Despite decades of research on hot Jupiters, there are still several theories for their formation. Perhaps hot Jupiters form in several ways. Atmospheric and dynamical studies have the capability to constrain the formation scenarios. However, potential targets have to be well characterized before these observations can further constrain the theories. We present the confirmation and characterization of five hot and warm Jupiters discovered by the TESS space mission. Using TESS data combined with ground-based observations, we determine the masses, radii, and other parameters of TOI-2040 b, TOI-2049 b, TOI-2578 b, TOI-4427 b, and TOI-4458 b. Three of the planets have equilibrium temperatures of about 1800 K while two have temperatures of about 1000 K. Particularly interesting for future atmospheric characterizations are TOI-2578 b and TOI-4427 b, because of their low density and large transmission spectroscopy metric. TOI-4458 b is of special interest because it is in the northern PLATO field. It appears that TOI-2040 b has a small, but measurable eccentricity.

The population of Jupiter-sized exoplanets with orbital periods between 10 and 200 days (WJs) exhibits a broad range of orbital eccentricities and system architectures, suggesting a diversity of formation and migration pathways. In this work, we report the detection and characterization of two new eccentric WJs, TOI-2147 b and TOI-6019 b, initially identified as planet candidates by the Transiting Exoplanet Survey Satellite (TESS). We combined TESS photometry with ground-based follow-up observations, including multiband photometry from LCOGT and MuSCAT2, high-angular-resolution speckle imaging, and high-precision radial velocity measurements from the high-resolution Manfred Hirt Planet Finder Spectrograph (MaHPS). Using these data, we were able to confirm the planetary nature of both candidates. TOI-2147 b has a radius of 10.5 ± 0.3 R_⊕ and a mass of 116 ± 22 M_⊕. It orbits its slightly metal-poor ([Fe/H] = -0.29^+0.07_-0.08) G-type host star on an eccentric orbit (e = 0.29 ± 0.07) with a period of 26.2 days. TOI-6019 b has a radius of 12.3 ± 0.3 R_⊕ and a mass of 149 ± 15 M_⊕. It orbits a slightly evolved, solar-metallicity G-type sub-giant with a period of 14.5 days on a significantly eccentric orbit (e = 0.48^+0.05_-0.04). Both planets have bulk densities below that of Jupiter, indicating mildly inflated radii, with interior structure modeling using GASTLI. This suggests that tidal heating from the nonzero eccentricities likely contributes to this inflation and disfavors large atmospheric metal enrichment. No significant signals from additional companions were detected in the radial velocity time series or transit timing variations. Together with the elevated eccentricities, this is consistent with a high-eccentricity migration origin for both systems.

We report the discovery and characterization of two sub-Saturns from the Transiting Exoplanet Survey Satellite ( TESS ) using high- resolution spectroscopic observations from the MaHPS spectrograph at the Wendelstein Observatory and the SOPHIE spectrograph at the Haute-Provence Observatory. Combining photometry from TESS, KeplerCam, LCOGT, and MuSCAT2, along with the radial velocity measurements from MaHPS and SOPHIE, we measured precise radii and masses for both planets. TOI-5108 b is a sub-Saturn, with a radius of 6.6 ± 0.1 R ⊕ and a mass of 32 ± 5 M ⊕ . TOI-5786 b is similar to Saturn, with a radius of 8.54 ± 0.13 R ⊕ and a mass of 73 ± 9 M ⊕ . The host star for TOI-5108 b is a moderately bright (Vmag 9.75) G-type star. TOI-5786 is a slightly dimmer (Vmag 10.2) F-type star. Both planets are close to their host stars, with periods of 6.75 days and 12.78 days, respectively. This puts TOI-5108 b just within the bounds of the Neptune desert, while TOI-5786 b is right above the upper edge. We estimated hydrogen-helium (H/He) envelope mass fractions of 38% for TOI-5108 b and 74% for TOI-5786 b. However, when using a model for the interior structure that includes tidal effects, the envelope fraction of TOI-5108 b could be much lower (~20%), depending on the obliquity. We estimated mass-loss rates between 1.0 x 10 9 g/s and 9.8 x 10 9 g/s for TOI-5108 b and between 3.6 x 10 8 g/s and 3.5 x 10 9 g/s for TOI-5786 b. Given their masses, both planets could be stable against photoevaporation. Furthermore, at these mass-loss rates, there is likely no detectable signal in the metastable helium triplet with the James Webb Space Telescope (JWST). We also detected a transit signal for a second planet candidate in the TESS data of TOI-5786, with a period of 6.998 days and a radius of 3.83 ± 0.16 R ⊕ . Using our RV data and photodynamical modeling, we were able to provide a 3-σ upper limit of 26.5 M ⊕ for the mass of the potential inner companion to TOI-5786 b.

We derive the g' band galaxy luminosity function (GLF) of quenched red sequence in the Coma cluster from a deep-imaging survey with ≈1.5 deg^2 around the cluster center. The dataset comprises deep u'-, g'-, and r'-band data obtained with the Wendelstein Wide Field Imager on the 2.1 m Fraunhofer Wendelstein Telescope reaching median 3σ surface brightness limits in 10"×10" boxes of (30.0 u', 29.6 g', 28.7 r') mag arcsec^-2. We measure structural parameters across a large dynamic range in galaxy brightness (-24.5 g' mag⪅ M⪅-11.3 g' mag), from the brightest cluster galaxy to low-luminosity dwarfs, including compact dwarf galaxies and ultra-diffuse galaxies. We automatically identify 5161 cluster member candidates based on their membership on the quiescent sequence in the u'-g' versus g'-r' color–color diagram and their red sequence membership. The structural parameters of bright galaxies are obtained via isophotal modeling, and fully automated parametric image fitting for faint ones. Injection-recovery tests and two identically analyzed reference fields provide statistical corrections for completeness and contamination, yielding a representative GLF that reliably probes the faint end and may serve as a benchmark for future studies. We report a best-fit double Schechter g' band GLF with a comparatively steep faint-end slope α_2=-1.539^+0.024_-0.024. We perform an apples-to-apples comparison with the Coma counterpart in the SLOW simulations, finding overall agreement but a deficit of bright and an excess of dwarf galaxies in the simulation, despite its shallower faint-end slope, highlighting the need for true apples-to-apples comparisons that consider both normalization and slope for a consistent interpretation of the GLF.

The Main Selection Mechanism (MSM) is the cryogenic mechanism that will allow to switch between the operational modes of MICADO, the first light instruments for the ESO Extremely Large Telescope (ELT). The mechanism, developed by the Universitats-Sternwarte Muenchen (USM), will be located inside the MICADO cryostat and operate under vacuum conditions at cryogenic temperatures. The MSM consists of a main support structure and a rotating platform, where the MICADO Low Resolution Imager, Spectrometer and Pupil Imager modules are located. Manufacturing and procurement activities for the MSM started in late 2022. In this paper we present the current status of manufacturing and procurement for the MSM, and its overall assembly, integration and test (AIT) plan. AIT activities will start end of 2024, and will be concluded with the cryogenic test of the mechanism inside the USM big test cryostat, before the delivery in 2026 of the mechanism to the MICADO lead institute, the Max-Planck-Institute fur Extraterrestrische Physik (MPE), for its final integration inside the instrument cryostat.

We report the confirmation and characterization of four hot Jupiter-type exoplanets initially detected by TESS: TOI-1295 b, TOI-2580 b, TOI-6016 b, and TOI-6130 b. Using observations with the high-resolution echelle spectrograph MaHPS on the 2.1m telescope at Wendelstein Observatory, together with NEID at Kitt Peak National Observatory and TRES at the Fred Lawrence Whipple Observatory, we confirmed the planetary nature of these four planet candidates. We also performed precise mass measurements. All four planets are found to be hot Jupiters with orbital periods between 2.4 and 4.0 days. The sizes of these planets range from 1.29 to 1.64 Jupiter radii, while their masses range from 0.6 to 1.5 Jupiter masses. Additionally, we investigated whether there are signs of other planets in the systems but have found none. Lastly, we compared the radii of our four objects to the results of an empirical study of radius inflation and see that all four demonstrate a good fit with the current models. These four planets belong to the first array of planets confirmed with MaHPS data, supporting the ability of the spectrograph to detect planets around fainter stars as faint as V=12.

MICADO is a first light instrument for the Extremely Large Telescope (ELT), set to start operating later this decade. It will provide diffraction limited imaging, astrometry, high contrast imaging, and long slit spectroscopy at near-infrared wavelengths. During the initial phase operations, adaptive optics (AO) correction will be provided by its own natural guide star wavefront sensor. In its final configuration, that AO system will be retained and complemented by the laser guide star multi-conjugate adaptive optics module MORFEO (formerly known as MAORY). Among many other things, MICADO will study exoplanets, distant galaxies and stars, and investigate black holes, such as Sagittarius A* at the centre of the Milky Way. After their final design phase, most components of MICADO have moved on to the manufacturing and assembly phase. Here we summarize the final design of the instrument and provide an overview about its current manufacturing status and the timeline. Some lessons learned from the final design review process will be presented in order to help future instrumentation projects to cope with the challenges arising from the substantial differences between projects for 8-10m class telescopes (e.g. ESO-VLT) and the next generation Extremely Large Telescopes (e.g. ESO-ELT). Finally, the expected performance will be discussed in the context of the current landscape of astronomical observatories and instruments. For instance, MICADO will have similar sensitivity as the James Webb Space Telescope (JWST), but with six times the spatial resolution.

We report the discovery and characterization of a small planet, TOI-1408 c, on a 2.2 day orbit located interior to a previously known hot Jupiter, TOI-1408 b ( P = 4.42 days, M = 1.86 ± 0.02 M Jup , R = 2.4 ± 0.5 R Jup ) that exhibits grazing transits. The two planets are near 2:1 period commensurability, resulting in significant transit timing variations (TTVs) for both planets and transit duration variations for the inner planet. The TTV amplitude for TOI-1408 c is 15% of the planet’s orbital period, marking the largest TTV amplitude relative to the orbital period measured to date. Photodynamical modeling of ground-based radial velocity (RV) observations and transit light curves obtained with the Transiting Exoplanet Survey Satellite and ground-based facilities leads to an inner planet radius of 2.22 ± 0.06 R ⊕ and mass of 7.6 ± 0.2 M ⊕ that locates the planet into the sub-Neptune regime. The proximity to the 2:1 period commensurability leads to the libration of the resonant argument of the inner planet. The RV measurements support the existence of a third body with an orbital period of several thousand days. This discovery places the system among the rare systems featuring a hot Jupiter accompanied by an inner low-mass planet.

We report the confirmation of a sub-Saturn-size exoplanet, TOI-1194 b with a mass about $0.456_{-0.051}^{+0.055}$ $M_{J}$, and a very low mass companion star with a mass of about $96.5\pm1.5$ $M_J$, TOI-1251 B. Exoplanet candidates provided by the Transiting Exoplanet Survey Satellite (TESS) are suitable for further follow-up observations by ground-based telescopes with small and medium apertures. The analysis is performed based on data from several telescopes worldwide, including telescopes in the Sino-German multiband photometric campaign, which aimed at confirming TESS Objects of Interest (TOIs) using ground-based small-aperture and medium-aperture telescopes, especially for long-period targets. TOI-1194 b is confirmed based on the consistent periodic transits depths from the multiband photometric data. We measure an orbital period of $2.310644\pm0.000001$ d, and radius is $0.767_{-0.041}^{+0.045}$ $R_J$, and amplitude of RV curve is $69.4_{-7.3}^{+7.9}$ m/s. TOI-1251 B is confirmed based on the multiband photometric and high-resolution spectroscopic data, whose orbiting period is $5.963054_{-0.000001}^{+0.000002}$ d, the radius is $0.947_{-0.033}^{+0.035}$ $R_J$, and amplitude of RV curve is $9849_{-40}^{+42}$ m/s.

The Multi-Adaptive Optics Imaging Camera for Deep Observations (MICADO) is one of the first light ESO Extremely-Large-Telescope (ELT) Instruments and is now nearing the completion of its final design stage. The MICADO instrument aims to generate high-resolution images of the Universe at near-infrared wavelengths, which requires maintaining a stable vacuum environment at 82 K inside the MICADO cryostat. To fulfill this requirement and for safety reasons, a PLC-based control software is used. This software communicates with over 180 sensors and devices simultaneously, to remotely maintain the cryostat environment. This paper discusses the software's design architecture and implementation.

The Main Selection Mechanism (MSM) is the cryogenic subsystem of the Multi-AO Imaging Camera for Deep Observations (MICADO) which allows to switch between the operational modes (imaging, spectroscopy, calibration) of the instrument. MICADO is one of the first light instruments for the ESO Extremely Large Telescope (ELT) and operates in the near-infrared wavelength range. The MSM is located inside the MICADO cryostat and it operates under vacuum conditions and cryogenic temperatures (`~82K). The mechanism consists of a main support structure and a rotating platform, where the MICADO Low Resolution Imager, Spectrometer and Pupil Imager modules are located. In this paper we give an overview of the final design of the MSM, which was presented at the MICADO final design review (FDR) in October 2021.

In the Bavarian Alps, an optimal exoplanet follow-up device is located. Besides a 43cm telescope for long term photometric observations, the observatory operates the 2.1m Fraunhofer Telescope Wendelstein, which is equipped with the highly temperature- and pressure-stabilized, frequency comb calibrated Échelle spectrograph MaHPS (R ∼ 65000) to conduct radial velocity measurements. Further, the 3KK instrument is able to conduct multiband photometry with its two Apogee-ALTA F3041 cameras for optical and its H2RG CMOS for NIR light, discerning different transit scenarios, since the characteristics of limb darkening cause differing eclipse depths and shapes, depending on the nature of the system. The combination of the photometric and spectroscopic observations allow for confident confirmation or discarding of exoplanetary candidates.

Astronomy has always been a technology driven science. This drive to ever greater sensitivity and performance is placing great pressure on the development community to meet this ongoing need. Extrapolating demand indicates a fundamental problem of affordability and timely development for both space and ground based systems. We note, that this trend is not unique to UV/VIS band. Other systems such as very long baseline interferometry in space leads to the need of large aperture radio telescopes, gravitational wave experiments like the Laser Interferometer Space Antenna (LISA) and occulter and starshade missions for coronography demand for high performance at acceptable cost. This begs the question, what can be done about it? In this initial paper, we plan to explore the roles of standardization, specialization and trans-national partnerships to realize future system design and implementation. We conclude our discussion with examples of areas where standardization in hardware and engineering approaches will improve productivity to help realize the next generation of cutting edge systems.

Hot Jupiters seem to get rarer with decreasing stellar mass. The goal of the Pan-Planets transit survey was the detection of such planets and a statistical characterization of their frequency. Here, we announce the discovery and validation of two planets found in that survey, Wendelstein-1b and Wendelstein-2b, which are two short-period hot Jupiters that orbit late K host stars. We validated them both by the traditional method of radial velocity measurements with the HIgh Resolution Echelle Spectrometer and the Habitable-zone Planet Finder instruments and then by their Transit Color Signature (TraCS). We observed the targets in the wavelength range of 4000−24 000 Å and performed a simultaneous multiband transit fit and additionally determined their thermal emission via secondary eclipse observations. Wendelstein-1b is a hot Jupiter with a radius of 1.0314−0.0061+0.0061 RJ and mass of 0.592−0.129+0.0165 MJ, orbiting a K7V dwarf star at a period of 2.66 d, and has an estimated surface temperature of about 1727−90+78 K. Wendelstein-2b is a hot Jupiter with a radius of 1.1592−0.0210+0.0204 RJ and a mass of 0.731−0.311+0.0541 MJ, orbiting a K6V dwarf star at a period of 1.75 d, and has an estimated surface temperature of about 1852−140+120 K. With this, we demonstrate that multiband photometry is an effective way of validating transiting exoplanets, in particular for fainter targets since radial velocity follow-up becomes more and more costly for those targets.

The Manfred Hirt Planet Spectrograph - formerly operated under the name FOCES - started its regular scientific observation program in fall 2019 at the 2m telescope of the Wendelstein Observatory, operated by the University Observatory of the LMU Munich. We present the first radial velocity stability measurements of an astronomical target, the 51 Pegasi b exoplanet system, utilizing our Astro Frequency Comb (ACF) for wavelength calibration. For computing RV shifts from orderwisely extracted Echelle spectra we have developed a new software pipeline. In this proceeding we will introduce the most important features of our pipeline: wavelength calibration with simultaneously recorded spectra of the AFC, generation of spectral templates, and an optional fit or cross- correlation function (CCF) for the calculation of the relative RV signals. Finally, the performance of the pipeline real data is demonstrated.

The Manfred Hirt Planet Spectrograph (MaHPS) — formerly also referred to as FOCES — is a high-resolution echelle spectrograph at the 2m telescope of the Wendelstein Observatory. One of its main scientific goals is the detection of planets at the few m/s level. To achieve such high precisions on a long-term scale, environmental stabilization of the instrument is required. The currently used temperature and pressure control systems are introduced and we present two different temperature control setups, with two and three actively controlled layers respectively. A series of measurements with an Astro Frequency Comb (AFC) as calibrator is shown to illustrate the system performance.

The Wendelstein 2 m Telescope has been in regular science operation since 2013. It is equipped with a three channel camera and an Echelle spectrograph called FOCES on one of it’s two Nasmyth foci. FOCES is a wavelength comb stabilized instrument which aims at <1m/s precision. High stability and repeatability of the entire system, including its fiber feed, are required and fast exchange times, between imaging mode and radial velocity measurement, is desirable. We are in the advanced implementation phase of an automated multifocal exchange system to allow for stable and fast exchange between the three different science instruments, a wavefront sensor and a calibration system. We present the final optical design and discuss the mechanical design choices we made in particular with respect to the limited design volume. We will conclude with presenting results from first tests on the system’s optomechanical stability.