cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-i9r1rnb
title: 2319894

description:   Target RA (J2000):  141.107849  and deg    Target Dec (J2000):  5.76606  and deg    Gaia GMag:  10.164    Programme ID:  CH_PR140083   Programme Manager:  SERRANO   PI of observing programme:  Benz   Title of programme:  Axis 1 - ChOIs-reloaded   Abstract:  While the TESS mission is monitoring the sky for planetary transits its photometric precision is lower than that of CHEOPS. This means that signals detected at low signal-to-noise by TESS can be confirmed with CHEOPS. We will observe such low SNR candidates from TESS with a three-fold objective:   1) we will follow-up tentative signals in multi-planet systems as these are less likely to be false positives than systems with a single planet   2) we will prioritize the confirmation of candidates that can be confirmed by ongoing and future radial-velocity campaigns   3) we will collect sufficient transits to measure radii with a precision of at least 6%. Such precision coupled with a 10% precision on the planetary mass is necessary for a detailed analysis of both the internal structure of the exoplanet and the formation/evolution process of the system.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ia2ukld
title: 2104114

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-iaasxc4
title: 2249462

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-ib2sg6g
title: 2044986

description:   Target RA (J2000):  197.317459  and deg    Target Dec (J2000):  -60.30836  and deg    Gaia GMag:  8.09    Programme ID:  CH_PR100017   Programme Manager:  PAGANO   PI of observing programme:  Benz   Title of programme:  ANCILLARY SCIENCE - Recovering ephemeris   Abstract:  There are a number (about 2 tens) of transiting planetst of interest for follow-up characterizing measurements (JWST E-ELT) whose ephemeris must be recovered before going with large facilities and this can be done by CHEOPS.  It is proposed to monitor one transit per target  the observing window centered on the transit time predicted by the best available ephemeris and lasting two times the uncertainty on T0 plus the transit duration. Target list and target priority shall be modified according to results from K2 and TESS campaigns.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ibcu264
title: 2161817

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-igvlnwr
title: 2187945

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-ijggayh
title: 2243718

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-ijj4gh5
title: 2106675

description:   Target RA (J2000):  241.824097  and deg    Target Dec (J2000):  -22.06020  and deg    Gaia GMag:  8.519    Programme ID:  CH_PR230004   PI of observing programme:  Deeg   Title of programme:  Determining the internal structure of the young hierarchical triple HD 144548   Abstract:  HD 144548 is a young (8-11 Myr) triply eclipsing triple star in the Upper Scorpius OB association that displays complex eclipses from simultaneous occultations of all components (syzygys). This system is unique for the availability of both precise Kepler/K2 eclipse light curves from and radial velocities of all three components. In Alonso et al. (2015) we derived the components’ physical and orbital parameters with high precision indicating significantly inflated stellar sizes albeit the size of the system’s largest component is in tension with established models of young stars. With  CHEOPS we intend to reobserve several eclipses towards an actualized determination of the systems parameters. Particularly this should lead to a much improved determination of the system’s osculating orbital parameters due to a coverage that would span 9 years versus the 79 days from K2. Such improved osculating parameters should permit a derivation of the internal mass-distribution of the system’s inner binary through determination of the apsidal constant k_2. Reducing uncertainties on the orbital parameters found by Alonso et al. will also significantly improve the precision of the system’s physical parameters and permit a calibration of pre-main sequence star parameters and of the evolution of their stellar interiors. CHEOPS is uniquely suited to perform the observations of the long complex eclipses with a required (and expected) precision that should rival the original Kepler/K2 data.    [truncated! Please see actual data for full text]
DOI: 10.15468/dl.ssd5a7
title: Occurrence Download

description: A dataset containing 183 species occurrences available in GBIF matching the query:
{
 "TaxonKey" : [
 "is Rhodolaena humblotii Baill."
 ]
}

 The dataset includes 183 records from 11 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0097758-240321170329656/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.57780/esa-ijmd2g8
title: 2209396

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-ik5t8h1
title: 2188544

description:   Target RA (J2000):  284.500580  and deg    Target Dec (J2000):  5.90812  and deg    Gaia GMag:  8.46    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-ik6pu02
title: 2252689

description:   Target RA (J2000):  38.205170  and deg    Target Dec (J2000):  10.07261  and deg    Gaia GMag:  11.53    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-ilja7jh
title: 2073715

description:   Target RA (J2000):  197.669632  and deg    Target Dec (J2000):  -15.40602  and deg    Gaia GMag:  13.653    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-ilp398v
title: 2235716

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-ils5i6d
title: 2059318

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-iop7ysf
title: 2138017

description:   Target RA (J2000):  260.210907  and deg    Target Dec (J2000):  -45.42083  and deg    Gaia GMag:  7.24    Programme ID:  CH_PR140070   Programme Manager:  SZABO   PI of observing programme:  Benz   Title of programme:  Axis 3 - Photometric transits of exocomets   Abstract:  We aim to observe the spectroscopically proven exocomet-hosting systems with CHEOPS. Emphasis  will be on the two-band TESS+CHEOPS photometry and the synchronous spectroscopic observation to observe  the same transit in spectroscopy and  photometry for the first time. Photometric observations will give  us an insight to the structure and the total scattering cross section of the comet in transit while  spectroscopy shows us the total amount of refractory elements in the line of sight. Combining these two  we will be able to observe the parameters of the dust such as the content of refractory elements in the  dust and we can infer to the size distribution index of the dust grains.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ipomud0
title: 2162612

description:   Target RA (J2000):  271.281586  and deg    Target Dec (J2000):  -3.03132  and deg    Gaia GMag:  8.52    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-ira8895
title: 2159951

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]