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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <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/2502.19558">arXiv:2502.19558</a> <span> [<a href="https://arxiv.org/pdf/2502.19558">pdf</a>, <a href="https://arxiv.org/format/2502.19558">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"> Characterization of AF Lep b at high spectral resolution with VLT/HiRISE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Denis%2C+A">A. Denis</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Chauvin%2C+G">G. Chauvin</a>, <a href="/search/astro-ph?searchtype=author&query=Radcliffe%2C+A">A. Radcliffe</a>, <a href="/search/astro-ph?searchtype=author&query=Ravet%2C+M">M. Ravet</a>, <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W">W. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Palma-Bifani%2C+P">P. Palma-Bifani</a>, <a href="/search/astro-ph?searchtype=author&query=Petrus%2C+S">S. Petrus</a>, <a href="/search/astro-ph?searchtype=author&query=Parmentier%2C+V">V. Parmentier</a>, <a href="/search/astro-ph?searchtype=author&query=Martos%2C+S">S. Martos</a>, <a href="/search/astro-ph?searchtype=author&query=Simonnin%2C+A">A. Simonnin</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Cadet%2C+R">R. Cadet</a>, <a href="/search/astro-ph?searchtype=author&query=Forveille%2C+T">T. Forveille</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a>, <a href="/search/astro-ph?searchtype=author&query=Kiefer%2C+F">F. Kiefer</a>, <a href="/search/astro-ph?searchtype=author&query=Lagrange%2C+A+-">A. -M. Lagrange</a>, <a href="/search/astro-ph?searchtype=author&query=Chiavassa%2C+A">A. Chiavassa</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Lavail%2C+A">A. Lavail</a>, <a href="/search/astro-ph?searchtype=author&query=Godoy%2C+N">N. Godoy</a>, <a href="/search/astro-ph?searchtype=author&query=Janson%2C+M">M. Janson</a>, <a href="/search/astro-ph?searchtype=author&query=Pourcelot%2C+R">R. Pourcelot</a>, <a href="/search/astro-ph?searchtype=author&query=Delorme%2C+P">P. Delorme</a> , et al. (19 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="2502.19558v1-abstract-short" style="display: inline;"> Since the recent discovery of the directly imaged super-Jovian planet AF Lep b, several studies have been conducted to characterize its atmosphere and constrain its orbital parameters. AF Lep b has a measured dynamical mass of $3.68 \pm 0.48$ MJup, a radius of $1.3 \pm 0.15$ RJup, a nearly circular orbit in spin-orbit alignment with the host star, a relatively high metallicity, and a near-solar to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.19558v1-abstract-full').style.display = 'inline'; document.getElementById('2502.19558v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.19558v1-abstract-full" style="display: none;"> Since the recent discovery of the directly imaged super-Jovian planet AF Lep b, several studies have been conducted to characterize its atmosphere and constrain its orbital parameters. AF Lep b has a measured dynamical mass of $3.68 \pm 0.48$ MJup, a radius of $1.3 \pm 0.15$ RJup, a nearly circular orbit in spin-orbit alignment with the host star, a relatively high metallicity, and a near-solar to super-solar C/O ratio. However, key parameters such as the rotational velocity and radial velocity could not be estimated as they require high-resolution spectroscopic data that is impossible to obtain with classical spectrographs. AF Lep b was recently observed with the new HiRISE visitor instrument at the VLT, with the goal of obtaining high-resolution (R~140,000) spectroscopic observations to better constrain the orbital and atmospheric parameters of the young giant exoplanet. We compare the extracted spectrum of AF Lep b to self-consistent atmospheric models using ForMoSA. We then use our measurements of the radial velocity of the planet to provide new constraints on the orbit of the planet. From the forward modeling, we find a C/O ratio that aligns with previous low-resolution analyses, and we confirm the super-solar metallicity. We also confirm unambiguously the presence of methane in the atmosphere of the companion. Based on all available relative astrometry and radial velocity measurements of the host star, we show that two distinct orbital populations are possible for the companion. We derive the radial velocity of AF Lep b to be $10.51 \pm 1.03$ km/s, and show that this value agrees well with one of the two orbital solutions, allowing us to rule out an entire family of orbits. Additionally, assuming that the rotation and orbit are coplanar, the derived planet's rotation rate is consistent with the observed trend of increasing spin velocity with higher planet mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.19558v1-abstract-full').style.display = 'none'; document.getElementById('2502.19558v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 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">Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.04523">arXiv:2501.04523</a> <span> [<a href="https://arxiv.org/pdf/2501.04523">pdf</a>, <a href="https://arxiv.org/format/2501.04523">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae2799">10.1093/mnras/stae2799 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGTS-EB-7, an eccentric, long-period, low-mass eclipsing binary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodel%2C+T">Toby Rodel</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C+A">Christopher. A. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Ulmer-Moll%2C+S">Sol猫ne Ulmer-Moll</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">Samuel Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Maxted%2C+P+F+L">Pierre F. L. Maxted</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">Sarah L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Brahm%2C+R">Rafael Brahm</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson%2C+T+G">Thomas G Wilson</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Eschen%2C+Y+N+E">Yoshi Nike Emilia Eschen</a>, <a href="/search/astro-ph?searchtype=author&query=Doyle%2C+L">Lauren Doyle</a>, <a href="/search/astro-ph?searchtype=author&query=Freckelton%2C+A+V">Alix V. Freckelton</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+D+R">Douglas R. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Apergis%2C+I">Ioannis Apergis</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">Daniel Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Francois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">Matthew R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Dumusque%2C+X">Xavier Dumusque</a>, <a href="/search/astro-ph?searchtype=author&query=Eberhardt%2C+J">Jan Eberhardt</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez%2C+J+F">Jorge Fern谩ndez Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">Edward Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">Michael R. Goad</a>, <a href="/search/astro-ph?searchtype=author&query=Hawthorn%2C+F">Faith Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Helled%2C+R">Ravit Helled</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Thomas Henning</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="2501.04523v3-abstract-short" style="display: inline;"> Despite being the most common types of stars in the Galaxy, the physical properties of late M dwarfs are often poorly constrained. A trend of radius inflation compared to evolutionary models has been observed for earlier type M dwarfs in eclipsing binaries, possibly caused by magnetic activity. It is currently unclear whether this trend also extends to later type M dwarfs below the convective boun… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04523v3-abstract-full').style.display = 'inline'; document.getElementById('2501.04523v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.04523v3-abstract-full" style="display: none;"> Despite being the most common types of stars in the Galaxy, the physical properties of late M dwarfs are often poorly constrained. A trend of radius inflation compared to evolutionary models has been observed for earlier type M dwarfs in eclipsing binaries, possibly caused by magnetic activity. It is currently unclear whether this trend also extends to later type M dwarfs below the convective boundary. This makes the discovery of lower-mass, fully convective, M dwarfs in eclipsing binaries valuable for testing evolutionary models especially in longer-period binaries where tidal interaction between the primary and secondary is negligible. With this context, we present the discovery of the NGTS-EB-7 AB system, an eclipsing binary containing a late M dwarf secondary and an evolved G-type primary star. The secondary star has a radius of $0.125 \pm 0.006 R_\odot$ , a mass of $0.096 \pm 0.004 M_\odot$ and follows a highly eccentric $(e=0.71436 \pm 0.00085)$ orbit every $193.35875 \pm 0.00034$ days. This makes NGTS-EB-7 AB the third longest-period eclipsing binary system with a secondary smaller than $200 M_J$ with the mass and radius constrained to better than $5 \%$. In addition, NGTS-EB-7 is situated near the centre of the proposed LOPS2 southern field of the upcoming PLATO mission, allowing for detection of the secondary eclipse and measurement of the companion`s temperature. With its long-period and well-constrained physical properties - NGTS-EB-7 B will make a valuable addition to the sample of M dwarfs in eclipsing binaries and help in determining accurate empirical mass/radius relations for later M dwarf stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04523v3-abstract-full').style.display = 'none'; document.getElementById('2501.04523v3-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Main body: 14 pages, 6 figures, 5 tables. Appendices: 7 pages, 5 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/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/astro-ph?searchtype=author&query=Rauer%2C+H">Heike Rauer</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J">Juan Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Deleuil%2C+M">Magali Deleuil</a>, <a href="/search/astro-ph?searchtype=author&query=Erikson%2C+A">Anders Erikson</a>, <a href="/search/astro-ph?searchtype=author&query=Gizon%2C+L">Laurent Gizon</a>, <a href="/search/astro-ph?searchtype=author&query=Goupil%2C+M">Mariejo Goupil</a>, <a href="/search/astro-ph?searchtype=author&query=Heras%2C+A">Ana Heras</a>, <a href="/search/astro-ph?searchtype=author&query=Lorenzo-Alvarez%2C+J">Jose Lorenzo-Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Marliani%2C+F">Filippo Marliani</a>, <a href="/search/astro-ph?searchtype=author&query=Martin-Garcia%2C+C">C茅sar Martin-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Mas-Hesse%2C+J+M">J. Miguel Mas-Hesse</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Rourke%2C+L">Laurence O'Rourke</a>, <a href="/search/astro-ph?searchtype=author&query=Osborn%2C+H">Hugh Osborn</a>, <a href="/search/astro-ph?searchtype=author&query=Pagano%2C+I">Isabella Pagano</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">Giampaolo Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">Don Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Ragazzoni%2C+R">Roberto Ragazzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">Gavin Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Udry%2C+S">St茅phane Udry</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">Thierry Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Benz%2C+W">Willy Benz</a>, <a href="/search/astro-ph?searchtype=author&query=Brandeker%2C+A">Alexis Brandeker</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCdel%2C+M">Manuel G眉del</a>, <a href="/search/astro-ph?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/2405.17155">arXiv:2405.17155</a> <span> [<a href="https://arxiv.org/pdf/2405.17155">pdf</a>, <a href="https://arxiv.org/format/2405.17155">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/10.1051/0004-6361/202449559">10.1051/0004-6361/202449559 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A low-mass sub-Neptune planet transiting the bright active star HD 73344 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sulis%2C+S">S. Sulis</a>, <a href="/search/astro-ph?searchtype=author&query=Crossfield%2C+I+J+M">I. J. M. Crossfield</a>, <a href="/search/astro-ph?searchtype=author&query=Santerne%2C+A">A. Santerne</a>, <a href="/search/astro-ph?searchtype=author&query=Saillenfest%2C+M">M. Saillenfest</a>, <a href="/search/astro-ph?searchtype=author&query=Sousa%2C+S">S. Sousa</a>, <a href="/search/astro-ph?searchtype=author&query=Mary%2C+D">D. Mary</a>, <a href="/search/astro-ph?searchtype=author&query=Aguichine%2C+A">A. Aguichine</a>, <a href="/search/astro-ph?searchtype=author&query=Deleuil%2C+M">M. Deleuil</a>, <a href="/search/astro-ph?searchtype=author&query=Mena%2C+E+D">E. Delgado Mena</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Polanski%2C+A">A. Polanski</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Boisse%2C+I">I. Boisse</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">J. C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Cretignier%2C+M">M. Cretignier</a>, <a href="/search/astro-ph?searchtype=author&query=Heidari%2C+N">N. Heidari</a>, <a href="/search/astro-ph?searchtype=author&query=Lebarb%C3%A9%2C+C">C. Lebarb茅</a>, <a href="/search/astro-ph?searchtype=author&query=Forveille%2C+T">T. Forveille</a>, <a href="/search/astro-ph?searchtype=author&query=Hara%2C+N">N. Hara</a>, <a href="/search/astro-ph?searchtype=author&query=Meunier%2C+N">N. Meunier</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N">N. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Balcarcel-Salazar%2C+S">S. Balcarcel-Salazar</a>, <a href="/search/astro-ph?searchtype=author&query=Cort%C3%A9s-Zuleta%2C+P">P. Cort茅s-Zuleta</a>, <a href="/search/astro-ph?searchtype=author&query=Dalal%2C+S">S. Dalal</a>, <a href="/search/astro-ph?searchtype=author&query=Gorjian%2C+V">V. Gorjian</a> , et al. (11 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="2405.17155v1-abstract-short" style="display: inline;"> Context. Planets with radii of between 2-4 RE closely orbiting solar-type stars are of significant importance for studying the transition from rocky to giant planets. Aims. Our goal is to determine the mass of a transiting planet around the very bright F6 star HD 73344 . This star exhibits high activity and has a rotation period that is close to the orbital period of the planet. Methods. The t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17155v1-abstract-full').style.display = 'inline'; document.getElementById('2405.17155v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17155v1-abstract-full" style="display: none;"> Context. Planets with radii of between 2-4 RE closely orbiting solar-type stars are of significant importance for studying the transition from rocky to giant planets. Aims. Our goal is to determine the mass of a transiting planet around the very bright F6 star HD 73344 . This star exhibits high activity and has a rotation period that is close to the orbital period of the planet. Methods. The transiting planet, initially a K2 candidate, is confirmed through TESS observations . We refined its parameters and rule out a false positive with Spitzer observations. We analyzed high-precision RV data from the SOPHIE and HIRES spectrographs. We conducted separate and joint analyses using the PASTIS software. We used a novel observing strategy, targeting the star at high cadence for two consecutive nights with SOPHIE to understand the short-term stellar variability. We modeled stellar noise with two Gaussian processes. Results. High-cadence RV observations provide better constraints on stellar variability and precise orbital parameters for the transiting planet. The derived mean density suggests a sub-Neptune-type composition, but uncertainties in the planet's mass prevent a detailed characterization. In addition, we find a periodic signal in the RV data that we attribute to the signature of a nontransiting exoplanet, without totally excluding the possibility of a nonplanetary origin. Dynamical analyses confirm the stability of the two-planet system and provide constraints on the inclination of the candidate planet; these findings favor a near-coplanar system. Conclusions. While the transiting planet orbits the bright star at a short period, stellar activity prevented us from precise mass measurements. Long-term RV tracking of this planet could improve this measurement, as well as our understanding of the activity of the host star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17155v1-abstract-full').style.display = 'none'; document.getElementById('2405.17155v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.11523">arXiv:2404.11523</a> <span> [<a href="https://arxiv.org/pdf/2404.11523">pdf</a>, <a href="https://arxiv.org/format/2404.11523">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/10.1051/0004-6361/202348370">10.1051/0004-6361/202348370 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">J. C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Xuan%2C+J+W">J. W. Xuan</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/astro-ph?searchtype=author&query=Molli%C3%A8re%2C+P">P. Molli猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Bartos%2C+R">R. Bartos</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+G+A">G. A. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Calvin%2C+B">B. Calvin</a>, <a href="/search/astro-ph?searchtype=author&query=Cetre%2C+S">S. Cetre</a>, <a href="/search/astro-ph?searchtype=author&query=Delorme%2C+J">J. Delorme</a>, <a href="/search/astro-ph?searchtype=author&query=Doppmann%2C+G">G. Doppmann</a>, <a href="/search/astro-ph?searchtype=author&query=Echeveri%2C+D">D. Echeveri</a>, <a href="/search/astro-ph?searchtype=author&query=Finnerty%2C+L">L. Finnerty</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzgerald%2C+M+P">M. P. Fitzgerald</a>, <a href="/search/astro-ph?searchtype=author&query=Hsu%2C+C">C. Hsu</a>, <a href="/search/astro-ph?searchtype=author&query=Jovanovic%2C+N">N. Jovanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+R">R. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Mawet%2C+D">D. Mawet</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+E">E. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Pezzato%2C+J">J. Pezzato</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+C+L">C. L. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffio%2C+J">J. Ruffio</a>, <a href="/search/astro-ph?searchtype=author&query=Sappey%2C+B">B. Sappey</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="2404.11523v1-abstract-short" style="display: inline;"> Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear insights into the formation channel of individual objects. Aims. Using the Keck Planet Imager and Characterizer (KPIC; R = 35,000), we aim to characterize a young brown dwarf HD 984 B. By measuring its C/O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11523v1-abstract-full').style.display = 'inline'; document.getElementById('2404.11523v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.11523v1-abstract-full" style="display: none;"> Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear insights into the formation channel of individual objects. Aims. Using the Keck Planet Imager and Characterizer (KPIC; R = 35,000), we aim to characterize a young brown dwarf HD 984 B. By measuring its C/O and 12CO/13CO ratios, we expect to gain new knowledge about its origin by confirming the difference in the formation pathways between brown dwarfs and super-Jupiters. Methods. We analysed the KPIC high-resolution spectrum (2.29-2.49 渭m) of HD 984 B using an atmospheric retrieval framework based on nested sampling and petitRADTRANS, using both clear and cloudy models. Results. Using our best-fit model, we find C/O = 0.50+0.01-0.01 (0.01 is the statistical error) for HD 984 B which agrees with that of its host star within 1蟽 (0.40+0.20-0.20). We also retrieve an isotopolog 12CO/13CO ratio of 98+20-25 in its atmosphere, which is similar to that of the Sun. In addition, HD 984 B has a substellar metallicity with [Fe/H] = -0.62+0.02-0.02. Finally, we find that most of the retrieved parameters are independent of our choice of retrieval model. Conclusions. From our measured C/O and 12CO/13CO, the favored formation mechanism of HD 984 B seems to be via gravitational collapse or disk instability and not core accretion, which is a favored formation mechanism for giant exoplanets with m < 13 MJup and semimajor axis between 10 and 100 au. However, with only a few brown dwarfs with a measured 12CO/13CO ratio, similar analyses using high-resolution spectroscopy will become essential in order to determine planet formation processes more precisely. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11523v1-abstract-full').style.display = 'none'; document.getElementById('2404.11523v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A294 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.13527">arXiv:2311.13527</a> <span> [<a href="https://arxiv.org/pdf/2311.13527">pdf</a>, <a href="https://arxiv.org/format/2311.13527">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> <p class="title is-5 mathjax"> $尾$ Pictoris b through the eyes of the upgraded CRIRES+ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Landman%2C+R">Rico Landman</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">Tomas Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I">Ignas Snellen</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">Jean Costes</a>, <a href="/search/astro-ph?searchtype=author&query=de+Regt%2C+S">Sam de Regt</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Yapeng Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Gandhi%2C+S">Siddharth Gandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Molli%C3%A8re%2C+P">Paul Molli猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Kesseli%2C+A">Aurora Kesseli</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">Arthur Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-L%C3%B3pez%2C+A">Alejandro S谩nchez-L贸pez</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="2311.13527v1-abstract-short" style="display: inline;"> Context: High-resolution spectrographs fed by adaptive optics (AO) provide a unique opportunity to characterize directly imaged exoplanets. Observations with such instruments allow us to probe the atmospheric composition, spin rotation, and radial velocity of the planet, thereby helping to reveal information on its formation and migration history. The recent upgrade of the Cryogenic High-Resolutio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13527v1-abstract-full').style.display = 'inline'; document.getElementById('2311.13527v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.13527v1-abstract-full" style="display: none;"> Context: High-resolution spectrographs fed by adaptive optics (AO) provide a unique opportunity to characterize directly imaged exoplanets. Observations with such instruments allow us to probe the atmospheric composition, spin rotation, and radial velocity of the planet, thereby helping to reveal information on its formation and migration history. The recent upgrade of the Cryogenic High-Resolution Infrared Echelle Spectrograph (CRIRES+) at the VLT makes it a highly suitable instrument for characterizing directly imaged exoplanets. Aims: In this work, we report on observations of $尾$ Pictoris b with CRIRES+ and use them to constrain the planets atmospheric properties and update the estimation of its spin rotation. Methods: The data were reduced using the open-source \textit{pycrires} package. We subsequently forward-modeled the stellar, planetary, and systematic contribution to the data to detect molecules in the planet's atmosphere. We also used atmospheric retrievals to provide new constraints on its atmosphere. Results: We confidently detected water and carbon monoxide in the atmosphere of $尾$ Pictoris b and retrieved a slightly sub-solar carbon-to-oxygen ratio, which is in agreement with previous results. The interpretation is hampered by our limited knowledge of the C/O ratio of the host star. We also obtained a much improved constraint on its spin rotation of $19.9 \pm 1.0$ km/s, which gives a rotation period of $8.7 \pm 0.8$ hours, assuming no obliquity. We find that there is a degeneracy between the metallicity and clouds, but this has minimal impact on the retrieved C/O, $v\sin{i}$, and radial velocity. Our results show that CRIRES+ is performing well and stands as a highly useful instrument for characterizing directly imaged planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13527v1-abstract-full').style.display = 'none'; document.getElementById('2311.13527v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 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">Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.12390">arXiv:2309.12390</a> <span> [<a href="https://arxiv.org/pdf/2309.12390">pdf</a>, <a href="https://arxiv.org/format/2309.12390">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"> First light of VLT/HiRISE: High-resolution spectroscopy of young giant exoplanets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Morsy%2C+M+E">M. El Morsy</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+M">M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J">J. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Muslimov%2C+E">E. Muslimov</a>, <a href="/search/astro-ph?searchtype=author&query=Viret%2C+A">A. Viret</a>, <a href="/search/astro-ph?searchtype=author&query=Charles%2C+Y">Y. Charles</a>, <a href="/search/astro-ph?searchtype=author&query=Zins%2C+G">G. Zins</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+G">G. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Costille%2C+A">A. Costille</a>, <a href="/search/astro-ph?searchtype=author&query=Paufique%2C+J">J. Paufique</a>, <a href="/search/astro-ph?searchtype=author&query=Seemann%2C+U">U. Seemann</a>, <a href="/search/astro-ph?searchtype=author&query=Houll%C3%A9%2C+M">M. Houll茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anwand-Heerwart%2C+H">H. Anwand-Heerwart</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M">M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Abinanti%2C+A">A. Abinanti</a>, <a href="/search/astro-ph?searchtype=author&query=Balard%2C+P">P. Balard</a>, <a href="/search/astro-ph?searchtype=author&query=Baraffe%2C+I">I. Baraffe</a>, <a href="/search/astro-ph?searchtype=author&query=Benedetti%2C+J+-">J. -A. Benedetti</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+P">P. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Blanco%2C+L">L. Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Beuzit%2C+J+-">J. -L. Beuzit</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+E">E. Choquet</a> , et al. (24 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="2309.12390v2-abstract-short" style="display: inline;"> A major endeavor of this decade is the direct characterization of young giant exoplanets at high spectral resolution to determine the composition of their atmosphere and infer their formation processes and evolution. Such a goal represents a major challenge owing to their small angular separation and luminosity contrast with respect to their parent stars. Instead of designing and implementing comp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12390v2-abstract-full').style.display = 'inline'; document.getElementById('2309.12390v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.12390v2-abstract-full" style="display: none;"> A major endeavor of this decade is the direct characterization of young giant exoplanets at high spectral resolution to determine the composition of their atmosphere and infer their formation processes and evolution. Such a goal represents a major challenge owing to their small angular separation and luminosity contrast with respect to their parent stars. Instead of designing and implementing completely new facilities, it has been proposed to leverage the capabilities of existing instruments that offer either high contrast imaging or high dispersion spectroscopy, by coupling them using optical fibers. In this work we present the implementation and first on-sky results of the HiRISE instrument at the very large telescope (VLT), which combines the exoplanet imager SPHERE with the recently upgraded high resolution spectrograph CRIRES using single-mode fibers. The goal of HiRISE is to enable the characterization of known companions in the $H$ band, at a spectral resolution of the order of $R = 位/螖位= 100\,000$, in a few hours of observing time. We present the main design choices and the technical implementation of the system, which is constituted of three major parts: the fiber injection module inside of SPHERE, the fiber bundle around the telescope, and the fiber extraction module at the entrance of CRIRES. We also detail the specific calibrations required for HiRISE and the operations of the instrument for science observations. Finally, we detail the performance of the system in terms of astrometry, temporal stability, optical aberrations, and transmission, for which we report a peak value of $\sim$3.9% based on sky measurements in median observing conditions. Finally, we report on the first astrophysical detection of HiRISE to illustrate its potential. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12390v2-abstract-full').style.display = 'none'; document.getElementById('2309.12390v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">17 pages, 15 figures, 3 tables. Accepted in A&A on 24 October 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.01044">arXiv:2211.01044</a> <span> [<a href="https://arxiv.org/pdf/2211.01044">pdf</a>, <a href="https://arxiv.org/format/2211.01044">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/stac3192">10.1093/mnras/stac3192 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The discovery of three hot Jupiters, NGTS-23b, 24b and 25b, and updated parameters for HATS-54b from the Next Generation Transit Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+D+G">David G. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C+A">Christopher A. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mooij%2C+E+J+W">Ernst J. W. de Mooij</a>, <a href="/search/astro-ph?searchtype=author&query=Acton%2C+J+S">Jack S. Acton</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+D+R">Douglas R. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">David R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+D+J">David J. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">Daniel Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Belardi%2C+C">Claudia Belardi</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Fran莽ois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+E+M">Edward M. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">Matthew R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">Sarah L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Eigm%C3%BCller%2C+P">Phillip Eigm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">Michael R. Goad</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">Samuel Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">Edward Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M+N">Maximilian N. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Hawthorn%2C+F">Faith Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Henderson%2C+B+A">Beth A. Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Jackman%2C+J+A+G">James A. G. Jackman</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J+S">James S. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Lendl%2C+M">Monika Lendl</a>, <a href="/search/astro-ph?searchtype=author&query=Kendall%2C+A">Alicia Kendall</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="2211.01044v1-abstract-short" style="display: inline;"> We report the discovery of three new hot Jupiters with the Next Generation Transit Survey (NGTS) as well as updated parameters for HATS-54b, which was independently discovered by NGTS. NGTS-23b, NGTS-24b and NGTS-25b have orbital periods of 4.076, 3.468, and 2.823 days and orbit G-, F- and K-type stars, respectively. NGTS-24 and HATS-54 appear close to transitioning off the main-sequence (if they… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.01044v1-abstract-full').style.display = 'inline'; document.getElementById('2211.01044v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.01044v1-abstract-full" style="display: none;"> We report the discovery of three new hot Jupiters with the Next Generation Transit Survey (NGTS) as well as updated parameters for HATS-54b, which was independently discovered by NGTS. NGTS-23b, NGTS-24b and NGTS-25b have orbital periods of 4.076, 3.468, and 2.823 days and orbit G-, F- and K-type stars, respectively. NGTS-24 and HATS-54 appear close to transitioning off the main-sequence (if they are not already doing so), and therefore are interesting targets given the observed lack of Hot Jupiters around sub-giant stars. By considering the host star luminosities and the planets' small orbital separations (0.037 - 0.050 au), we find that all four hot Jupiters are above the minimum irradiance threshold for inflation mechanisms to be effective. NGTS-23b has a mass of 0.61 $M_{J}$ and radius of 1.27 $R_{J}$ and is likely inflated. With a radius of 1.21 $R_{J}$ and mass of 0.52 $M_{J}$, NGTS-24b has a radius larger than expected from non-inflated models but its radius is smaller than the predicted radius from current Bayesian inflationary models. Finally, NGTS-25b is intermediate between the inflated and non-inflated cases, having a mass of 0.64 $M_{J}$ and a radius of 1.02 $R_{J}$. The physical processes driving radius inflation remain poorly understood, and by building the sample of hot Jupiters we can aim to identify the additional controlling parameters, such as metallicity and stellar age. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.01044v1-abstract-full').style.display = 'none'; document.getElementById('2211.01044v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 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">17 pages, 8 figures. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.01027">arXiv:2210.01027</a> <span> [<a href="https://arxiv.org/pdf/2210.01027">pdf</a>, <a href="https://arxiv.org/format/2210.01027">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/stac2884">10.1093/mnras/stac2884 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGTS-21b: An Inflated Super-Jupiter Orbiting a Metal-poor K dwarf </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alves%2C+D+R">Douglas R. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J+S">James S. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Vines%2C+J+I">Jose I. Vines</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+L+D">Louise D. Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">Samuel Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Acton%2C+J+S">Jack S. Acton</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">D. R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">Daniel Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Fran莽ois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Breytenbach%2C+H">Hannes Breytenbach</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+E+M">Edward M. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">Matthew R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">Sarah L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Eigm%C3%BCller%2C+P">Philipp Eigm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">Edward Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">Michael R. Goad</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M+N">Maximilian N. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Henderson%2C+B+A">Beth A. Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Kendall%2C+A">Alicia Kendall</a>, <a href="/search/astro-ph?searchtype=author&query=Lendl%2C+M">Monika Lendl</a>, <a href="/search/astro-ph?searchtype=author&query=Moyano%2C+M">Maximiliano Moyano</a>, <a href="/search/astro-ph?searchtype=author&query=Sefako%2C+R+R">Ramotholo R. Sefako</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+A+M+S">Alexis M. S. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Tilbrook%2C+R+H">Rosanne H. Tilbrook</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="2210.01027v2-abstract-short" style="display: inline;"> We report the discovery of NGTS-21b, a massive hot Jupiter orbiting a low-mass star as part of the Next Generation Transit Survey (NGTS). The planet has a mass and radius of $2.36 \pm 0.21$ M$_{\rm J}$, and $1.33 \pm 0.03$ R$_{\rm J}$, and an orbital period of 1.543 days. The host is a K3V ($T_{\rm eff}=4660 \pm 41$, K) metal-poor (${\rm [Fe/H]}=-0.26 \pm 0.07$, dex) dwarf star with a mass and rad… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.01027v2-abstract-full').style.display = 'inline'; document.getElementById('2210.01027v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.01027v2-abstract-full" style="display: none;"> We report the discovery of NGTS-21b, a massive hot Jupiter orbiting a low-mass star as part of the Next Generation Transit Survey (NGTS). The planet has a mass and radius of $2.36 \pm 0.21$ M$_{\rm J}$, and $1.33 \pm 0.03$ R$_{\rm J}$, and an orbital period of 1.543 days. The host is a K3V ($T_{\rm eff}=4660 \pm 41$, K) metal-poor (${\rm [Fe/H]}=-0.26 \pm 0.07$, dex) dwarf star with a mass and radius of $0.72 \pm 0.04$, M$_{\odot}$,and $0.86 \pm 0.04$, R$_{\odot}$. Its age and rotation period of $10.02^{+3.29}_{-7.30}$, Gyr and $17.88 \pm 0.08$, d respectively, are in accordance with the observed moderately low stellar activity level. When comparing NGTS-21b with currently known transiting hot Jupiters with similar equilibrium temperatures, it is found to have one of the largest measured radii despite its large mass. Inflation-free planetary structure models suggest the planet's atmosphere is inflated by $\sim21\%$, while inflationary models predict a radius consistent with observations, thus pointing to stellar irradiation as the probable origin of NGTS-21b's radius inflation. Additionally, NGTS-21b's bulk density ($1.25 \pm 0.15$, g/cm$^3$) is also amongst the largest within the population of metal-poor giant hosts ([Fe/H] < 0.0), helping to reveal a falling upper boundary in metallicity-planet density parameter space that is in concordance with core accretion formation models. The discovery of rare planetary systems such as NGTS-21 greatly contributes towards better constraints being placed on the formation and evolution mechanisms of massive planets orbiting low-mass stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.01027v2-abstract-full').style.display = 'none'; document.getElementById('2210.01027v2-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">12 pages, 13 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.06436">arXiv:2207.06436</a> <span> [<a href="https://arxiv.org/pdf/2207.06436">pdf</a>, <a href="https://arxiv.org/format/2207.06436">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"> Connecting SPHERE and CRIRES+ for the characterisation of young exoplanets at high spectral resolution: status update of VLT/HiRISE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+M">M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Morsy%2C+M+E">M. El Morsy</a>, <a href="/search/astro-ph?searchtype=author&query=Muslimov%2C+E">E. Muslimov</a>, <a href="/search/astro-ph?searchtype=author&query=Viret%2C+A">A. Viret</a>, <a href="/search/astro-ph?searchtype=author&query=Zins%2C+G">G. Zins</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+G">G. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Costille%2C+A">A. Costille</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Seemann%2C+U">U. Seemann</a>, <a href="/search/astro-ph?searchtype=author&query=Anwand-Heerwart%2C+H">H. Anwand-Heerwart</a>, <a href="/search/astro-ph?searchtype=author&query=Dohlen%2C+K">K. Dohlen</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+P">P. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J">J. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Charles%2C+Y">Y. Charles</a>, <a href="/search/astro-ph?searchtype=author&query=Tchoubaklian%2C+N">N. Tchoubaklian</a>, <a href="/search/astro-ph?searchtype=author&query=Ely%2C+T">T. Ely</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M">M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Paufique%2C+J">J. Paufique</a>, <a href="/search/astro-ph?searchtype=author&query=Beuzit%2C+J+-">J. -L. Beuzit</a>, <a href="/search/astro-ph?searchtype=author&query=Houll%C3%A9%2C+M">M. Houll茅</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Pourcelot%2C+R">R. Pourcelot</a>, <a href="/search/astro-ph?searchtype=author&query=Baraffe%2C+I">I. Baraffe</a>, <a href="/search/astro-ph?searchtype=author&query=Dorn%2C+R">R. Dorn</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="2207.06436v1-abstract-short" style="display: inline;"> New generation exoplanet imagers on large ground-based telescopes are highly optimised for the detection of young giant exoplanets in the near-infrared, but they are intrinsically limited for their characterisation by the low spectral resolution of their integral field spectrographs ($R<100$). High-dispersion spectroscopy at $R \gg 10^4$ would be a powerful tool for the characterisation of these p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06436v1-abstract-full').style.display = 'inline'; document.getElementById('2207.06436v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.06436v1-abstract-full" style="display: none;"> New generation exoplanet imagers on large ground-based telescopes are highly optimised for the detection of young giant exoplanets in the near-infrared, but they are intrinsically limited for their characterisation by the low spectral resolution of their integral field spectrographs ($R<100$). High-dispersion spectroscopy at $R \gg 10^4$ would be a powerful tool for the characterisation of these planets, but there is currently no high-resolution spectrograph with extreme adaptive optics and coronagraphy that would enable such characterisation. With project HiRISE we propose to use fiber coupling to combine the capabilities of two flagship instruments at the Very Large Telescope in Chile: the exoplanet imager SPHERE and the high-resolution spectrograph CRIRES+. The coupling will be implemented at the telescope in early 2023. We provide a general overview of the implementation of HiRISE, of its assembly, integration and testing (AIT) phase in Europe, and a brief assessment of its expected performance based on the final hardware. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06436v1-abstract-full').style.display = 'none'; document.getElementById('2207.06436v1-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 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">Submitted to SPIE Astronomical Telescopes + Instrumentation 2022, Adaptive Optics Systems VIII, Paper 12185-27</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.15894">arXiv:2203.15894</a> <span> [<a href="https://arxiv.org/pdf/2203.15894">pdf</a>, <a href="https://arxiv.org/format/2203.15894">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> </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/stac898">10.1093/mnras/stac898 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Periodic stellar variability from almost a million NGTS light curves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Briegal%2C+J+T">Joshua T. Briegal</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">Edward Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=Queloz%2C+D">Didier Queloz</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S">Simon Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Acton%2C+J+S">Jack S. Acton</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">David R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+D+J">David J. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Battley%2C+M+P">Matthew P. Battley</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">Daniel Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">Matthew R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+E+M">Edward M. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">Sarah L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Eigmuller%2C+P">Philipp Eigmuller</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">Samuel Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">Michael R. Goad</a>, <a href="/search/astro-ph?searchtype=author&query=Gunther%2C+M+N">Maximilian N. Gunther</a>, <a href="/search/astro-ph?searchtype=author&query=Henderson%2C+B+A">Beth A. Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Jackman%2C+J+A+G">James A. G. Jackman</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J+S">James S. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kreutzer%2C+L+T">Lars T. Kreutzer</a>, <a href="/search/astro-ph?searchtype=author&query=Moyano%2C+M">Maximiliano Moyano</a>, <a href="/search/astro-ph?searchtype=author&query=Lendl%2C+M">Monika Lendl</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+G+D">Gareth D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Tilbrook%2C+R+H">Rosanna H. Tilbrook</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="2203.15894v1-abstract-short" style="display: inline;"> We analyse 829,481 stars from the Next Generation Transit Survey (NGTS) to extract variability periods. We utilise a generalisation of the autocorrelation function (the G-ACF), which applies to irregularly sampled time series data. We extract variability periods for 16,880 stars from late-A through to mid-M spectral types and periods between 0.1 and 130 days with no assumed variability model. We f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15894v1-abstract-full').style.display = 'inline'; document.getElementById('2203.15894v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.15894v1-abstract-full" style="display: none;"> We analyse 829,481 stars from the Next Generation Transit Survey (NGTS) to extract variability periods. We utilise a generalisation of the autocorrelation function (the G-ACF), which applies to irregularly sampled time series data. We extract variability periods for 16,880 stars from late-A through to mid-M spectral types and periods between 0.1 and 130 days with no assumed variability model. We find variable signals associated with a number of astrophysical phenomena, including stellar rotation, pulsations and multiple-star systems. The extracted variability periods are compared with stellar parameters taken from Gaia DR2, which allows us to identify distinct regions of variability in the Hertzsprung-Russell Diagram. We explore a sample of rotational main-sequence objects in period-colour space, in which we observe a dearth of rotation periods between 15 and 25 days. This 'bi-modality' was previously only seen in space-based data. We demonstrate that stars in sub-samples above and below the period gap appear to arise from a stellar population not significantly contaminated by excess multiple systems. We also observe a small population of long-period variable M-dwarfs, which highlight a departure from the predictions made by rotational evolution models fitted to solar-type main-sequence objects. The NGTS data spans a period and spectral type range that links previous rotation studies such as those using data from Kepler, K2 and MEarth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15894v1-abstract-full').style.display = 'none'; document.getElementById('2203.15894v1-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 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">22 pages, 13 figures, 3 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.01915">arXiv:2105.01915</a> <span> [<a href="https://arxiv.org/pdf/2105.01915">pdf</a>, <a href="https://arxiv.org/format/2105.01915">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab1183">10.1093/mnras/stab1183 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Long-term stellar activity variations and their effect on radial-velocity measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C+A">Christopher A. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mooij%2C+E">Ernst de Mooij</a>, <a href="/search/astro-ph?searchtype=author&query=Saar%2C+S+H">Steven H. Saar</a>, <a href="/search/astro-ph?searchtype=author&query=Dumusque%2C+X">Xavier Dumusque</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+C">Andrew Collier Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+D+F">David F. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M+N">Maximilian N. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J+S">James S. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Mortier%2C+A">Annelies Mortier</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+A+P+G">Andrew P. G. Thompson</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="2105.01915v1-abstract-short" style="display: inline;"> Long-term stellar activity variations can affect the detectability of long-period and Earth-analogue extrasolar planets. We have, for 54 stars, analysed the long-term trend of five activity indicators: log$R'_\mathrm{HK}$, the cross-correlation function (CCF) bisector span, CCF full-width-at-half-maximum, CCF contrast, and the area of the Gaussian fit to the CCF; and studied their correlation with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.01915v1-abstract-full').style.display = 'inline'; document.getElementById('2105.01915v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.01915v1-abstract-full" style="display: none;"> Long-term stellar activity variations can affect the detectability of long-period and Earth-analogue extrasolar planets. We have, for 54 stars, analysed the long-term trend of five activity indicators: log$R'_\mathrm{HK}$, the cross-correlation function (CCF) bisector span, CCF full-width-at-half-maximum, CCF contrast, and the area of the Gaussian fit to the CCF; and studied their correlation with the RVs. The sign of the correlations appears to vary as a function of stellar spectral type, and the transition in sign signals a noteworthy change in the stellar activity properties where earlier type stars appear more plage dominated. These transitions become more clearly defined when considered as a function of the convective zone depth. Therefore, it is the convective zone depth (which can be altered by stellar metallicity) that appears to be the underlying fundamental parameter driving the observed activity correlations. In addition, for most of the stars, we find that the RVs become increasingly red-shifted as activity levels increase, which can be explained by the increase in the suppression of convective blue-shift. However, we also find a minority of stars where the RVs become increasingly blue-shifted as activity levels increase. Finally, using the correlation found between activity indicators and RVs, we removed RV signals generated by long-term changes in stellar activity. We find that performing simple cleaning of such long-term signals enables improved planet detection at longer orbital periods. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.01915v1-abstract-full').style.display = 'none'; document.getElementById('2105.01915v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">22 pages, 9 figures, accepted for publication in the 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/2103.10302">arXiv:2103.10302</a> <span> [<a href="https://arxiv.org/pdf/2103.10302">pdf</a>, <a href="https://arxiv.org/format/2103.10302">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/stab815">10.1093/mnras/stab815 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGTS 15b, 16b, 17b and 18b: four hot Jupiters from the Next Generation Transit Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tilbrook%2C+R+H">Rosanna H. Tilbrook</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">Matthew R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">Samuel Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+L+D">Louise D. Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Vines%2C+J+I">Jos茅 I. Vines</a>, <a href="/search/astro-ph?searchtype=author&query=Queloz%2C+D">Didier Queloz</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">Simon T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Worters%2C+H+L">Hannah L. Worters</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">Michael R. Goad</a>, <a href="/search/astro-ph?searchtype=author&query=Acton%2C+J+S">Jack S. Acton</a>, <a href="/search/astro-ph?searchtype=author&query=Henderson%2C+B+A">Beth A. Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+D+J">David J. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">David R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">Daniel Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Fran莽ois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Briegal%2C+J+T">Joshua T. Briegal</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+E+M">Edward M. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">Sarah L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Chaushev%2C+A">Alexander Chaushev</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+B+F">Benjamin F. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Eigm%C3%BCller%2C+P">Philipp Eigm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">Edward Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M+N">Maximilian N. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Hogan%2C+A">Aleisha Hogan</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="2103.10302v1-abstract-short" style="display: inline;"> We report the discovery of four new hot Jupiters with the Next Generation Transit Survey (NGTS). NGTS-15b, NGTS-16b, NGTS-17b, and NGTS-18b are short-period ($P<5$d) planets orbiting G-type main sequence stars, with radii and masses between $1.10-1.30$ $R_J$ and $0.41-0.76$ $M_J$. By considering the host star luminosities and the planets' small orbital separations ($0.039-0.052$ AU), we find that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.10302v1-abstract-full').style.display = 'inline'; document.getElementById('2103.10302v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.10302v1-abstract-full" style="display: none;"> We report the discovery of four new hot Jupiters with the Next Generation Transit Survey (NGTS). NGTS-15b, NGTS-16b, NGTS-17b, and NGTS-18b are short-period ($P<5$d) planets orbiting G-type main sequence stars, with radii and masses between $1.10-1.30$ $R_J$ and $0.41-0.76$ $M_J$. By considering the host star luminosities and the planets' small orbital separations ($0.039-0.052$ AU), we find that all four hot Jupiters are highly irradiated and therefore occupy a region of parameter space in which planetary inflation mechanisms become effective. Comparison with statistical studies and a consideration of the planets' high incident fluxes reveals that NGTS-16b, NGTS-17b, and NGTS-18b are indeed likely inflated, although some disparities arise upon analysis with current Bayesian inflationary models. However, the underlying relationships which govern radius inflation remain poorly understood. We postulate that the inclusion of additional hyperparameters to describe latent factors such as heavy element fraction, as well as the addition of an updated catalogue of hot Jupiters, would refine inflationary models, thus furthering our understanding of the physical processes which give rise to inflated planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.10302v1-abstract-full').style.display = 'none'; document.getElementById('2103.10302v1-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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 in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.01470">arXiv:2101.01470</a> <span> [<a href="https://arxiv.org/pdf/2101.01470">pdf</a>, <a href="https://arxiv.org/format/2101.01470">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/10.1051/0004-6361/202039712">10.1051/0004-6361/202039712 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGTS-14Ab: a Neptune-sized transiting planet in the desert </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Acton%2C+J+S">J. S. Acton</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">D. R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+D+J">D. J. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">D. Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Belardi%2C+C">C. Belardi</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">F. Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Brahm%2C+R">R. Brahm</a>, <a href="/search/astro-ph?searchtype=author&query=Briegal%2C+J+T">J. T. Briegal</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+E+M">E. M. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">M. R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Chaushev%2C+A">A. Chaushev</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+B+F">B. F. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">J. C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Csizmadia%2C+S">Sz. Csizmadia</a>, <a href="/search/astro-ph?searchtype=author&query=Eigm%C3%BCller%2C+P">Ph. Eigm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Erikson%2C+A">A. Erikson</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">S. Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">E. Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">M. R. Goad</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Henderson%2C+B+A">B. A. Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Hogan%2C+A">A. Hogan</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">A. Jord谩n</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="2101.01470v1-abstract-short" style="display: inline;"> Context: The sub-Jovian or Neptunian desert is a previously-identified region of parameter space where there is a relative dearth of intermediate-mass planets at short orbital periods. Aims: We present the discovery of a new transiting planetary system within the Neptunian desert, NGTS-14. Methods: Transits of NGTS-14Ab were discovered in photometry from the Next Generation Transit Survey (NGT… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01470v1-abstract-full').style.display = 'inline'; document.getElementById('2101.01470v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.01470v1-abstract-full" style="display: none;"> Context: The sub-Jovian or Neptunian desert is a previously-identified region of parameter space where there is a relative dearth of intermediate-mass planets at short orbital periods. Aims: We present the discovery of a new transiting planetary system within the Neptunian desert, NGTS-14. Methods: Transits of NGTS-14Ab were discovered in photometry from the Next Generation Transit Survey (NGTS). Follow-up transit photometry was conducted from several ground-based facilities, as well as extracted from TESS full-frame images. We combine radial velocities from the HARPS spectrograph with the photometry in a global analysis to determine the system parameters. Results: NGTS-14Ab has a radius about 30 per cent larger than that of Neptune ($0.444\pm0.030~\mathrm{R_{Jup}}$), and is around 70 per cent more massive than Neptune ($0.092 \pm 0.012~\mathrm{M_{Jup}}$). It transits the main-sequence K1 star, NGTS-14A, with a period of 3.54 days, just far enough to have maintained at least some of its primordial atmosphere. We have also identified a possible long-period stellar mass companion to the system, NGTS-14B, and we investigate the binarity of exoplanet host stars inside and outside the Neptunian desert using Gaia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01470v1-abstract-full').style.display = 'none'; document.getElementById('2101.01470v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">11 pages, 7 figures. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 646, A183 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.09830">arXiv:2004.09830</a> <span> [<a href="https://arxiv.org/pdf/2004.09830">pdf</a>, <a href="https://arxiv.org/format/2004.09830">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> <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/10.1093/mnras/staa1010">10.1093/mnras/staa1010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The spectral impact of magnetic activity on disk-integrated HARPS-N solar observations: exploring new activity indicators </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+A+P+G">A. P. G. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C+A">C. A. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">J. C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mooij%2C+E">E. de Mooij</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+D+F">D. F. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Saar%2C+S+H">S. H. Saar</a>, <a href="/search/astro-ph?searchtype=author&query=Mortier%2C+A">A. Mortier</a>, <a href="/search/astro-ph?searchtype=author&query=Milbourne%2C+T+W">T. W. Milbourne</a>, <a href="/search/astro-ph?searchtype=author&query=Aigrain%2C+S">S. Aigrain</a>, <a href="/search/astro-ph?searchtype=author&query=Cegla%2C+H+M">H. M. Cegla</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonneau%2C+D">D. Charbonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/astro-ph?searchtype=author&query=Ghedina%2C+A">A. Ghedina</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+D+W">D. W. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Morales%2C+M">M. L贸pez-Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+S">S. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Walsworth%2C+R">R. Walsworth</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="2004.09830v1-abstract-short" style="display: inline;"> Stellar activity is the major roadblock on the path to finding true Earth-analogue planets with the Doppler technique. Thus, identifying new indicators that better trace magnetic activity (i.e. faculae and spots) is crucial to aid in disentangling these signals from that of a planet's Doppler wobble. In this work, we investigate activity related features as seen in disk-integrated spectra from the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.09830v1-abstract-full').style.display = 'inline'; document.getElementById('2004.09830v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.09830v1-abstract-full" style="display: none;"> Stellar activity is the major roadblock on the path to finding true Earth-analogue planets with the Doppler technique. Thus, identifying new indicators that better trace magnetic activity (i.e. faculae and spots) is crucial to aid in disentangling these signals from that of a planet's Doppler wobble. In this work, we investigate activity related features as seen in disk-integrated spectra from the HARPS-N solar telescope. We divide high-activity spectral echelle orders by low-activity master templates (as defined using both log R'HK and images from the Solar Dynamics Observatory, SDO), creating "relative spectra". With resolved images of the surface of the Sun (via SDO), the faculae and spot filling factors can be calculated, giving a measure of activity independent of, and in addition to, log R'HK. We find pseudo-emission (and pseudo-absorption) features in the relative spectra that are similar to those reported in our previous work on alpha Cen B. In alpha Cen B, the features are shown to correlate better to changes in faculae filling factor than spot filling factor. In this work we more confidently identify changes in faculae coverage of the visible hemisphere of the Sun as the source of features produced in the relative spectra. Finally, we produce trailed spectra to observe the RV component of the features, which show that the features move in a redward direction as one would expect when tracking active regions rotating on the surface of a star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.09830v1-abstract-full').style.display = 'none'; document.getElementById('2004.09830v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 10 figures, accepted for publication in the 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/1911.02814">arXiv:1911.02814</a> <span> [<a href="https://arxiv.org/pdf/1911.02814">pdf</a>, <a href="https://arxiv.org/format/1911.02814">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/10.1093/mnras/stz3140">10.1093/mnras/stz3140 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGTS-8b and NGTS-9b: two non-inflated hot-Jupiters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C+A">Christopher A. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Belardi%2C+C">Claudia Belardi</a>, <a href="/search/astro-ph?searchtype=author&query=Braker%2C+I+P">Ian P. Braker</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">Matthew R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">Sarah L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Eigm%C3%BCller%2C+P">Philipp Eigm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M+N">Maximilian N. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Jackman%2C+J+A+G">James A. G. Jackman</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+L+D">Louise D. Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Soto%2C+M+G">Maritza G. Soto</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+O">Oliver Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">David R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">Daniel Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Fran莽ois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Briegal%2C+J+T">Joshua T. Briegal</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+E+M">Edward M. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J">Juan Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Chaushev%2C+A">Alexander Chaushev</a>, <a href="/search/astro-ph?searchtype=author&query=Csizmadia%2C+S">Szilard Csizmadia</a>, <a href="/search/astro-ph?searchtype=author&query=Erikson%2C+A">Anders Erikson</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">Samuel Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">Edward Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">Michael R. Goad</a>, <a href="/search/astro-ph?searchtype=author&query=Hooton%2C+M+J">Matthew J. Hooton</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="1911.02814v1-abstract-short" style="display: inline;"> We report the discovery, by the Next Generation Transit Survey (NGTS), of two hot-Jupiters NGTS-8b and NGTS-9b. These orbit a V = 13.68 K0V star (Teff = 5241 +/- 50 K) with a period of 2.49970 days, and a V = 12.80 F8V star (Teff = 6330 +/- 130 K) in 4.43527 days, respectively. The transits were independently verified by follow-up photometric observations with the SAAO 1.0-m and Euler telescopes,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.02814v1-abstract-full').style.display = 'inline'; document.getElementById('1911.02814v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.02814v1-abstract-full" style="display: none;"> We report the discovery, by the Next Generation Transit Survey (NGTS), of two hot-Jupiters NGTS-8b and NGTS-9b. These orbit a V = 13.68 K0V star (Teff = 5241 +/- 50 K) with a period of 2.49970 days, and a V = 12.80 F8V star (Teff = 6330 +/- 130 K) in 4.43527 days, respectively. The transits were independently verified by follow-up photometric observations with the SAAO 1.0-m and Euler telescopes, and we report on the planetary parameters using HARPS, FEROS and CORALIE radial velocities. NGTS-8b has a mass, 0.93 +0.04 -0.03 MJ and a radius, 1.09 +/- 0.03 RJ similar to Jupiter, resulting in a density of 0.89 +0.08 -0.07 g cm-3. This is in contrast to NGTS-9b, which has a mass of 2.90 +/- 0.17 MJ and a radius of 1.07 +/- 0.06 RJ , resulting in a much greater density of 2.93 +0.53 -0.49 g cm-3. Statistically, the planetary parameters put both objects in the regime where they would be expected to exhibit larger than predicted radii. However, we find that their radii are in agreement with predictions by theoretical non-inflated models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.02814v1-abstract-full').style.display = 'none'; document.getElementById('1911.02814v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </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, 7 figures, accepted for publication in the 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/1909.12424">arXiv:1909.12424</a> <span> [<a href="https://arxiv.org/pdf/1909.12424">pdf</a>, <a href="https://arxiv.org/format/1909.12424">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/staa115">10.1093/mnras/staa115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGTS-10b: The shortest period hot Jupiter yet discovered </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McCormac%2C+J">James McCormac</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">Edward Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=Jackman%2C+J+A+G">James A. G. Jackman</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+D+J+A">David J. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">Daniel Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Wheatley%2C+P+J">Peter J. Wheatley</a>, <a href="/search/astro-ph?searchtype=author&query=West%2C+R+G">Richard G. West</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">David R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+D+J">David J. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Francois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Briegal%2C+J+T">Joshua T. Briegal</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">Matthew R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J">Juan Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">Sarah L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Chaushev%2C+A">Alexander Chaushev</a>, <a href="/search/astro-ph?searchtype=author&query=Chazelas%2C+B">Bruno Chazelas</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">Paul Chote</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+B+F">Benjamin F. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Csizmadia%2C+S">Szilard Csizmadia</a>, <a href="/search/astro-ph?searchtype=author&query=Eigmuller%2C+P">Philipp Eigmuller</a>, <a href="/search/astro-ph?searchtype=author&query=Erikson%2C+A">Anders Erikson</a>, <a href="/search/astro-ph?searchtype=author&query=Foxell%2C+E">Emma Foxell</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensicke%2C+B+T">Boris T. Gaensicke</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">Michael R. Goad</a> , et al. (22 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="1909.12424v2-abstract-short" style="display: inline;"> We report the discovery of a new ultra-short period transiting hot Jupiter from the Next Generation Transit Survey (NGTS). NGTS-10b has a mass and radius of $2.162\,^{+0.092}_{-0.107}$ M$_{\rm J}$ and $1.205\,^{+0.117}_{-0.083}$ R$_{\rm J}$ and orbits its host star with a period of $0.7668944\pm0.0000003$ days, making it the shortest period hot Jupiter yet discovered. The host is a $10.4\pm2.5$ Gy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.12424v2-abstract-full').style.display = 'inline'; document.getElementById('1909.12424v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.12424v2-abstract-full" style="display: none;"> We report the discovery of a new ultra-short period transiting hot Jupiter from the Next Generation Transit Survey (NGTS). NGTS-10b has a mass and radius of $2.162\,^{+0.092}_{-0.107}$ M$_{\rm J}$ and $1.205\,^{+0.117}_{-0.083}$ R$_{\rm J}$ and orbits its host star with a period of $0.7668944\pm0.0000003$ days, making it the shortest period hot Jupiter yet discovered. The host is a $10.4\pm2.5$ Gyr old K5V star ($T_\mathrm{eff}$=$4400\pm100$\,K) of Solar metallicity ([Fe/H] = $-0.02\pm0.12$\,dex) showing moderate signs of stellar activity. NGTS-10b joins a short list of ultra-short period Jupiters that are prime candidates for the study of star-planet tidal interactions. NGTS-10b orbits its host at just $1.46\pm0.18$ Roche radii, and we calculate a median remaining inspiral time of $38$\,Myr and a potentially measurable transit time shift of $7$\,seconds over the coming decade, assuming a stellar tidal quality factor $Q'_{\rm s}=2\times10^{7}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.12424v2-abstract-full').style.display = 'none'; document.getElementById('1909.12424v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 19 figures and 5 tables. Submitted 27 Sept 2019. Accepted 10 Jan 2020. Published 20 Feb 2020</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.08219">arXiv:1906.08219</a> <span> [<a href="https://arxiv.org/pdf/1906.08219">pdf</a>, <a href="https://arxiv.org/format/1906.08219">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz2496">10.1093/mnras/stz2496 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGTS-7Ab: An ultra-short period brown dwarf transiting a tidally-locked and active M dwarf </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jackman%2C+J+A+G">James A. G. Jackman</a>, <a href="/search/astro-ph?searchtype=author&query=Wheatley%2C+P+J">Peter J. Wheatley</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+D">Dan Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">Samuel Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">Simon T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">Matthew R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Braker%2C+I+P">Ian P. Braker</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M+N">Maximilian N. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Louden%2C+T">Tom Louden</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+O">Oliver Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">David R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Belardi%2C+C">Claudia Belardi</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Fran莽ois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Briegal%2C+J+T">Joshua T. Briegal</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+E+M">Edward M. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J">Juan Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">Sarah L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Chaushev%2C+A">Alexander Chaushev</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J+C">Jean C. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Csizmadia%2C+S">Szilard Csizmadia</a>, <a href="/search/astro-ph?searchtype=author&query=Eigm%C3%BCller%2C+P">Philipp Eigm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Erikson%2C+A">Anders Erikson</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A4nsicke%2C+B+T">Boris T. G盲nsicke</a>, <a href="/search/astro-ph?searchtype=author&query=Gillen%2C+E">Edward Gillen</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">Michael R. Goad</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="1906.08219v2-abstract-short" style="display: inline;"> We present the discovery of NGTS-7Ab, a high mass brown dwarf transiting an M dwarf with a period of 16.2 hours, discovered as part of the Next Generation Transit Survey (NGTS). This is the shortest period transiting brown dwarf around a main or pre-main sequence star to date. The M star host (NGTS-7A) has an age of roughly 55 Myr and is in a state of spin-orbit synchronisation, which we attribute… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.08219v2-abstract-full').style.display = 'inline'; document.getElementById('1906.08219v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.08219v2-abstract-full" style="display: none;"> We present the discovery of NGTS-7Ab, a high mass brown dwarf transiting an M dwarf with a period of 16.2 hours, discovered as part of the Next Generation Transit Survey (NGTS). This is the shortest period transiting brown dwarf around a main or pre-main sequence star to date. The M star host (NGTS-7A) has an age of roughly 55 Myr and is in a state of spin-orbit synchronisation, which we attribute to tidal interaction with the brown dwarf acting to spin up the star. The host star is magnetically active and shows multiple flares across the NGTS and follow up lightcurves, which we use to probe the flare-starspot phase relation. The host star also has an M star companion at a separation of 1.13 arcseconds with very similar proper motion and systemic velocity, suggesting the NGTS-7 system is a hierarchical triple. The combination of tidal synchronisation and magnetic braking is expected to drive ongoing decay of the brown dwarf orbit, with a remaining lifetime of only 5-10 Myr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.08219v2-abstract-full').style.display = 'none'; document.getElementById('1906.08219v2-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </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, 16 figures, accepted for publication in the 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/1906.03002">arXiv:1906.03002</a> <span> [<a href="https://arxiv.org/pdf/1906.03002">pdf</a>, <a href="https://arxiv.org/format/1906.03002">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> </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/10.1051/0004-6361/201935233">10.1051/0004-6361/201935233 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Temporal evolution and correlations of optical activity indicators measured in Sun-as-a-star observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+D+F">D. F. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/astro-ph?searchtype=author&query=Lanza%2C+A+F">A. F. Lanza</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Mortier%2C+A">A. Mortier</a>, <a href="/search/astro-ph?searchtype=author&query=Saar%2C+S+H">S. H. Saar</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+K">K. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Milbourne%2C+T">T. Milbourne</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconi%2C+M">M. Cecconi</a>, <a href="/search/astro-ph?searchtype=author&query=Cegla%2C+H+M">H. M. Cegla</a>, <a href="/search/astro-ph?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Ghedina%2C+A">A. Ghedina</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+M">M. Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+J">J. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+N">N. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+C+-">C. -H. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lodi%2C+M">M. Lodi</a>, <a href="/search/astro-ph?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F">F. Pepe</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="1906.03002v1-abstract-short" style="display: inline;"> (Abridged) We perform a detailed study of the main optical activity indicators (Ca II H & K, Balmer lines, Na I D$_{\rm 1}$ D$_{\rm 2}$, and He I D$_{\rm 3}$) measured for the Sun using the data provided by the HARPS-N solar-telescope feed at the Telescopio Nazionale Galileo. The value of the solar rotation period is found in all the activity indicators, with the only exception being H$未$. The der… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.03002v1-abstract-full').style.display = 'inline'; document.getElementById('1906.03002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.03002v1-abstract-full" style="display: none;"> (Abridged) We perform a detailed study of the main optical activity indicators (Ca II H & K, Balmer lines, Na I D$_{\rm 1}$ D$_{\rm 2}$, and He I D$_{\rm 3}$) measured for the Sun using the data provided by the HARPS-N solar-telescope feed at the Telescopio Nazionale Galileo. The value of the solar rotation period is found in all the activity indicators, with the only exception being H$未$. The derived values vary from 26.29 days (H$纬$ line) to 31.23 days (He I). From an analysis of sliding periodograms we find that in most of the activity indicators the spectral power is split into several "bands" of periods around 26 and 30 days, that might be explained by the migration of active regions between the equator and a latitude of $\sim$ 30$^{\circ}$, spot evolution or a combination of both effects. In agreement with previous works a typical lifetime of active regions of $\sim$ ten rotation periods is inferred from the pooled variance diagrams. We find that H$伪$, H$尾$, H$纬$, H$蔚$, and He I show a significant correlation with the S index. Significant correlations between the contrast, bisector span, and the heliocentric radial velocity with the activity indexes are also found. We show that the full width at half maximum, the bisector, and the disc-integrated magnetic field correlate with the radial velocity variations. The correlation of the S index and H$伪$ changes with time, increasing with larger sun spot numbers and solar irradiance. A similar tendency with the S index - radial velocity correlation is also present in the data. Our results are consistent with a scenario in which higher activity favours the correlation between the S index and the H$伪$ activity indicators and between the S index and radial velocity variations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.03002v1-abstract-full').style.display = 'none'; document.getElementById('1906.03002v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </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</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 627, A118 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.12186">arXiv:1904.12186</a> <span> [<a href="https://arxiv.org/pdf/1904.12186">pdf</a>, <a href="https://arxiv.org/format/1904.12186">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz1215">10.1093/mnras/stz1215 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Three years of Sun-as-a-star radial-velocity observations on the approach to solar minimum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Mortier%2C+A">A. Mortier</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+D">D. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/astro-ph?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/astro-ph?searchtype=author&query=Langellier%2C+N">N. Langellier</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C+A">C. A. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Cegla%2C+H+M">H. M. Cegla</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonneau%2C+D">D. Charbonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Coffinet%2C+A">A. Coffinet</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+D+W">D. W. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez-Morales%2C+M">M. Lopez-Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/astro-ph?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Milbourne%2C+T">T. Milbourne</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Saar%2C+S+H">S. H. Saar</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+S">S. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Buchschacher%2C+N">N. Buchschacher</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconi%2C+M">M. Cecconi</a>, <a href="/search/astro-ph?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/astro-ph?searchtype=author&query=Ghedina%2C+A">A. Ghedina</a>, <a href="/search/astro-ph?searchtype=author&query=Glenday%2C+A">A. Glenday</a> , et al. (11 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="1904.12186v1-abstract-short" style="display: inline;"> The time-variable velocity fields of solar-type stars limit the precision of radial-velocity determinations of their planets' masses, obstructing detection of Earth twins. Since 2015 July we have been monitoring disc-integrated sunlight in daytime using a purpose-built solar telescope and fibre feed to the HARPS-N stellar radial-velocity spectrometer. We present and analyse the solar radial-veloci… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.12186v1-abstract-full').style.display = 'inline'; document.getElementById('1904.12186v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.12186v1-abstract-full" style="display: none;"> The time-variable velocity fields of solar-type stars limit the precision of radial-velocity determinations of their planets' masses, obstructing detection of Earth twins. Since 2015 July we have been monitoring disc-integrated sunlight in daytime using a purpose-built solar telescope and fibre feed to the HARPS-N stellar radial-velocity spectrometer. We present and analyse the solar radial-velocity measurements and cross-correlation function (CCF) parameters obtained in the first 3 years of observation, interpreting them in the context of spatially-resolved solar observations. We describe a Bayesian mixture-model approach to automated data-quality monitoring. We provide dynamical and daily differential-extinction corrections to place the radial velocities in the heliocentric reference frame, and the CCF shape parameters in the sidereal frame. We achieve a photon-noise limited radial-velocity precision better than 0.43 m s$^{-1}$ per 5-minute observation. The day-to-day precision is limited by zero-point calibration uncertainty with an RMS scatter of about 0.4 m s$^{-1}$. We find significant signals from granulation and solar activity. Within a day, granulation noise dominates, with an amplitude of about 0.4 m s$^{-1}$ and an autocorrelation half-life of 15 minutes. On longer timescales, activity dominates. Sunspot groups broaden the CCF as they cross the solar disc. Facular regions temporarily reduce the intrinsic asymmetry of the CCF. The radial-velocity increase that accompanies an active-region passage has a typical amplitude of 5 m s$^{-1}$ and is correlated with the line asymmetry, but leads it by 3 days. Spectral line-shape variability thus shows promise as a proxy for recovering the true radial velocity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.12186v1-abstract-full').style.display = 'none'; document.getElementById('1904.12186v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 15 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.04184">arXiv:1902.04184</a> <span> [<a href="https://arxiv.org/pdf/1902.04184">pdf</a>, <a href="https://arxiv.org/format/1902.04184">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> </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/10.3847/1538-4357/ab064a">10.3847/1538-4357/ab064a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HARPS-N Solar Radial-Velocity Variations Are Dominated By Large, Bright Magnetic Regions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Milbourne%2C+T+W">T. W. Milbourne</a>, <a href="/search/astro-ph?searchtype=author&query=Haywood%2C+R+D">R. D. Haywood</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+D+F">D. F. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Saar%2C+S+H">S. H. Saar</a>, <a href="/search/astro-ph?searchtype=author&query=Cegla%2C+H+M">H. M. Cegla</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+C">A. C. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Dumusque%2C+X">X. Dumusque</a>, <a href="/search/astro-ph?searchtype=author&query=Langellier%2C+N">N. Langellier</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+D+W">D. W. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=Maldonado%2C+J">J. Maldonado</a>, <a href="/search/astro-ph?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/astro-ph?searchtype=author&query=Mortier%2C+A">A. Mortier</a>, <a href="/search/astro-ph?searchtype=author&query=Palumbo%2C+M+L">M. L. Palumbo Iii</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+S">S. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C+A">C. A. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">F. Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Buchschacher%2C+N">N. Buchschacher</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconi%2C+M">M. Cecconi</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonneau%2C+D">D. Charbonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/astro-ph?searchtype=author&query=Ghedina%2C+A">A. Ghedina</a>, <a href="/search/astro-ph?searchtype=author&query=Glenday%2C+A+G">A. G. Glenday</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+M">M. Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+C">C-H. Li</a> , et al. (15 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="1902.04184v1-abstract-short" style="display: inline;"> State of the art radial-velocity (RV) exoplanet searches are currently limited by RV signals arising from stellar magnetic activity. We analyze solar observations acquired over a 3-year period during the decline of Carrington Cycle 24 to test models of RV variation of Sun-like stars. A purpose-built solar telescope at the High Accuracy Radial velocity Planet Searcher for the Northern hemisphere (H… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.04184v1-abstract-full').style.display = 'inline'; document.getElementById('1902.04184v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.04184v1-abstract-full" style="display: none;"> State of the art radial-velocity (RV) exoplanet searches are currently limited by RV signals arising from stellar magnetic activity. We analyze solar observations acquired over a 3-year period during the decline of Carrington Cycle 24 to test models of RV variation of Sun-like stars. A purpose-built solar telescope at the High Accuracy Radial velocity Planet Searcher for the Northern hemisphere (HARPS-N) provides disk-integrated solar spectra, from which we extract RVs and $\log{R'_{\rm HK}}$. The Solar Dynamics Observatory (SDO) provides disk-resolved images of magnetic activity. The Solar Radiation and Climate Experiment (SORCE) provides near-continuous solar photometry, analogous to a Kepler light curve. We verify that the SORCE photometry and HARPS-N $\log{R'_{\rm HK}}$ correlate strongly with the SDO-derived magnetic filling factor, while the HARPS-N RV variations do not. To explain this discrepancy, we test existing models of RV variations. We estimate the contributions of the suppression of convective blueshift and the rotational imbalance due to brightness inhomogeneities to the observed HARPS-N RVs. We investigate the time variation of these contributions over several rotation periods, and how these contributions depend on the area of active regions. We find that magnetic active regions smaller than $60 \ \rm Mm^2$ do not significantly suppress convective blueshift. Our area-dependent model reduces the amplitude of activity-induced RV variations by a factor of two. The present study highlights the need to identify a proxy that correlates specifically with large, bright magnetic regions on the surfaces of exoplanet-hosting stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.04184v1-abstract-full').style.display = 'none'; document.getElementById('1902.04184v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 7 figures, accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.05981">arXiv:1707.05981</a> <span> [<a href="https://arxiv.org/pdf/1707.05981">pdf</a>, <a href="https://arxiv.org/ps/1707.05981">ps</a>, <a href="https://arxiv.org/format/1707.05981">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</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/pasj/psx061">10.1093/pasj/psx061 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) I: Project Overview and Initial Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Umemoto%2C+T">Tomofumi Umemoto</a>, <a href="/search/astro-ph?searchtype=author&query=Minamidani%2C+T">Tetsuhiro Minamidani</a>, <a href="/search/astro-ph?searchtype=author&query=Kuno%2C+N">Nario Kuno</a>, <a href="/search/astro-ph?searchtype=author&query=Fujita%2C+S">Shinji Fujita</a>, <a href="/search/astro-ph?searchtype=author&query=Matsuo%2C+M">Mitsuhiro Matsuo</a>, <a href="/search/astro-ph?searchtype=author&query=Nishimura%2C+A">Atsushi Nishimura</a>, <a href="/search/astro-ph?searchtype=author&query=Torii%2C+K">Kazufumi Torii</a>, <a href="/search/astro-ph?searchtype=author&query=Tosaki%2C+T">Tomoka Tosaki</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+M">Mikito Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Kuriki%2C+M">Mika Kuriki</a>, <a href="/search/astro-ph?searchtype=author&query=Tsuda%2C+Y">Yuya Tsuda</a>, <a href="/search/astro-ph?searchtype=author&query=Hirota%2C+A">Akihiko Hirota</a>, <a href="/search/astro-ph?searchtype=author&query=Ohashi%2C+S">Satoshi Ohashi</a>, <a href="/search/astro-ph?searchtype=author&query=Yamagishi%2C+M">Mitsuyoshi Yamagishi</a>, <a href="/search/astro-ph?searchtype=author&query=Handa%2C+T">Toshihiro Handa</a>, <a href="/search/astro-ph?searchtype=author&query=Nakanishi%2C+H">Hiroyuki Nakanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Omodaka%2C+T">Toshihiro Omodaka</a>, <a href="/search/astro-ph?searchtype=author&query=Koide%2C+N">Nagito Koide</a>, <a href="/search/astro-ph?searchtype=author&query=Matsumoto%2C+N">Naoko Matsumoto</a>, <a href="/search/astro-ph?searchtype=author&query=Onishi%2C+T">Toshikazu Onishi</a>, <a href="/search/astro-ph?searchtype=author&query=Tokuda%2C+K">Kazuki Tokuda</a>, <a href="/search/astro-ph?searchtype=author&query=Seta%2C+M">Masumichi Seta</a>, <a href="/search/astro-ph?searchtype=author&query=Kobayashi%2C+Y">Yukinori Kobayashi</a>, <a href="/search/astro-ph?searchtype=author&query=Tachihara%2C+K">Kengo Tachihara</a>, <a href="/search/astro-ph?searchtype=author&query=Sano%2C+H">Hidetoshi Sano</a> , et al. (19 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="1707.05981v1-abstract-short" style="display: inline;"> The FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) project is one of the legacy projects using the new multi-beam FOREST receiver installed on the Nobeyama 45-m telescope. This project aims to investigate the distribution, kinematics, and physical properties of both diffuse and dense molecular gas in the Galaxy at once by observing 12CO, 13CO, and C18O J=1-0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.05981v1-abstract-full').style.display = 'inline'; document.getElementById('1707.05981v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.05981v1-abstract-full" style="display: none;"> The FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) project is one of the legacy projects using the new multi-beam FOREST receiver installed on the Nobeyama 45-m telescope. This project aims to investigate the distribution, kinematics, and physical properties of both diffuse and dense molecular gas in the Galaxy at once by observing 12CO, 13CO, and C18O J=1-0 lines simultaneously. The mapping regions are a part of the 1st quadrant (10d < l < 50d, |b| < 1d) and the 3rd quadrant (198d < l <236d, |b| < 1d) of the Galaxy, where spiral arms, bar structure, and the molecular gas ring are included. This survey achieves the highest angular resolution to date (~20") for the Galactic plane survey in the CO J=1-0 lines, which makes it possible to find dense clumps located farther away than the previous surveys. FUGIN will provide us with an invaluable dataset for investigating the physics of the galactic interstellar medium (ISM), particularly the evolution of interstellar gas covering galactic scale structures to the internal structures of giant molecular clouds, such as small filament/clump/core. We present an overview of the FUGIN project, observation plan, and initial results, which reveal wide-field and detailed structures of molecular clouds, such as entangled filaments that have not been obvious in previous surveys, and large-scale kinematics of molecular gas such as spiral arms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.05981v1-abstract-full').style.display = 'none'; document.getElementById('1707.05981v1-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 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 14 figures, accepted for publication in PASJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.06002">arXiv:1706.06002</a> <span> [<a href="https://arxiv.org/pdf/1706.06002">pdf</a>, <a href="https://arxiv.org/ps/1706.06002">ps</a>, <a href="https://arxiv.org/format/1706.06002">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A new view of the giant molecular cloud M16 (Eagle Nebula) in 12CO J=1-0 and 2-1 transitions with NANTEN2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nishimura%2C+A">Atsushi Nishimura</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">Jean Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Inaba%2C+T">Tetsuta Inaba</a>, <a href="/search/astro-ph?searchtype=author&query=Tachihara%2C+K">Kengo Tachihara</a>, <a href="/search/astro-ph?searchtype=author&query=Hattori%2C+Y">Yusuke Hattori</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+M">Mikito Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Ohama%2C+A">Akio Ohama</a>, <a href="/search/astro-ph?searchtype=author&query=Torii%2C+K">Kazufumi Torii</a>, <a href="/search/astro-ph?searchtype=author&query=Sano%2C+H">Hidetoshi Sano</a>, <a href="/search/astro-ph?searchtype=author&query=Yamamoto%2C+H">Hiroaki Yamamoto</a>, <a href="/search/astro-ph?searchtype=author&query=Hasegawa%2C+Y">Yutaka Hasegawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kimura%2C+K">Kimihiro Kimura</a>, <a href="/search/astro-ph?searchtype=author&query=Ogawa%2C+H">Hideo Ogawa</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+Y">Yasuo Fukui</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="1706.06002v1-abstract-short" style="display: inline;"> M16, the Eagle Nebula, is an outstanding HII region where extensive high-mass star formation is taking place in the Sagittarius Arm, and hosts the remarkable "pillars" observed with HST. We made new CO observations of the region in the 12CO J=1--0 and J=2--1 transitions with NANTEN2. These observations revealed for the first time that a giant molecular cloud of $\sim 1.3 \times 10^5$ \Msun \ is as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.06002v1-abstract-full').style.display = 'inline'; document.getElementById('1706.06002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.06002v1-abstract-full" style="display: none;"> M16, the Eagle Nebula, is an outstanding HII region where extensive high-mass star formation is taking place in the Sagittarius Arm, and hosts the remarkable "pillars" observed with HST. We made new CO observations of the region in the 12CO J=1--0 and J=2--1 transitions with NANTEN2. These observations revealed for the first time that a giant molecular cloud of $\sim 1.3 \times 10^5$ \Msun \ is associated with M16, which is elongated vertically to the Galactic plane over 35 pc at a distance of 1.8 kpc. We found a cavity of the molecular gas of $\sim 10$ pc diameter toward the heart of M16 at \lbeq (16.95\degree, 0.85\degree), where more than 10 O-type stars and $\sim 400$ stars are associated, in addition to a close-by molecular cavity toward a Spitzer bubble N19 at \lbeq (17.06\degree, 1.0\degree). We found three velocity components which show spatially complementary distribution in the entire M16 giant molecular cloud (GMC) including NGC6611 and N19, suggesting collisional interaction between them. Based on the above results we frame a hypothesis that collision between the red-shifted and blue-shifted components at a relative of $\sim 10$ \kms \ triggered formation of the O-type stars in the M16 GMC in the last 1-2 Myr. The collision is two fold in the sense that one of the collisional interactions is major toward the M16 cluster and the other toward N19 with a RCW120 type, the former triggered most of the O star formation with almost full ionization of the parent gas, and the latter an O star formation in N19. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.06002v1-abstract-full').style.display = 'none'; document.getElementById('1706.06002v1-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 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures, submitted to PASJ</span> </p> </li> </ol> <div class="is-hidden-tablet">  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