cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-q8xrjtn
title: 2703104

description:   Target RA (J2000):  119.059852600098  and deg    Target Dec (J2000):  -35.1166687011719  and deg    Gaia GMag:  11.83   Programme ID:  CH_PR149004   Programme Manager:  WILSON   PI of observing programme:  Benz   Title of programme:  SoM - Pre-PLATO TTVIGIL (Transit Timing Variation observations to fill In Gaps In Long-baseline data)   Abstract:  Important current questions of exoplanet science require an underlying precise determination of planet internal structures that can be done by studying their mass and/or orbital evolution. Transit timing variations (TTVs) can bypass stellar activity issues that can hinder RVs observations to achieve accurate mass determination and transit timing monitoring may reveal tidal decay that can inform the orbital evolution history of planets. The accuracy of these methods is mainly driven by 1) the knowledge of individual transit centre times and 2) the number of transits obtained and their baseline and sampling.   PLATO will launch at the end of 2026 and focus on the detection of new exoplanets around bright stars. A supplementary scientific outcome will be the continuous observation of known exoplanets that will provide TTV/tidal decay monitoring. However to constrain planetary masses and orbit evolution we need to fill in gaps in the long-baseline data between the discovery transits and those that PLATO will observe. To do this we will observe transits of known exoplanets in the PLATO long- stare fields that are visible by CHEOPS.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-qdyvlrj
title: 2714806

description:   Target RA (J2000):  128.640289306641  and deg    Target Dec (J2000):  9.03532981872559  and deg    Gaia GMag:  11.13   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]
DOI: 10.57780/esa-qgl0yhz
title: 2719716

description:   Target RA (J2000):  229.838119506836  and deg    Target Dec (J2000):  29.206169128418  and deg    Gaia GMag:  9.72   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: 10.57780/esa-qla1i0v
title: 2747862

description:   Target RA (J2000):  186.817169189453  and deg    Target Dec (J2000):  -29.8328304290772  and deg    Gaia GMag:  11.342   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-qmzv5tm
title: 2719417

description:   Target RA (J2000):  164.776077270508  and deg    Target Dec (J2000):  40.9836082458496  and deg    Gaia GMag:  8.09   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: 10.57780/esa-qp3xvqa
title: 2797844

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-qsixqeo
title: 2824903

description:   Target RA (J2000):  283.305511474609  and deg    Target Dec (J2000):  24.1273803710937  and deg    Gaia GMag:  10.67   Programme ID:  CH_PR149003   Programme Manager:  BRANDEKER   PI of observing programme:  Benz   Title of programme:  SoM - Simultaneous exoplanet observations with JWST   Abstract:  JWST observations of exoplanet transits occultations and phase curves can strongly benefit from simultaneous high-precision photometry in the optical. Advantages range from disentangling even minute stellar variability from the planetary signal to help characterise the exoplanet atmosphere from e.g. the strong wavelength dependence of potentially time variable aerosol hazes. Since approved JWST programmes are scheduled well in advance this synergy programme is designed to attempt simultaneous exoplanet observations with CHEOPS whenever possible. The total number of requested orbits is expected to be around 100 per year.     [truncated! Please see actual data for full text]
DOI: 10.57780/esa-qsuv490
title: 2747552

description:   Target RA (J2000):  164.859588623047  and deg    Target Dec (J2000):  -56.6230392456055  and deg    Gaia GMag:  8.382   Programme ID:  CH_PR140072   Programme Manager:  SIMON   PI of observing programme:  Benz   Title of programme:  Axis 3 - Where are the exomoons?   Abstract:  During the past thirty years astronomers have discovered many extrasolar planets (e.g. Batalha et al. (2013)) which has sparked an excitement in the community whether these exoplanets may host a detectable and/or a habitable satellite so called extrasolar moon or exomoon. The technological and theoretical methods now allow the detection of sub-Earth-sized extrasolar planets and the first detection of an extrasolar moon appears feasible (Heller et al. 2014) but so far there is not a single case where the existence of an exomoon could have been demonstrated. Detecting the first exomoon would be a major discovery because moons can be new places for habitability Awiphan and Kerins 2013  Heller and Barnes 2013a  Heller 2012 can play a significant role in the evolution of the host planets and can play a key role in stabilising rotation axis (as Moon does for Earth Laskar et al. (1993)). Even though the mechanisms of moon formation are not fully understood moons seem to be an outcome of planet formation and a presence of exomoons would provide invaluable information on the planets interior and formation process (Crida and Charnoz 2012). To answer the question Where are the exomoons? we would like to continue the search for them in the extended phase of the CHEOPS mission.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-qwdbrcr
title: 2646427

description:   Target RA (J2000):  83.2691497802735  and deg    Target Dec (J2000):  -26.7245807647705  and deg    Gaia GMag:  8.799   Programme ID:  CH_PR149004   Programme Manager:  WILSON   PI of observing programme:  Benz   Title of programme:  SoM - Pre-PLATO TTVIGIL (Transit Timing Variation observations to fill In Gaps In Long-baseline data)   Abstract:  Important current questions of exoplanet science require an underlying precise determination of planet internal structures that can be done by studying their mass and/or orbital evolution. Transit timing variations (TTVs) can bypass stellar activity issues that can hinder RVs observations to achieve accurate mass determination and transit timing monitoring may reveal tidal decay that can inform the orbital evolution history of planets. The accuracy of these methods is mainly driven by 1) the knowledge of individual transit centre times and 2) the number of transits obtained and their baseline and sampling.   PLATO will launch at the end of 2026 and focus on the detection of new exoplanets around bright stars. A supplementary scientific outcome will be the continuous observation of known exoplanets that will provide TTV/tidal decay monitoring. However to constrain planetary masses and orbit evolution we need to fill in gaps in the long-baseline data between the discovery transits and those that PLATO will observe. To do this we will observe transits of known exoplanets in the PLATO long- stare fields that are visible by CHEOPS.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-qwolfxj
title: 2781304

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-r78bnbb
title: 2791946

description:   Target RA (J2000):  274.405456542969  and deg    Target Dec (J2000):  36.6214408874512  and deg    Gaia GMag:  11.816   Programme ID:  CH_PR149004   Programme Manager:  WILSON   PI of observing programme:  Benz   Title of programme:  SoM - Pre-PLATO TTVIGIL (Transit Timing Variation observations to fill In Gaps In Long-baseline data)   Abstract:  Important current questions of exoplanet science require an underlying precise determination of planet internal structures that can be done by studying their mass and/or orbital evolution. Transit timing variations (TTVs) can bypass stellar activity issues that can hinder RVs observations to achieve accurate mass determination and transit timing monitoring may reveal tidal decay that can inform the orbital evolution history of planets. The accuracy of these methods is mainly driven by 1) the knowledge of individual transit centre times and 2) the number of transits obtained and their baseline and sampling.   PLATO will launch at the end of 2026 and focus on the detection of new exoplanets around bright stars. A supplementary scientific outcome will be the continuous observation of known exoplanets that will provide TTV/tidal decay monitoring. However to constrain planetary masses and orbit evolution we need to fill in gaps in the long-baseline data between the discovery transits and those that PLATO will observe. To do this we will observe transits of known exoplanets in the PLATO long- stare fields that are visible by CHEOPS.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-r8jer3r
title: 2833761

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-r9m4ff0
title: 2706594

description:   Target RA (J2000):  119.774345397949  and deg    Target Dec (J2000):  15.3914499282837  and deg    Gaia GMag:  11.35   Programme ID:  CH_PR149003   Programme Manager:  BRANDEKER   PI of observing programme:  Benz   Title of programme:  SoM - Simultaneous exoplanet observations with JWST   Abstract:  JWST observations of exoplanet transits occultations and phase curves can strongly benefit from simultaneous high-precision photometry in the optical. Advantages range from disentangling even minute stellar variability from the planetary signal to help characterise the exoplanet atmosphere from e.g. the strong wavelength dependence of potentially time variable aerosol hazes. Since approved JWST programmes are scheduled well in advance this synergy programme is designed to attempt simultaneous exoplanet observations with CHEOPS whenever possible. The total number of requested orbits is expected to be around 100 per year.     [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rm2c4g6
title: 2652692

description:   Target RA (J2000):  145.827865600586  and deg    Target Dec (J2000):  15.0043601989746  and deg    Gaia GMag:  10.5   Programme ID:  CH_PR140068   Programme Manager:  EGGER   PI of observing programme:  Benz   Title of programme:  Axis 1 - Constraining the abundance of water in hot planets (HotWatermelon)   Abstract:  Planets located close enough to their star experience evaporation which leads to a dichotomy in the possible gas content of these objects. These planets either contain more than around one percent of gas (in mass) or no gas at all (see Owen and Wu 2017). This dichotomy when expressed in term of mass-radius relation implies the existence of a region in the mass-radius diagram of hot planets where dry planets cannot exist. We propose to observe planets that could lie in this region with CHEOPS. Combining a precise radius and mass will allow us to identify planets in this forbidden region hence showing that they have to contain volatiles most likely water. Our data combined with future JWST observations will also constrain the efficiency of evaporation.    [truncated! Please see actual data for full text]
DOI: 10.5281/zenodo.17277118
title: Georeferenced toponyms relating to the Consegne dei Boschi (1822)

description: The dataset contains 37 georeferenced place names relating to the Consegne del Bosco (1822) and located in the area north of Monte Chiodo (Santo Stefano d'Aveto, Liguria, Italy).The dataset has been developed within the framework of the project PRIN 2022 “Bridging geography and history of woodlands: analysing mountain wooded landscapes through multiple sources and historical GIS” (2022EKECST), funded by the European Union – Next Generation EU (CUP E53D23010170006).
DOI: 10.5281/zenodo.17277119
title: Georeferenced toponyms relating to the Consegne dei Boschi (1822)

description: The dataset contains 37 georeferenced place names relating to the Consegne del Bosco (1822) and located in the area north of Monte Chiodo (Santo Stefano d'Aveto, Liguria, Italy).The dataset has been developed within the framework of the project PRIN 2022 “Bridging geography and history of woodlands: analysing mountain wooded landscapes through multiple sources and historical GIS” (2022EKECST), funded by the European Union – Next Generation EU (CUP E53D23010170006).
DOI: 10.57780/esa-rrcpmgj
title: 2822595

description:   Target RA (J2000):  319.699584960938  and deg    Target Dec (J2000):  -26.6163692474365  and deg    Gaia GMag:  8.227   Programme ID:  CH_PR149002   Programme Manager:  EDWARDS   PI of observing programme:  Benz   Title of programme:  SoM - ArielExoClock   Abstract:  To uncover the demographics of exoplanet atmospheres Ariel will require a large diverse list of potential targets. Luckily ground-based and space-based surveys have detected hundreds of transiting planets around bright stars. However simply knowing of the planets existence is not enough and preliminary characterisation efforts must be undertaken to ensure the suitability of the target for study. A key piece of information is an accurate knowledge of the predicted transit time of a planet. In this programme CHEOPS observations will be used to support the Ariel mission by maintaining the ephemeris of critical targets.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rskpwvd
title: 2654148

description:   Target RA (J2000):  98.3511123657227  and deg    Target Dec (J2000):  -23.4861907958984  and deg    Gaia GMag:  10.142   Programme ID:  CH_PR149004   Programme Manager:  WILSON   PI of observing programme:  Benz   Title of programme:  SoM - Pre-PLATO TTVIGIL (Transit Timing Variation observations to fill In Gaps In Long-baseline data)   Abstract:  Important current questions of exoplanet science require an underlying precise determination of planet internal structures that can be done by studying their mass and/or orbital evolution. Transit timing variations (TTVs) can bypass stellar activity issues that can hinder RVs observations to achieve accurate mass determination and transit timing monitoring may reveal tidal decay that can inform the orbital evolution history of planets. The accuracy of these methods is mainly driven by 1) the knowledge of individual transit centre times and 2) the number of transits obtained and their baseline and sampling.   PLATO will launch at the end of 2026 and focus on the detection of new exoplanets around bright stars. A supplementary scientific outcome will be the continuous observation of known exoplanets that will provide TTV/tidal decay monitoring. However to constrain planetary masses and orbit evolution we need to fill in gaps in the long-baseline data between the discovery transits and those that PLATO will observe. To do this we will observe transits of known exoplanets in the PLATO long- stare fields that are visible by CHEOPS.    [truncated! Please see actual data for full text]