cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-7lp329t
title: 2833759

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-7n4k4mi
title: 2748045

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-7p3hadv
title: 2757865

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: 10.57780/esa-7pzkqcv
title: 2658667

description:   Target RA (J2000):  108.123123168945  and deg    Target Dec (J2000):  -24.9535598754883  and deg    Gaia GMag:  9.602   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-7xihj11
title: 2789721

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_vzgl03_v1/1
title: vzgl03_p1_sl_v1_r3.tab

description: :unav
DOI: 10.17898/adp_vzgl03_v1/2
title: vzgl03_vp1_sl_v1_r1.pdf

description: :unav
DOI: 10.57780/esa-7zeg28l
title: 2787247

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_vzgl03_v1
title: Vsakdanje življenje gejev in lezbijk, 2003

description: Prva sociološka raziskava o vsakdanjem življenju gejev in lezbijk je nastala v okviru ciljno-raziskovalnega projekta »Družinski in socialni konteksti življenja istospolno usmerjenih v Sloveniji« (2002–2004). Namen raziskave je bil pridobiti prve sistematične podatke o vsakdanjem življenju gejev in lezbijk, ki predstavljajo raziskovalno težko dostopno oz. skrito socialno manjšino. Cilj je bil ugotoviti, kakšne so socio-demografske značilnosti te populacije ter s katerimi problemi se v vsakdanjem življenju srečujejo zaradi svoje spolne usmerjenosti. Raziskovanje temelji na ugotovitvah iz tujih raziskav ter teoretskih izhodišč tako s področja sociologije, LGBT študij kot tudi študij spolov in seksualnosti. Pri tem so bili raziskovalci pozorni tudi na širše družbene okoliščine in značilnosti poznomodernih zahodnih družb (kot so refleksivni individualizem, preobrazba intimnosti, spremembe na področju družinskega življenja ter starševstva), ter hkrati posebnosti populacije istospolno usmerjenih zaradi umeščenosti v heteronormativni družbeni kontekst (socialna izključenost, diskriminacija, nasilje ipd.). Raziskava je zajela različne teme, ki so bile identificirane kot ključne v vsakdanjem življenju gejev in lezbijk (razkritje v različnih socialnih okoljih, kot so prijateljske mreže, starši oz. družina, šolsko okolje, delovno okolje, javni prostori ipd., izkušnje nasilja zaradi spolne usmerjenosti, intimna partnerstva, družine ipd.). Raziskava je bila izvedena s kombinacijo kvantitativnega (anketa) in kvalitativnega raziskovanja (fokusne skupine). V ADP hranimo le anketne podatke.
DOI: 10.57780/esa-8rxzyxc
title: 2748047

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-90r5k35
title: 2806062

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-94aiy1q
title: 2861346

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-95l8swu
title: 2714759

description:   Target RA (J2000):  184.96696472168  and deg    Target Dec (J2000):  55.165641784668  and deg    Gaia GMag:  11.65   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-96q3l6r
title: 2755315

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-9arxew9
title: 2672710

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: 10.57780/esa-9c1mhtv
title: 2763520

description:   Target RA (J2000):  183.705001831055  and deg    Target Dec (J2000):  -63.0866088867188  and deg    Gaia GMag:  10.67   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-9r5n0tk
title: 2652665

description:   Target RA (J2000):  125.188789367676  and deg    Target Dec (J2000):  46.2037200927734  and deg    Gaia GMag:  11.327   Programme ID:  CH_PR140085   Programme Manager:  VENTURINI   PI of observing programme:  Benz   Title of programme:  Axis 1 - Towards an S-type radius valley determination (S-valley)   Abstract:  The number of planets orbiting binary stars has notably increased in the past three years thanks to follow-up of Tess Objects of Interest by direct imaging and GAIA. The demographic properties of planets in binaries are only starting to be unveiled. An important question to address for planets around binaries is that of the radius valley a deficit of exoplanets with 1.5 to 2.0 Earth radii found for planets orbiting single stars. A recent study by Sullivan et al. 2023 reports that no radius valley exists for S-type planets (planets in binaries orbiting only one of the stellar components).  The study was performed with a sample of Kepler planets which suffers from large errors in the planetary radii. In addition the planets were assumed to orbit the primary star which adds an additional (and large) source of error in case a planet orbits in reality the secondary star. With this program we re-address the radius valley question by combining past observational data with new measurements from CHEOPS.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-9tgdp9t
title: 2842156

description:   Target RA (J2000):  0.32574999332428  and deg    Target Dec (J2000):  -8.92628955841064  and deg    Gaia GMag:  9.82   Programme ID:  CH_PR149001   Programme Manager:  BRUNO   PI of observing programme:  Benz   Title of programme:  SoM - ArielGranulation   Abstract:  This is a pilot study to characterise stellar granulation in a representative subset of the Ariel Reference Sample. Sulis et al. (2023) showed that granulation has a strong chromatic effect and is able to significantly contaminate observations in the visible channels of the Ariel telescope.  Results from CHEOPS photometry will be combined with the spectroscopic information collected by the Ariel Stellar Characterisation working group in order to provide a more detailed picture of stellar granulation in the observed targets constraints to optimise Ariel observing time and input for the development of modelling and data analysis techniques.    [truncated! Please see actual data for full text]