cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-c7x54y4
title: 2731383

description:   Target RA (J2000):  154.90837097168  and deg    Target Dec (J2000):  -9.8062801361084  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: 10.17898/adp_novep23_v1/1
title: novep23_om1_sl_v1_r0.pdf

description: :unav
DOI: 10.57780/esa-ccwhol8
title: 2787801

description:   Target RA (J2000):  207.526168823242  and deg    Target Dec (J2000):  -40.8358001708984  and deg    Gaia GMag:  9.61   Programme ID:  CH_PR240004   PI of observing programme:  Ekaterina ilin   Title of programme:  HIP 67522 b - a Hot Jupiter that triggers flares on its host   Abstract:  The habitability of exoplanets depends crucially on the space weather they experience. A planet orbiting _inwards_ of the habitable zone is a natural probe of the magnetized winds and energetic radiation traveling towards a potentially habitable planet. When a planet orbits close enough to its host it can perturb the stars magnetic field setting off energetic flares in the stellar corona. In the optical these flares appear as recurrent brightenings in phase with the orbit. If we measure such flares we immediately know that the planet moves inside the closed-field corona critical information for space weather modelers. To measure this planet-induced flaring we have to find flares occurring in excess of intrinsic stellar flaring. This is done by testing for deviations from a random distribution of flares with the orbital phase of the planet. HIP 67522 a 17 Myr Sun with a Hot Jupiter in a 7-day orbit detected in 2020 has the ideal properties to exhibit such excess flares. But there is more: In recent TESS data HIP 67522 flared a total of four times. Each time the flare took place within 10h after transit the same 4% of the planets orbit. This is very unlikely to happen if these flares occurred randomly. We propose to observe HIP 67522 using CHEOPS high sensitivity for flares for 16 visits for 8 orbits each during the critical 4% of HIP 67522 bs orbit to measure for the first time planet induced flares at high significance.    [truncated! Please see actual data for full text]
DOI: 10.17898/adp_novep23_v1/2
title: novep23_p12_sl_v1_r1.pdf

description: :unav
DOI: 10.57780/esa-cmqelp4
title: 2771626

description:   Target RA (J2000):  261.243927001953  and deg    Target Dec (J2000):  32.7981109619141  and deg    Gaia GMag:  11.63   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: 10.17898/adp_novep23_v1/3
title: novep23_rm1_sl_v1_r1.tab

description: :unav
DOI: 10.57780/esa-criunst
title: 2753517

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-crs4l52
title: 2732520

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: 10.17898/adp_novep23_v1/4
title: novep23_vp1_sl_v1_r1.pdf

description: :unav
DOI: 10.57780/esa-cwek7te
title: 2848071

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: 10.17898/adp_novep23_v1/5
title: novep23_vp2_sl_v1_r1.pdf

description: :unav
DOI: 10.57780/esa-d00715k
title: 2701420

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-d63vlrj
title: 2724320

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: 10.17898/adp_novep23_v1/6
title: novep23_vp3_sl_v1_r1.pdf

description: :unav
DOI: 10.57780/esa-d7y2l9p
title: 2815135

description:   Target RA (J2000):  319.699584960938  and deg    Target Dec (J2000):  -26.6163692474365  and deg    Gaia GMag:  8.227   Programme ID:  CH_PR149002   Programme Manager:  EDWARDS   PI of observing programme:  Benz   Title of programme:  SoM - ArielExoClock   Abstract:  To uncover the demographics of exoplanet atmospheres Ariel will require a large diverse list of potential targets. Luckily ground-based and space-based surveys have detected hundreds of transiting planets around bright stars. However simply knowing of the planets existence is not enough and preliminary characterisation efforts must be undertaken to ensure the suitability of the target for study. A key piece of information is an accurate knowledge of the predicted transit time of a planet. In this programme CHEOPS observations will be used to support the Ariel mission by maintaining the ephemeris of critical targets.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-d8fseti
title: 2822323

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: 10.17898/adp_novep23_v1
title: Novinarstvo v ekonomiji pozornosti, 2023

description: Novinarstvo kot poklic in način ustvarjanja znanja se močno spreminja, predvsem pod vplivom komunikacijske tehnologije. Zaradi širših družbenih in zgodovinskih sprememb je ključnega pomena, da podrobno preučimo nove tehnološke pripomočke, družbene trende in poklicne smernice v novinarstvu. To ni pomembno le za prihodnost novinarstva, ampak tudi za javno sfero, ki temelji na kakovostnih informacijah. Raziskava se ukvarja z vprašanjem, kako digitalna komunikacija vpliva na slovensko novinarstvo v kontekstu globalne ekonomije pozornosti in spreminjajoče se javne sfere. Raziskava zajema štiri glavna vprašanja: (1) Spremembe v delovnih procesih: Kako te spremembe vplivajo na naravo novinarskega dela, poklicni status novinarjev, njihove spretnosti, delitev dela v redakcijah ter stopnjo njihove avtonomije v odnosu do vodstva? (2) Ekonomija pozornosti in poslovni modeli: Kako oglaševanje in trženje vplivata na poslovne modele medijev in hkrati prispevata k deprofesionalizaciji novinarstva zaradi preobilja informacij ter omejene in razdrobljene pozornosti? (3) Vpliv tehnoloških podjetij: Ali finančna podpora tehnoloških podjetij krepi povezavo med novinarji in skupnostmi ali ogroža novinarske prakse, avtonomijo in ugled? (4) Vpliv politike in regulacije: Kako politični ukrepi in delovanje državnih institucij vplivajo na zmožnost novinarstva, da opravlja svojo vlogo varuha javnega interesa? Pri raziskavi so sodelovali predstavniki medijskih agencij, medijskih in oglaševalskih združenj, medijski menedžerji in tržni analitiki.
DOI: 10.17898/adp_novep23_v1/7
title: novep23_vp4_sl_v1_r1.pdf

description: :unav
DOI: 10.57780/esa-dda26d7
title: 2794122

description:   Target RA (J2000):  286.041046142578  and deg    Target Dec (J2000):  36.6326217651367  and deg    Gaia GMag:  11.552   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: 10.57780/esa-dnzpqss
title: 2753651

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-dvrxiqg
title: 2833008

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-e33pq16
title: 2712527

description:   Target RA (J2000):  229.838119506836  and deg    Target Dec (J2000):  29.206169128418  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]