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breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Bonomo%2C+A+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Bonomo%2C+A+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Bonomo%2C+A+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Bonomo%2C+A+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Bonomo%2C+A+S&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <ol 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/2502.07996">arXiv:2502.07996</a> <span> [<a href="https://arxiv.org/pdf/2502.07996">pdf</a>, <a href="https://arxiv.org/format/2502.07996">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> <p class="title is-5 mathjax"> In-depth characterization of the Kepler-10 three-planet system with HARPS-N RVs and Kepler TTVs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Rajpaul%2C+V+M">V. M. Rajpaul</a>, <a href="/search/?searchtype=author&query=Zeng%2C+L">L. Zeng</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Hara%2C+N+C">N. C. Hara</a>, <a href="/search/?searchtype=author&query=Cretignier%2C+M">M. Cretignier</a>, <a href="/search/?searchtype=author&query=Leleu%2C+A">A. Leleu</a>, <a href="/search/?searchtype=author&query=Unger%2C+N">N. Unger</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/?searchtype=author&query=Lienhard%2C+F">F. Lienhard</a>, <a href="/search/?searchtype=author&query=Mortier%2C+A">A. Mortier</a>, <a href="/search/?searchtype=author&query=Naponiello%2C+L">L. Naponiello</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">D. W. Latham</a>, <a href="/search/?searchtype=author&query=Rice%2C+K">K. Rice</a>, <a href="/search/?searchtype=author&query=Bongiolatti%2C+R">R. Bongiolatti</a>, <a href="/search/?searchtype=author&query=Buchhave%2C+L">L. Buchhave</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. C. Cameron</a>, <a href="/search/?searchtype=author&query=Fiorenzano%2C+A+F">A. F. Fiorenzano</a>, <a href="/search/?searchtype=author&query=Ghedina%2C+A">A. Ghedina</a>, <a href="/search/?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/?searchtype=author&query=Lacedelli%2C+G">G. Lacedelli</a>, <a href="/search/?searchtype=author&query=Massa%2C+A">A. Massa</a> , et al. (3 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="2502.07996v1-abstract-short" style="display: inline;"> The old G3V star Kepler-10 is known to host two transiting planets, the ultra-short-period super-Earth Kepler-10b ($P=0.837$ d; $R_{\rm p}=1.47~\rm R_\oplus$) and the long-period sub-Neptune Kepler-10c ($P=45.294$ d; $R_{\rm p}=2.35~\rm R_\oplus$), and a non-transiting planet causing variations in the Kepler-10c transit times. Measurements of the mass of Kepler-10c in the literature have shown dis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07996v1-abstract-full').style.display = 'inline'; document.getElementById('2502.07996v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.07996v1-abstract-full" style="display: none;"> The old G3V star Kepler-10 is known to host two transiting planets, the ultra-short-period super-Earth Kepler-10b ($P=0.837$ d; $R_{\rm p}=1.47~\rm R_\oplus$) and the long-period sub-Neptune Kepler-10c ($P=45.294$ d; $R_{\rm p}=2.35~\rm R_\oplus$), and a non-transiting planet causing variations in the Kepler-10c transit times. Measurements of the mass of Kepler-10c in the literature have shown disagreement, depending on the radial-velocity dataset and/or the modeling technique used. Here we report on the analysis of almost 300 high-precision radial velocities gathered with the HARPS-N spectrograph at the Telescopio Nazionale Galileo over $\sim11$~years, and extracted with the YARARA-v2 tool correcting for possible systematics and/or low-level activity variations at the spectrum level. To model these radial velocities, we used three different noise models and various numerical techniques, which all converged to the solution: $M_{\rm p, b}=3.24 \pm 0.32~\rm M_\oplus$ (10$蟽$) and $蟻_{\rm p, b}=5.54 \pm 0.64~\rm g\;cm^{-3}$ for planet b; $M_{\rm p, c}=11.29 \pm 1.24~\rm M_\oplus$ (9$蟽$) and $蟻_{\rm p, c}=4.75 \pm 0.53~\rm g\;cm^{-3}$ for planet c; and $M_{\rm p, d}\sin{i}=12.00 \pm 2.15~\rm M_\oplus$ (6$蟽$) and $P=151.06 \pm 0.48$ d for the non-transiting planet Kepler-10d. This solution is further supported by the analysis of the Kepler-10c transit timing variations and their simultaneous modeling with the HARPS-N radial velocities. While Kepler-10b is consistent with a rocky composition and a small or no iron core, Kepler-10c may be a water world that formed beyond the water snowline and subsequently migrated inward. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07996v1-abstract-full').style.display = 'none'; document.getElementById('2502.07996v1-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">15 pages, 12 figures, 5 tables, 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/2502.05056">arXiv:2502.05056</a> <span> [<a href="https://arxiv.org/pdf/2502.05056">pdf</a>, <a href="https://arxiv.org/format/2502.05056">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 GAPS Programme at TNG LXVII. Detection of water and preliminary characterisation of the atmospheres of the two hot Jupiters KELT-8 b and KELT-23 Ab </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Basilicata%2C+M">M. Basilicata</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=Amadori%2C+F">F. Amadori</a>, <a href="/search/?searchtype=author&query=Pacetti%2C+E">E. Pacetti</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Turrini%2C+D">D. Turrini</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Andreuzzi%2C+G">G. Andreuzzi</a>, <a href="/search/?searchtype=author&query=Boschin%2C+W">W. Boschin</a>, <a href="/search/?searchtype=author&query=Cabona%2C+L">L. Cabona</a>, <a href="/search/?searchtype=author&query=Colombo%2C+S">S. Colombo</a>, <a href="/search/?searchtype=author&query=D%27Arpa%2C+M+C">M. C. D'Arpa</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Manni%2C+F">F. Manni</a>, <a href="/search/?searchtype=author&query=Naponiello%2C+L">L. Naponiello</a>, <a href="/search/?searchtype=author&query=Pinamonti%2C+M">M. Pinamonti</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a> </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="2502.05056v1-abstract-short" style="display: inline;"> Expanding the number of hot giant planets with atmospheric characterisation can improve our understanding of their atmospheres as well as their formation and evolution mechanisms. In this work, we use high-resolution spectroscopy in the near-infrared (NIR) to search for chemical signatures in the atmospheres of the two hot Jupiters KELT-8 b and KELT-23 Ab, and perform a first characterisation of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.05056v1-abstract-full').style.display = 'inline'; document.getElementById('2502.05056v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.05056v1-abstract-full" style="display: none;"> Expanding the number of hot giant planets with atmospheric characterisation can improve our understanding of their atmospheres as well as their formation and evolution mechanisms. In this work, we use high-resolution spectroscopy in the near-infrared (NIR) to search for chemical signatures in the atmospheres of the two hot Jupiters KELT-8 b and KELT-23 Ab, and perform a first characterisation of their atmospheric properties. We measured the transmission spectrum of each target with the NIR high-resolution spectrograph GIANO-B at the TNG and searched for atmospheric signals by cross-correlating the data with synthetic transmission spectra. In order to characterise the chemical-physical properties of the two atmospheres, we ran two different atmospheric retrievals for each dataset: a retrieval assuming chemical equilibrium and a ``free-chemistry'' retrieval, in which the abundance of each molecule could vary freely. We detect $H_2O$ in the atmospheres of KELT-8 b and KELT-23 Ab with an S/N = 6.6 and S/N = 4.2, respectively. The two retrievals indicate a water-rich atmosphere for both targets. For KELT-8 b, we determine a water volume mixing ratio of log$_{10}$(VMR$_{\rm H_2O})=-2.07^{+0.53}_{-0.72}$, a metallicity [M/H] $=0.77^{+0.61}_{-0.89}$ dex, and a sub-solar C/O ratio (C/O $\leq0.30$, at $2\,蟽$). For KELT-23 Ab, we find log$_{10}$(VMR$_{\rm H_2O})=-2.26^{+0.75}_{-1.24}$, [M/H] $=-0.42^{+1.56}_{-1.35}$ dex, and a C/O ratio $\leq0.78$ (at $2\,蟽$). Comparing these chemical properties with those of the host stars, we suggest that, for both planets, the accretion of gaseous material occurred within the $H_2O$ snowline in a pebble-rich disk enriched in oxygen due to sublimation of water ice from the inward-drifting pebbles. In conclusion, we measure the atmospheric signals of KELT-8 b and KELT-23 Ab for the first time and place first constraints on their properties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.05056v1-abstract-full').style.display = 'none'; document.getElementById('2502.05056v1-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 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">14 pages, 6 figures, accepted for publication in Astronomy & Astrophysics (A&A) journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.05423">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/2412.04330">arXiv:2412.04330</a> <span> [<a href="https://arxiv.org/pdf/2412.04330">pdf</a>, <a href="https://arxiv.org/format/2412.04330">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/10.1051/0004-6361/202451937">10.1051/0004-6361/202451937 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS programme at TNG LXVI. A homogeneous search for Na i and its possible variability in ten gas giant exoplanets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Biassoni%2C+F">F. Biassoni</a>, <a href="/search/?searchtype=author&query=D%27Arpa%2C+M+C">M. C. D'Arpa</a>, <a href="/search/?searchtype=author&query=Pagano%2C+I">I. Pagano</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Stangret%2C+M">M. Stangret</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Lodi%2C+M">M. Lodi</a>, <a href="/search/?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Pedani%2C+M">M. Pedani</a> </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="2412.04330v2-abstract-short" style="display: inline;"> The neutral sodium resonance doublet (Na i D) has been detected in the upper atmosphere of several close-in gas giants, through high-resolution transmission spectroscopy. We aim to investigate whether its variability is linked to the planets' properties, the data quality, or the accuracy of the system parameters used. Using the public code SLOPpy, we extracted the transmission spectrum in the Na… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04330v2-abstract-full').style.display = 'inline'; document.getElementById('2412.04330v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.04330v2-abstract-full" style="display: none;"> The neutral sodium resonance doublet (Na i D) has been detected in the upper atmosphere of several close-in gas giants, through high-resolution transmission spectroscopy. We aim to investigate whether its variability is linked to the planets' properties, the data quality, or the accuracy of the system parameters used. Using the public code SLOPpy, we extracted the transmission spectrum in the Na i D region of ten gas giants for which a large number of HARPS-N observations are available. We modelled the absorption signals found, performing an MCMC analysis, and converted the measured absorption depth to the corresponding atmospheric height over which most sodium absorption occurs. While two targets (GJ 436 b and KELT-7 b) show no Na i D feature, we found variability in the transmission spectrum of the other targets. Three of them (HD 209458 b, WASP-80 b, and WASP-127 b) present absorption on only some nights, while in the other five targets (HD 189733 b, KELT-9 b, KELT-20 b, WASP-69 b, and WASP-76 b), a significant absorption signal is present on most of the nights analysed. Except for WASP-69 b, the measured absorption depths lead to a ratio of the two Na I D depths that is compatible with or slightly larger than one. As was expected from literature, the relative atmospheric height follows an empirical exponential trend as a function of a scaled product of the planet's equilibrium temperature and surface gravity. We confirm the sodium detection on HD 189733 b, KELT-9 b, KELT-20 b, WASP-69 b, and WASP-76 b. The signal detected in WASP-127 b requires further observations for definitive confirmation. We exclude a planetary origin for the signals found on HD 209458 b and WASP-80 b. The sodium absorption variability does not appear to be related to planetary properties, but rather to data quality, sub-optimal data treatment, or stellar activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04330v2-abstract-full').style.display = 'none'; document.getElementById('2412.04330v2-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">v1</span> submitted 5 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">Accepted for publication in Astronomy & Astrophysics on 26 November 2024. Additional material (Figures B.1-B.3 and Tables B.1-B.9) are available on Zenodo</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 693, A316 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.12795">arXiv:2411.12795</a> <span> [<a href="https://arxiv.org/pdf/2411.12795">pdf</a>, <a href="https://arxiv.org/ps/2411.12795">ps</a>, <a href="https://arxiv.org/format/2411.12795">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/10.1051/0004-6361/202452236">10.1051/0004-6361/202452236 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG. LXV. Precise density measurement of TOI-1430 b, a young planet with an evaporating atmosphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Murphy%2C+J+M+A">J. M. Akana Murphy</a>, <a href="/search/?searchtype=author&query=Spinelli%2C+R">R. Spinelli</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Locci%2C+D">D. Locci</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Batalha%2C+N+M">N. M. Batalha</a>, <a href="/search/?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/?searchtype=author&query=Oelkers%2C+R+J">R. J. Oelkers</a>, <a href="/search/?searchtype=author&query=Mallonn%2C+M">M. Mallonn</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Cabona%2C+L">L. Cabona</a> , et al. (12 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="2411.12795v1-abstract-short" style="display: inline;"> Small-sized exoplanets in tight orbits around young stars (10-1000 Myr) give us the opportunity to investigate the mechanisms that led to their formation, the evolution of their physical and orbital properties and, especially, of their atmospheres. Thanks to the all-sky survey carried out by TESS, many of these exoplanets have been discovered and have subsequently been characterized with dedicated… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12795v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12795v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12795v1-abstract-full" style="display: none;"> Small-sized exoplanets in tight orbits around young stars (10-1000 Myr) give us the opportunity to investigate the mechanisms that led to their formation, the evolution of their physical and orbital properties and, especially, of their atmospheres. Thanks to the all-sky survey carried out by TESS, many of these exoplanets have been discovered and have subsequently been characterized with dedicated follow-up observations. In the context of a collaboration among the GAPS, TKS and CPS teams, we measured with a high level of precision the mass and the radius of TOI-1430 b, a young (~700 Myr) exoplanet with an escaping He atmosphere orbiting the K-dwarf star HD 235088 (TOI-1430). By adopting appropriate stellar parameters, which were measured in this work, we were able to simultaneously model the signals due to strong stellar activity and the transiting planet TOI-1430 b in both photometric and spectroscopic series. This allowed us to measure the density of the planet with high precision, and reconstruct the evolution of its atmosphere. TOI-1430 is an active K-dwarf star born 700+/-150 Myr ago and rotates in ~12 d. It hosts a mini-Neptune whose orbital period is Pb=7.434133+/-0.000004 d. Thanks to long-term monitoring of this target performed with TESS, HARPS-N, HIRES, and APF, we estimated a radius Rb=1.98+/-0.07 $R_{\oplus}$, a mass Mb=4.2+/-0.8 $M_{\oplus}$, and thus a planetary density $蟻$b=0.5+/-0.1 $蟻_{\oplus}$. TOI-1430 b is hence a low-density mini-Neptune with an extended atmosphere, at the edge of the radius gap. Because this planet is known to have an evaporating atmosphere of He, we reconstructed its atmospheric history. Our analysis supports the scenario in which, shortly after its birth, TOI-1430 b may have been super-puffy, with a radius 5x-13x and a mass 1.5x-2x that of today; in ~200 Myr from now, TOI-1430 b should lose its envelope, showing its Earth-size core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12795v1-abstract-full').style.display = 'none'; document.getElementById('2411.12795v1-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 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">30 pages, 19 figures, 8 tables. Accepted for publication in Astronomy & Astrophysics on 16 November 2024. Electronic material (tables G1-G3) will soon be available on the CDS or upon request to the first author. Abstract shortened</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 693, A32 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.09417">arXiv:2411.09417</a> <span> [<a href="https://arxiv.org/pdf/2411.09417">pdf</a>, <a href="https://arxiv.org/format/2411.09417">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/10.1051/0004-6361/202451859">10.1051/0004-6361/202451859 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS programme at TNG LXIV: An inner eccentric sub-Neptune and an outer sub-Neptune-mass candidate around BD+00 444 (TOI-2443) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Naponiello%2C+L">L. Naponiello</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Steinmeyer%2C+M+L">M. L. Steinmeyer</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Polychroni%2C+D">D. Polychroni</a>, <a href="/search/?searchtype=author&query=Dorn%2C+C">C. Dorn</a>, <a href="/search/?searchtype=author&query=Turrini%2C+D">D. Turrini</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Collins%2C+K+A">K. A. Collins</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Collins%2C+K+I">K. I. Collins</a>, <a href="/search/?searchtype=author&query=Colombo%2C+S">S. Colombo</a>, <a href="/search/?searchtype=author&query=D%27Arpa%2C+M+C">M. C. D'Arpa</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/?searchtype=author&query=Gonzalez%2C+M">M. Gonzalez</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Lorenzi%2C+V">V. Lorenzi</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=Pinamonti%2C+M">M. Pinamonti</a>, <a href="/search/?searchtype=author&query=Schwarz%2C+R+P">R. P. Schwarz</a> , et al. (3 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="2411.09417v1-abstract-short" style="display: inline;"> We examined in depth the star BD+00 444 (GJ 105.5, TOI-2443; V = 9.5 mag; d = 23.9 pc), with the aim of characterizing and confirming the planetary nature of its small companion, the planet candidate TOI-2443.01, which was discovered by TESS. We monitored BD+00 444 with the HARPS-N spectrograph for 1.5 years to search for planet-induced radial-velocity (RV) variations, and then analyzed the RV mea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09417v1-abstract-full').style.display = 'inline'; document.getElementById('2411.09417v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.09417v1-abstract-full" style="display: none;"> We examined in depth the star BD+00 444 (GJ 105.5, TOI-2443; V = 9.5 mag; d = 23.9 pc), with the aim of characterizing and confirming the planetary nature of its small companion, the planet candidate TOI-2443.01, which was discovered by TESS. We monitored BD+00 444 with the HARPS-N spectrograph for 1.5 years to search for planet-induced radial-velocity (RV) variations, and then analyzed the RV measurements jointly with TESS and ground-based photometry. We determined that the host is a quiet K5 V, and we revealed that the sub-Neptune BD+00 444 b has a radius of $R_b=2.36\pm0.05 R_{\oplus}$, a mass of $M_b=4.8\pm1.1 M_{\oplus}$ and, consequently, a rather low-density value of $蟻_b=2.00+0.49-0.45$ g cm-3, which makes it compatible with both an Earth-like rocky interior with a thin H-He atmosphere and a half-rocky, half-water composition with a small amount of H-He. Having an orbital period of about 15.67 days and an equilibrium temperature of about 519 K, BD+00 444 b has an estimated transmission spectroscopy metric of about 159, which makes it ideal for atmospheric follow-up with the JWST. Notably, it is the second most eccentric inner transiting planet, $e=0.302+0.051-0.035$, with a mass below 20 $M_{\oplus}$, among those with well-determined eccentricities. We estimated that tidal forces from the host star affect both planet b's rotation and eccentricity, and strong tidal dissipation may signal intense volcanic activity. Furthermore, our analysis suggests the presence of a sub-Neptune-mass planet candidate, BD+00 444 c, having an orbital period of $P=96.6\pm1.4$ days, and a minimum mass $M\sin{i}=9.3+1.8-2.0 M_{\oplus}$. With an equilibrium temperature of about 283 K, BD+00 444 c is right inside the habitable zone; however, this candidate necessitates further observations and stronger statistical evidence to be confirmed. [...] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09417v1-abstract-full').style.display = 'none'; document.getElementById('2411.09417v1-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> 14 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 on November 13 2024. 20 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 693, A7 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.15917">arXiv:2410.15917</a> <span> [<a href="https://arxiv.org/pdf/2410.15917">pdf</a>, <a href="https://arxiv.org/format/2410.15917">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/10.1051/0004-6361/202451237">10.1051/0004-6361/202451237 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS programme at TNG -- LXIII. Photo-evaporating puzzle: Exploring the enigmatic nature of TOI-5398 b atmospheric signal </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=D%27Arpa%2C+M+C">M. C. D'Arpa</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a>, <a href="/search/?searchtype=author&query=Biassoni%2C+F">F. Biassoni</a>, <a href="/search/?searchtype=author&query=Spinelli%2C+R">R. Spinelli</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Locci%2C+D">D. Locci</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Petralia%2C+A">A. Petralia</a>, <a href="/search/?searchtype=author&query=Di+Maio%2C+C">C. Di Maio</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Cabona%2C+L">L. Cabona</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Stangret%2C+M">M. Stangret</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Amadori%2C+F">F. Amadori</a> , et al. (4 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="2410.15917v1-abstract-short" style="display: inline;"> Atmospheric characterization is key to understanding exoplanetary systems, offering insights into the planets current and past conditions. By analyzing key lines like H alpha and the He I triplet, we can trace the evolution of planets through atmospheric photo-evaporation. While ultra-hot Jupiters have been the focus for years, attention is shifting toward smaller, colder planets, which are more c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.15917v1-abstract-full').style.display = 'inline'; document.getElementById('2410.15917v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.15917v1-abstract-full" style="display: none;"> Atmospheric characterization is key to understanding exoplanetary systems, offering insights into the planets current and past conditions. By analyzing key lines like H alpha and the He I triplet, we can trace the evolution of planets through atmospheric photo-evaporation. While ultra-hot Jupiters have been the focus for years, attention is shifting toward smaller, colder planets, which are more challenging to study due to weaker signals, requiring more precise techniques. This study aims to characterize the atmosphere of TOI-5398 b, a warm Saturn with a 10.59-day orbit around a young (650 Myr) G-type star. The system also hosts a smaller inner planet, TOI-5398 c, with a 4.77-day orbit. Both planets are ideal for atmospheric studies due to their proximity to the host star, which drives strong photo-evaporation, especially in planet b, whose high transmission spectroscopy metric (288) makes it a prime target. We analyzed data from a transit observed with the HARPS-N and GIANO-B high-resolution spectrographs, using cross-correlation and single-line analysis to search for atomic species. During this observation, planet c was also transiting, so we investigated the source of the signals. Based on photo-evaporation models, we attribute the signal mainly to planet b, which is expected to lose more mass. We detected H alpha and He I triplets, key markers of photo-evaporation, corresponding to atmospheric heights of 2.33 Rp and 1.65 Rp, respectively. The ATES models supported our observations, predicting a similar He I absorption for planet b and suggesting an He/H ratio of 1/99. Additionally, we detected an Na I doublet via single-line analysis, though cross-correlation did not reveal other atomic species. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.15917v1-abstract-full').style.display = 'none'; document.getElementById('2410.15917v1-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> 21 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">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 692, A77 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.11731">arXiv:2410.11731</a> <span> [<a href="https://arxiv.org/pdf/2410.11731">pdf</a>, <a href="https://arxiv.org/format/2410.11731">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/10.1051/0004-6361/202451277">10.1051/0004-6361/202451277 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS programme at TNG: TBD. Studies of atmospheric FeII winds in ultra-hot Jupiters KELT-9b and KELT-20b using HARPS-N spectrograph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Stangret%2C+M">M. Stangret</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=D%27Arpa%2C+M+C">M. C. D'Arpa</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Biassoni%2C+F">F. Biassoni</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Di+Maio%2C+C">C. Di Maio</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Harutyunyan%2C+A">A. Harutyunyan</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Fiorenzano%2C+A+F+M">A. F. Martinez Fiorenzano</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a> </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="2410.11731v1-abstract-short" style="display: inline;"> Ultra-hot Jupiters (UHJs) are gas giant planets orbiting close to their host star, with equilibrium temperatures exceeding 2000 K, and among the most studied planets in terms of their atmospheric composition. Thanks to a new generation of ultra-stable high-resolution spectrographs, it is possible to detect the signal from the individual lines of the species in the exoplanetary atmospheres. We empl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11731v1-abstract-full').style.display = 'inline'; document.getElementById('2410.11731v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.11731v1-abstract-full" style="display: none;"> Ultra-hot Jupiters (UHJs) are gas giant planets orbiting close to their host star, with equilibrium temperatures exceeding 2000 K, and among the most studied planets in terms of their atmospheric composition. Thanks to a new generation of ultra-stable high-resolution spectrographs, it is possible to detect the signal from the individual lines of the species in the exoplanetary atmospheres. We employed two techniques in this study. First, we used transmission spectroscopy, which involved examining the spectra around single lines of FeII. Then we carried out a set of cross-correlation studies for two UHJs: KELT-9b and KELT-20b. Both planets orbit fast-rotating stars, which resulted in the detection of the strong Rossiter-McLaughlin (RM) effect and center-to-limb variations in the transmission spectrum. These effects had to be corrected to ensure a precise analysis. Using the transmission spectroscopy method, we detected 21 single lines of FeII in the atmosphere of KELT-9b. All of the detected lines are blue-shifted, suggesting strong day-to-night side atmospheric winds. The cross-correlation method leads to the detection of the blue-shifted signal with a signal-to-noise ratio (S/N) of 13.46. Our results are in agreement with models based on non-local thermodynamical equilibrium (NLTE) effects, with a mean micro-turbulence of nu_mic = 2.73 +/- 1.5 km/s and macro-turbulence of nu_mac = 8.22 +/- 3.85 km/s. In the atmosphere of KELT-20b, we detected 17 single lines of FeII. Considering different measurements of the systemic velocity of the system, we conclude that the existence of winds in the atmosphere of KELT-20b cannot be determined conclusively. The detected signal with the cross-correlation method presents a S/N of 11.51. The results are consistent with NLTE effects, including means of nu_mic = 3.04 +/- 0.35 km/s and nu_mac = 6.76 +/- 1.17 km/s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11731v1-abstract-full').style.display = 'none'; document.getElementById('2410.11731v1-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> 15 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">38 pages, 19 Figures (39 figures in Appendix), 6 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 692, A76 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.01779">arXiv:2409.01779</a> <span> [<a href="https://arxiv.org/pdf/2409.01779">pdf</a>, <a href="https://arxiv.org/format/2409.01779">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/10.1051/0004-6361/202449341">10.1051/0004-6361/202449341 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS programme at TNG LX Atmospheric characterisation of KELT-9 b via single-line analysis: Detection of six H I Balmer lines, Na I, Ca I, Ca II, Fe I, Fe II, Mg I, Ti II, Sc II, and Cr II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=D%27Arpa%2C+M+C">M. C. D'Arpa</a>, <a href="/search/?searchtype=author&query=Saba%2C+A">A. Saba</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Di+Maio%2C+C">C. Di Maio</a>, <a href="/search/?searchtype=author&query=Stangret%2C+M">M. Stangret</a>, <a href="/search/?searchtype=author&query=Tripodo%2C+G">G. Tripodo</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=Fardella%2C+V">V. Fardella</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Spinelli%2C+R">R. Spinelli</a>, <a href="/search/?searchtype=author&query=Andreuzzi%2C+G">G. Andreuzzi</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a> , et al. (5 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="2409.01779v1-abstract-short" style="display: inline;"> We analysed six primary transits of the ultra-hot Jupiter KELT-9,b obtained with the HARPS-N high-resolution spectrograph in the context of the Global Architecture of Planetary Systems (GAPS2) project, to characterise the atmosphere via single-line analysis. We extracted the transmission spectrum of each individual line by comparing the master out-of-transit spectrum with the in-transit spectra an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.01779v1-abstract-full').style.display = 'inline'; document.getElementById('2409.01779v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.01779v1-abstract-full" style="display: none;"> We analysed six primary transits of the ultra-hot Jupiter KELT-9,b obtained with the HARPS-N high-resolution spectrograph in the context of the Global Architecture of Planetary Systems (GAPS2) project, to characterise the atmosphere via single-line analysis. We extracted the transmission spectrum of each individual line by comparing the master out-of-transit spectrum with the in-transit spectra and computing the weighted average of the tomography in the planet reference frame. We corrected for the centre-to-limb variation and the Rossiter-McLaughlin effect by modelling the region of the star disc obscured by the planet during the transit and subtracting it from the master-out spectrum. We detected all six observable lines of the Balmer series within the HARPS-N wavelength range, from H$伪$ to H$味$, with a significance exceeding 5$蟽$. We focussed on metal species, detecting Na I, Ca I, Ca II, Fe I, Fe II, Mg I, Ti II, Sc II, and Cr II lines. This is the first detection in the atmosphere of an exoplanet of H$蔚$ and H$味$ lines, as well as of individual lines of Sc II and Cr II. Our detections are supported by a comparison with published synthetic transmission spectra of KELT-9b obtained accounting for non-local thermodynamic equilibrium effects. The results underline the presence of a systematic blueshift due to night-side to day-side winds. The single-line analysis allowed us not only to assess the presence of atomic species in the atmosphere of KELT-9 b, but also to further characterise the local stratification of the atmosphere. Coupling the height distribution of the detected species with the velocity shift retrieved, we acknowledged the height distribution of night-side to day-side winds. Moreover, the study of the rotational broadening of different species supports the prediction of a tidally locked planet rotating as a rigid body. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.01779v1-abstract-full').style.display = 'none'; document.getElementById('2409.01779v1-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 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 690, A237 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.00675">arXiv:2409.00675</a> <span> [<a href="https://arxiv.org/pdf/2409.00675">pdf</a>, <a href="https://arxiv.org/ps/2409.00675">ps</a>, <a href="https://arxiv.org/format/2409.00675">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 GAPS Programme at TNG. LXI. Atmospheric parameters and elemental abundances of TESS young exoplanet host stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Filomeno%2C+S">S. Filomeno</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Messina%2C+S">S. Messina</a>, <a href="/search/?searchtype=author&query=Polychroni%2C+D">D. Polychroni</a>, <a href="/search/?searchtype=author&query=Turrini%2C+D">D. Turrini</a>, <a href="/search/?searchtype=author&query=Cabona%2C+L">L. Cabona</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</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=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Andreuzzi%2C+G">G. Andreuzzi</a>, <a href="/search/?searchtype=author&query=Antoniucci%2C+S">S. Antoniucci</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a> , et al. (4 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="2409.00675v1-abstract-short" style="display: inline;"> The study of exoplanets at different evolutionary stages can shed light on their formation, migration, and evolution. The determination of exoplanet properties depends on the properties of their host stars. It is therefore important to characterise the host stars for accurate knowledge on their planets. Our final goal is to derive, in a homogeneous and accurate way, the stellar atmospheric paramet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.00675v1-abstract-full').style.display = 'inline'; document.getElementById('2409.00675v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.00675v1-abstract-full" style="display: none;"> The study of exoplanets at different evolutionary stages can shed light on their formation, migration, and evolution. The determination of exoplanet properties depends on the properties of their host stars. It is therefore important to characterise the host stars for accurate knowledge on their planets. Our final goal is to derive, in a homogeneous and accurate way, the stellar atmospheric parameters and elemental abundances of ten young TESS transiting planet-hosting GK stars followed up with the HARPS-N at TNG spectrograph within the GAPS programme. We derived stellar kinematic properties, atmospheric parameters, and abundances of 18 elements. Lithium line measurements were used as approximate age estimations. We exploited chemical abundances and their ratios to derive information on planetary composition. Elemental abundances and kinematic properties are consistent with the nearby Galactic thin disk. All targets show C/O<0.8 and 1.0<Mg/Si<1.5, compatible with silicate mantles made of a mixture of pyroxene and olivine assemblages. The Fe/Mg ratios, with values of $\sim$0.7-1.0, show a propensity for the planets to have big (iron) cores. All stars hosting very low-mass planets show Mg/Si values consistent with the Earth values, thus demonstrating their similar mantle composition. Hot Jupiter host stars show a lower content of O/Si, which could be related to the lower presence of water content. We confirm a trend found in the literature between stellar [O/Fe] and total planetary mass, implying an important role of the O in shaping the mass fraction of heavy elements in stars and their disks. The detailed host star abundances provided can be employed for further studies on the composition of the planets within the current sample, when their atmospheres will be exploited. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.00675v1-abstract-full').style.display = 'none'; document.getElementById('2409.00675v1-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> 1 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">Accepted for publication on A&A. Abstract abridged</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.10629">arXiv:2408.10629</a> <span> [<a href="https://arxiv.org/pdf/2408.10629">pdf</a>, <a href="https://arxiv.org/format/2408.10629">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/10.1051/0004-6361/202450366">10.1051/0004-6361/202450366 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG. LIX. A characterisation study of the $\sim$300 Myr old multi-planetary system orbiting the star BD+40 2790 (TOI-2076) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Locci%2C+D">D. Locci</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/?searchtype=author&query=Wang%2C+S">S. Wang</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Messina%2C+S">S. Messina</a>, <a href="/search/?searchtype=author&query=Nowak%2C+G">G. Nowak</a>, <a href="/search/?searchtype=author&query=Goyal%2C+A">A. Goyal</a>, <a href="/search/?searchtype=author&query=Bejar%2C+V+J+S">V. J. S. Bejar</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Cabona%2C+L">L. Cabona</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Filomeno%2C+S">S. Filomeno</a>, <a href="/search/?searchtype=author&query=Knapic%2C+C">C. Knapic</a>, <a href="/search/?searchtype=author&query=Lodieu%2C+N">N. Lodieu</a>, <a href="/search/?searchtype=author&query=Lorenzi%2C+V">V. Lorenzi</a> , et al. (13 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="2408.10629v1-abstract-short" style="display: inline;"> We collected more than 300 high-resolution spectra of the 300 Myr old star BD+40 2790 (TOI-2076) over ~3 years. This star hosts three transiting planets discovered by TESS, with orbital periods ~10, 21, and 35 days. BD+40 2790 shows an activity-induced scatter larger than 30 m/s in the radial velocities. We employed different methods to measure the stellar radial velocities and several models to f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10629v1-abstract-full').style.display = 'inline'; document.getElementById('2408.10629v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.10629v1-abstract-full" style="display: none;"> We collected more than 300 high-resolution spectra of the 300 Myr old star BD+40 2790 (TOI-2076) over ~3 years. This star hosts three transiting planets discovered by TESS, with orbital periods ~10, 21, and 35 days. BD+40 2790 shows an activity-induced scatter larger than 30 m/s in the radial velocities. We employed different methods to measure the stellar radial velocities and several models to filter out the dominant stellar activity signal, in order to bring to light the planet-induced signals which are expected to have semi-amplitudes one order of magnitude lower. We evaluated the mass loss rate of the planetary atmospheres using photoionization hydrodynamic modeling. The dynamical analysis confirms that the three sub-Neptune-sized companions (our radius measurements are $R_b$=2.54$\pm$0.04, $R_c$=3.35$\pm$0.05, and $R_d$=3.29$\pm$0.06 $R_{\rm Earth}$) have masses in the planetary regime. We derive 3$蟽$ upper limits below or close to the mass of Neptune for all the planets: 11--12, 12--13.5, and 14--19 $M_{\rm Earth}$ for planet $b$, $c$, and $d$ respectively. In the case of planet $d$, we found promising clues that the mass could be between ~7 and 8 $M_{\rm Earth}$, with a significance level between 2.3--2.5$蟽$ (at best). This result must be further investigated using other analysis methods or using high-precision near-IR spectrographs to collect new radial velocities, which could be less affected by stellar activity. Atmospheric photo-evaporation simulations predict that BD+40~2790 b is currently losing its H-He gaseous envelope, which will be completely lost at an age within 0.5--3 Gyr if its current mass is lower than 12 $M_{\rm Earth}$. BD+40 2790 c could have a lower bulk density than $b$, and it could retain its atmosphere up to an age of 5 Gyr. For the outermost planet $d$, we predict almost negligible evolution of its mass and radius induced by photo-evaporation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10629v1-abstract-full').style.display = 'none'; document.getElementById('2408.10629v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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 on A&A. Abstract abridged</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A235 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.08949">arXiv:2406.08949</a> <span> [<a href="https://arxiv.org/pdf/2406.08949">pdf</a>, <a href="https://arxiv.org/format/2406.08949">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/10.1051/0004-6361/202450679">10.1051/0004-6361/202450679 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TOI-837 b: characterisation, formation and evolutionary history of an infant warm Saturn-mass planet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Polychroni%2C+D">D. Polychroni</a>, <a href="/search/?searchtype=author&query=Locci%2C+D">D. Locci</a>, <a href="/search/?searchtype=author&query=Turrini%2C+D">D. Turrini</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">P. E. Cubillos</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</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=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Pinamonti%2C+M">M. Pinamonti</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Marzari%2C+F">F. Marzari</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Spinelli%2C+R">R. Spinelli</a> </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="2406.08949v1-abstract-short" style="display: inline;"> We aim to determine the fundamental properties of the $\sim$35 Myr old star TOI-837 and its close-in Saturn-sized planet, and to investigate the system's formation and evolutionary history. We analysed TESS photometry and HARPS spectroscopic data, measured stellar and planetary parameters, and characterised the stellar activity. We performed population synthesis simulations to track the formation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.08949v1-abstract-full').style.display = 'inline'; document.getElementById('2406.08949v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.08949v1-abstract-full" style="display: none;"> We aim to determine the fundamental properties of the $\sim$35 Myr old star TOI-837 and its close-in Saturn-sized planet, and to investigate the system's formation and evolutionary history. We analysed TESS photometry and HARPS spectroscopic data, measured stellar and planetary parameters, and characterised the stellar activity. We performed population synthesis simulations to track the formation history of TOI-837 $b$, and to reconstruct its possible internal structure. We investigated the planetary atmospheric evolution through photo-evaporation, and quantified the prospects for atmospheric characterisation with JWST. TOI-837 $b$ has radius and mass similar to those of Saturn ($r_b$=9.71$^{+0.93}_{-0.60}$ \rearth, $m_b$=116$^{+17}_{-18}$ M$_\odot$, and $蟻_b$=0.68$^{+0.20}_{-0.18}$ gcm$^{-3}$), on a primordial circular orbit. Population synthesis and early migration simulations suggest that the planet could have originated between 2-4 au, and have either a large and massive core, or a smaller Saturn-like core, depending on the opacity of the protoplanetary gas and on the growth rate of the core. We found that photo-evaporation produced negligible effects even at early ages (3-10 Myr). Transmission spectroscopy with JWST is very promising, and expected to provide constraints on atmospheric metallicity, abundance of H$_2$O, CO$_2$, CH$_4$ molecules, and to probe the presence of refractory elements. TOI-837 offers valuable prospects for follow-up observations, which are needed for a thorough characterisation. JWST will help to better constraining the formation and evolution history of the system, and understand whether TOI-837 $b$ is a Saturn-analogue. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.08949v1-abstract-full').style.display = 'none'; document.getElementById('2406.08949v1-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> 13 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 on A&A on June 12 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 688, A15 (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/2405.18950">arXiv:2405.18950</a> <span> [<a href="https://arxiv.org/pdf/2405.18950">pdf</a>, <a href="https://arxiv.org/format/2405.18950">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> <p class="title is-5 mathjax"> The GAPS programme at TNG. LVII. TOI-5076b: A warm sub-Neptune planet orbiting a thin-to-thick-disk transition star in a wide binary system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montalto%2C+M">M. Montalto</a>, <a href="/search/?searchtype=author&query=Greco%2C+N">N. Greco</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Andreuzzi%2C+G">G. Andreuzzi</a>, <a href="/search/?searchtype=author&query=Bieryla%2C+A">A. Bieryla</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Brice%C3%B1o%2C+C">C. Brice帽o</a>, <a href="/search/?searchtype=author&query=Cabona%2C+L">L. Cabona</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Fiorenzano%2C+A">A. Fiorenzano</a>, <a href="/search/?searchtype=author&query=Fong%2C+W">W. Fong</a>, <a href="/search/?searchtype=author&query=Goeke%2C+B">B. Goeke</a>, <a href="/search/?searchtype=author&query=Hesse%2C+K+M">K. M. Hesse</a>, <a href="/search/?searchtype=author&query=Kostov%2C+V+B">V. B. Kostov</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">D. W. Latham</a>, <a href="/search/?searchtype=author&query=Law%2C+N">N. Law</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Molinaro%2C+M">M. Molinaro</a>, <a href="/search/?searchtype=author&query=Mann%2C+A+W">A. W. Mann</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a> , et al. (14 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="2405.18950v1-abstract-short" style="display: inline;"> Aims. We report the confirmation of a new transiting exoplanet orbiting the star TOI-5076. Methods. We present our vetting procedure and follow-up observations which led to the confirmation of the exoplanet TOI-5076b. In particular, we employed high-precision {\it TESS} photometry, high-angular-resolution imaging from several telescopes, and high-precision radial velocities from HARPS-N. Results.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18950v1-abstract-full').style.display = 'inline'; document.getElementById('2405.18950v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.18950v1-abstract-full" style="display: none;"> Aims. We report the confirmation of a new transiting exoplanet orbiting the star TOI-5076. Methods. We present our vetting procedure and follow-up observations which led to the confirmation of the exoplanet TOI-5076b. In particular, we employed high-precision {\it TESS} photometry, high-angular-resolution imaging from several telescopes, and high-precision radial velocities from HARPS-N. Results. From the HARPS-N spectroscopy, we determined the spectroscopic parameters of the host star: T$\rm_{eff}$=(5070$\pm$143) K, log~g=(4.6$\pm$0.3), [Fe/H]=(+0.20$\pm$0.08), and [$伪$/Fe]=0.05$\pm$0.06. The transiting planet is a warm sub-Neptune with a mass m$\rm_p=$(16$\pm$2) M$\rm_{\oplus}$, a radius r$\rm_p=$(3.2$\pm$0.1)~R$\rm_{\oplus}$ yielding a density $蟻_p$=(2.8$\pm$0.5) g cm$^{-3}$. It revolves around its star approximately every 23.445 days. Conclusions. The host star is a metal-rich, K2V dwarf, located at about 82 pc from the Sun with a radius of R$_{\star}$=(0.78$\pm$0.01) R$_{\odot}$ and a mass of M$_{\star}$=(0.80$\pm$0.07) M$_{\odot}$. It forms a common proper motion pair with an M-dwarf companion star located at a projected separation of 2178 au. The chemical analysis of the host-star and the Galactic-space velocities indicate that TOI-5076 belongs to the old population of thin-to-thick-disk transition stars. The density of TOI-5076b suggests the presence of a large fraction by volume of volatiles overlying a massive core. We found that a circular orbit solution is marginally favored with respect to an eccentric orbit solution for TOI-5076b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18950v1-abstract-full').style.display = 'none'; document.getElementById('2405.18950v1-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 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 by Astronomy & Astrophysics: 15 pages, 19 figures, 4 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/2404.13586">arXiv:2404.13586</a> <span> [<a href="https://arxiv.org/pdf/2404.13586">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> </div> </div> <p class="title is-5 mathjax"> The PEPSI Exoplanet Transit Survey (PETS). V: New Na D transmission spectra indicate a quieter atmosphere on HD 189733b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Keles%2C+E">E. Keles</a>, <a href="/search/?searchtype=author&query=Czesla%2C+S">S. Czesla</a>, <a href="/search/?searchtype=author&query=Poppenhaeger%2C+K">K. Poppenhaeger</a>, <a href="/search/?searchtype=author&query=Hauschildt%2C+P">P. Hauschildt</a>, <a href="/search/?searchtype=author&query=Carroll%2C+T+A">T. A. Carroll</a>, <a href="/search/?searchtype=author&query=Ilyin%2C+I">I. Ilyin</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=Steffen%2C+M">M. Steffen</a>, <a href="/search/?searchtype=author&query=Strassmeier%2C+K+G">K. G. Strassmeier</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">T. Henning</a>, <a href="/search/?searchtype=author&query=Johnson%2C+M+C">M. C. Johnson</a>, <a href="/search/?searchtype=author&query=Molaverdikhani%2C+K">K. Molaverdikhani</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Patience%2C+J">J. Patience</a>, <a href="/search/?searchtype=author&query=Reiners%2C+A">A. Reiners</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Schlawin%2C+E">E. Schlawin</a>, <a href="/search/?searchtype=author&query=Shkolnik%2C+E">E. Shkolnik</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Mallonn%2C+M">M. Mallonn</a>, <a href="/search/?searchtype=author&query=Veillet%2C+C">C. Veillet</a>, <a href="/search/?searchtype=author&query=Wang%2C+J">J. Wang</a> , et al. (1 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="2404.13586v1-abstract-short" style="display: inline;"> Absorption lines from exoplanet atmospheres observed in transmission allow us to study atmospheric characteristics such as winds. We present a new high-resolution transit time-series of HD 189733b, acquired with the PEPSI instrument at the LBT and analyze the transmission spectrum around the Na D lines. We model the spectral signature of the RM-CLV-effect using synthetic PHOENIX spectra based on s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13586v1-abstract-full').style.display = 'inline'; document.getElementById('2404.13586v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.13586v1-abstract-full" style="display: none;"> Absorption lines from exoplanet atmospheres observed in transmission allow us to study atmospheric characteristics such as winds. We present a new high-resolution transit time-series of HD 189733b, acquired with the PEPSI instrument at the LBT and analyze the transmission spectrum around the Na D lines. We model the spectral signature of the RM-CLV-effect using synthetic PHOENIX spectra based on spherical LTE atmospheric models. We find a Na D absorption signature between the second and third contact but not during the ingress and egress phases, which casts doubt on the planetary origin of the signal. Presupposing a planetary origin of the signal, the results suggest a weak day-to-nightside streaming wind in the order of 0.7 km/s and a moderate super-rotational streaming wind in the order of 3 - 4 km/s, challenging claims of prevailing strong winds on HD 189733b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13586v1-abstract-full').style.display = 'none'; document.getElementById('2404.13586v1-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> 21 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">Accepted for publication in Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03317">arXiv:2404.03317</a> <span> [<a href="https://arxiv.org/pdf/2404.03317">pdf</a>, <a href="https://arxiv.org/format/2404.03317">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/10.1051/0004-6361/202349116">10.1051/0004-6361/202349116 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG. XXX: Characterization of the low-density gas giant HAT-P-67 b with GIARPS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Esposito%2C+M">M. Esposito</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Stangret%2C+M">M. Stangret</a>, <a href="/search/?searchtype=author&query=Di+Maio%2C+C">C. Di Maio</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Rainer%2C+M">M. Rainer</a>, <a href="/search/?searchtype=author&query=D%27Arpa%2C+M+C">M. C. D'Arpa</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Colombo%2C+S">S. Colombo</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a> , et al. (6 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="2404.03317v1-abstract-short" style="display: inline;"> HAT-P-67 b is one of the lowest-density gas giants known to date, making it an excellent target for atmospheric characterization through the transmission spectroscopy technique. In the framework of the GAPS large programme, we collected four transit events, with the aim of studying the exoplanet atmosphere and deriving the orbital projected obliquity. We exploited the high-precision GIARPS observi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03317v1-abstract-full').style.display = 'inline'; document.getElementById('2404.03317v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03317v1-abstract-full" style="display: none;"> HAT-P-67 b is one of the lowest-density gas giants known to date, making it an excellent target for atmospheric characterization through the transmission spectroscopy technique. In the framework of the GAPS large programme, we collected four transit events, with the aim of studying the exoplanet atmosphere and deriving the orbital projected obliquity. We exploited the high-precision GIARPS observing mode of the TNG, along with additional archival TESS photometry, to explore the activity level of the host star. We performed transmission spectroscopy, both in the VIS and in the nIR wavelength range, and analysed the RML effect both fitting the RVs and the Doppler shadow. Based on the TESS photometry, we redetermined the transit parameters of HAT-P-67 b. By modelling the RML effect, we derived a sky-projected obliquity of ($2.2\pm0.4$)掳 indicating an aligned planetary orbit. The chromospheric activity index $\log\,R^{\prime}_{\rm HK}$, the CCF profile, and the variability in the transmission spectrum of the H$伪$ line suggest that the host star shows signatures of stellar activity and/or pulsations. We found no evidence of atomic or molecular species in the VIS transmission spectra, with the exception of pseudo-signals corresponding to Cr I, Fe I, H$伪$, Na I, and Ti I. In the nIR range, we found an absorption signal of the He I triplet of 5.56$^{+0.29}_{-0.30}$%(19.0$蟽$), corresponding to an effective planetary radius of $\sim$3$R_p$ (where $R_p\sim$2$R_J$) which extends beyond the planet's Roche Lobe radius. Owing to the stellar variability, together with the high uncertainty of the model, we could not confirm the planetary origin of the signals found in the optical transmission spectrum. On the other hand, we confirmed previous detections of the infrared He I triplet, providing a 19.0$蟽$ detection. Our finding indicates that the planet's atmosphere is evaporating. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03317v1-abstract-full').style.display = 'none'; document.getElementById('2404.03317v1-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> 4 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">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 687, A143 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.01527">arXiv:2403.01527</a> <span> [<a href="https://arxiv.org/pdf/2403.01527">pdf</a>, <a href="https://arxiv.org/format/2403.01527">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/10.1051/0004-6361/202347659">10.1051/0004-6361/202347659 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG LV. Multiple molecular species in the atmosphere of HAT-P-11 b and review of the HAT-P-11 planetary system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Basilicata%2C+M">M. Basilicata</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/?searchtype=author&query=Di+Paola%2C+A">A. Di Paola</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">P. E. Cubillos</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Cabona%2C+L">L. Cabona</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Ghedina%2C+A">A. Ghedina</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Mainella%2C+G">G. Mainella</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Molinaro%2C+M">M. Molinaro</a> , et al. (7 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="2403.01527v3-abstract-short" style="display: inline;"> The atmospheric characterisation of hot and warm Neptune-size exoplanets is challenging due to their small radius and atmospheric scale height. The warm-Neptune HAT-P-11b is a remarkable target for such characterisation due to the large brightness of its host star (V=9.46 mag; H=7.13 mag). The aims of this work are to review the main physical and architectural properties of the HAT-P-11 planetary… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.01527v3-abstract-full').style.display = 'inline'; document.getElementById('2403.01527v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.01527v3-abstract-full" style="display: none;"> The atmospheric characterisation of hot and warm Neptune-size exoplanets is challenging due to their small radius and atmospheric scale height. The warm-Neptune HAT-P-11b is a remarkable target for such characterisation due to the large brightness of its host star (V=9.46 mag; H=7.13 mag). The aims of this work are to review the main physical and architectural properties of the HAT-P-11 planetary system, and to probe the presence of 8 molecular species in the atmosphere of HAT-P-11b at high spectral resolution in the near-infrared. The planetary system was reviewed by analysing transits and occultations of HAT-P-11b from the Kepler data set as well as HIRES at Keck archival radial-velocity (RV) data. We modelled the latter with Gaussian-process regression and a combined quasi-periodic and squared-exponential kernel to account for stellar variations on both (short-term) rotation and (long-term) activity-cycle timescales. In order to probe the atmospheric composition of HAT-P-11b, we observed 4 transits of this target with GIANO-B at TNG. We find that the long-period ($P\sim9.3$ years) RV signal previously attributed to planet HAT-P-11c is more likely due to the stellar magnetic activity cycle. Nonetheless, the Hipparcos-Gaia difference in the proper-motion anomaly suggests that an outer-bound companion might still exist. For HAT-P-11b, we measure a radius $R_{\rm p}=0.4466\pm0.0059\,R_{\rm J}$, a mass $M_{\rm p}=0.0787\pm0.0048\,M_{\rm J}$, and an eccentricity $e=0.2577^{+0.0033}_{-0.0025}$, in accordance with values in the literature. Probing its atmosphere, we detect $NH_3$ (S/N$=5.3$, significance$=5.0蟽$) and confirm the presence of $H_2O$ (S/N$=5.1$, significance$=3.4蟽$). We also tentatively detect the signal of $CO_2$ (S/N$=3.0$, significance$=3.2蟽$) and $CH_4$ (S/N$=4.8$, significance$=2.6蟽$), whose presence need to be confirmed by further observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.01527v3-abstract-full').style.display = 'none'; document.getElementById('2403.01527v3-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">25 pages, 19 figures, accepted for publication in Astronomy & Astrophysics (A&A) journal. Version corrected by the language editor, title edited</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A127 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.00608">arXiv:2403.00608</a> <span> [<a href="https://arxiv.org/pdf/2403.00608">pdf</a>, <a href="https://arxiv.org/format/2403.00608">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 GAPS Programme at TNG: LIV. A HeI survey of close-in giant planets hosted by M-K dwarf stars with GIANO-B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=D%27Arpa%2C+M+C">M. C. D'Arpa</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Spinelli%2C+R">R. Spinelli</a>, <a href="/search/?searchtype=author&query=Biassoni%2C+F">F. Biassoni</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Rainer%2C+M">M. Rainer</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Andreuzzi%2C+G">G. Andreuzzi</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Boschin%2C+W">W. Boschin</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Cecconi%2C+M">M. Cecconi</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Fardella%2C+V">V. Fardella</a>, <a href="/search/?searchtype=author&query=Ghedina%2C+A">A. Ghedina</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a> , et al. (8 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="2403.00608v3-abstract-short" style="display: inline;"> Atmospheric escape plays a fundamental role in shaping the properties of exoplanets. The metastable near-infrared helium triplet at 1083.3 nm (HeI) is a powerful proxy of extended and evaporating atmospheres. We used the GIARPS (GIANO-B+HARPS-N) observing mode of the Telescopio Nazionale Galileo to search for HeI absorption in the upper atmosphere of five close-in giant planets hosted by the K and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.00608v3-abstract-full').style.display = 'inline'; document.getElementById('2403.00608v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.00608v3-abstract-full" style="display: none;"> Atmospheric escape plays a fundamental role in shaping the properties of exoplanets. The metastable near-infrared helium triplet at 1083.3 nm (HeI) is a powerful proxy of extended and evaporating atmospheres. We used the GIARPS (GIANO-B+HARPS-N) observing mode of the Telescopio Nazionale Galileo to search for HeI absorption in the upper atmosphere of five close-in giant planets hosted by the K and M dwarf stars of our sample, namely WASP-69b, WASP-107b, HAT-P-11b, GJ436b, and GJ3470b. We focused our analysis on the HeI triplet by performing high-resolution transmission spectroscopy. When nightly variability in the HeI absorption signal was identified, we investigated the potential influence of stellar magnetic activity by searching for variations in the H$伪$. We spectrally resolve the HeI triplet and confirm the published detections for WASP-69b (3.91$\pm$0.22%, 17.6$蟽$), WASP-107b (8.17$^{+0.80}_{-0.76}$%, 10.5$蟽$), HAT-P-11b (1.36$\pm$0.17%, 8.0$蟽$), and GJ3470b (1.75$^{+0.39}_{-0.36}$%, 4.7$蟽$). We do not find evidence of extra absorption for GJ436b. We observe night-to-night variations in the HeI absorption signal for WASP-69b, associated with variability in H$伪$, which likely indicates the influence of stellar activity. Additionally, we find that the HeI signal of GJ3470b originates from a single transit, thereby corroborating the discrepancies in the existing literature. An inspection of the H$伪$ reveals an absorption signal during the same transit. By combining our findings with previous analyses of GIANO-B HeI measurements of planets around K dwarfs, we explore potential trends with planetary/stellar parameters that are thought to affect the HeI absorption. Our analysis is unable to identify clear patterns, emphasising the need for further measurements and the exploration of additional potential parameters that might influence HeI absorption. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.00608v3-abstract-full').style.display = 'none'; document.getElementById('2403.00608v3-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> 4 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">23 pages, 13 figures, accepted for publication in A&A. v3 includes language editing</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17876">arXiv:2401.17876</a> <span> [<a href="https://arxiv.org/pdf/2401.17876">pdf</a>, <a href="https://arxiv.org/format/2401.17876">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/10.1051/0004-6361/202348042">10.1051/0004-6361/202348042 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG. LIII. New insights on the peculiar XO-2 system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ruggieri%2C+A">A. Ruggieri</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Pinamonti%2C+M">M. Pinamonti</a>, <a href="/search/?searchtype=author&query=Marzari%2C+F">F. Marzari</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Gratton%2C+R">R. Gratton</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Andreuzzi%2C+G">G. Andreuzzi</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Cabona%2C+L">L. Cabona</a>, <a href="/search/?searchtype=author&query=Knapic%2C+C">C. Knapic</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a> </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="2401.17876v1-abstract-short" style="display: inline;"> Planets in binary systems are a fascinating and yet poorly understood phenomenon. Since there are only a few known large-separation systems in which both components host planets, characterizing them is a key target for planetary science. In this paper, we aim to carry out an exhaustive analysis of the interesting XO-2 system, where one component appears to be a system with only one planet, while t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17876v1-abstract-full').style.display = 'inline'; document.getElementById('2401.17876v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17876v1-abstract-full" style="display: none;"> Planets in binary systems are a fascinating and yet poorly understood phenomenon. Since there are only a few known large-separation systems in which both components host planets, characterizing them is a key target for planetary science. In this paper, we aim to carry out an exhaustive analysis of the interesting XO-2 system, where one component appears to be a system with only one planet, while the other has at least three planets. Over the last 9 years, we have collected 39 spectra of XO-2N and 106 spectra of XO-2S with the High Accuracy Radial velocity Planet Searcher for the Northern emisphere (HARPS-N) in the framework of the Global Architecture of Planetary Systems project, from which we derived precise radial velocity and activity indicator measurements. Additional spectroscopic data from the High Resolution Echelle Spectrometer and from the High Dispersion Spectrograph, and the older HARPS-N data presented in previous papers, have also been used to increase the total time span. We also used photometric data from TESS to search for potential transits that have not been detected yet. For our analysis, we mainly used PyORBIT, an advanced Python tool for the Bayesian analysis of RVs, activity indicators, and light curves. We found evidence for an additional long-period planet around XO-2S and characterized the activity cycle likely responsible for the long-term RV trend noticed for XO-2N. The new candidate is an example of a Jovian analog with $m\sin i \sim 3.7$ M$_J$, $a \sim 5.5$ au, and $e = 0.09$. We also analyzed the stability and detection limits to get some hints about the possible presence of additional planets. Our results show that the planetary system of XO-2S is at least one order of magnitude more massive than that of XO-2N. The implications of these findings for the interpretation of the previously known abundance difference between components are also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17876v1-abstract-full').style.display = 'none'; document.getElementById('2401.17876v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.17075">arXiv:2311.17075</a> <span> [<a href="https://arxiv.org/pdf/2311.17075">pdf</a>, <a href="https://arxiv.org/format/2311.17075">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"> Ground-breaking Exoplanet Science with the ANDES spectrograph at the ELT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Palle%2C+E">Enric Palle</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">Katia Biazzo</a>, <a href="/search/?searchtype=author&query=Bolmont%2C+E">Emeline Bolmont</a>, <a href="/search/?searchtype=author&query=Molliere%2C+P">Paul Molliere</a>, <a href="/search/?searchtype=author&query=Poppenhaeger%2C+K">Katja Poppenhaeger</a>, <a href="/search/?searchtype=author&query=Birkby%2C+J">Jayne Birkby</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">Matteo Brogi</a>, <a href="/search/?searchtype=author&query=Chauvin%2C+G">Gael Chauvin</a>, <a href="/search/?searchtype=author&query=Chiavassa%2C+A">Andrea Chiavassa</a>, <a href="/search/?searchtype=author&query=Hoeijmakers%2C+J">Jens Hoeijmakers</a>, <a href="/search/?searchtype=author&query=Lellouch%2C+E">Emmanuel Lellouch</a>, <a href="/search/?searchtype=author&query=Lovis%2C+C">Christophe Lovis</a>, <a href="/search/?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/?searchtype=author&query=Nortmann%2C+L">Lisa Nortmann</a>, <a href="/search/?searchtype=author&query=Parviainen%2C+H">Hannu Parviainen</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">Lorenzo Pino</a>, <a href="/search/?searchtype=author&query=Turbet%2C+M">Martin Turbet</a>, <a href="/search/?searchtype=author&query=Wender%2C+J">Jesse Wender</a>, <a href="/search/?searchtype=author&query=Albrecht%2C+S">Simon Albrecht</a>, <a href="/search/?searchtype=author&query=Antoniucci%2C+S">Simone Antoniucci</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C">Susana C. Barros</a>, <a href="/search/?searchtype=author&query=Beaudoin%2C+A">Andre Beaudoin</a>, <a href="/search/?searchtype=author&query=Benneke%2C+B">Bjorn Benneke</a>, <a href="/search/?searchtype=author&query=Boisse%2C+I">Isabelle Boisse</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</a> , et al. (34 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="2311.17075v1-abstract-short" style="display: inline;"> In the past decade the study of exoplanet atmospheres at high-spectral resolution, via transmission/emission spectroscopy and cross-correlation techniques for atomic/molecular mapping, has become a powerful and consolidated methodology. The current limitation is the signal-to-noise ratio during a planetary transit. This limitation will be overcome by ANDES, an optical and near-infrared high-resolu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.17075v1-abstract-full').style.display = 'inline'; document.getElementById('2311.17075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.17075v1-abstract-full" style="display: none;"> In the past decade the study of exoplanet atmospheres at high-spectral resolution, via transmission/emission spectroscopy and cross-correlation techniques for atomic/molecular mapping, has become a powerful and consolidated methodology. The current limitation is the signal-to-noise ratio during a planetary transit. This limitation will be overcome by ANDES, an optical and near-infrared high-resolution spectrograph for the ELT. ANDES will be a powerful transformational instrument for exoplanet science. It will enable the study of giant planet atmospheres, allowing not only an exquisite determination of atmospheric composition, but also the study of isotopic compositions, dynamics and weather patterns, mapping the planetary atmospheres and probing atmospheric formation and evolution models. The unprecedented angular resolution of ANDES, will also allow us to explore the initial conditions in which planets form in proto-planetary disks. The main science case of ANDES, however, is the study of small, rocky exoplanet atmospheres, including the potential for biomarker detections, and the ability to reach this science case is driving its instrumental design. Here we discuss our simulations and the observing strategies to achieve this specific science goal. Since ANDES will be operational at the same time as NASA's JWST and ESA's ARIEL missions, it will provide enormous synergies in the characterization of planetary atmospheres at high and low spectral resolution. Moreover, ANDES will be able to probe for the first time the atmospheres of several giant and small planets in reflected light. In particular, we show how ANDES will be able to unlock the reflected light atmospheric signal of a golden sample of nearby non-transiting habitable zone earth-sized planets within a few tenths of nights, a scientific objective that no other currently approved astronomical facility will be able to reach. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.17075v1-abstract-full').style.display = 'none'; document.getElementById('2311.17075v1-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, 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">66 pages (103 with references) 20 figures. Submitted to Experimental Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.01464">arXiv:2309.01464</a> <span> [<a href="https://arxiv.org/pdf/2309.01464">pdf</a>, <a href="https://arxiv.org/format/2309.01464">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/s41586-023-06499-2">10.1038/s41586-023-06499-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A super-massive Neptune-sized planet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Naponiello%2C+L">L. Naponiello</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Morbidelli%2C+A">A. Morbidelli</a>, <a href="/search/?searchtype=author&query=Dou%2C+J">J. Dou</a>, <a href="/search/?searchtype=author&query=Zeng%2C+L">L. Zeng</a>, <a href="/search/?searchtype=author&query=Leinhardt%2C+Z+M">Z. M. Leinhardt</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P">P. Cubillos</a>, <a href="/search/?searchtype=author&query=Pinamonti%2C+M">M. Pinamonti</a>, <a href="/search/?searchtype=author&query=Locci%2C+D">D. Locci</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Lissauer%2C+J+J">J. J. Lissauer</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Boschin%2C+W">W. Boschin</a>, <a href="/search/?searchtype=author&query=Bouma%2C+L+G">L. G. Bouma</a>, <a href="/search/?searchtype=author&query=Carter%2C+P+J">P. J. Carter</a>, <a href="/search/?searchtype=author&query=Ciardi%2C+D+R">D. R. Ciardi</a>, <a href="/search/?searchtype=author&query=Collins%2C+K+A">K. A. Collins</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Crossfield%2C+I">I. Crossfield</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a> , et al. (33 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="2309.01464v1-abstract-short" style="display: inline;"> Neptune-sized planets exhibit a wide range of compositions and densities, depending onf cators related to their formation and evolution history, such as the distance from their host stars and atmospheric escape processes. They can vary from relatively low-density planets with thick hydrogen-helium atmospheres to higher-density planets with a substantial amount of water or a rocky interior with a t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.01464v1-abstract-full').style.display = 'inline'; document.getElementById('2309.01464v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.01464v1-abstract-full" style="display: none;"> Neptune-sized planets exhibit a wide range of compositions and densities, depending onf cators related to their formation and evolution history, such as the distance from their host stars and atmospheric escape processes. They can vary from relatively low-density planets with thick hydrogen-helium atmospheres to higher-density planets with a substantial amount of water or a rocky interior with a thinner atmosphere, such as HD 95338 b, TOI-849 b and TOI-2196 b. The discovery of exoplanets in the hot-Neptune desert, a region close to the host stars with a deficit of Neptune-sized planets, provides insights into the formation and evolution of planetary systems, including the existence of this region itself. Here we show observations of the transiting planet TOI-1853 b, which has a radius of 3.46 +- 0.08 Earth radii and orbits a dwarf star every 1.24 days. This planet has a mass of 73.2 +- 2.7 Earth masses, almost twice that of any other Neptune-sized planet known so far, and a density of 9.7 +- 0.8 grams per cubic centimetre. These values place TOI-1853 b in the middle of the Neptunian desert and imply that heavy elements dominate its mass. The properties of TOI-1853 b present a puzzle for conventional theories of planetary formation and evolution, and could be the result of several proto-planet collisions or the final state of an initially high-eccentricity planet that migrated closer to its parent star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.01464v1-abstract-full').style.display = 'none'; document.getElementById('2309.01464v1-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> 4 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">Preprint submitted to Nature. Please refer to the published version for the final parameters estimations</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature, published online on the 30th of August 2023 and printed the 12th of October 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.05669">arXiv:2308.05669</a> <span> [<a href="https://arxiv.org/pdf/2308.05669">pdf</a>, <a href="https://arxiv.org/format/2308.05669">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/10.1051/0004-6361/202346887">10.1051/0004-6361/202346887 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A review of planetary systems around HD 99492, HD 147379 and HD 190007 with HARPS-N </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Stalport%2C+M">M. Stalport</a>, <a href="/search/?searchtype=author&query=Cretignier%2C+M">M. Cretignier</a>, <a href="/search/?searchtype=author&query=Udry%2C+S">S. Udry</a>, <a href="/search/?searchtype=author&query=John%2C+A+A">A. Anna John</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Delisle%2C+J+-">J. -B. Delisle</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Buchhave%2C+L+A">L. A. Buchhave</a>, <a href="/search/?searchtype=author&query=Charbonneau%2C+D">D. Charbonneau</a>, <a href="/search/?searchtype=author&query=Dalal%2C+S">S. Dalal</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Di+Fabrizio%2C+L">L. Di Fabrizio</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/?searchtype=author&query=Fiorenzano%2C+A">A. Fiorenzano</a>, <a href="/search/?searchtype=author&query=Harutyunyan%2C+A">A. Harutyunyan</a>, <a href="/search/?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">D. W. Latham</a>, <a href="/search/?searchtype=author&query=L%C3%B3pez-Morales%2C+M">M. L贸pez-Morales</a>, <a href="/search/?searchtype=author&query=Lorenzi%2C+V">V. Lorenzi</a>, <a href="/search/?searchtype=author&query=Lovis%2C+C">C. Lovis</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Mortier%2C+A">A. Mortier</a>, <a href="/search/?searchtype=author&query=Pedani%2C+M">M. Pedani</a>, <a href="/search/?searchtype=author&query=Pepe%2C+F">F. Pepe</a> , et al. (4 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="2308.05669v1-abstract-short" style="display: inline;"> The Rocky Planet Search (RPS) program is dedicated to a blind radial velocity (RV) search of planets around bright stars in the Northern hemisphere, using the high-resolution echelle spectrograph HARPS-N installed on the Telescopio Nazionale Galileo (TNG). The goal of this work is to revise and update the properties of three planetary systems by analysing the HARPS-N data with state-of-the-art s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.05669v1-abstract-full').style.display = 'inline'; document.getElementById('2308.05669v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.05669v1-abstract-full" style="display: none;"> The Rocky Planet Search (RPS) program is dedicated to a blind radial velocity (RV) search of planets around bright stars in the Northern hemisphere, using the high-resolution echelle spectrograph HARPS-N installed on the Telescopio Nazionale Galileo (TNG). The goal of this work is to revise and update the properties of three planetary systems by analysing the HARPS-N data with state-of-the-art stellar activity mitigation tools. The stars considered are HD 99492 (83Leo B), HD 147379 (Gl617 A) and HD 190007. We employ a systematic process of data modelling, that we selected from the comparison of different approaches. We use YARARA to remove instrumental systematics from the RV, and then use SPLEAF to further mitigate the stellar noise with a multidimensional correlated noise model. We also search for transit features in the Transiting Exoplanets Survey Satellite (TESS) data of these stars. We report on the discovery of a new planet around HD 99492, namely HD 99492 c, with an orbital period of 95.2 days and a minimum mass of msin i = 17.9 M_Earth, and refine the parameters of HD 99492 b. We also update and refine the Keplerian solutions for the planets around HD 147379 and HD 190007, but do not detect additional planetary signals. We discard the transiting geometry for the planets, but stress that TESS did not exhaustively cover all the orbital phases. The addition of the HARPS-N data, and the use of advanced data analysis tools, has allowed us to present a more precise view of these three planetary systems. It demonstrates once again the importance of long observational efforts such as the RPS program. Added to the RV exoplanet sample, these planets populate two apparently distinct populations revealed by a bimodality in the planets minimum mass distribution. The separation is located between 30 and 50 M_Earth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.05669v1-abstract-full').style.display = 'none'; document.getElementById('2308.05669v1-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 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">27 pages, 26 figures (13 in Appendix); 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, A90 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.00967">arXiv:2307.00967</a> <span> [<a href="https://arxiv.org/pdf/2307.00967">pdf</a>, <a href="https://arxiv.org/format/2307.00967">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/10.1051/0004-6361/202346419">10.1051/0004-6361/202346419 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> DREAM: III.A helium survey in exoplanets on the edge of the hot Neptune desert with GIANO-B@TNG </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Bourrier%2C+V">V. Bourrier</a>, <a href="/search/?searchtype=author&query=Jaziri%2C+Y">Y. Jaziri</a>, <a href="/search/?searchtype=author&query=Dethier%2C+W">W. Dethier</a>, <a href="/search/?searchtype=author&query=Mounzer%2C+D">D. Mounzer</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Attia%2C+O">O. Attia</a>, <a href="/search/?searchtype=author&query=Allart%2C+R">R. Allart</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Santos%2C+L+A+D">L. A. Dos Santos</a>, <a href="/search/?searchtype=author&query=Rainer%2C+M">M. Rainer</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a> </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="2307.00967v2-abstract-short" style="display: inline;"> The population of close-in exoplanets features a desert of hot Neptunes whose origin is uncertain. These planets may have lost their atmosphere, eroding into mini-Neptunes and super-Earths. Direct observations of evaporating atmospheres are essential to derive mass-loss estimates and constrain this scenario. The metastable 1083.3nm HeI triplet represents a powerful diagnostic of atmospheric evapor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.00967v2-abstract-full').style.display = 'inline'; document.getElementById('2307.00967v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.00967v2-abstract-full" style="display: none;"> The population of close-in exoplanets features a desert of hot Neptunes whose origin is uncertain. These planets may have lost their atmosphere, eroding into mini-Neptunes and super-Earths. Direct observations of evaporating atmospheres are essential to derive mass-loss estimates and constrain this scenario. The metastable 1083.3nm HeI triplet represents a powerful diagnostic of atmospheric evaporation since it traces the hot gas in extended exoplanet atmospheres, is observable from the ground, and is weakly affected by interstellar medium absorption. We conducted a uniform HeI transmission spectroscopy survey, focusing on 9 planets located at the edges of the Neptunian desert, aiming to gain insights into the role of photo-evaporation in its formation. We observed one transit per planet using the high-resolution, near-infrared spectrograph GIANO-B on the Telescopio Nazionale Galileo. We focused our analysis on the HeI triplet by computing high-resolution transmission spectra. We then employed the p-winds model to interpret the observed transmission spectra. We found no sign of planetary absorption in the HeI triplet in any of the investigated targets. We thus provided 3sigma upper-limit estimations on the thermosphere absorption, temperature, and mass loss, and combined them with past measurements to search for correlations with parameters thought to be drivers in the formation of the HeI triplet. Our results strengthen the importance of performing homogeneous surveys and analyses to bring clarification in the HeI detection and hence in the Neptunian desert origin. Our findings corroborate the literature expectations that the HeI absorption signal correlates with the stellar mass and the received XUV flux. However, these trends seem to disappear in terms of mass-loss rates; further studies are essential to shed light on this aspect and to understand better the photo-evaporation process. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.00967v2-abstract-full').style.display = 'none'; document.getElementById('2307.00967v2-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">23 pages, 13 figures, accepted for publication in A&A, after language editing</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A130 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.15776">arXiv:2306.15776</a> <span> [<a href="https://arxiv.org/pdf/2306.15776">pdf</a>, <a href="https://arxiv.org/format/2306.15776">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/10.1051/0004-6361/202346787">10.1051/0004-6361/202346787 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS programme at TNG. XLV. HI Balmer lines transmission spectroscopy and NLTE atmospheric modelling of the ultra-hot Jupiter KELT-20b/MASCARA-2b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Biassoni%2C+F">F. Biassoni</a>, <a href="/search/?searchtype=author&query=Cappello%2C+G+M">G. M. Cappello</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Shulyak%2C+D">D. Shulyak</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Haardt%2C+F">F. Haardt</a>, <a href="/search/?searchtype=author&query=Koskinen%2C+T">T. Koskinen</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Young%2C+M">M. Young</a>, <a href="/search/?searchtype=author&query=Aresu%2C+G">G. Aresu</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Knapic%2C+C">C. Knapic</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Pinamonti%2C+M">M. Pinamonti</a> , et al. (5 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="2306.15776v1-abstract-short" style="display: inline;"> We aim at extracting the transmission spectrum of the HI Balmer lines of the ultra-hot Jupiter (UHJ) KELT-20b/MASCARA-2b from observations and to further compare the results with what obtained through forward modelling accounting for non-local thermodynamic equilibrium (NLTE) effects. We extract the line profiles from six transits obtained with the HARPS-N high-resolution spectrograph attached to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.15776v1-abstract-full').style.display = 'inline'; document.getElementById('2306.15776v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.15776v1-abstract-full" style="display: none;"> We aim at extracting the transmission spectrum of the HI Balmer lines of the ultra-hot Jupiter (UHJ) KELT-20b/MASCARA-2b from observations and to further compare the results with what obtained through forward modelling accounting for non-local thermodynamic equilibrium (NLTE) effects. We extract the line profiles from six transits obtained with the HARPS-N high-resolution spectrograph attached to the Telescopio Nazionale Galileo telescope. We compute the temperature-pressure (TP) profile employing the helios code in the lower atmosphere and the Cloudy NLTE code in the middle and upper atmosphere. We further use Cloudy to compute the theoretical planetary transmission spectrum in LTE and NLTE for comparison with observations. We detected the Halpha (0.79+/-0.03%; 1.25 Rp), Hbeta (0.52+/-0.03%; 1.17 Rp), and Hgamma (0.39+/-0.06%; 1.13 Rp) lines, while we detected the Hdelta line at almost 4 sigma (0.27+/-0.07%; 1.09 Rp). The models predict an isothermal temperature of about2200 K at pressures >10^-2 bar and of about 7700 K at pressures <10^-8 bar, with a roughly linear temperature rise in between. In the middle and upper atmosphere, the NLTE TP profile is up to about 3000 K hotter than in LTE. The synthetic transmission spectrum derived from the NLTE TP profile is in good agreement with the observed HI Balmer line profiles, validating our obtained atmospheric structure. Instead, the synthetic transmission spectrum derived from the LTE TP profile leads to significantly weaker absorption compared to the observations. Metals appear to be the primary agents leading to the temperature inversion in UHJs and the impact of NLTE effects on them increases the magnitude of the inversion. We find that the impact of NLTE effects on the TP profile of KELT-20b/MASCARA-2b is larger than for the hotter UHJ KELT-9b, and thus NLTE effects might be relevant also for planets cooler than KELT-20b/MASCARA-2b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.15776v1-abstract-full').style.display = 'none'; document.getElementById('2306.15776v1-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 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">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 676, A99 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.05773">arXiv:2304.05773</a> <span> [<a href="https://arxiv.org/pdf/2304.05773">pdf</a>, <a href="https://arxiv.org/ps/2304.05773">ps</a>, <a href="https://arxiv.org/format/2304.05773">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/10.1051/0004-6361/202346211">10.1051/0004-6361/202346211 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/?searchtype=author&query=Massa%2C+A">A. Massa</a>, <a href="/search/?searchtype=author&query=Mortier%2C+A">A. Mortier</a>, <a href="/search/?searchtype=author&query=Bongiolatti%2C+R">R. Bongiolatti</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Buchhave%2C+L+A">L. A. Buchhave</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/?searchtype=author&query=Morbidelli%2C+A">A. Morbidelli</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">D. W. Latham</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Pepe%2C+F">F. Pepe</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/?searchtype=author&query=Udry%2C+S">S. Udry</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Boschin%2C+W">W. Boschin</a>, <a href="/search/?searchtype=author&query=Charbonneau%2C+D">D. Charbonneau</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Cretignier%2C+M">M. Cretignier</a>, <a href="/search/?searchtype=author&query=Ghedina%2C+A">A. Ghedina</a>, <a href="/search/?searchtype=author&query=Lega%2C+E">E. Lega</a>, <a href="/search/?searchtype=author&query=L%C3%B3pez-Morales%2C+M">M. L贸pez-Morales</a>, <a href="/search/?searchtype=author&query=Margini%2C+M">M. Margini</a> , et al. (9 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="2304.05773v2-abstract-short" style="display: inline;"> The exoplanet population characterized by relatively short orbital periods ($P<100$ d) around solar-type stars is dominated by super-Earths and sub-Neptunes. However, these planets are missing in our Solar System and the reason behind this absence is still unknown. Two theoretical scenarios invoke the role of Jupiter as the possible culprit: Jupiter may have acted as a dynamical barrier to the inw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05773v2-abstract-full').style.display = 'inline'; document.getElementById('2304.05773v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.05773v2-abstract-full" style="display: none;"> The exoplanet population characterized by relatively short orbital periods ($P<100$ d) around solar-type stars is dominated by super-Earths and sub-Neptunes. However, these planets are missing in our Solar System and the reason behind this absence is still unknown. Two theoretical scenarios invoke the role of Jupiter as the possible culprit: Jupiter may have acted as a dynamical barrier to the inward migration of sub-Neptunes from beyond the water iceline; alternatively, Jupiter may have reduced considerably the inward flux of material (pebbles) required to form super-Earths inside that iceline. Both scenarios predict an anti-correlation between the presence of small planets (SPs) and that of cold Jupiters (CJs) in exoplanetary systems. To test that prediction, we homogeneously analyzed the radial-velocity (RV) measurements of 38 Kepler and K2 transiting SP systems gathered over almost 10 years with the HARPS-N spectrograph, as well as publicly available RVs collected with other facilities. We detected five CJs in three systems, two in Kepler-68, two in Kepler-454, and a very eccentric one in K2-312. We derived an occurrence rate of $9.3^{+7.7}_{-2.9}\%$ for CJs with $0.3-13~M_{Jup}$ and 1-10 AU, which is lower but still compatible at $1.3蟽$ with that measured from RV surveys for solar-type stars, regardless of the presence or absence of SPs. The sample is not large enough to draw a firm conclusion about the predicted anti-correlation between SPs and CJs; nevertheless, we found no evidence of previous claims of an excess of CJs in SP systems. As an important by-product of our analyses, we homogeneously determined the masses of 64 Kepler and K2 small planets, reaching a precision better than 5, 7.5 and 10$蟽$ for 25, 13 and 8 planets, respectively. Finally, we release the 3661 HARPS-N radial velocities used in this work to the scientific community. [Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05773v2-abstract-full').style.display = 'none'; document.getElementById('2304.05773v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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, 10 tables, published in Astronomy and Astrophysics. The updated version of the article takes into account the A&A language editing and guidelines. Tables 1, A.1 and full Table 2 are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A33</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 677, A33 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.04477">arXiv:2304.04477</a> <span> [<a href="https://arxiv.org/pdf/2304.04477">pdf</a>, <a href="https://arxiv.org/format/2304.04477">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/10.1051/0004-6361/202346096">10.1051/0004-6361/202346096 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS programme at TNG XLIII. A massive brown dwarf orbiting the active M dwarf TOI-5375 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/?searchtype=author&query=Petralia%2C+A">A. Petralia</a>, <a href="/search/?searchtype=author&query=Mantovan%2C+G">G. Mantovan</a>, <a href="/search/?searchtype=author&query=Rainer%2C+M">M. Rainer</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Di+Maio%2C+C">C. Di Maio</a>, <a href="/search/?searchtype=author&query=Colombo%2C+S">S. Colombo</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Lund%2C+M+B">M. B. Lund</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a> , et al. (1 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="2304.04477v2-abstract-short" style="display: inline;"> Context. Massive substellar companions orbiting active low-mass stars are rare. They, however, offer an excellent opportunity to study the main mechanisms involved in the formation and evolution of substellar objects. Aims. We aim to unravel the physical nature of the transit signal observed by the TESS space mission on the active M dwarf TOI-5375. Methods. We analysed the available TESS photometr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04477v2-abstract-full').style.display = 'inline'; document.getElementById('2304.04477v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.04477v2-abstract-full" style="display: none;"> Context. Massive substellar companions orbiting active low-mass stars are rare. They, however, offer an excellent opportunity to study the main mechanisms involved in the formation and evolution of substellar objects. Aims. We aim to unravel the physical nature of the transit signal observed by the TESS space mission on the active M dwarf TOI-5375. Methods. We analysed the available TESS photometric data as well as high-resolution (R $\sim$ 115000) HARPS-N spectra. We combined these data to characterise the star TOI-5375 and to disentangle signals related to stellar activity from the companion transit signal in the light-curve data. We ran an MCMC analysis to derive the orbital solution and apply state-of-the-art Gaussian process regression to deal with the stellar activity signal. Results. We reveal the presence of a companion in the brown dwarf / very-low-mass star boundary orbiting around the star TOI-5375. The best-fit model corresponds to a companion with an orbital period of 1.721564 $\pm$ 10$^{\rm -6}$ d, a mass of 77 $\pm$ 8 $M_{\rm J}$ and a radius of 0.99 $\pm$ 0.16 $R_{\rm J}$. Conclusions. We derive a rotation period for the host star of 1.9692 $\pm$ 0.0004 d, and we conclude that the star is very close to synchronising its rotation with the orbital period of the companion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04477v2-abstract-full').style.display = 'none'; document.getElementById('2304.04477v2-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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 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 674, A132 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.03328">arXiv:2304.03328</a> <span> [<a href="https://arxiv.org/pdf/2304.03328">pdf</a>, <a href="https://arxiv.org/format/2304.03328">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/10.1051/0004-6361/202245539">10.1051/0004-6361/202245539 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The PEPSI Exoplanet Transit Survey. III: The detection of FeI, CrI and TiI in the atmosphere of MASCARA-1 b through high-resolution emission spectroscopy </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=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">Th. Henning</a>, <a href="/search/?searchtype=author&query=Ilyin%2C+I">I. Ilyin</a>, <a href="/search/?searchtype=author&query=Johnson%2C+M+C">M. C. Johnson</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Mallonn%2C+M">M. Mallonn</a>, <a href="/search/?searchtype=author&query=Molaverdikhani%2C+K">K. Molaverdikhani</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Patience%2C+J">J. Patience</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Poppenhaeger%2C+K">K. Poppenhaeger</a>, <a href="/search/?searchtype=author&query=Schlawin%2C+E">E. Schlawin</a>, <a href="/search/?searchtype=author&query=Shkolnik%2C+E+L">E. L. Shkolnik</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">D. Sicilia</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Strassmeier%2C+K+G">K. G. Strassmeier</a>, <a href="/search/?searchtype=author&query=Veillet%2C+C">C. Veillet</a>, <a href="/search/?searchtype=author&query=Wang%2C+J">J. Wang</a>, <a href="/search/?searchtype=author&query=Yan%2C+F">F. Yan</a> </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="2304.03328v1-abstract-short" style="display: inline;"> Hot giant planets like MASCARA-1 b are expected to have thermally inverted atmospheres, that makes them perfect laboratory for the atmospheric characterization through high-resolution spectroscopy. Nonetheless, previous attempts of detecting the atmosphere of MASCARA-1 b in transmission have led to negative results. In this paper we aim at the detection of the optical emission spectrum of MASCAR… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.03328v1-abstract-full').style.display = 'inline'; document.getElementById('2304.03328v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.03328v1-abstract-full" style="display: none;"> Hot giant planets like MASCARA-1 b are expected to have thermally inverted atmospheres, that makes them perfect laboratory for the atmospheric characterization through high-resolution spectroscopy. Nonetheless, previous attempts of detecting the atmosphere of MASCARA-1 b in transmission have led to negative results. In this paper we aim at the detection of the optical emission spectrum of MASCARA-1 b. We used the high-resolution spectrograph PEPSI to observe MASCARA-1 (spectral type A8) near the secondary eclipse of the planet. We cross-correlated the spectra with synthetic templates computed for several atomic and molecular species. We obtained the detection of FeI, CrI and TiI in the atmosphere of MASCARA-1 b with a S/N ~7, 4 and 5 respectively, and confirmed the expected systemic velocity of ~13 km/s and the radial velocity semi-amplitude of MASCARA-1 b of ~200 km/s. The detection of Ti is of particular importance in the context of the recently proposed Ti cold-trapping below a certain planetary equilibrium temperature. We confirm the presence of an the atmosphere around MASCARA-1 b through emission spectroscopy. We conclude that the atmospheric non detection in transmission spectroscopy is due to the high gravity of the planet and/or to the overlap between the planetary track and its Doppler shadow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.03328v1-abstract-full').style.display = 'none'; document.getElementById('2304.03328v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A58 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.02779">arXiv:2304.02779</a> <span> [<a href="https://arxiv.org/pdf/2304.02779">pdf</a>, <a href="https://arxiv.org/format/2304.02779">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="Astrophysics of Galaxies">astro-ph.GA</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/10.3847/1538-3881/acca1c">10.3847/1538-3881/acca1c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mayo%2C+A+W">Andrew W. Mayo</a>, <a href="/search/?searchtype=author&query=Dressing%2C+C+D">Courtney D. Dressing</a>, <a href="/search/?searchtype=author&query=Vanderburg%2C+A">Andrew Vanderburg</a>, <a href="/search/?searchtype=author&query=Fortenbach%2C+C+D">Charles D. Fortenbach</a>, <a href="/search/?searchtype=author&query=Lienhard%2C+F">Florian Lienhard</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">Luca Malavolta</a>, <a href="/search/?searchtype=author&query=Mortier%2C+A">Annelies Mortier</a>, <a href="/search/?searchtype=author&query=N%C3%BA%C3%B1ez%2C+A">Alejandro N煤帽ez</a>, <a href="/search/?searchtype=author&query=Richey-Yowell%2C+T">Tyler Richey-Yowell</a>, <a href="/search/?searchtype=author&query=Turtelboom%2C+E+V">Emma V. Turtelboom</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">David W. Latham</a>, <a href="/search/?searchtype=author&query=L%C3%B3pez-Morales%2C+M">Mercedes L贸pez-Morales</a>, <a href="/search/?searchtype=author&query=Shkolnik%2C+E">Evgenya Shkolnik</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">Alessandro Sozzetti</a>, <a href="/search/?searchtype=author&query=Ag%C3%BCeros%2C+M+A">Marcel A. Ag眉eros</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">Luca Borsato</a>, <a href="/search/?searchtype=author&query=Charbonneau%2C+D">David Charbonneau</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">Rosario Cosentino</a>, <a href="/search/?searchtype=author&query=Douglas%2C+S+T">Stephanie T. Douglas</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">Xavier Dumusque</a>, <a href="/search/?searchtype=author&query=Ghedina%2C+A">Adriano Ghedina</a>, <a href="/search/?searchtype=author&query=Gibson%2C+R">Rose Gibson</a>, <a href="/search/?searchtype=author&query=Granata%2C+V">Valentina Granata</a>, <a href="/search/?searchtype=author&query=Harutyunyan%2C+A">Avet Harutyunyan</a> , et al. (17 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="2304.02779v1-abstract-short" style="display: inline;"> K2-136 is a late-K dwarf ($0.742\pm0.039$ M$_\odot$) in the Hyades open cluster with three known, transiting planets and an age of $650\pm70$ Myr. Analyzing K2 photometry, we found that planets K2-136b, c, and d have periods of $8.0$, $17.3$, and $25.6$ days and radii of $1.014\pm0.050$ R$_\oplus$, $3.00\pm0.13$ R$_\oplus$, and $1.565\pm0.077$ R$_\oplus$, respectively. We collected 93 radial veloc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02779v1-abstract-full').style.display = 'inline'; document.getElementById('2304.02779v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02779v1-abstract-full" style="display: none;"> K2-136 is a late-K dwarf ($0.742\pm0.039$ M$_\odot$) in the Hyades open cluster with three known, transiting planets and an age of $650\pm70$ Myr. Analyzing K2 photometry, we found that planets K2-136b, c, and d have periods of $8.0$, $17.3$, and $25.6$ days and radii of $1.014\pm0.050$ R$_\oplus$, $3.00\pm0.13$ R$_\oplus$, and $1.565\pm0.077$ R$_\oplus$, respectively. We collected 93 radial velocity measurements (RVs) with the HARPS-N spectrograph (TNG) and 22 RVs with the ESPRESSO spectrograph (VLT). Analyzing HARPS-N and ESPRESSO data jointly, we found K2-136c induced a semi-amplitude of $5.49\pm0.53$ m s$^{-1}$, corresponding to a mass of $18.1\pm1.9$ M$_\oplus$. We also placed $95$% upper mass limits on K2-136b and d of $4.3$ and $3.0$ M$_\oplus$, respectively. Further, we analyzed HST and XMM-Newton observations to establish the planetary high-energy environment and investigate possible atmospheric loss. K2-136c is now the smallest planet to have a measured mass in an open cluster and one of the youngest planets ever with a mass measurement. K2-136c has $\sim$75% the radius of Neptune but is similar in mass, yielding a density of $3.69^{+0.67}_{-0.56}$ g cm$^{-3}$ ($\sim$2-3 times denser than Neptune). Mass estimates for K2-136b (and possibly d) may be feasible with more RV observations, and insights into all three planets' atmospheres through transmission spectroscopy would be challenging but potentially fruitful. This research and future mass measurements of young planets are critical for investigating the compositions and characteristics of small exoplanets at very early stages of their lives and providing insights into how exoplanets evolve with time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02779v1-abstract-full').style.display = 'none'; document.getElementById('2304.02779v1-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> 5 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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 in AJ, 25 pages, 10 figures, 5 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/2303.15242">arXiv:2303.15242</a> <span> [<a href="https://arxiv.org/pdf/2303.15242">pdf</a>, <a href="https://arxiv.org/format/2303.15242">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/10.1051/0004-6361/202245391">10.1051/0004-6361/202245391 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG XLII. A characterisation study of the multi-planet system around the 400 Myr-old star HD 63433 (TOI-1726) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Locci%2C+D">D. Locci</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/?searchtype=author&query=Mallonn%2C+M">M. Mallonn</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Marzari%2C+F">F. Marzari</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Dolcetta%2C+R+C">R. Capuzzo Dolcetta</a>, <a href="/search/?searchtype=author&query=Cecconi%2C+M">M. Cecconi</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a> , et al. (12 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="2303.15242v1-abstract-short" style="display: inline;"> For more than two years, we monitored with the HARPS-N spectrograph the 400 Myr-old star HD\,63433, which hosts two close-in (orbital periods $P_b\sim7.1$ and $P_c\sim20.5$ days) sub-Neptunes detected by the TESS space telescope, and it was announced in 2020. Using radial velocities and additional TESS photometry, we aim to provide the first measurement of their masses, improve the measure of thei… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15242v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15242v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15242v1-abstract-full" style="display: none;"> For more than two years, we monitored with the HARPS-N spectrograph the 400 Myr-old star HD\,63433, which hosts two close-in (orbital periods $P_b\sim7.1$ and $P_c\sim20.5$ days) sub-Neptunes detected by the TESS space telescope, and it was announced in 2020. Using radial velocities and additional TESS photometry, we aim to provide the first measurement of their masses, improve the measure of their size and orbital parameters, and study the evolution of the atmospheric mass-loss rate due to photoevaporation. We tested state-of-the-art analysis techniques and different models to mitigate the dominant signals due to stellar activity that are detected in the radial velocity time series. We used a hydro-based analytical description of the atmospheric mass-loss rate, coupled with a core-envelope model and stellar evolutionary tracks, to study the past and future evolution of the planetary masses and radii. We derived new measurements of the planetary orbital periods and radii ($P_b=7.10794\pm0.000009$ d, $r_b=2.02^{+0.06}_{-0.05}$ $R_{\oplus}$; $P_c=20.54379\pm0.00002$ d, $r_c=2.44\pm0.07$ $R_{\oplus}$), and determined mass upper limits ($m_b\lesssim$11 $M_{\oplus}$; $m_c\lesssim$31 $M_{\oplus}$; 95$\%$ confidence level), with evidence at a 2.1--2.7$蟽$ significance level that HD\,63433\,c might be a dense mini-Neptune with a Neptune-like mass. For a grid of test masses below our derived dynamical upper limits, we found that HD\,63433\,b has very likely lost any gaseous H-He envelope, supporting HST-based observations that are indicative of there being no ongoing atmospheric evaporation. HD\,63433\,c will keep evaporating over the next $\sim$5 Gyr if its current mass is $m_c\lesssim$15 $M_{\oplus}$, while it should be hydrodynamically stable for higher masses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15242v1-abstract-full').style.display = 'none'; document.getElementById('2303.15242v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">22 pages, accepted for publication on 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/2211.05196">arXiv:2211.05196</a> <span> [<a href="https://arxiv.org/pdf/2211.05196">pdf</a>, <a href="https://arxiv.org/format/2211.05196">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/10.3847/1538-3881/aca64d">10.3847/1538-3881/aca64d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Kepler-102: Masses and Compositions for a Super-Earth and Sub-Neptune Orbiting an Active Star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Brinkman%2C+C">Casey Brinkman</a>, <a href="/search/?searchtype=author&query=Cadman%2C+J">James Cadman</a>, <a href="/search/?searchtype=author&query=Weiss%2C+L">Lauren Weiss</a>, <a href="/search/?searchtype=author&query=Gaidos%2C+E">Eric Gaidos</a>, <a href="/search/?searchtype=author&query=Rice%2C+K">Ken Rice</a>, <a href="/search/?searchtype=author&query=Huber%2C+D">Daniel Huber</a>, <a href="/search/?searchtype=author&query=Claytor%2C+Z+R">Zachary R. Claytor</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</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=Cosentino%2C+R">Rosario Cosentino</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">Xavier Dumusque</a>, <a href="/search/?searchtype=author&query=Fiorenzano%2C+A+F+M">Aldo F Martinez Fiorenzano</a>, <a href="/search/?searchtype=author&query=Ghedina%2C+A">Adriano Ghedina</a>, <a href="/search/?searchtype=author&query=Harutyunyan%2C+A">Avet Harutyunyan</a>, <a href="/search/?searchtype=author&query=Howard%2C+A">Andrew Howard</a>, <a href="/search/?searchtype=author&query=Isaacson%2C+H">Howard Isaacson</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">David W. Latham</a>, <a href="/search/?searchtype=author&query=Lopez-Morales%2C+M">Mercedes Lopez-Morales</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">Luca Malavolta</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">Giuseppina Micela</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">Emilio Molinari</a>, <a href="/search/?searchtype=author&query=Pepe%2C+F">Francesco Pepe</a>, <a href="/search/?searchtype=author&query=Philips%2C+D+F">David F Philips</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">Ennio Poretti</a> , et al. (2 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="2211.05196v1-abstract-short" style="display: inline;"> Radial velocity (RV) measurements of transiting multiplanet systems allow us to understand the densities and compositions of planets unlike those in the Solar System. Kepler-102, which consists of 5 tightly packed transiting planets, is a particularly interesting system since it includes a super-Earth (Kepler-102d) and a sub-Neptune-sized planet (Kepler-102e) for which masses can be measured using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.05196v1-abstract-full').style.display = 'inline'; document.getElementById('2211.05196v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.05196v1-abstract-full" style="display: none;"> Radial velocity (RV) measurements of transiting multiplanet systems allow us to understand the densities and compositions of planets unlike those in the Solar System. Kepler-102, which consists of 5 tightly packed transiting planets, is a particularly interesting system since it includes a super-Earth (Kepler-102d) and a sub-Neptune-sized planet (Kepler-102e) for which masses can be measured using radial velocities. Previous work found a high density for Kepler-102d, suggesting a composition similar to that of Mercury, while Kepler-102e was found to have a density typical of sub-Neptune size planets; however, Kepler-102 is an active star, which can interfere with RV mass measurements. To better measure the mass of these two planets, we obtained 111 new RVs using Keck/HIRES and TNG/HARPS-N and modeled Kepler-102's activity using quasi-periodic Gaussian Process Regression. For Kepler-102d, we report a mass upper limit of M$_{d} < $5.3 M$_{\oplus}$ [95\% confidence], a best-fit mass of M$_{d}$=2.5 $\pm$ 1.4 M$_{\oplus}$, and a density of $蟻_{d}$=5.6 $\pm$ 3.2 g/cm$^{3}$ which is consistent with a rocky composition similar in density to the Earth. For Kepler-102e we report a mass of M$_{e}$=4.7 $\pm$ 1.7 M$_{\oplus}$ and a density of $蟻_{e}$=1.8 $\pm$ 0.7 g/cm$^{3}$. These measurements suggest that Kepler-102e has a rocky core with a thick gaseous envelope comprising 2-4% of the planet mass and 16-50% of its radius. Our study is yet another demonstration that accounting for stellar activity in stars with clear rotation signals can yield more accurate planet masses, enabling a more realistic interpretation of planet interiors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.05196v1-abstract-full').style.display = 'none'; document.getElementById('2211.05196v1-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> 9 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 AJ 11/08/2022</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.12211">arXiv:2210.12211</a> <span> [<a href="https://arxiv.org/pdf/2210.12211">pdf</a>, <a href="https://arxiv.org/format/2210.12211">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/10.3847/1538-3881/ac9ccd">10.3847/1538-3881/ac9ccd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Independent validation of the temperate Super-Earth HD79211 b using HARPS-N </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DiTomasso%2C+V">Victoria DiTomasso</a>, <a href="/search/?searchtype=author&query=Nava%2C+C">Chantanelle Nava</a>, <a href="/search/?searchtype=author&query=L%C3%B3pez-Morales%2C+M">Mercedes L贸pez-Morales</a>, <a href="/search/?searchtype=author&query=Bieryla%2C+A">Allyson Bieryla</a>, <a href="/search/?searchtype=author&query=Cloutier%2C+R">Ryan Cloutier</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">Luca Malavolta</a>, <a href="/search/?searchtype=author&query=Mortier%2C+A">Annelies Mortier</a>, <a href="/search/?searchtype=author&query=Buchhave%2C+L+A">Lars A. Buchhave</a>, <a href="/search/?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">Alessandro Sozzetti</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo Stefano Bonomo</a>, <a href="/search/?searchtype=author&query=Charbonneau%2C+D">David Charbonneau</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">Andrew Collier Cameron</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">Rosario Cosentino</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">Mario Damasso</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">Xavier Dumusque</a>, <a href="/search/?searchtype=author&query=Fiorenzano%2C+A+F+M">A. F. Mart铆nez Fiorenzano</a>, <a href="/search/?searchtype=author&query=Ghedina%2C+A">Adriano Ghedina</a>, <a href="/search/?searchtype=author&query=Harutyunyan%2C+A">Avet Harutyunyan</a>, <a href="/search/?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/?searchtype=author&query=Latham%2C+D">David Latham</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">Emilio Molinari</a>, <a href="/search/?searchtype=author&query=Pepe%2C+F+A">Francesco A. Pepe</a>, <a href="/search/?searchtype=author&query=Pinamonti%2C+M">Matteo Pinamonti</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">Ennio Poretti</a> , et al. (6 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="2210.12211v1-abstract-short" style="display: inline;"> We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of $24.421^{+0.016}_{-0.017}$ days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12211v1-abstract-full').style.display = 'inline'; document.getElementById('2210.12211v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.12211v1-abstract-full" style="display: none;"> We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of $24.421^{+0.016}_{-0.017}$ days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to $P=24.422\pm0.014$ days, $K=3.19\pm0.27$ m/s, $M$ sin $i = 10.6 \pm 1.2 M_\oplus$, and $a = 0.142 \pm0.005$ au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12211v1-abstract-full').style.display = 'none'; document.getElementById('2210.12211v1-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> 21 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">Accepted for publication in AJ, 29 pages, 17 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/2209.11735">arXiv:2209.11735</a> <span> [<a href="https://arxiv.org/pdf/2209.11735">pdf</a>, <a href="https://arxiv.org/format/2209.11735">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/10.1051/0004-6361/202244593">10.1051/0004-6361/202244593 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG. XLI. The climate of KELT-9b revealed with a new approach to high spectral resolution phase curves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=D%C3%A9sert%2C+J+M">J. M. D茅sert</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Rauscher%2C+E">E. Rauscher</a>, <a href="/search/?searchtype=author&query=Basilicata%2C+M">M. Basilicata</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Covino%2C+E">E. Covino</a>, <a href="/search/?searchtype=author&query=Di+Mauro%2C+M+P">M. P. Di Mauro</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Molinaro%2C+M">M. Molinaro</a>, <a href="/search/?searchtype=author&query=Montalto%2C+M">M. Montalto</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Pedani%2C+M">M. Pedani</a>, <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/?searchtype=author&query=Rainer%2C+M">M. Rainer</a> , et al. (3 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="2209.11735v1-abstract-short" style="display: inline;"> [Abridged] We present a novel method to study the thermal emission of exoplanets as a function of orbital phase at very high spectral resolution, and apply it to investigate the climate of the ultra-hot Jupiter KELT-9b. We combine 3 nights of HARPS-N and 2 nights of CARMENES optical spectra, covering orbital phases between quadratures (0.25 < phi < 0.75), when the planet shows its day-side hemisph… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.11735v1-abstract-full').style.display = 'inline'; document.getElementById('2209.11735v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.11735v1-abstract-full" style="display: none;"> [Abridged] We present a novel method to study the thermal emission of exoplanets as a function of orbital phase at very high spectral resolution, and apply it to investigate the climate of the ultra-hot Jupiter KELT-9b. We combine 3 nights of HARPS-N and 2 nights of CARMENES optical spectra, covering orbital phases between quadratures (0.25 < phi < 0.75), when the planet shows its day-side hemisphere with different geometries. We co-add the signal of thousands of FeI lines through cross-correlation, which we map to a likelihood function. We investigate the phase-dependence of: (i) the line depths of FeI, and (ii) their Doppler shifts, by introducing a new method that exploits the very high spectral resolution of our observations. We confirm a previous detection of FeI emission and demonstrate a combined precision of 0.5 km s-1 on the orbital properties of KELT-9b. By studying the phase-resolved Doppler shift of FeI lines, we detect an anomaly in the planet's orbital radial velocity well-fitted with a slightly eccentric orbit (e = 0.016$\pm$0.003, w = 150$^{+13\circ}_{-11},~5蟽$ preference). However, we argue that such anomaly can be explained by a day-night wind of a few km s-1 blowing neutral iron gas. Additionally, we find that the FeI emission line depths are symmetric around the substellar point within 10 deg ($2蟽$). We show that these results are qualitatively compatible with predictions from general circulation models for ultra-hot Jupiter planets. Very high-resolution spectroscopy phase curves have the sensitivity to reveal a phase dependence in both the line depths and their Doppler shifts throughout the orbit. They are highly complementary to space-based phase curves obtained with HST and JWST, and open a new window into the still poorly understood climate and atmospheric structure of the hottest planets known. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.11735v1-abstract-full').style.display = 'none'; document.getElementById('2209.11735v1-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 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">Recommended for publication on A&A after referee report, awaiting acceptance. 25 pages, 19 figures, 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 668, A176 (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/2207.09761">arXiv:2207.09761</a> <span> [<a href="https://arxiv.org/pdf/2207.09761">pdf</a>, <a href="https://arxiv.org/format/2207.09761">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/10.3847/1538-3881/ac80bf">10.3847/1538-3881/ac80bf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG XXXIX -- Multiple molecular species in the atmosphere of the warm giant planet WASP-80 b unveiled at high resolution with GIANO-B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Carleo%2C+I">Ilaria Carleo</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">Paolo Giacobbe</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">Gloria Guilluy</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">Patricio E. Cubillos</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">Alessandro Sozzetti</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">Matteo Brogi</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+S">Siddharth Gandhi</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">Luca Fossati</a>, <a href="/search/?searchtype=author&query=Turrini%2C+D">Diego Turrini</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">Katia Biazzo</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">Francesco Borsa</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">Antonino F. Lanza</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">Luca Malavolta</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">Antonio Maggio</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">Luigi Mancini</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">Giusi Micela</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">Lorenzo Pino</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">Ennio Poretti</a>, <a href="/search/?searchtype=author&query=Rainer%2C+M">Monica Rainer</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">Gaetano Scandariato</a>, <a href="/search/?searchtype=author&query=Schisano%2C+E">Eugenio Schisano</a>, <a href="/search/?searchtype=author&query=Andreuzzi%2C+G">Gloria Andreuzzi</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">Andrea Bignamini</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">Rosario Cosentino</a> , et al. (6 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="2207.09761v1-abstract-short" style="display: inline;"> Detections of molecules in the atmosphere of gas giant exoplanets allow us to investigate the physico-chemical properties of the atmospheres. Their inferred chemical composition is used as tracer of planet formation and evolution mechanisms. Currently, an increasing number of detections is showing a possible rich chemistry of the hotter gaseous planets, but whether this extends to cooler giants is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09761v1-abstract-full').style.display = 'inline'; document.getElementById('2207.09761v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.09761v1-abstract-full" style="display: none;"> Detections of molecules in the atmosphere of gas giant exoplanets allow us to investigate the physico-chemical properties of the atmospheres. Their inferred chemical composition is used as tracer of planet formation and evolution mechanisms. Currently, an increasing number of detections is showing a possible rich chemistry of the hotter gaseous planets, but whether this extends to cooler giants is still unknown. We observed four transits of WASP-80 b, a warm transiting giant planet orbiting a late-K dwarf star with the near-infrared GIANO-B spectrograph installed at the Telescopio Nazionale Galileo and performed high resolution transmission spectroscopy analysis. We report the detection of several molecular species in its atmosphere. Combining the four nights and comparing our transmission spectrum to planetary atmosphere models containing the signature of individual molecules within the cross-correlation framework, we find the presence of H2O, CH4, NH3 and HCN with high significance, tentative detection of CO2, and inconclusive results for C2H2 and CO. A qualitative interpretation of these results, using physically motivated models, suggests an atmosphere consistent with solar composition and the presence of disequilibrium chemistry and we therefore recommend the inclusion of the latter in future modelling of sub-1000K planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09761v1-abstract-full').style.display = 'none'; document.getElementById('2207.09761v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">12 pages, 4 figures. AJ, Accepted July 11th, 2022</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.09760">arXiv:2207.09760</a> <span> [<a href="https://arxiv.org/pdf/2207.09760">pdf</a>, <a href="https://arxiv.org/format/2207.09760">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/10.1051/0004-6361/202243854">10.1051/0004-6361/202243854 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG XXXVIII. Five molecules in the atmosphere of the warm giant planet WASP-69b detected at high spectral resolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Cubillos%2C+P+E">P. E. Cubillos</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+S">S. Gandhi</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Turrini%2C+D">D. Turrini</a>, <a href="/search/?searchtype=author&query=Schisano%2C+E">E. Schisano</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Rainer%2C+M">M. Rainer</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Covino%2C+E">E. Covino</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a> , et al. (10 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="2207.09760v2-abstract-short" style="display: inline;"> The field of exo-atmospheric characterisation is progressing at an extraordinary pace. Atmospheric observations are now available for tens of exoplanets, mainly hot and warm inflated gas giants, and new molecular species continue to be detected revealing a richer atmospheric composition than previously expected. Thanks to its warm equilibrium temperature (963$\pm$18~K) and low-density (0.219$\pm$0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09760v2-abstract-full').style.display = 'inline'; document.getElementById('2207.09760v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.09760v2-abstract-full" style="display: none;"> The field of exo-atmospheric characterisation is progressing at an extraordinary pace. Atmospheric observations are now available for tens of exoplanets, mainly hot and warm inflated gas giants, and new molecular species continue to be detected revealing a richer atmospheric composition than previously expected. Thanks to its warm equilibrium temperature (963$\pm$18~K) and low-density (0.219$\pm$0.031~g cm$^{-3}$), the close-in gas giant WASP-69b represents a golden target for atmospheric characterization. With the aim of searching for molecules in the atmosphere of WASP-69b and investigating its properties, we performed high-resolution transmission spectroscopy with the GIANO-B near-infrared spectrograph at the Telescopio Nazionale Galileo. We observed three transit events of WASP-69b. During a transit, the planetary lines are Doppler-shifted due to the large change in the planet's radial velocity, allowing us to separate the planetary signal from the quasi-stationary telluric and stellar spectrum. Considering the three nights together, we report the detection of CH$_4$, NH$_3$, CO, C$_2$H$_2$, and H$_2$O, at more than $3.3蟽$ level. We did not identify the presence of HCN and CO$_2$ with confidence level higher than 3$蟽$. This is the first time that five molecules are simultaneously detected in the atmosphere of a warm giant planet. These results suggest that the atmosphere of WASP-69b is possibly carbon-rich and characterised by the presence of disequilibrium chemistry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09760v2-abstract-full').style.display = 'none'; document.getElementById('2207.09760v2-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> 21 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">10 pages, 5 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 665, A104 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.03293">arXiv:2207.03293</a> <span> [<a href="https://arxiv.org/pdf/2207.03293">pdf</a>, <a href="https://arxiv.org/format/2207.03293">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/10.1051/0004-6361/202244079">10.1051/0004-6361/202244079 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG XL: A puffy and warm Neptune-sized planet and an outer Neptune-mass candidate orbiting the solar-type star TOI-1422 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Naponiello%2C+L">L. Naponiello</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Stognone%2C+R+G">R. G. Stognone</a>, <a href="/search/?searchtype=author&query=Lillo-Box%2C+J">J. Lillo-Box</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/?searchtype=author&query=Lissauer%2C+J+J">J. J. Lissauer</a>, <a href="/search/?searchtype=author&query=Zeng%2C+L">L. Zeng</a>, <a href="/search/?searchtype=author&query=Bieryla%2C+A">A. Bieryla</a>, <a href="/search/?searchtype=author&query=H%C3%A9brard%2C+G">G. H茅brard</a>, <a href="/search/?searchtype=author&query=Basilicata%2C+M">M. Basilicata</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Covino%2C+E">E. Covino</a>, <a href="/search/?searchtype=author&query=de+Gurtubai%2C+A">A. de Gurtubai</a>, <a href="/search/?searchtype=author&query=Delfosse%2C+X">X. Delfosse</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a> , et al. (33 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="2207.03293v2-abstract-short" style="display: inline;"> We investigate the exoplanet candidate TOI-1422b, which was discovered by the TESS space telescope around the high proper-motion G2V star TOI-1422 ($V=10.6$ mag), 155pc away, with the primary goal of confirming its planetary nature and characterising its properties. We monitored TOI-1422 with the HARPS-N spectrograph for 1.5 years to precisely quantify its radial velocity variation. The radial vel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03293v2-abstract-full').style.display = 'inline'; document.getElementById('2207.03293v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.03293v2-abstract-full" style="display: none;"> We investigate the exoplanet candidate TOI-1422b, which was discovered by the TESS space telescope around the high proper-motion G2V star TOI-1422 ($V=10.6$ mag), 155pc away, with the primary goal of confirming its planetary nature and characterising its properties. We monitored TOI-1422 with the HARPS-N spectrograph for 1.5 years to precisely quantify its radial velocity variation. The radial velocity measurements are analyzed jointly with TESS photometry and we also check for blended companions through high-spatial resolution images using the AstraLux instrument. We estimate that the parent star has a radius and a mass of $R^*=1.019_{-0.013}^{+0.014} R_{\odot}$, $M^*=0.981_{-0.065}^{+0.062} M_{\odot}$, respectively. Our analysis confirms the planetary nature of TOI-1422b and also suggests the presence of a Neptune-mass planet on a more distant orbit, the candidate TOI-1422c, which is not detected in TESS light curves. The inner planet, TOI-1422b, orbits on a period $P_{\rm b}=12.9972\pm0.0006$ days and has an equilibrium temperature $T_{\rm eq, b}=867\pm17$ K. With a radius of $R_{\rm b}=3.96^{+0.13}_{-0.11} R_{\oplus}$, a mass of $M_{\rm b}=9.0^{+2.3}_{-2.0} M_{\oplus}$ and, consequently, a density of $蟻_{\rm b}=0.795^{+0.290}_{-0.235}$ g cm$^{-3}$, it can be considered a warm Neptune-size planet. Compared to other exoplanets of similar mass range, TOI-1422b is among the most inflated ones and we expect this planet to have an extensive gaseous envelope that surrounds a core with a mass fraction around $10\%-25\%$ of the total mass of the planet. The outer non-transiting planet candidate, TOI-1422c, has an orbital period of $P_{\rm c}=29.29^{+0.21}_{-0.20}$ days, a minimum mass, $M_{\rm c}\sin{i}$, of $11.1^{+2.6}_{-2.3} M_{\oplus}$, an equilibrium temperature of $T_{\rm eq, c}=661\pm13$ K and, therefore, if confirmed, it could be considered as another warm Neptune. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03293v2-abstract-full').style.display = 'none'; document.getElementById('2207.03293v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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, 20 figures, 6 tables. Accepted for publication in Astronomy & Astrophysics on July 7, 2022. Abstract abridged</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> aa44079-22 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A8 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.03496">arXiv:2206.03496</a> <span> [<a href="https://arxiv.org/pdf/2206.03496">pdf</a>, <a href="https://arxiv.org/ps/2206.03496">ps</a>, <a href="https://arxiv.org/format/2206.03496">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/10.1051/0004-6361/202243743">10.1051/0004-6361/202243743 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme with HARPS-N at TNG. XXXVII. A precise density measurement of the young ultra-short period planet TOI-1807 b </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/?searchtype=author&query=Messina%2C+S">S. Messina</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Rajpaul%2C+V+M">V. M. Rajpaul</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Dolcetta%2C+R+C">R. Capuzzo Dolcetta</a>, <a href="/search/?searchtype=author&query=Mallonn%2C+M">M. Mallonn</a>, <a href="/search/?searchtype=author&query=Cale%2C+B">B. Cale</a>, <a href="/search/?searchtype=author&query=Plavchan%2C+P">P. Plavchan</a>, <a href="/search/?searchtype=author&query=Mufti%2C+M+E">M. El Mufti</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Covino%2C+E">E. Covino</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a> , et al. (16 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="2206.03496v1-abstract-short" style="display: inline;"> Great strides have been made in recent years in the understanding of the mechanisms involved in the formation and evolution of planetary systems; despite this, many observational facts still do not have an explanation. A great contribution to the study of planetary formation processes comes from the study of young, low-mass planets, with short orbital periods. In the last years, the TESS satellite… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.03496v1-abstract-full').style.display = 'inline'; document.getElementById('2206.03496v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.03496v1-abstract-full" style="display: none;"> Great strides have been made in recent years in the understanding of the mechanisms involved in the formation and evolution of planetary systems; despite this, many observational facts still do not have an explanation. A great contribution to the study of planetary formation processes comes from the study of young, low-mass planets, with short orbital periods. In the last years, the TESS satellite has identified many planets of this kind, and their characterization is mandatory to understand how they formed and evolved. Within the framework of the GAPS project, we performed the validation and characterization of the ultra-short period planet (USPP) TOI-1807b, orbiting its young host star BD+39 2643 (~300 Myr) in only 13 hours. This is the youngest USPP discovered so far. Thanks to a joint modeling of the stellar activity and planetary signals in the TESS light curve and in HARPS-N radial-velocity measurements, combined with accurate estimation of stellar parameters, we validated the planetary nature of TOI-1807b and measured its orbital and physical parameters. By using astrometric, photometric, and spectroscopic observations we found that BD+39 2643 is a young, active K dwarf star, member of a 300+/-80 Myr old moving group and that it rotates in Prot=8.8+/-0.1 days. This star hosts an USPP with an orbital period of only P_b=0.54937+/-0.00001 d. Thanks to the exquisite photometric and spectroscopic series, and the accurate information on the stellar activity, we measured both the radius and the mass of TOI-1807b with high precision, obtaining R_b=1.37+/-0.09 R_Earth and M_b=2.57+/-0.50 M_Earth. These planet parameters correspond to a rocky planet with an Earth-like density and no extended H/He envelope. From the analysis of the age-R_P distribution for planets with well measured ages, we inferred that TOI-1807b may have already lost a large part of its atmosphere during its 300 Myr life. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.03496v1-abstract-full').style.display = 'none'; document.getElementById('2206.03496v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">33 pages, 17 figures, 11 tables. Accepted for publication in Astronomy & Astrophysics on June 3, 2022. Electronic material (light curves, spectroscopic series, table B1) will soon be available on the CDS or upon request to the first author. Abstract shortened</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A163 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.15796">arXiv:2205.15796</a> <span> [<a href="https://arxiv.org/pdf/2205.15796">pdf</a>, <a href="https://arxiv.org/ps/2205.15796">ps</a>, <a href="https://arxiv.org/format/2205.15796">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/10.1051/0004-6361/202243467">10.1051/0004-6361/202243467 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme with HARPS-N at TNG. XXXV. Fundamental properties of transiting exoplanet host stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Turrini%2C+D">D. Turrini</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Gratton%2C+R">R. Gratton</a>, <a href="/search/?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Covino%2C+E">E. Covino</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Di+Mauro%2C+M+P">M. P. Di Mauro</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/?searchtype=author&query=Marzari%2C+F">F. Marzari</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/?searchtype=author&query=Vitello%2C+F">F. Vitello</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a> , et al. (16 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="2205.15796v1-abstract-short" style="display: inline;"> Exoplanetary properties depend on stellar properties: to know the planet with accuracy and precision it is necessary to know the star as accurately and precisely as possible. Our immediate aim is to characterize in a homogeneous and accurate way a sample of 27 transiting planet-hosting stars observed within the GAPS program. We determined stellar parameters (effective temperature, surface gravity,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.15796v1-abstract-full').style.display = 'inline'; document.getElementById('2205.15796v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.15796v1-abstract-full" style="display: none;"> Exoplanetary properties depend on stellar properties: to know the planet with accuracy and precision it is necessary to know the star as accurately and precisely as possible. Our immediate aim is to characterize in a homogeneous and accurate way a sample of 27 transiting planet-hosting stars observed within the GAPS program. We determined stellar parameters (effective temperature, surface gravity, rotational velocity) and abundances of 26 elements (Li,C,N,O,Na,Mg,Al,Si,S,Ca,Sc,Ti,V,Cr,Fe,Mn,Co,Ni,Cu,Zn,Y,Zr,Ba,La,Nd,Eu). Our study is based on high-resolution HARPS-N@TNG and FEROS@ESO spectra and uniform techniques. We derived kinematic properties from Gaia data and estimated for the first time in exoplanet host stars ages using elemental ratios as chemical clocks. Teff of our stars is of 4400-6700 K, while [Fe/H] is within -0.3 and 0.4 dex. Lithium is present in 7 stars. [X/H] and [X/Fe] abundances vs [Fe/H] are consistent with the Galactic Chemical Evolution. The dependence of [X/Fe] with the condensation temperature is critically analyzed with respect to stellar and kinematic properties. All targets with measured C and O abundances show C/O<0.8, compatible with Si present in rock-forming minerals. Most of targets show 1.0<Mg/Si<1.5, compatible with Mg distributed between olivine and pyroxene. HAT-P-26, the target hosting the lowest-mass planet, shows the highest Mg/Si ratio. From our chemo-dinamical analysis we find agreement between ages and position within the Galactic disk. We note a tendency for higher density planets to be around metal-rich stars and hints of higher stellar abundances of some volatiles for lower mass planets. We cannot exclude that part of our results could be also related to the location of the stars within the Galactic disk. We trace the planetary migration scenario from the composition of the planets related to the chemical composition of the hosting stars <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.15796v1-abstract-full').style.display = 'none'; document.getElementById('2205.15796v1-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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 for publication in A&A. 31 pages, 19 figures, 10 tables. Abstract shortened</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A161 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.12162">arXiv:2205.12162</a> <span> [<a href="https://arxiv.org/pdf/2205.12162">pdf</a>, <a href="https://arxiv.org/format/2205.12162">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/10.3847/1538-3881/acb7e2">10.3847/1538-3881/acb7e2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Johnson%2C+M+C">Marshall C. Johnson</a>, <a href="/search/?searchtype=author&query=Wang%2C+J">Ji Wang</a>, <a href="/search/?searchtype=author&query=Asnodkar%2C+A+P">Anusha Pai Asnodkar</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</a>, <a href="/search/?searchtype=author&query=Gaudi%2C+B+S">B. Scott Gaudi</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/?searchtype=author&query=Ilyin%2C+I">Ilya Ilyin</a>, <a href="/search/?searchtype=author&query=Keles%2C+E">Engin Keles</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">Luca Malavolta</a>, <a href="/search/?searchtype=author&query=Mallonn%2C+M">Matthias Mallonn</a>, <a href="/search/?searchtype=author&query=Molaverdikhani%2C+K">Karan Molaverdikhani</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">Valerio Nascimbeni</a>, <a href="/search/?searchtype=author&query=Patience%2C+J">Jennifer Patience</a>, <a href="/search/?searchtype=author&query=Poppenhaeger%2C+K">Katja Poppenhaeger</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">Gaetano Scandariato</a>, <a href="/search/?searchtype=author&query=Schlawin%2C+E">Everett Schlawin</a>, <a href="/search/?searchtype=author&query=Shkolnik%2C+E">Evgenya Shkolnik</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">Daniela Sicilia</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">Alessandro Sozzetti</a>, <a href="/search/?searchtype=author&query=Strassmeier%2C+K+G">Klaus G. Strassmeier</a>, <a href="/search/?searchtype=author&query=Veillet%2C+C">Christian Veillet</a>, <a href="/search/?searchtype=author&query=Yan%2C+F">Fei Yan</a> </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="2205.12162v2-abstract-short" style="display: inline;"> Recent observations have shown that the atmospheres of ultra hot Jupiters (UHJs) commonly possess temperature inversions, where the temperature increases with increasing altitude. Nonetheless, which opacity sources are responsible for the presence of these inversions remains largely observationally unconstrained. We used LBT/PEPSI to observe the atmosphere of the UHJ KELT-20 b in both transmission… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12162v2-abstract-full').style.display = 'inline'; document.getElementById('2205.12162v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.12162v2-abstract-full" style="display: none;"> Recent observations have shown that the atmospheres of ultra hot Jupiters (UHJs) commonly possess temperature inversions, where the temperature increases with increasing altitude. Nonetheless, which opacity sources are responsible for the presence of these inversions remains largely observationally unconstrained. We used LBT/PEPSI to observe the atmosphere of the UHJ KELT-20 b in both transmission and emission in order to search for molecular agents which could be responsible for the temperature inversion. We validate our methodology by confirming previous detections of Fe I in emission at $16.9蟽$. Our search for the inversion agents TiO, VO, FeH, and CaH results in non-detections. Using injection-recovery testing we set $4蟽$ upper limits upon the volume mixing ratios for these constituents as low as $\sim1\times10^{-9}$ for TiO. For TiO, VO, and CaH, our limits are much lower than expectations from an equilibrium chemical model, while we cannot set constraining limits on FeH with our data. We thus rule out TiO and CaH as the source of the temperature inversion in KELT-20 b, and VO only if the line lists are sufficiently accurate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12162v2-abstract-full').style.display = 'none'; document.getElementById('2205.12162v2-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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, 11 figures. Accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.10549">arXiv:2205.10549</a> <span> [<a href="https://arxiv.org/pdf/2205.10549">pdf</a>, <a href="https://arxiv.org/ps/2205.10549">ps</a>, <a href="https://arxiv.org/format/2205.10549">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/10.1051/0004-6361/202243742">10.1051/0004-6361/202243742 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG: XXXVI. Measurement of the Rossiter-McLaughlin effect and revising the physical and orbital parameters of the HAT-P-15, HAT-P-17, HAT-P-21, HAT-P-26, HAT-P-29 eccentric planetary systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Esposito%2C+M">M. Esposito</a>, <a href="/search/?searchtype=author&query=Covino%2C+E">E. Covino</a>, <a href="/search/?searchtype=author&query=Southworth%2C+J">J. Southworth</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/?searchtype=author&query=Andreuzzi%2C+G">G. Andreuzzi</a>, <a href="/search/?searchtype=author&query=Barbato%2C+D">D. Barbato</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Bruni%2C+I">I. Bruni</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Di+Fabrizio%2C+L">L. Di Fabrizio</a>, <a href="/search/?searchtype=author&query=Evans%2C+D+F">D. F. Evans</a>, <a href="/search/?searchtype=author&query=Granata%2C+V">V. Granata</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Naponiello%2C+L">L. Naponiello</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Pinamonti%2C+M">M. Pinamonti</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Tregloan-Reed%2C+J">J. Tregloan-Reed</a>, <a href="/search/?searchtype=author&query=Basilicata%2C+M">M. Basilicata</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a> , et al. (12 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="2205.10549v2-abstract-short" style="display: inline;"> Aim: We aim to refine the orbital and physical parameters and determine the sky-projected planet orbital obliquity of five eccentric transiting planetary systems: HAT-P-15, HAT-P-17, HAT-P-21, HAT-P-26, and HAT-P-29. Each of the systems hosts a hot Jupiter, except for HAT-P-26 which hosts a Neptune-mass planet. Methods: We observed transit events of these planets with the HARPS-N spectrograph, obt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10549v2-abstract-full').style.display = 'inline'; document.getElementById('2205.10549v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.10549v2-abstract-full" style="display: none;"> Aim: We aim to refine the orbital and physical parameters and determine the sky-projected planet orbital obliquity of five eccentric transiting planetary systems: HAT-P-15, HAT-P-17, HAT-P-21, HAT-P-26, and HAT-P-29. Each of the systems hosts a hot Jupiter, except for HAT-P-26 which hosts a Neptune-mass planet. Methods: We observed transit events of these planets with the HARPS-N spectrograph, obtaining high-precision radial velocity measurements that allow us to measure the Rossiter-McLaughlin effect for each of the target systems. We used these new HARPS-N spectra and archival data, including those from Gaia, to better characterise the stellar atmospheric parameters. The photometric parameters for four of the hot Jupiters were recalculated using 17 new transit light curves, obtained with an array of medium-class telescopes, and data from the TESS space telescope. HATNet time-series photometric data were checked for the signatures of rotation periods of the target stars and their spin axis inclination. Results: From the analysis of the Rossiter-McLaughlin effect, we derived a sky-projected obliquity of 13, -26.3, -0.7, -26 degree for HAT-P-15b, HAT-P-17b, HAT-P-21b and HAT-P-29b, respectively. Due to the quality of the data, we were not able to well constrain the sky-projected obliquity for HAT-P-26b, although a prograde orbit is favoured. The stellar activity of HAT-P-21 indicates a rotation period of 15.88 days, which allowed us to determine its true misalignment angle (25 degree). Our new analysis of the physical parameters of the five exoplanetary systems returned values compatible with those existing in the literature. Using TESS and the available transit light curves, we reviewed the orbital ephemeris for the five systems and confirmed that the HAT-P-26 system shows transit timing variations, which may tentatively be attributed to the presence of a third body. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10549v2-abstract-full').style.display = 'none'; document.getElementById('2205.10549v2-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> 13 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">31 pages, 16 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 664, A162 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.08984">arXiv:2204.08984</a> <span> [<a href="https://arxiv.org/pdf/2204.08984">pdf</a>, <a href="https://arxiv.org/format/2204.08984">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/10.1051/0004-6361/202143002">10.1051/0004-6361/202143002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE and HARPS-N </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=K%C3%B6nig%2C+P+-">P. -C. K枚nig</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=H%C3%A9brard%2C+G">G. H茅brard</a>, <a href="/search/?searchtype=author&query=Naponiello%2C+L">L. Naponiello</a>, <a href="/search/?searchtype=author&query=Cort%C3%A9s-Zuleta%2C+P">P. Cort茅s-Zuleta</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=%C3%89tangs%2C+A+L+d">A. Lecavelier des 脡tangs</a>, <a href="/search/?searchtype=author&query=Zeng%2C+L">L. Zeng</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Almenara%2C+J+M">J. M. Almenara</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Bieryla%2C+A">A. Bieryla</a>, <a href="/search/?searchtype=author&query=Boisse%2C+I">I. Boisse</a>, <a href="/search/?searchtype=author&query=Bonfils%2C+X">X. Bonfils</a>, <a href="/search/?searchtype=author&query=Boschin%2C+W">W. Boschin</a>, <a href="/search/?searchtype=author&query=Carmona%2C+A">A. Carmona</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Collins%2C+K+A">K. A. Collins</a>, <a href="/search/?searchtype=author&query=Dalal%2C+S">S. Dalal</a>, <a href="/search/?searchtype=author&query=Deleuil%2C+M">M. Deleuil</a>, <a href="/search/?searchtype=author&query=Delfosse%2C+X">X. Delfosse</a> , et al. (28 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="2204.08984v2-abstract-short" style="display: inline;"> We report the discovery and characterization of the transiting extrasolar planet TOI-1710$\:$b. It was first identified as a promising candidate by the Transiting Exoplanet Survey Satellite (TESS). Its planetary nature was then established with SOPHIE and HARPS-N spectroscopic observations via the radial-velocity method. The stellar parameters for the host star are derived from the spectra and a j… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.08984v2-abstract-full').style.display = 'inline'; document.getElementById('2204.08984v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.08984v2-abstract-full" style="display: none;"> We report the discovery and characterization of the transiting extrasolar planet TOI-1710$\:$b. It was first identified as a promising candidate by the Transiting Exoplanet Survey Satellite (TESS). Its planetary nature was then established with SOPHIE and HARPS-N spectroscopic observations via the radial-velocity method. The stellar parameters for the host star are derived from the spectra and a joint Markov chain Monte-Carlo (MCMC) adjustment of the spectral energy distribution and evolutionary tracks of TOI-1710. A joint MCMC analysis of the TESS light curve and the radial-velocity evolution allows us to determine the planetary system properties. From our analysis, TOI-1710$\:$b is found to be a massive warm super-Neptune ($M_{\rm p}=28.3\:\pm\:4.7\:{\rm M}_{\rm Earth}$ and $R_{\rm p}=5.34\:\pm\:0.11\:{\rm R}_{\rm Earth}$) orbiting a G5V dwarf star ($T_{\rm eff}=5665\pm~55\mathrm{K}$) on a nearly circular 24.3-day orbit ($e=0.16\:\pm\:0.08$). The orbital period of this planet is close to the estimated rotation period of its host star $P_{\rm rot}=22.5\pm2.0~\mathrm{days}$ and it has a low Keplerian semi-amplitude $K=6.4\pm1.0~\mathrm{m\:s^{-1}}$; we thus performed additional analyses to show the robustness of the retrieved planetary parameters. With a low bulk density of $1.03\pm0.23~\mathrm{g\:cm^{-3}}$ and orbiting a bright host star ($J=8.3$, $V=9.6$), TOI-1710$\:$b is one of the best targets in this mass-radius range (near the Neptunian desert) for atmospheric characterization via transmission spectroscopy, a key measurement in constraining planet formation and evolutionary models of sub-Jovian planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.08984v2-abstract-full').style.display = 'none'; document.getElementById('2204.08984v2-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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, 16 figures, 5 tables, A&A in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, A183 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.04948">arXiv:2204.04948</a> <span> [<a href="https://arxiv.org/pdf/2204.04948">pdf</a>, <a href="https://arxiv.org/format/2204.04948">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/10.1051/0004-6361/202142768">10.1051/0004-6361/202142768 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG XXXIII. HARPS-N detects multiple atomic species in emission from the dayside of KELT-20b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">L. Pino</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Amadori%2C+F">F. Amadori</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Boschin%2C+W">W. Boschin</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/?searchtype=author&query=Covino%2C+E">E. Covino</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Fiorenzano%2C+A+F+M">A. F. M. Fiorenzano</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Harutyunyan%2C+A">A. Harutyunyan</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a> , et al. (9 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="2204.04948v1-abstract-short" style="display: inline;"> The detection of lines in emission in planetary atmospheres provides direct evidence of temperature inversion. We confirm the trend of ultra-hot Jupiters orbiting A-type stars showing temperature inversions on their daysides, by detecting metals emission lines in the dayside of KELT-20b. We first detect the planetary emission by using the G2 stellar mask of the HARPS-N pipeline, which is mainly co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04948v1-abstract-full').style.display = 'inline'; document.getElementById('2204.04948v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.04948v1-abstract-full" style="display: none;"> The detection of lines in emission in planetary atmospheres provides direct evidence of temperature inversion. We confirm the trend of ultra-hot Jupiters orbiting A-type stars showing temperature inversions on their daysides, by detecting metals emission lines in the dayside of KELT-20b. We first detect the planetary emission by using the G2 stellar mask of the HARPS-N pipeline, which is mainly composed of neutral iron lines, as a template. Using neutral iron templates, we perform a retrieval of the atmospheric temperature-pressure profile of the planet, confirming a thermal inversion. Then we create models of planetary emission of different species using the retrieved inverted temperature-pressure profile. By using the cross-correlation technique, we detect FeI, FeII and CrI at signal-to-noise ratio levels of 7.1, 3.9 and 3.6, respectively. The latter is detected for the first time in emission in the atmosphere of an exoplanet. Contrary to FeI, FeII and CrI are detected only after the occultation and not before, hinting for different atmospheric properties in view on the pre- and post- occultation orbital phases. A further retrieval of the temperature-pressure profile performed independently on the pre- and post- occultation phases, while not highly significant, points to a steeper thermal inversion in the post-occultation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04948v1-abstract-full').style.display = 'none'; document.getElementById('2204.04948v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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 for publication in A&A. Submitted 27 Nov. 2021</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 663, A141 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.16856">arXiv:2203.16856</a> <span> [<a href="https://arxiv.org/pdf/2203.16856">pdf</a>, <a href="https://arxiv.org/ps/2203.16856">ps</a>, <a href="https://arxiv.org/format/2203.16856">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/stac810">10.1093/mnras/stac810 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The PEPSI Exoplanet Transit Survey (PETS) I: Investigating the presence of a silicate atmosphere on the super-Earth 55 Cnc e </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Keles%2C+E">Engin Keles</a>, <a href="/search/?searchtype=author&query=Mallonn%2C+M">Matthias Mallonn</a>, <a href="/search/?searchtype=author&query=Kitzmann%2C+D">Daniel Kitzmann</a>, <a href="/search/?searchtype=author&query=Poppenhaeger%2C+K">Katja Poppenhaeger</a>, <a href="/search/?searchtype=author&query=Hoeijmakers%2C+H+J">H. Jens Hoeijmakers</a>, <a href="/search/?searchtype=author&query=Ilyin%2C+I">Ilya Ilyin</a>, <a href="/search/?searchtype=author&query=Alexoudi%2C+X">Xanthippi Alexoudi</a>, <a href="/search/?searchtype=author&query=Carroll%2C+T+A">Thorsten A. Carroll</a>, <a href="/search/?searchtype=author&query=Alvarado-Gomez%2C+J">Julian Alvarado-Gomez</a>, <a href="/search/?searchtype=author&query=Ketzer%2C+L">Laura Ketzer</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">Francesco Borsa</a>, <a href="/search/?searchtype=author&query=Gaudi%2C+S">Scott Gaudi</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">Luca Malavolta</a>, <a href="/search/?searchtype=author&query=Molaverdikhani%2C+K">Karan Molaverdikhani</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">Valerio Nascimbeni</a>, <a href="/search/?searchtype=author&query=Patience%2C+J">Jennifer Patience</a>, <a href="/search/?searchtype=author&query=Pino%2C+L">Lorenzo Pino</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">Gaetano Scandariato</a>, <a href="/search/?searchtype=author&query=Schlawin%2C+E">Everett Schlawin</a>, <a href="/search/?searchtype=author&query=Shkolnik%2C+E">Evgenya Shkolnik</a>, <a href="/search/?searchtype=author&query=Sicilia%2C+D">Daniela Sicilia</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">Alessandro Sozzetti</a>, <a href="/search/?searchtype=author&query=Foster%2C+M+G">Mary G. Foster</a> , et al. (4 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="2203.16856v1-abstract-short" style="display: inline;"> The study of exoplanets and especially their atmospheres can reveal key insights on their evolution by identifying specific atmospheric species. For such atmospheric investigations, high-resolution transmission spectroscopy has shown great success, especially for Jupiter-type planets. Towards the atmospheric characterization of smaller planets, the super-Earth exoplanet 55 Cnc e is one of the most… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.16856v1-abstract-full').style.display = 'inline'; document.getElementById('2203.16856v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.16856v1-abstract-full" style="display: none;"> The study of exoplanets and especially their atmospheres can reveal key insights on their evolution by identifying specific atmospheric species. For such atmospheric investigations, high-resolution transmission spectroscopy has shown great success, especially for Jupiter-type planets. Towards the atmospheric characterization of smaller planets, the super-Earth exoplanet 55 Cnc e is one of the most promising terrestrial exoplanets studied to date. Here, we present a high-resolution spectroscopic transit observation of this planet, acquired with the PEPSI instrument at the Large Binocular Telescope. Assuming the presence of Earth-like crust species on the surface of 55 Cnc e, from which a possible silicate-vapor atmosphere could have originated, we search in its transmission spectrum for absorption of various atomic and ionized species such as Fe , Fe+, Ca , Ca+, Mg and K , among others. Not finding absorption for any of the investigated species, we are able to set absorption limits with a median value of 1.9 x RP. In conclusion, we do not find evidence of a widely extended silicate envelope on this super-Earth reaching several planetary radii. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.16856v1-abstract-full').style.display = 'none'; document.getElementById('2203.16856v1-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">MNRAS, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.04648">arXiv:2203.04648</a> <span> [<a href="https://arxiv.org/pdf/2203.04648">pdf</a>, <a href="https://arxiv.org/format/2203.04648">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/10.1051/0004-6361/202142828">10.1051/0004-6361/202142828 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HADES RV Programme with HARPS-N at TNG XV. Planetary occurrence rates around early-M dwarfs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pinamonti%2C+M">M. Pinamonti</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Perger%2C+M">M. Perger</a>, <a href="/search/?searchtype=author&query=Ribas%2C+I">I. Ribas</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Covino%2C+E">E. Covino</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez-%C3%81lvarez%2C+E">E. Gonz谩lez-脕lvarez</a>, <a href="/search/?searchtype=author&query=Herrero%2C+E">E. Herrero</a>, <a href="/search/?searchtype=author&query=Leto%2C+G">G. Leto</a>, <a href="/search/?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Morales%2C+J+C">J. C. Morales</a>, <a href="/search/?searchtype=author&query=Pagano%2C+I">I. Pagano</a>, <a href="/search/?searchtype=author&query=Petralia%2C+A">A. Petralia</a>, <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a> , et al. (6 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="2203.04648v1-abstract-short" style="display: inline;"> We present the complete Bayesian statistical analysis of the HArps-n red Dwarf Exoplanet Survey (HADES), which monitored the radial velocities of a large sample of M dwarfs with HARPS-N at TNG, over the last 6 years. The targets were selected in a narrow range of spectral types from M0 to M3, $0.3$ M$_\odot < M_\star < 0.71$ M$_\odot$, in order to study the planetary population around a well-defin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04648v1-abstract-full').style.display = 'inline'; document.getElementById('2203.04648v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.04648v1-abstract-full" style="display: none;"> We present the complete Bayesian statistical analysis of the HArps-n red Dwarf Exoplanet Survey (HADES), which monitored the radial velocities of a large sample of M dwarfs with HARPS-N at TNG, over the last 6 years. The targets were selected in a narrow range of spectral types from M0 to M3, $0.3$ M$_\odot < M_\star < 0.71$ M$_\odot$, in order to study the planetary population around a well-defined class of host stars. We take advantage of Bayesian statistics to derive an accurate estimate of the detectability function of the survey. Our analysis also includes the application of Gaussian Process approach to take into account stellar activity induced radial velocity variations, and improve the detection limits, around the most-observed and most-active targets. The Markov chain Monte Carlo and Gaussian process technique we apply in this analysis has proven very effective in the study of M-dwarf planetary systems, helping the detection of most of the HADES planets. From the detectability function we can calculate the occurrence rate of small mass planets around early-M dwarfs, either taking into account only the 11 already published HADES planets or adding also the 5 new planetary candidates discovered in this analysis, and compare them with the previous estimates of planet occurrence around M-dwarf or Solar-type stars: considering only the confirmed planets, we find the highest frequency for low-mass planets ($1$ M$_\oplus < m_p \sin i < 10$ M$_\oplus$) with periods $10$ d$ < P < 100$ d, $f_\text{occ} = 85^{+5}_{-19}\%$, while for short-period planets ($1$ d$ < P < 10$ d) we find a frequency of $f_\text{occ} = 10.3^{+8.4}_{-3.3}\%$, significantly lower than for later-M dwarfs. These results, and their comparison with other surveys focused on different stellar types, confirms the central role that stellar mass plays in the formation and evolution of planetary systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04648v1-abstract-full').style.display = 'none'; document.getElementById('2203.04648v1-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> 9 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">21 pages, 14 figures, 8 table. Accepted by 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 664, A65 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.11179">arXiv:2112.11179</a> <span> [<a href="https://arxiv.org/pdf/2112.11179">pdf</a>, <a href="https://arxiv.org/format/2112.11179">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/10.1051/0004-6361/202142336">10.1051/0004-6361/202142336 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GAPS Programme at TNG. XXXII. The revealing non-detection of metastable HeI in the atmosphere of the hot Jupiter WASP-80b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Guilluy%2C+G">G. Guilluy</a>, <a href="/search/?searchtype=author&query=Shaikhislamov%2C+I+F">I. F. Shaikhislamov</a>, <a href="/search/?searchtype=author&query=Carleo%2C+I">I. Carleo</a>, <a href="/search/?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/?searchtype=author&query=Rainer%2C+M">M. Rainer</a>, <a href="/search/?searchtype=author&query=Cecchi-Pestellini%2C+C">C. Cecchi-Pestellini</a>, <a href="/search/?searchtype=author&query=Khodachenko%2C+M+L">M. L. Khodachenko</a>, <a href="/search/?searchtype=author&query=Efimov%2C+M+A">M. A. Efimov</a>, <a href="/search/?searchtype=author&query=Rumenskikh%2C+M+S">M. S. Rumenskikh</a>, <a href="/search/?searchtype=author&query=Miroshnichenko%2C+I+B">I. B. Miroshnichenko</a>, <a href="/search/?searchtype=author&query=Berezutsky%2C+A+G">A. G. Berezutsky</a>, <a href="/search/?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/?searchtype=author&query=Brogi%2C+M">M. Brogi</a>, <a href="/search/?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/?searchtype=author&query=Mancini%2C+L">L. Mancini</a>, <a href="/search/?searchtype=author&query=Affer%2C+L">L. Affer</a>, <a href="/search/?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/?searchtype=author&query=Bignamini%2C+A">A. Bignamini</a>, <a href="/search/?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a> , et al. (16 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="2112.11179v1-abstract-short" style="display: inline;"> The hot Jupiter WASP-80b has been identified as a possible excellent target for detecting and measuring HeI absorption in the upper atmosphere. We observed 4 primary transits of WASP-80b in the optical and near-IR using the HARPS-N and GIANO-B high-resolution spectrographs, focusing on the HeI triplet. We further employed a three-dimensional hydrodynamic aeronomy model to understand the observatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11179v1-abstract-full').style.display = 'inline'; document.getElementById('2112.11179v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.11179v1-abstract-full" style="display: none;"> The hot Jupiter WASP-80b has been identified as a possible excellent target for detecting and measuring HeI absorption in the upper atmosphere. We observed 4 primary transits of WASP-80b in the optical and near-IR using the HARPS-N and GIANO-B high-resolution spectrographs, focusing on the HeI triplet. We further employed a three-dimensional hydrodynamic aeronomy model to understand the observational results. We did not find any signature of planetary absorption at the position of the HeI triplet with an upper limit of 0.7% (i.e. 1.11 planetary radii; 95% confidence level). We re-estimated the stellar high-energy emission that we combined with a stellar photospheric model to generate the input for the hydrodynamic modelling. We obtained that, assuming a solar He to H abundance ratio, HeI absorption should have been detected. Considering a stellar wind 25 times weaker than solar, we could reproduce the non-detection only assuming a He to H abundance ratio about 16 times smaller than solar. Instead, considering a stellar wind 10 times stronger than solar, we could reproduce the non-detection only with a He to H abundance ratio about 10 times smaller than solar. We attempted to understand this result by collecting all past HeI measurements looking for correlations with stellar high-energy emission and planetary gravity, but without finding any. WASP-80b is not the only planet with a sub-solar estimated He to H abundance ratio, suggesting the presence of efficient physical mechanisms (e.g. phase separation, magnetic fields) capable of significantly modifying the He to H content in the upper atmosphere of hot Jupiters. The planetary macroscopic properties and the shape of the stellar spectral energy distribution are not sufficient for predicting the presence or absence of detectable metastable He in a planetary atmosphere, as also the He abundance appears to play a major role. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11179v1-abstract-full').style.display = 'none'; document.getElementById('2112.11179v1-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> 21 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </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 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 658, A136 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.08956">arXiv:2112.08956</a> <span> [<a href="https://arxiv.org/pdf/2112.08956">pdf</a>, <a href="https://arxiv.org/format/2112.08956">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/10.1007/s10686-021-09824-7">10.1007/s10686-021-09824-7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On The Synergy Between Ariel And Ground-Based High-Resolution Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Guilluy%2C+G">Gloria Guilluy</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">Alessandro Sozzetti</a>, <a href="/search/?searchtype=author&query=Giacobbe%2C+P">Paolo Giacobbe</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</a>, <a href="/search/?searchtype=author&query=Micela%2C+G">Giuseppina Micela</a> </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="2112.08956v1-abstract-short" style="display: inline;"> Since the first discovery of an extra-solar planet around a main-sequence star, in 1995, the number of detected exoplanets has increased enormously. Over the past two decades, observational instruments (both onboard and on ground-based facilities) have revealed an astonishing diversity in planetary physical features (i. e. mass and radius), and orbital parameters (e.g. period, semi-major axis, inc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.08956v1-abstract-full').style.display = 'inline'; document.getElementById('2112.08956v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.08956v1-abstract-full" style="display: none;"> Since the first discovery of an extra-solar planet around a main-sequence star, in 1995, the number of detected exoplanets has increased enormously. Over the past two decades, observational instruments (both onboard and on ground-based facilities) have revealed an astonishing diversity in planetary physical features (i. e. mass and radius), and orbital parameters (e.g. period, semi-major axis, inclination). Exoplanetary atmospheres provide direct clues to understand the origin of these differences through their observable spectral imprints. In the near future, upcoming ground and space-based telescopes will shift the focus of exoplanetary science from an era of 'species discovery' to one of 'atmospheric characterization'. In this context, the Atmospheric Remote-sensing Infrared Exoplanet Large (Ariel) survey, will play a key role. As it is designed to observe and characterize a large and diverse sample of exoplanets, Ariel will provide constraints on a wide gamut of atmospheric properties allowing us to extract much more information than has been possible so far (e.g. insights into the planetary formation and evolution processes). The low resolution spectra obtained with Ariel will probe layers different from those observed by ground-based high resolution spectroscopy, therefore the synergy between these two techniques offers a unique opportunity to understanding the physics of planetary atmospheres. In this paper, we set the basis for building up a framework to effectively utilise, at near-infrared wavelengths, high-resolution datasets (analyzed via the cross-correlation technique) with spectral retrieval analyses based on Ariel low-resolution spectroscopy. We show preliminary results, using a benchmark object, namely HD 209458 b, addressing the possibility of providing improved constraints on the temperature structure and molecular/atomic abundances. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.08956v1-abstract-full').style.display = 'none'; document.getElementById('2112.08956v1-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </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,6 figures, accepted for publication in EXPA as EXPA-D-20-00055R2 ---- for the ARIEL Phase B Special Issue</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.08709">arXiv:2111.08709</a> <span> [<a href="https://arxiv.org/pdf/2111.08709">pdf</a>, <a href="https://arxiv.org/format/2111.08709">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1007/s10686-021-09781-1">10.1007/s10686-021-09781-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Faint objects in motion: the new frontier of high precision astrometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Malbet%2C+F">Fabien Malbet</a>, <a href="/search/?searchtype=author&query=Boehm%2C+C">C茅line Boehm</a>, <a href="/search/?searchtype=author&query=Krone-Martins%2C+A">Alberto Krone-Martins</a>, <a href="/search/?searchtype=author&query=Amorim%2C+A">Antonio Amorim</a>, <a href="/search/?searchtype=author&query=Anglada-Escud%C3%A9%2C+G">Guillem Anglada-Escud茅</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">Alexis Brandeker</a>, <a href="/search/?searchtype=author&query=Courbin%2C+F">Fr茅d茅ric Courbin</a>, <a href="/search/?searchtype=author&query=En%C3%9Flin%2C+T">Torsten En脽lin</a>, <a href="/search/?searchtype=author&query=Falc%C3%A3o%2C+A">Antonio Falc茫o</a>, <a href="/search/?searchtype=author&query=Freese%2C+K">Katherine Freese</a>, <a href="/search/?searchtype=author&query=Holl%2C+B">Berry Holl</a>, <a href="/search/?searchtype=author&query=Labadie%2C+L">Lucas Labadie</a>, <a href="/search/?searchtype=author&query=L%C3%A9ger%2C+A">Alain L茅ger</a>, <a href="/search/?searchtype=author&query=Mamon%2C+G">Gary Mamon</a>, <a href="/search/?searchtype=author&query=Mcarthur%2C+B">Barbara Mcarthur</a>, <a href="/search/?searchtype=author&query=Mora%2C+A">Alcione Mora</a>, <a href="/search/?searchtype=author&query=Shao%2C+M">Mike Shao</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">Alessandro Sozzetti</a>, <a href="/search/?searchtype=author&query=Spolyar%2C+D">Douglas Spolyar</a>, <a href="/search/?searchtype=author&query=Villaver%2C+E">Eva Villaver</a>, <a href="/search/?searchtype=author&query=Abbas%2C+U">Ummi Abbas</a>, <a href="/search/?searchtype=author&query=Albertus%2C+C">Conrado Albertus</a>, <a href="/search/?searchtype=author&query=Alves%2C+J">Jo茫o Alves</a>, <a href="/search/?searchtype=author&query=Barnes%2C+R">Rory Barnes</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo Stefano Bonomo</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="2111.08709v1-abstract-short" style="display: inline;"> Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the front… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.08709v1-abstract-full').style.display = 'inline'; document.getElementById('2111.08709v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.08709v1-abstract-full" style="display: none;"> Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the frontier of precision astrometry from evidence of Earth-mass habitable worlds around the nearest stars, to distant Milky Way objects, and out to the Local Group of galaxies. As we enter the era of the James Webb Space Telescope and the new ground-based, adaptive-optics-enabled giant telescopes, by obtaining these high precision measurements on key objects that Gaia could not reach, a mission that focuses on high precision astrometry science can consolidate our theoretical understanding of the local Universe, enable extrapolation of physical processes to remote redshifts, and derive a much more consistent picture of cosmological evolution and the likely fate of our cosmos. Already several missions have been proposed to address the science case of faint objects in motion using high precision astrometry missions: NEAT proposed for the ESA M3 opportunity, micro-NEAT for the S1 opportunity, and Theia for the M4 and M5 opportunities. Additional new mission configurations adapted with technological innovations could be envisioned to pursue accurate measurements of these extremely small motions. The goal of this White Paper is to address the fundamental science questions that are at stake when we focus on the motions of faint sky objects and to briefly review instrumentation and mission profiles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.08709v1-abstract-full').style.display = 'none'; document.getElementById('2111.08709v1-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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">arXiv admin note: substantial text overlap with arXiv:1910.08028, arXiv:1707.01348</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Experimental Astronomy, Springer Link, 2021, 51 (3), pp.845-886 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.05716">arXiv:2111.05716</a> <span> [<a href="https://arxiv.org/pdf/2111.05716">pdf</a>, <a href="https://arxiv.org/format/2111.05716">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/10.1051/0004-6361/202039037">10.1051/0004-6361/202039037 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing Kepler's hottest small planets via homogeneous search and analysis of optical secondary eclipses and phase variations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Singh%2C+V">Vikash Singh</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">A. S. Bonomo</a>, <a href="/search/?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/?searchtype=author&query=Cibrario%2C+N">N. Cibrario</a>, <a href="/search/?searchtype=author&query=Barbato%2C+D">D. Barbato</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Pagano%2C+I">I. Pagano</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a> </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="2111.05716v2-abstract-short" style="display: inline;"> We perform a homogeneous search for and analysis of optical occultations and phase variations of the most favorable ultra-short-period (USP) ($P<1$~d) sub-Neptunes ($R_{p}<4 R_{\oplus}$) observed by $\textit{Kepler}$ and K2, with the aim of better understanding their nature. We first selected 16 $\textit{Kepler}$ and K2 USP sub-Neptunes, based on the expected occultation signal. We filtered out st… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05716v2-abstract-full').style.display = 'inline'; document.getElementById('2111.05716v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05716v2-abstract-full" style="display: none;"> We perform a homogeneous search for and analysis of optical occultations and phase variations of the most favorable ultra-short-period (USP) ($P<1$~d) sub-Neptunes ($R_{p}<4 R_{\oplus}$) observed by $\textit{Kepler}$ and K2, with the aim of better understanding their nature. We first selected 16 $\textit{Kepler}$ and K2 USP sub-Neptunes, based on the expected occultation signal. We filtered out stellar variability in the $\textit{Kepler}$ light curves, using a sliding linear fitting and, when required, a more sophisticated approach based on Gaussian Process regression. We simultaneously modeled the primary transit, secondary eclipse, and phase variations in a Bayesian framework, by using information from previous studies and knowledge of the Gaia parallaxes. We confirm the optical secondary eclipses for Kepler-10b ($13蟽$), Kepler-78b ($9.5蟽$), and K2-141b ($6.9蟽$), with marginal evidence for K2-312b ($2.2蟽$). We report new detections for K2-106b ($3.3蟽$), K2-131b (3.2$蟽$), Kepler-407b ($3.0蟽$), and hints for K2-229b (2.5$蟽$). For all targets with the exception of K2-229b and K2-312b, we also find phase curve variations with a confidence level higher than $2蟽$. Two USP planets, namely Kepler-10b and Kepler-78b, show non-negligible nightside emission. This questions the scenario of magma-ocean worlds with inefficient heat redistribution to the night-side for both planets. Due to the youth of the Kepler-78 system and the small planetary orbital separation, the planet may still retain a collisional secondary atmosphere capable of conducting heat from the day to the night side. Instead, the presence of an outgassing magma ocean on the dayside and the low high-energy irradiation of the old host star may have enabled Kepler-10b to build up and retain a recently-formed collisional secondary atmosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05716v2-abstract-full').style.display = 'none'; document.getElementById('2111.05716v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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, 19 figures, including corrections from the language editor</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 658, A132 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.02608">arXiv:2111.02608</a> <span> [<a href="https://arxiv.org/pdf/2111.02608">pdf</a>, <a href="https://arxiv.org/format/2111.02608">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/10.3847/1538-3881/ac3141">10.3847/1538-3881/ac3141 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> K2-79b and K2-222b: Mass measurements of two small exoplanets with periods beyond 10 days that overlap with periodic magnetic activity signals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nava%2C+C">Chantanelle Nava</a>, <a href="/search/?searchtype=author&query=L%C3%B3pez-Morales%2C+M">Mercedes L贸pez-Morales</a>, <a href="/search/?searchtype=author&query=Mortier%2C+A">Annelies Mortier</a>, <a href="/search/?searchtype=author&query=Zeng%2C+L">Li Zeng</a>, <a href="/search/?searchtype=author&query=Giles%2C+H+A+C">Helen A. C. Giles</a>, <a href="/search/?searchtype=author&query=Bieryla%2C+A">Allyson Bieryla</a>, <a href="/search/?searchtype=author&query=Vanderburg%2C+A">Andrew Vanderburg</a>, <a href="/search/?searchtype=author&query=Buchhave%2C+L+A">Lars A. Buchhave</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">Ennio Poretti</a>, <a href="/search/?searchtype=author&query=Saar%2C+S+H">Steven H. Saar</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">Xavier Dumusque</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">David W. Latham</a>, <a href="/search/?searchtype=author&query=Charbonneau%2C+D">David Charbonneau</a>, <a href="/search/?searchtype=author&query=Damasso%2C+M">Mario Damasso</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</a>, <a href="/search/?searchtype=author&query=Lovis%2C+C">Christophe Lovis</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">Andrew Collier Cameron</a>, <a href="/search/?searchtype=author&query=Eastman%2C+J+D">Jason D. Eastman</a>, <a href="/search/?searchtype=author&query=Sozzetti%2C+A">Alessandro Sozzetti</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">Rosario Cosentino</a>, <a href="/search/?searchtype=author&query=Pedani%2C+M">Marco Pedani</a>, <a href="/search/?searchtype=author&query=Pepe%2C+F">Francesco Pepe</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">Emilio Molinari</a>, <a href="/search/?searchtype=author&query=Sasselov%2C+D">Dimitar Sasselov</a>, <a href="/search/?searchtype=author&query=Mayor%2C+M">Michel Mayor</a> , et al. (6 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="2111.02608v1-abstract-short" style="display: inline;"> We present mass and radius measurements of K2-79b and K2-222b, two transiting exoplanets orbiting active G-type stars. Their respective 10.99d and 15.39d orbital periods fall near periods of signals induced by stellar magnetic activity. The two signals might therefore interfere and lead to an inaccurate estimate of exoplanet mass. We present a method to mitigate these effects when radial velocity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.02608v1-abstract-full').style.display = 'inline'; document.getElementById('2111.02608v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.02608v1-abstract-full" style="display: none;"> We present mass and radius measurements of K2-79b and K2-222b, two transiting exoplanets orbiting active G-type stars. Their respective 10.99d and 15.39d orbital periods fall near periods of signals induced by stellar magnetic activity. The two signals might therefore interfere and lead to an inaccurate estimate of exoplanet mass. We present a method to mitigate these effects when radial velocity and activity indicator observations are available over multiple observing seasons and the orbital period of the exoplanet is known. We perform correlation and periodogram analyses on sub-sets composed of each target's two observing seasons, in addition to the full data sets. For both targets, these analyses reveal an optimal season with little to no interference at the orbital period of the known exoplanet. We make a confident mass detection of each exoplanet by confirming agreement between fits to the full radial velocity set and the optimal season. For K2-79b, we measure a mass of 11.8 $\pm$ 3.6 $M_{Earth}$ and a radius of 4.09 $\pm$ 0.17 $R_{Earth}$. For K2-222b, we measure a mass of 8.0 $\pm$ 1.8 $M_{Earth}$ and a radius of 2.35 $\pm$ 0.08 $R_{Earth}$. According to model predictions, K2-79b is a highly irradiated Uranus-analog and K2-222b hosts significant amounts of water ice. We also present an RV solution for a candidate second companion orbiting K2-222 at 147.5d. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.02608v1-abstract-full').style.display = 'none'; document.getElementById('2111.02608v1-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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">33 pages, 17 figures, 13 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/2107.08092">arXiv:2107.08092</a> <span> [<a href="https://arxiv.org/pdf/2107.08092">pdf</a>, <a href="https://arxiv.org/format/2107.08092">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/10.3847/1538-3881/ac1590">10.3847/1538-3881/ac1590 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Wolf 503 b: Characterization of a Sub-Neptune Orbiting a Metal-Poor K Dwarf </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Polanski%2C+A+S">Alex S. Polanski</a>, <a href="/search/?searchtype=author&query=Crossfield%2C+I+J+M">Ian J. M. Crossfield</a>, <a href="/search/?searchtype=author&query=Burt%2C+J+A">Jennifer A. Burt</a>, <a href="/search/?searchtype=author&query=Nowak%2C+G">Grzegorz Nowak</a>, <a href="/search/?searchtype=author&query=L%C3%B3pez-Morales%2C+M">Mercedes L贸pez-Morales</a>, <a href="/search/?searchtype=author&query=Mortier%2C+A">Annelies Mortier</a>, <a href="/search/?searchtype=author&query=Poretti%2C+E">Ennio Poretti</a>, <a href="/search/?searchtype=author&query=Behmard%2C+A">Aida Behmard</a>, <a href="/search/?searchtype=author&query=Benneke%2C+B">Bj枚rn Benneke</a>, <a href="/search/?searchtype=author&query=Blunt%2C+S">Sarah Blunt</a>, <a href="/search/?searchtype=author&query=Bonomo%2C+A+S">Aldo S. Bonomo</a>, <a href="/search/?searchtype=author&query=Butler%2C+R+P">R. Paul Butler</a>, <a href="/search/?searchtype=author&query=Chontos%2C+A">Ashley Chontos</a>, <a href="/search/?searchtype=author&query=Cosentino%2C+R">Rosario Cosentino</a>, <a href="/search/?searchtype=author&query=Crane%2C+J+D">Jeffrey D. Crane</a>, <a href="/search/?searchtype=author&query=Dumusque%2C+X">Xavier Dumusque</a>, <a href="/search/?searchtype=author&query=Fulton%2C+B+J">Benjamin J. Fulton</a>, <a href="/search/?searchtype=author&query=Ghedina%2C+A">Adriano Ghedina</a>, <a href="/search/?searchtype=author&query=Gorjian%2C+V">Varoujan Gorjian</a>, <a href="/search/?searchtype=author&query=Grunblatt%2C+S+K">Samuel K. Grunblatt</a>, <a href="/search/?searchtype=author&query=Harutyunyan%2C+A">Avet Harutyunyan</a>, <a href="/search/?searchtype=author&query=Howard%2C+A+W">Andrew W. Howard</a>, <a href="/search/?searchtype=author&query=Isaacson%2C+H">Howard Isaacson</a>, <a href="/search/?searchtype=author&query=Kosiarek%2C+M+R">Molly R. Kosiarek</a>, <a href="/search/?searchtype=author&query=Latham%2C+D+W">David W. Latham</a> , et al. (13 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="2107.08092v1-abstract-short" style="display: inline;"> Using radial velocity measurements from four instruments, we report the mass and density of a $2.043\pm0.069 ~\rm{R}_{\oplus}$ sub-Neptune orbiting the quiet K-dwarf Wolf 503 (HIP 67285). In addition, we present improved orbital and transit parameters by analyzing previously unused short-cadence $K2$ campaign 17 photometry and conduct a joint radial velocity-transit fit to constrain the eccentrici… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08092v1-abstract-full').style.display = 'inline'; document.getElementById('2107.08092v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08092v1-abstract-full" style="display: none;"> Using radial velocity measurements from four instruments, we report the mass and density of a $2.043\pm0.069 ~\rm{R}_{\oplus}$ sub-Neptune orbiting the quiet K-dwarf Wolf 503 (HIP 67285). In addition, we present improved orbital and transit parameters by analyzing previously unused short-cadence $K2$ campaign 17 photometry and conduct a joint radial velocity-transit fit to constrain the eccentricity at $0.41\pm0.05$. The addition of a transit observation by $Spitzer$ also allows us to refine the orbital ephemeris in anticipation of further follow-up. Our mass determination, $6.26^{+0.69}_{-0.70}~\rm{M}_{\odot}$, in combination with the updated radius measurements, gives Wolf 503 b a bulk density of $蟻= 2.92\pm ^{+0.50}_{-0.44}$ $\rm{g}~\rm{cm}^{-3}$. Using interior composition models, we find this density is consistent with an Earth-like core with either a substantial $\rm{H}_2\rm{O}$ mass fraction ($45^{+19.12}_{-16.15}\%$) or a modest H/He envelope ($0.5\pm0.28\%$). The low H/He mass fraction, along with the old age of Wolf 503 ($11\pm2$ Gyrs), makes this sub-Neptune an opportune subject for testing theories of XUV-driven mass loss while the brightness of its host ($J=8.3$ mag) makes it an attractive target for transmission spectroscopy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08092v1-abstract-full').style.display = 'none'; document.getElementById('2107.08092v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </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 ApJ 2021 July 15</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" 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