cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-spx7r72
title: 2316431

description:   Target RA (J2000):  94.404305  and deg    Target Dec (J2000):  31.61034  and deg    Gaia GMag:  10.682    Programme ID:  CH_PR230034   PI of observing programme:  Edwards   Title of programme:  Rescuing Longer Period TESS Planet Candidates for Future Atmospheric Characterisation   Abstract:  Keeping track of the colossal number of new exoplanet detections is becoming ever more difficult. Yet if we wish to conduct a thorough characterisation of these worlds by studying its atmosphere for instance we must be sure of when the planet is going to transit. Due to the short observing sectors of TESS (< 30 days) our knowledge of the ephemerides of these worlds is quickly decaying. In fact by the time most planet confirmation papers are published the uncertainty on the transit time is often into the tens of minutes and when followed-up large shifts are often seen in the transit times. The situation is even worse for longer period planets which are also more rarely found by the TESS mission. Hence we propose to conduct timely observations of seven of the best longer period TESS planet candidates for atmospheric characterisation. These data will ensure that our knowledge of their ephemeris remains up-to-date and so will facilitate the possibility for atmospheric characterisation in the near-future. CHEOPS is the only facility capable of these observations and the dataset proposed will be of great value to the exoplanet community.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-sr2ovlg
title: 2251714

description:   Target RA (J2000):  73.795753  and deg    Target Dec (J2000):  30.36649  and deg    Gaia GMag:  11.72    Programme ID:  CH_PR140069   Programme Manager:  SZABO   PI of observing programme:  Benz   Title of programme:  Axis 3 - Photometric Transients in Dusty Debris Disks   Abstract:  We observe systems with warm dust disks regardless to the orientation of the disk but with positive detections of photometric transients from the disk with TESS. The targets will be selected from the results of Ansdell et al 2020 and Gaidos et al. 2022 in respect to the expected efficiency of CHEOPS observations and if possible simultaneously to TESS observations. The simultaneous CHEOPS+TESS multiband data will give us the first two-band space photometry of scattering dust in distant solar systems.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-sw8b9y0
title: 2326909

description:   Target RA (J2000):  73.841423  and deg    Target Dec (J2000):  19.28089  and deg    Gaia GMag:  9.4    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-swtpcu3
title: 2155439

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 star's 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-szjm8q2
title: 2060435

description:   Target RA (J2000):  202.499100  and deg    Target Dec (J2000):  10.37716  and deg    Gaia GMag:  8.21    Programme ID:  CH_PR100018   Programme Manager:  PAGANO   PI of observing programme:  Benz   Title of programme:  ANCILLARY SCIENCE - Low level variability on short time scales of Mdwarfs   Abstract:  This is a filler program aimimg to characterize the stellar noise (mainly microflares  dips and short lasting oscillations) at short time scales  for Mdwarfs of different level of variability and other active late type stars hosting exoplanets. Being interested to micro-variability on time scales from few seconds to a hours even one CHEOPS orbit can get useful data. The measured parameters - mean variance pooled variaance flares/microflares occurence rate dips occurence rate power spectrum -  will be related  to stellar properties (Teff H-alpha Ca II H and K X-ray and UV fluxes).  Selected targets spans subclasess of late type stars with different level of activity. They have been selected among those  with already know stellar properties (typicall surveyed for exoplanet detection)  and include all  dM / late K and TTau  with  planets.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-szxlly8
title: 2260422

description:   Target RA (J2000):  73.795753  and deg    Target Dec (J2000):  30.36649  and deg    Gaia GMag:  11.72    Programme ID:  CH_PR140069   Programme Manager:  SZABO   PI of observing programme:  Benz   Title of programme:  Axis 3 - Photometric Transients in Dusty Debris Disks   Abstract:  We observe systems with warm dust disks regardless to the orientation of the disk but with positive detections of photometric transients from the disk with TESS. The targets will be selected from the results of Ansdell et al 2020 and Gaidos et al. 2022 in respect to the expected efficiency of CHEOPS observations and if possible simultaneously to TESS observations. The simultaneous CHEOPS+TESS multiband data will give us the first two-band space photometry of scattering dust in distant solar systems.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-t3r0ob7
title: 2183849

description:   Target RA (J2000):  311.289703  and deg    Target Dec (J2000):  -31.34090  and deg    Gaia GMag:  7.84    Programme ID:  CH_PR130057   Programme Manager:  SZABO   PI of observing programme:  Benz   Title of programme:  Pinning down a young planetary system: CHEOPS observations of AU Mic (CHAUMic)   Abstract:  We propose to carry out an intensive in-transit and out-of-transit CHEOPS observing campaign of the golden target AU Mic aiming at: • constraining the TTV signals of AU Mic b and c and measuring their masses. High-precision radial velocity observations of AU Mic are hampered by the activity of the star as recently shown by Zicher et al. 2022 (MNRAS 512 3060) who measured the masses of planet b and c with a precision of “only” 43 % and 30 % using more than 100 HARPS measurements evenly spread across one year. Conversely CHEOPS have proven to be very effective in measuring planet masses of near-resonant transiting systems such as TOI-1130 b and c for which a precision of ?9 % has been achieved exploiting the TTV method. Our program requires transit observations of planet b and c to be carried out in July August. • studying the evolution time-scale of active regions across the transit cord using AU Mic b as a “scanner”. Unbiased measurements of Rp/R? can be determined only by modeling the transit light curves along with the map of the occulted (and unocculted see below) spots. This requires CHEOPS multiple observations of the transits of AU Mic b at the 4 possible star-planet configurations. By observing spot-crossing events of transits occurring at the same stellar longitudes as in 2020 and 2021’s CHEOPS observations we will also assess whether the distribution of spots has evolved or not. On the other hand transit observations at stellar longitudes that have not yet b [truncated! Please see actual data for full text]
DOI: 10.57780/esa-t3zxfd4
title: 2048847

description:   Target RA (J2000):  188.346664  and deg    Target Dec (J2000):  6.42167  and deg    Gaia GMag:  13.126    Programme ID:  CH_PR100002   Programme Manager:  VANGROOTEL   PI of observing programme:  Benz   Title of programme:  ANCILLARY SCIENCE - Planet remnants around evolved stars with CHEOPS   Abstract:  This filler programme is to search for planet remnants transiting subdwarf B (sdB) stars which are evolved stars after the first red giant branch.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-t5r9xof
title: 2197843

description:   Target RA (J2000):  314.268463  and deg    Target Dec (J2000):  31.66097  and deg    Gaia GMag:  11.796    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 planet's shape (Correia 2014  Barros et al. 2022) and shrinkage of the planet's orbit. Measuring the tidal deformation of the planet allows us to estimate the second-degree fluid Love number and gain insight into the planet's 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-t7qo2r3
title: 2248335

description:   Target RA (J2000):  48.582321  and deg    Target Dec (J2000):  -34.03414  and deg    Gaia GMag:  11.412    Programme ID:  CH_PR240023   PI of observing programme:  Scarsdale   Title of programme:  Period Measurement of The Brightest-Host Transiting Habitable Zone Terrestrial Exoplanet   Abstract:  We propose to use CHEOPS photometry to measure the period of the Transiting Exoplanet Survey Satellite (TESS) planet candidate TOI4353.01 (TIC176797879) initially a duo-transit object that was confirmed with a transit detection in previous CHEOPS observations (priv. comm.). This object is a terrestrial-size exoplanet with three transits each separated by 718 days (two in TESS one in CHEOPS). This even separation and minimal phase coverage means that the period still needs to be determined. Based on the transit duration and a priori likelihood of transit the true period is very unlikely to be 718 days and instead is more likely to be an alias of that spacing in the 34-60 day range. This planet is therefore a likely-terrestrial planet candidate in its star’s optimistic habitable zone (OHZ). It has potential for future mass measurement and even transmission spectroscopy thanks to its bright (for an M star) host. In fact no other OHZ terrestrial has a host star as bright as TOI4353.01. Because of the rarity of terrestrial OHZ exoplanets and the difficulty of discovering more with TESS due to its short sectors followup of candidates like this one is of critical importance.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-t7sg9kd
title: 2040931

description:   Target RA (J2000):  177.780563  and deg    Target Dec (J2000):  35.27201  and deg    Gaia GMag:  8.85    Programme ID:  CH_PR100018   Programme Manager:  PAGANO   PI of observing programme:  Benz   Title of programme:  ANCILLARY SCIENCE - Low level variability on short time scales of Mdwarfs   Abstract:  This is a filler program aimimg to characterize the stellar noise (mainly microflares  dips and short lasting oscillations) at short time scales  for Mdwarfs of different level of variability and other active late type stars hosting exoplanets. Being interested to micro-variability on time scales from few seconds to a hours even one CHEOPS orbit can get useful data. The measured parameters - mean variance pooled variaance flares/microflares occurence rate dips occurence rate power spectrum -  will be related  to stellar properties (Teff H-alpha Ca II H and K X-ray and UV fluxes).  Selected targets spans subclasess of late type stars with different level of activity. They have been selected among those  with already know stellar properties (typicall surveyed for exoplanet detection)  and include all  dM / late K and TTau  with  planets.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-t8bt8d3
title: 2055648

description:   Target RA (J2000):  227.087692  and deg    Target Dec (J2000):  7.22079  and deg    Gaia GMag:  12.371    Programme ID:  CH_PR100002   Programme Manager:  VANGROOTEL   PI of observing programme:  Benz   Title of programme:  ANCILLARY SCIENCE - Planet remnants around evolved stars with CHEOPS   Abstract:  This filler programme is to search for planet remnants transiting subdwarf B (sdB) stars which are evolved stars after the first red giant branch.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-t9w6rp4
title: 2052403

description:   Target RA (J2000):  165.365326  and deg    Target Dec (J2000):  5.13948  and deg    Gaia GMag:  11.82    Programme ID:  CH_PR140066   Programme Manager:  NASCIMBENI   PI of observing programme:  Benz   Title of programme:  Axis 1 - Uncovering a maverick population: CHEOPS observations of hot Jupiter systems with inner small companions (MAVERICK)   Abstract:  Planetary systems hosting a hot or warm Jupiter (HJ/WJ) plus nearby small companion(s) such as WASP-47 (Nascimbeni et al. 2023) are extremely rare and very valuable to constrain formation and migration models. Only five such systems are known so far. Our goal is to increase the sample size by confirming and characterizing five TESS candidates with such an architecture and improving their orbital/physical parameters including ephemeris radii and (when feasible) planetary masses through TTVs. As demonstrated by our work on WASP-47 RVs and TTVs are very synergistic at decoding these complex systems. A dedicated RV follow-up will be coordinated.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ta29sgs
title: 2057440

description:   Target RA (J2000):  189.839218  and deg    Target Dec (J2000):  20.02734  and deg    Gaia GMag:  8.172    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 o [truncated! Please see actual data for full text]
DOI: 10.57780/esa-taxle5d
title: 2133209

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 star's 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-tb2qcpf
title: 2087099

description:   Target RA (J2000):  206.847687  and deg    Target Dec (J2000):  -6.13686  and deg    Gaia GMag:  9.901    Programme ID:  CH_PR230026   PI of observing programme:  Edwards   Title of programme:  Ephemeris Refinement of Key Targets for the ESA-Ariel Mission   Abstract:  The ESA-Ariel mission seeks to observe the atmospheres of around 1000 exoplanets. To maximise the science yield of the mission the sample of planets studied must be as diverse as possible probing all areas of the exoplanet population. To allow for this the catalogue of planets from which the Ariel sample is chosen must be significantly larger. For each of these potential targets a likely requirement is that number of key parameters are well characterised. One piece of knowledge that is undeniably obligatory is the predicted transit time of the planet in question. Keeping track of such a large number of worlds necessitates a well-structured follow-up programme and so the Ariel consortium has launched ExoClock which allows professional and amateur astronomers from around the world to support this effort. Nevertheless there are some planets which simply cannot be studied from the ground and for which TESS data is also of insufficient quality so another solution is required. Here we propose to use the excellent photometric performance of CHEOPS to study 9 key worlds for the Ariel mission. By observing these targets CHEOPS will be ensuring they are available for future atmospheric characterisation and thereby providing key support for another ESA mission.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-tcfc97y
title: 2161803

description:   Target RA (J2000):  269.452087  and deg    Target Dec (J2000):  4.69336  and deg    Gaia GMag:  8.2    Programme ID:  CH_PR100018   Programme Manager:  PAGANO   PI of observing programme:  Benz   Title of programme:  ANCILLARY SCIENCE - Low level variability on short time scales of Mdwarfs   Abstract:  This is a filler program aimimg to characterize the stellar noise (mainly microflares  dips and short lasting oscillations) at short time scales  for Mdwarfs of different level of variability and other active late type stars hosting exoplanets. Being interested to micro-variability on time scales from few seconds to a hours even one CHEOPS orbit can get useful data. The measured parameters - mean variance pooled variaance flares/microflares occurence rate dips occurence rate power spectrum -  will be related  to stellar properties (Teff H-alpha Ca II H and K X-ray and UV fluxes).  Selected targets spans subclasess of late type stars with different level of activity. They have been selected among those  with already know stellar properties (typicall surveyed for exoplanet detection)  and include all  dM / late K and TTau  with  planets.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-tgvkd7w
title: 2088869

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 star's 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]