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 (\(M_\star=2.4\,M_\odot\)) 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 (\(m_2\sin{i}=7.8\,M_{\rm J}\) for the model with a linear trend, or \(m_2\sin{i}=9.0\,M_{\rm J}\) 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.