cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-628op32
title: 2728505

description:   Target RA (J2000):  210.044494628906  and deg    Target Dec (J2000):  38.7057800292969  and deg    Gaia GMag:  11.94   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: 10.17026/ar/xfc0n5
title: Woudhuizermark, zonnepark A50 te Apeldoorn, gemeente Apeldoorn, een oppervlaktekartering

description: Een oppervlaktekartering
DOI: 10.57780/esa-67vxx2s
title: 2709332

description:   Target RA (J2000):  216.924026489258  and deg    Target Dec (J2000):  41.9534187316895  and deg    Gaia GMag:  9.659   Programme ID:  CH_PR150100   Programme Manager:  ZULETA   PI of observing programme:  Benz   Title of programme:  SoM - TRACE   Abstract:  The TRACE (Measuring the TRansit light sourCe Effect with CHEOPS) program aims to use the CHEOPS telescope to characterize the transit light source effect (TLSE) for exoplanet targets scheduled for observation with the JWST. This effort addresses a critical challenge in exoplanet atmosphere analysis: contamination from stellar activity such as star spots and faculae which can skew measurements of planetary atmospheres by introducing variability in observed spectra. The program will conduct high-precision photometric observations in the optical band an essential range that JWST does not cover but is critical to identify and mitigate stellar contamination in transmission spectra. Focusing on two primary targets in a first stage --TOI-1416 and GJ9827--the project plans long-baseline in and out-of-transit observations spread across a few stellar rotations to model activity-related flux variations. These findings are expected to help the JWST data interpretation of the planets atmosphere and support the broader scientific community by making data publicly available immediately. By characterizing activity in CHEOPS-observed systems TRACE aims to enhance our understanding of exoplanet atmospheres and prepare for future synergy with upcoming missions such as PANDORA.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-6b4czn0
title: 2882751

description:   Target RA (J2000):  311.289703369141  and deg    Target Dec (J2000):  -31.3409004211426  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-6bdn07p
title: 2722011

description:   Target RA (J2000):  139.231170654297  and deg    Target Dec (J2000):  -20.6763095855713  and deg    Gaia GMag:  11.515   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-6eftrcm
title: 2889659

description:   Target RA (J2000):  351.770172119141  and deg    Target Dec (J2000):  -1.28627002239227  and deg    Gaia GMag:  9.841   Programme ID:  CH_PR159006   Programme Manager:  ZULETA   PI of observing programme:  Benz   Title of programme:  SoM - TRACE   Abstract:  The TRACE (Measuring the TRansit light sourCe Effect with CHEOPS) program aims to use the CHEOPS telescope to characterize the transit light source effect (TLSE) for exoplanet targets scheduled for observation with the JWST. This effort addresses a critical challenge in exoplanet atmosphere analysis: contamination from stellar activity such as star spots and faculae which can skew measurements of planetary atmospheres by introducing variability in observed spectra. The program will conduct high-precision photometric observations in the optical band an essential range that JWST does not cover but is critical to identify and mitigate stellar contamination in transmission spectra. Focusing on two primary targets in a first stage --TOI-1416 and GJ9827--the project plans long-baseline in and out-of-transit observations spread across a few stellar rotations to model activity-related flux variations. These findings are expected to help the JWST data interpretation of the planets atmosphere and support the broader scientific community by making data publicly available immediately. By characterizing activity in CHEOPS-observed systems TRACE aims to enhance our understanding of exoplanet atmospheres and prepare for future synergy with upcoming missions such as PANDORA.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-6ovnc7a
title: 2769162

description:   Target RA (J2000):  311.289703369141  and deg    Target Dec (J2000):  -31.3409004211426  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-759tzcw
title: 2771302

description:   Target RA (J2000):  267.640502929688  and deg    Target Dec (J2000):  36.5702209472656  and deg    Gaia GMag:  10.486   Programme ID:  CH_PR149004   Programme Manager:  WILSON   PI of observing programme:  Benz   Title of programme:  SoM - Pre-PLATO TTVIGIL (Transit Timing Variation observations to fill In Gaps In Long-baseline data)   Abstract:  Important current questions of exoplanet science require an underlying precise determination of planet internal structures that can be done by studying their mass and/or orbital evolution. Transit timing variations (TTVs) can bypass stellar activity issues that can hinder RVs observations to achieve accurate mass determination and transit timing monitoring may reveal tidal decay that can inform the orbital evolution history of planets. The accuracy of these methods is mainly driven by 1) the knowledge of individual transit centre times and 2) the number of transits obtained and their baseline and sampling.   PLATO will launch at the end of 2026 and focus on the detection of new exoplanets around bright stars. A supplementary scientific outcome will be the continuous observation of known exoplanets that will provide TTV/tidal decay monitoring. However to constrain planetary masses and orbit evolution we need to fill in gaps in the long-baseline data between the discovery transits and those that PLATO will observe. To do this we will observe transits of known exoplanets in the PLATO long- stare fields that are visible by CHEOPS.    [truncated! Please see actual data for full text]
DOI: 10.17869/enu.2025.4792248
title: Interprofessional competency attainment among pre-registration health and social care professions students

description: Two datasets measuring interprofessional competency attainment among pre-registration health and social care professions students across different academic years. Data were collected using the Interprofessional Collaborative Competency Attainment Scale following Interprofessional Learning (IPL) events in the respective years.
DOI: 10.57780/esa-7824tfl
title: 2652602

description:   Target RA (J2000):  68.59375  and deg    Target Dec (J2000):  43.0374183654785  and deg    Gaia GMag:  12.3   Programme ID:  CH_PR149003   Programme Manager:  BRANDEKER   PI of observing programme:  Benz   Title of programme:  SoM - Simultaneous exoplanet observations with JWST   Abstract:  JWST observations of exoplanet transits occultations and phase curves can strongly benefit from simultaneous high-precision photometry in the optical. Advantages range from disentangling even minute stellar variability from the planetary signal to help characterise the exoplanet atmosphere from e.g. the strong wavelength dependence of potentially time variable aerosol hazes. Since approved JWST programmes are scheduled well in advance this synergy programme is designed to attempt simultaneous exoplanet observations with CHEOPS whenever possible. The total number of requested orbits is expected to be around 100 per year.     [truncated! Please see actual data for full text]
DOI: 10.57780/esa-79ii1ex
title: 2719409

description:   Target RA (J2000):  144.555297851562  and deg    Target Dec (J2000):  23.5466995239258  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 planets 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: 10.17026/ar/4y7til
title: Bonrepas 7a te Vlist, gemeente Krimpenerwaard
title: Een bureauonderzoek en inventariserend veldonderzoek in de vorm van een verkennend booronderzoek

description: Op basis van het bureauonderzoek is een gespecificeerde verwachting opgesteld. In het onderzoeks¬gebied was het Benschop- en Graaf-rivierensysteem actief gedurende het Neolithicum tot en met de Bronstijd Op de oeverafzettingen van dit systeem kunnen dus archeologische resten uit het Neolithicum tot en met de Bronstijd worden aangetroffen. Maar in het plangebied zijn deze afzettingen waarschijnlijk niet aanwezig. Dit rivierensysteem is noordelijker gelegen. Daarom geldt er een lage verwachting voor resten uit de periode Neolithicum tot en met de Bronstijd.

Gedurende de IJzertijd tot en met de Vroege Middeleeuwen was er een uitgestrekt veenmoeras aanwezig. Het is niet waarschijnlijk dat het veenmoeras geschikt is geweest voor bewoning gedurende deze perioden. Kleinschalige bewoningsactiviteiten kunnen wel hebben plaatsgevonden langs de oeverzone van de Vlist. Die werd actief vanaf circa 200 tot 1150 n. Chr. hoewel er geen sprake was van goed ontwikkelde oeverwallen. Voor deze perioden geldt daarom een middelhoge archeologische verwachting.

De ontginning van het veengebied begon in de Late Middeleeuwen. De ontginning gebeurde in fases en het plangebied ligt ter plaatse van een ontginningslint dat behoort tot de eerste fase. De bewoning en ontginning is daarom vermoedelijk in de 11e en 12e eeuw ontstaan. Door de ontwatering begon de ondergrond in te klinken en werden er verhogingen (terpen) gemaakt om daar de boerderijen op te bouwen. In het plangebied is geen sprake van een dergelijke terp. Daarnaast is op kaartmateriaal ook geen historische bebouwing waargenomen. Hierdoor wordt vermoed dat het plangebied onbebouwd is gebleven en in gebruik is geweest als agrarisch land. Daarom is de archeologische verwachting voor deze periode laag.

De natuurlijke ondergrond bestaat uit mineraalarm veen (Formatie van Nieuwkoop Hollandveen Laagpakket. In boring 3 is de top van het pakket veraard. In boringen 2, 3 en 4 zijn hierboven komafzettingen van de Vlist of de Lek aanwezig. In boring 1 ontbreekt dit pakket. De bovengrond bestaat uit omgewerkte komafzettingen of een zand- en puinhoudend ophogingspakket.

Vanwege het ontbreken archeologisch relevante lagen (oeverafzettingen van de Vlist) worden in het plangebied geen archeologische resten meer verwacht.

ADC ArcheoProjecten adviseert om het plangebied vrij te geven voor de voorgenomen ontwik-keling. Het is altijd mogelijk dat tijdens grondwerkzaamheden onverwacht archeologische vondsten aan het licht komen. Het verdient daarom aanbeveling om de uitvoerder van de grondwerkzaam¬heden te wijzen op de plicht deze zogenoemde toevalsvondsten te melden bij de bevoegde overheid, zo¬als aangegeven in artikel 5.10 en 5.11 van de Erfgoedwet. De melding dient behalve bij de Rijksdienst voor het Cultureel Erfgoed (RCE) tevens plaats te vinden bij de gemeente Krimpenerwaard.
DOI: 10.57780/esa-7f3mx9a
title: 2881000

description:   Target RA (J2000):  351.770172119141  and deg    Target Dec (J2000):  -1.28627002239227  and deg    Gaia GMag:  9.841   Programme ID:  CH_PR159006   Programme Manager:  ZULETA   PI of observing programme:  Benz   Title of programme:  SoM - TRACE   Abstract:  The TRACE (Measuring the TRansit light sourCe Effect with CHEOPS) program aims to use the CHEOPS telescope to characterize the transit light source effect (TLSE) for exoplanet targets scheduled for observation with the JWST. This effort addresses a critical challenge in exoplanet atmosphere analysis: contamination from stellar activity such as star spots and faculae which can skew measurements of planetary atmospheres by introducing variability in observed spectra. The program will conduct high-precision photometric observations in the optical band an essential range that JWST does not cover but is critical to identify and mitigate stellar contamination in transmission spectra. Focusing on two primary targets in a first stage --TOI-1416 and GJ9827--the project plans long-baseline in and out-of-transit observations spread across a few stellar rotations to model activity-related flux variations. These findings are expected to help the JWST data interpretation of the planets atmosphere and support the broader scientific community by making data publicly available immediately. By characterizing activity in CHEOPS-observed systems TRACE aims to enhance our understanding of exoplanet atmospheres and prepare for future synergy with upcoming missions such as PANDORA.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-7hpbz0i
title: 2712484

description:   Target RA (J2000):  164.648620605469  and deg    Target Dec (J2000):  14.6238603591919  and deg    Gaia GMag:  12.24   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-7i7vsi6
title: 2763609

description:   Target RA (J2000):  186.817169189453  and deg    Target Dec (J2000):  -29.8328304290772  and deg    Gaia GMag:  11.342   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-7kqaaht
title: 2882782

description:   Target RA (J2000):  311.289703369141  and deg    Target Dec (J2000):  -31.3409004211426  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]