# K2-290: a warm Jupiter and a mini-Neptune in a triple-star system

## TL;DR

This paper reports the discovery and characterization of a triple-star system hosting a mini-Neptune and a warm Jupiter, providing insights into their formation and the system's architecture.

## Contribution

It presents the first detailed characterization of a system with a mini-Neptune and a warm Jupiter in a triple-star environment, including their orbital and physical properties.

## Key findings

- Mini-Neptune with 3.06 R_earth and 9.2-day orbit
- Warm Jupiter with 0.774 M_J and 48.4-day orbit
- System's architecture suggests in situ formation or disk migration

## Abstract

We report the discovery of two transiting planets orbiting K2-290 (EPIC 249624646), a bright (V=11.11) late F-type star residing in a triple-star system. It was observed during Campaign 15 of the K2 mission, and in order to confirm and characterise the system, follow-up spectroscopy and AO imaging were carried out using the FIES, HARPS, HARPS-N, and IRCS instruments. From AO imaging and Gaia data we identify two M-dwarf companions at a separation of $113 \pm 2$ AU and $2467_{-155}^{+177}$ AU. From radial velocities, K2 photometry, and stellar characterisation of the host star, we find the inner planet to be a mini-Neptune with a radius of $3.06 \pm 0.16 R_{\oplus}$ and an orbital period of $P = 9.2$ days. The radius of the mini-Neptune suggests that the planet is located above the radius valley, and with an incident flux of $F\sim 400 F_{\oplus}$, it lies safely outside the super-Earth desert. The outer warm Jupiter has a mass of $0.774\pm 0.047 M_{\rm J}$ and a radius of $1.006\pm 0.050R_{\rm J}$, and orbits the host star every 48.4 days on an orbit with an eccentricity $e<0.241$. Its mild eccentricity and mini-Neptune sibling suggest that the warm Jupiter originates from in situ formation or disk migration.