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class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.07887">arXiv:2502.07887</a> <span> [<a href="https://arxiv.org/pdf/2502.07887">pdf</a>, <a href="https://arxiv.org/format/2502.07887">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Searching for Hot Water World Candidates with CHEOPS: Refining the radii and analysing the internal structures and atmospheric lifetimes of TOI-238 b and TOI-1685 b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Kubyshkina%2C+D">D. Kubyshkina</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Kitzmann%2C+D">D. Kitzmann</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Mordasini%2C+C">C. Mordasini</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/?searchtype=author&query=Pezzotti%2C+C">C. Pezzotti</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Ulmer-Moll%2C+S">S. Ulmer-Moll</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C">S. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.07887v1-abstract-short" style="display: inline;"> Studying the composition of exoplanets is one of the most promising approaches to observationally constrain planet formation and evolution processes. However, this endeavour is complicated for small exoplanets by the fact that a wide range of compositions is compatible with their bulk properties. To overcome this issue, we identify triangular regions in the mass-radius space where part of this deg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07887v1-abstract-full').style.display = 'inline'; document.getElementById('2502.07887v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.07887v1-abstract-full" style="display: none;"> Studying the composition of exoplanets is one of the most promising approaches to observationally constrain planet formation and evolution processes. However, this endeavour is complicated for small exoplanets by the fact that a wide range of compositions is compatible with their bulk properties. To overcome this issue, we identify triangular regions in the mass-radius space where part of this degeneracy is lifted for close-in planets, since low-mass H/He envelopes would not be stable due to high-energy stellar irradiation. Planets in these Hot Water World triangles need to contain at least some heavier volatiles and are therefore interesting targets for atmospheric follow-up observations. We perform a demographic study to show that only few well-characterised planets in these regions are currently known and introduce our CHEOPS GTO programme aimed at identifying more of these potential hot water worlds. Here, we present CHEOPS observations for the first two targets of our programme, TOI-238 b and TOI-1685 b. Combined with TESS photometry and published RVs, we use the precise radii and masses of both planets to study their location relative to the corresponding Hot Water World triangles, perform an interior structure analysis and study the lifetimes of H/He and water-dominated atmospheres under these conditions. We find that TOI-238 b lies, at the 1-sigma level, inside the corresponding triangle. While a pure H/He atmosphere would have evaporated after 0.4-1.3 Myr, it is likely that a water-dominated atmosphere would have survived until the current age of the system, which makes TOI-238 b a promising hot water world candidate. Conversely, TOI-1685 b lies below the mass-radius model for a pure silicate planet, meaning that even though a water-dominated atmosphere would be compatible both with our internal structure and evaporation analysis, we cannot rule out the planet to be a bare core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07887v1-abstract-full').style.display = 'none'; document.getElementById('2502.07887v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 16 figures, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.13575">arXiv:2501.13575</a> <span> [<a href="https://arxiv.org/pdf/2501.13575">pdf</a>, <a href="https://arxiv.org/format/2501.13575">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Transit-timing variations in the AU Mic system observed with CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Boldog%2C+%C3%81">脕. Boldog</a>, <a href="/search/?searchtype=author&query=Szab%C3%B3%2C+G+M">Gy. M. Szab贸</a>, <a href="/search/?searchtype=author&query=Kriskovics%2C+L">L. Kriskovics</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Garai%2C+Z">Z. Garai</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Correia%2C+A+C+M">A. C. M. Correia</a>, <a href="/search/?searchtype=author&query=Csizmadia%2C+S">Sz. Csizmadia</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">P. E. Cubillos</a>, <a href="/search/?searchtype=author&query=Davies%2C+M+B">M. B. Davies</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.13575v1-abstract-short" style="display: inline;"> AU Mic is a very active M dwarf with an edge-on debris disk and two transiting sub-Neptunes with a possible third planetary companion. The two transiting planets exhibit significant transit-timing variations (TTVs) that are caused by the gravitational interaction between the bodies in the system. Using photometrical observations taken with the CHaracterizing ExOPlanet Satellite (CHEOPS), our goal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.13575v1-abstract-full').style.display = 'inline'; document.getElementById('2501.13575v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.13575v1-abstract-full" style="display: none;"> AU Mic is a very active M dwarf with an edge-on debris disk and two transiting sub-Neptunes with a possible third planetary companion. The two transiting planets exhibit significant transit-timing variations (TTVs) that are caused by the gravitational interaction between the bodies in the system. Using photometrical observations taken with the CHaracterizing ExOPlanet Satellite (CHEOPS), our goal is to constrain the planetary radii, the orbital distances and periods of AU Mic b and c. We aim to determine the superperiod of the TTVs for AU Mic b and to update the transit ephemeris for both planets. Based on the observed TTVs, we study the possible presence of a third planet in the system. We conducted high precision photometric observations with CHEOPS in 2022 and 2023. We used Allesfitter to fit the planetary transits and to constrain the planetary and orbital parameters. We combined our new measurements with results from previous years to determine the periods and amplitudes of the TTVs. We applied dynamical modelling based on TTV measurements from the 2018-2023 period to reconstruct the perceived variations. The orbital distances and periods for AU Mic b and c agree with the results from previous works. However, the values for the planetary radii deviate slightly from previous values, which we attribute to the effect of stellar spots. AU Mic c showed very strong TTVs, with transits that occurred ~80 minutes later in 2023 than in 2021. Through dynamical analysis of the system, we found that the observed TTVs can be explained by a third planet with an orbital period of ~12.6 days and a mass of 0.203+0.022-0.024 M_E. We explored the orbital geometry of the system and found that AU Mic c has a misaligned retrograde orbit. Due limited number of observations the exact configuration and planetary parameters could not be determined. Further monitoring with CHEOPS may improve these results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.13575v1-abstract-full').style.display = 'none'; document.getElementById('2501.13575v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.08557">arXiv:2412.08557</a> <span> [<a href="https://arxiv.org/pdf/2412.08557">pdf</a>, <a href="https://arxiv.org/format/2412.08557">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202452151">10.1051/0004-6361/202452151 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CHEOPS observations confirm nodal precession in the WASP-33 system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/?searchtype=author&query=Csizmadia%2C+S">Sz. Csizmadia</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Harre%2C+J+-">J. -V. Harre</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Kalman%2C+S">Sz. Kalman</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Szab%C3%B3%2C+G+M">Gy. M. Szab贸</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.08557v1-abstract-short" style="display: inline;"> Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $未$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08557v1-abstract-full').style.display = 'inline'; document.getElementById('2412.08557v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.08557v1-abstract-full" style="display: none;"> Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $未$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the stellar pulsations from the light curves, as well as the usual CHEOPS systematic effects. We also performed a comprehensive analysis of low-resolution spectral and Gaia data to re-determine the stellar properties of WASP-33. Results: We measure an orbital obliquity 111.3 +0.2 -0.7 degrees, which is consistent with previous measurements made via Doppler tomography. We also measure the planetary impact parameter, and confirm that this parameter is undergoing rapid secular evolution as a result of nodal precession of the planetary orbit. This precession allows us to determine the second-order fluid Love number of the star, which we find agrees well with the predictions of theoretical stellar models. We are unable to robustly measure a unique value of the occultation depth, and emphasise the need for long-baseline observations to better measure the pulsation periods. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08557v1-abstract-full').style.display = 'none'; document.getElementById('2412.08557v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 12 figures. Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 2025 693 A128 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.05423">arXiv:2412.05423</a> <span> [<a href="https://arxiv.org/pdf/2412.05423">pdf</a>, <a href="https://arxiv.org/format/2412.05423">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> A joint effort to discover and characterize two resonant mini Neptunes around TOI-1803 with TESS, HARPS-N and CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Turrini%2C+D">D. Turrini</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Polychroni%2C+D">D. Polychroni</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Naponiello%2C+L">L. Naponiello</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a> , et al. (108 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.05423v1-abstract-short" style="display: inline;"> We present the discovery of two mini Neptunes near a 2:1 orbital resonance configuration orbiting the K0 star TOI-1803. We describe their orbital architecture in detail and suggest some possible formation and evolution scenarios. Using CHEOPS, TESS, and HARPS-N datasets we can estimate the radius and the mass of both planets. We used a multidimensional Gaussian Process with a quasi-periodic kernel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05423v1-abstract-full').style.display = 'inline'; document.getElementById('2412.05423v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.05423v1-abstract-full" style="display: none;"> We present the discovery of two mini Neptunes near a 2:1 orbital resonance configuration orbiting the K0 star TOI-1803. We describe their orbital architecture in detail and suggest some possible formation and evolution scenarios. Using CHEOPS, TESS, and HARPS-N datasets we can estimate the radius and the mass of both planets. We used a multidimensional Gaussian Process with a quasi-periodic kernel to disentangle the planetary components from the stellar activity in the HARPS-N dataset. We performed dynamical modeling to explain the orbital configuration and performed planetary formation and evolution simulations. For the least dense planet, we define possible atmospheric characterization scenarios with simulated JWST observations. TOI-1803 b and TOI-1803 c have orbital periods of $\sim$6.3 and $\sim$12.9 days, respectively, residing in close proximity to a 2:1 orbital resonance. Ground-based photometric follow-up observations revealed significant transit timing variations (TTV) with an amplitude of $\sim$10 min and $\sim$40 min, respectively, for planet -b and -c. With the masses computed from the radial velocities data set, we obtained a density of (0.39$\pm$0.10) $蟻_{earth}$ and (0.076$\pm$0.038) $蟻_{earth}$ for planet -b and -c, respectively. TOI-1803 c is among the least dense mini Neptunes currently known, and due to its inflated atmosphere, it is a suitable target for transmission spectroscopy with JWST. We report the discovery of two mini Neptunes close to a 2:1 orbital resonance. The detection of significant TTVs from ground-based photometry opens scenarios for a more precise mass determination. TOI-1803 c is one of the least dense mini Neptune known so far, and it is of great interest among the scientific community since it could constrain our formation scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05423v1-abstract-full').style.display = 'none'; document.getElementById('2412.05423v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 Pages, 21 Figures Accepted for Publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.18326">arXiv:2411.18326</a> <span> [<a href="https://arxiv.org/pdf/2411.18326">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.jsse.2024.08.005">10.1016/j.jsse.2024.08.005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-situ observations of resident space objects with the CHEOPS space telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Billot%2C+N">Nicolas Billot</a>, <a href="/search/?searchtype=author&query=Hellmich%2C+S">Stephan Hellmich</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">Willy Benz</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">Andrea Fortier</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">David Ehrenreich</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">Christopher Broeg</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">Alexis Heitzmann</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">Anja Bekkelien</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">Alexis Brandeker</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Yann Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">Roi Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">Tamas B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">David Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">Susana C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">Wolfgang Baumjohann</a>, <a href="/search/?searchtype=author&query=Biondi%2C+F">Federico Biondi</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">Luca Borsato</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">Andrew Collier Cameron</a>, <a href="/search/?searchtype=author&query=van+Damme%2C+C+C">Carlos Corral van Damme</a>, <a href="/search/?searchtype=author&query=Correia%2C+A+C+M">Alexandre C. M. Correia</a>, <a href="/search/?searchtype=author&query=Csizmadia%2C+S">Szilard Csizmadia</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">Patricio E. Cubillos</a>, <a href="/search/?searchtype=author&query=Davies%2C+M+B">Melvyn B. Davies</a>, <a href="/search/?searchtype=author&query=Deleuil%2C+M">Magali Deleuil</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">Adrien Deline</a> , et al. (58 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.18326v1-abstract-short" style="display: inline;"> The CHaracterising ExOPlanet Satellite (CHEOPS) is a partnership between the European Space Agency and Switzerland with important contributions by 10 additional ESA member States. It is the first S-class mission in the ESA Science Programme. CHEOPS has been flying on a Sun-synchronous low Earth orbit since December 2019, collecting millions of short-exposure images in the visible domain to study e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.18326v1-abstract-full').style.display = 'inline'; document.getElementById('2411.18326v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.18326v1-abstract-full" style="display: none;"> The CHaracterising ExOPlanet Satellite (CHEOPS) is a partnership between the European Space Agency and Switzerland with important contributions by 10 additional ESA member States. It is the first S-class mission in the ESA Science Programme. CHEOPS has been flying on a Sun-synchronous low Earth orbit since December 2019, collecting millions of short-exposure images in the visible domain to study exoplanet properties. A small yet increasing fraction of CHEOPS images show linear trails caused by resident space objects crossing the instrument field of view. To characterize the population of satellites and orbital debris observed by CHEOPS, all and every science images acquired over the past 3 years have been scanned with a Hough transform algorithm to identify the characteristic linear features that these objects cause on the images. Thousands of trails have been detected. This statistically significant sample shows interesting trends and features such as an increased occurrence rate over the past years as well as the fingerprint of the Starlink constellation. The cross-matching of individual trails with catalogued objects is underway as we aim to measure their distance at the time of observation and deduce the apparent magnitude of the detected objects. As space agencies and private companies are developing new space-based surveillance and tracking activities to catalogue and characterize the distribution of small debris, the CHEOPS experience is timely and relevant. With the first CHEOPS mission extension currently running until the end of 2026, and a possible second extension until the end of 2029, the longer time coverage will make our dataset even more valuable to the community, especially for characterizing objects with recurrent crossings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.18326v1-abstract-full').style.display = 'none'; document.getElementById('2411.18326v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 8 figures, Special Issue of the Journal of Space Safety Engineering</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Space Safety Engineering, Volume 11, Issue 3, September 2024, Pages 498-506 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.16958">arXiv:2411.16958</a> <span> [<a href="https://arxiv.org/pdf/2411.16958">pdf</a>, <a href="https://arxiv.org/format/2411.16958">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae2655">10.1093/mnras/stae2655 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A possible misaligned orbit for the young planet AU Mic c </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Yu%2C+H">H. Yu</a>, <a href="/search/?searchtype=author&query=Garai%2C+Z">Z. Garai</a>, <a href="/search/?searchtype=author&query=Cretignier%2C+M">M. Cretignier</a>, <a href="/search/?searchtype=author&query=Szab%C3%B3%2C+G+M">Gy. M. Szab贸</a>, <a href="/search/?searchtype=author&query=Aigrain%2C+S">S. Aigrain</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Bryant%2C+E+M">E. M. Bryant</a>, <a href="/search/?searchtype=author&query=Correia%2C+A+C+M">A. C. M. Correia</a>, <a href="/search/?searchtype=author&query=Klein%2C+B">B. Klein</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Owen%2C+J+E">J. E. Owen</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Winn%2C+J+N">J. N. Winn</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Cegla%2C+H+M">H. M. Cegla</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Gill%2C+S">S. Gill</a>, <a href="/search/?searchtype=author&query=Kriskovics%2C+L">L. Kriskovics</a>, <a href="/search/?searchtype=author&query=Barrag%C3%A1n%2C+O">O. Barrag谩n</a>, <a href="/search/?searchtype=author&query=Boldog%2C+A">A. Boldog</a>, <a href="/search/?searchtype=author&query=Nielsen%2C+L+D">L. D. Nielsen</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Lafarga%2C+M">M. Lafarga</a>, <a href="/search/?searchtype=author&query=Meech%2C+A">A. Meech</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a> , et al. (76 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.16958v2-abstract-short" style="display: inline;"> The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously with the European Southern Observatory's (ESO's) Very Large Telescope (VLT)/Echelle SPectrograph for R… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16958v2-abstract-full').style.display = 'inline'; document.getElementById('2411.16958v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.16958v2-abstract-full" style="display: none;"> The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously with the European Southern Observatory's (ESO's) Very Large Telescope (VLT)/Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO), CHaracterising ExOPlanet Satellite (CHEOPS), and Next-Generation Transit Survey (NGTS). After correcting for flares and for the magnetic activity of the host star, and accounting for transit-timing variations, we find the sky-projected spin-orbit angle of planet c to be in the range $位_c=67.8_{-49.0}^{+31.7}$\,degrees (1-$蟽$). We examine the possibility that planet c is misaligned with respect to the orbit of the inner planet b ($位_b=-2.96_{-10.30}^{+10.44}$\,degrees), and the equatorial plane of the host star, and discuss scenarios that could explain both this and the planet's high density, including secular interactions with other bodies in the system or a giant impact. We note that a significantly misaligned orbit for planet c is in some degree of tension with the dynamical stability of the system, and with the fact that we see both planets in transit, though these arguments alone do not preclude such an orbit. Further observations would be highly desirable to constrain the spin-orbit angle of planet c more precisely. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16958v2-abstract-full').style.display = 'none'; document.getElementById('2411.16958v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.07797">arXiv:2411.07797</a> <span> [<a href="https://arxiv.org/pdf/2411.07797">pdf</a>, <a href="https://arxiv.org/format/2411.07797">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451068">10.1051/0004-6361/202451068 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A close outer companion to the ultra-hot Jupiter TOI-2109 b? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Harre%2C+J+-">J. -V. Harre</a>, <a href="/search/?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Korth%2C+J">J. Korth</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Csizmadia%2C+S">Sz. Csizmadia</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Parviainen%2C+H">H. Parviainen</a>, <a href="/search/?searchtype=author&query=Correia%2C+A+C+M">A. C. M. Correia</a>, <a href="/search/?searchtype=author&query=Akinsanmi%2C+B">B. Akinsanmi</a>, <a href="/search/?searchtype=author&query=Rosario%2C+N">N. Rosario</a>, <a href="/search/?searchtype=author&query=Leonardi%2C+P">P. Leonardi</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.07797v1-abstract-short" style="display: inline;"> Hot Jupiters with close-by planetary companions are rare, with only a handful of them having been discovered so far. This could be due to their suggested dynamical histories, leading to the possible ejection of other planets. TOI-2109 b is special in this regard because it is the hot Jupiter with the closest relative separation from its host star, being separated by less than 2.3 stellar radii. Un… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07797v1-abstract-full').style.display = 'inline'; document.getElementById('2411.07797v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.07797v1-abstract-full" style="display: none;"> Hot Jupiters with close-by planetary companions are rare, with only a handful of them having been discovered so far. This could be due to their suggested dynamical histories, leading to the possible ejection of other planets. TOI-2109 b is special in this regard because it is the hot Jupiter with the closest relative separation from its host star, being separated by less than 2.3 stellar radii. Unexpectedly, transit timing measurements from recently obtained CHEOPS observations show low amplitude transit-timing variations (TTVs). We aim to search for signs of orbital decay and to characterise the apparent TTVs, trying to gain information about a possible companion. We fit the newly obtained CHEOPS light curves using TLCM and extract the resulting mid-transit timings. Successively, we use these measurements in combination with TESS and archival photometric data and radial velocity data to estimate the rate of tidal orbital decay of TOI-2109 b, as well as characterise the TTVs using the N-body code TRADES and the photodynamical approach of PyTTV. We find tentative evidence at $3蟽$ for orbital decay in the TOI-2109 system, when we correct the mid-transit timings using the best-fitting sinusoidal model of the TTVs. We do not detect additional transits in the available photometric data, but find evidence towards the authenticity of the apparent TTVs, indicating a close-by, outer companion with $P_\mathrm{c} > 1.125\,$d. Due to the fast rotation of the star, the new planetary candidate cannot be detected in the available radial velocity (RV) measurements, and its parameters can only be loosely constrained by our joint TTV and RV modelling. TOI-2109 could join a small group of rare hot Jupiter systems that host close-by planetary companions, only one of which (WASP-47 b) has an outer companion. More high-precision photometric measurements are necessary to confirm the planetary companion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07797v1-abstract-full').style.display = 'none'; document.getElementById('2411.07797v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. 21 pages, 21 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692, A254 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.18169">arXiv:2410.18169</a> <span> [<a href="https://arxiv.org/pdf/2410.18169">pdf</a>, <a href="https://arxiv.org/format/2410.18169">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Architecture of TOI-561 planetary system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Correia%2C+A+C+M">A. C. M. Correia</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+G">H. G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Lacedelli%2C+G">G. Lacedelli</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.18169v3-abstract-short" style="display: inline;"> We present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.18169v3-abstract-full').style.display = 'inline'; document.getElementById('2410.18169v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.18169v3-abstract-full" style="display: none;"> We present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7 days (TOI-561 d), and 77.1 days (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 days. The precise characterisation of TOI-561's orbital architecture is interesting since old and metal-poor thick disk stars are less likely to host ultra-short period Super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be $77.14399\pm0.00025$ days, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius ($R_p = 2.517 \pm 0.045 R_{\oplus}$ from 5$\%$ to 2$\%$ precision) and mass ($M_p = 12.4 \pm 1.4 M_{\oplus}$) estimates, implying a density of $蟻_p = 0.778 \pm 0.097 蟻_{\oplus}$. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-minute accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.18169v3-abstract-full').style.display = 'none'; document.getElementById('2410.18169v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 10 Figures. Accepted on MNRAS. Updated the author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.16268">arXiv:2409.16268</a> <span> [<a href="https://arxiv.org/pdf/2409.16268">pdf</a>, <a href="https://arxiv.org/format/2409.16268">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451049">10.1051/0004-6361/202451049 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The CHEOPS view on the climate of WASP-3 b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Carone%2C+L">L. Carone</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">P. E. Cubillos</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/?searchtype=author&query=Krenn%2C+A">A. Krenn</a>, <a href="/search/?searchtype=author&query=Valdes%2C+E+M">E. Meier Valdes</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Swayne%2C+M+I">M. I. Swayne</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a> , et al. (61 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.16268v1-abstract-short" style="display: inline;"> Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere makes them the most amenable targets for the atmospheric characterization. In this paper we analyze the photometry collected during the secondary eclipses of the hot Jupiter WASP-3 b by CHEOPS, TESS and Spitzer. Our aim is to characterize the atmosphere of the planet by m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16268v1-abstract-full').style.display = 'inline'; document.getElementById('2409.16268v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.16268v1-abstract-full" style="display: none;"> Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere makes them the most amenable targets for the atmospheric characterization. In this paper we analyze the photometry collected during the secondary eclipses of the hot Jupiter WASP-3 b by CHEOPS, TESS and Spitzer. Our aim is to characterize the atmosphere of the planet by measuring the secondary eclipse depth in several passbands and constrain the planetary dayside spectrum. Our update of the stellar and planetary properties is consistent with previous works. The analysis of the occultations returns an eclipse depth of 92+-21 ppm in the CHEOPS passband, 83+-27 ppm for TESS and >2000 ppm in the IRAC 1-2-4 Spitzer passbands. Using the eclipse depths in the Spitzer bands we propose a set of likely emission spectra which constrain the emission contribution in the \cheops and TESS passbands to approximately a few dozens of parts per million. This allowed us to measure a geometric albedo of 0.21+-0.07 in the CHEOPS passband, while the TESS data lead to a 95\% upper limit of $\sim$0.2. WASP-3 b belongs to the group of ultra-hot Jupiters which are characterized by low Bond albedo (<0.3+-0.1), as predicted by different atmospheric models. On the other hand, it unexpectedly seems to efficiently recirculate the absorbed stellar energy, unlike similar highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms may be at play other than advection (for example, dissociation and recombination of H_2). Another possibility is that the observations in different bandpasses probe different atmospheric layers, making the atmospheric analysis difficult without an appropriate modeling of the thermal emission spectrum of WASP-3 b, which is not feasible with the limited spectroscopic data available to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16268v1-abstract-full').style.display = 'none'; document.getElementById('2409.16268v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692, A129 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.02995">arXiv:2409.02995</a> <span> [<a href="https://arxiv.org/pdf/2409.02995">pdf</a>, <a href="https://arxiv.org/format/2409.02995">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450852">10.1051/0004-6361/202450852 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The K2-24 planetary system revisited by CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Leonardi%2C+P">P. Leonardi</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">A. Fortier</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a>, <a href="/search/?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C">S. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Biondi%2C+F">F. Biondi</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Busch%2C+M+-">M. -D. Busch</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a> , et al. (60 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.02995v3-abstract-short" style="display: inline;"> K2-24 is a planetary system composed of two transiting low-density Neptunians locked in an almost perfect 2:1 resonance and showing large TTVs, i.e., an excellent laboratory to search for signatures of planetary migration. Previous studies performed with K2, Spitzer and RV data tentatively claimed a significant non-zero eccentricity for one or both planets, possibly high enough to challenge the sc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02995v3-abstract-full').style.display = 'inline'; document.getElementById('2409.02995v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02995v3-abstract-full" style="display: none;"> K2-24 is a planetary system composed of two transiting low-density Neptunians locked in an almost perfect 2:1 resonance and showing large TTVs, i.e., an excellent laboratory to search for signatures of planetary migration. Previous studies performed with K2, Spitzer and RV data tentatively claimed a significant non-zero eccentricity for one or both planets, possibly high enough to challenge the scenario of pure disk migration through resonant capture. With 13 new CHEOPS light curves (seven of planet -b, six of planet -c), we carried out a global photometric and dynamical re-analysis by including all the available literature data as well. We got the most accurate set of planetary parameters to date for the K2-24 system, including radii and masses at 1% and 5% precision (now essentially limited by the uncertainty on stellar parameters) and non-zero eccentricities $e_b=0.0498_{-0.0018}^{+0.0011}$, $e_c=0.0282_{-0.0007}^{+0.0003}$ detected at very high significance for both planets. Such relatively large values imply the need for an additional physical mechanism of eccentricity excitation during or after the migration stage. Also, while the accuracy of the previous TTV model had drifted by up to 0.5 days at the current time, we constrained the orbital solution firmly enough to predict the forthcoming transits for the next ~15 years, thus enabling an efficient follow-up with top-level facilities such as JWST or ESPRESSO. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02995v3-abstract-full').style.display = 'none'; document.getElementById('2409.02995v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 11 figures, 8 tables. Accepted for publication in A&A on September 4, 2024. Typos corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A349 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.20525">arXiv:2407.20525</a> <span> [<a href="https://arxiv.org/pdf/2407.20525">pdf</a>, <a href="https://arxiv.org/format/2407.20525">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> TOI-757 b: an eccentric transiting mini-Neptune on a 17.5-d orbit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Alqasim%2C+A">A. Alqasim</a>, <a href="/search/?searchtype=author&query=Grieves%2C+N">N. Grieves</a>, <a href="/search/?searchtype=author&query=Ros%C3%A1rio%2C+N+M">N. M. Ros谩rio</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Livingston%2C+J+H">J. H. Livingston</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S">S. Sousa</a>, <a href="/search/?searchtype=author&query=Collins%2C+K+A">K. A. Collins</a>, <a href="/search/?searchtype=author&query=Teske%2C+J+K">J. K. Teske</a>, <a href="/search/?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Hellier%2C+C">C. Hellier</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Van+Eylen%2C+V">V. Van Eylen</a>, <a href="/search/?searchtype=author&query=Bouchy%2C+F">F. Bouchy</a>, <a href="/search/?searchtype=author&query=Oelkers%2C+R+J">R. J. Oelkers</a>, <a href="/search/?searchtype=author&query=Srdoc%2C+G">G. Srdoc</a>, <a href="/search/?searchtype=author&query=Shectman%2C+S">S. Shectman</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M">M. G眉nther</a>, <a href="/search/?searchtype=author&query=Goffo%2C+E">E. Goffo</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T">T. Wilson</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Wang%2C+S+X">S. X. Wang</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a> , et al. (107 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.20525v1-abstract-short" style="display: inline;"> We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-day orbit transiting a bright star ($V = 9.7$ mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20525v1-abstract-full').style.display = 'inline'; document.getElementById('2407.20525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.20525v1-abstract-full" style="display: none;"> We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-day orbit transiting a bright star ($V = 9.7$ mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of $R_{\mathrm{p}} = 2.5 \pm 0.1 R_{\oplus}$ and a mass of $M_{\mathrm{p}} = 10.5^{+2.2}_{-2.1} M_{\oplus}$, implying a bulk density of $蟻_{\text{p}} = 3.6 \pm 0.8$ g cm$^{-3}$. Our internal composition modeling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with $e$ = 0.39$^{+0.08}_{-0.07}$, making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b's formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star-star interactions during the earlier epoch of the Galactic disk formation, given the low metallicity and older age of TOI-757. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20525v1-abstract-full').style.display = 'none'; document.getElementById('2407.20525v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS; 26 pages, 14 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.06097">arXiv:2407.06097</a> <span> [<a href="https://arxiv.org/pdf/2407.06097">pdf</a>, <a href="https://arxiv.org/format/2407.06097">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450974">10.1051/0004-6361/202450974 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterisation of the Warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Degen%2C+D">D. Degen</a>, <a href="/search/?searchtype=author&query=Leleu%2C+A">A. Leleu</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Correia%2C+A+C+M">A. C. M. Correia</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Guillot%2C+T">T. Guillot</a>, <a href="/search/?searchtype=author&query=Triaud%2C+A+H+M+J">A. H. M. J. Triaud</a>, <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Abe%2C+L">L. Abe</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.06097v1-abstract-short" style="display: inline;"> Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as "lonely" and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06097v1-abstract-full').style.display = 'inline'; document.getElementById('2407.06097v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.06097v1-abstract-full" style="display: none;"> Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as "lonely" and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed and well characterised. Within the contest of multi-planet system hosting gas-giant on short orbits, we characterise TOI-1130 system by measuring masses and orbital parameters. This is a 2-transiting planet system with a Jupiter-like planet (c) on a 8.35 days orbit and a Neptune-like planet (b) on an inner (4.07 days) orbit. Both planets show strong anti-correlated transit timing variations (TTVs). Furthermore, radial velocity (RV) analysis showed an additional linear trend, a possible hint of a non-transiting candidate planet on a far outer orbit. Since 2019, extensive transit and radial velocity observations of the TOI-1130 have been acquired using TESS and various ground-based facilities. We present a new photo-dynamical analysis of all available transit and RV data, with the addition of new CHEOPS and ASTEP+ data that achieve the best precision to date on the planetary radii and masses and on the timings of each transit. We were able to model interior structure of planet b constraining the presence of a gaseous envelope of H/He, while it was not possible to assess the possible water content. Furthermore, we analysed the resonant state of the two transiting planets, and we found that they lie just outside the resonant region. This could be the result of the tidal evolution that the system underwent. We obtained both masses of the planets with a precision less than 1.5%, and radii with a precision of about 1% and 3% for planet b and c, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06097v1-abstract-full').style.display = 'none'; document.getElementById('2407.06097v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 10 figures, Accepted for publication by Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A52 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.18653">arXiv:2406.18653</a> <span> [<a href="https://arxiv.org/pdf/2406.18653">pdf</a>, <a href="https://arxiv.org/format/2406.18653">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450472">10.1051/0004-6361/202450472 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Kubyshkina%2C+D">D. Kubyshkina</a>, <a href="/search/?searchtype=author&query=Mordasini%2C+C">C. Mordasini</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Leleu%2C+A">A. Leleu</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Haldemann%2C+J">J. Haldemann</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a> , et al. (69 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.18653v1-abstract-short" style="display: inline;"> Multiplanetary systems spanning the radius valley are ideal testing grounds for exploring the proposed explanations for the observed bimodality in the radius distribution of close-in exoplanets. One such system is HIP 29442 (TOI-469), an evolved K0V star hosting two super-Earths and a sub-Neptune. We observe HIP 29442 with CHEOPS for a total of 9.6 days, which we model jointly with 2 sectors of TE… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18653v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18653v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18653v1-abstract-full" style="display: none;"> Multiplanetary systems spanning the radius valley are ideal testing grounds for exploring the proposed explanations for the observed bimodality in the radius distribution of close-in exoplanets. One such system is HIP 29442 (TOI-469), an evolved K0V star hosting two super-Earths and a sub-Neptune. We observe HIP 29442 with CHEOPS for a total of 9.6 days, which we model jointly with 2 sectors of TESS data to derive planetary radii of $3.410\pm0.046$, $1.551\pm0.045$ and $1.538\pm0.049$ R$_\oplus$ for planets b, c and d, which orbit HIP 29442 with periods of 13.6, 3.5 and 6.4 days. For planet d, this value deviates by more than 3 sigma from the median value reported in the discovery paper, leading us to conclude that caution is required when using TESS photometry to determine the radii of small planets with low per-transit S/N and large gaps between observations. Given the high precision of these new radii, combining them with published RVs from ESPRESSO and HIRES provides us with ideal conditions to investigate the internal structure and formation pathways of the planets in the system. We introduce the publicly available code plaNETic, a fast and robust neural network-based Bayesian internal structure modelling framework. We then apply hydrodynamic models to explore the upper atmospheric properties of these inferred structures. Finally, we identify planetary system analogues in a synthetic population generated with the Bern model for planet formation and evolution. Based on this analysis, we find that the planets likely formed on opposing sides of the water iceline from a protoplanetary disk with an intermediate solid mass. We finally report that the observed parameters of the HIP 29442 system are compatible with both a scenario where the second peak in the bimodal radius distribution corresponds to sub-Neptunes with a pure H/He envelope as well as a scenario with water-rich sub-Neptunes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18653v1-abstract-full').style.display = 'none'; document.getElementById('2406.18653v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 17 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 688, A223 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05447">arXiv:2406.05447</a> <span> [<a href="https://arxiv.org/pdf/2406.05447">pdf</a>, <a href="https://arxiv.org/format/2406.05447">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The PLATO Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rauer%2C+H">Heike Rauer</a>, <a href="/search/?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">Juan Cabrera</a>, <a href="/search/?searchtype=author&query=Deleuil%2C+M">Magali Deleuil</a>, <a href="/search/?searchtype=author&query=Erikson%2C+A">Anders Erikson</a>, <a href="/search/?searchtype=author&query=Gizon%2C+L">Laurent Gizon</a>, <a href="/search/?searchtype=author&query=Goupil%2C+M">Mariejo Goupil</a>, <a href="/search/?searchtype=author&query=Heras%2C+A">Ana Heras</a>, <a href="/search/?searchtype=author&query=Lorenzo-Alvarez%2C+J">Jose Lorenzo-Alvarez</a>, <a href="/search/?searchtype=author&query=Marliani%2C+F">Filippo Marliani</a>, <a href="/search/?searchtype=author&query=Martin-Garcia%2C+C">C茅sar Martin-Garcia</a>, <a href="/search/?searchtype=author&query=Mas-Hesse%2C+J+M">J. Miguel Mas-Hesse</a>, <a href="/search/?searchtype=author&query=O%27Rourke%2C+L">Laurence O'Rourke</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H">Hugh Osborn</a>, <a href="/search/?searchtype=author&query=Pagano%2C+I">Isabella Pagano</a>, <a href="/search/?searchtype=author&query=Piotto%2C+G">Giampaolo Piotto</a>, <a href="/search/?searchtype=author&query=Pollacco%2C+D">Don Pollacco</a>, <a href="/search/?searchtype=author&query=Ragazzoni%2C+R">Roberto Ragazzoni</a>, <a href="/search/?searchtype=author&query=Ramsay%2C+G">Gavin Ramsay</a>, <a href="/search/?searchtype=author&query=Udry%2C+S">St茅phane Udry</a>, <a href="/search/?searchtype=author&query=Appourchaux%2C+T">Thierry Appourchaux</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">Willy Benz</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">Alexis Brandeker</a>, <a href="/search/?searchtype=author&query=G%C3%BCdel%2C+M">Manuel G眉del</a>, <a href="/search/?searchtype=author&query=Janot-Pacheco%2C+E">Eduardo Janot-Pacheco</a> , et al. (820 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05447v2-abstract-short" style="display: inline;"> PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05447v2-abstract-full').style.display = 'inline'; document.getElementById('2406.05447v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05447v2-abstract-full" style="display: none;"> PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5 %, 10 %, 10 % for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO's target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile at the beginning of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05447v2-abstract-full').style.display = 'none'; document.getElementById('2406.05447v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.01716">arXiv:2406.01716</a> <span> [<a href="https://arxiv.org/pdf/2406.01716">pdf</a>, <a href="https://arxiv.org/format/2406.01716">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> CHEOPS in-flight performance: A comprehensive look at the first 3.5 years of operations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fortier%2C+A">A. Fortier</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Demory%2C+B+-">B. -O. Demory</a>, <a href="/search/?searchtype=author&query=Futyan%2C+D">D. Futyan</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Isaak%2C+K+G">K. G. Isaak</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Stalport%2C+M">M. Stalport</a> , et al. (106 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.01716v1-abstract-short" style="display: inline;"> CHEOPS is a space telescope specifically designed to monitor transiting exoplanets orbiting bright stars. In September 2023, CHEOPS completed its nominal mission and remains in excellent operational conditions. The mission has been extended until the end of 2026. Scientific and instrumental data have been collected throughout in-orbit commissioning and nominal operations, enabling a comprehensive… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01716v1-abstract-full').style.display = 'inline'; document.getElementById('2406.01716v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.01716v1-abstract-full" style="display: none;"> CHEOPS is a space telescope specifically designed to monitor transiting exoplanets orbiting bright stars. In September 2023, CHEOPS completed its nominal mission and remains in excellent operational conditions. The mission has been extended until the end of 2026. Scientific and instrumental data have been collected throughout in-orbit commissioning and nominal operations, enabling a comprehensive analysis of the mission's performance. In this article, we present the results of this analysis with a twofold goal. First, we aim to inform the scientific community about the present status of the mission and what can be expected as the instrument ages. Secondly, we intend for this publication to serve as a legacy document for future missions, providing insights and lessons learned from the successful operation of CHEOPS. To evaluate the instrument performance in flight, we developed a comprehensive monitoring and characterisation programme. It consists of dedicated observations that allow us to characterise the instrument's response. In addition to the standard collection of nominal science and housekeeping data, these observations provide input for detecting, modelling, and correcting instrument systematics, discovering and addressing anomalies, and comparing the instrument's actual performance with expectations. The precision of the CHEOPS measurements has enabled the mission objectives to be met and exceeded. Careful modelling of the instrumental systematics allows the data quality to be significantly improved during the light curve analysis phase, resulting in more precise scientific measurements. CHEOPS is compliant with the driving scientific requirements of the mission. Although visible, the ageing of the instrument has not affected the mission's performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01716v1-abstract-full').style.display = 'none'; document.getElementById('2406.01716v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.20077">arXiv:2405.20077</a> <span> [<a href="https://arxiv.org/pdf/2405.20077">pdf</a>, <a href="https://arxiv.org/format/2405.20077">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449689">10.1051/0004-6361/202449689 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HIP 41378 observed by CHEOPS: Where is planet d? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sulis%2C+S">S. Sulis</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Grouffal%2C+S">S. Grouffal</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Santerne%2C+A">A. Santerne</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C">S. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Bergomi%2C+M">M. Bergomi</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=van+Damme%2C+C+C">C. Corral van Damme</a> , et al. (62 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.20077v1-abstract-short" style="display: inline;"> HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, $P_\mathrm{d} = 278.36$ d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on $P_\mathrm{d}= 278.36$ d, but th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.20077v1-abstract-full').style.display = 'inline'; document.getElementById('2405.20077v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.20077v1-abstract-full" style="display: none;"> HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, $P_\mathrm{d} = 278.36$ d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on $P_\mathrm{d}= 278.36$ d, but the observations show no transit. We find that large ($>22.4$ hours) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If $P_\mathrm{d} \neq 278.36$ d, the periods that minimize the eccentricity would be $101.22$ d and $371.14$ d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January 2025. Our study shows the importance of a mission like CHEOPS, which today is the only mission able to make long observations (i.e., from space) to track the ephemeris of long-period planets possibly affected by large TTVs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.20077v1-abstract-full').style.display = 'none'; document.getElementById('2405.20077v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, L18 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13732">arXiv:2405.13732</a> <span> [<a href="https://arxiv.org/pdf/2405.13732">pdf</a>, <a href="https://arxiv.org/format/2405.13732">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450212">10.1051/0004-6361/202450212 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photo-dynamical characterisation of the TOI-178 resonant chain </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Leleu%2C+A">A. Leleu</a>, <a href="/search/?searchtype=author&query=Delisle%2C+J+-">J. -B. Delisle</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Bryant%2C+E+M">E. M. Bryant</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Hara%2C+N">N. Hara</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Chakraborty%2C+H">H. Chakraborty</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Alves%2C+D+R">D. R. Alves</a>, <a href="/search/?searchtype=author&query=Anderson%2C+D+R">D. R. Anderson</a>, <a href="/search/?searchtype=author&query=Apergis%2C+I">I. Apergis</a>, <a href="/search/?searchtype=author&query=Armstrong%2C+D">D. Armstrong</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Battley%2C+M+P">M. P. Battley</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a> , et al. (82 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13732v1-abstract-short" style="display: inline;"> The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with radii ranging from 1.2 to 2.9 earth radius and orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. The fine-tuning and fragility of such orbital configurations ensure that no significant scattering or collision ev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13732v1-abstract-full').style.display = 'inline'; document.getElementById('2405.13732v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13732v1-abstract-full" style="display: none;"> The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with radii ranging from 1.2 to 2.9 earth radius and orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. The fine-tuning and fragility of such orbital configurations ensure that no significant scattering or collision event has taken place since the formation and migration of the planets in the protoplanetary disc, hence providing important anchors for planet formation models. We aim to improve the characterisation of the architecture of this key system, and in particular the masses and radii of its planets. In addition, since this system is one of the few resonant chains that can be characterised by both photometry and radial velocities, we aim to use it as a test bench for the robustness of the planetary mass determination with each technique. We perform a global analysis of all available photometry and radial velocity. We also try different sets of priors on the masses and eccentricity, as well as different stellar activity models, to study their effects on the masses estimated by each method. We show how stellar activity is preventing us from obtaining a robust mass estimation for the three outer planets using radial velocity data alone. We also show that our joint photo-dynamical and radial velocity analysis resulted in a robust mass determination for planets c to g, with precision of 12% for the mass of planet c, and better than 10% for planets d to g. The new precisions on the radii range from 2 to 3%. The understanding of this synergy between photometric and radial velocity measurements will be valuable during the PLATO mission. We also show that TOI-178 is indeed currently locked in the resonant configuration, librating around an equilibrium of the chain. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13732v1-abstract-full').style.display = 'none'; document.getElementById('2405.13732v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 688, A211 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.11074">arXiv:2404.11074</a> <span> [<a href="https://arxiv.org/pdf/2404.11074">pdf</a>, <a href="https://arxiv.org/format/2404.11074">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Characterisation of the TOI-421 planetary system using CHEOPS, TESS, and archival radial velocity data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Krenn%2C+A+F">A. F. Krenn</a>, <a href="/search/?searchtype=author&query=Kubyshkina%2C+D">D. Kubyshkina</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Leleu%2C+A">A. Leleu</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Correira%2C+A+C+M">A. C. M. Correira</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Patel%2C+J+A">J. A. Patel</a>, <a href="/search/?searchtype=author&query=Venturini%2C+J">J. Venturini</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a> , et al. (66 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.11074v1-abstract-short" style="display: inline;"> The TOI-421 planetary system contains two sub-Neptune-type planets and is a prime target to study the formation and evolution of planets and their atmospheres. The inner planet is especially interesting as the existence of a hydrogen-dominated atmosphere at its orbital separation cannot be explained by current formation models without previous orbital migration. We jointly analysed photometric dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11074v1-abstract-full').style.display = 'inline'; document.getElementById('2404.11074v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.11074v1-abstract-full" style="display: none;"> The TOI-421 planetary system contains two sub-Neptune-type planets and is a prime target to study the formation and evolution of planets and their atmospheres. The inner planet is especially interesting as the existence of a hydrogen-dominated atmosphere at its orbital separation cannot be explained by current formation models without previous orbital migration. We jointly analysed photometric data of three TESS sectors and six CHEOPS visits as well as 156 radial velocity data points to retrieve improved planetary parameters. We also searched for TTVs and modelled the interior structure of the planets. Finally, we simulated the evolution of the primordial H-He atmospheres of the planets using two different modelling frameworks. We determine the planetary radii and masses of TOI-421 b and c to be $R_{\rm b} = 2.64 \pm 0.08 \, R_{\oplus}$, $M_{\rm b} = 6.7 \pm 0.6 \, M_{\oplus}$, $R_{\rm c} = 5.09 \pm 0.07 \, R_{\oplus}$, and $M_{\rm c} = 14.1 \pm 1.4 \, M_{\oplus}$. We do not detect any statistically significant TTV signals. Assuming the presence of a hydrogen-dominated atmosphere, the interior structure modelling results in both planets having extensive envelopes. While the modelling of the atmospheric evolution predicts for TOI-421 b to have lost any primordial atmosphere that it could have accreted at its current orbital position, TOI-421 c could have started out with an initial atmospheric mass fraction somewhere between 10 and 35%. We conclude that the low observed mean density of TOI-421 b can only be explained by either a bias in the measured planetary parameters (e.g. driven by high-altitude clouds) and/or in the context of orbital migration. We also find that the results of atmospheric evolution models are strongly dependent on the employed planetary structure model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11074v1-abstract-full').style.display = 'none'; document.getElementById('2404.11074v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 12 figures, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.17065">arXiv:2403.17065</a> <span> [<a href="https://arxiv.org/pdf/2403.17065">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Detailed cool star flare morphology with CHEOPS and TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/?searchtype=author&query=Pagano%2C+I">I. Pagano</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">A. Fortier</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Sulis%2C+S">S. Sulis</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Garai%2C+Z">Z. Garai</a>, <a href="/search/?searchtype=author&query=Boldog%2C+A">A. Boldog</a>, <a href="/search/?searchtype=author&query=Kriskovics%2C+L">L. Kriskovics</a>, <a href="/search/?searchtype=author&query=Szab%C3%B3%2C+M+G">M. Gy. Szab贸</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a> , et al. (57 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.17065v1-abstract-short" style="display: inline;"> Context. White-light stellar flares are proxies for some of the most energetic types of flares, but their triggering mechanism is still poorly understood. As they are associated with strong X and UV emission, their study is particularly relevant to estimate the amount of high-energy irradiation onto the atmospheres of exoplanets, especially those in their stars' habitable zone. Aims. We used the h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.17065v1-abstract-full').style.display = 'inline'; document.getElementById('2403.17065v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.17065v1-abstract-full" style="display: none;"> Context. White-light stellar flares are proxies for some of the most energetic types of flares, but their triggering mechanism is still poorly understood. As they are associated with strong X and UV emission, their study is particularly relevant to estimate the amount of high-energy irradiation onto the atmospheres of exoplanets, especially those in their stars' habitable zone. Aims. We used the high-cadence, high-photometric capabilities of the CHEOPS and TESS space telescopes to study the detailed morphology of white-light flares occurring in a sample of 130 late-K and M stars, and compared our findings with results obtained at a lower cadence. We developed dedicated software for this purpose. Results. Multi-peak flares represent a significant percentage ($\gtrsim 30$\%) of the detected outburst events. Our findings suggest that high-impulse flares are more frequent than suspected from lower-cadence data, so that the most impactful flux levels that hit close-in exoplanets might be more time-limited than expected. We found significant differences in the duration distributions of single-peak and complex flare components, but not in their peak luminosity. A statistical analysis of the flare parameter distributions provides marginal support for their description with a log-normal instead of a power-law function, leaving the door open to several flare formation scenarios. We tentatively confirmed previous results about quasi-periodic pulsations in high-cadence photometry, report the possible detection of a pre-flare dip, and did not find hints of photometric variability due to an undetected flare background. Conclusions. The high-cadence study of stellar hosts might be crucial to evaluate the impact of their flares on close-in exoplanets, as their impulsive phase emission might otherwise be incorrectly estimated. Future telescopes such as PLATO and Ariel will help in this respect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.17065v1-abstract-full').style.display = 'none'; document.getElementById('2403.17065v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 25 figures, 4 tables, to be published in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.16621">arXiv:2403.16621</a> <span> [<a href="https://arxiv.org/pdf/2403.16621">pdf</a>, <a href="https://arxiv.org/format/2403.16621">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347759">10.1051/0004-6361/202347759 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precise characterisation of HD 15337 with CHEOPS: a laboratory for planet formation and evolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ros%C3%A1rio%2C+N+M">N. M. Ros谩rio</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Guterman%2C+P">P. Guterman</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Nigioni%2C+A">A. Nigioni</a>, <a href="/search/?searchtype=author&query=Venturini%2C+J">J. Venturini</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.16621v1-abstract-short" style="display: inline;"> We aim to constrain the internal structure and composition of HD 15337 b and c, two short-period planets situated on opposite sides of the radius valley, using new transit photometry and radial velocity data. We acquire 6 new transit visits with the CHaracterising ExOPlanet Satellite (CHEOPS) and 32 new radial velocity measurements from the High Accuracy Radial Velocity Planet Searcher (HARPS) to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16621v1-abstract-full').style.display = 'inline'; document.getElementById('2403.16621v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.16621v1-abstract-full" style="display: none;"> We aim to constrain the internal structure and composition of HD 15337 b and c, two short-period planets situated on opposite sides of the radius valley, using new transit photometry and radial velocity data. We acquire 6 new transit visits with the CHaracterising ExOPlanet Satellite (CHEOPS) and 32 new radial velocity measurements from the High Accuracy Radial Velocity Planet Searcher (HARPS) to improve the accuracy of the mass and radius estimates for both planets. We reanalyse light curves from TESS sectors 3 and 4 and analyse new data from sector 30, correcting for long-term stellar activity. Subsequently, we perform a joint fit of the TESS and CHEOPS light curves, and all available RV data from HARPS and the Planet Finder Spectrograph (PFS). Our model fits the planetary signals, the stellar activity signal and the instrumental decorrelation model for the CHEOPS data simultaneously. The stellar activity was modelled using a Gaussian-process regression on both the RV and activity indicators. We finally employ a Bayesian retrieval code to determine the internal composition and structure of the planets. We derive updated and highly precise parameters for the HD 15337 system. Our improved precision on the planetary parameters makes HD 15337 b one of the most precisely characterised rocky exoplanets, with radius and mass measurements achieving a precision better than 2\% and 7\%, respectively. We are able to improve the precision of the radius measurement of HD 15337 c to 3\%. Our results imply that the composition of HD 15337 b is predominantly rocky, while HD 15337 c exhibits a gas envelope with a mass of at least $0.01\ M_\oplus$.Our results lay the groundwork for future studies, which can further unravel the atmospheric evolution of these exoplanets and give new insights into their composition and formation history and the causes behind the radius gap. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16621v1-abstract-full').style.display = 'none'; document.getElementById('2403.16621v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, including appendix</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A282 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.10486">arXiv:2402.10486</a> <span> [<a href="https://arxiv.org/pdf/2402.10486">pdf</a>, <a href="https://arxiv.org/format/2402.10486">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> The tidal deformation and atmosphere of WASP-12b from its phase curve </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Akinsanmi%2C+B">B. Akinsanmi</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Carone%2C+L">L. Carone</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">P. E. Cubillos</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">A. Fortier</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Bou%C3%A9%2C+G">G. Bou茅</a>, <a href="/search/?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/?searchtype=author&query=Demory%2C+B+-">B. -O. Demory</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Correia%2C+A+C+M">A. C. M. Correia</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.10486v2-abstract-short" style="display: inline;"> Ultra-hot Jupiters present a unique opportunity to understand the physics and chemistry of planets at extreme conditions. WASP-12b stands out as an archetype of this class of exoplanets. We performed comprehensive analyses of the transits, occultations, and phase curves of WASP-12b by combining new CHEOPS observations with previous TESS and Spitzer data to measure the planet's tidal deformation, a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10486v2-abstract-full').style.display = 'inline'; document.getElementById('2402.10486v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.10486v2-abstract-full" style="display: none;"> Ultra-hot Jupiters present a unique opportunity to understand the physics and chemistry of planets at extreme conditions. WASP-12b stands out as an archetype of this class of exoplanets. We performed comprehensive analyses of the transits, occultations, and phase curves of WASP-12b by combining new CHEOPS observations with previous TESS and Spitzer data to measure the planet's tidal deformation, atmospheric properties, and orbital decay rate. The planet was modeled as a triaxial ellipsoid parameterized by the second-order fluid Love number, $h_2$, which quantifies its radial deformation and provides insight into the interior structure. We measured the tidal deformation of WASP-12b and estimated a Love number of $h_2=1.55_{-0.49}^{+0.45}$ (at 3.2$蟽$) from its phase curve. We measured occultation depths of $333\pm24$ppm and $493\pm29$ppm in the CHEOPS and TESS bands, respectively, while the dayside emission spectrum indicates that CHEOPS and TESS probe similar pressure levels in the atmosphere at a temperature of 2900K. We also estimated low geometric albedos of $0.086\pm0.017$ and $0.01\pm0.023$ in the CHEOPS and TESS passbands, respectively, suggesting the absence of reflective clouds in the dayside of the WASP-12b. The CHEOPS occultations do not show strong evidence for variability in the dayside atmosphere of the planet. Finally, we refine the orbital decay rate by 12% to a value of -30.23$\pm$0.82 ms/yr. WASP-12b becomes the second exoplanet, after WASP-103b, for which the Love number has been measured (at 3$sigma$) from the effect of tidal deformation in the light curve. However, constraining the core mass fraction of the planet requires measuring $h_2$ with a higher precision. This can be achieved with high signal-to-noise observations with JWST since the phase curve amplitude, and consequently the induced tidal deformation effect, is higher in the infrared. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10486v2-abstract-full').style.display = 'none'; document.getElementById('2402.10486v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.15709">arXiv:2401.15709</a> <span> [<a href="https://arxiv.org/pdf/2401.15709">pdf</a>, <a href="https://arxiv.org/format/2401.15709">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Discovery of two warm mini-Neptunes with contrasting densities orbiting the young K3V star TOI-815 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Psaridi%2C+A">Angelica Psaridi</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H">Hugh Osborn</a>, <a href="/search/?searchtype=author&query=Bouchy%2C+F">Fran莽ois Bouchy</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">Monika Lendl</a>, <a href="/search/?searchtype=author&query=Parc%2C+L">L茅na Parc</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">Nicolas Billot</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">Christopher Broeg</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S茅rgio G. Sousa</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">Vardan Adibekyan</a>, <a href="/search/?searchtype=author&query=Attia%2C+O">Omar Attia</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">Andrea Bonfanti</a>, <a href="/search/?searchtype=author&query=Chakraborty%2C+H">Hritam Chakraborty</a>, <a href="/search/?searchtype=author&query=Collins%2C+K+A">Karen A. Collins</a>, <a href="/search/?searchtype=author&query=Davoult%2C+J">Jeanne Davoult</a>, <a href="/search/?searchtype=author&query=Delgado-Mena%2C+E">Elisa Delgado-Mena</a>, <a href="/search/?searchtype=author&query=Grieves%2C+N">Nolan Grieves</a>, <a href="/search/?searchtype=author&query=Guillot%2C+T">Tristan Guillot</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">Alexis Heitzmann</a>, <a href="/search/?searchtype=author&query=Helled%2C+R">Ravit Helled</a>, <a href="/search/?searchtype=author&query=Hellier%2C+C">Coel Hellier</a>, <a href="/search/?searchtype=author&query=Jenkins%2C+J+M">Jon M. Jenkins</a>, <a href="/search/?searchtype=author&query=Knierim%2C+H">Henrik Knierim</a>, <a href="/search/?searchtype=author&query=Krenn%2C+A">Andreas Krenn</a>, <a href="/search/?searchtype=author&query=Lissauer%2C+J">JackJ. Lissauer</a>, <a href="/search/?searchtype=author&query=Luque%2C+R">Rafael Luque</a> , et al. (108 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.15709v2-abstract-short" style="display: inline;"> We present the discovery and characterization of two warm mini-Neptunes transiting the K3V star TOI-815 in a K-M binary system. Analysis of the spectra and rotation period reveal it to be a young star with an age of $200^{+400}_{-200}$Myr. TOI-815b has a 11.2-day period and a radius of 2.94$\pm$0.05$\it{R_{\rm\mathrm{\oplus}}}$ with transits observed by TESS, CHEOPS, ASTEP, and LCOGT. The outer pl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.15709v2-abstract-full').style.display = 'inline'; document.getElementById('2401.15709v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.15709v2-abstract-full" style="display: none;"> We present the discovery and characterization of two warm mini-Neptunes transiting the K3V star TOI-815 in a K-M binary system. Analysis of the spectra and rotation period reveal it to be a young star with an age of $200^{+400}_{-200}$Myr. TOI-815b has a 11.2-day period and a radius of 2.94$\pm$0.05$\it{R_{\rm\mathrm{\oplus}}}$ with transits observed by TESS, CHEOPS, ASTEP, and LCOGT. The outer planet, TOI-815c, has a radius of 2.62$\pm$0.10$\it{R_{\rm\mathrm{\oplus}}}$, based on observations of three non-consecutive transits with TESS, while targeted CHEOPS photometry and radial velocity follow-up with ESPRESSO were required to confirm the 35-day period. ESPRESSO confirmed the planetary nature of both planets and measured masses of 7.6$\pm$1.5 $\it{M_{\rm \mathrm{\oplus}}}$ ($蟻_\mathrm{P}$=1.64$^{+0.33}_{-0.31}$gcm$^{-3}$) and 23.5$\pm$2.4$\it{M_{\rm\mathrm{\oplus}}}$ ($蟻_\mathrm{P}$=7.2$^{+1.1}_{-1.0}$gcm$^{-3}$) respectively. Thus, the planets have very different masses, unlike the usual similarity of masses in compact multi-planet systems. Moreover, our statistical analysis of mini-Neptunes orbiting FGK stars suggests that weakly irradiated planets tend to have higher bulk densities compared to those suffering strong irradiation. This could be ascribed to their cooler atmospheres, which are more compressed and denser. Internal structure modeling of TOI-815b suggests it likely has a H-He atmosphere constituting a few percent of the total planet mass, or higher if the planet is assumed to have no water. In contrast, the measured mass and radius of TOI-815c can be explained without invoking any atmosphere, challenging planetary formation theories. Finally, we infer from our measurements that the star is viewed close to pole-on, which implies a spin-orbit misalignment at the 3$蟽$ level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.15709v2-abstract-full').style.display = 'none'; document.getElementById('2401.15709v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 27 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.11339">arXiv:2312.11339</a> <span> [<a href="https://arxiv.org/pdf/2312.11339">pdf</a>, <a href="https://arxiv.org/format/2312.11339">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> The EBLM Project XI. Mass, radius and effective temperature measurements for 23 M-dwarf companions to solar-type stars observed with CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Swayne%2C+M+I">M. I. Swayne</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Triaud%2C+A+H+M+J">A. H. M. J. Triaud</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Boisse%2C+I">I. Boisse</a>, <a href="/search/?searchtype=author&query=Duck%2C+A">A. Duck</a>, <a href="/search/?searchtype=author&query=Gill%2C+S">S. Gill</a>, <a href="/search/?searchtype=author&query=Martin%2C+D">D. Martin</a>, <a href="/search/?searchtype=author&query=McCormac%2C+J">J. McCormac</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Santerne%2C+A">A. Santerne</a>, <a href="/search/?searchtype=author&query=Sebastian%2C+D">D. Sebastian</a>, <a href="/search/?searchtype=author&query=Standing%2C+M+R">M. R. Standing</a>, <a href="/search/?searchtype=author&query=Acu%C3%B1a%2C+L">L. Acu帽a</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a> , et al. (82 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.11339v1-abstract-short" style="display: inline;"> Observations of low-mass stars have frequently shown a disagreement between observed stellar radii and radii predicted by theoretical stellar structure models. This ``radius inflation'' problem could have an impact on both stellar and exoplanetary science. We present the final results of our observation programme with the CHEOPS satellite to obtain high-precision light curves of eclipsing binaries… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11339v1-abstract-full').style.display = 'inline'; document.getElementById('2312.11339v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.11339v1-abstract-full" style="display: none;"> Observations of low-mass stars have frequently shown a disagreement between observed stellar radii and radii predicted by theoretical stellar structure models. This ``radius inflation'' problem could have an impact on both stellar and exoplanetary science. We present the final results of our observation programme with the CHEOPS satellite to obtain high-precision light curves of eclipsing binaries with low mass stellar companions (EBLMs). Combined with the spectroscopic orbits of the solar-type companion, we can derive the masses, radii and effective temperatures of 23 M-dwarf stars. We use the PYCHEOPS data analysis software to analyse their primary and secondary occultations. For all but one target, we also perform analyses with TESS light curves for comparison. We have assessed the impact of starspot-induced variation on our derived parameters and account for this in our radius and effective temperature uncertainties using simulated light curves. We observe trends for inflation with both metallicity and orbital separation. We also observe a strong trend in the difference between theoretical and observational effective temperatures with metallicity. There is no such trend with orbital separation. These results are not consistent with the idea that observed inflation in stellar radius combines with lower effective temperature to preserve the luminosity predicted by low-mass stellar models. Our EBLM systems are high-quality and homogeneous measurements that can be used in further studies into radius inflation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11339v1-abstract-full').style.display = 'none'; document.getElementById('2312.11339v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 10 figures, accepted for publication in MNRAS, Supplementary material provided as ancillary files</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.17775">arXiv:2311.17775</a> <span> [<a href="https://arxiv.org/pdf/2311.17775">pdf</a>, <a href="https://arxiv.org/format/2311.17775">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-023-06692-3">10.1038/s41586-023-06692-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A resonant sextuplet of sub-Neptunes transiting the bright star HD 110067 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Leleu%2C+A">A. Leleu</a>, <a href="/search/?searchtype=author&query=Pall%C3%A9%2C+E">E. Pall茅</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Barrag%C3%A1n%2C+O">O. Barrag谩n</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Delisle%2C+J+-">J. -B. Delisle</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Nowak%2C+G">G. Nowak</a>, <a href="/search/?searchtype=author&query=Lafarga%2C+M">M. Lafarga</a>, <a href="/search/?searchtype=author&query=Rapetti%2C+D">D. Rapetti</a>, <a href="/search/?searchtype=author&query=Twicken%2C+J+D">J. D. Twicken</a>, <a href="/search/?searchtype=author&query=Morales%2C+J+C">J. C. Morales</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Orell-Miquel%2C+J">J. Orell-Miquel</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a> , et al. (127 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.17775v1-abstract-short" style="display: inline;"> Planets with radii between that of the Earth and Neptune (hereafter referred to as sub-Neptunes) are found in close-in orbits around more than half of all Sun-like stars. Yet, their composition, formation, and evolution remain poorly understood. The study of multi-planetary systems offers an opportunity to investigate the outcomes of planet formation and evolution while controlling for initial con… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.17775v1-abstract-full').style.display = 'inline'; document.getElementById('2311.17775v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.17775v1-abstract-full" style="display: none;"> Planets with radii between that of the Earth and Neptune (hereafter referred to as sub-Neptunes) are found in close-in orbits around more than half of all Sun-like stars. Yet, their composition, formation, and evolution remain poorly understood. The study of multi-planetary systems offers an opportunity to investigate the outcomes of planet formation and evolution while controlling for initial conditions and environment. Those in resonance (with their orbital periods related by a ratio of small integers) are particularly valuable because they imply a system architecture practically unchanged since its birth. Here, we present the observations of six transiting planets around the bright nearby star HD 110067. We find that the planets follow a chain of resonant orbits. A dynamical study of the innermost planet triplet allowed the prediction and later confirmation of the orbits of the rest of the planets in the system. The six planets are found to be sub-Neptunes with radii ranging from 1.94 to 2.85 Re. Three of the planets have measured masses, yielding low bulk densities that suggest the presence of large hydrogen-dominated atmospheres. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.17775v1-abstract-full').style.display = 'none'; document.getElementById('2311.17775v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Nature on November 30, 2023. Supplementary Information can be found in the online version of the paper in the journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature 623, 932-937 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.12577">arXiv:2311.12577</a> <span> [<a href="https://arxiv.org/pdf/2311.12577">pdf</a>, <a href="https://arxiv.org/format/2311.12577">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Characterising TOI-732 b and c: New insights into the M-dwarf radius and density valley </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Brady%2C+M">M. Brady</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Venturini%2C+J">J. Venturini</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">D. Queloz</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Kubyshkina%2C+D">D. Kubyshkina</a>, <a href="/search/?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/?searchtype=author&query=Murgas%2C+F">F. Murgas</a>, <a href="/search/?searchtype=author&query=Mustill%2C+A+J">A. J. Mustill</a>, <a href="/search/?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=Bandy%2C+T">T. Bandy</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a> , et al. (66 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.12577v2-abstract-short" style="display: inline;"> TOI-732 is an M dwarf hosting two transiting planets that are located on the two opposite sides of the radius valley. By doubling the number of available space-based observations and increasing the number of radial velocity (RV) measurements, we aim at refining the parameters of TOI-732 b and c. We also use the results to study the slope of the radius valley and the density valley for a well-chara… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12577v2-abstract-full').style.display = 'inline'; document.getElementById('2311.12577v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.12577v2-abstract-full" style="display: none;"> TOI-732 is an M dwarf hosting two transiting planets that are located on the two opposite sides of the radius valley. By doubling the number of available space-based observations and increasing the number of radial velocity (RV) measurements, we aim at refining the parameters of TOI-732 b and c. We also use the results to study the slope of the radius valley and the density valley for a well-characterised sample of M-dwarf exoplanets. We performed a global MCMC analysis by jointly modelling ground-based light curves and CHEOPS and TESS observations, along with RV time series both taken from the literature and obtained with the MAROON-X spectrograph. The slopes of the M-dwarf valleys were quantified via a Support Vector Machine (SVM) procedure. TOI-732 b is an ultrashort-period planet ($P\sim0.77$ d) with a radius $R_b=1.325_{-0.058}^{+0.057}$ $R_{\oplus}$ and a mass $M_b=2.46\pm0.19$ $M_{\oplus}$ (mean density $蟻_b=5.8_{-0.8}^{+1.0}$ g cm$^{-3}$), while the outer planet at $P\sim12.25$ d has $R_c=2.39_{-0.11}^{+0.10}$ $R_{\oplus}$, $M_c=8.04_{-0.48}^{+0.50}$ $M_{\oplus}$, and thus $蟻_c=3.24_{-0.43}^{+0.55}$ g cm$^{-3}$. Also taking into account our interior structure calculations, TOI-732 b is a super-Earth and TOI-732 c is a mini-Neptune. Following the SVM approach, we quantified $\mathrm{d}\log{R_{p,{\mathrm{valley}}}}/\mathrm{d}\log{P}=-0.065_{-0.013}^{+0.024}$, which is flatter than for Sun-like stars. In line with former analyses, we note that the radius valley for M-dwarf planets is more densely populated, and we further quantify the slope of the density valley as $\mathrm{d}\log{\hat蟻_{\mathrm{valley}}}/\mathrm{d}\log{P}=-0.02_{-0.04}^{+0.12}$. Compared to FGK stars, the weaker dependence of the position of the radius valley on the orbital period might indicate that the formation shapes the radius valley around M dwarfs more strongly than the evolution mechanisms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12577v2-abstract-full').style.display = 'none'; document.getElementById('2311.12577v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages (17 in the main text), 18 figures (9 in the main text), 11 tables (7 in the main text). Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.03264">arXiv:2311.03264</a> <span> [<a href="https://arxiv.org/pdf/2311.03264">pdf</a>, <a href="https://arxiv.org/format/2311.03264">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> CHEOPS observations of KELT-20 b/MASCARA-2 b: An aligned orbit and signs of variability from a reflective dayside </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">P. E. Cubillos</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">A. Fortier</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">D. Queloz</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Csizmadia%2C+S">Sz. Csizmadia</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Carone%2C+L">L. Carone</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Akinsanmi%2C+B">B. Akinsanmi</a>, <a href="/search/?searchtype=author&query=Patel%2C+J+A">J. A. Patel</a>, <a href="/search/?searchtype=author&query=Krenn%2C+A">A. Krenn</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/?searchtype=author&query=Pagano%2C+I">I. Pagano</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.03264v2-abstract-short" style="display: inline;"> Occultations are windows of opportunity to indirectly peek into the dayside atmosphere of exoplanets. High-precision transit events provide information on the spin-orbit alignment of exoplanets around fast-rotating hosts. We aim to precisely measure the planetary radius and geometric albedo of the ultra-hot Jupiter (UHJ) KELT-20 b as well as the system's spin-orbit alignment. We obtained optical h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03264v2-abstract-full').style.display = 'inline'; document.getElementById('2311.03264v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.03264v2-abstract-full" style="display: none;"> Occultations are windows of opportunity to indirectly peek into the dayside atmosphere of exoplanets. High-precision transit events provide information on the spin-orbit alignment of exoplanets around fast-rotating hosts. We aim to precisely measure the planetary radius and geometric albedo of the ultra-hot Jupiter (UHJ) KELT-20 b as well as the system's spin-orbit alignment. We obtained optical high-precision transits and occultations of KELT-20 b using CHEOPS observations in conjunction with the simultaneous TESS observations. We interpreted the occultation measurements together with archival infrared observations to measure the planetary geometric albedo and dayside temperatures. We further used the host star's gravity-darkened nature to measure the system's obliquity. We present a time-averaged precise occultation depth of 82(6) ppm measured with seven CHEOPS visits and 131(+8/-7) ppm from the analysis of all available TESS photometry. Using these measurements, we precisely constrain the geometric albedo of KELT-20 b to 0.26(0.04) and the brightness temperature of the dayside hemisphere to 2566(+77/-80) K. Assuming Lambertian scattering law, we constrain the Bond albedo to 0.36(+0.04/-0.05) along with a minimal heat transfer to the night side. Furthermore, using five transit observations we provide stricter constraints of 3.9(1.1) degrees on the sky-projected obliquity of the system. The aligned orbit of KELT-20 b is in contrast to previous CHEOPS studies that have found strongly inclined orbits for planets orbiting other A-type stars. The comparably high planetary geometric albedo of KELT-20 b corroborates a known trend of strongly irradiated planets being more reflective. Finally, we tentatively detect signs of temporal variability in the occultation depths, which might indicate variable cloud cover advecting onto the planetary day side. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03264v2-abstract-full').style.display = 'none'; document.getElementById('2311.03264v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 15 figures, Accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.10332">arXiv:2310.10332</a> <span> [<a href="https://arxiv.org/pdf/2310.10332">pdf</a>, <a href="https://arxiv.org/format/2310.10332">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347779">10.1051/0004-6361/202347779 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> No random transits in CHEOPS observations of HD 139139 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Deleuil%2C+M">M. Deleuil</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Guterman%2C+P">P. Guterman</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Bonfils%2C+X">X. Bonfils</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">Ch. Broeg</a>, <a href="/search/?searchtype=author&query=Charnoz%2C+S">S. Charnoz</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a> , et al. (56 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.10332v2-abstract-short" style="display: inline;"> HD 139139 (a.k.a. 'The Random Transiter') is a star that exhibited enigmatic transit-like features with no apparent periodicity in K2 data. The shallow depth of the events ($\sim$200 ppm -- equivalent to transiting objects with radii of $\sim$1.5 R$_\oplus$ in front of a Sun-like star), and their non-periodicity, constitutes a challenge for the photometric follow-up of this star. The goal of this… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.10332v2-abstract-full').style.display = 'inline'; document.getElementById('2310.10332v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.10332v2-abstract-full" style="display: none;"> HD 139139 (a.k.a. 'The Random Transiter') is a star that exhibited enigmatic transit-like features with no apparent periodicity in K2 data. The shallow depth of the events ($\sim$200 ppm -- equivalent to transiting objects with radii of $\sim$1.5 R$_\oplus$ in front of a Sun-like star), and their non-periodicity, constitutes a challenge for the photometric follow-up of this star. The goal of this study is to confirm with independent measurements the presence of shallow, non-periodic transit-like features on this object. We performed observations with CHEOPS, for a total accumulated time of 12.75 d, distributed in visits of roughly 20 h in two observing campaigns in years 2021 and 2022. The precision of the data is sufficient to detect 150 ppm features with durations longer than 1.5 h. We use the duration and times of the events seen in the K2 curve to estimate how many should have been detected in our campaigns, under the assumption that their behaviour during the CHEOPS observations would be the same as in the K2 data of 2017. We do not detect events with depths larger than 150 ppm in our data set. If the frequency, depth, and duration of the events were the same as in the K2 campaign, we estimate the probability of having missed all events due to our limited observing window would be 4.8 %. We suggest three different scenarios to explain our results: 1) Our observing window was not long enough, and the events were missed with the estimated 4.8 % probability. 2) The events recorded in the K2 observations were time critical, and the mechanism producing them was either not active in the 2021 and 2022 campaigns or created shallower events under our detectability level. 3) The enigmatic events in the K2 data are the result of an unidentified and infrequent instrumental noise in the original data set or its data treatment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.10332v2-abstract-full').style.display = 'none'; document.getElementById('2310.10332v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures, accepted for publication in A&A. Language-corrected version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A78 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.09037">arXiv:2309.09037</a> <span> [<a href="https://arxiv.org/pdf/2309.09037">pdf</a>, <a href="https://arxiv.org/format/2309.09037">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Constraining the reflective properties of WASP-178b using Cheops photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pagano%2C+I">I. Pagano</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">D. Queloz</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Sulis%2C+S">S. Sulis</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Bonfils%2C+X">X. Bonfils</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a> , et al. (57 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.09037v1-abstract-short" style="display: inline;"> Multiwavelength photometry of the secondary eclipses of extrasolar planets is able to disentangle the reflected and thermally emitted light radiated from the planetary dayside. This leads to the measurement of the planetary geometric albedo $A_g$, which is an indicator of the presence of clouds in the atmosphere, and the recirculation efficiency $蔚$, which quantifies the energy transport within th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.09037v1-abstract-full').style.display = 'inline'; document.getElementById('2309.09037v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.09037v1-abstract-full" style="display: none;"> Multiwavelength photometry of the secondary eclipses of extrasolar planets is able to disentangle the reflected and thermally emitted light radiated from the planetary dayside. This leads to the measurement of the planetary geometric albedo $A_g$, which is an indicator of the presence of clouds in the atmosphere, and the recirculation efficiency $蔚$, which quantifies the energy transport within the atmosphere. In this work we aim to measure $A_g$ and $蔚$ for the planet WASP-178 b, a highly irradiated giant planet with an estimated equilibrium temperature of 2450 K.} We analyzed archival spectra and the light curves collected by Cheops and Tess to characterize the host WASP-178, refine the ephemeris of the system and measure the eclipse depth in the passbands of the two respective telescopes. We measured a marginally significant eclipse depth of 70$\pm$40 ppm in the Tess passband and statistically significant depth of 70$\pm$20 ppm in the Cheops passband. Combining the eclipse depth measurement in the Cheops (lambda_eff=6300 AA) and Tess (lambda_eff=8000 AA) passbands we constrained the dayside brightness temperature of WASP-178 b in the 2250-2800 K interval. The geometric albedo 0.1<$\rm A_g$<0.35 is in general agreement with the picture of poorly reflective giant planets, while the recirculation efficiency $蔚>$0.7 makes WASP-178 b an interesting laboratory to test the current heat recirculation models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.09037v1-abstract-full').style.display = 'none'; document.getElementById('2309.09037v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Astronomy and Astrophysics on 31/08/2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.11394">arXiv:2308.11394</a> <span> [<a href="https://arxiv.org/pdf/2308.11394">pdf</a>, <a href="https://arxiv.org/format/2308.11394">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245479">10.1051/0004-6361/202245479 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Refining the properties of the TOI-178 system with CHEOPS and TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Leleu%2C+A">A. Leleu</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Gillon%2C+M">M. Gillon</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">A. Fortier</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">D. Queloz</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B+y">D. Barrado y Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a> , et al. (62 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.11394v1-abstract-short" style="display: inline;"> The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. Mass estimates derived from a preliminary radial velocity (RV) dataset suggest that the planetary densities do not decrease in a monotonic way with the orbital d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11394v1-abstract-full').style.display = 'inline'; document.getElementById('2308.11394v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.11394v1-abstract-full" style="display: none;"> The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. Mass estimates derived from a preliminary radial velocity (RV) dataset suggest that the planetary densities do not decrease in a monotonic way with the orbital distance to the star, contrary to what one would expect based on simple formation and evolution models. To improve the characterisation of this key system and prepare for future studies (in particular with JWST), we perform a detailed photometric study based on 40 new CHEOPS visits, one new TESS sector, as well as previously published CHEOPS, TESS, and NGTS data. First we perform a global analysis of the 100 transits contained in our data to refine the transit parameters of the six planets and study their transit timing variations (TTVs). We then use our extensive dataset to place constraints on the radii and orbital periods of potential additional transiting planets in the system. Our analysis significantly refines the transit parameters of the six planets, most notably their radii, for which we now obtain relative precisions $\lesssim$3%, with the exception of the smallest planet $b$ for which the precision is 5.1%. Combined with the RV mass estimates, the measured TTVs allow us to constrain the eccentricities of planets $c$ to $g$, which are found to be all below 0.02, as expected from stability requirements. Taken alone, the TTVs also suggest a higher mass for planet $d$ than the one estimated from the RVs, which had been found to yield a surprisingly low density for this planet. However, the masses derived from the current TTV dataset are very prior-dependent and further observations, over a longer temporal baseline, are needed to deepen our understanding of this iconic planetary system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11394v1-abstract-full').style.display = 'none'; document.getElementById('2308.11394v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 5 figures, 9 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A200 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.08687">arXiv:2308.08687</a> <span> [<a href="https://arxiv.org/pdf/2308.08687">pdf</a>, <a href="https://arxiv.org/format/2308.08687">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244946">10.1051/0004-6361/202244946 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CHEOPS and TESS view of the ultra-short period super-Earth TOI-561 b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Patel%2C+J+A">J. A. Patel</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Bourrier%2C+V">V. Bourrier</a>, <a href="/search/?searchtype=author&query=Carone%2C+L">L. Carone</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Lam%2C+K+W+F">K. W. F. Lam</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Bonfils%2C+X">X. Bonfils</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Busch%2C+M+-">M. -D. Busch</a> , et al. (53 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.08687v1-abstract-short" style="display: inline;"> Ultra-short period planets (USPs) are a unique class of super-Earths with an orbital period of less than a day and hence subject to intense radiation from their host star. While most of them are consistent with bare rocks, some show evidence of a heavyweight envelope, which could be a water layer or a secondary metal-rich atmosphere sustained by an outgassing surface. Much remains to be learned ab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.08687v1-abstract-full').style.display = 'inline'; document.getElementById('2308.08687v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.08687v1-abstract-full" style="display: none;"> Ultra-short period planets (USPs) are a unique class of super-Earths with an orbital period of less than a day and hence subject to intense radiation from their host star. While most of them are consistent with bare rocks, some show evidence of a heavyweight envelope, which could be a water layer or a secondary metal-rich atmosphere sustained by an outgassing surface. Much remains to be learned about the nature of USPs. The prime goal of the present work is to study the bulk planetary properties and atmosphere of TOI-561b, through the study of its transits and occultations. We obtained ultra-precise transit photometry of TOI-561b with CHEOPS and performed a joint analysis of this data with four TESS sectors. Our analysis of TOI-561b transit photometry put strong constraints on its properties, especially on its radius, Rp=1.42 +/- 0.02 R_Earth (at ~2% error). The internal structure modelling of the planet shows that the observations are consistent with negligible H/He atmosphere, however requiring other lighter materials, in addition to pure iron core and silicate mantle to explain the observed density. We find that this can be explained by the inclusion of a water layer in our model. We searched for variability in the measured Rp/R* over time to trace changes in the structure of the planetary envelope but none found within the data precision. In addition to the transit event, we tentatively detect occultation signal in the TESS data with an eclipse depth of ~27 +/- 11 ppm. Using the models of outgassed atmospheres from the literature we find that the thermal emission from the planet can mostly explain the observation. Based on this, we predict that NIR/MIR observations with JWST should be able to detect silicate species in the atmosphere of the planet. This could also reveal important clues about the planetary interior and help disentangle planet formation and evolution models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.08687v1-abstract-full').style.display = 'none'; document.getElementById('2308.08687v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 10 + 3 figures, 4 tables, accepted for publication in A&A (abstract abbreviated)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, A92 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.06085">arXiv:2307.06085</a> <span> [<a href="https://arxiv.org/pdf/2307.06085">pdf</a>, <a href="https://arxiv.org/format/2307.06085">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346050">10.1051/0004-6361/202346050 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating the visible phase-curve variability of 55 Cnc e </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vald%C3%A9s%2C+E+A+M">E. A. Meier Vald茅s</a>, <a href="/search/?searchtype=author&query=Morris%2C+B+M">B. M. Morris</a>, <a href="/search/?searchtype=author&query=Demory%2C+B+-">B. -O. Demory</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Kitzmann%2C+D">D. Kitzmann</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Bourrier%2C+V">V. Bourrier</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Heng%2C+K">K. Heng</a>, <a href="/search/?searchtype=author&query=Strugarek%2C+A">A. Strugarek</a>, <a href="/search/?searchtype=author&query=Bower%2C+D+J">D. J. Bower</a>, <a href="/search/?searchtype=author&query=J%C3%A4ggi%2C+N">N. J盲ggi</a>, <a href="/search/?searchtype=author&query=Carone%2C+L">L. Carone</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Jones%2C+K">K. Jones</a>, <a href="/search/?searchtype=author&query=Oza%2C+A+V">A. V. Oza</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.06085v2-abstract-short" style="display: inline;"> 55 Cnc e is an ultra-short period super-Earth transiting a Sun-like star. Previous observations in the optical range detected a time-variable flux modulation that is phased with the planetary orbital period, whose amplitude is too large to be explained by reflected light and thermal emission alone. The goal of the study is to investigate the origin of the variability and timescale of the phase-cur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.06085v2-abstract-full').style.display = 'inline'; document.getElementById('2307.06085v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.06085v2-abstract-full" style="display: none;"> 55 Cnc e is an ultra-short period super-Earth transiting a Sun-like star. Previous observations in the optical range detected a time-variable flux modulation that is phased with the planetary orbital period, whose amplitude is too large to be explained by reflected light and thermal emission alone. The goal of the study is to investigate the origin of the variability and timescale of the phase-curve modulation in 55 Cnc e. To this end, we used the CHaracterising ExOPlanet Satellite (CHEOPS), whose exquisite photometric precision provides an opportunity to characterise minute changes in the phase curve from one orbit to the next. CHEOPS observed 29 individual visits of 55 Cnc e between March 2020 and February 2022. Based on these observations, we investigated the different processes that could be at the origin of the observed modulation. In particular, we built a toy model to assess whether a circumstellar torus of dust driven by radiation pressure and gravity might match the observed flux variability timescale. We find that the phase-curve amplitude and peak offset of 55 Cnc e do vary between visits. The sublimation timescales of selected dust species reveal that silicates expected in an Earth-like mantle would not survive long enough to explain the observed phase-curve modulation. We find that silicon carbide, quartz, and graphite are plausible candidates for the circumstellar torus composition because their sublimation timescales are long. The extensive CHEOPS observations confirm that the phase-curve amplitude and offset vary in time.We find that dust could provide the grey opacity source required to match the observations. However, the data at hand do not provide evidence that circumstellar material with a variable grain mass per unit area causes the observed variability. Future observations with the James Webb Space Telescope promise exciting insights into this iconic super-Earth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.06085v2-abstract-full').style.display = 'none'; document.getElementById('2307.06085v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 22 figures. Accepted for publication on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 677, A112 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04511">arXiv:2306.04511</a> <span> [<a href="https://arxiv.org/pdf/2306.04511">pdf</a>, <a href="https://arxiv.org/format/2306.04511">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1369">10.1093/mnras/stad1369 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TESS and CHEOPS Discover Two Warm Sub-Neptunes Transiting the Bright K-dwarf HD 15906 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tuson%2C+A">Amy Tuson</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">Didier Queloz</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">Hugh P. Osborn</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">Thomas G. Wilson</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">Matthew J. Hooton</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">Mathias Beck</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">Monika Lendl</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G枚ran Olofsson</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">Andrea Fortier</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">Andrea Bonfanti</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">Alexis Brandeker</a>, <a href="/search/?searchtype=author&query=Buchhave%2C+L+A">Lars A. Buchhave</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">Andrew Collier Cameron</a>, <a href="/search/?searchtype=author&query=Ciardi%2C+D+R">David R. Ciardi</a>, <a href="/search/?searchtype=author&query=Collins%2C+K+A">Karen A. Collins</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">Davide Gandolfi</a>, <a href="/search/?searchtype=author&query=Garai%2C+Z">Zoltan Garai</a>, <a href="/search/?searchtype=author&query=Giacalone%2C+S">Steven Giacalone</a>, <a href="/search/?searchtype=author&query=da+Silva%2C+J+G">Jo茫o Gomes da Silva</a>, <a href="/search/?searchtype=author&query=Howell%2C+S+B">Steve B. Howell</a>, <a href="/search/?searchtype=author&query=Patel%2C+J+A">Jayshil A. Patel</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">Carina M. Persson</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">Luisa M. Serrano</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S茅rgio G. Sousa</a>, <a href="/search/?searchtype=author&query=Ulmer-Moll%2C+S">Sol猫ne Ulmer-Moll</a> , et al. (97 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.04511v1-abstract-short" style="display: inline;"> We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04511v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04511v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04511v1-abstract-full" style="display: none;"> We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by $\sim$ 734 days, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 $\pm$ 0.08 R$_\oplus$ and a period of 10.924709 $\pm$ 0.000032 days, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R$_\oplus$ and a period of 21.583298$^{+0.000052}_{-0.000055}$ days. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 $\pm$ 13 K and 532 $\pm$ 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm ($\lesssim$ 700 K) sub-Neptune sized planets transiting a bright star (G $\leq$ 10 mag). It is an excellent target for detailed characterisation studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04511v1-abstract-full').style.display = 'none'; document.getElementById('2306.04511v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 20 figures, 11 tables (including appendix). Published in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, volume 523, issue 2, pp 3090-3118 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04468">arXiv:2306.04468</a> <span> [<a href="https://arxiv.org/pdf/2306.04468">pdf</a>, <a href="https://arxiv.org/format/2306.04468">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202345943">10.1051/0004-6361/202345943 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Refined parameters of the HD 22946 planetary system and the true orbital period of planet d </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Garai%2C+Z">Z. Garai</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Tuson%2C+A">A. Tuson</a>, <a href="/search/?searchtype=author&query=Ulmer-Moll%2C+S">S. Ulmer-Moll</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B+y">D. Barrado y Navascues</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.04468v1-abstract-short" style="display: inline;"> Multi-planet systems are important sources of information regarding the evolution of planets. However, the long-period planets in these systems often escape detection. HD 22946 is a bright star around which 3 transiting planets were identified via TESS photometry, but the true orbital period of the outermost planet d was unknown until now. We aim to use CHEOPS to uncover the true orbital period of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04468v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04468v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04468v1-abstract-full" style="display: none;"> Multi-planet systems are important sources of information regarding the evolution of planets. However, the long-period planets in these systems often escape detection. HD 22946 is a bright star around which 3 transiting planets were identified via TESS photometry, but the true orbital period of the outermost planet d was unknown until now. We aim to use CHEOPS to uncover the true orbital period of HD 22946d and to refine the orbital and planetary properties of the system, especially the radii of the planets. We used the available TESS photometry of HD 22946 and observed several transits of the planets b, c, and d using CHEOPS. We identified 2 transits of planet d in the TESS photometry, calculated the most probable period aliases based on these data, and then scheduled CHEOPS observations. The photometric data were supplemented with ESPRESSO radial velocity data. Finally, a combined model was fitted to the entire dataset. We successfully determined the true orbital period of the planet d to be 47.42489 $\pm$ 0.00011 d, and derived precise radii of the planets in the system, namely 1.362 $\pm$ 0.040 R$_\oplus$, 2.328 $\pm$ 0.039 R$_\oplus$, and 2.607 $\pm$ 0.060 R$_\oplus$ for planets b, c, and d, respectively. Due to the low number of radial velocities, we were only able to determine 3$蟽$ upper limits for these respective planet masses, which are 13.71 M$_\oplus$, 9.72 M$_\oplus$, and 26.57 M$_\oplus$. We estimated that another 48 ESPRESSO radial velocities are needed to measure the predicted masses of all planets in HD 22946. Planet c appears to be a promising target for future atmospheric characterisation. We can also conclude that planet d, as a warm sub-Neptune, is very interesting because there are only a few similar confirmed exoplanets to date. Such objects are worth investigating in the near future, for example in terms of their composition and internal structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04468v1-abstract-full').style.display = 'none'; document.getElementById('2306.04468v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A44 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04450">arXiv:2306.04450</a> <span> [<a href="https://arxiv.org/pdf/2306.04450">pdf</a>, <a href="https://arxiv.org/format/2306.04450">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1319">10.1093/mnras/stad1319 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Two Warm Neptunes transiting HIP 9618 revealed by TESS & Cheops </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Osborn%2C+H+P">Hugh P. Osborn</a>, <a href="/search/?searchtype=author&query=Nowak%2C+G">Grzegorz Nowak</a>, <a href="/search/?searchtype=author&query=H%C3%A9brard%2C+G">Guillaume H茅brard</a>, <a href="/search/?searchtype=author&query=Masseron%2C+T">Thomas Masseron</a>, <a href="/search/?searchtype=author&query=Lillo-Box%2C+J">J. Lillo-Box</a>, <a href="/search/?searchtype=author&query=Pall%C3%A9%2C+E">Enric Pall茅</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">Anja Bekkelien</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H">Hans-Gustav Flor茅n</a>, <a href="/search/?searchtype=author&query=Guterman%2C+P">Pascal Guterman</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">Attila E. Simon</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Bieryla%2C+A">Allyson Bieryla</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">Luca Borsato</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">Alexis Brandeker</a>, <a href="/search/?searchtype=author&query=Ciardi%2C+D+R">David R. Ciardi</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">Andrew Collier Cameron</a>, <a href="/search/?searchtype=author&query=Collins%2C+K+A">Karen A. Collins</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">Jo A. Egger</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">Davide Gandolfi</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">Matthew J. Hooton</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">David W. Latham</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">Monika Lendl</a>, <a href="/search/?searchtype=author&query=Matthews%2C+E+C">Elisabeth C. Matthews</a>, <a href="/search/?searchtype=author&query=Tuson%2C+A">Amy Tuson</a>, <a href="/search/?searchtype=author&query=Ulmer-Moll%2C+S">Sol猫ne Ulmer-Moll</a> , et al. (104 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.04450v1-abstract-short" style="display: inline;"> HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright ($G=9.0$ mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of $3.9 \pm 0.044$ $R_\oplus$ (HIP 9618 b) and $3.343 \pm 0.039$ $R_\oplus$ (HIP 9618 c). While the 20.77291 day period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-day gap in the time s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04450v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04450v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04450v1-abstract-full" style="display: none;"> HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright ($G=9.0$ mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of $3.9 \pm 0.044$ $R_\oplus$ (HIP 9618 b) and $3.343 \pm 0.039$ $R_\oplus$ (HIP 9618 c). While the 20.77291 day period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-day gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE and CAFE revealed a mass of $10.0 \pm 3.1 M_\oplus$ for HIP 9618 b, which, according to our interior structure models, corresponds to a $6.8\pm1.4\%$ gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of $< 18M_\oplus$. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion ($0.08^{+0.12}_{-0.05} M_\odot$) orbiting at $26^{+19}_{-11}$ au. This detection makes HIP 9618 one of only five bright ($K<8$ mag) transiting multi-planet systems known to host a planet with $P>50$ d, opening the door for the atmospheric characterisation of warm ($T_{\rm eq}<750$ K) sub-Neptunes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04450v1-abstract-full').style.display = 'none'; document.getElementById('2306.04450v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 16 figures, 9 tables. Accepted at MNRAS. CHEOPS, RV and ground-based photometric data is available on CDS at https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/523/3069</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, Vol. 523, 2023, issue 2, pp 3069-3089 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04295">arXiv:2306.04295</a> <span> [<a href="https://arxiv.org/pdf/2306.04295">pdf</a>, <a href="https://arxiv.org/format/2306.04295">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245478">10.1051/0004-6361/202245478 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TOI-5678 b: A 48-day transiting Neptune-mass planet characterized with CHEOPS and HARPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ulmer-Moll%2C+S">S. Ulmer-Moll</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Tuson%2C+A">A. Tuson</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P">P. Maxted</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Bouchy%2C+F">F. Bouchy</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Mordasini%2C+C">C. Mordasini</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Rieder%2C+M">M. Rieder</a>, <a href="/search/?searchtype=author&query=Hasiba%2C+J">J. Hasiba</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a> , et al. (70 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.04295v1-abstract-short" style="display: inline;"> A large sample of long-period giant planets has been discovered thanks to long-term radial velocity surveys, but only a few dozen of these planets have a precise radius measurement. Transiting gas giants are crucial targets for the study of atmospheric composition across a wide range of equilibrium temperatures and for shedding light on the formation and evolution of planetary systems. Indeed, com… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04295v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04295v1-abstract-full" style="display: none;"> A large sample of long-period giant planets has been discovered thanks to long-term radial velocity surveys, but only a few dozen of these planets have a precise radius measurement. Transiting gas giants are crucial targets for the study of atmospheric composition across a wide range of equilibrium temperatures and for shedding light on the formation and evolution of planetary systems. Indeed, compared to hot Jupiters, the atmospheric properties and orbital parameters of cooler gas giants are unaltered by intense stellar irradiation and tidal effects. We identify long-period planets in the Transiting Exoplanet Survey Satellite (TESS) data as duo-transit events. To solve the orbital periods of TESS duo-transit candidates, we use the CHaracterising ExOPlanet Satellite (CHEOPS) to observe the highest-probability period aliases in order to discard or confirm a transit event at a given period. We also collect spectroscopic observations with CORALIE and HARPS in order to confirm the planetary nature and measure the mass of the candidates. We report the discovery of a warm transiting Neptune-mass planet orbiting TOI-5678. After four non-detections corresponding to possible periods, CHEOPS detected a transit event matching a unique period alias. Joint modeling reveals that TOI-5678 hosts a 47.73 day period planet. TOI-5678 b has a mass of 20 (+-4) Me and a radius of 4.91 (+-0.08 Re) . Using interior structure modeling, we find that TOI-5678 b is composed of a low-mass core surrounded by a large H/He layer with a mass of 3.2 (+1.7, -1.3) Me. TOI-5678 b is part of a growing sample of well-characterized transiting gas giants receiving moderate amounts of stellar insolation (11 Se). Precise density measurement gives us insight into their interior composition, and the objects orbiting bright stars are suitable targets to study the atmospheric composition of cooler gas giants. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04295v1-abstract-full').style.display = 'none'; document.getElementById('2306.04295v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 10 figures, accepted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.10664">arXiv:2302.10664</a> <span> [<a href="https://arxiv.org/pdf/2302.10664">pdf</a>, <a href="https://arxiv.org/format/2302.10664">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245607">10.1051/0004-6361/202245607 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Krenn%2C+A">A. Krenn</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Barrag%C3%A1n%2C+O">O. Barrag谩n</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Esposito%2C+M">M. Esposito</a>, <a href="/search/?searchtype=author&query=Goffo%2C+E">E. Goffo</a>, <a href="/search/?searchtype=author&query=Osborne%2C+H">H. Osborne</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Van+Eylen%2C+V">V. Van Eylen</a> , et al. (67 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.10664v2-abstract-short" style="display: inline;"> TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of planetary masses that differ by $\sim$ 2$蟽$. Our aim in this work is to solve the inconsistency in the published planetary masses by significantly ex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10664v2-abstract-full').style.display = 'inline'; document.getElementById('2302.10664v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.10664v2-abstract-full" style="display: none;"> TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of planetary masses that differ by $\sim$ 2$蟽$. Our aim in this work is to solve the inconsistency in the published planetary masses by significantly extending the set of HARPS RV measurements and employing a new analysis tool that is able to account and correct for stellar activity. Our further aim was to improve the precision on measurements of the planetary radius by observing two transits of the planet with the CHEOPS space telescope. We fit a skew normal (SN) function to each cross correlation function extracted from the HARPS spectra to obtain RV measurements and hyperparameters to be used for the detrending. We evaluated the correlation changes of the hyperparameters along the RV time series using the breakpoint technique. We performed a joint photometric and RV analysis using a Markov chain Monte Carlo (MCMC) scheme to simultaneously detrend the light curves and the RV time series. We firmly detected the Keplerian signal of TOI-1055 b, deriving a planetary mass of $M_b=20.4_{-2.5}^{+2.6} M_{\oplus}$ ($\sim$12%). This value is in agreement with one of the two estimates in the literature, but it is significantly more precise. Thanks to the TESS transit light curves combined with exquisite CHEOPS photometry, we also derived a planetary radius of $R_b=3.490_{-0.064}^{+0.070} R_{\oplus}$ ($\sim$1.9%). Our mass and radius measurements imply a mean density of $蟻_b=2.65_{-0.35}^{+0.37}$ g cm$^{-3}$ ($\sim$14%). We further inferred the planetary structure and found that TOI-1055 b is very likely to host a substantial gas envelope with a mass of $0.41^{+0.34}_{-0.20}$ M$_\oplus$ and a thickness of $1.05^{+0.30}_{-0.29}$ R$_\oplus$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10664v2-abstract-full').style.display = 'none'; document.getElementById('2302.10664v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 6 figures, 5 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, L8 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.02710">arXiv:2302.02710</a> <span> [<a href="https://arxiv.org/pdf/2302.02710">pdf</a>, <a href="https://arxiv.org/format/2302.02710">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245101">10.1051/0004-6361/202245101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Glancing through the debris disk: Photometric analysis of DE Boo with CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Boldog%2C+%C3%81">脕. Boldog</a>, <a href="/search/?searchtype=author&query=Szab%C3%B3%2C+G+M">Gy. M. Szab贸</a>, <a href="/search/?searchtype=author&query=Kriskovics%2C+L">L. Kriskovics</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Kiefer%2C+F">F. Kiefer</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Guterman%2C+P">P. Guterman</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Etangs%2C+A+L+d">A. Lecavelier des Etangs</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Bandy%2C+T">T. Bandy</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a> , et al. (54 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.02710v1-abstract-short" style="display: inline;"> DE Boo is a unique system, with an edge-on view through the debris disk around the star. The disk, which is analogous to the Kuiper belt in the Solar System, was reported to extend from 74 to 84 AU from the central star. The high photometric precision of the Characterising Exoplanet Satellite (CHEOPS) provided an exceptional opportunity to observe small variations in the light curve due to transit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02710v1-abstract-full').style.display = 'inline'; document.getElementById('2302.02710v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.02710v1-abstract-full" style="display: none;"> DE Boo is a unique system, with an edge-on view through the debris disk around the star. The disk, which is analogous to the Kuiper belt in the Solar System, was reported to extend from 74 to 84 AU from the central star. The high photometric precision of the Characterising Exoplanet Satellite (CHEOPS) provided an exceptional opportunity to observe small variations in the light curve due to transiting material in the disk. This is a unique chance to investigate processes in the debris disk. Photometric observations of DE Boo of a total of four days were carried out with CHEOPS. Photometric variations due to spots on the stellar surface were subtracted from the light curves by applying a two-spot model and a fourth-order polynomial. The photometric observations were accompanied by spectroscopic measurements with the 1m RCC telescope at Piszk茅stet艖 and with the SOPHIE spectrograph in order to refine the astrophysical parameters of DE Boo. We present a detailed analysis of the photometric observation of DE Boo. We report the presence of nonperiodic transient features in the residual light curves with a transit duration of 0.3-0.8 days. We calculated the maximum distance of the material responsible for these variations to be 2.47 AU from the central star, much closer than most of the mass of the debris disk. Furthermore, we report the first observation of flaring events in this system. We interpreted the transient features as the result of scattering in an inner debris disk around DE Boo. The processes responsible for these variations were investigated in the context of interactions between planetesimals in the system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02710v1-abstract-full').style.display = 'none'; document.getElementById('2302.02710v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures, 5 tables; accepted by Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A127 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.01853">arXiv:2302.01853</a> <span> [<a href="https://arxiv.org/pdf/2302.01853">pdf</a>, <a href="https://arxiv.org/format/2302.01853">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244790">10.1051/0004-6361/202244790 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A full transit of $谓^2$ Lupi d and the search for an exomoon in its Hill sphere with CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Akinsanmi%2C+B">B. Akinsanmi</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">D. Queloz</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Charnoz%2C+S">S. Charnoz</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M">M. Hooton</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.01853v1-abstract-short" style="display: inline;"> The planetary system around the naked-eye star $谓^2$ Lupi (HD 136352; TOI-2011) is composed of three exoplanets with masses of 4.7, 11.2, and 8.6 Earth masses. The TESS and CHEOPS missions revealed that all three planets are transiting and have radii straddling the radius gap separating volatile-rich and volatile-poor super-earths. Only a partial transit of planet d had been covered so we re-obser… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01853v1-abstract-full').style.display = 'inline'; document.getElementById('2302.01853v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.01853v1-abstract-full" style="display: none;"> The planetary system around the naked-eye star $谓^2$ Lupi (HD 136352; TOI-2011) is composed of three exoplanets with masses of 4.7, 11.2, and 8.6 Earth masses. The TESS and CHEOPS missions revealed that all three planets are transiting and have radii straddling the radius gap separating volatile-rich and volatile-poor super-earths. Only a partial transit of planet d had been covered so we re-observed an inferior conjunction of the long-period 8.6 Earth-mass exoplanet $谓^2$ Lup d with the CHEOPS space telescope. We confirmed its transiting nature by covering its whole 9.1 h transit for the first time. We refined the planet transit ephemeris to P = 107.1361 (+0.0019/-0.0022) days and Tc = 2,459,009.7759 (+0.0101/-0.0096) BJD_TDB, improving by ~40 times on the previously reported transit timing uncertainty. This refined ephemeris will enable further follow-up of this outstanding long-period transiting planet to search for atmospheric signatures or explore the planet's Hill sphere in search for an exomoon. In fact, the CHEOPS observations also cover the transit of a large fraction of the planet's Hill sphere, which is as large as the Earth's, opening the tantalising possibility of catching transiting exomoons. We conducted a search for exomoon signals in this single-epoch light curve but found no conclusive photometric signature of additional transiting bodies larger than Mars. Yet, only a sustained follow-up of $谓^2$ Lup d transits will warrant a comprehensive search for a moon around this outstanding exoplanet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01853v1-abstract-full').style.display = 'none'; document.getElementById('2302.01853v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 9 figures. Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A154 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.01352">arXiv:2302.01352</a> <span> [<a href="https://arxiv.org/pdf/2302.01352">pdf</a>, <a href="https://arxiv.org/format/2302.01352">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245486">10.1051/0004-6361/202245486 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new dynamical modeling of the WASP-47 system with CHEOPS observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/?searchtype=author&query=Pagano%2C+I">I. Pagano</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Majidi%2C+F+Z">F. Z. Majidi</a>, <a href="/search/?searchtype=author&query=Granata%2C+V">V. Granata</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Mustill%2C+A+J">A. J. Mustill</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a> , et al. (58 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.01352v2-abstract-short" style="display: inline;"> Among the hundreds of known hot Jupiters (HJs), only five have been found to have companions on short-period orbits. Within this rare class of multiple planetary systems, the architecture of WASP-47 is unique, hosting an HJ (planet -b) with both an inner and an outer sub-Neptunian mass companion (-e and -d, respectively) as well as an additional non-transiting, long-period giant (-c). The small pe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01352v2-abstract-full').style.display = 'inline'; document.getElementById('2302.01352v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.01352v2-abstract-full" style="display: none;"> Among the hundreds of known hot Jupiters (HJs), only five have been found to have companions on short-period orbits. Within this rare class of multiple planetary systems, the architecture of WASP-47 is unique, hosting an HJ (planet -b) with both an inner and an outer sub-Neptunian mass companion (-e and -d, respectively) as well as an additional non-transiting, long-period giant (-c). The small period ratio between planets -b and -d boosts the transit time variation (TTV) signal, making it possible to reliably measure the masses of these planets in synergy with the radial velocity (RV) technique. In this paper, we present new space- and ground-based photometric data of WASP-47b and WASP-47-d, including 11 unpublished light curves from the ESA mission CHEOPS. We analyzed the light curves in a homogeneous way together with all the publicly available data to carry out a global $N$-body dynamical modeling of the TTV and RV signals. We retrieved, among other parameters, a mass and density for planet -d of $M_\mathrm{d}=15.5\pm 0.8$ $M_\oplus$ and $蟻_\mathrm{d}=1.69\pm 0.22$ g\,cm$^{-3}$, which is in good agreement with the literature and consistent with a Neptune-like composition. For the inner planet (-e), we found a mass and density of $M_\mathrm{e}=9.0\pm 0.5$ $M_\oplus$ and $蟻_\mathrm{e}=8.1\pm 0.5$ g\,cm$^{-3}$, suggesting an Earth-like composition close to other ultra-hot planets at similar irradiation levels. Though this result is in agreement with previous RV+TTV studies, it is not in agreement with the most recent RV analysis (at 2.8$蟽$), which yielded a lower density compatible with a pure silicate composition. This discrepancy highlights the still unresolved issue of suspected systematic offsets between RV and TTV measurements. In this paper, we also significantly improve the orbital ephemerides of all transiting planets, which will be crucial for any future follow-up. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01352v2-abstract-full').style.display = 'none'; document.getElementById('2302.01352v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 8 figures, 10 tables, A&A in press. Typos corrected</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07731">arXiv:2301.07731</a> <span> [<a href="https://arxiv.org/pdf/2301.07731">pdf</a>, <a href="https://arxiv.org/format/2301.07731">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245016">10.1051/0004-6361/202245016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The geometric albedo of the hot Jupiter HD 189733b measured with CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Krenn%2C+A+F">A. F. Krenn</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Patel%2C+J+A">J. A. Patel</a>, <a href="/search/?searchtype=author&query=Carone%2C+L">L. Carone</a>, <a href="/search/?searchtype=author&query=Deleuil%2C+M">M. Deleuil</a>, <a href="/search/?searchtype=author&query=Sulis%2C+S">S. Sulis</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Guterman%2C+P">P. Guterman</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">D. Queloz</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Heng%2C+K">K. Heng</a>, <a href="/search/?searchtype=author&query=Akinsanmi%2C+B">B. Akinsanmi</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Kitzmann%2C+D">D. Kitzmann</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a> , et al. (62 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.07731v2-abstract-short" style="display: inline;"> Context. Measurements of the occultation of an exoplanet at visible wavelengths allow us to determine the reflective properties of a planetary atmosphere. The observed occultation depth can be translated into a geometric albedo. This in turn aids in characterising the structure and composition of an atmosphere by providing additional information on the wavelength-dependent reflective qualities of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07731v2-abstract-full').style.display = 'inline'; document.getElementById('2301.07731v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07731v2-abstract-full" style="display: none;"> Context. Measurements of the occultation of an exoplanet at visible wavelengths allow us to determine the reflective properties of a planetary atmosphere. The observed occultation depth can be translated into a geometric albedo. This in turn aids in characterising the structure and composition of an atmosphere by providing additional information on the wavelength-dependent reflective qualities of the aerosols in the atmosphere. Aims. Our aim is to provide a precise measurement of the geometric albedo of the gas giant HD 189733b by measuring the occultation depth in the broad optical bandpass of CHEOPS (350 - 1100 nm). Methods. We analysed 13 observations of the occultation of HD 189733b performed by CHEOPS utilising the Python package PyCHEOPS. The resulting occultation depth is then used to infer the geometric albedo accounting for the contribution of thermal emission from the planet. We also aid the analysis by refining the transit parameters combining observations made by the TESS and CHEOPS space telescopes. Results. We report the detection of an $24.7 \pm 4.5$ ppm occultation in the CHEOPS observations. This occultation depth corresponds to a geometric albedo of $0.076 \pm 0.016$. Our measurement is consistent with models assuming the atmosphere of the planet to be cloud-free at the scattering level and absorption in the CHEOPS band to be dominated by the resonant Na doublet. Taking into account previous optical-light occultation observations obtained with the Hubble Space Telescope, both measurements combined are consistent with a super-stellar Na elemental abundance in the dayside atmosphere of HD 189733b. We further constrain the planetary Bond albedo to between 0.013 and 0.42 at 3$蟽$ confidence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07731v2-abstract-full').style.display = 'none'; document.getElementById('2301.07731v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 10 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A24 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07418">arXiv:2301.07418</a> <span> [<a href="https://arxiv.org/pdf/2301.07418">pdf</a>, <a href="https://arxiv.org/format/2301.07418">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245104">10.1051/0004-6361/202245104 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hint of an exocomet transit in the CHEOPS lightcurve of HD 172555 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kiefer%2C+F">F. Kiefer</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Etangs%2C+A+L+d">A. Lecavelier des Etangs</a>, <a href="/search/?searchtype=author&query=Szab%C3%B3%2C+G+M">Gy. M. Szab贸</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=H%C3%A9brard%2C+G">G. H茅brard</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Bonfils%2C+X">X. Bonfils</a> , et al. (50 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.07418v1-abstract-short" style="display: inline;"> HD$\,$172555 is a young ($\sim$20$\,$Myr) A7V star surrounded by a 10$\,$au wide debris disk suspected to be replenished partly by collisions between large planetesimals. Small evaporating transiting bodies, exocomets, have also been detected in this system by spectroscopy. After $尾\,$Pictoris, this is another example of a system possibly witnessing a phase of heavy bombardment of planetesimals. I… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07418v1-abstract-full').style.display = 'inline'; document.getElementById('2301.07418v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07418v1-abstract-full" style="display: none;"> HD$\,$172555 is a young ($\sim$20$\,$Myr) A7V star surrounded by a 10$\,$au wide debris disk suspected to be replenished partly by collisions between large planetesimals. Small evaporating transiting bodies, exocomets, have also been detected in this system by spectroscopy. After $尾\,$Pictoris, this is another example of a system possibly witnessing a phase of heavy bombardment of planetesimals. In such system, small bodies trace dynamical evolution processes. We aim at constraining their dust content by using transit photometry. We performed a 2-day-long photometric monitoring of HD$\,$172555 with the CHEOPS space telescope in order to detect shallow transits of exocomets with a typical expected duration of a few hours. The large oscillations in the lightcurve indicate that HD$\,$172555 is a $未\,$Scuti pulsating star. Once removing those dominating oscillations, we find a hint for a transient absorption. If fitted with an exocomet transit model, it corresponds to an evaporating body passing near the star at a distance of $6.8\pm1.4\,$R$_\star$ (or $0.05\pm 0.01\,$au) with a radius of 2.5 km. These properties are comparable to those of the exocomets already found in this system using spectroscopy, as well as those found in the $尾\,$Pic system. The nuclei of solar system's Jupiter family comets, with radii of 2-6$\,$km, are also comparable in size. This is the first evidence for an exocomet photometric transit detection in the young system of HD$\,$172555. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07418v1-abstract-full').style.display = 'none'; document.getElementById('2301.07418v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures, 5 tables, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A25 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.04307">arXiv:2212.04307</a> <span> [<a href="https://arxiv.org/pdf/2212.04307">pdf</a>, <a href="https://arxiv.org/format/2212.04307">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac3639">10.1093/mnras/stac3639 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of TOI-1260d and the characterisation of the multi-planet system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lam%2C+K+W+F">Kristine W. F. Lam</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+.+G">T . G. Wilson</a>, <a href="/search/?searchtype=author&query=Georgieva%2C+I+Y">I. Y. Georgieva</a>, <a href="/search/?searchtype=author&query=Nowak%2C+G">Gr. Nowak</a>, <a href="/search/?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Alonso%2C+V+A+R">V. Adibekyan R. Alonso</a>, <a href="/search/?searchtype=author&query=Escud%C3%A9%2C+G+A">G. Anglada Escud茅</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a> , et al. (61 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.04307v1-abstract-short" style="display: inline;"> We report the discovery of a third planet transiting the star TOI-1260, previously known to host two transiting sub-Neptune planets with orbital periods of 3.127 and 7.493 days, respectively. The nature of the third transiting planet with a 16.6-day orbit is supported by ground-based follow-up observations, including time-series photometry, high-angular resolution images, spectroscopy, and archiva… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.04307v1-abstract-full').style.display = 'inline'; document.getElementById('2212.04307v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.04307v1-abstract-full" style="display: none;"> We report the discovery of a third planet transiting the star TOI-1260, previously known to host two transiting sub-Neptune planets with orbital periods of 3.127 and 7.493 days, respectively. The nature of the third transiting planet with a 16.6-day orbit is supported by ground-based follow-up observations, including time-series photometry, high-angular resolution images, spectroscopy, and archival imagery. Precise photometric monitoring with CHEOPS allows to improve the constraints on the parameters of the system, improving our knowledge on their composition. The improved radii of TOI-1260b, TOI-1260c are $2.36 \pm 0.06 \rm R_{\oplus}$, $2.82 \pm 0.08 \rm R_{\oplus}$, respectively while the newly discovered third planet has a radius of $3.09 \pm 0.09 \rm R_{\oplus}$. The radius uncertainties are in the range of 3\%, allowing a precise interpretation of the interior structure of the three planets. Our planet interior composition model suggests that all three planets in the TOI-1260 system contains some fraction of gas. The innermost planet TOI-1260b has most likely lost all of its primordial hydrogen-dominated envelope. Planets c and d were also likely to have experienced significant loss of atmospheric through escape, but to a lesser extent compared to planet b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.04307v1-abstract-full').style.display = 'none'; document.getElementById('2212.04307v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 10 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.14398">arXiv:2211.14398</a> <span> [<a href="https://arxiv.org/pdf/2211.14398">pdf</a>, <a href="https://arxiv.org/format/2211.14398">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244223">10.1051/0004-6361/202244223 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sulis%2C+S">S. Sulis</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Cegla%2C+H">H. Cegla</a>, <a href="/search/?searchtype=author&query=Diaz%2C+L+F+R">L. F. Rodriguez Diaz</a>, <a href="/search/?searchtype=author&query=Bigot%2C+L">L. Bigot</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Lovis%2C+C">C. Lovis</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Krenn%2C+A">A. Krenn</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Santerne%2C+A">A. Santerne</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a> , et al. (61 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.14398v2-abstract-short" style="display: inline;"> Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. In this study, we aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. For the first time, we observed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14398v2-abstract-full').style.display = 'inline'; document.getElementById('2211.14398v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.14398v2-abstract-full" style="display: none;"> Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. In this study, we aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. For the first time, we observed two bright stars (Teff = 5833 K and 6205 K) with high-precision observations taken simultaneously with CHEOPS and ESPRESSO. We analyzed the properties of the stellar granulation signal in each individual data set. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. The signature of stellar granulation is detected and precisely characterized for the hotter F star in the CHEOPS and ESPRESSO observations. For the cooler G star, we obtain a clear detection in the CHEOPS dataset only. The TESS observations are blind to this stellar signal. Based on CHEOPS observations, we show that the inferred properties of stellar granulation are in agreement with both Kepler observations and hydrodynamic models. Comparing their periodograms, we observe a strong link between spectroscopic and photometric observables. Correlations of this stellar signal in the time domain (flux vs RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to signal-to-noise dependent variations. In the context of the upcoming PLATO mission and the extreme precision RV surveys, a thorough understanding of the properties of the stellar granulation signal is needed. The CHEOPS and ESPRESSO observations pave the way for detailed analyses of this stellar process. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14398v2-abstract-full').style.display = 'none'; document.getElementById('2211.14398v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to A&A, 30 pages, 21 figures, 10 tables (one online)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 670, A24 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.05646">arXiv:2211.05646</a> <span> [<a href="https://arxiv.org/pdf/2211.05646">pdf</a>, <a href="https://arxiv.org/format/2211.05646">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244529">10.1051/0004-6361/202244529 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Examining the orbital decay targets KELT-9 b, KELT-16 b and WASP-4 b, and the transit-timing variations of HD 97658 b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Harre%2C+J+-">J. -V. Harre</a>, <a href="/search/?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Bou%C3%A9%2C+G">G. Bou茅</a>, <a href="/search/?searchtype=author&query=Csizmadia%2C+S">Sz. Csizmadia</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">A. Fortier</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Akinsanmi%2C+B">B. Akinsanmi</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Ros%C3%A1rio%2C+N+M">N. M. Ros谩rio</a>, <a href="/search/?searchtype=author&query=Demory%2C+B+-">B. -O. Demory</a>, <a href="/search/?searchtype=author&query=Jones%2C+K">K. Jones</a>, <a href="/search/?searchtype=author&query=Laskar%2C+J">J. Laskar</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anderson%2C+D+R">D. R. Anderson</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B+y">D. Barrado y Navascues</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.05646v1-abstract-short" style="display: inline;"> Tidal orbital decay is suspected to occur especially for hot Jupiters, with the only observationally confirmed case of this being WASP-12 b. By examining this effect, information on the properties of the host star can be obtained using the so-called stellar modified tidal quality factor $Q_*'$, which describes the efficiency with which kinetic energy of the planet is dissipated within the star. Th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.05646v1-abstract-full').style.display = 'inline'; document.getElementById('2211.05646v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.05646v1-abstract-full" style="display: none;"> Tidal orbital decay is suspected to occur especially for hot Jupiters, with the only observationally confirmed case of this being WASP-12 b. By examining this effect, information on the properties of the host star can be obtained using the so-called stellar modified tidal quality factor $Q_*'$, which describes the efficiency with which kinetic energy of the planet is dissipated within the star. This can help to get information about the interior of the star. In this study, we aim to improve constraints on the tidal decay of the KELT-9, KELT-16 and WASP-4 systems, to find evidence for or against the presence of this particular effect. With this, we want to constrain each star's respective $Q_*'$ value. In addition to that, we also aim to test the existence of the transit timing variations (TTVs) in the HD 97658 system, which previously favoured a quadratic trend with increasing orbital period. Making use of newly acquired photometric observations from CHEOPS and TESS, combined with archival transit and occultation data, we use Markov chain Monte Carlo (MCMC) algorithms to fit three models, a constant period model, an orbital decay model, and an apsidal precession model, to the data. We find that the KELT-9 system is best described by an apsidal precession model for now, with an orbital decay trend at over 2 $蟽$ being a possible solution as well. A Keplerian orbit model with a constant orbital period fits the transit timings of KELT-16 b the best due to the scatter and scale of their error bars. The WASP-4 system is represented the best by an orbital decay model at a 5 $蟽$ significance, although apsidal precession cannot be ruled out with the present data. For HD 97658 b, using recently acquired transit observations, we find no conclusive evidence for a previously suspected strong quadratic trend in the data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.05646v1-abstract-full').style.display = 'none'; document.getElementById('2211.05646v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 11 figures, 9 tables, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 669, A124 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.03582">arXiv:2211.03582</a> <span> [<a href="https://arxiv.org/pdf/2211.03582">pdf</a>, <a href="https://arxiv.org/format/2211.03582">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244894">10.1051/0004-6361/202244894 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 55 Cancri e's occultation captured with CHEOPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Demory%2C+B+-">B. -O. Demory</a>, <a href="/search/?searchtype=author&query=Sulis%2C+S">S. Sulis</a>, <a href="/search/?searchtype=author&query=Valdes%2C+E+M">E. Meier Valdes</a>, <a href="/search/?searchtype=author&query=Delrez%2C+L">L. Delrez</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Fortier%2C+A">A. Fortier</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Heng%2C+K">K. Heng</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Krenn%2C+A">A. Krenn</a>, <a href="/search/?searchtype=author&query=Morris%2C+B+M">B. M. Morris</a>, <a href="/search/?searchtype=author&query=Patel%2C+J+A">J. A. Patel</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Barczy%2C+T">T. Barczy</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Bonfils%2C+X">X. Bonfils</a> , et al. (51 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.03582v1-abstract-short" style="display: inline;"> Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e's occultation with an average d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03582v1-abstract-full').style.display = 'inline'; document.getElementById('2211.03582v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.03582v1-abstract-full" style="display: none;"> Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e's occultation with an average depth of $12\pm3$ ppm. We derive a corresponding 2-$蟽$ upper limit on the geometric albedo of $A_g < 0.55$ once decontaminated from the thermal emission measured by Spitzer at 4.5$渭$m. CHEOPS's photometric performance enables, for the first time, the detection of individual occultations of this super-Earth in the visible and identifies short-timescale photometric corrugations likely induced by stellar granulation. We also find a clear 47.3-day sinusoidal pattern in the time-dependent occultation depths that we are unable to relate to stellar noise, nor instrumental systematics, but whose planetary origin could be tested with upcoming JWST occultation observations of this iconic super-Earth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03582v1-abstract-full').style.display = 'none'; document.getElementById('2211.03582v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">In press. Accepted for publication in Astronomy and Astrophysics on 13 October 2022. 10 pages, 7 figures and 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 669, A64 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.08912">arXiv:2210.08912</a> <span> [<a href="https://arxiv.org/pdf/2210.08912">pdf</a>, <a href="https://arxiv.org/format/2210.08912">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243720">10.1051/0004-6361/202243720 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the HD 108236 system with CHEOPS and TESS. Confirmation of a fifth transiting planet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Leleu%2C+A">A. Leleu</a>, <a href="/search/?searchtype=author&query=Acu%C3%B1a%2C+L">L. Acu帽a</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Deleuil%2C+M">M. Deleuil</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Floren%2C+H+-">H. -G. Floren</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">D. Queloz</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.08912v1-abstract-short" style="display: inline;"> The HD108236 system was first announced with the detection of four small planets based on TESS data. Shortly after, the transit of an additional planet with a period of 29.54d was serendipitously detected by CHEOPS. In this way, HD108236 (V=9.2) became one of the brightest stars known to host five small transiting planets (R$_p$<3R$_{\oplus}$). We characterize the planetary system by using all the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08912v1-abstract-full').style.display = 'inline'; document.getElementById('2210.08912v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.08912v1-abstract-full" style="display: none;"> The HD108236 system was first announced with the detection of four small planets based on TESS data. Shortly after, the transit of an additional planet with a period of 29.54d was serendipitously detected by CHEOPS. In this way, HD108236 (V=9.2) became one of the brightest stars known to host five small transiting planets (R$_p$<3R$_{\oplus}$). We characterize the planetary system by using all the data available from CHEOPS and TESS space missions. We use the flexible pointing capabilities of CHEOPS to follow up the transits of all the planets in the system, including the fifth transiting body. After updating the host star parameters by using the results from Gaia eDR3, we analyzed 16 and 43 transits observed by CHEOPS and TESS, respectively, to derive the planets physical and orbital parameters. We carried out a timing analysis of the transits of each of the planets of HD108236 to search for the presence of transit timing variations. We derived improved values for the radius and mass of the host star (R$_{\star}$=0.876$\pm$0.007 R$_{\odot}$ and M$_{\star}$=0.867$_{-0.046}^{+0.047}$ M$_{\odot}$). We confirm the presence of the fifth transiting planet f in a 29.54d orbit. Thus, the system consists of five planets of R$_b$=1.587$\pm$0.028, R$_c$=2.122$\pm$0.025, R$_d$=2.629$\pm$0.031, R$_e$=3.008$\pm$0.032, and R$_f$=1.89$\pm$0.04 [R$_{\oplus}$]. We refine the transit ephemeris for each planet and find no significant transit timing variations for planets c, d, and e. For planets b and f, instead, we measure significant deviations on their transit times (up to 22 and 28 min, respectively) with a non-negligible dispersion of 9.6 and 12.6 min in their time residuals. We confirm the presence of planet f and find no significant evidence for a potential transiting planet in a 10.9d orbital period, as previously suggested. Full abstract in the PDF file. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08912v1-abstract-full').style.display = 'none'; document.getElementById('2210.08912v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 Figures and 25 pages. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A117 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.06937">arXiv:2209.06937</a> <span> [<a href="https://arxiv.org/pdf/2209.06937">pdf</a>, <a href="https://arxiv.org/format/2209.06937">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243778">10.1051/0004-6361/202243778 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A CHEOPS-enhanced view of the HD3167 system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bourrier%2C+V">V. Bourrier</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Krenn%2C+A">A. Krenn</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Petit%2C+A+C">A. C. Petit</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Cretignier%2C+M">M. Cretignier</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+-">H. -G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Queloz%2C+D">D. Queloz</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Delisle%2C+J+-">J. -B. Delisle</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Demory%2C+B+-">B. -O. Demory</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/?searchtype=author&query=Howell%2C+S+B">S. B Howell</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Mortier%2C+A">A. Mortier</a>, <a href="/search/?searchtype=author&query=Nigro%2C+G">G. Nigro</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a> , et al. (70 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.06937v2-abstract-short" style="display: inline;"> Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmosphe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06937v2-abstract-full').style.display = 'inline'; document.getElementById('2209.06937v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.06937v2-abstract-full" style="display: none;"> Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD\,3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD3167 system, which remains a target of choice for follow-up observations and simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06937v2-abstract-full').style.display = 'none'; document.getElementById('2209.06937v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 23 pages, accepted for publication in A&A (18 August 2022). Updated author list in new version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.05303">arXiv:2209.05303</a> <span> [<a href="https://arxiv.org/pdf/2209.05303">pdf</a>, <a href="https://arxiv.org/format/2209.05303">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243974">10.1051/0004-6361/202243974 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The phase curve and the geometric albedo of WASP-43b measured with CHEOPS, TESS and HST WFC3/UVIS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Kitzmann%2C+D">D. Kitzmann</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/?searchtype=author&query=Bekkelien%2C+A">A. Bekkelien</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Gutermann%2C+P">P. Gutermann</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Charnoz%2C+S">S. Charnoz</a>, <a href="/search/?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/?searchtype=author&query=Heng%2C+K">K. Heng</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Pagano%2C+I">I. Pagano</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=Bergomi%2C+M">M. Bergomi</a>, <a href="/search/?searchtype=author&query=Gambicorti%2C+L">L. Gambicorti</a>, <a href="/search/?searchtype=author&query=Hasiba%2C+J">J. Hasiba</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a> , et al. (57 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.05303v1-abstract-short" style="display: inline;"> Observations of the phase curves and secondary eclipses of extrasolar planets provide a window on the composition and thermal structure of the planetary atmospheres. For example, the photometric observations of secondary eclipses lead to the measurement of the planetary geometric albedo $A_g$, which is an indicator of the presence of clouds in the atmosphere. In this work we aim to measure the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05303v1-abstract-full').style.display = 'inline'; document.getElementById('2209.05303v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.05303v1-abstract-full" style="display: none;"> Observations of the phase curves and secondary eclipses of extrasolar planets provide a window on the composition and thermal structure of the planetary atmospheres. For example, the photometric observations of secondary eclipses lead to the measurement of the planetary geometric albedo $A_g$, which is an indicator of the presence of clouds in the atmosphere. In this work we aim to measure the $A_g$ in the optical domain of WASP-43b, a moderately irradiated giant planet with an equilibrium temperature of $\sim$1400~K. To this purpose, we analyze the secondary eclipse light curves collected by CHEOPS, together with TESS observations of the system and the publicly available photometry obtained with HST WFC3/UVIS. We also analyze the archival infrared observations of the eclipses and retrieve the thermal emission spectrum of the planet. By extrapolating the thermal spectrum to the optical bands, we correct the optical eclipses for thermal emission and derive the optical $A_g$. The fit of the optical data leads to a marginal detection of the phase curve signal, characterized by an amplitude of $160\pm60$~ppm and 80$^{+60}_{-50}$~ppm in the CHEOPS and TESS passband respectively, with an eastward phase shift of $\sim50^\circ$ (1.5$蟽$ detection). The analysis of the infrared data suggests a non-inverted thermal profile and solar-like metallicity. The combination of optical and infrared analysis allows us to derive an upper limit for the optical albedo of $A_g<0.087$ with a confidence of 99.9\%. Our analysis of the atmosphere of WASP-43b places this planet in the sample of irradiated hot Jupiters, with monotonic temperature-pressure profile and no indication of condensation of reflective clouds on the planetary dayside. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05303v1-abstract-full').style.display = 'none'; document.getElementById('2209.05303v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A17 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.03890">arXiv:2209.03890</a> <span> [<a href="https://arxiv.org/pdf/2209.03890">pdf</a>, <a href="https://arxiv.org/format/2209.03890">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244117">10.1051/0004-6361/202244117 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CHEOPS finds KELT-1b darker than expected in visible light: Discrepancy between the CHEOPS and TESS eclipse depths </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Parviainen%2C+H">H. Parviainen</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Kitzmann%2C+D">D. Kitzmann</a>, <a href="/search/?searchtype=author&query=Pall%C3%A9%2C+E">E. Pall茅</a>, <a href="/search/?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</a>, <a href="/search/?searchtype=author&query=Valdes%2C+E+M">E. Meier Valdes</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Deline%2C+A">A. Deline</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=Guterman%2C+P">P. Guterman</a>, <a href="/search/?searchtype=author&query=Heng%2C+K">K. Heng</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B+y">D. Barrado y Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a> , et al. (56 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.03890v1-abstract-short" style="display: inline;"> Recent TESS-based studies have suggested that the dayside of KELT-1b, a strongly-irradiated brown dwarf, is significantly brighter in visible light than what would be expected based on Spitzer observations in infrared. We observe eight eclipses of KELT-1b with CHEOPS (CHaracterising ExOPlanet Satellite) to measure its dayside brightness temperature in the bluest passband observed so far, and model… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03890v1-abstract-full').style.display = 'inline'; document.getElementById('2209.03890v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.03890v1-abstract-full" style="display: none;"> Recent TESS-based studies have suggested that the dayside of KELT-1b, a strongly-irradiated brown dwarf, is significantly brighter in visible light than what would be expected based on Spitzer observations in infrared. We observe eight eclipses of KELT-1b with CHEOPS (CHaracterising ExOPlanet Satellite) to measure its dayside brightness temperature in the bluest passband observed so far, and model the CHEOPS photometry jointly with the existing optical and NIR photometry from TESS, LBT, CFHT, and Spitzer. Our modelling leads to a self-consistent dayside spectrum for KELT-1b covering the CHEOPS, TESS, H , Ks, and Spitzer IRAC 3.6 and 4.5 $渭$m bands, where our TESS, H , Ks, and Spitzer band estimates largely agree with the previous studies, but we discover a strong discrepancy between the CHEOPS and TESS bands. The CHEOPS observations yield a higher photometric precision than the TESS observations, but do not show a significant eclipse signal, while a deep eclipse is detected in the TESS band. The derived TESS geometric albedo of $0.36^{+0.12}_{-0.13}$ is difficult to reconcile with a CHEOPS geometric albedo that is consistent with zero because the two passbands have considerable overlap. Variability in cloud cover caused by the transport of transient nightside clouds to the dayside could provide an explanation for reconciling the TESS and CHEOPS geometric albedos, but this hypothesis needs to be tested by future observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03890v1-abstract-full').style.display = 'none'; document.getElementById('2209.03890v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A93 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.03128">arXiv:2209.03128</a> <span> [<a href="https://arxiv.org/pdf/2209.03128">pdf</a>, <a href="https://arxiv.org/format/2209.03128">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac2565">10.1093/mnras/stac2565 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The EBLM project -- IX. Five fully convective M-dwarfs, precisely measured with CHEOPS and TESS light curves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sebastian%2C+D">D. Sebastian</a>, <a href="/search/?searchtype=author&query=Swayne%2C+M+I">M. I. Swayne</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Triaud%2C+A+H+M+J">A. H. M. J. Triaud</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Gill%2C+S">S. Gill</a>, <a href="/search/?searchtype=author&query=Heidari%2C+N">N. Heidari</a>, <a href="/search/?searchtype=author&query=Martin%2C+D+V">D. V. Martin</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Standing%2C+M+R">M. R. Standing</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=Anglada%2C+G">G. Anglada</a>, <a href="/search/?searchtype=author&query=Asquier%2C+J">J. Asquier</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Battley%2C+M+P">M. P. Battley</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.03128v1-abstract-short" style="display: inline;"> Eclipsing binaries are important benchmark objects to test and calibrate stellar structure and evolution models. This is especially true for binaries with a fully convective M-dwarf component for which direct measurements of these stars' masses and radii are difficult using other techniques. Within the potential of M-dwarfs to be exoplanet host stars, the accuracy of theoretical predictions of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03128v1-abstract-full').style.display = 'inline'; document.getElementById('2209.03128v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.03128v1-abstract-full" style="display: none;"> Eclipsing binaries are important benchmark objects to test and calibrate stellar structure and evolution models. This is especially true for binaries with a fully convective M-dwarf component for which direct measurements of these stars' masses and radii are difficult using other techniques. Within the potential of M-dwarfs to be exoplanet host stars, the accuracy of theoretical predictions of their radius and effective temperature as a function of their mass is an active topic of discussion. Not only the parameters of transiting exoplanets but also the success of future atmospheric characterisation rely on accurate theoretical predictions. We present the analysis of five eclipsing binaries with low-mass stellar companions out of a sub-sample of 23, for which we obtained ultra high-precision light curves using the CHEOPS satellite. The observation of their primary and secondary eclipses are combined with spectroscopic measurements to precisely model the primary parameters and derive the M-dwarfs mass, radius, surface gravity, and effective temperature estimates using the PYCHEOPS data analysis software. Combining these results to the same set of parameters derived from TESS light curves, we find very good agreement (better than 1\% for radius and better than 0.2% for surface gravity). We also analyse the importance of precise orbits from radial velocity measurements and find them to be crucial to derive M-dwarf radii in a regime below 5% accuracy. These results add five valuable data points to the mass-radius diagram of fully-convective M-dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03128v1-abstract-full').style.display = 'none'; document.getElementById('2209.03128v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 12 figures, accepted for publication in MNRAS</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a 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