 6254033894121581952 | 76901 | 84.92 |

Gaia DR3 6378584028690858496 | 113229 | 46.6 |

Gaia DR3 6583272171336048640 | 105090 | 20.11 |

Gaia DR3 6894054664842632448 | 106255 | $-$57.7 |