A Long-period Eccentric Substellar Companion to the Evovled Intermediate-Mass Star HD 14067

We report the detection of a substellar companion orbiting an evolved intermediate-mass ($M_{\star }=2.4M_{\odot }$) star HD 14067 (G9 III) using precise Doppler technique. Radial velocities of this star can be well fitted either by a periodic Keplerian variation with a decreasing linear velocity trend (P=1455 days, $K_1=92.2$ m s${}^{-1}$, $e=0.533$, and $\dot{\gamma }=-22.4$ m s${}^{-1}$ yr${}^{-1}$) or a single Keplerian orbit without linear trend (P=2850 days, $K_1=100.1$ m s${}^{-1}$, and $e=0.697$). The minimum mass ($m_2\sin i=7.8M_{\mathrm{J}}$ for the model with a linear trend, or $m_2\sin i=9.0M_{\mathrm{J}}$ for the model without a linear trend) suggests a long-period giant planet around an evolved intermediate-mass star. The eccentricity of the orbit is among the highest known for planets ever detected around evolved stars.