cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-12t1q2v
title: 2790721

description:   Target RA (J2000):  311.289703369141  and deg    Target Dec (J2000):  -31.3409004211426  and deg    Gaia GMag:  7.84   Programme ID:  CH_PR140071   Programme Manager:  SZABO   PI of observing programme:  Benz   Title of programme:  Axis 1 - Opening the treasure chest of the young golden system AU Mic with CHEOPS   Abstract:  AU Mic is a young (~22 Myr) active M1 star known to host two transiting warm Neptunes close to the 9:4 mean-motion resonance. Transit Timing Variations suggest that an additional resonant planet is likely present in the system. The rotation period of the star and the orbital period of AU Mic b are in a 7:4 spin-orbit commensurability. We also foundThere are systematic variations in the transit depth that correlate with the stars brightness strongly hampering the accuracy on the planetary radii. AU Mic displays differential rotation making it the youngest red star known to feature equator-to-pole spot migration.  AU Mic is a young goldmine for planetary and stellar physics a treasure chest just waiting to be opened. Thanks to its short-cadence space-born photometry CHEOPS is uniquely well suited to seize this opportunity. We propose to carry out an intensive CHEOPS observing campaign of AU Mic.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1a5d059
title: 2719381

description:   Target RA (J2000):  139.231170654297  and deg    Target Dec (J2000):  -20.6763095855713  and deg    Gaia GMag:  11.515   Programme ID:  CH_PR140079   Programme Manager:  OSBORN   PI of observing programme:  Benz   Title of programme:  Axis 1 - DETECTIVE CHEOPS: Confirming small transiting planets on long orbital periods   Abstract:  Transiting planets orbiting bright stars are key for the characterisation of exoplanet atmospheres and internal structures. However the vast majority of such planets have short (P<20d) orbital periods. This is because long-period transiting planets do not produce consecutive transits in photometric survey data. However these planets are some of the most interesting as unlike their interior companions they are less affected by the gravitational and electromagnetic effects of their host stars. This programme will use CHEOPS to efficiently detect characterisable small transiting planets on long orbital periods. We will do this by leveraging as much external information as possible to constrain orbital periods - from nonconsecutive transits (i.e. mono- duo- or trio-transit candidates) in photometric survey data such as K2 or TESS and from radial velocities where available. Such techniques have been successful in the CHEOPS nominal mission with for example the photometrically-constrained TOI-2076 c  and  d (Osborn et al 2022) or the monotransit+RV case of TOI-561 d  and  e (Lacedelli et al 2021  and  2022). These planets once found by CHEOPS may also form interesting science targets for other parts of the GTO extended mission science case such as studying the architectural diversity of exoplanetary systems and even searches for exomoon  and  rings.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1edktwf
title: 2861251

description:   Target RA (J2000):  294.661407470703  and deg    Target Dec (J2000):  31.2192001342773  and deg    Gaia GMag:  7.575   Programme ID:  CH_PR140061   Programme Manager:  LENDL   PI of observing programme:  Benz   Title of programme:  Axis 2 - A Deep search for hot JupIter VAriability (DIVA)   Abstract:  The temporal stability of hot Jupiter atmospheres remains an open question. While there are several tentative detections of changes in the observed planetary occultation depths phase curve shapes or transmission spectra no indisputable evidence exists to date. This program will perform a deep search for variability in the dayside brightness of several hot Jupiters. A detection of clear variability and the measurement of its timescale would open the door to a suite of follow-up studies involving the dynamical behaviour of exoplanet atmospheres.     [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1ehjztd
title: 2752202

description:   Target RA (J2000):  216.924026489258  and deg    Target Dec (J2000):  41.9534187316895  and deg    Gaia GMag:  9.659   Programme ID:  CH_PR159006   Programme Manager:  ZULETA   PI of observing programme:  Benz   Title of programme:  SoM - TRACE   Abstract:  The TRACE (Measuring the TRansit light sourCe Effect with CHEOPS) program aims to use the CHEOPS telescope to characterize the transit light source effect (TLSE) for exoplanet targets scheduled for observation with the JWST. This effort addresses a critical challenge in exoplanet atmosphere analysis: contamination from stellar activity such as star spots and faculae which can skew measurements of planetary atmospheres by introducing variability in observed spectra. The program will conduct high-precision photometric observations in the optical band an essential range that JWST does not cover but is critical to identify and mitigate stellar contamination in transmission spectra. Focusing on two primary targets in a first stage --TOI-1416 and GJ9827--the project plans long-baseline in and out-of-transit observations spread across a few stellar rotations to model activity-related flux variations. These findings are expected to help the JWST data interpretation of the planets atmosphere and support the broader scientific community by making data publicly available immediately. By characterizing activity in CHEOPS-observed systems TRACE aims to enhance our understanding of exoplanet atmospheres and prepare for future synergy with upcoming missions such as PANDORA.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1gx4eif
title: 2859771

description:   Target RA (J2000):  348.949035644531  and deg    Target Dec (J2000):  -10.8496904373169  and deg    Gaia GMag:  12.0   Programme ID:  CH_PR140080   Programme Manager:  LELEU   PI of observing programme:  Benz   Title of programme:  Axis 1 - Architecture of Resonant Chains (ARC)   Abstract:  Resonant chains are gold mines for fueling our understanding of planetary systems. The minute details of their architectures encode the history of their formation: the order of the capture of the planets in the chain (Delisle 2017) the local shape of the proto-planetary disc and its dispersal (e.g.  Nesvorny et al 2022) and the long-term evolution of the system through tidal dissipation (e.g. Papaloizou et al 2018). The high multiplicity of these systems also makes them especially valuable to constrain our models of the formation of planetary systems (See Emsenhuber et al 2022 and other papers of the NGPPS series) since all the planets have to form in the same environment and the relative fragility of the configuration ensures that no violent evolution (e.g. close encounters/impacts) occurred after the dissipation of the proto-planetary disc (Leleu et al 2021). In addition the transit timing variations induced by the compactness of the systems allow for precise mass determination down to a few per cent in the case of Trappist-1 (Agol et al 2021). This allows an in-depth characterization of moderately insolated rocky planets and mini-Neptune with a precision which is rarely reachable through radial velocities enabling studies of their interiors and atmospheres. The brightness of the current targets of the program (Gaia band mag 11 for TOI178 12 for K2-138 8.4 for TOI1835) allows to combine RVs and photometric measurements. The two methods have a great synergy as TTVs allow for in-depth characte [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1j7xjib
title: 2711034

description:   Target RA (J2000):  216.924026489258  and deg    Target Dec (J2000):  41.9534187316895  and deg    Gaia GMag:  9.659   Programme ID:  CH_PR150100   Programme Manager:  ZULETA   PI of observing programme:  Benz   Title of programme:  SoM - TRACE   Abstract:  The TRACE (Measuring the TRansit light sourCe Effect with CHEOPS) program aims to use the CHEOPS telescope to characterize the transit light source effect (TLSE) for exoplanet targets scheduled for observation with the JWST. This effort addresses a critical challenge in exoplanet atmosphere analysis: contamination from stellar activity such as star spots and faculae which can skew measurements of planetary atmospheres by introducing variability in observed spectra. The program will conduct high-precision photometric observations in the optical band an essential range that JWST does not cover but is critical to identify and mitigate stellar contamination in transmission spectra. Focusing on two primary targets in a first stage --TOI-1416 and GJ9827--the project plans long-baseline in and out-of-transit observations spread across a few stellar rotations to model activity-related flux variations. These findings are expected to help the JWST data interpretation of the planets atmosphere and support the broader scientific community by making data publicly available immediately. By characterizing activity in CHEOPS-observed systems TRACE aims to enhance our understanding of exoplanet atmospheres and prepare for future synergy with upcoming missions such as PANDORA.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1l0afsd
title: 2889625

description:   Target RA (J2000):  42.9843635559082  and deg    Target Dec (J2000):  -30.8145294189453  and deg    Gaia GMag:  6.25   Programme ID:  CH_PR140067   Programme Manager:  ALIBERT   PI of observing programme:  Benz   Title of programme:  Axis 1 - Probing the architecture-composition-metallicity link (ArchiCHESS)   Abstract:  Planet formation models predict the existence of a link between the orbital architecture of a planetary system the composition of its planets and the metallicity of the central star. This correlation results from the following two processes: On one hand the temporal evolution of the gas content of the protoplanetary disk causes migration of the planets and therefore determines the orbital architecture of the system. On the other hand the composition of the planets depends on the structure and composition of the disk of solids itself related to the gas content of the disk and the solid-to-gas ratio in the disk. This latter quantity is finally correlated with the stellar metallicity. The goal of ArchiCHESS is to observe multi-planetary systems to constrain their architecture (using architecture coefficients of Mishra et al. 2023) and relate this to the water fractions of the planets as well as to the metallicity of the central star.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1rf5ube
title: 2858873

description:   Target RA (J2000):  351.770172119141  and deg    Target Dec (J2000):  -1.28627002239227  and deg    Gaia GMag:  9.841   Programme ID:  CH_PR159006   Programme Manager:  ZULETA   PI of observing programme:  Benz   Title of programme:  SoM - TRACE   Abstract:  The TRACE (Measuring the TRansit light sourCe Effect with CHEOPS) program aims to use the CHEOPS telescope to characterize the transit light source effect (TLSE) for exoplanet targets scheduled for observation with the JWST. This effort addresses a critical challenge in exoplanet atmosphere analysis: contamination from stellar activity such as star spots and faculae which can skew measurements of planetary atmospheres by introducing variability in observed spectra. The program will conduct high-precision photometric observations in the optical band an essential range that JWST does not cover but is critical to identify and mitigate stellar contamination in transmission spectra. Focusing on two primary targets in a first stage --TOI-1416 and GJ9827--the project plans long-baseline in and out-of-transit observations spread across a few stellar rotations to model activity-related flux variations. These findings are expected to help the JWST data interpretation of the planets atmosphere and support the broader scientific community by making data publicly available immediately. By characterizing activity in CHEOPS-observed systems TRACE aims to enhance our understanding of exoplanet atmospheres and prepare for future synergy with upcoming missions such as PANDORA.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1th1hku
title: 2666226

description:   Target RA (J2000):  107.866432189941  and deg    Target Dec (J2000):  48.3303909301758  and deg    Gaia GMag:  11.39   Programme ID:  CH_PR140065   Programme Manager:  WILSON   PI of observing programme:  Benz   Title of programme:  Axis 1 -  Solidifying Planet-Star Composition Links by Studying Why the Internal Structures of Planets Across the Galaxy Vary (YGAL)   Abstract:  Terrestrial planets form through the accretion of building blocks from dust grains to proto-planets. Heavier components sink and form metallic cores whilst pebbles from beyond snow lines deliver volatiles influencing atmospheres or water on Earth-like planets. Understanding the composition of planetary ingredients is vital. Planetary refractory elemental abundances mirror stellar values  the Earth is a devolatised piece of the Sun. If this is universal we would expect a diversity in internal structures and atmospheres of planets orbiting metal-diverse stars. This is currently not well investigated however in recent years tantalising evidence has emerged for metallicity-driven trends in the physical characteristics of super-Earth and sub-Neptune exoplanets. These first pieces of evidence might be pointing towards chemically-diverse formation scenarios impacting the internal structures of planets however this is currently unclear as there are very few well-characterised small planets around metal-poor stars. Therefore this program will refine the radii of a handful of key planets around Galactic thick-disk metal-poor host stars to an unprecedented level in order to solve the current mysteries that we are just starting to unravel.    [truncated! Please see actual data for full text]
DOI: 10.13140/2.1.2804.0481
title: SS1-41 meteorite
DOI: 10.57780/esa-2207778
title: 2847470

description:   Target RA (J2000):  348.949035644531  and deg    Target Dec (J2000):  -10.8496904373169  and deg    Gaia GMag:  12.0   Programme ID:  CH_PR140080   Programme Manager:  LELEU   PI of observing programme:  Benz   Title of programme:  Axis 1 - Architecture of Resonant Chains (ARC)   Abstract:  Resonant chains are gold mines for fueling our understanding of planetary systems. The minute details of their architectures encode the history of their formation: the order of the capture of the planets in the chain (Delisle 2017) the local shape of the proto-planetary disc and its dispersal (e.g.  Nesvorny et al 2022) and the long-term evolution of the system through tidal dissipation (e.g. Papaloizou et al 2018). The high multiplicity of these systems also makes them especially valuable to constrain our models of the formation of planetary systems (See Emsenhuber et al 2022 and other papers of the NGPPS series) since all the planets have to form in the same environment and the relative fragility of the configuration ensures that no violent evolution (e.g. close encounters/impacts) occurred after the dissipation of the proto-planetary disc (Leleu et al 2021). In addition the transit timing variations induced by the compactness of the systems allow for precise mass determination down to a few per cent in the case of Trappist-1 (Agol et al 2021). This allows an in-depth characterization of moderately insolated rocky planets and mini-Neptune with a precision which is rarely reachable through radial velocities enabling studies of their interiors and atmospheres. The brightness of the current targets of the program (Gaia band mag 11 for TOI178 12 for K2-138 8.4 for TOI1835) allows to combine RVs and photometric measurements. The two methods have a great synergy as TTVs allow for in-depth characte [truncated! Please see actual data for full text]
DOI: 10.13140/2.1.1493.3287
title: SS1-28 ？？？？
DOI: 10.57780/esa-2mkq21r
title: 2709743

description:   Target RA (J2000):  156.837921142578  and deg    Target Dec (J2000):  34.3910293579102  and deg    Gaia GMag:  9.8   Programme ID:  CH_PR140084   Programme Manager:  ULMER-MOLL   PI of observing programme:  Benz   Title of programme:  Axis 1 - CompoSubNeptu   Abstract:  Sub-Neptunes are the most common type of known planets in the galactic neighborhood. In spite of that their interior composition and therefore their origin has to date not been constrained observationally. The reason is the degeneracy in possible compositions that can explain their observed properties. Two end member compositions are theoretically suggested: dry rocky cores + about 1% of H/He or ocean planets containing about 50% water in mass. The former is suggested by evolutionary evaporation models the later by formation models. These compositions correspond to fundamentally different in situ formation versus orbital migration pathways. If observationally it should turn out that close-in sub-Neptunian planets are indeed water worlds this could be seen as one of the largest successes of planet formation theory. The opposite case would mean that one or several elements of our current understanding of the origin of planets is fundamentally flawed. It is therefore of paramount importance to answer the fundamental question What are sub-Neptunes made of?. With this program we propose a three-faceted approach to answer this question: 1) is there a grouping in density? 2) Preparing for the JWST opportunity. 3) Is the ice mass fraction correlated with the stellar composition? We propose to use CHEOPS for the precise radius determination of a carefully chosen sample of TESS planet candidate whose radii make them susceptible to be either ocean worlds or rocky cores with H/He envelopes.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-2s1lkyy
title: 2748049

description:   Target RA (J2000):  216.924026489258  and deg    Target Dec (J2000):  41.9534187316895  and deg    Gaia GMag:  9.659   Programme ID:  CH_PR159006   Programme Manager:  ZULETA   PI of observing programme:  Benz   Title of programme:  SoM - TRACE   Abstract:  The TRACE (Measuring the TRansit light sourCe Effect with CHEOPS) program aims to use the CHEOPS telescope to characterize the transit light source effect (TLSE) for exoplanet targets scheduled for observation with the JWST. This effort addresses a critical challenge in exoplanet atmosphere analysis: contamination from stellar activity such as star spots and faculae which can skew measurements of planetary atmospheres by introducing variability in observed spectra. The program will conduct high-precision photometric observations in the optical band an essential range that JWST does not cover but is critical to identify and mitigate stellar contamination in transmission spectra. Focusing on two primary targets in a first stage --TOI-1416 and GJ9827--the project plans long-baseline in and out-of-transit observations spread across a few stellar rotations to model activity-related flux variations. These findings are expected to help the JWST data interpretation of the planets atmosphere and support the broader scientific community by making data publicly available immediately. By characterizing activity in CHEOPS-observed systems TRACE aims to enhance our understanding of exoplanet atmospheres and prepare for future synergy with upcoming missions such as PANDORA.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-2sw9yb6
title: 2824908

description:   Target RA (J2000):  348.949035644531  and deg    Target Dec (J2000):  -10.8496904373169  and deg    Gaia GMag:  12.0   Programme ID:  CH_PR140080   Programme Manager:  LELEU   PI of observing programme:  Benz   Title of programme:  Axis 1 - Architecture of Resonant Chains (ARC)   Abstract:  Resonant chains are gold mines for fueling our understanding of planetary systems. The minute details of their architectures encode the history of their formation: the order of the capture of the planets in the chain (Delisle 2017) the local shape of the proto-planetary disc and its dispersal (e.g.  Nesvorny et al 2022) and the long-term evolution of the system through tidal dissipation (e.g. Papaloizou et al 2018). The high multiplicity of these systems also makes them especially valuable to constrain our models of the formation of planetary systems (See Emsenhuber et al 2022 and other papers of the NGPPS series) since all the planets have to form in the same environment and the relative fragility of the configuration ensures that no violent evolution (e.g. close encounters/impacts) occurred after the dissipation of the proto-planetary disc (Leleu et al 2021). In addition the transit timing variations induced by the compactness of the systems allow for precise mass determination down to a few per cent in the case of Trappist-1 (Agol et al 2021). This allows an in-depth characterization of moderately insolated rocky planets and mini-Neptune with a precision which is rarely reachable through radial velocities enabling studies of their interiors and atmospheres. The brightness of the current targets of the program (Gaia band mag 11 for TOI178 12 for K2-138 8.4 for TOI1835) allows to combine RVs and photometric measurements. The two methods have a great synergy as TTVs allow for in-depth characte [truncated! Please see actual data for full text]
DOI: 10.57780/esa-2yvpkyh
title: 2677920

description:   Target RA (J2000):  125.188789367676  and deg    Target Dec (J2000):  46.2037200927734  and deg    Gaia GMag:  11.327   Programme ID:  CH_PR140085   Programme Manager:  VENTURINI   PI of observing programme:  Benz   Title of programme:  Axis 1 - Towards an S-type radius valley determination (S-valley)   Abstract:  The number of planets orbiting binary stars has notably increased in the past three years thanks to follow-up of Tess Objects of Interest by direct imaging and GAIA. The demographic properties of planets in binaries are only starting to be unveiled. An important question to address for planets around binaries is that of the radius valley a deficit of exoplanets with 1.5 to 2.0 Earth radii found for planets orbiting single stars. A recent study by Sullivan et al. 2023 reports that no radius valley exists for S-type planets (planets in binaries orbiting only one of the stellar components).  The study was performed with a sample of Kepler planets which suffers from large errors in the planetary radii. In addition the planets were assumed to orbit the primary star which adds an additional (and large) source of error in case a planet orbits in reality the secondary star. With this program we re-address the radius valley question by combining past observational data with new measurements from CHEOPS.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-339hcg1
title: 2674758

description:   Target RA (J2000):  172.014541625977  and deg    Target Dec (J2000):  39.6726684570312  and deg    Gaia GMag:  10.59   Programme ID:  CH_PR149000   Programme Manager:  OSBORN   PI of observing programme:  Benz   Title of programme:  SoM - CHeops And TEss vAlidate Unconfirmed eXoplanets   Abstract:  The vast majority of TESS Objects of Interest remain unconfirmed in part due to a lack of follow-up observations. There are so many such targets that even with strict filters to ensure targets are small planets several unconfirmed TESS candidates are transiting at any one time. CHATEAUX proposes to use time-critical P3 Cheops observations of a filtered  and  ranked set of TOIs which would be able to be scheduled between higher-priority time-critical Cheops observations. We expect these filler observations will produce useful scientific observations of TOI candidates including ephemeris improvements TTV detection improved radius precision and improved false positive probabilities (thanks to both ruling our chromaticity and centroid shifts).    [truncated! Please see actual data for full text]