The HARPS search for southern extra-solar planets XXXV. The interesting case of HD41248: stellar activity, no planets?

TL;DR

This study used HARPS data to investigate the existence of planets around the metal-poor star HD41248, finding that previously claimed planets are likely due to stellar activity rather than actual planetary signals.

Contribution

The paper presents a detailed analysis of radial velocity data for HD41248, challenging prior planet claims and exploring stellar activity as the source of observed signals.

Findings

No evidence for the previously announced planetary system.

The 25-day signal correlates with stellar rotation and activity.

The 18-day signal was not confirmed in new data.

Abstract

The search for planets orbiting metal-poor stars is of uttermost importance for our understanding of the planet formation models. However, no dedicated searches have been conducted so far for very low mass planets orbiting such objects. Only a few cases of low mass planets orbiting metal-poor stars are thus known. Amongst these, HD41248 is a metal-poor, solar-type star on which a resonant pair of super-Earth like planets has In the present paper we present a new planet search program that is using the HARPS spectrograph to search for Neptunes and Super-Earths orbiting a sample of metal-poor FGK dwarfs. We then present a detailed analysis of an additional 162 radial velocity measurements of HD41248, obtained within this program, with the goal of confirming the existence of the proposed planetary system. We analyzed the precise radial velocities, obtained with the HARPS spectrograph, together with several stellar activity diagnostics and line profile indicators. A careful analysis shows no evidence for the planetary system previously announced. One of the signals, with a period of about 25 days, is shown to be related to the rotational period of the star, and is clearly seen in some of the activity proxies. The remaining signal (P~18 days) could not be convincingly retrieved in the new data set. We discuss possible causes for the complex (evolving) signals observed in the data of HD41248, proposing that they may be explained by the appearance and disappearance of active regions on the surface of a star with strong differential rotation, or by a combination of the sparse data sampling and active region evolution.