© ESO, 2017

1. Introduction

The first Gaia data release (Gaia DR1; Gaia Collaboration 2016a) on 14 September 2016 provides astrometric parameters for nearly 2 million stars and positions for over 1 billion sources with improved accuracy, and leads to several improvements in fundamental astrometry, especially in the practical realization of the optical reference frame.

The definition and realization of the reference frame has been one of the main concerns for astrometry. The Gaia reference frame links directly to the extragalactic objects through the quasar observations, and surpasses the former Hipparcos reference frame in accuracy and inertia. The final Gaia celestial reference frame is supposed to reach a level of a few tens of micro-arcseconds (μas), similar to the International Celestial Reference Frame (ICRF). The Gaia-ICRF link will be important and has been used in the construction of the third generation of ICRF (ICRF3; for example, see Jacobs et al. 2014). A detailed analysis of the Gaia reference frame and ICRF should be performed to prepare for the future optical-radio link.

As a preliminary result of the Gaia reference frame, the Gaia DR1 reference frame has been aligned to ICRF better than 0.1 mas at epoch J2015.0 (Lindegren et al. 2016). Analysis of the Gaia DR1 reference frame can help to illustrate potential properties of the final Gaia reference frame. Detailed comparisons and analysis between Gaia DR1 with other catalogues have been performed in Lindegren et al. (2016) and Mignard et al. (2016), including the optical property of ICRF sources.

This work aims to provide an extra overall property analysis of the Gaia DR1 reference frame. We begin with some tests of the auxiliary quasar solution in Sect. 2. Then the analysis of the the joint Tycho-Gaia astrometric solution (TGAS) proper motion system have been performed in light of global rotation (Sect. 3), and Galactic kinematics (Sect. 4).

2. Overall analysis of the radio reference frame

2.1. Overall property of the auxiliary quasar solution

The auxiliary quasar solution in Gaia DR1 was used to align the Gaia DR1 reference frame to the second generation of ICRF (ICRF2) by a solid rotation (Lindegren et al. 2016, Eq. (5)). The available version contains 2191 ICRF2 sources with their positions in the Gaia DR1 reference frame. Mignard et al. (2016) provide a detailed comparison between the auxiliary quasar solution and the ICRF2 catalogue and find a systematical declination bias at the order of −0.1 mas.

The declination bias can be confirmed and then removed by adding a parameter dz to the declination component of the Eq. (5) in Lindegren et al. (2016), as performed in the alignment between ICRF1 and ICRF2 (Fey et al. 2015). As such, the equation for alignment can be written as (e.g. Feissel-Vernier et al. 2006):

$\begin{array}{ccc}& & \mathrm{\Delta }{\mathit{\alpha }}^{\mathrm{\ast }}\mathrm{=}\mathrm{-}{\mathit{ϵ}}_{\mathit{X}}\cos \mathit{\alpha }\sin \mathit{\delta }\mathrm{-}{\mathit{ϵ}}_{\mathit{Y}}\sin \mathit{\alpha }\sin \mathit{\delta }\mathrm{+}{\mathit{ϵ}}_{\mathit{Z}}\cos \mathit{\delta }\\ & & \end{array}$(1)where Δα^∗ = Δαcosδ. Parameters ϵ_X, ϵ_Y, and ϵ_Z are three relative rotation angles between two celestial reference frames around the X, Y, and Z axes and dz accounts for the systematical declination differences, which is caused by the possible inaccuracy of the tropospherical model, in the case of alignment between ICRF1 and ICRF2. The positional differences (Δα^∗, Δδ) between Gaia and ICRF2 is calculated based on Gaia−ICRF2. To verify the declination bias, we used four subsets: all 2191 sources, all 262 defining sources, 1929 non-defining sources, and 260 defining sources used for fixing the Gaia DR1 frame (two sources 0119+115 and 1823+568 are only used for the right ascension component). For comparison, we also estimated just the solid rotation between the auxiliary quasar solution and the ICRF2.

From the results of the least squares using Eq. (1) (Table 1), we can clearly see a declination bias dz~−0.1mas, as reported in Mignard et al. (2016). We note that the Gaia DR1 reference frame has been aligned to the ICRF2, and we should not expect any rotation components. The results for mutual orientations from the full samples are insignificant and small compared to the claimed value 0.1 mas in Lindegren et al. (2016), which meets expectations.

To obtain more insight of the systematic declination bias, we further only considered the sources in the northern and southern hemispheres, respectively. The result is presented in the last two rows in Table 1. On the one hand, both hemispheres yield a similar declination bias, which indicates that the systematic declination bias less possibly arises from the southern or northern declination offsets in the VLBI or Gaia data. On the other hand, although the obtained result that no orientation component is larger than 0.15 mas agrees with that in Lindegren et al. (2016), the signs of the orientation components from the northern and southern hemispheres are totally opposite, indicating possible regional deformations in the ICRF2 or Gaia DR1 reference frame. Limited by the small sample available, it is hard to obtain a clear explanation so far.

2.2. Galactic aberration effect on Gaia DR1 reference frame

Mignard et al. (2016) clearly claim that no models of the Galactic acceleration have been introduced in auxiliary quasar solution. The Galactic acceleration effect will be certainly removed in the final Gaia reference frame, but is not considered yet in present very long baseline interferometry (VLBI) data reductions. A possible effect on the reference frame owing to the Galactic acceleration should be estimated. In general, the Galactic acceleration of the solar system barycenter produces apparent proper motions for extragalactic sources, which results in a dipole pattern of apparent proper motions. This is called the Galactic aberration effect (Malkin 2011). In addition, the celestial reference frame, based on the subset of extragalactic sources, has some systematic effects, such as global rotation and deformation, which results from the apparent proper motions. Recently Malkin (2016) took the Galactic aberration effect into consideration and provided possible methods to create a future link of the Gaia reference frame with the next generation of ICRF.

We estimated the accumulated orientation difference from the global rotation due to the Galactic aberration effect over the J2000.0–J2015.0 period. We note that the small orientation offset depends on the distribution of extragalactic sources (Liu et al. 2012). Four subsets in Table 1 are tested to evaluate the possible orientation offsets of the celestial reference frame owing to the Galactic aberration effect. The orientation offset was denoted as three rotation angles Δϵ_X, Δϵ_Y, and Δϵ_Z around the X, Y, and Z axes of the celestial reference frame. We adopted the apex of the dipole pattern as the Galactic center and the Galactic aberration constant A=5μas yr^-1 to obtain the apparent proper motions of extragalactic sources. Based on this, we then estimated the global rotation of the celestial reference frame. Afterwards, the orientation offset was obtained by multiplying the global rotation by the 15-yr epoch span (J 2000.0–J 2015.0).

Table 2 reports the influence of the Galactic aberration effect on the Gaia DR1 reference frame. We found no significant components except for Δϵ_x~ 0.01 mas, which would cause a displacement of the Z axis and should possibly be taken into consideration in the final Gaia-ICRF alignment.

3. Global rotation between TGAS and Tycho-2 proper motions

The Hipparcos reference frame is estimated to rotate with respect to the Gaia DR1 reference frame at a rate of 0.24 mas yr^-1, and this rotation can be represented by a vector ω ≃ (−0.126, + 0.185, + 0.076)^Tmas yr^-1 (Lindegren et al. 2016). The Tycho-2 catalogue contains position and proper motion data for 2.5 million brightest stars, referring to the Hipparcos reference frame (Høg et al. 2000). The joint Tycho-Gaia astrometric solution (TGAS; Michalik et al. 2015) provides astrometric parameters for stars common in the Tycho-2 catalogue in the frame of the Gaia DR1 reference frame. Therefore, in a global sense, the Tycho-2 proper motion system should differ from the TGAS proper motion system by a global rotation that may be not totally consistent with, but comparable to, ω in the magnitude. Lindegren et al. (2016) compared the TGAS positions and proper motions with the Hipparcos and Tycho-2 catalogues for individual sources, but did not consider the global difference between the proper motion systems. This motivated us to perform further analysis of the overall difference between the Tycho-2 and TGAS proper motion systems.

In Gaia DR1, all sources were treated as single stars. Any astrometric effects due to the orbital motion in binaries or the perspective acceleration were ignored. As a result, for the binaries, multiples, and suspected non-single systems, the nonlinear motion of the photo-centre may cause an instantaneous proper motion. To avoid these distortions in the proper motion system, we only considered single stars in the Tycho-2 catalogue (the flag “posflg” is set as ⊔¹) and hence we obtained a sample of 1 969 315 single stars that are common to TGAS and the Tycho-2 catalogues.

To exclude the effect of color-dependent errors in the proper motion systems (Gaia Collaboration 2016b), we divided the stars into three groups: all stars, the O-B5 stars (young stars, age older than 3×10⁷ yr to reject the stars in the Gould belt), and the K-M giants (luminosity class III). These classifications need further information on the MK spectral types and the luminosity classes, which is provided in the Tycho-2 Spectral Type Catalog (Wright et al. 2003). By cross-identification, we obtained a group of 5479 O–B5 stars and 32 242 K–M giants.

The global rotation between TGAS and Tycho-2 can be determined by the least squares fit, using the following equations:

$\begin{array}{ccc}& & \mathrm{\Delta }{\mathit{\mu }}_{{\mathit{\alpha }}^{\mathrm{\ast }}}\mathrm{=}\mathrm{-}{\mathit{\omega }}_{\mathit{X}}^{\mathrm{\prime }}\cos \mathit{\alpha }\sin \mathit{\delta }\mathrm{-}{\mathit{\omega }}_{\mathit{Y}}^{\mathrm{\prime }}\sin \mathit{\alpha }\sin \mathit{\delta }\mathrm{+}{\mathit{\omega }}_{\mathit{Z}}^{\mathrm{\prime }}\cos \mathit{\delta }\\ & & \end{array}$(2)where μ_α^∗ = μ_αcosδ. The vector ${{\omega }}^{\mathrm{\prime }}\mathrm{=}\mathrm{(}{\mathit{\omega }}_{\mathit{X}}^{\mathrm{\prime }}\mathit{,}{\mathit{\omega }}_{\mathit{Y}}^{\mathrm{\prime }}\mathit{,}{\mathit{\omega }}_{\mathit{Z}}^{\mathrm{\prime }}{\mathrm{)}}^{\mathrm{T}}$ represents the spin between the two celestial reference frames, taken in the sense Tycho-2 − TGAS. The 2.6σ principle was introduced in the least squares to exclude the outlier proper motions.

From the results in Table 3, we found no obvious global rotations for all and M–K giants, and a relatively large ${\mathit{\omega }}_{\mathit{Y}}^{\mathrm{\prime }}$ component for the group of the O–B5 stars. However, none of them has a magnitude exceeding 0.10 mas yr^-1. The global rotation ω′ in Table 3, by directly comparing the stellar proper motions, is much smaller than the value (0.24 mas yr^-1), which was obtained by combining the stellar positions at J1991.25 with the quasar positions at J2015.0 (Lindegren et al. 2016). The Tycho-2 proper motions are derived by incorporating the original Tycho-1 catalogue (ESA 1997) with century-old ground-based catalogues, and thus contain systematic errors from old data, possibly responsible for the inconsistency.

Then we compared the TGAS proper motions with the revised Hipparcos proper motions, using the same method as for the Tycho-2 catalogue. The revised Hipparcos catalogue (van Leeuwen 2007) is a new reduction of the astrometric data of the Hipparcos mission with improved accuracies for astrometric parameters, compared with the original catalogue, and the reference frame remains the same as for the old Hipparcos catalogue. Unlike the Tycho-2 proper motions, the revised Hipparcos proper motions contain no systematic errors from old ground-based catalogues. Thus the comparison between TGAS and the revised Hipparcos proper motions were supposed to yield a reliable global rotation vector. The results obtained from different samples (Table 4) yielded similar global rotation components to those in Table 3, indicating that the systematic errors from the old data in Tycho-2 catalogue should not be responsible for the inconsistency between ω and ω′.

To illustrate possible causes, we need further investigations of the TGAS proper motions. In the following section, we analyzed the kinematics property of the Milky Way using the TGAS proper motion to deepen our understanding of the Gaia DR1 reference frame.

4. Property of Gaia DR1 reference frame inferred from Galactic kinematics analysis

4.1. Analytic strategy

The proper motion system of a catalogue not only reflects the inertial characteristic of the stellar reference frame, but also critically affects the analysis on the kinematics and dynamics of the Galaxy (Zhu 2007). The Gaia DR1 reference frame is an ideally rigid and inertial reference frame with respect to the extragalactic objects, so that the observed stellar proper motions in this reference frame are the sum of the following three terms except for the observational errors:

• 1.

  the stellar peculiar motion;

• 2.

  the solar peculiar motion (the origin of the reference frame is set on the solar system barycenter);

• 3.

  the Galactic rotation.

The stellar peculiar motion is always considered as an ellipsoidal velocity distribution and statistically treated as the random variables with zero mean. If one uses the TGAS proper motions of a specific group of stars and performs the kinematical analysis of the Galaxy, the solution should be compatible with the results obtained by the physical theories or models to within uncertainties.

The sample of K-M giants, one of the old and well-relaxed populations of stars, is supposed to be a steady-state constituent of the Galaxy. This stellar ensemble should exhibit only the familiar in-plane galactic rotation (described by the Oort constants A and B; Miyamoto & Soma 1993) in an ideal inertial reference frame. The unexplained motion of stars should be attributed to possible problems of the current Galactic kinematical model or the Gaia DR1 reference frame.

4.2. Materials and results

To investigate the property of the reference frame, we adopted the Ogorodmikov–Milne model (Milne 1935), in which the stellar proper motion field in the solar neighborhood can be described by $\left(\begin{array}{c}\\ {\mathit{\mu }}_{\mathit{l}}\cos \mathit{b}\\ {\mathit{\mu }}_{\mathit{b}}\end{array}\right)\mathrm{=}\mathrm{ℳ}\mathit{X,}$(3)where ℳ is a 2 × 9 matrix consisting of known trigonometric functions of the galactic coordinates of stars. The vector X can be given by the following equation: ${{X}}^{\mathrm{T}}\mathrm{=}\mathrm{(}{\mathit{S}}_{\mathrm{1}}\mathit{,}{\mathit{S}}_{\mathrm{2}}\mathit{,}{\mathit{S}}_{\mathrm{3}}\mathit{,}{\mathit{D}}_{\mathrm{32}}^{\mathrm{-}}\mathit{,}{\mathit{D}}_{\mathrm{13}}^{\mathrm{-}}\mathit{,}{\mathit{D}}_{\mathrm{21}}^{\mathrm{-}}\mathit{,}{\mathit{D}}_{\mathrm{12}}^{\mathrm{+}}\mathit{,}{\mathit{D}}_{\mathrm{13}}^{\mathrm{+}}\mathit{,}{\mathit{D}}_{\mathrm{23}}^{\mathrm{+}}{\mathrm{)}}^{\mathrm{T}}\mathit{,}$(4)where the unknowns can be divided into three components: the solar peculiar motion (S₁,S₂,S₃)^T, the Galactic rigid rotation $\mathrm{(}{\mathit{D}}_{\mathrm{32}}^{\mathrm{-}}\mathit{,}{\mathit{D}}_{\mathrm{13}}^{\mathrm{-}}\mathit{,}{\mathit{D}}_{\mathrm{21}}^{\mathrm{-}}{\mathrm{)}}^{\mathrm{T}}$, and the Galactic differential rotation $\mathrm{(}{\mathit{D}}_{\mathrm{23}}^{\mathrm{+}}\mathit{,}{\mathit{D}}_{\mathrm{13}}^{\mathrm{+}}\mathit{,}{\mathit{D}}_{\mathrm{12}}^{\mathrm{+}}{\mathrm{)}}^{\mathrm{T}}$. The rotation components ${\mathit{D}}_{\mathrm{12}}^{\mathrm{+}}$ and ${\mathit{D}}_{\mathrm{21}}^{\mathrm{-}}$ are equivalent to the Oort constants A and B in the two-dimensional case.

The initial sample of K-M giants is the same as that in Sect. 3 (32 242 K–M giants in Table 3). In the next step, we rejected 89 objects with the negative parallax and 4 425 with the relative parallax uncertainty larger than 30%. Then we set limits for the heliocentric distance r and the galactic height z: $\mathrm{0.2}\hspace{0.17em}\mathrm{kpc}\mathrm{\le }\mathit{r}\mathrm{\le }\mathrm{1.0}\hspace{0.17em}\mathrm{kpc}\mathit{,} \mathrm{\left|}\mathit{z}\mathrm{\right|}\mathrm{\le }\mathrm{0.5}\hspace{0.17em}\mathrm{kpc}\mathit{.}$(5)The upper limit of 1 kpc for r was set, since the Ogorodmikov–Milne model is the first order Taylor expansion near the Sun. In the solar vicinity, the velocity dispersions may dominate the proper motion field rather than the systematic motion owing to the small distance, so that a lower limit of 0.2 kpc was set for r to avoid this effect. A maximum of 0.5 kpc for z was set to keep the stars in the thick disk. As a result, we obtained a sample of 23 612 K–M giants in this step.

Fig. 1 Distribution of the sample of all K–M III giants on XG–YG plane of Galactic coordinate. Blue points represent the stars accepted by Eq. (5), while red points stand for the rejected ones.

Figure 1 gives the sample distribution in X_G–Y_G plane of the galactic coordinate system. One can clearly see an inhomogeneous distribution, which may arise from the incompleteness of the spectral catalog and property of the scanning law in the Gaia observation.

To test the possible influence of the inhomogeneous distribution of the sample on determining the vector X, we set different lower limits for r and obtained different samples. Then we applied the least squares to Eq. (3) with different star samples. The results are given as solution A to D in Table 5 for samples with different lower limits of r. The circular rotation velocity V₀ at the Sun was obtained by combining the rotational components ${\mathit{D}}_{\mathrm{21}}^{\mathrm{-}}$ and ${\mathit{D}}_{\mathrm{12}}^{\mathrm{+}}$ and adopting the solar distance to the Galactic center R₀ = 8.34 kpc (Reid et al. 2014). The determination of the solar peculiar motion and the Oort’s constants ${\mathit{D}}_{\mathrm{12}}^{\mathrm{+}}$ and ${\mathit{D}}_{\mathrm{21}}^{\mathrm{-}}$ was robust, leading to a relatively stable value of V₀, which is consistent with the result 240 ± 8km s^-1 in Reid et al. (2014). The rotational components ${\mathit{D}}_{\mathrm{13}}^{\mathrm{-}}$ and ${\mathit{D}}_{\mathrm{13}}^{\mathrm{+}}$ around the Y_G axis seemed to be non-zero, while the components ${\mathit{D}}_{\mathrm{32}}^{\mathrm{-}}$ and ${\mathit{D}}_{\mathrm{23}}^{\mathrm{+}}$ around the X_G axis were estimated to be zero within the standard error in most cases.

We then applied a constraint ${\mathit{D}}_{\mathrm{32}}^{\mathrm{-}}\mathrm{=}\mathrm{0}\mathit{,}{\mathit{D}}_{\mathrm{23}}^{\mathrm{+}}\mathrm{=}\mathrm{0}$ in the least squares and the number of parameters to be determined in Eq. (4) became seven. The results are shown as solution E in Table 5. Only the result of sample with 0.2 kpc ≤ r ≤ 1.0 kpc is given; other samples yield similar results. Compared with the result solution A without any constraint (see Row 1 in Table 5), we found very little difference and hence considered that the constraint is reasonable. In other words, no obvious ${\mathit{D}}_{\mathrm{13}}^{\mathrm{-}}$ and ${\mathit{D}}_{\mathrm{13}}^{\mathrm{+}}$ components could be found from the TGAS K–M giant proper motions. In contrast, the non-zero Galactic rotational components around the Y_G axis might exist and the solution E gives

$\begin{array}{ccc}& & {\mathit{\omega }}_{{\mathit{Y}}_{\mathrm{G}}}\mathrm{=}{\mathit{D}}_{\mathrm{13}}^{\mathrm{-}}\mathrm{=}\mathrm{-}\mathrm{0.38}\mathrm{\pm }\mathrm{0.15}\hspace{0.17em}\mathrm{mas}\hspace{0.17em}\mathrm{y}{\mathrm{r}}^{-1}\\ & & \end{array}$(6)Gaia Collaboration (2016a) point out that the Gaia DR1 parallax system have a systematic error of ~0.3 mas, which were validated by Stassun & Torres (2016) and Jao et al. (2016), respectively. To test the possible influence of the parallax systematic error on our results, we enlarged the parallax, i.e. by a factor of 110% or 120%, and performed the same least squares fits. The test we performed indicated that changes in parallax affected the determination of the solar peculiar motion and the Oort’s constants but not the other Galactic rotational components such as ${\mathit{D}}_{\mathrm{13}}^{\mathrm{-}}$ and ${\mathit{D}}_{\mathrm{13}}^{\mathrm{+}}$.

4.3. Possible residual rotation of the Gaia DR1 reference frame

Assuming that the Galactic rotations around the X_G and Z_G axis were well determined and taking only the two non-zero components ω_YG and ${\mathit{\omega }}_{{\mathit{Y}}_{\mathrm{G}}}^{\mathrm{\prime }}$ into consideration, the possible residual rotation of the reference frame in equatorial coordinates can be calculated: $\left(\begin{array}{c}\\ {\mathit{\omega }}_{\mathrm{1}}\\ {\mathit{\omega }}_{\mathrm{2}}\\ {\mathit{\omega }}_{\mathrm{3}}\end{array}\right)\mathrm{=}{\mathrm{𝒩}}_{\mathrm{J}\mathrm{2000}}^{\mathrm{T}}\left(\begin{array}{c}\\ \mathrm{0}\\ {\mathit{\omega }}_{{\mathit{Y}}_{\mathrm{G}}}\\ \mathrm{0}\end{array}\right)\mathrm{=}\left(\begin{array}{c}\\ -0.19\\ \mathrm{+}\mathrm{0.17}\\ -0.28\end{array}\right)\hspace{0.17em}\mathrm{mas}\mathrm{y}{\mathrm{r}}^{-1}$(7)$\left(\begin{array}{c}\\ {\mathit{\omega }}_{\mathrm{1}}^{\mathrm{\prime }}\\ {\mathit{\omega }}_{\mathrm{2}}^{\mathrm{\prime }}\\ {\mathit{\omega }}_{\mathrm{3}}^{\mathrm{\prime }}\end{array}\right)\mathrm{=}{\mathrm{𝒩}}_{\mathrm{J}\mathrm{2000}}^{\mathrm{T}}\left(\begin{array}{c}\\ \mathrm{0}\\ {\mathit{\omega }}_{{\mathit{Y}}_{\mathrm{G}}}^{\mathrm{\prime }}\\ \mathrm{0}\end{array}\right)\mathrm{=}\left(\begin{array}{c}\\ -0.14\\ \mathrm{+}\mathrm{0.13}\\ -0.22\end{array}\right)\hspace{0.17em}\mathrm{mas}\mathrm{y}{\mathrm{r}}^{-1}\mathit{,}$(8)where is the commonly used equatorial-to-Galactic transformation matrix, i.e. adopted in ESA (1997).

However, the determination of unknowns is limited by the sample. The sample of all the available K–M giants yields the inhomogeneous and anisotropic distribution on the X_G–Y_G plane (as seen from Fig. 1). Additionally, the Tycho-2 Catalogue is complete at a magnitude of about V~ 11.0, therefore the sample we obtained is a subsample of bright K–M giants. Table 6 reports the correlation coefficients in solution E. We find a strong correlation between the solar peculiar motion and the Galactic rotation (i.e. S₁ and ${\mathit{D}}_{\mathrm{21}}^{\mathrm{-}}$), which might be caused by the limitation of the sample. Hence the residual rotations that were obtained here require further investigations.

5. Conclusions

In this paper, we present a detailed analysis of the overall properties of the Gaia DR1 reference frame. Initially, we validated the declination bias of ~−0.1 mas in Gaia auxiliary quasar solution with respect to the ICRF2 and find that the systematic declination bias exists in both northern and southern hemispheres. The Galactic aberration effect is thought to produce an offset ~0.01 mas of the Z axis over the J2000.0–J2015.0 period, which should be taken into consideration in the future Gaia-ICRF link. All the tests indicate that Gaia DR1 reference frame is well aligned to ICRF2 and a quasi-inertial reference frame with respect to extragalactic objects.

To compare the TGAS with Tycho-2 proper motion systems, we picked out single stars from the Tycho-2 catalogue, divided them into three groups according to the spectral types and luminosity classes, and determined the global rotation of the Hipparcos reference frame relative to the Gaia DR1 reference frame by a least squares fit. Although different samples give different values for global rotation (Tables 3 and 4), the magnitude of global rotation obtained is much smaller than 0.24 mas yr^-1 in Lindegren et al. (2016).

The kinematical analysis of the TGAS K-M giant proper motions gives consistent results of the solar peculiar motion and Oort constants to those in literature. But we found possible non-zero components of Galactic rotation (the rigid rotation component ω_YG and the differential rotation component ${\mathit{\omega }}_{{\mathit{Y}}_{\mathrm{G}}}^{\mathrm{\prime }}$), which were non-negligible in our solution. This result indicates a possible residual rotation in the Gaia DR1 reference frame or problems in the current Galactic kinematical model. However, owing to the limitation of the sample domain, the result is not robust at present. Here we call attention to the possible residual rotation presented in this work, which should be carefully examined in later studies and the future Gaia data release.

Acknowledgments

The authors are grateful to Dr Zacharias, who provided very useful comments and suggestions to improve the manuscript. This research is funded by the National Natural Science Foundation of China (NSFC) under grant No. 11473013. This work made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC was provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France.

References

All Tables

All Figures

	Fig. 1 Distribution of the sample of all K–M III giants on XG–YG plane of Galactic coordinate. Blue points represent the stars accepted by Eq. (5), while red points stand for the rejected ones.
In the text