). These results point toward high-eccentricity migration as the dominant formation mechanism for HJs. However, some HJs have been found to possess smaller close-in companions (e.g., Becker et al. 2015; Korth et al. 2023, 2024; Grieves et al. 2025). Additionally, analysis of transit timing variations found that 12 ± 6%
⋆Email:lthomas@mpe.mpg.de ⋆⋆ESO Fellow
Article number, page 1 of 14 of HJs might host nearby companions (Wu et al.

2023), indicating a more diverse formation and migration pathway. On the other hand, WJs are found to exist preferentially in multiplanet systems with nearby companions, pointing to more quiescent formation mechanisms (Wu et al. 2023). Measurements of the sky-projected stellar obliquity through the Rossiter-McLaughlin (RM) effect support these results. HJs orbiting cooler stars below the Kraft break are preferentially aligned, while planets around hot stars have a diverse obliquity distribution (Winn et al. 2010; Albrecht et al. 2022). These observations are consistent with high-eccentricity migration and the obliquity distribution being shaped by dissipative mechanisms (Rice et al. 2022a). Overall, WJs are preferentially found in aligned orbits (Rice et al. 2022b), supporting quiescent migration. The observed eccentricity distribution of WJs, however, paints a more diverse picture for their formation and migration, with a significant fraction (∼70%) of WJs exhibiting dynamically "hot" orbits (e > 0.1) (Dong et al. 2021a; Morgan et al. 2026). Some of the highly eccentric WJs, such as TOI-3362 b (Dong et al. 2021b) and TIC 241249530 b (Gupta et al. 2024), are expected to end up as HJs after circularization, and thus they can be considered proto-HJs. The population of eccentric WJs could come from stalled high-eccentricity migration, where the eccentricity was not excited to a degree high enough to bring the planet close to the star for the tidal forces to fully circularize the orbit. Alternatively, they could migrate through disk migration and then have their eccentricities excited later in their lifetime. The eccentricities of WJs have been found to correlate with host star metallicity, with metal-rich stars harboring more eccentric planets (Dawson & Murray-Clay 2013; Morgan et al. 2026). This correlation likely arises from the enhanced formation efficiency of giant planets in metal-rich disks, leading to increased dynamical interactions and eccentricity excitation (Santos et al. 2004; Fischer & Valenti 2005; Johnson et al. 2010). In this paper, we present the detection and characterization of the two WJs TOI-2147 b and TOI-6019 b, initially reported as planet candidates by the Transiting Exoplanet Survey Satellite (TESS). We obtained high-resolution spectroscopy observations using the Manfred Hirt Planet Finder Spectrograph (MaHPS) to confirm their planetary nature and measure precise masses. The structure of this paper is as follows. Section 2 describes the observations used to detect and characterize the new WJs. Sections 3 and 4 present the analysis and derivation of the stellar and planetary parameters. Section 5 discusses the properties of the two planets and places them within the population of known giant planets. Finally, Section 6 summarizes our conclusions.