cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-wjlot2a
title: 2423021

description:   Target RA (J2000):  273.602203  and deg    Target Dec (J2000):  -66.41981  and deg    Gaia GMag:  10.86    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-wl7hleq
title: 2487384

description:   Target RA (J2000):  309.353363  and deg    Target Dec (J2000):  22.65461  and deg    Gaia GMag:  9.081    Programme ID:  CH_PR140085   Programme Manager:  VENTURINI   PI of observing programme:  Benz   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-wme877x
title: 2366590

description:   Target RA (J2000):  123.949913  and deg    Target Dec (J2000):  5.83677  and deg    Gaia GMag:  10.3    Programme ID:  CH_PR140076   Programme Manager:  PATEL   PI of observing programme:  Benz   Title of programme:  Axis2 - Terminators   Abstract:  Exoplanetary atmospheres are 3D objects and various physical processes make them inhomogeneous over different parts of the planet. In particular several studies have demonstrated that different thermal structures and wind patterns over the morning and evening terminator can produce an inhomogeneous cloud coverage over the atmosphere. However a common assumption made while performing transmission spectroscopy of exoplanets is of a homogeneous atmosphere. Considering such an inhomogeneous atmosphere as a homogeneous one can lead to biases in retrieved atmospheric properties. Inhomogeneities in the atmosphere also leave an impact on broadband photometry. In this program we aim to detect this effect directly on the transit lightcurve of three planets. The magnitude of this effect could be as large as 1000 ppm for suitable targets which CHEOPS should be able to detect comfortably. While inhomogeneity can be in chemical structure or aerosol properties we mainly aim to put constraints on asymmetric cloud coverage with CHEOPS observations. We have identified WASP-54 b HAT-P-30 b and WASP-131 b as being the best candidates for detection due to their atmospheric transmission signal transit duration and temperature. Our observations would pave a way for future observations with spectroscopic capabilities to constrain the inhomogeneous atmospheres of these planets.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-wpdgffr
title: 2516515

description:   Target RA (J2000):  311.289703  and deg    Target Dec (J2000):  -31.34090  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-wrvh904
title: 2534938

description:   Target RA (J2000):  42.984364  and deg    Target Dec (J2000):  -30.81453  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-wuxhbvh
title: 2549173

description:   Target RA (J2000):  24.354305  and deg    Target Dec (J2000):  -45.67788  and deg    Gaia GMag:  9.166    Programme ID:  CH_PR140063   Programme Manager:  BARROS   PI of observing programme:  Benz   Title of programme:  Axis 3 - Measuring tides that shape planetary systems (TIDES)   Abstract:  Ultra-short orbital period planets suffer from intense tidal forces which lead to a deformation of the planets shape (Correia 2014  Barros et al. 2022) and shrinkage of the planets orbit. Measuring the tidal deformation of the planet allows us to estimate the second-degree fluid Love number and gain insight into the planets internal structure. Moreover measuring the tidal decay timescale allows us to estimate the stellar tidal quality factor which is key to constraining stellar physics. Therefore studying tidal effects in ultra-short orbital period planets gives us a wealth of information on planet-to-star tidal interactions that shape planetary systems. We also propose to estimate the tidal decay of a few hot-Jupiters for which we expect a measurable orbital period decrease within the next 3 years. The longer baseline allowed by the CHEOPS extension will be crucial for our ability to measure the tidal decay of some systems. During the CHEOPS nominal mission we achieved a breakthrough on the direct detection of the tidal deformation of exoplanets. Building on these results we also propose to better constrain the tidal deformation of WASP-103b and WASP-12b directly from the transit deformation signature (similar to  Barros et al. 2022) and also from the signature in the phase curve (similar to Akinsanmi et al. in prep.).    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-wzt0go0
title: 2562860

description:   Target RA (J2000):  0.362169  and deg    Target Dec (J2000):  39.38383  and deg    Gaia GMag:  10.591    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-x29ixwi
title: 2421843

description:   Target RA (J2000):  175.169495  and deg    Target Dec (J2000):  -58.10433  and deg    Gaia GMag:  8.69    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-x4xr35u
title: 2530031

description:   Target RA (J2000):  330.794861  and deg    Target Dec (J2000):  18.88431  and deg    Gaia GMag:  7.509    Programme ID:  CH_PR140078   Programme Manager:  DEMANGEON   PI of observing programme:  Benz   Title of programme:  Axis 2 - Beyond Geometrical Albedo: A deeper understanding of the reflective behavior of exoplanet atmospheres (BENGAL)   Abstract:  Our knowledge of the reflective properties of exoplanet atmospheres is extremely limited outside of the Solar System planets. The geometric and Bond albedo measurements constitute the majority of the subjects observational constraints. Reflected light phase curves hold the key to gaining a better understanding of the fundamental scattering properties: single scattering albedo and asymmetry as well as determining the degree of inhomogeneity in the spatial distribution of clouds hazes and aerosols. However due to observational biases the vast majority of existing datasets that show a clear phase curve signal in the visible are aimed at hot gas giants. As a result they are plagued by the degeneracy between reflected and thermal light. Only Kepler-7 b was cool enough and Kepler sensitive enough to deliver a high precision phase curve that is dominated by reflected light. Kepler-7 b is thus the only exoplanet for which we have direct measurements of  cloud distribution inhomogeneity and fundamental scattering properties.  With this program we will leverage CHEOPS’ photometric precision bandpass and pointing flexibility to perform repeated phase curves observations of a few key targets. These canonical datasets will provide precise reflected light phase curves and will offer long-awaited counterparts to Kepler-7 b. We will investigate atmospheric inhomogeneity and measure fundamental scattering properties. We will begin to explore the [truncated! Please see actual data for full text]
DOI: 10.57780/esa-x5v0s44
title: 2542567

description:   Target RA (J2000):  311.289703  and deg    Target Dec (J2000):  -31.34090  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-xa5okjn
title: 2414012

description:   Target RA (J2000):  175.169495  and deg    Target Dec (J2000):  -58.10433  and deg    Gaia GMag:  8.69    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-xblrbnz
title: 2599166

description:   Target RA (J2000):  82.864151  and deg    Target Dec (J2000):  -3.67723  and deg    Gaia GMag:  7.11    Programme ID:  CH_PR250004   PI of observing programme:  Poyatos   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-xey5awv
title: 2574269

description:   Target RA (J2000):  65.717537  and deg    Target Dec (J2000):  -12.67708  and deg    Gaia GMag:  10.86    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: 10.57780/esa-xgb1i2q
title: 2518241

description:   Target RA (J2000):  353.357452  and deg    Target Dec (J2000):  -41.17151  and deg    Gaia GMag:  11.9    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-xmqgkom
title: 2549277

description:   Target RA (J2000):  348.949036  and deg    Target Dec (J2000):  -10.84969  and deg    Gaia GMag:  12    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 characterization of  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-xpnr35a
title: 2444115

description:   Target RA (J2000):  207.526169  and deg    Target Dec (J2000):  -40.83580  and deg    Gaia GMag:  9.61    Programme ID:  CH_PR240004   PI of observing programme:  Ilin   Title of programme:  HIP 67522 b – a Hot Jupiter that triggers flares on its host   Abstract:  The habitability of exoplanets depends crucially on the space weather they experience. A planet orbiting _inwards_ of the habitable zone is a natural probe of the magnetized winds and energetic radiation traveling towards a potentially habitable planet. When a planet orbits close enough to its host it can perturb the star’s magnetic field setting off energetic flares in the stellar corona. In the optical these flares appear as recurrent brightenings in phase with the orbit. If we measure such flares we immediately know that the planet moves inside the closed-field corona critical information for space weather modelers. To measure this planet-induced flaring we have to find flares occurring in excess of intrinsic stellar flaring. This is done by testing for deviations from a random distribution of flares with the orbital phase of the planet. HIP 67522 a 17 Myr Sun with a Hot Jupiter in a 7-day orbit detected in 2020 has the ideal properties to exhibit such excess flares. But there is more: In recent TESS data HIP 67522 flared a total of four times. Each time the flare took place within 10h after transit the same 4% of the planet’s orbit. This is very unlikely to happen if these flares occurred randomly. We propose to observe HIP 67522 using CHEOPS high sensitivity for flares for 16 visits for 8 orbits each during the critical 4% of HIP 67522 bs orbit to measure for the first time planet induced flares at high significance.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-xqfufr8
title: 2431555

description:   Target RA (J2000):  197.317459  and deg    Target Dec (J2000):  -60.30836  and deg    Gaia GMag:  8.09    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]