stellar model spectrum with the following parameter set: $T_\mathrm{eff}=5000$ K, $\log g=1.0$, and $Z=Z_\odot$. We applied this method to each of the following ranges in five echelle orders: 17500–17870 Å in the order $H32$, 16960–17340 Å in $H33$, 16460–16840 Å in $H34$, 15980–16150 Å in $H35$, and 15680–15840 Å in $H36$. In case of the $K$-band spectrum of GCC-a, the following five ranges are used: 23920–24480 Å in $K23$, 22920–23480 Å in $K24$, 22000–22560 Å in $K25$, 21160–21680 Å in $K26$, and 20460–20780 Å in $K27$. The telluric absorption lines distributed in these ranges ensure well-calibrated wavelength scales. These spectral ranges yielded consistent velocities (within a few ${{\mathrm{km~s}^{-1}}}$; see $\sigma _V$ in Table \[tab:vel\]), and the statistical error was estimated from the scattering in the measured velocities over the five ranges. The obtained velocities were then transformed into barycentric velocities, $V_{\rm bary}$, and velocities relative to the Local Standard of Rest (LSR), $V_{\rm LSR}$, assuming the standard solar motion [@Crovisier-1978; @Reid-2009].

![ Illustration of the method used to measure the radial velocities. A telluric spectrum constructed from an A-type star (1) was convolved with a model spectrum shifted by a trial velocity (2) to construct a synthesized spectrum (3). This 