cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-guzbh4v
title: 2569967

description:   Target RA (J2000):  68.593750  and deg    Target Dec (J2000):  43.03742  and deg    Gaia GMag:  12.3    Programme ID:  CH_PR140068   Programme Manager:  EGGER   PI of observing programme:  Benz   Title of programme:  Axis 1 - Constraining the abundance of water in hot planets (HotWatermelon)   Abstract:  Planets located close enough to their star experience evaporation which leads to a dichotomy in the possible gas content of these objects. These planets either contain more than around one percent of gas (in mass) or no gas at all (see Owen and Wu 2017). This dichotomy when expressed in term of mass-radius relation implies the existence of a region in the mass-radius diagram of hot planets where dry planets cannot exist. We propose to observe planets that could lie in this region with CHEOPS. Combining a precise radius and mass will allow us to identify planets in this forbidden region hence showing that they have to contain volatiles most likely water. Our data combined with future JWST observations will also constrain the efficiency of evaporation.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-gvcayc6
title: 2450900

description:   Target RA (J2000):  197.317459  and deg    Target Dec (J2000):  -60.30836  and deg    Gaia GMag:  8.09    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-h07ru85
title: 2415406

description:   Target RA (J2000):  197.317459  and deg    Target Dec (J2000):  -60.30836  and deg    Gaia GMag:  8.09    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-h1w9zll
title: 2517205

description:   Target RA (J2000):  308.538666  and deg    Target Dec (J2000):  -29.67211  and deg    Gaia GMag:  9.77    Programme ID:  CH_PR140068   Programme Manager:  EGGER   PI of observing programme:  Benz   Title of programme:  Axis 1 - Constraining the abundance of water in hot planets (HotWatermelon)   Abstract:  Planets located close enough to their star experience evaporation which leads to a dichotomy in the possible gas content of these objects. These planets either contain more than around one percent of gas (in mass) or no gas at all (see Owen and Wu 2017). This dichotomy when expressed in term of mass-radius relation implies the existence of a region in the mass-radius diagram of hot planets where dry planets cannot exist. We propose to observe planets that could lie in this region with CHEOPS. Combining a precise radius and mass will allow us to identify planets in this forbidden region hence showing that they have to contain volatiles most likely water. Our data combined with future JWST observations will also constrain the efficiency of evaporation.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-h3z8pft
title: 2402943

description:   Target RA (J2000):  207.526169  and deg    Target Dec (J2000):  -40.83580  and deg    Gaia GMag:  9.615    Programme ID:  CH_PR240017   PI of observing programme:  Chakraborty   Title of programme:  Accurate and precise characterisation of the HIP 67522 system in the presence of significant stellar variability   Abstract:  Young planets are excellent laboratories to test planet formation and evolution pathways. However the accurate characterisation of parameters like the radius of the planet is limited by the enhanced activity of the host star. The impact of features like unocculted and occulted active regions is a growing challenge in the era of high-precision photometry and transmission spectroscopy and better characterisation of these features is now more vital than ever for the correct interpretation of atmospheres on exoplanets. Here we propose to precisely characterise the HIP 67522 system a 17 Myr Solar-like star exhibiting significant stellar activity and one of the youngest planet-hosting stars discovered to date. The HIP 67522 system consists of one confirmed transiting hot Jupiter (planet b) and an unconfirmed outer planet candidate (planet c). To characterise this key young system we aim to: i) obtain an accurate and precise radius measurement for the known transiting planet (planet b) by quantifying the effect of stellar activity on its transit depth and ii) confirm the candidate exoplanet (planet c) by following up the most likely period aliases of its two known transits. While accurately measuring the radius of planet b is vital for testing different planet formation and evolution models for hot Jupiters confirming planet c will make this the youngest multi-planet transiting system ever discovered making this a very compelling system to be observed by CHEOPS.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-haiuzie
title: 2370611

description:   Target RA (J2000):  207.526169  and deg    Target Dec (J2000):  -40.83580  and deg    Gaia GMag:  9.61    Programme ID:  CH_PR240004   PI of observing programme:  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 star’s 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 planet’s 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-hckoo1p
title: 2446625

description:   Target RA (J2000):  313.691254  and deg    Target Dec (J2000):  -72.80463  and deg    Gaia GMag:  11.806    Programme ID:  CH_PR240009   PI of observing programme:  Garai   Title of programme:  Refining parameters of grazing transiting exoplanets with CHEOPS and TESS   Abstract:  Grazing transiting exoplanets still constitute only a tiny fraction of the known exoplanet population. However confirming/investigating grazing transiting exoplanets is also important. In a grazing transit the second and third contact points are missing the transit profile is V-shaped similar to that of an eclipsing binary. Consequently the light-curve solution is degenerate. Fortunately there is a solution: we need very high-quality multicolour photometric observations. Following this possibility we propose to utilise the colour difference between TESS and CHEOPS in order to refine the parameters and to confirm the grazing nature of selected transiting exoplanets namely TOI-3540 b and TOI-2193 b.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-hcpftu9
title: 2413432

description:   Target RA (J2000):  217.609116  and deg    Target Dec (J2000):  -46.15920  and deg    Gaia GMag:  11.75    Programme ID:  CH_PR140066   Programme Manager:  NASCIMBENI   PI of observing programme:  Benz   Title of programme:  Axis 1 - Uncovering a maverick population: CHEOPS observations of hot Jupiter systems with inner small companions (MAVERICK)   Abstract:  Planetary systems hosting a hot or warm Jupiter (HJ/WJ) plus nearby small companion(s) such as WASP-47 (Nascimbeni et al. 2023) are extremely rare and very valuable to constrain formation and migration models. Only five such systems are known so far. Our goal is to increase the sample size by confirming and characterizing five TESS candidates with such an architecture and improving their orbital/physical parameters including ephemeris radii and (when feasible) planetary masses through TTVs. As demonstrated by our work on WASP-47 RVs and TTVs are very synergistic at decoding these complex systems. A dedicated RV follow-up will be coordinated.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-hddw17c
title: 2547795

description:   Target RA (J2000):  348.949036  and deg    Target Dec (J2000):  -10.84969  and deg    Gaia GMag:  12    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 characterization of  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-he2wnk9
title: 2514755

description:   Target RA (J2000):  344.622711  and deg    Target Dec (J2000):  -44.71686  and deg    Gaia GMag:  10.76    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-hftdbrs
title: 2509921

description:   Target RA (J2000):  294.661407  and deg    Target Dec (J2000):  31.21920  and deg    Gaia GMag:  7.575    Programme ID:  CH_PR140061   Programme Manager:  LENDL   PI of observing programme:  Benz   Title of programme:  Axis 2 - A Deep search for hot JupIter VAriability (DIVA)   Abstract:  The temporal stability of hot Jupiter atmospheres remains an open question. While there are several tentative detections of changes in the observed planetary occultation depths phase curve shapes or transmission spectra no indisputable evidence exists to date. This program will perform a deep search for variability in the dayside brightness of several hot Jupiters. A detection of clear variability and the measurement of its timescale would open the door to a suite of follow-up studies involving the dynamical behaviour of exoplanet atmospheres.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-hftmean
title: 2578594

description:   Target RA (J2000):  42.984364  and deg    Target Dec (J2000):  -30.81453  and deg    Gaia GMag:  6.25    Programme ID:  CH_PR140067   Programme Manager:  ALIBERT   PI of observing programme:  Benz   Title of programme:  Axis 1 - Probing the architecture-composition-metallicity link (ArchiCHESS)   Abstract:  Planet formation models predict the existence of a link between the orbital architecture of a planetary system the composition of its planets and the metallicity of the central star. This correlation results from the following two processes: On one hand the temporal evolution of the gas content of the protoplanetary disk causes migration of the planets and therefore determines the orbital architecture of the system. On the other hand the composition of the planets depends on the structure and composition of the disk of solids itself related to the gas content of the disk and the solid-to-gas ratio in the disk. This latter quantity is finally correlated with the stellar metallicity. The goal of ArchiCHESS is to observe multi-planetary systems to constrain their architecture (using architecture coefficients of Mishra et al. 2023) and relate this to the water fractions of the planets as well as to the metallicity of the central star.    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-hgubnvh
title: 2591586

description:   Target RA (J2000):  76.649544  and deg    Target Dec (J2000):  -20.24559  and deg    Gaia GMag:  11.63    Programme ID:  CH_PR250026   PI of observing programme:  Chakraborty   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-hhbs36r
title: 2415025

description:   Target RA (J2000):  247.623413  and deg    Target Dec (J2000):  38.34731  and deg    Gaia GMag:  8.027    Programme ID:  CH_PR149004   Programme Manager:  WILSON   PI of observing programme:  Benz   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-hj4yx0h
title: 2372690

description:   Target RA (J2000):  129.572037  and deg    Target Dec (J2000):  -23.55022  and deg    Gaia GMag:  10.74    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: 10.6084/m9.figshare.c.3823168_d1.v1
title: Additional file 1: Dataset S1. of PAT-H-MS coupled with laser microdissection to study histone post-translational modifications in selected cell populations from pathology samples

description: Dataset containing the measured AUCs for the glioblastoma xenografts and mouse brain samples shown in Fig.Â 2. (XLSX 33 kb)
DOI: 10.57780/esa-hjm83cw
title: 2555762

description:   Target RA (J2000):  343.319733  and deg    Target Dec (J2000):  -14.26370  and deg    Gaia GMag:  8.88    Programme ID:  CH_PR250004   PI of observing programme:  Poyatos   Title of programme:  Not known   Abstract:  Not known    [truncated! Please see actual data for full text]
DOI: 10.57780/esa-hn8ddoh
title: 2517888

description:   Target RA (J2000):  292.579865  and deg    Target Dec (J2000):  37.37639  and deg    Gaia GMag:  15.67    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-hnr8u4r
title: 2517096

description:   Target RA (J2000):  348.949036  and deg    Target Dec (J2000):  -10.84969  and deg    Gaia GMag:  12    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 characterization of  [truncated! Please see actual data for full text]