consider the corresponding reddening vector in Figure \[HRDnew\_fig3.pdf\]. [The extinction data published in [[*Gaia*]{}]{}DR2 does not allow]{} to check [this option]{} as @2018arXiv180409374A mention in their paper. To summarize, we refrained from de-reddening the stars in the BS.

### Kinematic analysis {#kinematics}

To reveal the members of the potential moving group characterized by Eq. \[CPcoo\], we then studied the kinematics of the stars in the BS. Unfortunately, only about 12with a common space motion should have tangential velocities directed towards a convergent point, in our case defined by Eq. \[CPcoo\]. We computed the components of the observed tangential velocity parallel and perpendicular to the local vector in the direction of this convergent point by a simple rotation around an angle $\psi$ which we determine below.

We followed the formalism of the convergent point method as described, e.g. in and transformed the cartesian velocity vector of the group motion $\vec{V_c}$ from Eq.\[CPcoo\] by $$\left[\begin{array}{l}V_{c,\alpha,i} \\ 
V_{c,\delta,i} \\\end{array}\right] = 
\left[\begin{array}{rrr} -\sin\alpha_i & \cos\alpha_i & 0 \\ 
-\cos\alpha_i\sin\delta_i & -\sin\alpha_i\sin\delta_i & \cos\delta_i \\
\end{array}\right]
\,\cdot\,\vec{V_c}.
\label{equ:spacVel3}$$ With Eq. (8) from the angle $\psi$ is given as $\psi=\arctan(V_{c,\delta,i}/V_{c,\alpha,i})$, and the desired rotation reads $$\left[\begin{array}{l}v_{\parallel,i}\\
 v_{\bot,i}\\\end{array}\right] = 
\left[\begin{array}{rr} \cos\psi & \sin\psi \\
-\sin\psi & \cos\psi 