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We present \\(\\texttt{moes}\\), a ray tracing software package that computes the path of rays through echelle spectrographs. Our algorithm is based on sequential direct tracing with Seidel aberration corrections applied at the detector plane. As a test case, we model the CARMENES VIS spectrograph. After subtracting the best model from the data, the residuals yield an rms of 0.024 pix, setting a new standard to the precision of the wavelength solution of state-of-the-art radial velocity instruments. By including the influence of the changes of the environment in the ray propagation, we are able to predict instrumental radial velocity systematics at the 1 m/s level.

Essential information about the formation and evolution of planetary systems can be found in their architectures -- in particular, in stellar obliquity (\\(\\psi\\)) -- as they serve as a signature of their dynamical evolution. Here, we present ESPRESSO observations of the Rossiter-Mclaughlin (RM) effect of 8 warm gas giants, revealing that independent of the eccentricities, all of them have relatively aligned orbits. Our 5 warm Jupiters -- WASP-106 b, WASP-130 b, TOI-558 b, TOI-4515 b, and TOI-5027 b -- have sky-projected obliquities \\(|\\lambda|\\simeq0-10\\) deg while the 2 less massive warm Saturns -- K2-139 b and K2-329 A b -- are slightly misaligned having \\(|\\lambda|\\simeq15-25\\) deg. Furthermore, for K2-139 b, K2-329 A b, and TOI-4515 b, we also measure true 3D obliquities \\(\\psi\\simeq15-30\\) deg. We also report a non-detection of the RM effect produced by TOI-2179 b. Through hierarchical Bayesian modeling of the true 3D obliquities of hot and warm Jupiters, we find that around single stars, warm Jupiters are statistically more aligned than hot Jupiters. Independent of eccentricities, 95\\% of the warm Jupiters have \\(\\psi\\lesssim30\\) deg with no misaligned planets, while hot Jupiters show an almost isotropic distribution of misaligned systems. This implies that around single stars, warm Jupiters form in primordially aligned protoplanetary disks and subsequently evolve in a more quiescent way than hot Jupiters. Finally, we find that Saturns may have slightly more misaligned orbits than warm Jupiters, but more obliquity measurements are necessary to be conclusive.

We constrain the sky-projected obliquities of two low-density hot Neptune planets, HATS-38 b and WASP-139 b, orbiting nearby G and K stars using Rossiter-McLaughlin (RM) observations with VLT/ESPRESSO, yielding \\(\\lambda = -108_{-16}^{+11}\\) deg and \\(-85.6_{-4.2}^{+7.7}\\) deg, respectively. To model the RM effect, we use a new publicly available code, ironman, which is capable of jointly fitting transit photometry, Keplerian radial velocities, and RM effects. WASP-139 b has a residual eccentricity \\(e=0.103_{-0.041}^{+0.050}\\) while HATS-38 b has an eccentricity of \\(e=0.112_{-0.070}^{+0.072}\\), which is compatible with a circular orbit given our data. Using the obliquity constraints, we show that they join a growing group of hot and low-density Neptunes on polar orbits. We use long-term radial velocities to rule out companions with masses \\(\\sim 0.3-50\\) \\(M_J\\) within \\(\\sim10\\) au. We show that the orbital architectures of the two Neptunes can be explained with high-eccentricity migration from \\(\\gtrsim 2\\) au driven by an unseen distant companion. If HATS-38b has no residual eccentricity, its polar and circular orbit can also be consistent with a primordial misalignment. Finally, we performed a hierarchical Bayesian modeling of the true obliquity distribution of Neptunes and found suggestive evidence for a higher preponderance of polar orbits of hot Neptunes compared to Jupiters. However, we note that the exact distribution is sensitive to the choice of priors, highlighting the need for additional obliquity measurements of Neptunes to robustly compare the hot Neptune obliquity distribution to Jupiters.

We report the discovery and characterisation of three transiting warm Jupiters: TIC 147027702b, TIC 245076932b and TIC 87422071b. These systems were initially identified as transiting candidates using light curves generated from the full-frame images of the TESS mission. We confirmed the planetary nature of these objects with ground-based spectroscopic follow-up observations using FEROS and the new PLATOSpec spectrograph attached to the ESO 1.52 m telescope at the La Silla Observatory, and with ground-based photometric observations of the Observatoire Moana, Las Cumbres Observatory Global Telescope and ASTEP. From a global fit to the photometry and radial velocities, we determine that the planet TIC 147027702b has a low-eccentric orbit (\\(e = 0.13 \\pm 0.05\\)) with a period of 44.4 days and has a mass of \\(1.09^{+0.07}_{-0.13}\\) M\\(_J\\) and a radius of \\(0.98 \\pm 0.06\\) R\\(_J\\). TIC 245076932b has a moderately low mass of \\(0.51 \\pm 0.05\\) M\\(_J\\), a radius of \\(0.97 \\pm 0.05\\) R\\(_J\\), and an eccentric orbit (\\(e = 0.43 \\pm 0.02\\)) with a period of 21.6 days. TIC 87422071b has a mass of \\(1.29 \\pm 0.10\\) M\\(_J\\), a radius of \\(0.97 \\pm 0.08\\) R\\(_J\\), and has a slightly eccentric orbit (\\(e = 0.12 \\pm 0.07\\)) with a period of 11.3 days. These well-characterised warm Jupiters expand the currently limited sample of similar gas giants and provide valuable benchmarks for testing models of giant-planet formation, migration, and tidal evolution.

We report the discovery of TOI-4507 b, a transiting sub-Saturn with a density \\(<\\) 0.2 g/cm\\(^3\\) on a 105-day prograde orbit around a 700 Myr old F star. The transits were detected using data from TESS as well as the Antarctic telescope ASTEP. A joint analysis of the light curves and radial velocities from HARPS, FEROS, and CORALIE confirmed the planetary nature of the signal by limiting the mass to be below 20 \\(M_\\oplus\\) at 95% confidence. The radial velocities also exhibit the Rossiter-McLaughlin effect and imply that the planet orbits the star in a prograde orbit with a sky-projected obliquity \\(\\lambda=-15_{-44}^{+50}\\) deg (\\(|\\lambda|<80\\) deg at \\(3\\sigma\\)). With these characteristics, TOI-4507 is one of the longest-period systems for which the stellar obliquity has been measured, and the planet is among the longest-period and youngest ''super-puff'' planets yet discovered.

We present a joint analysis of TTVs and Doppler data for the transiting exoplanet system TOI-4504. TOI-4504 c is a warm Jupiter-mass planet that exhibits the largest known transit timing variations (TTVs), with a peak-to-node amplitude of \\(\\sim\\) 2 days, the largest value ever observed, and a super-period of \\(\\sim\\) 930 d. TOI-4504 b and c were identified in public TESS data, while the TTVs observed in TOI-4504 c, together with radial velocity (RV) data collected with FEROS, allowed us to uncover a third, non-transiting planet in this system, TOI-4504 d. We were able to detect transits of TOI-4504 b in the TESS data with a period of 2.4261\\(\\pm 0.0001\\) days and derive a radius of 2.69\\(\\pm 0.19\\) R\\(_{\\oplus}\\). The RV scatter of TOI-4504 was too large to constrain the mass of TOI-4504 b, but the RV signals of TOI-4504 c \\& d were sufficiently large to measure their masses. The TTV+RV dynamical model we apply confirms TOI-4504 c as a warm Jupiter planet with an osculating period of 82.54\\(\\pm 0.02\\) d, mass of 3.77\\(\\pm 0.18\\) M\\(_{\\rm J}\\) and a radius of 0.99\\(\\pm 0.05\\) R\\(_{\\rm J}\\), while the non-transiting planet TOI-4504 d, has an orbital period of 40.56\\(\\pm 0.04\\) days and mass of 1.42\\(_{-0.06}^{+0.07}\\) M\\(_{\\rm J}\\). We present the discovery of a system with three exoplanets: a hot sub-Neptune and two warm Jupiter planets. The gas giant pair is stable and likely locked in a first-order 2:1 mean-motion resonance (MMR). The TOI-4504 system is an important addition to MMR pairs, whose increasing occurrence supports a smooth migration into a resonant configuration during the protoplanetary disk phase.

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 \\textbf{(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\\(\\pm\\)0.06~\\(M_\\mathrm{J}\\), a radius of 0.98\\(\\pm\\)0.05~\\(R_J\\) and is orbiting a metal-rich star with a period of 18.18424\\(\\pm{0.00001}\\) days and an eccentricity of 0.667\\(\\pm0.016\\), making it one of the most eccentric orbits of all known warm giants. TOI-3837~\\(b\\) has a mass of 0.59\\(\\pm\\)0.06~\\(M_\\mathrm{J}\\), a radius of 0.96\\(\\pm\\)0.05~\\(R_J\\) and orbits its host star every 11.88865\\(\\pm\\)0.00003~days, with a moderate eccentricity of 0.198\\(^{+0.046}_{-0.058}\\). With a mass of 2.01\\(\\pm\\)0.13~\\(M_\\mathrm{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\\(\\pm{0.00001}\\)~days. TOI-2328~\\(b\\) is a Saturn-like planet with a mass of 0.16\\(\\pm\\)0.02~\\(M_\\mathrm{J}\\) and a radius of 0.89\\(\\pm\\)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\\(\\pm{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.

Despite being the most common types of stars in the Galaxy, the physical properties of late M dwarfs are often poorly constrained. A trend of radius inflation compared to evolutionary models has been observed for earlier type M dwarfs in eclipsing binaries, possibly caused by magnetic activity. It is currently unclear whether this trend also extends to later type M dwarfs below the convective boundary. This makes the discovery of lower-mass, fully convective, M dwarfs in eclipsing binaries valuable for testing evolutionary models especially in longer-period binaries where tidal interaction between the primary and secondary is negligible. With this context, we present the discovery of the NGTS-EB-7 AB system, an eclipsing binary containing a late M dwarf secondary and an evolved G-type primary star. The secondary star has a radius of \\(0.125 \\pm 0.006 R_\\odot\\) , a mass of \\(0.096 \\pm 0.004 M_\\odot\\) and follows a highly eccentric \\((e=0.71436 \\pm 0.00085)\\) orbit every \\(193.35875 \\pm 0.00034\\) days. This makes NGTS-EB-7 AB the third longest-period eclipsing binary system with a secondary smaller than \\(200 M_J\\) with the mass and radius constrained to better than \\(5 \\%\\). In addition, NGTS-EB-7 is situated near the centre of the proposed LOPS2 southern field of the upcoming PLATO mission, allowing for detection of the secondary eclipse and measurement of the companion`s temperature. With its long-period and well-constrained physical properties - NGTS-EB-7 B will make a valuable addition to the sample of M dwarfs in eclipsing binaries and help in determining accurate empirical mass/radius relations for later M dwarf stars.

We report the discovery and characterization of three giant exoplanets orbiting solar-analog stars, detected by the \\tess space mission and confirmed through ground-based photometry and radial velocity (RV) measurements taken at La Silla observatory with \\textit{FEROS}. TOI-2373\\,b is a warm Jupiter orbiting its host star every \\(\\sim\\) 13.3 days, and is one of the two most massive known exoplanet with a precisely determined mass and radius around a star similar to the Sun, with an estimated mass of m\\(_p\\) = \\(9.3^{+0.2}_{-0.2}\\,M_{\\mathrm{jup}}\\), and a radius of \\(r_p\\) = \\(0.93^{+0.2}_{-0.2}\\,R_{\\mathrm{jup}}\\). With a mean density of \\(\\rho = 14.4^{+0.9}_{-1.0}\\,\\mathrm{g\\,cm}^{-3}\\), TOI-2373\\,b is among the densest planets discovered so far. TOI-2416\\,b orbits its host star on a moderately eccentric orbit with a period of \\(\\sim\\) 8.3 days and an eccentricity of \\(e\\) = \\(0.32^{+0.02}_{-0.02}\\). TOI-2416\\,b is more massive than Jupiter with \\(m_p\\) = 3.0\\(^{+0.10}_{-0.09}\\,M_{\\mathrm{jup}}\\), however is significantly smaller with a radius of \\(r_p\\) = \\(0.88^{+0.02}_{-0.02},R_{\\mathrm{jup}}\\), leading to a high mean density of \\(\\rho = 5.4^{+0.3}_{-0.3}\\,\\mathrm{g\\,cm}^{-3}\\). TOI-2524\\,b is a warm Jupiter near the hot Jupiter transition region, orbiting its star every \\(\\sim\\) 7.2 days on a circular orbit. It is less massive than Jupiter with a mass of \\(m_p\\) = \\(0.64^{+0.04}_{-0.04}\\,M_{\\mathrm{jup}}\\), and is consistent with an inflated radius of \\(r_p\\) = \\(1.00^{+0.02}_{-0.03}\\,R_{\\mathrm{jup}}\\), leading to a low mean density of \\(\\rho = 0.79^{+0.08}_{-0.08}\\,\\mathrm{g\\,cm}^{-3}\\). The newly discovered exoplanets TOI-2373\\,b, TOI-2416\\,b, and TOI-2524\\,b have estimated equilibrium temperatures of \\(860^{+10}_{-10}\\) K, \\(1080^{+10}_{-10}\\) K, and \\(1100^{+20}_{-20}\\) K, respectively, placing them in the sparsely populated transition zone between hot and warm Jupiters.

Based on recently-taken and archival HARPS, FEROS and HIRES radial velocities (RVs), we present evidence for a new planet orbiting the first ascent red giant star HD33142 (with an improved mass estimate of 1.52\\(\\pm\\)0.03 M\\(_\\odot\\)), already known to host two planets. We confirm the Jovian mass planets HD33142 b and c with periods of \\(P_{\\rm b}\\) = 330.0\\(_{-0.4}^{+0.4}\\) d and \\(P_{\\rm c}\\) = 810.2\\(_{-4.2}^{+3.8}\\) d and minimum dynamical masses of \\(m_{\\rm b}\\sin{i}\\) = 1.26\\(_{-0.05}^{+0.05}\\) M\\(_{\\rm Jup}\\) and \\(m_{\\rm c}\\sin{i}\\) = 0.89\\(_{-0.05}^{+0.06}\\) M\\(_{\\rm Jup}\\). Furthermore, our periodogram analysis of the precise RVs shows strong evidence for a short-period Doppler signal in the residuals of a two-planet Keplerian fit, which we interpret as a third, Saturn-mass planet with \\(m_\\mathrm{d}\\sin{i}\\) = 0.20\\(_{-0.03}^{+0.02}\\) M\\(_{\\rm Jup}\\) on a close-in orbit with an orbital period of \\(P_{\\rm d}\\) =89.9\\(_{-0.1}^{+0.1}\\) d. We study the dynamical behavior of the three-planet system configurations with an N-body integration scheme, finding it long-term stable with the planets alternating between low and moderate eccentricities episodes. We also performed N-body simulations, including stellar evolution and second-order dynamical effects such as planet-stellar tides and stellar mass-loss on the way to the white dwarf phase. We find that planets HD33142 b, c and d are likely to be engulfed near the tip of the red giant branch phase due to tidal migration. These results make the HD33142 system an essential benchmark for the planet population statistics of the multiple-planet systems found around evolved stars.