metric measurements in space. Since such bright stars are relatively scarce on the sky, a very large total field of view of 2132 deg² was required. Furthermore, to be able to observe in a given target field the brightest as well as fainter stars, the instrument photon collecting area is split into 26 individual cameras. The 24 cameras which are used exclusively for science operation are termed "normal" cameras whereas the two additional cameras, used also for fine-pointing on top of science operation, are termed "fast" cameras. With this configuration PLATO will be able to obtain very stable, high precision, long-time photometric data of a large number of bright stars. Combining the information provided by the planetary transits, with the stellar data derived by asteroseismology techniques and the radial velocity measurements obtained from the ground, PLATO will provide a high-precision characterisation of the radius, mass and age of exoplanetary systems.

The data read by the CCDs of each camera are first processed by a Data Processing Unit (DPU) handling two cameras at the same time. The processed data are then transferred to the Instrument Control Unit (ICU) that finally compresses them before sending them to the spacecraft on-board mass memory for downloading to ground. The different sub-systems composing the PLATO spacecraft and payload can be seen in Fig. 24.

Table 8 summarises the main data of the instrument. Each 20 cm class camera (12 cm entrance pupil) has a total field of view (FoV) of 1037 square degrees (see [271]). The 24 normal cameras are organised on the optical bench of the spacecraft in 4 groups of 6 co-aligned cameras each. The sky fields of the four camera groups are offset with respect to a central line of sight by 9.2 degrees, pointing towards the four corners of a square of 13.0 deg, in order to widen the total overlapping FoV of the instrument. With this approach the number of brightest stars within SNR requirements is augmented with respect to a full coalignment of the whole set of cameras. Figure 25 illustrates how many cameras observe the same part of the target field for a pointing. The total instrument field therefore is about 2132 deg² (with rounded edges). Figure 26 shows the Structural and Thermal Model (STM) of the payload during integration at OHB, ready for the qualification activities of the Payload Module.

The two fast cameras are optimised to observe the brightest stars (4 - 8.2 mag) and are part of the fine-pointing loop of the satellite. They point towards the center of the PLATO payload field of view. These two cameras provide full redundancy to secure the fine-pointing capabilities of the mission. They differ however in their entrance filter, one with a red and one with a blue spectral filter allowing for colour information on the bright targets. Thanks to a very fast readout of 2.5 s, they provide very high quality data for the Fine Guidance System (FGS) algorithm as shown in Grießbach et al. [145]. This algorithm allows the satellite to reach the excellent pointing stability required for the different science cases detailed above:

* FGS noise equivalent angle: < 0.025 arcsec around X and Y, and 0.1 arcsec around Z FGS measurement reference frame axes.

* FGS measurement bias stability: < 0.010 arcsec around X and Y, and 0.040 arcsec around Z FGS measurement reference frame axes.

<figure><img src="image_44.png" /></figure>
## 13.2 PLATO cameras

All the cameras are externally identical (except for the baffles) and their interfaces to the spacecraft optical bench are the same, with three main bipods, see Fig. 27. Mechanically, their central part is the tube of the Telescope Optical Unit (TOU), made of AlBeMet. The six lenses of the TOU are all mounted inside this tube. This tube is also the support for the baffle that acts both as straylight baffle and as a radiator for the whole camera. While the Focal Plane Assembly (FPA) with the CCDs is fixed to the TOU tube by three bipods, the Front End Electronics of the Normal Cameras (N-FEE) are mounted directly to the main interfaces of the cameras to the optical bench (the main bipods) with their own Support Structure (FSS). This allows for conductive coupling to evacuate the high-power dissipation. The Fast Front End Electronic units (F-FEE), much heavier and with a higher thermal dissipation, are however directly

<table><caption>**Table 8** PLATO Instrument parameters</caption><thead><tr><th colspan="2">PLATO Instrument</th></tr></thead><tbody><tr><td>Total FoV</td><td>2132 deg<sup>2</sup></td></tr><tr><td>FoV by 24 CAMs</td><td>294 deg<sup>2</sup></td></tr><tr><td>FoV by 18 CAMs</td><td>171 deg<sup>2</sup></td></tr><tr><td>FoV by 12 CAMs</td><td>796 deg<sup>2</sup></td></tr><tr><td>FoV by 6 CAMs</td><td>871 deg<sup>2</sup></td></tr><tr><td>Number of cameras</td><td>26 total: 24 normal, 2 fast cameras</td></tr><tr><td>Normal camera groups</td><td>4, with 6 normal cameras each</td></tr><tr><td>Angle between camera groups</td><td>Arranged on four corners of a 13.0 degrees side square</td></tr><tr><td>PDE</td><td>3 arcsec HCA over 3 months in the directional direction<br>6 arcsec HCA over 3 months in the rotational direction</td></tr><tr><td>PRE</td><td>3 arcsec HCA in the directional direction<br>6 arcsec HCA in the rotational direction</td></tr><tr><td>RPE</td><td>1 arcsec HCA over 25s in the directional direction<br>2 arcsec HCA over 25s in the rotational direction</td></tr><tr><td>Photometric range</td><td>4 - 16 magV</td></tr><tr><td>Instrument mass</td><td>&lt; 623.15 kg</td></tr><tr><td>Peak power consumption</td><td>&lt; 890 W</td></tr><tr><td>Daily data generation</td><td>435 Gbit/day</td></tr><tr><td>Normal electronic chain</td><td>12 DPUs: 1 for 2 normal cameras<br>2 normal AEUs: 1 for 12 normal cameras</td></tr><tr><td>Fast electronic chain</td><td>2 fast-DPUs: 1 per fast camera<br>1 fast AEU: 1 for both fast cameras</td></tr></tbody></table>

PDE: Attitude Pointing Drift Error; PRE: Attitude Pointing Repeatability Error; RPE: Relative Attitude Pointing Error

FoV: Total Field of View; HCA: half cone angle; DPU: Data Processing Unit; AEU: Ancillary Electronic Unit.
<figure><img src="image_45.png" /><figcaption>**Fig. 25** Illustration of the PLATO field coverage. Left: position on the sky of the optical axis of the four groups of 6 coaligned "normal" cameras, and of the two "fast" cameras (dashed black line). Right: Number of "normal" cameras observing simultaneously the different sectors of the overall PLATO field of view. The center of the field (dark blue) is observed by all 24 cameras. At the edges (orange) only 6 cameras observe simultaneously the same field on the sky</figcaption></figure>

mounted to the optical bench of the spacecraft and have no thermo-mechanical links to the cameras (except for the CCD flexi connections).

Thermally, each camera is individually controlled by a Thermal Control System (TCS) that sets its temperature thanks to three heaters placed on the tube of the TOU. Using a Proportional-Integral (PI) controller algorithm, the temperature of each camera can be held very stable, up to ±10mK over 14 hours using 600 s sliding window averages. Thanks to the athermal design of the camera and the AlBeMet tube properties, this temperature stability around the heaters is very well propagated to all the

<figure><img src="image_46.png" /><figcaption>**Fig. 26** The PLATO Payload Module Structural and Thermal Model (STM) during integration at the OHB facilities. Note the relative pointing of each of the 4 groups of 6 normal cameras, and the two fast cameras located at the top of the PLM. Credit: OHB AG</figcaption></figure>
camera sub-systems and especially the CCDs. The heat dissipated by the CCDs is conductively transferred directly to the baffle that can then dissipate it into cold space. This TCS is also used to fine tune the focus of each camera in space and ensure that each camera is operated in its best possible focus position [87, 270]. By changing the temperature of the camera, the characteristics of the optical system are changing leading to a slight shift of the focus. This thermal refocusing is used on-ground and then during commissioning to calibrate each camera individually to its best focus temperature. Testing under representative thermal vacuum conditions on 24 flight units up to now has shown that the best focus will be between -77°C and -86°C, with an average value around -81°C, well within the operational limits between -70°C and -90°C. The precise value for each camera will be determined during the commissioning phase once in space.

The optical design of each camera [221] consists of a six lens system with a central Calcium Fluoride lens [40] close to the stop, and with a first aspheric lens protected, for thermal and radiation hardness purposes, by a Suprasil window. All the optical materials have been the subject of specific radhard studies [94] and the whole design is a fine tuning balance between radiation, thermal and mass budgets [222]. To obtain more information on the current status of the point spread function analysis and the camera focusing activities, the interesting reader can refer to Borsa et al. [48] and Pagliazzi et al. [265].

An anti-reflection coating is placed on every optical surface to maximise the optical transmission in the spectral range [500-1000] nm. Each 12 cm aperture camera has a FoV of 1037 square degrees as shown in Pertenais et al. [271]. This wide FoV is achieved thanks to a circular optical FoV of the TOU of around 18.88° radius that

<figure><img src="image_47.png" /><figcaption>**Fig. 27** CAD views of Camera with all its sub-systems. Left: Complete camera; right: Internal structure
(credits: ESA/ATG Medialab)</figcaption></figure>
<figure><img src="image_48.png" /><figcaption>**Fig. 28** Left: Engineering model of a complete Focal Plane Assembly populated with full-frame CCDs. Right: Engineering models of the FPA and the Normal Front End Electronics integrated for functional testing at MSSL</figcaption></figure>

illuminates the 4 full-frame CCDs of 81.18 × 81.18 mm² each on the Focal Plane Assemblies (FPA). As mentioned above, each FPA is electrically connected to a Front End Electronics (either "normal" or "fast" ones), completing the PLATO Camera. One of the FPA models used for qualification is shown in Fig. 28, with 4 full-frame (i.e. "normal" CCDs). More details on the FPA can be found in Moreno et al. [247]. Table 9 summarises the main parameters of the individual cameras. The transmission and quantum efficiency curves can be consulted in [47].

## 13.3 PLATO data processing system

The PLATO Data Processing System (DPS) is made up of an on-board segment and a ground segment. The on-ground data processing approach is presented in Section 8. Concerning the on-board segment, with 24 normal cameras working at the cadence of 25 seconds and two fast cameras working at the cadence of 2.5 seconds, the amount of raw data produced each day is over 100 Terabit. This volume must be compared to the hundreds of Gigabit which can be actually downloaded each day to the ground. It is clearly not possible to transmit the whole amount of raw data. The role of the on-board processing is to reduce by a factor of more than 1000 the flow rate by downlinking star intensities, centroid curves and imagettes at the cadence required by the science applications.

The PLATO payload on-board data processing system is made up of an Instrument Control Unit (ICU), two Main Electronic Units (MEU) and a Fast Electronic Unit (FEU). Each MEU contains 6 normal Data Processing Units (N-DPUs) for processing data from the normal cameras. Each N-DPU is dealing with two normal cameras in terms of managing the N-FEE and acquiring data. The nominal processing cadence for the N-DPUs is 25 sec. There are two F-DPUs gathered in the FEU. Each F-DPU

<figure><img src="image_49.png" /></figure>
<table><caption>**Table 9** PLATO Camera parameters</caption><thead><tr><th></th><th></th></tr></thead><tbody><tr><td>Normal cameras</td><td></td></tr><tr><td>entrance pupil diameter</td><td>120 mm (the frontal lens is 200 mm wide)</td></tr><tr><td>focal length</td><td>247.5 mm</td></tr><tr><td>camera FoV</td><td>1037 deg<sup>2</sup></td></tr><tr><td>photometric range</td><td>4-16 magV</td></tr><tr><td>transmission</td><td>500-1000 nm</td></tr><tr><td>no. CCDs/camera</td><td>4</td></tr><tr><td>read-out mode</td><td>full frame</td></tr><tr><td>read-out cadence</td><td>25 sec</td></tr><tr><td>number of effective pixels</td><td>4510×4510</td></tr><tr><td>pixel size</td><td>18×18 µm</td></tr><tr><td>pixel scale</td><td>15 arcsec/pixel</td></tr><tr><td>nominal working temperature</td><td>-80°C</td></tr><tr><td>Fast cameras, where different from above</td><td></td></tr><tr><td>camera FoV</td><td>610 deg<sup>2</sup></td></tr><tr><td>photometric range</td><td>4 - 8.2 magV</td></tr><tr><td>transmission</td><td>505-700 nm<br>665-1000 nm</td></tr><tr><td>read-out mode</td><td>frame transfer</td></tr><tr><td>read-out cadence</td><td>2.5 sec</td></tr><tr><td>number of effective pixels</td><td>4490×2245</td></tr></tbody></table>

is responsible for processing the data of one fast camera. The processing cadence for F-DPUs is 2.5 sec. The F-DPUs main purpose is providing attitude data for the Fine Guidance System (FGS) directly to the Service Module (SVM) AOCS and to the ICU. Furthermore, it manages the F-FEE and handles scientific data of bright stars. There are two ICU channels which work in cold redundancy. The ICU is responsible for the management of the payload, the communication with the SVM and the compression of scientific data before transmitting them as telemetry to the SVM. Data is routed through a SpaceWire network from FEU and MEU to the ICU, and then from the ICU to the SVM. For the FGS data, dedicated SpaceWire links between FEU and spacecraft AOCS are used. Figure 29 gives an overview of the PLATO data processing system architecture and of the data flow rates while Fig. 30 shows the engineering models during tests. It focuses on the sharing of the main functions and the data flows. It is a simplified view of the hardware architecture.

An on-board software is present in the ICU and both normal and fast DPUs. The ICU software is in charge of collecting all science data and housekeeping. It manages the PLATO payload sub-systems (DPS and FEE). In observation mode the N-DPU software must first assemble windows from the images-data-stream, received from the FEE. Then the software performs an initial treatment, which consists of computing the background noise and some correction parameters like smearing and offset. A part
<figure><img src="image_50.png" /><figcaption>**Fig. 29** Simplified overview of the PLATO on-board data flow</figcaption></figure>

of the image data will be sent to the ICU as imagettes without further processing. On a selection of stars, the N-DPU calculates the centroid and the received flux. Flux and centroid measurements are computed on-board using optimal binary mask as explained in Marchiori et al. [223]. The N-DPU is able to stack fluxes and centroids from each camera over periods of 50 seconds and 600 seconds and send it to the ICU. Before averaging the values of fluxes and centroids, an outlier rejection algorithm is used on-board. These data are then compressed by a factor of at least 2.5 for transmission to the SVM mass memory from where they are downloaded to the ground. The star catalogue defined on-ground will be uploaded in the ICU and then forwarded to the DPUs.

<figure><img src="image_51.png" /><figcaption>**Fig. 30** DPS engineering models test bench at DLR</figcaption></figure>

<figure><img src="image_52.png" /></figure>
The main purpose of the F-DPU is however to perform the attitude calculation of the F-CAMs based on the positions of the stars on the CCD. This Fine Guidance System (FGS) data processing using the knowledge of the camera geometrical model and the differential aberration is providing quaternions of the CAM attitude to the AOCS system of the spacecraft. This is a key component needed to reach the pointing performance presented in Table 8.

## 14 Synergies with other Missions

Exoplanet missions form a significant part of ESA and NASA's ongoing and future space science programs ([309] for an overview). PLATO will start its science operations in 2027. By this time, the now ongoing extended operations periods for CHEOPS and TESS will have ended, but further prolongations could extend their lifetimes until and beyond PLATO launch. Prolongation of James-Webb-Space-Telescope (JWST) operations beyond 2026 will allow it to observe PLATO targets. Two years after PLATO, the ARIEL mission is set to launch and plans to spectroscopically observe transiting exoplanets. Here we outline the key aspects of synergies with PLATO for these and other missions:

**TESS:** A discussion of the planet yield of PLATO versus TESS [282] can be found in Section 2. The majority of planets detected by TESS have orbital periods <10 days [147], while PLATO planets focus on orbital periods >27 days, including a significant fraction on long-periods >100 days. Most of the planet detections around solar-like stars from PLATO will have <4 $R_{Earth}$, outnumbering the numbers expected from TESS for this type of stars. There is a clear complementarity of TESS and PLATO. We note that if TESS enters a third extended mission period from 2026-2029, it will overlap with PLATO. This offers the opportunity for dedicated complementary observations where beneficial. This could include, for example, a pre-characterization of the PLATO field for short-period planets to prolonge TTV measurement baselines.

**CHEOPS:** The 30 cm-aperture space telescope is a follow-up mission carrying out high-precision photometry of known bright exoplanetary systems [39, 124]. CHEOPS has been used primarily to measure precise planetary radii, revising the composition of small planets (e.g. [45, 114, 199]), to confirm transiting long-period planets (e.g., [106, 261]), characterise multiplanet systems (e.g. [205, 220] and has also been used to characterise the emissive and reflective properties of planetary atmospheres (e.g. [53, 206]).

A major benefit to PLATO from CHEOPS results from improvements made in the planetary composition and structure modelling that inform the interpretation of precise planet radii and masses in terms of, e.g. planet formation, evolution and interior-atmosphere coupling. While many of the related science questions can only be fully answered when a larger sample of accurately characterised planets from PLATO becomes available, the ongoing activities within CHEOPS pave the way for PLATO data to come. With large parts of the PLATO LOPS2 field accessible to CHEOPS, a cross-calibration of CHEOPS and PLATO data of the same transits will benchmark the calibration of PLATO data (e.g. in terms of contamination removal). Preparatory observations of known transiting planets in the PLATO LOPS2 field by CHEOPS have
started and will be beneficial to maximising science return on these objects, crucially extending the baseline of transit observations for TTV studies.

**Ariel:** will provide spectra of the atmospheres of a large number (around 1000) of transiting planets [316]. These planets will mostly be hot and warm gaseous exoplanets (Jupiters, Saturns, Neptunes) as well as of super-Earths/sub-Neptunes orbiting bright stars of various types, with FG stars being the predominant host. Several surveys are already identifying potential Ariel targets that meet its mission objectives. For instance, TESS is expected to discover over 4500 planets around bright stars and more than 10000 giant planets around fainter stars (see Section 2). Other surveys, including PLATO, are expected to provide thousands of additional candidates suitable for study with Ariel. Notably, about 20-40 targets are expected to come from a PLATO LOPs (see also Nascimbeni et al. [348]). Moreover, PLATO will likely uncover new small, warm planets around bright stars, providing an exciting pool of additional candidate targets for Ariel. PLATO will play a crucial role by delivering high-precision planetary radii, extended TTV datasets, and refined ephemerides for planets within its fields. Data from PLATO's N-CAM (white-light phase curves) and F-CAMs (two-colour information) will further aid in prioritizing Ariel candidates, particularly for hot, nearby targets (see Section 3.3). The combined insights on radii, masses, and stellar parameters - especially stellar ages - will significantly enhance the scientific output of Ariel. For example, precise ages from PLATO will help break degeneracies in the study of warm Jupiters, enabling detailed investigations of planetary evolution, including contraction, atmospheric loss, and tidal interactions. In addition, PLATO's pre-characterization of stellar activity (e.g., rotational modulation, activity cycles, flare and CME frequencies, granulation) will be invaluable. These data will be particularly useful for targets observed simultaneously by both missions.

**JWST:** The main synergy of PLATO and JWST [134] concerns newly detected warm and/or small planets which can be followed up by JWST to investigate their atmospheres, phase curves and albedos. PLATO will form a target finder for JWST on these highly interesting targets in future and provide relevant complementary planet and stellar activity data (see discussion on ARIEL above).

**GAIA:** Through its astrometric survey of the Milky Way, Gaia [128] will discover a large population of massive planets (expected to be super-Neptunes and more massive), many of which will be at long periods. Most of these will be found from their trigonometric signatures but some may also be detectable through their transits. A significant harvest of new long period (> 5 years), massive exoplanets is expected in the upcoming Gaia data releases (e.g. Gaia DR4). For those with sufficient orbital information, inclinations could be accurate enough to predict potential transit times and if these fall with the PLATO observation fields monitoring observations will be possible at low cost. These long period, transiting planets, would be extremely valuable. While many of these systems may only transit once during the PLATO observations, combined modelling of the astrometric and transit observations will produce accurate orbital and planetary parameters. For PLATO itself, the GAIA observations not only form the basis of the PLATO input catalogue, but allow contamination with the PLATO targets/pixels to be estimated. Furthermore, while GAIA produces limited temporal coverage it may reveal the presence of line of sight background eclipsing binaries as has been demonstrated for TESS candidates by Panahi et al. [266]. This vetting

<figure><img src="image_53.png" /></figure>
capability will be extremely important in keeping the PLATO ground based followup tractable.

*Euclid and Roman Space telescope:* The Nancy Grace Roman Space telescope [308] is expected to detect exoplanets from microlensing, from transits and from coronographic imaging, covering a wide range of planet system parameters. ESA’s Euclid mission also has some capability to detect extrasolar planets, and studies demonstrating the joint detection capabilities of the two missions have been performed (e.g. [20, 185]). In particular the microlensing technique used by these missions has the potential to detect planets as small as Earth, and smaller, at orbital distances of 1 AU, although not with accurate planet parameters as anticipated by PLATO. Nevertheless, PLATO together with Roman and Euclid will be help solidify our understanding of the frequency of earth-sized planets in earth-like orbits. Both Euclid and the Roman Space Telescope will study a relatively distant stellar and hence planetary population which will contrast with the nearby PLATO planets. The large number of planets detected by these surveys will enable biases in their planet catch to be understood, hence leading to a better understanding of the planetary demographics in these different environments.

For all the missions discussed here, a combined analysis of their planetary frequencies will enable the most comprehensive picture of planetary demographics to be determined, allowing us to deduce how planets are born and evolve (through modelling).

## Appendix A

We outline briefly the simple analytic model of the estimation of planet radius accuracy. All calculations below are valid for beginning of life (BOL). We start from the following form of the conversion of V magnitudes to fluxes measurable by PLATO

$$f = 180000e^{-/s} \cdot 10^{-0.4(V-11)} \quad (1)$$

The noise level at flux $f$ can be estimated (Cabrera et al., in prep.) as:

$$N = \sqrt{(9 \cdot 10^{-6})^2 + \frac{1/f + (150/f)^2}{N_{\text{camera}} \cdot T/t_{\text{exp}}}} \quad (2)$$

Here $N$ is the noise level for $T = 1$ hour time-scale and $N_{\text{camera}} = 24$ was assumed. $t_{\text{exp}} = 25$s is the exposure cadence. The first constant term is the jitter-noise, the last term is the readout noise. It is assumed that the magnitude zero-point is the same for all cameras and the readout-noise is also independent on which camera we consider.

The radius ratio precision can be derived from the equation

$$\delta = \left( \frac{R_{\text{planet}}}{R_{\text{star}}} \right)^2 L_D \quad (3)$$

where $L_D$ describes the effect of limb darkening. The current knowledge of limb darkening for low magnetic field, quiet, solar-type stars is known sufficiently well that
the contribution to the uncertainty in the radius ratio is negligible (c.f. Section 4.4. of Maxted [230] as well as Ludwig et al. [217]). However, numerical simulations show that about over 800 Gauss surface magnetic field the theory predicts higher limb darkening than that was observed. In the same way, some simulations result in limb brightening effects difficult to understand at this point (see [217]). So, the very active stars can have different properties and more work is needed to calibrate properly their limb darkening behaviour (c.f. [7, 96, 119, 269]). The results are not changing if we consider different limb darkening laws; therefore, for sake of simplicity, we used linear limb darkening with a constant linear limb darkening coefficient $u = 0.6$ which is a solar-like value ($L_D = 1/(1 - u/3)$). Then we have by differentiation that

$$ \frac{\Delta k}{k} = \frac{\sqrt{2} N(V)}{2 \delta} \frac{1}{\sqrt{N_{\text{transit}} D}} \quad (4) $$

abbreviating the planet-to-star radius ratio $k = R_{\text{planet}}/R_{\text{star}}$. The factor $\sqrt{2}$ is valid if the baseline is determined by observing only one full transit duration length before and after the transit. However, the factor will decrease to 1 if the baseline length is much longer than the transit duration (in the limit to infinity). Since the noise level is calculated for 1 hour in Cabrera et al. (in prep), the transit duration $D$ plays a role here. Despite the simplicity of this analytic model, the results are in quite good agreement with [26, 248]; and [98].

**Acknowledgements** This work presents results from the European Space Agency (ESA) space mission PLATO. The PLATO payload, the PLATO Ground Segment, and PLATO data processing are joint developments of ESA and the PLATO Mission Consortium (PMC). Funding for the PMC is provided at national levels, in particular by countries participating in the PLATO Multilateral Agreement (Austria, Belgium, Czech Republic, Denmark, France, Germany, Italy, Netherlands, Portugal, Spain, Sweden, Switzerland, Norway, and United Kingdom) and institutions from Brazil. Members of the PLATO Consortium can be found at https://platomission.com/. The ESA PLATO mission website is https://www.cosmos.esa.int/plato. We thank the teams working for PLATO for all their work. The authors gratefully thank David Ciardi and an unknown referee for carefully reading this publication and providing many helpful comments for clarifying the current status of PLATO to a large readership. Specific acknowledgements: The German PMC, PDC, DPS, and F-FEE team members are supported by the German Aerospace Agency (Deutsches Zentrum für Luft- und Raumfahrt, e.V., DLR) grant numbers 50001401, 500P2001, 500P2103, 500P2104, 500P2101, 500P1902, and 500P2102. The DLR team members acknowledge the funding by the Research and Development Department of the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt, e.V., DLR). M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. The contribution of M.L. has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. The research and results presented in this paper have received funding from the Belgian Federal Science Policy Office (BELSPO) through various PRODEX grants for PLATO development and from the KU Leuven Research Council (grant C16/18/005: PARADISE). This project was supported by the KKP-137523 "SeismoLab" Élvonal grant of the Hungarian Research, Development and Innovation Office (NKFIH) and by the Lendület Program of the Hungarian Academy of Sciences under project No. LP2018-7. Project no. C1746651 has been implemented with the support provided by the Ministry of Culture and Innovation of Hungary from the National Research, Development and Innovation Fund, financed under the NVKDP-2021 funding scheme. This work was supported by the Hungarian National Research, Development and Innovation Office grants OTKA K131508 and KH-130526, and the Élvonal grant KKP-143986. Authors acknowledge the financial support of the Austrian-Hungarian Action Foundation (101"ou13, 112"ou1). This work was supported by Fundação para a Ciência e a Tecnologia (FCT) through research grants UIDB/04434/2020 and UIDP/04434/2020. This work was supported by FCT - Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Com-
petitividade e Internacionalização by these grants: UIDB/04434/2020; UIDP/04434/2020 and co-funded by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. Views and opinions expressed are, however, those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work was (partially) supported by the Spanish MICIN/AEI/10.13039/501100011033 and by "ERDF A way of making Europe" by the "European Union" through grant PID2021-122842OB-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia 'María de Maeztu') through grant CEX2019-000918-M. This work is part of the project Advanced technologies for the exploration of the Universe and its components, of the area of Astrophysics and High Energy Physics, within the frame of the R&D&I Complementary Plans of the Spanish Government that are part component 17 of the Recovery and Resilience Mechanism. This contract is funded by the European Union - NextGenerationEU (MICIN/PRTR funds) and by Generalitat de Catalunya. We acknowledge financial support from the Agency Estatal de Investigación of the Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 and the ERDF "A way of making Europe" through project PID2021-125627OB-C31, from the Centre of Excellence "María de Maeztu" award to the Institut de Ciències de l'Espai (CEX2020-001058-M) and from the Generalitat de Catalunya/CERCA programme. Funding for the Stellar Astrophysics Centre was provided by The Danish National Research Foundation (Grant DNRF106). Support from PLATO ASI-INAF agreements n. 2022-28-HH.0. Giampaolo Piotto, Marco Montalto, Luca Malavolta, Valerio Nascimbeni, Luca Borsato, Giacomo Mantovan, Valentina Granata: Support from PLATO ASI-INAF agreements n. 2022-28-HH.0. This study is supported by the Research Council of Norway through its Centres of Excellence funding scheme, project number 223272 (CEED) and 332523 (PHAB). Brazilian participation on the PLATO mission is funded by Fundação de Amparo á Pesquisa do Estado de São Paulo (FAPESP) under grant 2016/13750-6. The team at IAC acknowledges support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under grant 'Contribution of the IAC to the PLATO Space Mission' with reference PID2019-107061GB-C66, DOI: 10.13039/501100011033. U.C.Kolb and C.A. Haswell were supported by grant ST/T000295/1 from STFC. C.A. Haswell was supported by grant ST/X001164/1 from STFC. NW, SA, PB, GB, FDA, DWE, DF, DLH, SH, JI, NM, MR, GR, LS, MW have been fully or partly supported by grant funding from the UK Space Agency through grants ST/R004838/1 and ST/X001571/1. The PDPC-C hardware is largely provided through the UK STFC IRIS digital research infrastructure (https://www.iris.ac.uk) project. D.M.B. gratefully acknowledges a senior postdoctoral fellowship from the Research Foundation Flanders (FWO; grant number [1286521N]), the Engineering and Physical Sciences Research Council (EPSRC) of UK Research and Innovation (UKRI) in the form of a Frontier Research grant under the UK government's ERC Horizon Europe funding guarantee (SYMPHONY; grant number [EP/Y031059/1]), and a Royal Society University Research Fellowship (grant number: URF\R1\231631). PK and MK would like to acknowledge the funding of the CZ contribution to PLATO mission from ESA PRODEX under PEA-4000127913 contract. MS and RK would like to acknowledge the funding from the LTT-20015 grant of the MEYS. UH, OK, TO acknowledge support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). I.L. and A.B. extend their gratitude to the Fundação para a Ciência e Tecnologia (FCT, Portugal) for the financial support provided to the Center for Astrophysics and Gravitation (CENTRA/IST/ULisboa) under Grant Project No. UIDB/00099/2020. The work of the Porto team was supported by FCT - Fundação para a Ciência e a Tecnologia through national funds by grants: UIDB/04434/2020; UIDP/04434/2020. The Portuguese team thanks the Portuguese Space Agency for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contracts number 4000133026, 4000140773, and 4000124770. CAB and INTA authors are funded by Spanish MCIN/AEI/10.13039/501100011033 grants PID2019-107061GB-C61 and -C62. JPG, MLM, JRR, ARB, and RGH acknowledge financial support from project PID2019-107061GB-C63 from the 'Programas Estatales de Generación de Conocimiento y Fortalecimiento Científico y Tecnológico del Sistema de I+D+i y de I+D+i Orientada a los Retos de la Sociedad. E.A.'s work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. RA acknowledges funding from the Science & Technology Facilities Council (STFC) through Consolidated Grant ST/W000857/1. Paul Beck acknowledges support by the Spanish Ministry of Science and Innovation with the Ramón y Cajal fellowship number RYC-2021-033137-I and the number MRR4032204. S.M. acknowledges support from the Spanish Ministry of Science and Innovation (MICINN) with the Ramón y Cajal fellowship no. RYC-2015-17697, the grant no. PID2019-107187GB-I00, and through AEI under the Severo Ochoa Centres of Excellence Programme
2020–2023 (CEX2019-000920-S). JMMH is funded by Spanish MCIN/AEI/10.13039/501100011033 grant PID2019-107061GB-C61. M.L.M. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. J.P.G. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. C.P.M. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. F.J.P. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. J.R.G. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. M.A.S.C. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. R.S.M. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. M.V.A. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. B.A.M. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. A.C. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. J.M.G.L. acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. Juan Carlos Morales acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 and the ERDF "A way of making Europe" through project PID2021-125627OB-C31, from the Centre of Excellence "María de Maeztu" award to the Institut de Ciències de l'Espai (CEX2020-001058-M) and from the Generalitat de Catalunya/CERCA programme. Ignasi Ribas acknowledges financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 and the ERDF "A way of making Europe" through project PID2021-125627OB-C31, from the Centre of Excellence "María de Maeztu" award to the Institut de Ciències de l'Espai (CEX2020-001058-M) and from the Generalitat de Catalunya/CERCA programme. Aldo Serenelli acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 and the ERDF "A way of making Europe" through project PID2021-125627OB-C31, from the Centre of Excellence "María de Maeztu" award to the Institut de Ciències de l'Espai (CEX2020-001058-M) and from the Generalitat de Catalunya/CERCA programme. DJA is supported by UKRI through the STFC (ST/R00384X/1) and EPSRC (EP/X027562/1). SLC acknowledges funding from the Science & Technology Facilities Council (STFC) through an Ernest Rutherford Research Fellowship ST/R003726/1. PPA acknowledges the support of Fundação para a Ciência e Tecnologia FCT/MCTES, Portugal, through national funds by the following grants UIDB/04434/2020, UIDP/04434/2020.FCT, 2022.03993.PTDC. Tiago Campante is supported by FCT in the form of a work contract (CEECIND/00476/2018). MC acknowledges the support of Fundação para a Ciência e Tecnologia FCT/MCTES, Portugal, through national funds by these grants UIDB/04434/2020, UIDP/04434/2020.FCT, 2022.06962.PTDC.FCT, 2022.03993.PTDC and CEECIND/02619/2017. ZsB acknowledges support by the János Bolyai Research Scholarship of the Hungarian Academy of Sciences. Gy. M. Szabó acknowledges support from the PRODEX Experiment Agreement No. 4000137122. Róbert Szabó: Lendület Program of the Hungarian Academy of Sciences, project No. LP2018-7/2022. Róbert Szabó: KKP-137523 "SeismoLab" Élvonal grant of the Hungarian Research, Development and Innovation Office (NKFIH). Róbert Szabó: MW-Gaia COST Action (CA18104). KV was supported by the Bolyai János Research Scholarship of the Hungarian Academy of Sciences, and by the Bolyai+ grant ÚNKP-22-5-ELTE-1093. Thibault Merle is granted by the BELSPO Belgian federal research program FED-tWIN under the research profile Prf-2020-033 BISTRO. Thierry Morel acknowledges financial support from Belspo for contract PRODEX PLATO mission development. S.N.B acknowledges support from PLATO ASI-INAF agreement n. 2015-019-R.1-2018. DLB acknowledges support from NASA through the Astrophysics Science Smallsat Studies program (80NSSC20K1246) and the TESS GI Program (80NSSC21K0334). DBdeF acknowledges financial support from the Brazilian agency CNPq-PQ2 (Grant No. 305566/2021-0). Research activities of STELLAR TEAM of Federal University of Ceará are supported by continuous grants from the Brazilian agency CNPq. J. K. gratefully acknowledges the support of the Swedish National Space Agency (SNSA; DNR 2020-00104) and of the Swedish Research Council (VR: Etableringsbidrag 2017-04945). AJM acknowledges support from the Swedish Research Council (grant 2017-04945) and the Swedish National Space Agency (grant 120/19C). Support for MC is provided by ANID grants ICN12_009 (Millennium Institute of Astrophysics, FB10003 (Basal-CATA2), and 1231637 (FONDECYT). CD acknowledges SNSF under grant TMSGI2_211313. MK acknowledges the support from ESA-PRODEX PEA-4000127913. TL was supported by a grant from the Branco Weiss Foundation. PM acknowledges support from STFC research grant number ST/M001040/1. F.J.P. acknowledges financial support from the grant CEX2021-
001131-S funded by MCIN/AEI/ 10.13039/501100011033. BR-A acknowledges funding support from FONDECYT Iniciación grant 11181295 and ANID Basal project FB210003. A.R.G.S. acknowledges the support by FCT through national funds and by FEDER through COMPETE2020 by these grants: UIDB/04434/2020 & UIDP/04434/2020. A.R.G.S. is supported by FCT through the work contract No. 2020.02480.CEECIND/CP1631/CT0001. CdB acknowledges support from a Beatriz Galindo senior fel- lowship (BG22/00166) from the Spanish Ministry of Science, Innovation and Universities. This work was also supported by the NKFIH excellence grant TKP2021-NKTA-64. This work on the PLATO space mis- sion was supported by CNES by The French teams acknowledge support by the Centre national d’études spatiales (CNES), on both the payload and the PDC development, through various grants.

**Author Contributions** To be completed for final manuscript, in view of about 800 co-authors to add.

**Funding** Open Access funding enabled and organized by Projekt DEAL.

**Data Availability** Data underlying the simulations presented in the manuscript are available by the authors upon request.

## Declarations

**Competing Interests** The authors declare no competing interests.

**Open Access** This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/.

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**Publisher's Note** Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

## Authors and Affiliations

Heike Rauer¹,², ∗ · Conny Aerts³ · Juan Cabrera¹ · Magali Deleuil⁴ ·

Anders Erikson¹ · Laurent Gizon⁵ · Mariejo Goupil⁶ · Ana Heras⁷ ·

Thomas Walloschek⁷ · Jose Lorenzo-Alvarez⁷ · Filippo Marliani⁷ ·

César Martin-Garcia¹,⁸ · J. Miguel Mas-Hesse⁹ · Laurence O'Rourke⁸ ·

Hugh Osborn¹⁰ · Isabella Pagano¹¹ · Giampaolo Piotto¹² · Don Pollacco¹³ ·

Roberto Ragazzoni¹⁴ · Gavin Ramsay¹⁵ · Stéphane Udry¹⁶ ·

Thierry Appourchaux¹⁷ · Willy Benz¹⁰ · Alexis Brandeker¹⁸ · Manuel Güdel¹⁹ ·

Eduardo Janot-Pacheco²⁰ · Petr Kabath²¹ · Hans Kjeldsen²² · Michiel Min²³ ·

Nuno Santos²⁴,²⁵ · Alan Smith²⁶ · Juan-Carlos Suarez²⁷ ·

Stephanie C. Werner²⁸ · Alessio Aboudan²⁹ · Manuel Abreu³⁰ ·

Lorena Acuña³¹ · Moritz Adams³² · Vardan Adibekyan²⁴ · Laura Affer³³ ·

François Agneray⁴ · Craig Agnor³⁴ · Victor Aguirre Børsen-Koch³⁵ ·

Saad Ahmed³⁶ · Suzanne Aigrain³⁷ · Ashraf Al-Bahlawan²⁶ ·

Ma de los Angeles Alcacera Gil³⁸ · Eleonora Alei¹⁴,¹⁵⁰ · Silvia Alencar⁴⁰ ·

Richard Alexander⁴¹ · Julia Alfonso-Garzón⁹ · Yann Alibert¹⁰ · Carlos Allende

Prieto⁴²,⁴³ · Leonardo Almeida⁴⁴ · Roi Alonso Sobrino⁴²,⁴³ ·

Giuseppe Altavilla⁴⁵,⁶⁸ · Christian Althaus¹ · Luis Alonso Alvarez Trujillo³⁸ ·

Anish Amarsi⁴⁶ · Matthias Ammler-von Eiff⁵ · Eduardo Amôres⁴⁷ ·

Laerte Andrade⁴⁸ · Alexandros Antoniadis-Karnavas²⁴ · Carlos António⁴⁹ ·

Beatriz Aparicio del Moral⁵⁰ · Matteo Appolloni⁷ · Claudio Arena¹¹ ·

David Armstrong¹³ · Jose Aroca Aliaga⁷ · Martin Asplund⁵¹ ·

Jeroen Audenaert³,⁵² · Natalia Auricchio⁵³ · Pedro Avelino²⁴,²⁵ ·

Ann Baeke⁵⁴ · Kevin Baillié⁵⁵ · Ana Balado³⁸ · Pau Ballber Balagueró⁹³,¹⁰² ·

Andrea Balestra¹⁴ · Warrick Ball⁵⁶ · Herve Ballans¹⁷ · Jerome Ballot⁵⁷ ·

Caroline Barban⁶ · Gaële Barbary⁶ · Mauro Barbieri⁵⁸ · Sebastià Barceló

Forteza⁹ · Adrian Barker⁵⁹ · Paul Barklem⁴⁶ · Sydney Barnes⁶⁰ ·

David Barrado Navascues⁹ · Oscar Barragan³⁷ · Clément Baruteau⁵⁷ ·

Sarbani Basu⁶¹ · Frederic Baudin¹⁷ · Philipp Baumeister¹ · Daniel Bayliss¹³ ·

Michael Bazot⁶² · Paul G. Beck⁴²,⁴³,⁶³ · Kevin Belkacem⁶ · Earl Bellinger⁶⁵ ·
Serena Benatti³³ · Othman Benomar⁶⁶,⁶⁷ · Diane Bérard⁵⁵ ·

Maria Bergemann³¹ · Maria Bergomi⁶⁸ · Pierre Bernardo⁴ · Katia Biazzo¹¹ ·

Andrea Bignamini⁶⁹ · Lionel Bigot⁷⁰ · Nicolas Billot¹⁶ · Martin Binet¹³ ·

David Biondi⁷¹ · Federico Biondi⁶⁸ · Aaron C. Birch⁵ · Bertram Bitsch³¹ ·

Paz Victoria Bluhm Ceballos² · Attila Bódi⁷²,⁷³ · Zsófia Bognár⁷²,⁷³ ·

Isabelle Boisse⁴ · Emeline Bolmont⁷⁴ · Alfio Bonanno¹¹ ·

Mariangela Bonavita⁷⁵ · Andrea Bonfanti⁷⁶ · Xavier Bonfils⁷⁷ ·

Rosaria Bonito³³ · Aldo Stefano Bonomo⁷⁸ · Anko Börner⁷⁹ · Sudeshna Boro ·

Saikia¹⁹ · Elisa Borreguero Martín³⁸ · Francesco Borsa⁸⁰ · Luca Borsato¹⁴ ·

Diego Bossini²⁴ · Francois Bouchy⁷⁴ · Gwenaël Boué⁵⁵ · Rodrigo Boufleur⁸¹ ·

Patrick Boumier¹⁷ · Vincent Bourrier⁷⁴ · Dominic M. Bowman³,⁸² ·

Enrico Bozzo¹⁶ · Louisa Bradley²⁶ · John Bray⁸³ · Alessandro Bressan⁸⁴ ·

Sylvain Breton¹¹ · Daniele Brienza⁷¹ · Ana Brito⁸⁵,²²⁰ · Matteo Brogi⁸⁶ ·

Beverly Brown⁷ · David J. A. Brown¹³ · Allan Sacha Brun⁸⁷ ·

Giovanni Bruno¹¹ · Michael Bruns⁵ · Lars A. Buchhave⁸⁸ · Lisa Bugnet⁸⁹ ·

Gaël Buldgen⁷⁴ · Patrick Burgess³⁶ · Andrea Busatta¹¹ · Giorgia Busso³⁶ ·

Derek Buzasi⁹⁰ · José A. Caballero⁹ · Alexandre Cabral³⁰ ·

Juan-Francisco Cabrero Gomez⁴² · Flavia Calderone¹¹ · Robert Cameron⁵ ·

Andrew Cameron⁹¹ · Tiago Campante²⁴ · Néstor Campos Gestal⁹³,¹⁰² ·

Bruno Leonardo Canto Martins⁴⁴ · Christophe Cara⁸⁷ · Ludmila Carone⁷⁶ ·

Josep Manel Carrasco³⁹,⁹²,⁹³ · Luca Casagrande⁵¹ · Sarah L. Casewell⁴¹ ·

Santi Cassisi⁹⁴,⁹⁵ · Marco Castellani⁶⁸ · Matthieu Castro⁴⁴ · Claude Catala⁶ ·

Irene Catalán Fernández³⁸ · Márcio Catelan⁹⁶,⁹⁷ · Heather Cegla¹³ ·

Chiara Cerruti³⁸ · Virginie Cessa¹⁰ · Merieme Chadid⁷⁰ · William Chaplin⁵⁶ ·

Stephane Charpinet⁵⁷ · Cristina Chiappini⁶⁰ · Simone Chiarucci⁹⁸ ·

Andrea Chiavassa⁷⁰ · Simonetta Chinellato⁶⁸ · Giovanni Chirulli⁷ ·

Jørgen Christensen-Dalsgaard⁹⁹ · Ross Church¹⁰⁰ · Antonio Claret⁵⁰ ·

Cathie Clarke³⁶ · Riccardo Claudi¹⁴ · Lionel Clermont⁵⁴ · Hugo Coelho⁴⁴ ·

Joao Coelho³⁰ · Fabrizio Cogato⁵³,¹⁰¹ · Josep Colomé⁹³,¹⁰² ·

Mathieu Condamin¹⁰³ · Fernando Conde García³⁸ · Simon Conseil⁴ ·

Thierry Corbard⁷⁰ · Alexandre C. M. Correia¹⁰⁴ · Enrico Corsaro¹¹ ·

Rosario Cosentino¹⁰⁵ · Jean Costes⁴ · Andrea Cottinelli¹⁴ ·

Giovanni Covone¹⁰⁶ · Orlagh L. Creevey⁷⁰ · Aurelien Crida⁷⁰ ·

Szilard Csizmadia¹ · Margarida Cunha²⁴ · Patrick Curry²⁶ · Jefferson da ·

Costa⁴⁴ · Francys da Silva⁴⁴ · Shweta Dalal¹⁰⁷ · Mario Damasso⁷⁸ ·

Cilia Damiani⁵ · Francesco Damiani³³ · Maria Liduina das Chagas¹⁰⁸ ·

Melvyn Davies¹⁰⁹ · Guy Davies⁵⁶ · Ben Davies¹¹⁰ · Gary Davison²⁶ ·

Leandro de Almeida⁴⁴,¹¹¹ · Francesca de Angeli³⁶ · Susana Cristina Cabral de ·

Barros²⁴ · Izan de Castro Leão⁴⁴ · Daniel Brito de Freitas¹¹² · Marcia Cristina de ·

Freitas⁴⁰ · Domitilla De Martino¹¹³ · José Renan de Medeiros⁴⁴ ·

Luiz Alberto de Paula²⁰ · Álvaro de Pedraza Gómez³⁸ · Jelle de Plaa²³ ·

Joris De Ridder³ · Morgan Deal¹¹⁴ · Leen Decin³ · Hans Deeg⁴²,⁴³ ·

Scilla Degl'Innocenti¹¹⁵ · Sebastien Deheuvels⁵⁷ · Carlos del Burgo⁴²,⁴³ ·

Fabio Del Sordo¹¹ · Elisa Delgado-Mena²⁴ · Olivier Demangeon²⁴ ·

Tilmann Denk¹ · Aliz Derekas¹¹⁶ · Jean-Michel Desert²²³ · Silvano Desidera¹⁴ ·

Marc Dexet¹⁷ · Marcella Di Criscienzo⁶⁸ · Anna Maria Di Giorgio⁷¹ ·

<figure><img src="image_54.png" /></figure>
Maria Pia Di Mauro<sup>71</sup> · Federico Jose Diaz Rial<sup>117</sup> · José-Javier Díaz-García<sup>42</sup>.

Marco Dima<sup>68</sup> · Giacomo Dinuzzi<sup>71</sup> · Odysseas Dionatos<sup>19</sup> · Elisa Distefano<sup>68</sup>.

Jose-Dias do Nascimento Jr.<sup>44</sup> · Albert Domingo<sup>9</sup> · Valentina D'Orazi<sup>14</sup>.

Caroline Dorn<sup>118</sup> · Lauren Doyle<sup>13</sup> · Elena Duarte<sup>30</sup> · Florent Ducellier<sup>6</sup>.

Luc Dumaye<sup>87</sup> · Xavier Dumusque<sup>74</sup> · Marc-Antoine Dupret<sup>54</sup>.

Patrick Eggenberger<sup>74</sup> · David Ehrenreich<sup>74</sup> · Philipp Eigmüller<sup>1</sup>.

Johannes Eising<sup>79</sup> · Marcelo Emilio<sup>48</sup> · Kjell Eriksson<sup>46</sup> · Marco Ermocida<sup>7</sup>.

Riano Isidoro Escate Giribaldi<sup>119</sup> · Yoshi Eschen<sup>13</sup> · Lucía Espinosa Yáñez<sup>38</sup>.

Inês Estrela<sup>49</sup> · Dafydd Wyn Evans<sup>36</sup> · Damian Fabbian<sup>148,224,225</sup>.

Michele Fabrizio<sup>45,68</sup> · João Pedro Faria<sup>24</sup> · Maria Farina<sup>71</sup>.

Jacopo Farinato<sup>68</sup> · Dax Feliz<sup>121</sup> · Sofia Feltzing<sup>100</sup> · Thomas Fenouillet<sup>4</sup>.

Miguel Fernández<sup>38</sup> · Lorenza Ferrari<sup>23</sup> · Sylvio Ferraz-Mello<sup>20</sup>.

Fabio Fialho<sup>122</sup> · Agnes Fienga<sup>70</sup> · Pedro Figueira<sup>123</sup> · Laura Fiori<sup>79</sup>.

Ettore Flaccomio<sup>33</sup> · Mauro Focardi<sup>98</sup> · Steve Foley<sup>124</sup> · Jean Fontignie<sup>87</sup>.

Dominic Ford<sup>36</sup> · Karin Fornazier<sup>20</sup> · Thierry Forveille<sup>77</sup> · Luca Fossati<sup>76</sup>.

Rodrigo de Marca Franca<sup>125</sup> · Lucas Franco da Silva<sup>122</sup> · Antonio Frasca<sup>11</sup>.

Malcolm Fridlund<sup>126</sup> · Marco Furlan<sup>125</sup> · Sarah-Maria Gabler<sup>5</sup> · Marco Gaido<sup>7</sup>.

Andrew Gallagher<sup>31</sup> · Paloma I. Gallego Sempere<sup>38</sup> · Emanuele Galli<sup>71</sup>.

Rafael A. García<sup>87</sup> · Antonio García Hernández<sup>27</sup> · Antonio Garcia Munoz<sup>87</sup>.

Hugo García-Vázquez<sup>42</sup> · Rafael Garrido Haba<sup>50</sup> · Patrick Gaulme<sup>5,127</sup>.

Nicolas Gauthier<sup>6</sup> · Charlotte Gehan<sup>5</sup> · Matthew Gent<sup>128</sup> · Iskra Georgieva<sup>126</sup>.

Mauro Ghigo<sup>68</sup> · Edoardo Giana<sup>7</sup> · Samuel Gill<sup>13</sup> · Leo Girardi<sup>68</sup>.

Silvia Giuliatti Winter<sup>129</sup> · Giovanni Giusi<sup>71</sup> · João Gomes da Silva<sup>24</sup>.

Luis Jorge Gómez Zazo<sup>38</sup> · Juan Manuel Gomez-Lopez<sup>50</sup> · Jonay Isai González

Hernández<sup>42,43</sup> · Kevin Gonzalez Murillo<sup>55</sup> · Alejandro Gonzalo Melchor<sup>38</sup>.

Nicolas Gorius<sup>11</sup> · Pierre-Vincent Gouel<sup>6</sup> · Duncan Goultty<sup>7</sup>.

Valentina Granata<sup>14,130</sup> · John Lee Grenfell<sup>1</sup> · Denis Grießbach<sup>79</sup>.

Emmanuel Grolleau<sup>6</sup> · Salomé Grouffal<sup>4</sup> · Sascha Grziwa<sup>131</sup>.

Mario Giuseppe Guarcello<sup>33</sup> · Loïc Gueguen<sup>6</sup> · Eike Wolf Guenther<sup>127</sup>.

Terrasa Guilhem<sup>54</sup> · Lucas Guillerot<sup>17</sup> · Tristan Guillot<sup>70</sup> · Pierre Guiot<sup>17</sup>.

Pascal Guterman<sup>4</sup> · Antonio Gutiérrez<sup>49</sup> · Fernando Gutiérrez-Canales<sup>6</sup>.

Janis Hagelberg<sup>16</sup> · Jonas Haldemann<sup>10</sup> · Cassandra Hall<sup>132</sup>.

Rasmus Handberg<sup>22</sup> · Ian Harrison<sup>7</sup> · Diana L. Harrison<sup>36,133</sup>.

Johann Hasiba<sup>76</sup> · Carole A. Haswell<sup>75</sup> · Petra Hatalova<sup>28</sup> · Artie Hatzes<sup>127</sup>.

Raphaëlle Haywood<sup>107</sup> · Guillaume Hébrard<sup>134</sup> · Frank Heckes<sup>5</sup>.

Ulrike Heiter<sup>46</sup> · Saskia Hekker<sup>62</sup> · René Heller<sup>5</sup> · Christiane Helling<sup>76</sup>.

Krzysztof Helminiak<sup>135</sup> · Simon Hemsley<sup>26</sup> · Kevin Heng<sup>10</sup> · Konstantin Herbst<sup>1,222</sup> · Aline Hermans<sup>54</sup> · JJ Hermes<sup>136</sup> · Nadia Hidalgo Torres<sup>7</sup>.

Natalie Hinkel<sup>137</sup> · David Hobbs<sup>100</sup> · Simon Hodgkin<sup>36</sup> · Karl Hofmann<sup>76</sup>.

Saeed Hojjatpanah<sup>4</sup> · Günter Houdek<sup>22</sup> · Daniel Huber<sup>138</sup> · Joseph Huesler<sup>7</sup>.

Alain Hui-Bon-Hoa<sup>57</sup> · Rik Huygen<sup>3</sup> · Duc-Dat Huynh<sup>87</sup> · Nicolas Iro<sup>19</sup>.

Jonathan Irwin<sup>36</sup> · Mike Irwin<sup>36</sup> · André Izidoro<sup>129,139</sup> · Sophie Jacquinod<sup>6</sup>.

Nicholas Emborg Jannsen<sup>3</sup> · Markus Janson<sup>18</sup> · Harald Jeszenszky<sup>76</sup>.

Chen Jiang<sup>5</sup> · Antonio José Jimenez Mancebo<sup>42,43</sup> · Paula Jofre<sup>140</sup>.

Anders Johansen<sup>100</sup> · Cole Johnston<sup>3</sup> · Geraint Jones<sup>26</sup> · Thomas Kallinger<sup>19</sup>.

Szilárd Kálmán<sup>72,116,141,142</sup> · Thomas Kanitz<sup>7</sup> · Marie Karjalainen<sup>21</sup>.
Raine Karjalainen²¹ · Christoffer Karoff²²,¹⁴³ · Steven Kawaler¹⁴⁴ ·

Daisuke Kawata²⁶ · Arnoud Keereman⁷ · David Keiderling⁵ · Tom Kennedy²⁶ ·

Matthew Kenworthy¹⁴⁵ · Franz Kerschbaum¹⁹ · Mark Kidger⁸ ·

Flavien Kiefer⁶ · Christian Kintziger⁵⁴ · Kristina Kislyakova¹⁹ ·

László Kiss⁷²,¹⁸¹ · Peter Klagyivik² · Hubert Klahr¹²⁸ · Jonas Klevas¹⁴⁶ ·

Oleg Kochukhov⁴⁶ · Ulrich Köhler¹ · Ulrich Kolb⁷⁵ · Alexander Koncz¹ ·

Judith Korth¹⁴⁷ · Nadiia Kostogryz⁵ · Gábor Kovács⁷² · József Kovács¹¹⁶ ·

Oleg Kozhura⁷⁵ · Natalie Krivova⁵ · Arūnas Kučinskas¹⁴⁶ · Ilyas Kuhlemann⁵ ·

Friedrich Kupka¹⁴⁸,²²⁴,²²⁵ · Wouter Laauwen¹⁴⁹ · Alvaro Labiano⁸ ·

Nadege Lagarde²²¹ · Philippe Laget⁷ · Gunter Laky⁷⁶ ·

Kristine Wai Fun Lam¹ · Michiel Lambrechts¹⁰⁰ · Helmut Lammer⁷⁶ ·

Antonino Francesco Lanza¹¹ · Alessandro Lanzafame¹⁵¹ · Mariel Lares

Martiz⁵⁰ · Jacques Laskar⁵⁵ · Henrik Latter¹⁵² · Tony Lavanant⁸⁷ ·

Alastair Lawrenson²⁶ · Cecilia Lazzoni¹⁴ · Agnes Lebre¹¹⁴ ·

Yveline Lebreton⁶,¹⁵³ · Alain Lecavelier des Etangs¹³⁴ · Katherine Lee³¹ ·

Zoe Leinhardt¹⁵⁴ · Adrien Leleu⁷⁴ · Monika Lendl⁷⁴ · Giuseppe Leto¹¹ ·

Yves Levillain⁷ · Anne-Sophie Libert¹⁵⁵ · Tim Lichtenberg¹⁵⁶ ·

Roxanne Ligi⁷⁰ · Francois Lignieres⁵⁷ · Jorge Lillo-Box⁹ · Jeffrey Linsky¹⁵⁷ ·

John Scige Liu⁷¹ · Dominik Loidolt¹⁹ · Yuying Longval¹⁷ · Ilídio Lopes⁸⁵ ·

Andrea Lorenzani⁹⁸ · Hans-Guenter Ludwig¹⁵⁸ · Mikkel Lund²² ·

Mia Sloth Lundkvist²² · Xavier Luri³⁹,⁹²,⁹³ · Carla Maceroni⁷¹ · Sean Madden⁷ ·

Nikku Madhusudhan³⁶ · Antonio Maggio³³ · Christian Magliano¹⁰⁶ ·

Demetrio Magrin¹⁴ · Laurent Mahy¹⁵⁹ · Olaf Maibaum¹⁶⁰ ·

LeeRoy Malac-Allain⁶ · Jean-Christophe Malapert¹⁶¹ · Luca Malavolta¹²,¹⁴ ·

Jesus Maldonado³³ · Elena Mamonova²⁸ · Louis Manchon⁵ ·

Andres Manjón³⁸ · Andrew Mann¹⁶² · Giacomo Mantovan¹² ·

Luca Marafatto⁶⁸ · Marcella Marconi¹¹³ · Rosemary Mardling¹⁶³ ·

Paola Marigo¹² · Silvia Marinoni⁴⁵,⁶⁸ · Rico Marques¹²⁵ ·

Joao Pedro Marques¹⁷ · Paola Maria Marrese⁴⁵,⁶⁸ · Douglas Marshall¹⁶⁴ ·

Silvia Martínez Perales³⁸ · David Mary⁷⁰ · Francesco Marzari¹² ·

Eduard Masana³⁹,⁹²,⁹³ · Andrina Mascher⁷⁹ · Stéphane Mathis⁸⁷ ·

Savita Mathur⁴²,⁴³ · Iris Martín Vodopivec³⁸ · Ana Carolina Mattiuci ·

Figueiredo⁴⁴ · Pierre F. L. Maxted¹⁶⁵ · Tsevi Mazeh¹⁶⁶ · Stephane Mazevet¹⁶⁷ ·

Francesco Mazzei⁷¹ · James McCormac¹³ · Paul McMillan¹⁰⁰ · Lucas Menou⁴ ·

Thibault Merle¹¹⁹,¹⁵⁹ · Farzana Meru¹³ · Dino Mesa⁶⁸ · Sergio Messina¹¹ ·

Szabolcs Mészáros¹¹⁶,¹⁶⁸ · Nadége Meunier⁷⁷ · Jean-Charles Meunier⁴ ·

Giuseppina Micela³³ · Harald Michaelis¹ · Eric Michel⁶ · Mathias Michielsen³ ·

Tatiana Michtchenko²⁰ · Andrea Miglio¹⁰¹ · Yamila Miguel¹⁴⁵ ·

David Milligan¹²⁴ · Giovanni Mirouh¹⁶⁹ · Morgan Mitchell¹³ ·

Nuno Moedas²⁴ · Francesca Molendini⁷ · László Molnár⁷²,¹⁸¹ ·

Joey Mombarg³ · Josefina Montalban¹⁰¹ · Marco Montalto¹² ·

Mário J. P. F. G. Monteiro²⁴ · Francisco Montoro Sánchez³⁸ ·

Juan Carlos Morales⁹³,¹⁰² · Maria Morales-Calderon⁹ ·

Alessandro Morbidelli⁷⁰ · Christoph Mordasini¹⁷⁰ · Chrystel Moreau⁴ ·

Thierry Morel⁵⁴ · Giuseppe Morello⁵⁰ · Julien Morin¹¹⁴ · Annelies Mortier⁵⁶ ·

Benoît Mosser⁶ · Denis Mourard⁷⁰ · Olivier Mousis⁴ · Claire Moutou⁵⁷ ·
Nami Mowlavi<sup>74</sup> · Andrés Moya<sup>171</sup> · Prisca Muehlmann<sup>7</sup> · Philip Muirhead<sup>136</sup>.

Matteo Munari<sup>11</sup> · Ilaria Musella<sup>113</sup> · Alexander James Mustill<sup>147</sup>.

Nicolas Nardetto<sup>70</sup> · Domenico Nardiello<sup>12,14</sup> · Norio Narita<sup>42,172,173</sup>.

Valerio Nascimbeni<sup>14</sup> · Anna Nash<sup>26</sup> · Coralie Neiner<sup>6</sup> · Richard P. Nelson<sup>34</sup>.

Nadine Nettelmann<sup>1</sup> · Gianalfredo Nicolini<sup>78</sup> · Martin Nielsen<sup>56</sup>.

Sami-Matias Niemi<sup>7</sup> · Lena Noack<sup>174</sup> · Arlette Noels-Grotsch<sup>54</sup>.

Anthony Noll<sup>62</sup> · Azib Norazman<sup>13</sup> · Andrew J. Norton<sup>75</sup> · Benard Nsamba<sup>65</sup>.

Aviv Ofir<sup>175</sup> · Gordon Ogilvie<sup>152</sup> · Terese Olander<sup>46</sup> · Christian Olivetto<sup>103</sup>.

Göran Olofsson<sup>18</sup> · Joel Ong<sup>138</sup> · Sergio Ortolani<sup>12</sup>.

Mahmoudreza Oshagh<sup>120</sup> · Harald Ottacher<sup>76</sup> · Roland Ottensamer<sup>19</sup>.

Rhita-Maria Ouazzani<sup>6</sup> · Sijme-Jan Paardekooper<sup>176</sup> · Emanuele Pace<sup>177</sup>.

Miriam Pajas<sup>38</sup> · Ana Palacios<sup>114</sup> · Gaelle Palandri<sup>6</sup> · Enric Palle<sup>42,43</sup>.

Carsten Paproth<sup>79</sup> · Vanderlei Parro<sup>125</sup> · Hannu Parviainen<sup>42,43</sup>.

Javier Pascual Granado<sup>50</sup> · Vera Maria Passegger<sup>42,43,178</sup>.

Carmen Pastor-Morales<sup>50</sup> · Martin Pätzold<sup>131</sup> · May Gade Pedersen<sup>64</sup>.

David Pena Hidalgo<sup>7</sup> · Francesco Pepe<sup>16</sup> · Filipe Pereira<sup>24</sup>.

Carina M. Persson<sup>126</sup> · Martin Pertenais<sup>79</sup> · Gisbert Peter<sup>79</sup>.

Antoine C. Petit<sup>70</sup> · Pascal Petit<sup>57</sup> · Stefania Pezzuto<sup>71</sup> · Gabriele Pichierri<sup>70</sup>.

Adriano Pietrinferni<sup>68</sup> · Fernando Pinheiro<sup>179</sup> · Marc Pinsonneault<sup>180</sup>.

Emese Plachy<sup>72,73,181</sup> · Philippe Plasson<sup>6</sup> · Bertrand Plez<sup>114</sup>.

Katja Poppenhaeger<sup>60,182</sup> · Ennio Poretti<sup>80</sup> · Elisa Portaluri<sup>14</sup>.

Jordi Portell<sup>39,92,93</sup> · Gustavo Frederico Porto de Mello<sup>183</sup>.

Julien Poyatos<sup>39,92,93</sup> · Francisco J. Pozuelos<sup>50</sup> · Pier Giorgio Prada Moroni<sup>115</sup>.

Dumitru Pricopi<sup>184</sup> · Loredana Prisinzano<sup>33</sup> · Matthias Quade<sup>5</sup>.

Andreas Quirrenbach<sup>158</sup> · Julio Arturo Rabanal Reina<sup>6</sup> · Maria Cristina Rabello

Soares<sup>40</sup> · Gabriella Raimondo<sup>94</sup> · Monica Rainer<sup>98</sup> · Jose Ramón Rodón<sup>50</sup>.

Alejandro Ramón-Ballesta<sup>50</sup> · Gonzalo Ramos Zapata<sup>38</sup> · Stefanie Rätz<sup>185</sup>.

Christoph Rauterberg<sup>5</sup> · Bob Redman<sup>26</sup> · Ronald Redmer<sup>186</sup> · Daniel Reese<sup>6</sup>.

Sara Regibo<sup>3</sup> · Ansgar Reiners<sup>120</sup> · Timo Reinhold<sup>5</sup> · Christian Renie<sup>6</sup>.

Ignasi Ribas<sup>93,102</sup> · Sergio Ribeiro<sup>125</sup> · Thiago Pereira Ricciardi<sup>125</sup>.

Ken Rice<sup>187</sup> · Olivier Richard<sup>114</sup> · Marco Riello<sup>36</sup> · Michel Rieutord<sup>57</sup>.

Vincenzo Ripepi<sup>113</sup> · Guy Rixon<sup>36</sup> · Steve Rockstein<sup>79</sup> · José Ramón Rodón

Ortiz<sup>50</sup> · María Teresa Rodrigo Rodríguez<sup>38</sup> · Alberto Rodríguez Amor<sup>38</sup>.

Luisa Fernanda Rodríguez Díaz<sup>22</sup> · Juan Pablo Rodriguez Garcia<sup>7</sup>.

Julio Rodriguez-Gomez<sup>50</sup> · Yannick Roehlly<sup>4</sup> · Fernando Roig<sup>188</sup>.

Bárbara Rojas-Ayala<sup>189</sup> · Tobias Rolf<sup>28</sup> · Jakob Lysgaard Rørsted<sup>22</sup>.

Hugo Rosado<sup>49</sup> · Giovanni Rosotti<sup>145</sup> · Olivier Roth<sup>6</sup> · Markus Roth<sup>127</sup>.

Alex Rousseau<sup>26</sup> · Ian Roxburgh<sup>34</sup> · Fabrice Roy<sup>6</sup> · Pierre Royer<sup>3</sup>.

Kirk Ruane<sup>26</sup> · Sergio Rufini Mastropasqua<sup>1</sup> · Claudia Ruiz de Galarreta<sup>17</sup>.

Andrea Russi<sup>71</sup> · Steven Saar<sup>190</sup> · Melaine Saillenfest<sup>55</sup> · Maurizio Salaris<sup>110</sup>.

Sebastien Salmon<sup>54</sup> · Ippocratis Saltas<sup>191</sup> · Réza Samadi<sup>6</sup> · Aunia Samadi<sup>5</sup>.

Dominic Samra<sup>76</sup> · Tiago Sanches da Silva<sup>125</sup> · Miguel Andrés Sánchez

Carrasco<sup>50</sup> · Alexandre Santerne<sup>4</sup> · Amaia Santiago Pé<sup>38</sup>.

Francesco Santoli<sup>71</sup> · Ängela R. G. Santos<sup>24</sup> · Rosario Sanz Mesa<sup>50</sup>.

Luis Manuel Sarro<sup>192</sup> · Gaetano Scandariato<sup>11</sup> · Martin Schäfer<sup>5</sup>.

Edward Schlafly<sup>193</sup> · François-Xavier Schmider<sup>70</sup> · Jean Schneider<sup>194</sup>.
Jesper Schou⁵ · Hannah Schunker¹⁹⁵ · Gabriel Jörg Schwarzkopf⁷⁹ ·

Aldo Serenelli⁹³,¹⁰² · Dries Seynaeve³ · Yutong Shan²⁸ · Alexander Shapiro⁵ ·

Russel Shipman¹⁴⁹ · Daniela Sicilia¹¹ · Maria Angeles Sierra sanmartin³⁸ ·

Axelle Sigot⁴ · Kyle Silliman²⁶ · Roberto Silvotti⁷⁸ · Attila E. Simon¹⁰ ·

Ricardo Simoyama Napoli¹²⁵ · Marek Skarka²¹,¹⁹⁶ · Barry Smalley¹⁹⁷ ·

Rodolfo Smiljanic¹⁹⁸ · Samuel Smit²⁶ · Alexis Smith¹ · Leigh Smith³⁶ ·

Ignas Snellen¹⁴⁵ · Ádám Sódor⁷² · Frank Sohl¹ · Sami K. Solanki⁵ ·

Francesca Sortino⁵³ · Sérgio Sousa²⁴ · John Southworth¹⁶⁵ · Diogo Souto¹⁹⁹ ·

Alessandro Sozzetti⁷⁸ · Dimitris Stamatellos²⁰⁰ · Keivan Stassun¹²¹ ·

Manfred Steller⁷⁶ · Dennis Stello²⁰¹ · Beate Stelzer¹⁸⁵ · Ulrike Stiebeler¹ ·

Amalie Stokholm⁵⁶ · Trude Storelvmo²⁸ · Klaus Strassmeier⁶⁰ ·

Paul Anthony Strøm¹³ · Antoine Strugarek⁸⁷ · Sophia Sulis⁴ ·

Michal Švanda²¹,²⁰² · László Szabados⁷²,⁷³ · Róbert Szabó⁷²,⁷³,¹⁸¹ ·

Gyula M. Szabó¹¹⁶,¹⁴¹ · Ewa Szuszkiewicz²⁰³ · Geert Jan Talens³⁷ ·

Daniele Teti⁷ · Tom Theisen³² · Frédéric Thévenin⁷⁰ · Anne Thoul⁵⁴ ·

Didier Tiphene⁶ · Ruth Titz-Weider¹ · Andrew Tkachenko³ · Daniel Tomecki¹ ·

Jorge Tonfat⁷⁶ · Nicola Tosi¹ · Regner Trampedach²⁰⁴ · Gregor Traven¹⁰⁰ ·

Amaury Triaud⁵⁶ · Reidar Trønnes²⁸ · Maria Tsantaki⁹⁸ ·

Matthias Tschentscher¹ · Arnaud Turin⁴ · Adam Tvaruzka⁷ · Bernd Ulmer⁷⁹ ·

Solène Ulmer-Moll¹⁶ · Ceren Ulusoy²⁰⁵ · Gabriele Umbriaco¹⁴,¹⁰¹ ·

Diana Valencia²⁰⁶ · Marica Valentini⁶⁰ · Adriana Valio²⁰⁷ · Ángel Luis Valverde

Guijarro³⁸ · Vincent Van Eylen²⁶ · Valerie Van Grootel⁵⁴ · Tim A. van

Kempen²³ · Timothy Van Reeth³ · Iris Van Zelst¹ · Bart Vandenbussche³ ·

Konstantinos Vasiliou¹ · Valeriy Vasilyev⁵ · David Vaz de Mascarenhas⁶ ·

Allona Vazan²⁰⁸ · Marina Vela Nunez⁹⁸ · Eduardo Nunes Velloso⁴⁴ ·

Rita Ventura¹¹ · Paolo Ventura⁶⁸ · Julia Venturini¹⁶ · Isabel Vera Trallero³⁸ ·

Dimitri Veras¹³,²⁰⁹,²¹⁰ · Eva Verdugo⁸ · Kuldeep Verma²¹¹ · Didier Vibert⁴ ·

Tobias Vicanek Martinez¹⁸⁵ · Krisztián Vida⁷²,²¹² · Arthur Vigan⁴ ·

Antonio Villacorta⁸ · Eva Villaver⁴²,⁴³ · Marcos Villaverde Aparicio⁵⁰ ·

Valentina Viotto¹⁴ · Eduard Vorobyov¹⁹ · Sergey Vorontsov³⁴ ·

Frank W. Wagner²¹³ · Nicholas Walton³⁶ · Dave Walton²⁶ ·

Haiyang Wang¹¹⁸,²¹⁴ · Rens Waters²³ · Christopher Watson²¹⁵ ·

Sven Wedemeyer²¹⁶ · Angharad Weeks²⁶ · Jörg Weingrill⁶⁰ · Annita Weiss⁵ ·

Belinda Wendler¹ · Richard West¹³ · Karsten Westerdorff⁷⁹ ·

Pierre-Amaury Westphal¹⁰³ · Peter Wheatley¹³ · Tim White⁵¹ ·

Amadou Whittaker⁷ · Kai Wickhusen¹ · Thomas Wilson¹³ · James Windsor⁷ ·

Othon Winter¹²⁹ · Mark Lykke Winther²² · Alistair Winton⁷ · Ulrike Witteck⁷⁹ ·

Veronika Witzke⁵ · Peter Woitke⁷⁶ · David Wolter¹ · Günther Wuchterl²¹⁷ ·

Mark Wyatt³⁶ · Dan Yang⁵ · Jie Yu⁵ · Ricardo Zanmar Sanchez⁶⁸ ·

María Rosa Zapatero Osorio⁹ · Mathias Zechmeister²¹⁸ · Yixiao Zhou⁹⁹ ·

Claas Ziemke⁷⁹ · Konstanze Zwintz²¹⁹ · Torsten Böhm⁵⁷ · Léo Michel Dansac⁴

<figure><img src="image_55.png" /></figure>

Heike Rauer
heike.rauer@dlr.de
1 Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, DLR, Rutherfordstrasse 2, 12489 Berlin, Germany

2 Fachbereich Geowissenschaften, Institut für Geologische, Freie Universität Berlin, Malteserstr. 74-100, 12249 Berlin, Germany

3 Institute of Astronomy, KU Leuven, Leuven, Belgium

4 CNRS, CNES, LAM, Aix Marseille University, Marseille, France

5 Max Planck Institute for Solar System Research, Göttingen, Germany

6 LESIA, Paris Observatory, PSL University, Sorbonne University, Paris Cité University, CNRS, Meudon, France

7 ESTEC, European Space Agency, Noordwijk, The Netherlands

8 ESAC, European Space Agency, Madrid, Spain

9 Centro de Astrobiología, CSIC-INTA, Campus ESAC, Madrid, Spain

10 Center for Space and Habitability, University of Bern, Bern, Switzerland

11 INAF - Osservatorio Astrofisico di Catania, Catania, Italy

12 Department of Physics and Astronomy, University of Padua, Padua, Italy

13 Department of Physics, University of Warwick, Coventry, United Kingdom

14 Astronomical Observatory of Padova, INAF - Italian National Institute for Astrophysics, Padua, Italy

15 Armagh Observatory and Planetarium, College Hill, Armagh, United Kingdom

16 Geneve Observatory, University of Geneva, Geneva, Switzerland

17 IAS, University of Paris-Saclay, Orsay, France

18 AlbaNove University Centre, Stockholm University, Stockholm, Sweden

19 Department of Astrophysics, University of Vienna, Vienna, Austria

20 Department of Astronomy, University of Sao Paulo, Sao Paulo, Brazil

21 Astronomical Institute of the Czech Academy of Sciences, Ondřejov, Czech Republic

22 Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark

23 Institute for Space Research, SRON, Leiden, The Netherlands

24 Instituto de Astrofísica e Ciências do Espaço, CAUP, Universidade do Porto, Porto, Portugal

25 Departamento de Física e Astronomia, Faculdade da Ciências, Universidade do Porto, Porto, Portugal

26 Mullard Space Science Laboratory, University College London, Holmbury Saint Mary, United Kingdom

27 Dept. Theoretical Physics and the Cosmos, University of Granada, Granada, Spain

28 Centre for Planetary Habitability, Centre for Earth Evolution and Dynamics, Department of Geosciences, University of Oslo, Oslo, Norway

29 CISAS G. Colombo University of Padua, Padua, Italy

30 Faculty of Sciences, University of Lisbon, Lisbon, Portugal

31 Max-Planck-Institute for Astronomy, Heidelberg, Germany

32 University of Applied Sciences Aachen, Aachen, Germany
33 Palermo Astronomical Observatory, INAF - Italian National Institute for Astrophysics, Palermo, Italy

34 Department of Physics & Astronomy, Queen Mary University of London, London, United Kingdom

35 DARK, Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark

36 Institute of Astronomy, University of Cambridge, Cambridge, United Kingdom

37 University of Oxford, Oxford, United Kingdom

38 INTA - National Institute of Aerospace Technology, Madrid, Spain

39 Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), Barcelona, Spain

40 Department of Physics, University of Minas Gerais, Minas Gerais, Brazil

41 School of Physics & Astronomy, University of Leicester, Leicester, United Kingdom

42 IAC - Instituto de Astrofísica de Canarias, Tenerife, Spain

43 Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain

44 Department of Physics, University Rio Grande do Norte, Rio Grande do Norte, Brazil

45 Space Science Data Center - ASI, Rome, Italy

46 Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden

47 Department of Physics, State University of Feira de Santana, Feira de Santana, Brazil

48 Astronomical Observatory, University of Ponta Grossa, Ponta Grossa, Brazil

49 Deimos Engenharia, Lisbon, Portugal

50 IAA - Institute of Astrophysics of Andalusia, CSIC - Spanish National Research Council, Granada, Spain

51 Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australia

52 Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, United States

53 Astrophysics and Space Science Observatory of Bologna, INAF - Italian National Institute for Astrophysics, Bologna, Italy

54 Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Liège, Belgium

55 IMCCE, Observatory of Paris, Paris, France

56 School of Physics & Astronomy, University of Birmingham, Birmingham, United Kingdom

57 IRAP - Institute for Research in Astrophysics and Planetology, Toulouse, France

58 University of Atacama, Copiapó, Chile

59 School of Mathematics, University of Leeds, Leeds, United Kingdom

60 Leibniz Institute for Astrophysics Potsdam, Potsdam, Germany

61 Astronomy Department, Yale University, New Haven, United States

62 Heidelberg Institute for Theoretical Studies, Heidelberg, Germany

63 Institute for Physics, University of Graz, Graz, Austria

64 School of Physics, University of Sydney, Sydney, Australia

65 Max Planck Institute for Astrophysics, Garching, Germany
66 Solar Science Observatory, National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan

67 Center for Space Science, New York University Abu Dhabi, Abu Dhabi, United Arab Emirates

68 Astronomical Observatory of Rome, INAF - Italian National Institute for Astrophysics, Rome, Italy

69 Astronomical Observatory of Trieste, INAF - Italian National Institute for Astrophysics, Trieste, Italy

70 Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Université Côte d'Azur, Nice, France

71 IAPS, INAF - Italian National Institute for Astrophysics, Rome, Italy

72 Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences, MTA Centre of Excellence, Budapest, Hungary

73 Near-Field Cosmology Research Group, MTA CSFK Lendlet, Budapest, Hungary

74 Departement of Astronomy, University of Geneve, Geneve, Switzerland

75 School of Physical Sciences, The Open University, Milton Keynes, United Kingdom

76 Space Research Institute, Austrian Academy of Science, Graz, Austria

77 IPAG, University of Grenoble Alpes, Grenoble, France

78 Turin Astrophysical Observatory, INAF - Italian National Institute for Astrophysics, Turin, Italy

79 Institute of Optical Sensor Systems, German Aerospace Center, Berlin, Germany

80 Brera Astronomical Observatory, INAF - Italian National Institute for Astrophysics, Merate, Italy

81 National Observatory, LIneA - International Laboratory of Astronomy, Rio de Janeiro, Brazil

82 School of Mathematics, Statistics and Physics, Newcastle University, Newcastle upon Tyne, United Kingdom

83 University of Auckland, Auckland, New Zealand

84 SISSA, International School for Advanced Studies, Trieste, Italy

85 Centro de Astrofísica e Gravitação (CENTRA), Departamento de Física, Instituto Superior Técnico - IST, Universidade de Lisboa, Lisboa, Portugal

86 Department of Physics, University of Turin, Turin, Italy

87 CEA, CNRS, AIM, Université Paris-Saclay, Université Paris Cité, Gif-sur-Yvette, France

88 DTU Space, Technical University of Denmark, Copenhagen, Denmark

89 Institute of Science & Technology, Klosterneuburg, Austria

90 Dept, of Chemistry and Physics, Florida Gulf Coast University, Fort Myers, United States

91 School of Physics and Astronomy, University of St Andrews, St Andrews, United Kingdom

92 Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), Barcelona, Spain

93 Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain

94 Astronomical Observatory of Abruzzo, INAF - Italian National Institute for Astrophysics, Teramo, Italy

95 INFN - Sezione di Pisa, Pisa, Italy

96 Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile

97 Millennium Institute of Astrophysics, Santiago, Chile
98 Arcetri Astrophysical Observatory, INAF - Italian National Institute for Astrophysics, Florence, Italy

99 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark

100 Lund Observatory, Lund University, Lund, Sweden

101 Department of Physics and Astronomy, University of Bologna, Bologna, Italy

102 Institut de Ciències de l'Espai (ICE, CSIC), Campus UAB, Barcelona, Spain

103 IAS, University of Paris-Saclay, Bures-sur-Yvette, France

104 CFisUC, Physics Department, University of Coimbra, Coimbra, Portugal

105 FGG, INAF - Italian National Institute for Astrophysics, Brena Baja, Spain

106 University of Naples Federico II, Napoli, Italy

107 College of Engineering, Mathematics and Physical Sciences, University of Exeter, Exeter, United Kingdom

108 Institute of Sciences, Federal University of Southern and Southeastern Pará, Marabá, Brazil

109 Centre for Mathematical Sciences, Lund University, Lund, Sweden

110 Astrophysics Research Institute, John Moores University, Liverpool, United Kingdom

111 National Astrophysics Laboratory, Itajubá - MG, Brazil

112 Department of Physics, Federal University of Ceará, Ceará, Brazil

113 Capodimonte Astronomical Observatory, INAF - Italian National Institute for Astrophysics, Napoli, Italy

114 Laboratoire Univers et Particules de Montpellier, CNRS, Université de Montpellier, Montpellier, France

115 Department of Physics, Pisa University, Pisa, Italy

116 Gothard Astrophysical Observatory, ELTE Eötvös Loránd University, Szombathely, Hungary

117 Valencia Internacional University, Alicante, Spain

118 Institute for Particle Physics and Astrophysics, ETH Zurich, Zurich, Switzerland

119 Free University of Brussels, Brussels, Belgium

120 Institute for Astrophysics and Geophysics, Georg-August-University of Göttingen, Göttingen, Germany

121 Department of Physics and Astronomy, Vanderbilt University, Nashville, United States

122 Polytechnic School, University of Sao Paulo, Sao Paulo, Brazil

123 European Southern Observatory, Santiago, Chile

124 ESOC, European Space Agency, European Space Agency, Germany

125 Maua Institute of Technology, IMT University, Sao Paulo, Brazil

126 Department of Space Earth and Environment, Chalmers University of Technology, Onsala, Sweden

127 Thüringer Landessternwarte Tautenburg, Tautenburg, Germany

128 Max-Planck-Institute for Astronomy, Neckargemuend, Germany

129 Sao Paulo State University, Sao Paulo, Brazil

130 Centro di Ateneo di Studi e Attività Spaziali "Giuseppe Colombo", Università di Padova, Padova, Italy
131 RIU, University of Cologne, Köln, Germany

132 Department of Physics & Astronomy, University of Georgia, Athens, United States

133 Kavli Institute for Cosmology, Institute of Astronomy, University of Cambridge, Cambridge, United Kingdom

134 IAP - Institute of Astrophysics, Paris, France

135 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Torun, Poland

136 Boston University, Boston, United States

137 Southwest Research Institute, Arizona State University, Texas, United States

138 University of Hawai'i, Honolulu, United States

139 Department of Earth, Environmental and Planetary Sciences, and Department of Physics and Astronomy, Rice University, Texas, United States

140 Astronomy Nucleus, Diego Portales University, Santiago, Chile

141 Exoplanet Research Group, MTA-ELTE, Szombathely, Hungary

142 Doctoral School of Physics, ELTE Eötvös Loránd University, Budapest, Hungary

143 Department of Geoscience, Aarhus University, Aarhus, Denmark

144 Iowa State University, Ames, United States

145 Leiden Observatory, Leiden University, Leiden, The Netherlands

146 Institute of Theoretical Physics and Astronomy, Vilnius University, Vilnius, Lithuania

147 Lund Observatory, Division of Astrophysics, Department of Physics, Lund University, Lund, Sweden

148 Dept. Applied Mathematics & Physics, University of Applied Sciences Technikum Wien, Vienna, Austria

149 Institute for Space Research, SRON, Groningen, The Netherlands

150 UTINAM Institute, Besançon, France

151 Department of Physics and Astronomy, University of Catania, Catania, Italy

152 Centre for Mathematical Sciences, University of Cambridge, Cambridge, United Kingdom

153 IPR, University of Rennes, Rennes, France

154 H.H. Wills Physics Laboratory, University of Bristol, Bristol, United Kingdom

155 naXys Research Institute, University of Namur, Namur, Belgium

156 Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands

157 University of Colorado, Boulder, United States

158 Landessternwarte, Heidelberg University, Heidelberg, Germany

159 Royal Observatory of Belgium, Brussels, Belgium

160 Institute for Software Technology, German Aerospace Center, Braunschweig, Germany

161 CNES - National Centre for Space Studies, Toulouse, France

162 University of North Carolina at Chapel Hill, Chapel Hill, United States

163 School of Physics and Astronomy, Monash University, Melbourne, Australia

164 AIM-CEA, Paris Diderot University, Paris, France

165 Astrophysics Group, Keele University, Staffordshire, United Kingdom
166 Tel Aviv University, Tel Aviv, Israel

167 PSL University, Paris, France

168 “Momentum” Milky Way Research Group, MTA-ELTE Lendület, Szombathely, Hungary

169 University of Surrey, Guildford, United Kingdom

170 Division of Space Research and Planetary Sciences, University of Bern, Bern, Switzerland

171 University of Valencia, Valencia, Spain

172 Komaba Institute for Science, University of Tokyo, Meguro, Tokyo, Japan

173 Astrobiology Center, Mitaka, Tokyo, Japan

174 Institute of Geological Sciences, Free University of Berlin, Berlin, Germany

175 Weizmann Institute of Science, Rehovot, Israel

176 Delft University of Technology, Delft, The Netherlands

177 University of Florence, Florence, Italy

178 Hamburg Observatory, University of Hamburg, Hamburg, Germany

179 Geophysical and Astronomical Observatory, University of Coimbra, Coimbra, Portugal

180 Institute for Astronomy, Ohio State University, Columbus, United States

181 Institute of Physics and Astronomy, ELTE Eötvös Loránd University, Budapest, Hungary

182 Institute for Physics and Astronomy, Potsdam University, Potsdam, Germany

183 Observatory of Valongo, Federal University of Rio de Janeiro, Rio de Janeiro, Brazil

184 Astronomical Institute, Romanian Academy, Bucharest, Romania

185 Institute for Astronomy and Astrophysics, University of Tuebingen, Tübingen, Germany

186 Institute of Physics, University of Rostock, Rostock, Germany

187 Institute for Astronomy, The Royal Observatory, University of Edinburgh, Edinburgh, United Kingdom

188 National Observatory Rio de Janeiro, Rio de Janeiro, Brazil

189 Instituto de Alta Investigación, Universidad de Tarapacá, Arica, Chile

190 Center for Astrophysics, Harvard & Smithsonian, Cambridge, United States

191 Institute of Physics, Czech Academy of Science, Praha, Czech Republic

192 National Distance Education University, Madrid, Spain

193 Lawrence Berkeley Laboratory, University of California, Berkeley, United States

194 LUTH, UMR 8102, Paris Observatory, Meudon, France

195 The University of Newcastle, Newcastle, Australia

196 Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic

197 Lennard-Jones Laboratory, Keele University, Staffordshire, United Kingdom

198 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Warsaw, Poland

199 Federal University of Sergipe, Sao Cristovao, Brazil

200 Jeremiah Horrocks Institute, University of Central Lancashire, Preston, United Kingdom

201 School of Physics, University of New South Wales, New South Wales, Australia

202 Faculty of Mathematics and Physics, Charles University, Praha, Czech Republic
203 Institute of Physics and CASA*, University of Szczecin, Szczecin, Poland

204 Space Science Institute, Boulder, United States

205 Girne American University, Kyrenia, Cyprus

206 University of Toronto, Toronto, Canada

207 Center for Radio Astronomy and Astrophysics, Mackenzie Presbyterian University, Sao Paulo, Brazil

208 Department of Natural Sciences, Open University of Israel, Ra'anana, Israel

209 Centre for Exoplanets and Habitability, University of Warwick, Coventry, United Kingdom

210 Centre for Space Domain Awareness, University of Warwick, Coventry, United Kingdom

211 Department of Physics, Indian Institute of Technology (BHU), Varanasi-221005, India

212 Department of Astronomy, ELTE Eötvös Loránd University, Budapest, Hungary

213 Institute for Advanced Simulation, Forschungszentrum Jülich, Jülich, Germany

214 Institute of Geochemistry and Petrology, ETH Zurich, Zurich, Switzerland

215 Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast, United Kingdom

216 Rosseland Centre for Solar Physics, Institute of Theoretical Astrophysics, University of Oslo, Oslo, Norway

217 Kuffner Observatory, Vienna, Austria

218 Universität Göttingen, Göttingen, Germany

219 Institute for Astro- and Particle Physics, University of Innsbruck, Innsbruck, Austria

220 Instituto Superior de Gestão, Universidade de Lisboa, Lisbon, Portugal

221 Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France

222 Institute for Experimental and Applied Physics, Christian-Albrechts-University Kiel, Kiel, Germany

223 Anton Pannekoek Institute, University of Amsterdam, Amsterdam, The Netherlands

224 Wolfgang-Pauli-Institut Wien, Vienna, Austria

225 MMM “Mathematics-Magnetism-Materials” Research Platform, Faculty of Mathematics, University of Vienna, Vienna, Austria