cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-kd5l26i
title: 2747709

description:   Target RA (J2000):  189.839218139648  and deg    Target Dec (J2000):  20.0273399353027  and deg    Gaia GMag:  8.172   Programme ID:  CH_PR140080   Programme Manager:  LELEU   PI of observing programme:  Benz   Title of programme:  Axis 1 - Architecture of Resonant Chains (ARC)   Abstract:  Resonant chains are gold mines for fueling our understanding of planetary systems. The minute details of their architectures encode the history of their formation: the order of the capture of the planets in the chain (Delisle 2017) the local shape of the proto-planetary disc and its dispersal (e.g.  Nesvorny et al 2022) and the long-term evolution of the system through tidal dissipation (e.g. Papaloizou et al 2018). The high multiplicity of these systems also makes them especially valuable to constrain our models of the formation of planetary systems (See Emsenhuber et al 2022 and other papers of the NGPPS series) since all the planets have to form in the same environment and the relative fragility of the configuration ensures that no violent evolution (e.g. close encounters/impacts) occurred after the dissipation of the proto-planetary disc (Leleu et al 2021). In addition the transit timing variations induced by the compactness of the systems allow for precise mass determination down to a few per cent in the case of Trappist-1 (Agol et al 2021). This allows an in-depth characterization of moderately insolated rocky planets and mini-Neptune with a precision which is rarely reachable through radial velocities enabling studies of their interiors and atmospheres. The brightness of the current targets of the program (Gaia band mag 11 for TOI178 12 for K2-138 8.4 for TOI1835) allows to combine RVs and photometric measurements. The two methods have a great synergy as TTVs allow for in-depth characte [truncated! Please see actual data for full text]
DOI: 10.57780/esa-kl1tz54
title: 2738913

description:   Target RA (J2000):  189.839218139648  and deg    Target Dec (J2000):  20.0273399353027  and deg    Gaia GMag:  8.172   Programme ID:  CH_PR140080   Programme Manager:  LELEU   PI of observing programme:  Benz   Title of programme:  Axis 1 - Architecture of Resonant Chains (ARC)   Abstract:  Resonant chains are gold mines for fueling our understanding of planetary systems. The minute details of their architectures encode the history of their formation: the order of the capture of the planets in the chain (Delisle 2017) the local shape of the proto-planetary disc and its dispersal (e.g.  Nesvorny et al 2022) and the long-term evolution of the system through tidal dissipation (e.g. Papaloizou et al 2018). The high multiplicity of these systems also makes them especially valuable to constrain our models of the formation of planetary systems (See Emsenhuber et al 2022 and other papers of the NGPPS series) since all the planets have to form in the same environment and the relative fragility of the configuration ensures that no violent evolution (e.g. close encounters/impacts) occurred after the dissipation of the proto-planetary disc (Leleu et al 2021). In addition the transit timing variations induced by the compactness of the systems allow for precise mass determination down to a few per cent in the case of Trappist-1 (Agol et al 2021). This allows an in-depth characterization of moderately insolated rocky planets and mini-Neptune with a precision which is rarely reachable through radial velocities enabling studies of their interiors and atmospheres. The brightness of the current targets of the program (Gaia band mag 11 for TOI178 12 for K2-138 8.4 for TOI1835) allows to combine RVs and photometric measurements. The two methods have a great synergy as TTVs allow for in-depth characte [truncated! Please see actual data for full text]
DOI: 10.57780/esa-kox20lw
title: 2704005

description:   Target RA (J2000):  176.380569458008  and deg    Target Dec (J2000):  65.5409927368164  and deg    Gaia GMag:  8.565   Programme ID:  CH_PR140073   Programme Manager:  LAM   PI of observing programme:  Benz   Title of programme:  Axis 1 - Gas Contents of Low Mass Planets (GCLMP)   Abstract:  The priority questions for planetary sciences are aimed at understanding the origin of planetary systems and life. Planet formation is a complex process that starts with the condensation of matter in a disc of molecular gas and dust. Planetesimals grow into planets accrete material lose volatiles chemically evolve and outgas contract as they cool down and finally are destroyed or survive when the star dies ejecting back material into the interstellar medium and possibly starting again a new cycle. Most of the evidence that we have on these processes comes from the study of our Solar System and astrophysical observations of neighboring stars. The detection and characterization of extrasolar planets revealed a diversity of planetary systems beyond the Solar System but these discoveries challenged existing planet formation theories. Precisely characterized bulk properties of exoplanets help place constraints on the varying formation conditions and evolution processes in order to understand the origin of exoplanets. In this program we propose the characterization of long-period (P > 15 days) low-mass gas-rich planets (defined as planets with radii between 2 and 4 Earth radii) by refining their planetary radii.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-kpewcen
title: 2785982

description:   Target RA (J2000):  218.85612487793  and deg    Target Dec (J2000):  -76.2140808105469  and deg    Gaia GMag:  10.91   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-kpm8ksg
title: 2735624

description:   Target RA (J2000):  142.179244995117  and deg    Target Dec (J2000):  -14.6864204406738  and deg    Gaia GMag:  9.616   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: 10.15468/dl.49fdxr
title: Occurrence Download

description: A dataset containing 634 species occurrences available in GBIF matching the query:
{
 "and" : [
 "TaxonKey is Ipomoea sagittata",
 "Country is Spain",
 "HasCoordinate is true"
 ]
}

 The dataset includes 634 records from 24 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0053371-250920141307145/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.57780/esa-l8xke5y
title: 2740085

description:   Target RA (J2000):  216.924026489258  and deg    Target Dec (J2000):  41.9534187316895  and deg    Gaia GMag:  9.659   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-lf3qfi6
title: 2771496

description:   Target RA (J2000):  311.289703369141  and deg    Target Dec (J2000):  -31.3409004211426  and deg    Gaia GMag:  7.84   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: 10.2908/ei_bsco_m
title: Consumers confidence indicator and survey results - monthly data
title: Verbraucher, Vertrauensindikator und Erhebungsergebnisse - monatliche Daten
title: Consommateurs, indicateur de confiance et résultats d'enquêtes - données mensuelles
DOI: 10.2908/ei_bsfs_q
title: Financial services survey results - quarterly data
title: Finanzdienstleistungen Erhebungsergebnisse - vierteljährliche Daten
title: Services financiers, résultats des enquêtes - données trimestrielles
DOI: 10.57780/esa-lm8glk1
title: 2776585

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: 10.2908/ei_bsin_m_r2
title: Industry confidence indicator and survey results - monthly data
title: Industrie, Vertrauensindikator und Erhebungsergebnisse - monatliche Daten
title: Industrie, indicateur de confiance et résultats d'enquêtes - données mensuelles
DOI: 10.2908/ei_bsse_q_r2
title: Services survey results - quarterly data
title: Dienstleistungen Erhebungsergebnisse - vierteljährliche Daten
title: Services, résultats des enquêtes - données trimestrielles
DOI: 10.57780/esa-lvcfmlg
title: 2776562

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: 10.2908/ei_bsco_q
title: Consumers survey results - quarterly data
title: Verbraucher Erhebungsergebnisse - vierteljährliche Daten
title: Consommateurs, résultats des enquêtes - données trimestrielles
DOI: 10.2908/ei_bsin_q_r2
title: Industry survey results - quarterly data
title: Industrie Industrie Erhebungsergebnisse - vierteljährliche Daten
title: Industrie, résultats des enquêtes - données trimestrielles
DOI: 10.57780/esa-lwaqu61
title: 2689092

description:   Target RA (J2000):  189.839218139648  and deg    Target Dec (J2000):  20.0273399353027  and deg    Gaia GMag:  8.172   Programme ID:  CH_PR140080   Programme Manager:  LELEU   PI of observing programme:  Benz   Title of programme:  Axis 1 - Architecture of Resonant Chains (ARC)   Abstract:  Resonant chains are gold mines for fueling our understanding of planetary systems. The minute details of their architectures encode the history of their formation: the order of the capture of the planets in the chain (Delisle 2017) the local shape of the proto-planetary disc and its dispersal (e.g.  Nesvorny et al 2022) and the long-term evolution of the system through tidal dissipation (e.g. Papaloizou et al 2018). The high multiplicity of these systems also makes them especially valuable to constrain our models of the formation of planetary systems (See Emsenhuber et al 2022 and other papers of the NGPPS series) since all the planets have to form in the same environment and the relative fragility of the configuration ensures that no violent evolution (e.g. close encounters/impacts) occurred after the dissipation of the proto-planetary disc (Leleu et al 2021). In addition the transit timing variations induced by the compactness of the systems allow for precise mass determination down to a few per cent in the case of Trappist-1 (Agol et al 2021). This allows an in-depth characterization of moderately insolated rocky planets and mini-Neptune with a precision which is rarely reachable through radial velocities enabling studies of their interiors and atmospheres. The brightness of the current targets of the program (Gaia band mag 11 for TOI178 12 for K2-138 8.4 for TOI1835) allows to combine RVs and photometric measurements. The two methods have a great synergy as TTVs allow for in-depth characte [truncated! Please see actual data for full text]
DOI: 10.2908/ei_bsbu_q_r2
title: Construction survey results - quarterly data
title: Baugewerbe Erhebungsergebnisse - vierteljährliche Daten
title: Construction, résultats des enquêtes - données trimestrielles
DOI: 10.2908/ei_bslh_m_r2
title: Indikatoren für die Arbeitskräftehortung - monatliche Daten
title: Indicateurs de rétention de main-d’œuvre - données mensuelles
title: Labour hoarding indicators - monthly data

description: La rétention de main-d’œuvre est définie comme «la partie de la main-d’œuvre qui n’est pas pleinement utilisée par une entreprise au cours de son processus de production à un moment donné», ce qui implique une sous-utilisation de la main-d’œuvre. Elle se produit généralement en période de sous-utilisation ou de ralentissement de l’activité économique. La raison pour laquelle les entreprises ne licencient pas de salariés pendant de telles périodes est que 1) le licenciement de travailleurs entraîne généralement des coûts et 2) le recrutement de travailleurs une fois l’activité économique rétablie entraîne également des coûts.
description: Das Horten von Arbeitskräften ist definiert als „der Teil des Arbeitseinsatzes, der von einem Unternehmen während seines Produktionsprozesses zu keinem Zeitpunkt vollständig genutzt wird“, was eine Unterauslastung der Arbeitskräfte bedeutet. Sie tritt in der Regel in Zeiten der Unterauslastung oder des Abschwungs der Wirtschaftstätigkeit auf. Der Grund dafür, dass Unternehmen ihre Beschäftigten in solchen Zeiträumen nicht entlassen, liegt darin, dass 1) die Entlassung von Arbeitnehmern in der Regel mit Kosten verbunden ist und 2) die Einstellung von Arbeitskräften, sobald sich die wirtschaftliche Tätigkeit erholt, auch Kosten verursacht.
description: Labour hoarding is defined as “that part of labour input which is not fully utilised by a company during its production process at any given time”, implying under-utilisation of the workforce. It typically occurs in periods of slack or downturn of economic activity. The rationale for companies not to lay off employees in such periods is that 1) dismissing workers usually involves costs, and 2) recruiting workers once economic activity recovers also entails costs.
DOI: 10.57780/esa-m5bjl6p
title: 2838356

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-mal0f3m
title: 2786037

description:   Target RA (J2000):  297.922973632812  and deg    Target Dec (J2000):  2.51950001716614  and deg    Gaia GMag:  10.92   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: 10.2908/ei_bsse_m_r2
title: Services confidence indicator and survey results - monthly data
title: Dienstleistungen, Vertrauensindikator und Erhebungsergebnisse - monatliche Daten
title: Services, indicateur de confiance et résultats d'enquêtes - données mensuelles
DOI: 10.57780/esa-mbb8wvo
title: 2684666

description:   Target RA (J2000):  98.3511123657227  and deg    Target Dec (J2000):  -23.4861907958984  and deg    Gaia GMag:  10.142   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]