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We report the discovery and characterization of three new transiting giant planets orbiting TOI-6628, TOI-3837 and TOI-5027, and one new warm sub-Saturn orbiting TOI-2328, whose transits events were detected in the lightcurves of the Transiting Exoplanet Survey Satellite (TESS) space mission. By combining TESS lightcurves with ground-based photometric and spectroscopic follow-up observations we confirm the planetary nature of the observed transits and radial velocity variations. TOI-6628~\\(b\\) has a mass of 0.75\\(\\)0.06~\\(M_J\\), a radius of 0.98\\(\\)0.05~\\(R_J\\) and is orbiting a metal-rich star with a period of 18.18424\\(0.00001\\) days and an eccentricity of 0.667\\(0.016\\), making it one of the most eccentric orbits of all known warm giants. TOI-3837~\\(b\\) has a mass of 0.59\\(\\)0.06~\\(M_J\\), a radius of 0.96\\(\\)0.05~\\(R_J\\) and orbits its host star every 11.88865\\(\\)0.00003~days, with a moderate eccentricity of 0.198\\(^+0.046_-0.058\\). With a mass of 2.01\\(\\)0.13~\\(M_J\\) and a radius of 0.99\\(^+0.07_-0.12\\) \\(R_J\\), TOI-5027~\\(b\\) orbits its host star in an eccentric orbit with \\(e\\)~=~0.395\\(^+0.032_-0.029\\) every 10.24368\\(0.00001\\)~days. TOI-2328~\\(b\\) is a Saturn-like planet with a mass of 0.16\\(\\)0.02~\\(M_J\\) and a radius of 0.89\\(\\)0.04~\\(R_J\\), orbiting its host star in a nearly circular orbit with \\(e\\)~=~0.057\\(^+0.046_-0.029\\) at an orbital period of 17.10197\\(0.00001\\) days. All four planets have orbital periods above 10 days, and our planet interior structure models are consistsent a rocky-icy core with a H/He envelope, providing evidence supporting the core accretion model of planet formation for this kind of planets.

We report the discovery and characterization of three new transiting giant planets orbiting TOI-6628, TOI-3837 and TOI-5027, and one new warm sub-Saturn orbiting TOI-2328, whose transits events were detected in the lightcurves of the Transiting Exoplanet Survey Satellite (TESS) space mission. By combining TESS lightcurves with ground-based photometric and spectroscopic follow-up observations we confirm the planetary nature of the observed transits and radial velocity variations. TOI-6628~\\(b\\) has a mass of 0.75\\(\\)0.06~\\(M_J\\), a radius of 0.98\\(\\)0.05~\\(R_J\\) and is orbiting a metal-rich star with a period of 18.18424\\(0.00001\\) days and an eccentricity of 0.667\\(0.016\\), making it one of the most eccentric orbits of all known warm giants. TOI-3837~\\(b\\) has a mass of 0.59\\(\\)0.06~\\(M_J\\), a radius of 0.96\\(\\)0.05~\\(R_J\\) and orbits its host star every 11.88865\\(\\)0.00003~days, with a moderate eccentricity of 0.198\\(^+0.046_-0.058\\). With a mass of 2.01\\(\\)0.13~\\(M_J\\) and a radius of 0.99\\(^+0.07_-0.12\\) \\(R_J\\), TOI-5027~\\(b\\) orbits its host star in an eccentric orbit with \\(e\\)~=~0.395\\(^+0.032_-0.029\\) every 10.24368\\(0.00001\\)~days. TOI-2328~\\(b\\) is a Saturn-like planet with a mass of 0.16\\(\\)0.02~\\(M_J\\) and a radius of 0.89\\(\\)0.04~\\(R_J\\), orbiting its host star in a nearly circular orbit with \\(e\\)~=~0.057\\(^+0.046_-0.029\\) at an orbital period of 17.10197\\(0.00001\\) days. All four planets have orbital periods above 10 days, and our planet interior structure models are consistsent a rocky-icy core with a H/He envelope, providing evidence supporting the core accretion model of planet formation for this kind of planets.

We report the discovery of two short-period massive giant planets from NASA's Transiting Exoplanet Survey Satellite (TESS). Both systems, TOI-558 (TIC 207110080) and TOI-559 (TIC 209459275), were identified from the 30-minute cadence Full Frame Images and confirmed using ground-based photometric and spectroscopic follow-up observations from TESS's Follow-up Observing Program Working Group. We find that TOI-558 b, which transits an F-dwarf (\\(M_{*}=1.349^{+0.064}_{-0.065}\\ M_{\\odot}\\), \\(R_{*}=1.496^{+0.042}_{-0.040}\\ R_{\\odot}\\), \\(T_{eff}=6466^{+95}_{-93}\\ K\\), age \\(1.79^{+0.91}_{-0.73}\\ Gyr\\)) with an orbital period of 14.574 days, has a mass of \\(3.61\\pm0.15\\ M_{\\rm J}\\), a radius of \\(1.086^{+0.041}_{-0.038}\\ R_{\\rm J}\\), and an eccentric (e=\\(0.300^{+0.022}_{-0.020}\\)) orbit. TOI-559 b transits a G-dwarf (\\(M_{*}=1.026\\pm0.057\\ M_{\\odot}\\), \\(R_{*}=1.233^{+0.028}_{-0.026}\\ R_{\\odot}\\), \\(T_{eff}=5925^{+85}_{-76}\\ K\\), age \\(6.8^{+2.5}_{-2.0}\\ Gyr\\)) in an eccentric (e=\\(0.151\\pm0.011\\)) 6.984-day orbit with a mass of \\(6.01^{+0.24}_{-0.23}\\ M_{\\rm J}\\) and a radius of \\(1.091^{+0.028}_{-0.025}\\ R_{\\rm J}\\). Our spectroscopic follow-up also reveals a long-term radial velocity trend for TOI-559, indicating a long-period companion. The statistically significant orbital eccentricity measured for each system suggests that these planets migrated to their current location through dynamical interactions. Interestingly, both planets are also massive (\\(>3\\ M_{\\rm J}\\)), adding to the population of massive giant planets identified by TESS. Prompted by these new detections of high-mass planets, we analyzed the known mass distribution of hot and warm Jupiters but find no significant evidence for multiple populations. TESS should provide a near magnitude-limited sample of transiting hot Jupiters, allowing for future detailed population studies.

NO INTEREST UNTIL 2014,\" READ THE MASSIVE RED SIGN OUTSIDE BIG'S FURniture in Henderson, Nev. It beckoned Diane Lewis to the store's year-end liquidation sale. \"I had to pull in,\" she said as her sons frolicked on mattresses nearby. \"We really need to get us a new bedroom set; their old one is kinda beat up. If we can get that financing deal, we can make it work.\" As with most in this hard-hit region, the economy hasn't been good to Lewis, whose husband just got a new job after being laid off for eight months. They're two months behind on their mortgage, \"but we're gonna catch up,\" and she figures the family probably owes about $20,000 on various credit cards.