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

TL;DR

This paper reports the discovery of a long-period, highly eccentric substellar companion to the evolved intermediate-mass star HD 14067, using precise Doppler measurements, indicating a giant planet with one of the highest known eccentricities around such stars.

Contribution

First detection of a long-period, eccentric substellar companion orbiting an evolved intermediate-mass star using Doppler spectroscopy.

Findings

Companion has a minimum mass around 8-9 Jupiter masses.

Orbit has a high eccentricity of approximately 0.53 to 0.70.

The orbital period is approximately 1455 to 2850 days.

Abstract

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.