cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-4y7gubk
title: 2368363

description:   Target RA (J2000):  154.908371  and deg    Target Dec (J2000):  -9.80628  and deg    Gaia GMag:  11.907    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-4ylhyh7
title: 2378775

description:   Target RA (J2000):  205.454254  and deg    Target Dec (J2000):  -0.12817  and deg    Gaia GMag:  10.244    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-55dt27j
title: 2422868

description:   Target RA (J2000):  231.955750  and deg    Target Dec (J2000):  -56.31886  and deg    Gaia GMag:  10.76    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-55leyzh
title: 2404306

description:   Target RA (J2000):  205.454254  and deg    Target Dec (J2000):  -0.12817  and deg    Gaia GMag:  10.244    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-569mxed
title: 2382612

description:   Target RA (J2000):  230.450623  and deg    Target Dec (J2000):  -48.31763  and deg    Gaia GMag:  5.462    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: 10.15468/dl.9utvuw
title: Occurrence Download

description: A dataset containing 4138 species occurrences available in GBIF matching the query:
{
 "and" : [
 "TaxonKey is Atherinops affinis (Ayres, 1860)",
 "HasGeospatialIssue is false",
 "HasCoordinate is true",
 "OccurrenceStatus is Present",
 "Year is greater than or equal to 1900",
 "CoordinateUncertaintyInMeters is less than or equal to 10000"
 ]
}

 The dataset includes 4138 records from 19 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0039000-241126133413365/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.57780/esa-56dsxz3
title: 2547047

description:   Target RA (J2000):  17.888014  and deg    Target Dec (J2000):  -36.70910  and deg    Gaia GMag:  11.368    Programme ID:  CH_PR250008   PI of observing programme:  Standing   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-56xhu26
title: 2424111

description:   Target RA (J2000):  223.193604  and deg    Target Dec (J2000):  -68.66654  and deg    Gaia GMag:  9.854    Programme ID:  CH_PR140087   Programme Manager:  BATTLEY   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-58aj9p8
title: 2576014

description:   Target RA (J2000):  53.232685  and deg    Target Dec (J2000):  -9.45826  and deg    Gaia GMag:  3.47    Programme ID:  CH_PR250017   PI of observing programme:  Roettenbacher   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-58f9cnr
title: 2450902

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]
DOI: 10.57780/esa-58o20ip
title: 2526798

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 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-5bez6p6
title: 2373093

description:   Target RA (J2000):  229.838120  and deg    Target Dec (J2000):  29.20617  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-5de6y6k
title: 2518892

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-5j2r33g
title: 2602618

description:   Target RA (J2000):  46.060631  and deg    Target Dec (J2000):  43.55794  and deg    Gaia GMag:  9.71    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: 10.6084/m9.figshare.c.3820399_d1
title: Additional file 1: of Physiological mechanisms of adaptive developmental plasticity in Rana temporaria island populations

description: Raw data obtained during the study and used in statistical analyses. (XLSX 114Â kb)
DOI: 10.57780/esa-5r53r8h
title: 2486702

description:   Target RA (J2000):  319.949707  and deg    Target Dec (J2000):  -58.14893  and deg    Gaia GMag:  10.261    Programme ID:  CH_PR149002   Programme Manager:  EDWARDS   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-5rgueai
title: 2598480

description:   Target RA (J2000):  62.966446  and deg    Target Dec (J2000):  -37.93978  and deg    Gaia GMag:  10.75    Programme ID:  CH_PR250035   PI of observing programme:  Shivkumar   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-5shqyvc
title: 2537250

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-5thy1sw
title: 2609627

description:   Target RA (J2000):  76.649544  and deg    Target Dec (J2000):  -20.24559  and deg    Gaia GMag:  11.63    Programme ID:  CH_PR250026   PI of observing programme:  Chakraborty   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.6084/m9.figshare.c.3820396_d2.v1
title: Additional file 2: of Identification and characterization of a FOXA2-regulated transcriptional enhancer at a type 2 diabetes intronic locus that controls GCKR expression in liver cells

description: Datasets. (XLSX 178 kb)
DOI: 10.57780/esa-5txtoou
title: 2573267

description:   Target RA (J2000):  17.888014  and deg    Target Dec (J2000):  -36.70910  and deg    Gaia GMag:  11.368    Programme ID:  CH_PR250008   PI of observing programme:  Standing   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.6084/m9.figshare.c.3820396_d2
title: Additional file 2: of Identification and characterization of a FOXA2-regulated transcriptional enhancer at a type 2 diabetes intronic locus that controls GCKR expression in liver cells

description: Datasets. (XLSX 178 kb)
DOI: 10.57780/esa-5ur0das
title: 2404021

description:   Target RA (J2000):  251.276459  and deg    Target Dec (J2000):  33.50923  and deg    Gaia GMag:  7.48    Programme ID:  CH_PR240019   PI of observing programme:  Stalport   Title of programme:  Understanding stellar activity patterns by coupling absolute photometry and intense RV monitoring   Abstract:  Nowadays stellar activity constitutes the main obstacle to the detection of planets with sub-meter per second radial velocity (RV) amplitudes. In the near future the PLATO mission will survey with high precision the photometric variations of bright stars inxa0specific areas of the sky. The combination of those observations with the most precise spectrographs will certainly be of upmost interest to alleviate stellar activity effects and provide mass measurements below the meter per second level needed to reach PLATO’s science goals. CHEOPS represents a unique opportunity to take a step ahead in prevision of PLATO and valuably support extensive RV surveys. We propose a long-term absolute photometry campaign in parallel to an already secured intense RV monitoring on HD151288 a moderately active star with yet-unclear activity patterns. In the fashion of a filler program with very limited constraints those observations could shed light on the complex RV stellar activity signals and they would serve as a benchmark for CHEOPS long-term stability and ability to conduct precise absolute photometry.    [truncated! Please see actual data for full text]