cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-923rinz
title: 2050298

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: 10.15468/dl.az5tzs
title: Occurrence Download

description: A dataset containing 76 species occurrences available in GBIF matching the query:
{
 "TaxonKey" : [
 "is Rubus glaucovirens G.Maass"
 ]
}

 The dataset includes 76 records from 15 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0097741-240321170329656/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.57780/esa-93yytu0
title: 2048713

description:   Target RA (J2000):  165.017731  and deg    Target Dec (J2000):  22.83296  and deg    Gaia GMag:  8.97    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-95fksxm
title: 2091094

description:   Target RA (J2000):  274.268921  and deg    Target Dec (J2000):  21.90944  and deg    Gaia GMag:  8.34    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-96uebs0
title: 2235767

description:   Target RA (J2000):  54.183800  and deg    Target Dec (J2000):  28.55046  and deg    Gaia GMag:  12.19    Programme ID:  CH_PR240024   PI of observing programme:  Vach   Title of programme:  Confirmation of the first planet to be associated with the Pleiades cluster   Abstract:  The processes that drive planet formation and evolution within the first billion years are key in sculpting the planet population we observe today. Observing young planetary systems is the only opportunity to characterize these processes as they happen in real time. The Pleiades open cluster is one of the most well aged stellar groups at 120 Myr making it the ideal parent population to anchor planet evolution models. We propose to use CHEOPS to observe two transits of the first planetary candidate TOI-5358.01 kinematically affiliated with the Pleiades group. TOI-5358.01 is a mini-Neptune (P = 2.66 d Rp = 2.754 Rearth) orbiting the young K4V star TOI-5358 originally discovered by TESS. CHEOPS observations are critical in the confirmation and characterization of the system and will enable us to distinguish between different atmospheric characteristics such as clouds and haze in future transmission spectroscopy observations.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-98h2iln
title: 2169793

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-99qmq71
title: 2038099

description:   Target RA (J2000):  188.764709  and deg    Target Dec (J2000):  -5.29336  and deg    Gaia GMag:  11.06    Programme ID:  CH_PR120052   Programme Manager:  MAXTED   PI of observing programme:  Benz   Title of programme:  ANCILLARY SCIENCE - Short-period EBLM and hot-Jupiter systems   Abstract:  EBLM systems are FGK-type dwarf stars with M-dwarf companions. They are found in large numbers by transit surveys like WASP and many of them now have spectroscopic orbits for the primary star.   This makes it possible to accumulate high-precision transit light curves for these binaries that can be used to study limb-darkening star spots transit-timing variations etc. There are also about 10 hot Jupiter systems that can be added to the sample.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-9ab8wey
title: 2213982

description:   Target RA (J2000):  59.771751  and deg    Target Dec (J2000):  6.92461  and deg    Gaia GMag:  10.91    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-9bagjca
title: 2330093

description:   Target RA (J2000):  164.776077  and deg    Target Dec (J2000):  40.98361  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-9bm7564
title: 2330517

description:   Target RA (J2000):  144.555298  and deg    Target Dec (J2000):  23.54670  and deg    Gaia GMag:  7.748    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 planet’s 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-9byactr
title: 2055983

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-9g3ifw1
title: 2187163

description:   Target RA (J2000):  344.145020  and deg    Target Dec (J2000):  16.55343  and deg    Gaia GMag:  7.79    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-9gapb0i
title: 2357907

description:   Target RA (J2000):  185.339417  and deg    Target Dec (J2000):  57.75247  and deg    Gaia GMag:  11.96    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: 10.15468/dl.evvb9g
title: Occurrence Download

description: A dataset containing 31550 species occurrences available in GBIF matching the query:
{
 "TaxonKey" : [
 "is Rhodometra sacraria (Linnaeus, 1767)"
 ]
}

 The dataset includes 31550 records from 410 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0097732-240321170329656/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.57780/esa-9ii7hnu
title: 2249273

description:   Target RA (J2000):  51.640358  and deg    Target Dec (J2000):  -43.61356  and deg    Gaia GMag:  9.018    Programme ID:  CH_PR230027   PI of observing programme:  Eisner   Title of programme:  Readying a warm sub-Neptune orbiting around the bright Sun-like star TOI-4320 for future atmospheric characterisation   Abstract:  Sub-Neptune sized planets are amongst the most common types of exoplanets in our Galaxy however their formation and composition are still widely debated. Through transit spectroscopy we can probe their atmospheric composition and thus help constrain theories of how these systems form and evolve. We propose to refine the ephemerides and radius of a sub-Neptune sized planet orbiting around a bright Sun-like star that was identified in the TESS data by citizen scientists taking part in the Planet Hunters TESS project. The refined orbital period that we can determine with just one additional transit observation with CHEOPS will ensure that the mid-transit time of this target will be sufficiently constrained for future atmospheric characterisation with JWST or Ariel. Furthermore the refined planet radius combined with our ongoing radial velocity campaign to determine the mass of this planet will allow us to constrain the bulk composition and thus infer the internal structure of the planet. Even though sub-Neptune sized planets are common this one stands out due to its long orbital period (~25 days) compared to the majority of TESS planets and due to the brightness of the host star (Vmag = 9.17). To date less than 3% of all known sub-Neptune size planets transit stars with a Vmag brighter than10 highlighting the unique opportunity presented by this system.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-9jawdyb
title: 2316482

description:   Target RA (J2000):  150.538498  and deg    Target Dec (J2000):  50.14553  and deg    Gaia GMag:  11.77    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-9m6i8s7
title: 2216517

description:   Target RA (J2000):  48.378750  and deg    Target Dec (J2000):  -32.00550  and deg    Gaia GMag:  11.02    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-9mo9y1b
title: 2198032

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-9n5gdd7
title: 2154988

description:   Target RA (J2000):  304.538849  and deg    Target Dec (J2000):  -1.07572  and deg    Gaia GMag:  9.572    Programme ID:  CH_PR100016   Programme Manager:  LENDL   PI of observing programme:  Benz   Title of programme:  ATMOS.CHAR - Occultations   Abstract:  Scientific Objective: Obtain a representative sample of planetary occultation measurements constraining geometric albedos across a wide parameter space. Uncover trends and provide constrains on atmosphere models in particular with regard to complementary observations.    [truncated! Please see actual data for full text]