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</div> <div class="control"> <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/2401.13153">arXiv:2401.13153</a> <span> [<a href="https://arxiv.org/pdf/2401.13153">pdf</a>, <a href="https://arxiv.org/format/2401.13153">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> JWST Directly Images Giant Planet Candidates Around Two Metal-Polluted White Dwarf Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Debes%2C+J">John Debes</a>, <a href="/search/astro-ph?searchtype=author&query=Cracraft%2C+M">Misty Cracraft</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+F">Fergal Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Poulsen%2C+S">Sabrina Poulsen</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+L">Loic Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Thibault%2C+K">Katherine Thibault</a>, <a href="/search/astro-ph?searchtype=author&query=Reach%2C+W+T">William T. Reach</a>, <a href="/search/astro-ph?searchtype=author&query=Hermes%2C+J+J">J. J. Hermes</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Kilic%2C+M">Mukremin Kilic</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.13153v1-abstract-short" style="display: inline;"> We report the discovery of two directly imaged, giant planet candidates orbiting the metal-rich DAZ white dwarfs WD 1202-232 and WD 2105-82. JWST's Mid-Infrared Instrument (MIRI) data on these two stars show a nearby resolved source at a projected separation of 11.47 and 34.62 au, respectively. Assuming the planets formed at the same time as their host stars, with total ages of 5.3 and 1.6Gyr, the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13153v1-abstract-full').style.display = 'inline'; document.getElementById('2401.13153v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.13153v1-abstract-full" style="display: none;"> We report the discovery of two directly imaged, giant planet candidates orbiting the metal-rich DAZ white dwarfs WD 1202-232 and WD 2105-82. JWST's Mid-Infrared Instrument (MIRI) data on these two stars show a nearby resolved source at a projected separation of 11.47 and 34.62 au, respectively. Assuming the planets formed at the same time as their host stars, with total ages of 5.3 and 1.6Gyr, the MIRI photometry is consistent with giant planets with masses about 1-7 Jupiter Masses. The probability of both candidates being false positives due to red background sources is approximately 1 in 3000. If confirmed, these would be the first directly imaged planets that are similar in both age and separation to the giant planets in our own solar system, and they would demonstrate that widely separated giant planets like Jupiter survive stellar evolution. Giant planet perturbers are widely used to explain the tidal disruption of asteroids around metal-polluted white dwarfs. Confirmation of these two planet candidates with future MIRI imaging would provide evidence that directly links giant planets to metal pollution in white dwarf stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13153v1-abstract-full').style.display = 'none'; document.getElementById('2401.13153v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 Pages, 3 Figures, 2 Tables, Accepted for Publication in The Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.14165">arXiv:2311.14165</a> <span> [<a href="https://arxiv.org/pdf/2311.14165">pdf</a>, <a href="https://arxiv.org/format/2311.14165">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> A MIRI Search for Planets and Dust Around WD 2149+02 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Poulsen%2C+S">Sabrina Poulsen</a>, <a href="/search/astro-ph?searchtype=author&query=Debes%2C+J">John Debes</a>, <a href="/search/astro-ph?searchtype=author&query=Cracraft%2C+M">Misty Cracraft</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Reach%2C+W+T">William T. Reach</a>, <a href="/search/astro-ph?searchtype=author&query=Kilic%2C+M">Mukremin Kilic</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+F">Fergal Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+L">Loic Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Thibault%2C+K">Katherine Thibault</a>, <a href="/search/astro-ph?searchtype=author&query=Hermes%2C+J+J">J. J. Hermes</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</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="2311.14165v1-abstract-short" style="display: inline;"> The launch of JWST has ushered in a new era of high precision infrared astronomy, allowing us to probe nearby white dwarfs for cold dust, exoplanets, and tidally heated exomoons. While previous searches for these exoplanets have successfully ruled out companions as small as 7-10 Jupiter masses, no instrument prior to JWST has been sensitive to the likely more common sub-Jovian mass planets around… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.14165v1-abstract-full').style.display = 'inline'; document.getElementById('2311.14165v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.14165v1-abstract-full" style="display: none;"> The launch of JWST has ushered in a new era of high precision infrared astronomy, allowing us to probe nearby white dwarfs for cold dust, exoplanets, and tidally heated exomoons. While previous searches for these exoplanets have successfully ruled out companions as small as 7-10 Jupiter masses, no instrument prior to JWST has been sensitive to the likely more common sub-Jovian mass planets around white dwarfs. In this paper, we present the first multi-band photometry (F560W, F770W, F1500W, F2100W) taken of WD 2149+021 with the Mid-Infrared Instrument (MIRI) on JWST. After a careful search for both resolved and unresolved planets, we do not identify any compelling candidates around WD 2149+021. Our analysis indicates that we are sensitive to companions as small as ~0.34 MJup outwards of 1."263 (28.3 au) and ~0.64 MJup at the innermost working angle (0."654, 14.7 au) with 5 sigma confidence, placing significant constraints on any undetected companions around this white dwarf. The results of these observations emphasize the exciting future of sub-Jovian planet detection limits by JWST, which can begin to constrain how often these planets survive their host stars evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.14165v1-abstract-full').style.display = 'none'; document.getElementById('2311.14165v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.04809">arXiv:2309.04809</a> <span> [<a href="https://arxiv.org/pdf/2309.04809">pdf</a>, <a href="https://arxiv.org/format/2309.04809">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> <p class="title is-5 mathjax"> Asteroseismological analysis of the polluted ZZ Ceti star G29-38 with TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Uzundag%2C+M">Murat Uzundag</a>, <a href="/search/astro-ph?searchtype=author&query=De+Ger%C3%B3nimo%2C+F+C">Francisco C. De Ger贸nimo</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B3rsico%2C+A+H">Alejandro H. C贸rsico</a>, <a href="/search/astro-ph?searchtype=author&query=Silvotti%2C+R">Roberto Silvotti</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+P+A">Paul A. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Montgomery%2C+M+H">Michael H. Montgomery</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M谩rcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Toloza%2C+O">Odette Toloza</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+K+J">Keaton J. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Kepler%2C+S+O">S. O. Kepler</a>, <a href="/search/astro-ph?searchtype=author&query=Althaus%2C+L+G">Leandro G. Althaus</a>, <a href="/search/astro-ph?searchtype=author&query=Kleinman%2C+S+J">Scot J. Kleinman</a>, <a href="/search/astro-ph?searchtype=author&query=Kilic%2C+M">Mukremin Kilic</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</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=B%C4%85kowska%2C+K">Karolina B膮kowska</a>, <a href="/search/astro-ph?searchtype=author&query=Barber%2C+S">Sam Barber</a>, <a href="/search/astro-ph?searchtype=author&query=Nitta%2C+A">Atsuko Nitta</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="2309.04809v1-abstract-short" style="display: inline;"> G\,29$-$38 (TIC~422526868) is one of the brightest ($V=13.1$) and closest ($d = 17.51$\,pc) pulsating white dwarfs with a hydrogen-rich atmosphere (DAV/ZZ Ceti class). It was observed by the {\sl TESS} spacecraft in sectors 42 and 56. The atmosphere of G~29$-$38 is polluted by heavy elements that are expected to sink out of visible layers on short timescales. The photometric {\sl TESS} data set sp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04809v1-abstract-full').style.display = 'inline'; document.getElementById('2309.04809v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.04809v1-abstract-full" style="display: none;"> G\,29$-$38 (TIC~422526868) is one of the brightest ($V=13.1$) and closest ($d = 17.51$\,pc) pulsating white dwarfs with a hydrogen-rich atmosphere (DAV/ZZ Ceti class). It was observed by the {\sl TESS} spacecraft in sectors 42 and 56. The atmosphere of G~29$-$38 is polluted by heavy elements that are expected to sink out of visible layers on short timescales. The photometric {\sl TESS} data set spans $\sim 51$ days in total, and from this, we identified 56 significant pulsation frequencies, that include rotational frequency multiplets. In addition, we identified 30 combination frequencies in each sector. The oscillation frequencies that we found are associated with $g$-mode pulsations, with periods spanning from $\sim$ 260 s to $\sim$ 1400 s. We identified %three distinct rotational frequency triplets with a mean separation $未谓_{\ell=1}$ of 4.67 $渭$Hz and a quintuplet with a mean separation $未谓_{\ell=2}$ of 6.67 $渭$Hz, from which we estimated a rotation period of about $1.35 \pm 0.1$ days. We determined a constant period spacing of 41.20~s for $\ell= 1$ modes and 22.58\,s for $\ell= 2$ modes. We performed period-to-period fit analyses and found an asteroseismological model with $M_{\star}/M_{\odot}=0.632 \pm 0.03$, $T_{\rm eff}=11\, 635\pm 178$ K, and $\log{g}=8.048\pm0.005$ (with a hydrogen envelope mass of $M_{\rm H}\sim 5.6\times 10^{-5}M_{\star}$), in good agreement with the values derived from spectroscopy. We obtained an asteroseismic distance of 17.54 pc, which is in excellent agreement with that provided by {\sl Gaia} (17.51 pc). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04809v1-abstract-full').style.display = 'none'; document.getElementById('2309.04809v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 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, 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/2304.12442">arXiv:2304.12442</a> <span> [<a href="https://arxiv.org/pdf/2304.12442">pdf</a>, <a href="https://arxiv.org/format/2304.12442">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"> Enabling Exoplanet Demographics Studies with Standardized Exoplanet Survey Meta-Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prepared+by+the+ExoPAG+Science+Interest+Group"> Prepared by the ExoPAG Science Interest Group</a>, <a href="/search/astro-ph?searchtype=author&query=Demographics%2C+2+o+E">2 on Exoplanet Demographics</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">Jessie L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Boss%2C+A+P">Alan P. Boss</a>, <a href="/search/astro-ph?searchtype=author&query=Bryson%2C+S">Steve Bryson</a>, <a href="/search/astro-ph?searchtype=author&query=Burt%2C+J+A">Jennifer A. Burt</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandes%2C+R+B">Rachel B. Fernandes</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+T+J">Todd J. Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Jao%2C+W">Wei-Chun Jao</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+S+A">Samson A. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+M+R">Michael R. Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Mulders%2C+G+D">Gijs D. Mulders</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+E+L">Eric L. Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Pascucci%2C+I">Ilaria Pascucci</a>, <a href="/search/astro-ph?searchtype=author&query=Pepper%2C+J">Joshua Pepper</a>, <a href="/search/astro-ph?searchtype=author&query=Plavchan%2C+P">Peter Plavchan</a>, <a href="/search/astro-ph?searchtype=author&query=Ragozzine%2C+D">Darin Ragozzine</a>, <a href="/search/astro-ph?searchtype=author&query=Rosenthal%2C+L+J">Lee J. Rosenthal</a>, <a href="/search/astro-ph?searchtype=author&query=Vrijmoet%2C+E+H">Eliot Halley Vrijmoet</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.12442v1-abstract-short" style="display: inline;"> Goal 1 of the National Academies of Science, Engineering and Mathematics Exoplanet Science Strategy is "to understand the formation and evolution of planetary systems as products of the process of star formation, and characterize and explain the diversity of planetary system architectures, planetary compositions, and planetary environments produced by these processes", with the finding that "Curre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12442v1-abstract-full').style.display = 'inline'; document.getElementById('2304.12442v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.12442v1-abstract-full" style="display: none;"> Goal 1 of the National Academies of Science, Engineering and Mathematics Exoplanet Science Strategy is "to understand the formation and evolution of planetary systems as products of the process of star formation, and characterize and explain the diversity of planetary system architectures, planetary compositions, and planetary environments produced by these processes", with the finding that "Current knowledge of the demographics and characteristics of planets and their systems is substantially incomplete." One significant roadblock to our ongoing efforts to improve our demographics analyses is the lack of comprehensive meta-data accompanying published exoplanet surveys. The Exoplanet Program Analysis Group (ExoPAG) Science Interest Group 2: Exoplanet Demographics has prepared this document to provide guidance to survey architects, authors, referees and funding agencies as to the most valuable such data products for five different exoplanet detection techniques - transit, radial velocity, direct imaging, microlensing and astrometry. We find that making these additional data easily available would greatly enhance the community's ability to perform robust, reproducible demographics analyses, and make progress on achieving the most important goals identified by the exoplanet and wider astronomical community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12442v1-abstract-full').style.display = 'none'; document.getElementById('2304.12442v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, final report after community feedback addressed</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.09189">arXiv:2304.09189</a> <span> [<a href="https://arxiv.org/pdf/2304.09189">pdf</a>, <a href="https://arxiv.org/format/2304.09189">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"> Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+E+A">Emily A. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Silverstein%2C+M+L">Michele L. Silverstein</a>, <a href="/search/astro-ph?searchtype=author&query=Schlieder%2C+J+E">Joshua E. Schlieder</a>, <a href="/search/astro-ph?searchtype=author&query=Cloutier%2C+R">Ryan Cloutier</a>, <a href="/search/astro-ph?searchtype=author&query=Quinn%2C+S+N">Samuel N. Quinn</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez%2C+J+E">Joseph E. Rodriguez</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderburg%2C+A">Andrew Vanderburg</a>, <a href="/search/astro-ph?searchtype=author&query=Hord%2C+B+J">Benjamin J. Hord</a>, <a href="/search/astro-ph?searchtype=author&query=Louie%2C+D+R">Dana R. Louie</a>, <a href="/search/astro-ph?searchtype=author&query=Ostberg%2C+C">Colby Ostberg</a>, <a href="/search/astro-ph?searchtype=author&query=Kane%2C+S+R">Stephen R. Kane</a>, <a href="/search/astro-ph?searchtype=author&query=Hoffman%2C+K">Kelsey Hoffman</a>, <a href="/search/astro-ph?searchtype=author&query=Rowe%2C+J+F">Jason F. Rowe</a>, <a href="/search/astro-ph?searchtype=author&query=Arney%2C+G+N">Giada N. Arney</a>, <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+P">Prabal Saxena</a>, <a href="/search/astro-ph?searchtype=author&query=Richardson%2C+T">Taran Richardson</a>, <a href="/search/astro-ph?searchtype=author&query=Clement%2C+M+S">Matthew S. Clement</a>, <a href="/search/astro-ph?searchtype=author&query=Kartvedt%2C+N+M">Nicholas M. Kartvedt</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+F+C">Fred C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Alfred%2C+M">Marcus Alfred</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+T">Travis Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bieryla%2C+A">Allyson Bieryla</a>, <a href="/search/astro-ph?searchtype=author&query=Bonney%2C+P">Paul Bonney</a> , et al. (33 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.09189v1-abstract-short" style="display: inline;"> We report the detection and validation of two planets orbiting TOI-2095 (TIC 235678745). The host star is a 3700K M1V dwarf with a high proper motion. The star lies at a distance of 42 pc in a sparsely populated portion of the sky and is bright in the infrared (K=9). With data from 24 Sectors of observation during TESS's Cycles 2 and 4, TOI-2095 exhibits two sets of transits associated with super-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.09189v1-abstract-full').style.display = 'inline'; document.getElementById('2304.09189v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.09189v1-abstract-full" style="display: none;"> We report the detection and validation of two planets orbiting TOI-2095 (TIC 235678745). The host star is a 3700K M1V dwarf with a high proper motion. The star lies at a distance of 42 pc in a sparsely populated portion of the sky and is bright in the infrared (K=9). With data from 24 Sectors of observation during TESS's Cycles 2 and 4, TOI-2095 exhibits two sets of transits associated with super-Earth-sized planets. The planets have orbital periods of 17.7 days and 28.2 days and radii of 1.30 and 1.39 Earth radii, respectively. Archival data, preliminary follow-up observations, and vetting analyses support the planetary interpretation of the detected transit signals. The pair of planets have estimated equilibrium temperatures of approximately 400 K, with stellar insolations of 3.23 and 1.73 times that of Earth, placing them in the Venus zone. The planets also lie in a radius regime signaling the transition between rock-dominated and volatile-rich compositions. They are thus prime targets for follow-up mass measurements to better understand the properties of warm, transition radius planets. The relatively long orbital periods of these two planets provide crucial data that can help shed light on the processes that shape the composition of small planets orbiting M dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.09189v1-abstract-full').style.display = 'none'; document.getElementById('2304.09189v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.04869">arXiv:2304.04869</a> <span> [<a href="https://arxiv.org/pdf/2304.04869">pdf</a>, <a href="https://arxiv.org/format/2304.04869">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> </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/10.1088/1538-3873/acd1b5">10.1088/1538-3873/acd1b5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The James Webb Space Telescope Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+J+P">Jonathan P. Gardner</a>, <a href="/search/astro-ph?searchtype=author&query=Mather%2C+J+C">John C. Mather</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">Randy Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abell%2C+J+S">James S. Abell</a>, <a href="/search/astro-ph?searchtype=author&query=Abernathy%2C+M">Mark Abernathy</a>, <a href="/search/astro-ph?searchtype=author&query=Abney%2C+F+E">Faith E. Abney</a>, <a href="/search/astro-ph?searchtype=author&query=Abraham%2C+J+G">John G. Abraham</a>, <a href="/search/astro-ph?searchtype=author&query=Abraham%2C+R">Roberto Abraham</a>, <a href="/search/astro-ph?searchtype=author&query=Abul-Huda%2C+Y+M">Yasin M. Abul-Huda</a>, <a href="/search/astro-ph?searchtype=author&query=Acton%2C+S">Scott Acton</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+K">Cynthia K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E">Evan Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adler%2C+D+S">David S. Adler</a>, <a href="/search/astro-ph?searchtype=author&query=Adriaensen%2C+M">Maarten Adriaensen</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">Jonathan Albert Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+M">Mansoor Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+N+S">Nasif S. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+T">Tanjira Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Albat%2C+R">R眉deger Albat</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+L">Lo茂c Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alberts%2C+S">Stacey Alberts</a>, <a href="/search/astro-ph?searchtype=author&query=Aldridge%2C+D">David Aldridge</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M+M">Mary Marsha Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+S">Shaune S. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Altenburg%2C+M">Martin Altenburg</a> , et al. (983 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.04869v1-abstract-short" style="display: inline;"> Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ James Webb Space Telescope. A generation of astrono… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04869v1-abstract-full').style.display = 'inline'; document.getElementById('2304.04869v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.04869v1-abstract-full" style="display: none;"> Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ James Webb Space Telescope. A generation of astronomers will celebrate their accomplishments for the life of the mission, potentially as long as 20 years, and beyond. This report and the scientific discoveries that follow are extended thank-you notes to the 20,000 team members. The telescope is working perfectly, with much better image quality than expected. In this and accompanying papers, we give a brief history, describe the observatory, outline its objectives and current observing program, and discuss the inventions and people who made it possible. We cite detailed reports on the design and the measured performance on orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04869v1-abstract-full').style.display = 'none'; document.getElementById('2304.04869v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by PASP for the special issue on The James Webb Space Telescope Overview, 29 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.07761">arXiv:2302.07761</a> <span> [<a href="https://arxiv.org/pdf/2302.07761">pdf</a>, <a href="https://arxiv.org/format/2302.07761">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acc2c1">10.3847/2041-8213/acc2c1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The first JWST spectrum of a GRB afterglow: No bright supernova in observations of the brightest GRB of all time, GRB 221009A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Levan%2C+A+J">A. J. Levan</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+G+P">G. P. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+B">B. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Hjorth%2C+J">J. Hjorth</a>, <a href="/search/astro-ph?searchtype=author&query=Zafar%2C+T">T. Zafar</a>, <a href="/search/astro-ph?searchtype=author&query=Postigo%2C+A+d+U">A. de Ugarte Postigo</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+B">B. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">S. E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Izzo%2C+L">L. Izzo</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Avanzo%2C+P">P. D'Avanzo</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez%2C+J+F+A">J. F. Ag眉铆 Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">T. Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+M+G">M. G. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bhirombhakdi%2C+K">K. Bhirombhakdi</a>, <a href="/search/astro-ph?searchtype=author&query=Bremer%2C+M">M. Bremer</a>, <a href="/search/astro-ph?searchtype=author&query=Brivio%2C+R">R. Brivio</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Chrimes%2C+A+A">A. A. Chrimes</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Elia%2C+V">V. D'Elia</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Valle%2C+M">M. Della Valle</a>, <a href="/search/astro-ph?searchtype=author&query=De+Pasquale%2C+M">M. De Pasquale</a>, <a href="/search/astro-ph?searchtype=author&query=Ferro%2C+M">M. Ferro</a>, <a href="/search/astro-ph?searchtype=author&query=Fong%2C+W">W. Fong</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A+S">A. S. Fruchter</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.07761v2-abstract-short" style="display: inline;"> We present JWST and Hubble Space Telescope (HST) observations of the afterglow of GRB 221009A, the brightest gamma-ray burst (GRB) ever observed. This includes the first mid-IR spectra of any GRB, obtained with JWST/NIRSPEC (0.6-5.5 micron) and MIRI (5-12 micron), 12 days after the burst. Assuming that the intrinsic spectral slope is a single power-law, with $F_谓 \propto 谓^{-尾}$, we obtain… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07761v2-abstract-full').style.display = 'inline'; document.getElementById('2302.07761v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.07761v2-abstract-full" style="display: none;"> We present JWST and Hubble Space Telescope (HST) observations of the afterglow of GRB 221009A, the brightest gamma-ray burst (GRB) ever observed. This includes the first mid-IR spectra of any GRB, obtained with JWST/NIRSPEC (0.6-5.5 micron) and MIRI (5-12 micron), 12 days after the burst. Assuming that the intrinsic spectral slope is a single power-law, with $F_谓 \propto 谓^{-尾}$, we obtain $尾\approx 0.35$, modified by substantial dust extinction with $A_V = 4.9$. This suggests extinction above the notional Galactic value, possibly due to patchy extinction within the Milky Way or dust in the GRB host galaxy. It further implies that the X-ray and optical/IR regimes are not on the same segment of the synchrotron spectrum of the afterglow. If the cooling break lies between the X-ray and optical/IR, then the temporal decay rates would only match a post jet-break model, with electron index $p<2$, and with the jet expanding into a uniform ISM medium. The shape of the JWST spectrum is near-identical in the optical/nIR to X-shooter spectroscopy obtained at 0.5 days and to later time observations with HST. The lack of spectral evolution suggests that any accompanying supernova (SN) is either substantially fainter or bluer than SN 1998bw, the proto-type GRB-SN. Our HST observations also reveal a disc-like host galaxy, viewed close to edge-on, that further complicates the isolation of any supernova component. The host galaxy appears rather typical amongst long-GRB hosts and suggests that the extreme properties of GRB 221009A are not directly tied to its galaxy-scale environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07761v2-abstract-full').style.display = 'none'; document.getElementById('2302.07761v2-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication to the Astrophysical Journal Letters for the GRB 221009A Special Issue. The results of this paper are under press embargo until March 28, 18 UT. 19 pages, 8 figures, 2 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/2301.10866">arXiv:2301.10866</a> <span> [<a href="https://arxiv.org/pdf/2301.10866">pdf</a>, <a href="https://arxiv.org/format/2301.10866">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> The transmission spectrum of the potentially rocky planet L 98-59 c </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Sheppard%2C+K+B">Kyle B. Sheppard</a>, <a href="/search/astro-ph?searchtype=author&query=Latouf%2C+N">Natasha Latouf</a>, <a href="/search/astro-ph?searchtype=author&query=Mandell%2C+A+M">Avi M. Mandell</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+E+A">Emily A. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzi%2C+G">Giuliano Liuzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+G+L">Geronimo L. Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Arney%2C+G">Giada Arney</a>, <a href="/search/astro-ph?searchtype=author&query=Brande%2C+J">Jonathan Brande</a>, <a href="/search/astro-ph?searchtype=author&query=Col%C3%B3n%2C+K+D">Knicole D. Col贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Covone%2C+G">Giovanni Covone</a>, <a href="/search/astro-ph?searchtype=author&query=Crossfield%2C+I+J+M">Ian J. M. Crossfield</a>, <a href="/search/astro-ph?searchtype=author&query=Damiano%2C+M">Mario Damiano</a>, <a href="/search/astro-ph?searchtype=author&query=Domagal-Goldman%2C+S+D">Shawn D. Domagal-Goldman</a>, <a href="/search/astro-ph?searchtype=author&query=Fauchez%2C+T+J">Thomas J. Fauchez</a>, <a href="/search/astro-ph?searchtype=author&query=Fiscale%2C+S">Stefano Fiscale</a>, <a href="/search/astro-ph?searchtype=author&query=Gallo%2C+F">Francesco Gallo</a>, <a href="/search/astro-ph?searchtype=author&query=Hedges%2C+C+L">Christina L. Hedges</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+R">Renyu Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Kite%2C+E+S">Edwin S. Kite</a>, <a href="/search/astro-ph?searchtype=author&query=Koll%2C+D">Daniel Koll</a>, <a href="/search/astro-ph?searchtype=author&query=Kopparapu%2C+R+K">Ravi K. Kopparapu</a>, <a href="/search/astro-ph?searchtype=author&query=Kostov%2C+V+B">Veselin B. Kostov</a>, <a href="/search/astro-ph?searchtype=author&query=Kreidberg%2C+L">Laura Kreidberg</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="2301.10866v1-abstract-short" style="display: inline;"> We present observations of the 1.35+/-0.07 Earth-radius planet L 98-59 c using Wide Field Camera~3 on the Hubble Space Telescope. L 98-59 is a nearby (10.6 pc), bright (H=7.4 mag), M3V star that harbors three small, transiting planets. As one of the closest known transiting multi-planet systems, L 98-59 offers one of the best opportunities to probe and compare the atmospheres of rocky planets that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.10866v1-abstract-full').style.display = 'inline'; document.getElementById('2301.10866v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.10866v1-abstract-full" style="display: none;"> We present observations of the 1.35+/-0.07 Earth-radius planet L 98-59 c using Wide Field Camera~3 on the Hubble Space Telescope. L 98-59 is a nearby (10.6 pc), bright (H=7.4 mag), M3V star that harbors three small, transiting planets. As one of the closest known transiting multi-planet systems, L 98-59 offers one of the best opportunities to probe and compare the atmospheres of rocky planets that formed in the same stellar environment. We measured the transmission spectrum of L 98-59 c during a single transit, with the extracted spectrum showing marginal evidence for wavelength-dependent transit depth variations which would indicate the presence of an atmosphere. Forward modeling was used to constrain possible atmospheric compositions of the planet based on the shape of the transmission spectrum. Although L 98-59 is a fairly quiet star, we have seen evidence for stellar activity, and therefore we cannot rule out a scenario where the source of the signal originates with inhomogeneities on the host-star surface. While intriguing, our results are inconclusive and additional data is needed to verify any atmospheric signal. Fortunately, additional data will soon be collected from both HST and JWST. Should this result be confirmed with additional data, L 98-59 c would be the first planet smaller than 2 Earth-radii with a detected atmosphere, and among the first small planets with a known atmosphere to be studied in detail by the JWST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.10866v1-abstract-full').style.display = 'none'; document.getElementById('2301.10866v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.01900">arXiv:2301.01900</a> <span> [<a href="https://arxiv.org/pdf/2301.01900">pdf</a>, <a href="https://arxiv.org/format/2301.01900">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"> False Alarms Revealed in a Planet Search of TESS Light Curves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kunimoto%2C+M">Michelle Kunimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Bryson%2C+S">Steve Bryson</a>, <a href="/search/astro-ph?searchtype=author&query=Daylan%2C+T">Tansu Daylan</a>, <a href="/search/astro-ph?searchtype=author&query=Lissauer%2C+J+J">Jack J. Lissauer</a>, <a href="/search/astro-ph?searchtype=author&query=Matesic%2C+M+R">Michael R. Matesic</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Rowe%2C+J+F">Jason F. Rowe</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="2301.01900v1-abstract-short" style="display: inline;"> We examined the period distribution of transit-like signatures uncovered in a Box-Least Squares transit search of TESS light curves, and show significant pileups at periods related to instrumental and astrophysical noise sources. Signatures uncovered in a search of inverted light curves feature similar structures in the period distribution. Automated vetting methods will need to remove these exces… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.01900v1-abstract-full').style.display = 'inline'; document.getElementById('2301.01900v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.01900v1-abstract-full" style="display: none;"> We examined the period distribution of transit-like signatures uncovered in a Box-Least Squares transit search of TESS light curves, and show significant pileups at periods related to instrumental and astrophysical noise sources. Signatures uncovered in a search of inverted light curves feature similar structures in the period distribution. Automated vetting methods will need to remove these excess detections, and light curve inversion appears to be a suitable method for simulating false alarms and designing new vetting metrics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.01900v1-abstract-full').style.display = 'none'; document.getElementById('2301.01900v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 1 figure, to be published in RNAAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.10008">arXiv:2210.10008</a> <span> [<a href="https://arxiv.org/pdf/2210.10008">pdf</a>, <a href="https://arxiv.org/format/2210.10008">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac9472">10.3847/1538-3881/ac9472 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A transmission spectrum of the sub-Earth planet L98-59~b in 1.1-1.7 $渭$m </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Damiano%2C+M">Mario Damiano</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+R">Renyu Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Zieba%2C+S">Sebastian Zieba</a>, <a href="/search/astro-ph?searchtype=author&query=Kreidberg%2C+L">Laura Kreidberg</a>, <a href="/search/astro-ph?searchtype=author&query=Brande%2C+J">Jonathan Brande</a>, <a href="/search/astro-ph?searchtype=author&query=Colon%2C+K+D">Knicole D. Colon</a>, <a href="/search/astro-ph?searchtype=author&query=Covone%2C+G">Giovanni Covone</a>, <a href="/search/astro-ph?searchtype=author&query=Crossfield%2C+I">Ian Crossfield</a>, <a href="/search/astro-ph?searchtype=author&query=Domagal-Goldman%2C+S+D">Shawn D. Domagal-Goldman</a>, <a href="/search/astro-ph?searchtype=author&query=Fauchez%2C+T+J">Thomas J. Fauchez</a>, <a href="/search/astro-ph?searchtype=author&query=Fiscale%2C+S">Stefano Fiscale</a>, <a href="/search/astro-ph?searchtype=author&query=Gallo%2C+F">Francesco Gallo</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+E">Emily Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Hedges%2C+C+L">Christina L. Hedges</a>, <a href="/search/astro-ph?searchtype=author&query=Kite%2C+E+S">Edwin S. Kite</a>, <a href="/search/astro-ph?searchtype=author&query=Kopparapu%2C+R+K">Ravi K. Kopparapu</a>, <a href="/search/astro-ph?searchtype=author&query=Kostov%2C+V+B">Veselin B. Kostov</a>, <a href="/search/astro-ph?searchtype=author&query=Morley%2C+C">Caroline Morley</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Pidhorodetska%2C+D">Daria Pidhorodetska</a>, <a href="/search/astro-ph?searchtype=author&query=Schlieder%2C+J+E">Joshua E. Schlieder</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</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="2210.10008v1-abstract-short" style="display: inline;"> With the increasing number of planets discovered by TESS, the atmospheric characterization of small exoplanets is accelerating. L98-59 is a M-dwarf hosting a multi-planet system, and so far, four small planets have been confirmed. The innermost planet b is $\sim15\%$ smaller and $\sim60\%$ lighter than Earth, and should thus have a predominantly rocky composition. The Hubble Space Telescope observ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10008v1-abstract-full').style.display = 'inline'; document.getElementById('2210.10008v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.10008v1-abstract-full" style="display: none;"> With the increasing number of planets discovered by TESS, the atmospheric characterization of small exoplanets is accelerating. L98-59 is a M-dwarf hosting a multi-planet system, and so far, four small planets have been confirmed. The innermost planet b is $\sim15\%$ smaller and $\sim60\%$ lighter than Earth, and should thus have a predominantly rocky composition. The Hubble Space Telescope observed five primary transits of L98-59b in $1.1-1.7\ 渭$m, and here we report the data analysis and the resulting transmission spectrum of the planet. We measure the transit depths for each of the five transits and, by combination, we obtain a transmission spectrum with an overall precision of $\sim20$ ppm in for each of the 18 spectrophotometric channels. With this level of precision, the transmission spectrum does not show significant modulation, and is thus consistent with a planet without any atmosphere or a planet having an atmosphere and high-altitude clouds or haze. The scenarios involving an aerosol-free, H$_2$-dominated atmosphere with H$_2$O or CH$_4$ are inconsistent with the data. The transmission spectrum also disfavors, but does not rules out, an H$_2$O-dominated atmosphere without clouds. A spectral retrieval process suggests that an H$_2$-dominated atmosphere with HCN and clouds or haze may be the preferred solution, but this indication is non-conclusive. Future James Webb Space Telescope observations may find out the nature of the planet among the remaining viable scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10008v1-abstract-full').style.display = 'none'; document.getElementById('2210.10008v1-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 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">17 pages, 5 figures, 7 tables, accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.13067">arXiv:2207.13067</a> <span> [<a href="https://arxiv.org/pdf/2207.13067">pdf</a>, <a href="https://arxiv.org/format/2207.13067">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> </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/10.3847/2041-8213/ac8a4e">10.3847/2041-8213/ac8a4e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The JWST Early Release Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pontoppidan%2C+K">Klaus Pontoppidan</a>, <a href="/search/astro-ph?searchtype=author&query=Barrientes%2C+J">Jaclyn Barrientes</a>, <a href="/search/astro-ph?searchtype=author&query=Blome%2C+C">Claire Blome</a>, <a href="/search/astro-ph?searchtype=author&query=Braun%2C+H">Hannah Braun</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M">Matthew Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Carruthers%2C+M">Margaret Carruthers</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=DePasquale%2C+J">Joseph DePasquale</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">Nestor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Marin%2C+M+G">Macarena Garcia Marin</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K+D">Karl D. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+A">Alaina Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Hustak%2C+L">Leah Hustak</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+A">Andi James</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=LaMassa%2C+S">Stephanie LaMassa</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+D">David Law</a>, <a href="/search/astro-ph?searchtype=author&query=Lockwood%2C+A">Alexandra Lockwood</a>, <a href="/search/astro-ph?searchtype=author&query=Moro-Martin%2C+A">Amaya Moro-Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Pagan%2C+A">Alyssa Pagan</a>, <a href="/search/astro-ph?searchtype=author&query=Player%2C+D">Dani Player</a>, <a href="/search/astro-ph?searchtype=author&query=Proffitt%2C+C">Charles Proffitt</a>, <a href="/search/astro-ph?searchtype=author&query=Pulliam%2C+C">Christine Pulliam</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+L">Leah Ramsay</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="2207.13067v2-abstract-short" style="display: inline;"> The James Webb Space Telescope (JWST) Early Release Observations (EROs) is a set of public outreach products created to mark the end of commissioning and the beginning of science operations for JWST. Colloquially known as the "Webb First Images and Spectra", these products were intended to demonstrate to the worldwide public that JWST is ready for science, and is capable of producing spectacular r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13067v2-abstract-full').style.display = 'inline'; document.getElementById('2207.13067v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.13067v2-abstract-full" style="display: none;"> The James Webb Space Telescope (JWST) Early Release Observations (EROs) is a set of public outreach products created to mark the end of commissioning and the beginning of science operations for JWST. Colloquially known as the "Webb First Images and Spectra", these products were intended to demonstrate to the worldwide public that JWST is ready for science, and is capable of producing spectacular results. The package was released on July 12, 2022, and included images and spectra of the galaxy cluster SMACS~J0723.3-7327 and distant lensed galaxies, the interacting galaxy group Stephan's Quintet, NGC 3324 in the Carina star-forming complex, the Southern Ring planetary nebula NGC 3132, and the transiting hot Jupiter WASP 96b. This paper describes the ERO technical design, observations, and scientific processing of data underlying the colorful outreach products. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13067v2-abstract-full').style.display = 'none'; document.getElementById('2207.13067v2-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">15 pages, accepted by ApJ Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL, 2022, 936, L14 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.06500">arXiv:2204.06500</a> <span> [<a href="https://arxiv.org/pdf/2204.06500">pdf</a>, <a href="https://arxiv.org/format/2204.06500">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac66dc">10.3847/1538-3881/ac66dc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The James Webb Space Telescope Absolute Flux Calibration. I. Program Design and Calibrator Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K+D">Karl D. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Bohlin%2C+R">Ralph Bohlin</a>, <a href="/search/astro-ph?searchtype=author&query=Sloan%2C+G+C">G. C. Sloan</a>, <a href="/search/astro-ph?searchtype=author&query=Rieke%2C+G">George Rieke</a>, <a href="/search/astro-ph?searchtype=author&query=Volk%2C+K">Kevin Volk</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M">Martha Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Muzerolle%2C+J">James Muzerolle</a>, <a href="/search/astro-ph?searchtype=author&query=Schlawin%2C+E">Everett Schlawin</a>, <a href="/search/astro-ph?searchtype=author&query=Deustua%2C+S+E">Susana E. Deustua</a>, <a href="/search/astro-ph?searchtype=author&query=Hines%2C+D+C">Dean C. Hines</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+K+E">Kathleen E. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+K+Y+L">Kate Y. L. Su</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="2204.06500v1-abstract-short" style="display: inline;"> It is critical for James Webb Space Telescope (JWST) science that instrumental units are converted to physical units. We detail the design of the JWST absolute flux calibration program that has the core goal of ensuring a robust flux calibration internal to and between all the science instruments for both point and extended source science. This program will observe a sample of calibration stars th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06500v1-abstract-full').style.display = 'inline'; document.getElementById('2204.06500v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.06500v1-abstract-full" style="display: none;"> It is critical for James Webb Space Telescope (JWST) science that instrumental units are converted to physical units. We detail the design of the JWST absolute flux calibration program that has the core goal of ensuring a robust flux calibration internal to and between all the science instruments for both point and extended source science. This program will observe a sample of calibration stars that have been extensively vetted based mainly on Hubble Space Telescope, Spitzer Space Telescope, and Transiting Exoplanet Survey Satellite observations. The program uses multiple stars of three different, well understood types (hot stars, A dwarfs, and solar analogs) to allow for the statistical (within a type) and systematic (between types) uncertainties to be quantified. The program explicitly includes observations to calibrate every instrument mode, further vet the set of calibration stars, measure the instrumental repeatability, measure the relative calibration between subarrays and full frame, and check the relative calibration between faint and bright stars. For photometry, we have set up our calibration to directly support both the convention based on the band average flux density and the convention based on the flux density at a fixed wavelength. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06500v1-abstract-full').style.display = 'none'; document.getElementById('2204.06500v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 3 figures, AJ, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.15826">arXiv:2203.15826</a> <span> [<a href="https://arxiv.org/pdf/2203.15826">pdf</a>, <a href="https://arxiv.org/format/2203.15826">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac652">10.1093/mnras/stac652 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TESS Triple-9 Catalog: 999 uniformly vetted candidate exoplanets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cacciapuoti%2C+L">Luca Cacciapuoti</a>, <a href="/search/astro-ph?searchtype=author&query=Kostov%2C+V+B">Veselin B. Kostov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuchner%2C+M">Marc Kuchner</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Col%C3%B3n%2C+K+D">Knicole D. Col贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Brande%2C+J">Jonathan Brande</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Chance%2C+Q">Quadry Chance</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">Jessie L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+J+P">John P. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Fraia%2C+M+Z">Marco Z. Di Fraia</a>, <a href="/search/astro-ph?searchtype=author&query=Luca%2C+H+A+D">Hugo A. Durantini Luca</a>, <a href="/search/astro-ph?searchtype=author&query=Ienco%2C+R+M">Riccardo M. Ienco</a>, <a href="/search/astro-ph?searchtype=author&query=Gallo%2C+F">Francesco Gallo</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lima%2C+L+T">Lucas T. de Lima</a>, <a href="/search/astro-ph?searchtype=author&query=Hyogo%2C+M">Michiharu Hyogo</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">Marc Andr茅s-Carcasona</a>, <a href="/search/astro-ph?searchtype=author&query=Fornear%2C+A+U">Aline U. Fornear</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lambilly%2C+J+S">Julien S. de Lambilly</a>, <a href="/search/astro-ph?searchtype=author&query=Salik%2C+R">Ryan Salik</a>, <a href="/search/astro-ph?searchtype=author&query=Yablonsky%2C+J+M">John M. Yablonsky</a>, <a href="/search/astro-ph?searchtype=author&query=Wallace%2C+S">Shaun Wallace</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+S">Sovan Acharya</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="2203.15826v1-abstract-short" style="display: inline;"> The Transiting Exoplanet Survey Satellite (TESS) has detected thousands of exoplanet candidates since 2018, most of which have yet to be confirmed. A key step in the confirmation process of these candidates is ruling out false positives through vetting. Vetting also eases the burden on follow-up observations, provides input for demographics studies, and facilitates training machine learning algori… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15826v1-abstract-full').style.display = 'inline'; document.getElementById('2203.15826v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.15826v1-abstract-full" style="display: none;"> The Transiting Exoplanet Survey Satellite (TESS) has detected thousands of exoplanet candidates since 2018, most of which have yet to be confirmed. A key step in the confirmation process of these candidates is ruling out false positives through vetting. Vetting also eases the burden on follow-up observations, provides input for demographics studies, and facilitates training machine learning algorithms. Here we present the TESS Triple-9 (TT9) catalog -- a uniformly-vetted catalog containing dispositions for 999 exoplanet candidates listed on ExoFOP-TESS, known as TESS Objects of Interest (TOIs). The TT9 was produced using the Discovery And Vetting of Exoplanets pipeline, DAVE, and utilizing the power of citizen science as part of the Planet Patrol project. More than 70% of the TOIs listed in the TT9 pass our diagnostic tests, and are thus marked as true planetary candidates. We flagged 144 candidates as false positives, and identified 146 as potential false positives. At the time of writing, the TT9 catalog contains ~20% of the entire ExoFOP-TESS TOIs list, demonstrates the synergy between automated tools and citizen science, and represents the first stage of our efforts to vet all TOIs. The DAVE generated results are publicly available on ExoFOP-TESS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15826v1-abstract-full').style.display = 'none'; document.getElementById('2203.15826v1-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">15 pages, 11 figures. Accepted on MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, Volume 513, Issue 1, June 2022, Pages 102 116 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.03670">arXiv:2201.03670</a> <span> [<a href="https://arxiv.org/pdf/2201.03670">pdf</a>, <a href="https://arxiv.org/format/2201.03670">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/10.3847/1538-3881/ac4bce">10.3847/1538-3881/ac4bce <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for TESS Photometric Variability of Possible JWST Spectrophotometric Standard Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Sloan%2C+G+C">G. C. Sloan</a>, <a href="/search/astro-ph?searchtype=author&query=Hermes%2C+J+J">J. J. Hermes</a>, <a href="/search/astro-ph?searchtype=author&query=Hambleton%2C+K">Kelly Hambleton</a>, <a href="/search/astro-ph?searchtype=author&query=Kunz%2C+M">Michael Kunz</a>, <a href="/search/astro-ph?searchtype=author&query=Bohlin%2C+R">Ralph Bohlin</a>, <a href="/search/astro-ph?searchtype=author&query=Fleming%2C+S+W">Scott W. Fleming</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K+D">Karl D. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Kaleida%2C+C">Catherine Kaleida</a>, <a href="/search/astro-ph?searchtype=author&query=Mohamed%2C+K">Khalid Mohamed</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="2201.03670v1-abstract-short" style="display: inline;"> We use data from the Transiting Exoplanet Survey Satellite (TESS) to search for, and set limits on, optical to near-infrared photometric variability of the well-vetted, candidate James Webb Space Telescope (JWST) spectrophotometric standards. Our search of 37 of these candidate standards has revealed measurable periodic variability in 15 stars. The majority of those show variability that is less t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03670v1-abstract-full').style.display = 'inline'; document.getElementById('2201.03670v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.03670v1-abstract-full" style="display: none;"> We use data from the Transiting Exoplanet Survey Satellite (TESS) to search for, and set limits on, optical to near-infrared photometric variability of the well-vetted, candidate James Webb Space Telescope (JWST) spectrophotometric standards. Our search of 37 of these candidate standards has revealed measurable periodic variability in 15 stars. The majority of those show variability that is less than half a percent; however, four stars are observed to vary photometrically, from minimum to maximum flux, by more than 1% (the G dwarf HD 38949 and three fainter A dwarfs). Variability of this size would likely impact the error budget in the spectrophotometric calibration of the science instruments aboard JWST. For the 22 candidate standards with no detected variability, we report upper limits on the observed changes in flux. Despite some systematic noise, all stars brighter than 12 magnitude in the TESS band show a 3 sigma upper limit on the total change in brightness of less than half a percent on time scales between an hour and multiple weeks, empirically establishing their suitability as spectrophotometric standards. We further discuss the value and limits of high-cadence, high-precision photometric monitoring with TESS as a tool to vet the suitability of stars to act as spectrophotometric standards. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03670v1-abstract-full').style.display = 'none'; document.getElementById('2201.03670v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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, 5 figures, 3 tables, accepted for publication by AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.14608">arXiv:2109.14608</a> <span> [<a href="https://arxiv.org/pdf/2109.14608">pdf</a>, <a href="https://arxiv.org/format/2109.14608">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac2824">10.3847/1538-3881/ac2824 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar surface inhomogeneities as a potential source of the atmospheric signal detected in the K2-18 b transmission spectrum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Kostov%2C+V+B">Veselin B. Kostov</a>, <a href="/search/astro-ph?searchtype=author&query=Col%C3%B3n%2C+K+D">Knicole D. Col贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Schlieder%2C+J+E">Joshua E. Schlieder</a>, <a href="/search/astro-ph?searchtype=author&query=Louie%2C+D+R">Dana R. Louie</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+E+A">Emily A. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</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="2109.14608v1-abstract-short" style="display: inline;"> Transmission spectroscopy of transiting exoplanets is a proven technique that can yield information on the composition and structure of a planet's atmosphere. However, transmission spectra may be compromised by inhomogeneities in the stellar photosphere. The sub-Neptune-sized habitable zone planet K2-18 b has water absorption detected in its atmosphere using data from the Hubble Space Telescope (H… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.14608v1-abstract-full').style.display = 'inline'; document.getElementById('2109.14608v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.14608v1-abstract-full" style="display: none;"> Transmission spectroscopy of transiting exoplanets is a proven technique that can yield information on the composition and structure of a planet's atmosphere. However, transmission spectra may be compromised by inhomogeneities in the stellar photosphere. The sub-Neptune-sized habitable zone planet K2-18 b has water absorption detected in its atmosphere using data from the Hubble Space Telescope (HST). Herein, we examine whether the reported planetary atmospheric signal seen from HST transmission spectroscopy of K2-18 b could instead be induced by time-varying star spots. We built a time-variable spectral model of K2-18 that is designed to match the variability amplitude seen in K2 photometric data, and used this model to simulate 1000 HST data-sets that follow the K2-18 b observation strategy. More than 1% of these provide a better fit to the data than the best-fitting exoplanet atmosphere model. After resampling our simulations to generate synthetic HST observations, we find that 40% of random draws would produce an atmospheric detection at a level at least as significant as that seen in the actual HST data of K2-18 b. This work illustrates that the inferred detection of an atmosphere on K2-18 b may alternatively be explained by stellar spectral contamination due to the inhomogeneous photosphere of K2-18. We do not rule out a detection of water in the planet's atmosphere, but provide a plausible alternative that should be considered, and conclude that more observations are needed to fully rule out stellar contamination. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.14608v1-abstract-full').style.display = 'none'; document.getElementById('2109.14608v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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 AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.02665">arXiv:2109.02665</a> <span> [<a href="https://arxiv.org/pdf/2109.02665">pdf</a>, <a href="https://arxiv.org/format/2109.02665">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> </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/10.1088/1538-3873/ac1d3f">10.1088/1538-3873/ac1d3f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TESS Mission Target Selection Procedure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fausnaugh%2C+M">Michael Fausnaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Morgan%2C+E">Ed Morgan</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderspek%2C+R">Roland Vanderspek</a>, <a href="/search/astro-ph?searchtype=author&query=Pepper%2C+J">Joshua Pepper</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+C+J">Christopher J. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Levine%2C+A+M">Alan M. Levine</a>, <a href="/search/astro-ph?searchtype=author&query=Rudat%2C+A">Alexander Rudat</a>, <a href="/search/astro-ph?searchtype=author&query=Villase%C3%B1or%2C+J+N+S">Jesus Noel S. Villase帽or</a>, <a href="/search/astro-ph?searchtype=author&query=Vezie%2C+M">Michael Vezie</a>, <a href="/search/astro-ph?searchtype=author&query=Goeke%2C+R+F">Robert F. Goeke</a>, <a href="/search/astro-ph?searchtype=author&query=Ricker%2C+G+R">George R. Ricker</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+D+W">David W. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=Seager%2C+S">S. Seager</a>, <a href="/search/astro-ph?searchtype=author&query=Winn%2C+J+N">Joshua N. Winn</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J+M">Jon M. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Bakos%2C+G+A">G. A. Bakos</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Berta-thompson%2C+Z+K">Zachory K. Berta-thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Bouma%2C+L+G">Luke G. Bouma</a>, <a href="/search/astro-ph?searchtype=author&query=Boyd%2C+P+T">Patricia T. Boyd</a>, <a href="/search/astro-ph?searchtype=author&query=Brasseur%2C+C+E">C. E. Brasseur</a>, <a href="/search/astro-ph?searchtype=author&query=Burt%2C+J">Jennifer Burt</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+D+A">Douglas A. Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonneau%2C+D">David Charbonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-dalsgaard%2C+J">J. Christensen-dalsgaard</a> , et al. (39 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="2109.02665v1-abstract-short" style="display: inline;"> We describe the target selection procedure by which stars are selected for 2-minute and 20-second observations by TESS. We first list the technical requirements of the TESS instrument and ground systems processing that limit the total number of target slots. We then describe algorithms used by the TESS Payload Operation Center (POC) to merge candidate targets requested by the various TESS mission… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.02665v1-abstract-full').style.display = 'inline'; document.getElementById('2109.02665v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.02665v1-abstract-full" style="display: none;"> We describe the target selection procedure by which stars are selected for 2-minute and 20-second observations by TESS. We first list the technical requirements of the TESS instrument and ground systems processing that limit the total number of target slots. We then describe algorithms used by the TESS Payload Operation Center (POC) to merge candidate targets requested by the various TESS mission elements (the Target Selection Working Group, TESS Asteroseismic Science Consortium, and Guest Investigator office). Lastly, we summarize the properties of the observed TESS targets over the two-year primary TESS mission. We find that the POC target selection algorithm results in 2.1 to 3.4 times as many observed targets as target slots allocated for each mission element. We also find that the sky distribution of observed targets is different from the sky distributions of candidate targets due to technical constraints that require a relatively even distribution of targets across the TESS fields of view. We caution researchers exploring statistical analyses of TESS planet-host stars that the population of observed targets cannot be characterized by any simple set of criteria applied to the properties of the input Candidate Target Lists. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.02665v1-abstract-full').style.display = 'none'; document.getElementById('2109.02665v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">15 pages, 6 figures, accepted for publication in PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.06438">arXiv:2108.06438</a> <span> [<a href="https://arxiv.org/pdf/2108.06438">pdf</a>, <a href="https://arxiv.org/format/2108.06438">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"> The Pandora SmallSat: Multiwavelength Characterization of Exoplanets and their Host Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Col%C3%B3n%2C+K+D">Knicole D. Col贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Mosby%2C+G">Gregory Mosby</a>, <a href="/search/astro-ph?searchtype=author&query=Schlieder%2C+J+E">Joshua E. Schlieder</a>, <a href="/search/astro-ph?searchtype=author&query=Supsinskas%2C+P">Pete Supsinskas</a>, <a href="/search/astro-ph?searchtype=author&query=Karburn%2C+J">Jordan Karburn</a>, <a href="/search/astro-ph?searchtype=author&query=Dotson%2C+J+L">Jessie L. Dotson</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+T+P">Thomas P. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Hedges%2C+C">Christina Hedges</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">D谩niel Apai</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">Jessie L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">N茅stor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+E+A">Emily A. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Hoffman%2C+K">Kelsey Hoffman</a>, <a href="/search/astro-ph?searchtype=author&query=Kostov%2C+V+B">Veselin B. Kostov</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+N+K">Nikole K. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Foote%2C+T+O">Trevor O. Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+J">James Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Youngblood%2C+A">Allison Youngblood</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+B+M">Brett M. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Newton%2C+E+R">Elisabeth R. Newton</a>, <a href="/search/astro-ph?searchtype=author&query=Pepper%2C+J">Joshua Pepper</a>, <a href="/search/astro-ph?searchtype=author&query=Rackham%2C+B+V">Benjamin V. Rackham</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.06438v2-abstract-short" style="display: inline;"> Pandora is a SmallSat mission designed to study the atmospheres of exoplanets, and was selected as part of NASA's Astrophysics Pioneers Program. Transmission spectroscopy of transiting exoplanets provides our best opportunity to identify the makeup of planetary atmospheres in the coming decade. Stellar brightness variations due to star spots, however, can impact these measurements and contaminate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.06438v2-abstract-full').style.display = 'inline'; document.getElementById('2108.06438v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.06438v2-abstract-full" style="display: none;"> Pandora is a SmallSat mission designed to study the atmospheres of exoplanets, and was selected as part of NASA's Astrophysics Pioneers Program. Transmission spectroscopy of transiting exoplanets provides our best opportunity to identify the makeup of planetary atmospheres in the coming decade. Stellar brightness variations due to star spots, however, can impact these measurements and contaminate the observed spectra. Pandora's goal is to disentangle star and planet signals in transmission spectra to reliably determine exoplanet atmosphere compositions. Pandora will collect long-duration photometric observations with a visible-light channel and simultaneous spectra with a near-IR channel. The broad-wavelength coverage will provide constraints on the spot and faculae covering fractions of low-mass exoplanet host stars and the impact of these active regions on exoplanetary transmission spectra. Pandora will subsequently identify exoplanets with hydrogen- or water-dominated atmospheres, and robustly determine which planets are covered by clouds and hazes. Pandora will observe at least 20 exoplanets with sizes ranging from Earth-size to Jupiter-size and host stars spanning mid-K to late-M spectral types. The project is made possible by leveraging investments in other projects, including an all-aluminum 0.45-meter Cassegrain telescope design, and a NIR sensor chip assembly from the James Webb Space Telescope. The mission will last five years from initial formulation to closeout, with one-year of science operations. Launch is planned for the mid-2020s as a secondary payload in Sun-synchronous low-Earth orbit. By design, Pandora has a diverse team, with over half of the mission leadership roles filled by early career scientists and engineers, demonstrating the high value of SmallSats for developing the next generation of space mission leaders. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.06438v2-abstract-full').style.display = 'none'; document.getElementById('2108.06438v2-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Proceedings of the Small Satellite Conference, Science/Mission Payloads, SSC21-VI-02 (2021)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.01944">arXiv:2105.01944</a> <span> [<a href="https://arxiv.org/pdf/2105.01944">pdf</a>, <a href="https://arxiv.org/format/2105.01944">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/stab1427">10.1093/mnras/stab1427 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TOI-220 $b$: a warm sub-Neptune discovered by TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/astro-ph?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</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=Deleuil%2C+M">M. Deleuil</a>, <a href="/search/astro-ph?searchtype=author&query=Acu%C3%B1a%2C+L">L. Acu帽a</a>, <a href="/search/astro-ph?searchtype=author&query=de+Medeiros%2C+J+R">J. R. de Medeiros</a>, <a href="/search/astro-ph?searchtype=author&query=Goffo%2C+E">E. Goffo</a>, <a href="/search/astro-ph?searchtype=author&query=Lillo-Box%2C+J">J. Lillo-Box</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=Lopez%2C+T+A">T. A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Santerne%2C+A">A. Santerne</a>, <a href="/search/astro-ph?searchtype=author&query=Sousa%2C+S">S. Sousa</a>, <a href="/search/astro-ph?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+K+A">K. A. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Serrano%2C+L+M">L. M. Serrano</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=Howell%2C+S+B">S. B. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Deeg%2C+H">H. Deeg</a>, <a href="/search/astro-ph?searchtype=author&query=Aguichine%2C+A">A. Aguichine</a>, <a href="/search/astro-ph?searchtype=author&query=Barrag%C3%A1n%2C+O">O. Barrag谩n</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=Martins%2C+B+L+C">B. L. Canto Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+K+I">K. I. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+B+F">B. F. Cooke</a> , et al. (55 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="2105.01944v1-abstract-short" style="display: inline;"> In this paper we report the discovery of TOI-220 $b$, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements we estimate a planetary mass of 13.8 $\pm$ 1.0 M$_{Earth}$ and radius of 3.0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.01944v1-abstract-full').style.display = 'inline'; document.getElementById('2105.01944v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.01944v1-abstract-full" style="display: none;"> In this paper we report the discovery of TOI-220 $b$, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements we estimate a planetary mass of 13.8 $\pm$ 1.0 M$_{Earth}$ and radius of 3.03 $\pm$ 0.15 R$_{Earth}$, implying a bulk density of 2.73 $\pm$ 0.47 $\textrm{g cm}^{-3}$. TOI-220 $b$ orbits a relative bright (V=10.4) and old (10.1$\pm$1.4 Gyr) K dwarf star with a period of $\sim$10.69 d. Thus, TOI-220 $b$ is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220 $b$ internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.01944v1-abstract-full').style.display = 'none'; document.getElementById('2105.01944v1-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">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/2103.12538">arXiv:2103.12538</a> <span> [<a href="https://arxiv.org/pdf/2103.12538">pdf</a>, <a href="https://arxiv.org/format/2103.12538">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/abefe1">10.3847/1538-4365/abefe1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TESS Objects of Interest Catalog from the TESS Prime Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guerrero%2C+N+M">Natalia M. Guerrero</a>, <a href="/search/astro-ph?searchtype=author&query=Seager%2C+S">S. Seager</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+C+X">Chelsea X. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderburg%2C+A">Andrew Vanderburg</a>, <a href="/search/astro-ph?searchtype=author&query=Soto%2C+A+G">Aylin Garcia Soto</a>, <a href="/search/astro-ph?searchtype=author&query=Mireles%2C+I">Ismael Mireles</a>, <a href="/search/astro-ph?searchtype=author&query=Hesse%2C+K">Katharine Hesse</a>, <a href="/search/astro-ph?searchtype=author&query=Fong%2C+W">William Fong</a>, <a href="/search/astro-ph?searchtype=author&query=Glidden%2C+A">Ana Glidden</a>, <a href="/search/astro-ph?searchtype=author&query=Shporer%2C+A">Avi Shporer</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+D+W">David W. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+K+A">Karen A. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Quinn%2C+S+N">Samuel N. Quinn</a>, <a href="/search/astro-ph?searchtype=author&query=Burt%2C+J">Jennifer Burt</a>, <a href="/search/astro-ph?searchtype=author&query=Dragomir%2C+D">Diana Dragomir</a>, <a href="/search/astro-ph?searchtype=author&query=Crossfield%2C+I">Ian Crossfield</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderspek%2C+R">Roland Vanderspek</a>, <a href="/search/astro-ph?searchtype=author&query=Fausnaugh%2C+M">Michael Fausnaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+C+J">Christopher J. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Ricker%2C+G">George Ricker</a>, <a href="/search/astro-ph?searchtype=author&query=Daylan%2C+T">Tansu Daylan</a>, <a href="/search/astro-ph?searchtype=author&query=Essack%2C+Z">Zahra Essack</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=Osborn%2C+H+P">Hugh P. Osborn</a>, <a href="/search/astro-ph?searchtype=author&query=Pepper%2C+J">Joshua Pepper</a> , et al. (80 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="2103.12538v2-abstract-short" style="display: inline;"> We present 2,241 exoplanet candidates identified with data from the Transiting Exoplanet Survey Satellite (TESS) during its two-year prime mission. We list these candidates in the TESS Objects of Interest (TOI) Catalog, which includes both new planet candidates found by TESS and previously-known planets recovered by TESS observations. We describe the process used to identify TOIs and investigate t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12538v2-abstract-full').style.display = 'inline'; document.getElementById('2103.12538v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.12538v2-abstract-full" style="display: none;"> We present 2,241 exoplanet candidates identified with data from the Transiting Exoplanet Survey Satellite (TESS) during its two-year prime mission. We list these candidates in the TESS Objects of Interest (TOI) Catalog, which includes both new planet candidates found by TESS and previously-known planets recovered by TESS observations. We describe the process used to identify TOIs and investigate the characteristics of the new planet candidates, and discuss some notable TESS planet discoveries. The TOI Catalog includes an unprecedented number of small planet candidates around nearby bright stars, which are well-suited for detailed follow-up observations. The TESS data products for the Prime Mission (Sectors 1-26), including the TOI Catalog, light curves, full-frame images, and target pixel files, are publicly available on the Mikulski Archive for Space Telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12538v2-abstract-full').style.display = 'none'; document.getElementById('2103.12538v2-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">39 pages, 16 figures. The Prime Mission TOI Catalog is included in the ancillary data as a CSV. For the most up-to-date catalog, refer to https://tess.mit.edu/toi-releases/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.02707">arXiv:2101.02707</a> <span> [<a href="https://arxiv.org/pdf/2101.02707">pdf</a>, <a href="https://arxiv.org/format/2101.02707">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/stab2129">10.1093/mnras/stab2129 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TOI-1259Ab -- a gas giant planet with 2.7% deep transits and a bound white dwarf companion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martin%2C+D+V">David V. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=El-Badry%2C+K">Kareem El-Badry</a>, <a href="/search/astro-ph?searchtype=author&query=Hod%C5%BEi%C4%87%2C+V+K">Vedad Kunovac Hod啪i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Triaud%2C+A+H+M+J">Amaury H. M. J. Triaud</a>, <a href="/search/astro-ph?searchtype=author&query=Angus%2C+R">Ruth Angus</a>, <a href="/search/astro-ph?searchtype=author&query=Birky%2C+J">Jessica Birky</a>, <a href="/search/astro-ph?searchtype=author&query=Foreman-Mackey%2C+D">Daniel Foreman-Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Hedges%2C+C">Christina Hedges</a>, <a href="/search/astro-ph?searchtype=author&query=Montet%2C+B+T">Benjamin T. Montet</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+S+J">Simon J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Santerne%2C+A">Alexandre Santerne</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Stephan%2C+A+P">Alexander P. Stephan</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Ji Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Benni%2C+P">Paul Benni</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V">Vadim Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+N">Nikita Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Mishevskiy%2C+N">Nikolay Mishevskiy</a>, <a href="/search/astro-ph?searchtype=author&query=Ziegler%2C+C">Carl Ziegler</a>, <a href="/search/astro-ph?searchtype=author&query=Soubkiou%2C+A">Abderahmane Soubkiou</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhaldoun%2C+Z">Zouhair Benkhaldoun</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+D+A">Douglas A. Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+K">Karen Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Henze%2C+C+E">Christopher E. Henze</a>, <a href="/search/astro-ph?searchtype=author&query=Guerrero%2C+N+M">Natalia M. Guerrero</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="2101.02707v2-abstract-short" style="display: inline;"> We present TOI-1259Ab, a 1.0 Rjup gas giant planet transiting a 0.71 Rsun K-dwarf on a 3.48 day orbit. The system also contains a bound white dwarf companion TOI-1259B with a projected distance of approximately 1600 AU from the planet host. Transits are observed in nine TESS sector and are 2.7 per cent deep - among the deepest known - making TOI-1259Ab a promising target for atmospheric characteri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02707v2-abstract-full').style.display = 'inline'; document.getElementById('2101.02707v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.02707v2-abstract-full" style="display: none;"> We present TOI-1259Ab, a 1.0 Rjup gas giant planet transiting a 0.71 Rsun K-dwarf on a 3.48 day orbit. The system also contains a bound white dwarf companion TOI-1259B with a projected distance of approximately 1600 AU from the planet host. Transits are observed in nine TESS sector and are 2.7 per cent deep - among the deepest known - making TOI-1259Ab a promising target for atmospheric characterization. Our follow-up radial velocity measurements indicate a variability of semiamplitude K = 71 m/s, implying a planet mass of 0.44 Mjup. By fitting the spectral energy distribution of the white dwarf we derive a total age of 4.08 (+1.21 -0.53) Gyr for the system. The K-dwarf's light curve reveals a rotational variability with a period of 28 days, which implies a gyrochronology age broadly consistent with the white dwarf's total age. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02707v2-abstract-full').style.display = 'none'; document.getElementById('2101.02707v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">Accepted to MNRAS. Some structural changes from first arXiv version but no significant changes to results. One figure got a bit prettier</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.01593">arXiv:2101.01593</a> <span> [<a href="https://arxiv.org/pdf/2101.01593">pdf</a>, <a href="https://arxiv.org/format/2101.01593">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/stab2143">10.1093/mnras/stab2143 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Masses and compositions of three small planets orbiting the nearby M dwarf L231-32 (TOI-270) and the M dwarf radius valley </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Van+Eylen%2C+V">Vincent Van Eylen</a>, <a href="/search/astro-ph?searchtype=author&query=Astudillo-Defru%2C+N">N. Astudillo-Defru</a>, <a href="/search/astro-ph?searchtype=author&query=Bonfils%2C+X">X. Bonfils</a>, <a href="/search/astro-ph?searchtype=author&query=Livingston%2C+J">J. Livingston</a>, <a href="/search/astro-ph?searchtype=author&query=Hirano%2C+T">T. Hirano</a>, <a href="/search/astro-ph?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/astro-ph?searchtype=author&query=Lam%2C+K+W+F">K. W. F. Lam</a>, <a href="/search/astro-ph?searchtype=author&query=Justesen%2C+A+B">A. B. Justesen</a>, <a href="/search/astro-ph?searchtype=author&query=Winn%2C+J+N">J. N. Winn</a>, <a href="/search/astro-ph?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+G">G. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">S. Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+F">F. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Estrada%2C+B+C">B. Campos Estrada</a>, <a href="/search/astro-ph?searchtype=author&query=Owen%2C+J+E">J. E. Owen</a>, <a href="/search/astro-ph?searchtype=author&query=Foreman-Mackey%2C+D">D. Foreman-Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/astro-ph?searchtype=author&query=Korth%2C+J">J. Korth</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Forveille%2C+T">T. Forveille</a>, <a href="/search/astro-ph?searchtype=author&query=Mikal-Evans%2C+T">T. Mikal-Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Osborne%2C+H+L+M">H. L. M. Osborne</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+C+S+K">C. S. K. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Almenara%2C+J+M">J. M. Almenara</a> , et al. (47 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="2101.01593v2-abstract-short" style="display: inline;"> We report on precise Doppler measurements of L231-32 (TOI-270), a nearby M dwarf ($d=22$ pc, $M_\star = 0.39$ M$_\odot$, $R_\star = 0.38$ R$_\odot$), which hosts three transiting planets that were recently discovered using data from the Transiting Exoplanet Survey Satellite (TESS). The three planets are 1.2, 2.4, and 2.1 times the size of Earth and have orbital periods of 3.4, 5.7, and 11.4 days.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01593v2-abstract-full').style.display = 'inline'; document.getElementById('2101.01593v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.01593v2-abstract-full" style="display: none;"> We report on precise Doppler measurements of L231-32 (TOI-270), a nearby M dwarf ($d=22$ pc, $M_\star = 0.39$ M$_\odot$, $R_\star = 0.38$ R$_\odot$), which hosts three transiting planets that were recently discovered using data from the Transiting Exoplanet Survey Satellite (TESS). The three planets are 1.2, 2.4, and 2.1 times the size of Earth and have orbital periods of 3.4, 5.7, and 11.4 days. We obtained 29 high-resolution optical spectra with the newly commissioned Echelle Spectrograph for Rocky Exoplanet and Stable Spectroscopic Observations (ESPRESSO) and 58 spectra using the High Accuracy Radial velocity Planet Searcher (HARPS). From these observations, we find the masses of the planets to be $1.58 \pm 0.26$, $6.15 \pm 0.37$, and $4.78 \pm 0.43$ M$_\oplus$, respectively. The combination of radius and mass measurements suggests that the innermost planet has a rocky composition similar to that of Earth, while the outer two planets have lower densities. Thus, the inner planet and the outer planets are on opposite sides of the `radius valley' -- a region in the radius-period diagram with relatively few members, which has been interpreted as a consequence of atmospheric photo-evaporation. We place these findings into the context of other small close-in planets orbiting M dwarf stars, and use support vector machines to determine the location and slope of the M dwarf ($T_\mathrm{eff} < 4000$ K) radius valley as a function of orbital period. We compare the location of the M dwarf radius valley to the radius valley observed for FGK stars, and find that its location is a good match to photo-evaporation and core-powered mass loss models. Finally, we show that planets below the M dwarf radius valley have compositions consistent with stripped rocky cores, whereas most planets above have a lower density consistent with the presence of a H-He atmosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01593v2-abstract-full').style.display = 'none'; document.getElementById('2101.01593v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">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/2011.11560">arXiv:2011.11560</a> <span> [<a href="https://arxiv.org/pdf/2011.11560">pdf</a>, <a href="https://arxiv.org/format/2011.11560">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac0f0a">10.3847/1538-4365/ac0f0a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Magellan-TESS Survey I: Survey Description and Mid-Survey Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Teske%2C+J">Johanna Teske</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+X">Sharon Xuesong Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wolfgang%2C+A">Angie Wolfgang</a>, <a href="/search/astro-ph?searchtype=author&query=Gan%2C+T">Tianjun Gan</a>, <a href="/search/astro-ph?searchtype=author&query=Plotnykov%2C+M">Mykhaylo Plotnykov</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=Butler%2C+R+P">R. Paul Butler</a>, <a href="/search/astro-ph?searchtype=author&query=Cale%2C+B">Bryson Cale</a>, <a href="/search/astro-ph?searchtype=author&query=Crane%2C+J+D">Jeffrey D. Crane</a>, <a href="/search/astro-ph?searchtype=author&query=Howard%2C+W">Ward Howard</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+E+L+N">Eric L. N. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+N">Nicholas Law</a>, <a href="/search/astro-ph?searchtype=author&query=Shectman%2C+S+A">Stephen A. Shectman</a>, <a href="/search/astro-ph?searchtype=author&query=Plavchan%2C+P">Peter Plavchan</a>, <a href="/search/astro-ph?searchtype=author&query=Valencia%2C+D">Diana Valencia</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderburg%2C+A">Andrew Vanderburg</a>, <a href="/search/astro-ph?searchtype=author&query=Ricker%2C+G">George Ricker</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderspek%2C+R">Roland Vanderspek</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+D+W">Dave W. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=Seager%2C+S">Sara Seager</a>, <a href="/search/astro-ph?searchtype=author&query=Winn%2C+J+W">Joshua W. Winn</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J+M">Jon M. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">Vardan Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Barrado%2C+D">David Barrado</a>, <a href="/search/astro-ph?searchtype=author&query=Barros%2C+S+C+C">Susana C. C. Barros</a> , et al. (44 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="2011.11560v2-abstract-short" style="display: inline;"> $Kepler… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.11560v2-abstract-full').style.display = 'inline'; document.getElementById('2011.11560v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.11560v2-abstract-full" style="display: none;"> $Kepler$ revealed that roughly one-third of Sun-like stars host planets orbiting within 100 days and between the size of Earth and Neptune. How do these planets form, what are they made of, and do they represent a continuous population or multiple populations? To help address these questions, we began the Magellan-TESS Survey (MTS), which uses Magellan II/PFS to obtain radial velocity (RV) masses of 30 TESS-detected exoplanets and develops an analysis framework that connects observed planet distributions to underlying populations. In the past, small planet RV measurements have been challenging to obtain due to host star faintness and low RV semi-amplitudes, and challenging to interpret due to the potential biases in target selection and observation planning decisions. The MTS attempts to minimize these biases by focusing on bright TESS targets and employing a quantitative selection function and observing strategy. In this paper, we (1) describe our motivation and survey strategy, (2) present our first catalog of planet density constraints for 27 TESS Objects of Interest (TOIs; 22 in our population analysis sample, 12 that are members of the same systems), and (3) employ a hierarchical Bayesian model to produce preliminary constraints on the mass-radius (M-R) relation. We find that the biases causing previous M-R relations to predict fairly high masses at $1~R_\oplus$ have been reduced. This work can inform more detailed studies of individual systems and offer a framework that can be applied to future RV surveys with the goal of population inferences. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.11560v2-abstract-full').style.display = 'none'; document.getElementById('2011.11560v2-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Minor updates to some masses, and new exploration of broken power law M-R relation. 66 pages (now some figures moved to figure sets, will be in HTML published version). Accepted to ApJS on June 22, 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.14812">arXiv:2010.14812</a> <span> [<a href="https://arxiv.org/pdf/2010.14812">pdf</a>, <a href="https://arxiv.org/format/2010.14812">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/abc418">10.3847/1538-3881/abc418 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Occurrence of Rocky Habitable Zone Planets Around Solar-Like Stars from Kepler Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bryson%2C+S">Steve Bryson</a>, <a href="/search/astro-ph?searchtype=author&query=Kunimoto%2C+M">Michelle Kunimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Kopparapu%2C+R+K">Ravi K. Kopparapu</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+J+L">Jeffrey L. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Borucki%2C+W+J">William J. Borucki</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+D">David Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">Victor Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+C">Christopher Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Barentsen%2C+G">Geert Barentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Batalha%2C+N+M">Natalie. M. Batalha</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+T">Travis Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Boss%2C+A">Alan Boss</a>, <a href="/search/astro-ph?searchtype=author&query=Buchhave%2C+L+A">Lars A. Buchhave</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+C+J">Christopher J. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+D+A">Douglas A. Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Campbell%2C+J+R">Jennifer R. Campbell</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzarite%2C+J">Joseph Catanzarite</a>, <a href="/search/astro-ph?searchtype=author&query=Chandrasekharan%2C+H">Hema Chandrasekharan</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">William J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">Jessie L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">Jorgen Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Ciardi%2C+D+R">David R. Ciardi</a>, <a href="/search/astro-ph?searchtype=author&query=Clarke%2C+B+D">Bruce D. Clarke</a>, <a href="/search/astro-ph?searchtype=author&query=Cochran%2C+W+D">William D. Cochran</a>, <a href="/search/astro-ph?searchtype=author&query=Dotson%2C+J+L">Jessie L. Dotson</a> , et al. (57 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.14812v2-abstract-short" style="display: inline;"> We present occurrence rates for rocky planets in the habitable zones (HZ) of main-sequence dwarf stars based on the Kepler DR25 planet candidate catalog and Gaia-based stellar properties. We provide the first analysis in terms of star-dependent instellation flux, which allows us to track HZ planets. We define $畏_\oplus$ as the HZ occurrence of planets with radius between 0.5 and 1.5 $R_\oplus$ orb… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14812v2-abstract-full').style.display = 'inline'; document.getElementById('2010.14812v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.14812v2-abstract-full" style="display: none;"> We present occurrence rates for rocky planets in the habitable zones (HZ) of main-sequence dwarf stars based on the Kepler DR25 planet candidate catalog and Gaia-based stellar properties. We provide the first analysis in terms of star-dependent instellation flux, which allows us to track HZ planets. We define $畏_\oplus$ as the HZ occurrence of planets with radius between 0.5 and 1.5 $R_\oplus$ orbiting stars with effective temperatures between 4800 K and 6300 K. We find that $畏_\oplus$ for the conservative HZ is between $0.37^{+0.48}_{-0.21}$ (errors reflect 68\% credible intervals) and $0.60^{+0.90}_{-0.36}$ planets per star, while the optimistic HZ occurrence is between $0.58^{+0.73}_{-0.33}$ and $0.88^{+1.28}_{-0.51}$ planets per star. These bounds reflect two extreme assumptions about the extrapolation of completeness beyond orbital periods where DR25 completeness data are available. The large uncertainties are due to the small number of detected small HZ planets. We find similar occurrence rates using both a Poisson likelihood Bayesian analysis and Approximate Bayesian Computation. Our results are corrected for catalog completeness and reliability. Both completeness and the planet occurrence rate are dependent on stellar effective temperature. We also present occurrence rates for various stellar populations and planet size ranges. We estimate with $95\%$ confidence that, on average, the nearest HZ planet around G and K dwarfs is about 6 pc away, and there are about 4 HZ rocky planets around G and K dwarfs within 10 pc of the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14812v2-abstract-full').style.display = 'none'; document.getElementById('2010.14812v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">To appear in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.04796">arXiv:2010.04796</a> <span> [<a href="https://arxiv.org/pdf/2010.04796">pdf</a>, <a href="https://arxiv.org/format/2010.04796">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/abab0b">10.3847/1538-3881/abab0b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measuring Transit Signal Recovery in the Kepler Pipeline IV: Completeness of the DR25 Planet Candidate catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">Jessie L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Clarke%2C+B+D">Bruce D. Clarke</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+C+J">Christopher J. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J+M">Jon M. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Bryson%2C+S+T">Stephen T. Bryson</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+J+L">Jeffrey L. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Twicken%2C+J+D">Joseph D. Twicken</a>, <a href="/search/astro-ph?searchtype=author&query=Batalha%2C+N+M">Natalie M. Batalha</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzarite%2C+J">Joseph Catanzarite</a>, <a href="/search/astro-ph?searchtype=author&query=Uddin%2C+A+K">AKM Kamal Uddin</a>, <a href="/search/astro-ph?searchtype=author&query=Zamudio%2C+K">Khadeejah Zamudio</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+C">Jeffrey C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Henze%2C+C+E">Christopher E. Henze</a>, <a href="/search/astro-ph?searchtype=author&query=Campbell%2C+J">Jennifer Campbell</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="2010.04796v1-abstract-short" style="display: inline;"> In this work we empirically measure the detection efficiency of Kepler pipeline used to create the final Kepler Threshold Crossing Event (TCE; Twicken et al. 2016) and planet candidate catalogs (Thompson et al. 2018), a necessary ingredient for occurrence rate calculations using these lists. By injecting simulated signals into the calibrated pixel data and processing those pixels through the pipel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.04796v1-abstract-full').style.display = 'inline'; document.getElementById('2010.04796v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.04796v1-abstract-full" style="display: none;"> In this work we empirically measure the detection efficiency of Kepler pipeline used to create the final Kepler Threshold Crossing Event (TCE; Twicken et al. 2016) and planet candidate catalogs (Thompson et al. 2018), a necessary ingredient for occurrence rate calculations using these lists. By injecting simulated signals into the calibrated pixel data and processing those pixels through the pipeline as normal, we quantify the detection probability of signals as a function of their signal strength and orbital period. In addition we investigate the dependence of the detection efficiency on parameters of the target stars and their location in the Kepler field of view. We find that the end-of-mission version of the Kepler pipeline returns to a high overall detection efficiency, averaging a 90-95% rate of detection for strong signals across a wide variety of parameter space. We find a weak dependence of the detection efficiency on the number of transits contributing to the signal and the orbital period of the signal, and a stronger dependence on the stellar effective temperature and correlated noise properties. We also find a weak dependence of the detection efficiency on the position within the field of view. By restricting the Kepler stellar sample to stars with well-behaved correlated noise properties, we can define a set of stars with high detection efficiency for future occurrence rate calculations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.04796v1-abstract-full').style.display = 'none'; document.getElementById('2010.04796v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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, 9 figure. This paper presents work that was previously presented in a Kepler technical document (KSCI-19110-001; Christiansen 2017), as well as new analysis, in a peer-reviewed journal article. Please update citations from Christiansen 2017 to this work</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> AJ, 2020, 160, 4, 159 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.11899">arXiv:2009.11899</a> <span> [<a href="https://arxiv.org/pdf/2009.11899">pdf</a>, <a href="https://arxiv.org/format/2009.11899">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/stab1567">10.1093/mnras/stab1567 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a young low-mass brown dwarf transiting a fast-rotating F-type star by the Galactic Plane eXoplanet (GPX) survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Benni%2C+P">P. Benni</a>, <a href="/search/astro-ph?searchtype=author&query=Burdanov%2C+A+Y">A. Y. Burdanov</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V+V">V. V. Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A9brard%2C+G">G. H茅brard</a>, <a href="/search/astro-ph?searchtype=author&query=Almenara%2C+J+M">J. M. Almenara</a>, <a href="/search/astro-ph?searchtype=author&query=Dalal%2C+S">S. Dalal</a>, <a href="/search/astro-ph?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/astro-ph?searchtype=author&query=Tsantaki%2C+M">M. Tsantaki</a>, <a href="/search/astro-ph?searchtype=author&query=Pepper%2C+J">J. Pepper</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">K. G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderburg%2C+A">A. Vanderburg</a>, <a href="/search/astro-ph?searchtype=author&query=Belinski%2C+A">A. Belinski</a>, <a href="/search/astro-ph?searchtype=author&query=Kashaev%2C+F">F. Kashaev</a>, <a href="/search/astro-ph?searchtype=author&query=Barkaoui%2C+K">K. Barkaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+T">T. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kang%2C+W">W. Kang</a>, <a href="/search/astro-ph?searchtype=author&query=Antonyuk%2C+K">K. Antonyuk</a>, <a href="/search/astro-ph?searchtype=author&query=Dyachenko%2C+V+V">V. V. Dyachenko</a>, <a href="/search/astro-ph?searchtype=author&query=Rastegaev%2C+D+A">D. A. Rastegaev</a>, <a href="/search/astro-ph?searchtype=author&query=Beskakotov%2C+A">A. Beskakotov</a>, <a href="/search/astro-ph?searchtype=author&query=Mitrofanova%2C+A+A">A. A. Mitrofanova</a>, <a href="/search/astro-ph?searchtype=author&query=Pozuelos%2C+F+J">F. J. Pozuelos</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+E+D">E. D. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Popov%2C+A">A. Popov</a> , et al. (42 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="2009.11899v2-abstract-short" style="display: inline;"> We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of $19.7\pm 1.6$ $M_{\mathrm{Jup}}$ and a radius of $1.47\pm0.10$ $R_{\mathrm{Jup}}$, the first sub-stellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright ($V$ = 12.3 mag) fast-rotating F-type star with a projected rotational velocity $v\sin{ i_*}=40\pm10$ km/s.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.11899v2-abstract-full').style.display = 'inline'; document.getElementById('2009.11899v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.11899v2-abstract-full" style="display: none;"> We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of $19.7\pm 1.6$ $M_{\mathrm{Jup}}$ and a radius of $1.47\pm0.10$ $R_{\mathrm{Jup}}$, the first sub-stellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright ($V$ = 12.3 mag) fast-rotating F-type star with a projected rotational velocity $v\sin{ i_*}=40\pm10$ km/s. We use the isochrone placement algorithm to characterize the host star, which has effective temperature $7000\pm200$ K, mass $1.68\pm0.10$ $M_{\mathrm{Sun}}$, radius $1.56\pm0.10$ $R_{\mathrm{Sun}}$ and approximate age $0.27_{-0.15}^{+0.09}$ Gyr. GPX-1 b has an orbital period of $\sim$1.75 d, and a transit depth of $0.90\pm0.03$ %. We describe the GPX transit detection observations, subsequent photometric and speckle-interferometric follow-up observations, and SOPHIE spectroscopic measurements, which allowed us to establish the presence of a sub-stellar object around the host star. GPX-1 was observed at 30-min integrations by TESS in Sector 18, but the data is affected by blending with a 3.4 mag brighter star 42 arcsec away. GPX-1 b is one of about two dozen transiting brown dwarfs known to date, with a mass close to the theoretical brown dwarf/gas giant planet mass transition boundary. Since GPX-1 is a moderately bright and fast-rotating star, it can be followed-up by the means of Doppler tomography. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.11899v2-abstract-full').style.display = 'none'; document.getElementById('2009.11899v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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, 13 figures, accepted to MNRAS in May 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.12535">arXiv:2008.12535</a> <span> [<a href="https://arxiv.org/pdf/2008.12535">pdf</a>, <a href="https://arxiv.org/format/2008.12535">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/staa2502">10.1093/mnras/staa2502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TOI-763 system: sub-Neptunes orbiting a Sun-like star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/astro-ph?searchtype=author&query=Livingston%2C+J">J. Livingston</a>, <a href="/search/astro-ph?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/astro-ph?searchtype=author&query=Lam%2C+K+W+F">K. W. F. Lam</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">K. G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Hellier%2C+C">C. Hellier</a>, <a href="/search/astro-ph?searchtype=author&query=Korth%2C+J">J. Korth</a>, <a href="/search/astro-ph?searchtype=author&query=Hatzes%2C+A+P">A. P. Hatzes</a>, <a href="/search/astro-ph?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/astro-ph?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/astro-ph?searchtype=author&query=Redfield%2C+S">S. Redfield</a>, <a href="/search/astro-ph?searchtype=author&query=Guenther%2C+E+W">E. W. Guenther</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">S. Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Barragan%2C+O">O. Barragan</a>, <a href="/search/astro-ph?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/astro-ph?searchtype=author&query=Bouma%2C+L">L. Bouma</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Cochran%2C+W+D">W. D. Cochran</a>, <a href="/search/astro-ph?searchtype=author&query=Csizmadia%2C+S">Sz. Csizmadia</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+F">F. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Deeg%2C+H+J">H. J. Deeg</a>, <a href="/search/astro-ph?searchtype=author&query=Esposito%2C+M">M. Esposito</a>, <a href="/search/astro-ph?searchtype=author&query=Georgieva%2C+I">I. Georgieva</a>, <a href="/search/astro-ph?searchtype=author&query=Grziwa%2C+S">S. Grziwa</a> , et al. (29 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="2008.12535v1-abstract-short" style="display: inline;"> We report the discovery of a planetary system orbiting TOI-763 (aka CD-39 7945), a $V=10.2$, high proper motion G-type dwarf star that was photometrically monitored by the TESS space mission in Sector 10. We obtain and model the stellar spectrum and find an object slightly smaller than the Sun, and somewhat older, but with a similar metallicity. Two planet candidates were found in the light curve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.12535v1-abstract-full').style.display = 'inline'; document.getElementById('2008.12535v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.12535v1-abstract-full" style="display: none;"> We report the discovery of a planetary system orbiting TOI-763 (aka CD-39 7945), a $V=10.2$, high proper motion G-type dwarf star that was photometrically monitored by the TESS space mission in Sector 10. We obtain and model the stellar spectrum and find an object slightly smaller than the Sun, and somewhat older, but with a similar metallicity. Two planet candidates were found in the light curve to be transiting the star. Combining TESS transit photometry with HARPS high-precision radial velocity follow-up measurements confirm the planetary nature of these transit signals. We determine masses, radii, and bulk densities of these two planets. A third planet candidate was discovered serendipitously in the radial velocity data. The inner transiting planet,TOI-763 b, has an orbital period of $P_\mathrm{b}$ = 5.6~days, a mass of $M_\mathrm{b}$ = $9.8\pm0.8$ $M_\oplus$, and a radius of $R_\mathrm{b}$ = $2.37\pm0.10$ $R_\oplus$. The second transiting planet,TOI-763 c, has an orbital period of $P_\mathrm{c}$ = 12.3~days, a mass of $M_\mathrm{c}$ = $9.3\pm1.0$ $M_\oplus$, and a radius of $R_\mathrm{c}$ = $2.87\pm0.11$ $R_\oplus$. We find the outermost planet candidate to orbit the star with a period of $\sim$48~days. If confirmed as a planet it would have a minimum mass of $M_\mathrm{d}$ = $9.5\pm1.6$ $M_\oplus$. We investigated the TESS light curve in order to search for a mono transit by planet~d without success. We discuss the importance and implications of this planetary system in terms of the geometrical arrangements of planets orbiting G-type stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.12535v1-abstract-full').style.display = 'none'; document.getElementById('2008.12535v1-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> 28 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.15719">arXiv:2006.15719</a> <span> [<a href="https://arxiv.org/pdf/2006.15719">pdf</a>, <a href="https://arxiv.org/format/2006.15719">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/abb316">10.3847/1538-3881/abb316 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reliability Correction is Key for Robust Kepler Occurrence Rates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bryson%2C+S">Steve Bryson</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+J+L">Jeffrey L. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Kunimoto%2C+M">Michelle Kunimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</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="2006.15719v1-abstract-short" style="display: inline;"> The Kepler DR25 planet candidate catalog was produced using an automated method of planet candidate identification based on various tests. These tests were tuned to obtain a reasonable but arbitrary balance between catalog completeness and reliability. We produce new catalogs with differing balances of completeness and reliability by varying these tests, and study the impact of these alternative c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.15719v1-abstract-full').style.display = 'inline'; document.getElementById('2006.15719v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.15719v1-abstract-full" style="display: none;"> The Kepler DR25 planet candidate catalog was produced using an automated method of planet candidate identification based on various tests. These tests were tuned to obtain a reasonable but arbitrary balance between catalog completeness and reliability. We produce new catalogs with differing balances of completeness and reliability by varying these tests, and study the impact of these alternative catalogs on occurrence rates. We find that if there is no correction for reliability, different catalogs give statistically inconsistent occurrence rates, while if we correct for both completeness and reliability, we get statistically consistent occurrence rates. This is a strong indication that correction for completeness and reliability is critical for the accurate computation of occurrence rates. Additionally, we find that this result is the same whether using Bayesian Poisson likelihood MCMC or Approximate Bayesian Computation methods. We also examine the use of a Robovetter disposition score cut as an alternative to reliability correction, and find that while a score cut does increase the reliability of the catalog, it is not as accurate as performing a full reliability correction. We get the same result when performing a reliability correction with and without a score cut. Therefore removing low-score planets removes data without providing any advantage, and should be avoided when possible. We make our alternative catalogs publicly available, and propose that these should be used as a test of occurrence rate methods, with the requirement that a method should provide statistically consistent occurrence rates for all these catalogs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.15719v1-abstract-full').style.display = 'none'; document.getElementById('2006.15719v1-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> 28 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Submitted to AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.06725">arXiv:2004.06725</a> <span> [<a href="https://arxiv.org/pdf/2004.06725">pdf</a>, <a href="https://arxiv.org/format/2004.06725">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ab84e5">10.3847/2041-8213/ab84e5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Habitable-Zone Earth-Sized Planet Rescued from False Positive Status </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanderburg%2C+A">Andrew Vanderburg</a>, <a href="/search/astro-ph?searchtype=author&query=Rowden%2C+P">Pamela Rowden</a>, <a href="/search/astro-ph?searchtype=author&query=Bryson%2C+S">Steve Bryson</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+J">Jeffrey Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Batalha%2C+N">Natalie Batalha</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+K+A">Karen A. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+D+W">David W. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Col%C3%B3n%2C+K+D">Knicole D. Col贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Henze%2C+C">Chris Henze</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+C+X">Chelsea X. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Quinn%2C+S+N">Samuel N. Quinn</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="2004.06725v1-abstract-short" style="display: inline;"> We report the discovery of an Earth-sized planet in the habitable zone of a low-mass star called Kepler-1649. The planet, Kepler-1649 c, is 1.06$^{+0.15}_{-0.10}$ times the size of Earth and transits its 0.1977 +/- 0.0051 Msun mid M-dwarf host star every 19.5 days. It receives 74 +/- 3 % the incident flux of Earth, giving it an equilibrium temperature of 234 +/- 20K and placing it firmly inside th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.06725v1-abstract-full').style.display = 'inline'; document.getElementById('2004.06725v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.06725v1-abstract-full" style="display: none;"> We report the discovery of an Earth-sized planet in the habitable zone of a low-mass star called Kepler-1649. The planet, Kepler-1649 c, is 1.06$^{+0.15}_{-0.10}$ times the size of Earth and transits its 0.1977 +/- 0.0051 Msun mid M-dwarf host star every 19.5 days. It receives 74 +/- 3 % the incident flux of Earth, giving it an equilibrium temperature of 234 +/- 20K and placing it firmly inside the circumstellar habitable zone. Kepler-1649 also hosts a previously-known inner planet that orbits every 8.7 days and is roughly equivalent to Venus in size and incident flux. Kepler-1649 c was originally classified as a false positive by the Kepler pipeline, but was rescued as part of a systematic visual inspection of all automatically dispositioned Kepler false positives. This discovery highlights the value of human inspection of planet candidates even as automated techniques improve, and hints that terrestrial planets around mid to late M-dwarfs may be more common than those around more massive stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.06725v1-abstract-full').style.display = 'none'; document.getElementById('2004.06725v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 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">11 pages, 3 figures, 1 table. Accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.11481">arXiv:2003.11481</a> <span> [<a href="https://arxiv.org/pdf/2003.11481">pdf</a>, <a href="https://arxiv.org/ps/2003.11481">ps</a>, <a href="https://arxiv.org/format/2003.11481">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/10.1051/0004-6361/202037470">10.1051/0004-6361/202037470 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TESS first look at evolved compact pulsators: Known ZZ Ceti stars of the southern ecliptic hemisphere as seen by TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bogn%C3%A1r%2C+Z">Zs. Bogn谩r</a>, <a href="/search/astro-ph?searchtype=author&query=Kawaler%2C+S+D">S. D. Kawaler</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+K+J">K. J. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Schrandt%2C+C">C. Schrandt</a>, <a href="/search/astro-ph?searchtype=author&query=Baran%2C+A+S">A. S. Baran</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+P+A">P. A. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Hermes%2C+J+J">J. J. Hermes</a>, <a href="/search/astro-ph?searchtype=author&query=Charpinet%2C+S">S. Charpinet</a>, <a href="/search/astro-ph?searchtype=author&query=Handler%2C+G">G. Handler</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">S. E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+S+J">S. J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Raddi%2C+R">R. Raddi</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%B3dor%2C+%C3%81">脕. S贸dor</a>, <a href="/search/astro-ph?searchtype=author&query=Tremblay%2C+P+-">P. -E. Tremblay</a>, <a href="/search/astro-ph?searchtype=author&query=Uzundag%2C+M">M. Uzundag</a>, <a href="/search/astro-ph?searchtype=author&query=Zong%2C+W">W. Zong</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="2003.11481v1-abstract-short" style="display: inline;"> Context. We present our findings on 18 formerly known ZZ Ceti stars observed by the TESS space telescope in 120s cadence mode during the survey observation of the southern ecliptic hemisphere. Aims. We focus on the frequency analysis of the space-based observations, comparing the results with the findings of the previous ground-based measurements. The frequencies detected by the TESS observation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.11481v1-abstract-full').style.display = 'inline'; document.getElementById('2003.11481v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.11481v1-abstract-full" style="display: none;"> Context. We present our findings on 18 formerly known ZZ Ceti stars observed by the TESS space telescope in 120s cadence mode during the survey observation of the southern ecliptic hemisphere. Aims. We focus on the frequency analysis of the space-based observations, comparing the results with the findings of the previous ground-based measurements. The frequencies detected by the TESS observations can serve as inputs for future asteroseismic analyses. Methods. We performed standard pre-whitening of the data sets to derive the possible pulsation frequencies of the different targets. In some cases, we fitted Lorentzians to the frequency groups that emerged as the results of short-term amplitude/phase variations that occurred during the TESS observations. Results. We detected more than 40 pulsation frequencies in seven ZZ Ceti stars observed in the 120s cadence by TESS, with better than 0.1 microHz precision. We found that HE 0532-5605 may be a new outbursting ZZ Ceti. Ten targets do not show any significant pulsation frequencies in their Fourier transforms, due to a combination of their intrinsic faintness and/or crowding on the large TESS pixels. We also detected possible amplitude/phase variations during the TESS observations in some cases. Such behaviour in these targets was not previously identified from ground-based observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.11481v1-abstract-full').style.display = 'none'; document.getElementById('2003.11481v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">21 pages, 19 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 638, A82 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.00952">arXiv:2001.00952</a> <span> [<a href="https://arxiv.org/pdf/2001.00952">pdf</a>, <a href="https://arxiv.org/format/2001.00952">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/aba4b2">10.3847/1538-3881/aba4b2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The First Habitable Zone Earth-sized Planet from TESS. I: Validation of the TOI-700 System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+E+A">Emily A. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Schlieder%2C+J+E">Joshua E. Schlieder</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Hord%2C+B+J">Benjamin J. Hord</a>, <a href="/search/astro-ph?searchtype=author&query=Kostov%2C+V+B">Veselin B. Kostov</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+E+D">Eric D. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Rowe%2C+J+F">Jason F. Rowe</a>, <a href="/search/astro-ph?searchtype=author&query=Hoffman%2C+K">Kelsey Hoffman</a>, <a href="/search/astro-ph?searchtype=author&query=Walkowicz%2C+L+M">Lucianne M. Walkowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Silverstein%2C+M+L">Michele L. Silverstein</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez%2C+J+E">Joseph E. Rodriguez</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderburg%2C+A">Andrew Vanderburg</a>, <a href="/search/astro-ph?searchtype=author&query=Suissa%2C+G">Gabrielle Suissa</a>, <a href="/search/astro-ph?searchtype=author&query=Airapetian%2C+V+S">Vladimir S. Airapetian</a>, <a href="/search/astro-ph?searchtype=author&query=Clement%2C+M+S">Matthew S. Clement</a>, <a href="/search/astro-ph?searchtype=author&query=Raymond%2C+S+N">Sean N. Raymond</a>, <a href="/search/astro-ph?searchtype=author&query=Mann%2C+A+W">Andrew W. Mann</a>, <a href="/search/astro-ph?searchtype=author&query=Kruse%2C+E">Ethan Kruse</a>, <a href="/search/astro-ph?searchtype=author&query=Lissauer%2C+J+J">Jack J. Lissauer</a>, <a href="/search/astro-ph?searchtype=author&query=Col%C3%B3n%2C+K+D">Knicole D. Col贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Kopparapu%2C+R+k">Ravi kumar Kopparapu</a>, <a href="/search/astro-ph?searchtype=author&query=Kreidberg%2C+L">Laura Kreidberg</a>, <a href="/search/astro-ph?searchtype=author&query=Zieba%2C+S">Sebastian Zieba</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+K+A">Karen A. Collins</a> , et al. (70 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.00952v2-abstract-short" style="display: inline;"> We present the discovery and validation of a three-planet system orbiting the nearby (31.1 pc) M2 dwarf star TOI-700 (TIC 150428135). TOI-700 lies in the TESS continuous viewing zone in the Southern Ecliptic Hemisphere; observations spanning 11 sectors reveal three planets with radii ranging from 1 R$_\oplus$ to 2.6 R$_\oplus$ and orbital periods ranging from 9.98 to 37.43 days. Ground-based follo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.00952v2-abstract-full').style.display = 'inline'; document.getElementById('2001.00952v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.00952v2-abstract-full" style="display: none;"> We present the discovery and validation of a three-planet system orbiting the nearby (31.1 pc) M2 dwarf star TOI-700 (TIC 150428135). TOI-700 lies in the TESS continuous viewing zone in the Southern Ecliptic Hemisphere; observations spanning 11 sectors reveal three planets with radii ranging from 1 R$_\oplus$ to 2.6 R$_\oplus$ and orbital periods ranging from 9.98 to 37.43 days. Ground-based follow-up combined with diagnostic vetting and validation tests enable us to rule out common astrophysical false-positive scenarios and validate the system of planets. The outermost planet, TOI-700 d, has a radius of $1.19\pm0.11$ R$_\oplus$ and resides in the conservative habitable zone of its host star, where it receives a flux from its star that is approximately 86% of the Earth's insolation. In contrast to some other low-mass stars that host Earth-sized planets in their habitable zones, TOI-700 exhibits low levels of stellar activity, presenting a valuable opportunity to study potentially-rocky planets over a wide range of conditions affecting atmospheric escape. While atmospheric characterization of TOI-700 d with the James Webb Space Telescope (JWST) will be challenging, the larger sub-Neptune, TOI-700 c (R = 2.63 R$_\oplus$), will be an excellent target for JWST and beyond. TESS is scheduled to return to the Southern Hemisphere and observe TOI-700 for an additional 11 sectors in its extended mission, which should provide further constraints on the known planet parameters and searches for additional planets and transit timing variations in the system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.00952v2-abstract-full').style.display = 'none'; document.getElementById('2001.00952v2-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Accepted for publication in AJ (30 pages, 13 figures, 4 tables, 2 appendices)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.03575">arXiv:1906.03575</a> <span> [<a href="https://arxiv.org/pdf/1906.03575">pdf</a>, <a href="https://arxiv.org/format/1906.03575">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab8a30">10.3847/1538-3881/ab8a30 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Probabilistic Approach to Kepler Completeness and Reliability for Exoplanet Occurrence Rates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bryson%2C+S">Steve Bryson</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+J">Jeffrey Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Batalha%2C+N+M">Natalie M. Batalha</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+T">Travis Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">Dan Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+C">Christopher Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Dotson%2C+J">Jessie Dotson</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</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="1906.03575v4-abstract-short" style="display: inline;"> Exoplanet catalogs produced by surveys suffer from a lack of completeness (not every planet is detected) and less than perfect reliability (not every planet in the catalog is a true planet), particularly near the survey's detection limit. Exoplanet occurrence rate studies based on such a catalog must be corrected for completeness and reliability. The final Kepler data release, DR25, features a uni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.03575v4-abstract-full').style.display = 'inline'; document.getElementById('1906.03575v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.03575v4-abstract-full" style="display: none;"> Exoplanet catalogs produced by surveys suffer from a lack of completeness (not every planet is detected) and less than perfect reliability (not every planet in the catalog is a true planet), particularly near the survey's detection limit. Exoplanet occurrence rate studies based on such a catalog must be corrected for completeness and reliability. The final Kepler data release, DR25, features a uniformly vetted planet candidate catalog and data products that facilitate corrections. We present a new probabilistic approach to the characterization of Kepler completeness and reliability, making full use of the Kepler DR25 products. We illustrate the impact of completeness and reliability corrections with a Poisson-likelihood occurrence rate method, using a recent stellar properties catalog that incorporates Gaia stellar radii and essentially uniform treatment of the stellar population. Correcting for reliability has a significant impact: the exoplanet occurrence rate for orbital period and radius within 20% of Earth's around GK dwarf stars, corrected for reliability, is 0.015+0.011-0.007, whereas not correcting results in 0.034+0.018-0.012 - correcting for reliability reduces this occurrence rate by more than a factor of two. We further show that using Gaia-based vs. DR25 stellar properties impacts the same occurrence rate by a factor of two. We critically examine the the DR25 catalog and the assumptions behind our occurrence rate method. We propose several ways in which confidence in both the Kepler catalog and occurrence rate calculations can be improved. This work provides an example of how the community can use the DR25 completeness and reliability products. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.03575v4-abstract-full').style.display = 'none'; document.getElementById('1906.03575v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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 for publication in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.07459">arXiv:1901.07459</a> <span> [<a href="https://arxiv.org/pdf/1901.07459">pdf</a>, <a href="https://arxiv.org/format/1901.07459">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab0110">10.3847/1538-3881/ab0110 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery and Vetting of Exoplanets I: Benchmarking K2 Vetting Tools </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kostov%2C+V+B">Veselin B. Kostov</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+S+E">Susan E. Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+E+V">Elisa V. Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+J+L">Jeffrey L. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Mullally%2C+F">Fergal Mullally</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Colon%2C+K+D">Knicole D. Colon</a>, <a href="/search/astro-ph?searchtype=author&query=Schlieder%2C+J+E">Joshua E. Schlieder</a>, <a href="/search/astro-ph?searchtype=author&query=Barentsen%2C+G">Geert Barentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+C+J">Christopher J. Burke</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="1901.07459v1-abstract-short" style="display: inline;"> We have adapted the algorithmic tools developed during the Kepler mission to vet the quality of transit-like signals for use on the K2 mission data. Using the four sets of publicly-available lightcurves on MAST, we produced a uniformly-vetted catalog of 772 transiting planet candidates from K2 as listed at the NASA Exoplanet archive in the K2 Table of Candidates. Our analysis marks 676 of these as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.07459v1-abstract-full').style.display = 'inline'; document.getElementById('1901.07459v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.07459v1-abstract-full" style="display: none;"> We have adapted the algorithmic tools developed during the Kepler mission to vet the quality of transit-like signals for use on the K2 mission data. Using the four sets of publicly-available lightcurves on MAST, we produced a uniformly-vetted catalog of 772 transiting planet candidates from K2 as listed at the NASA Exoplanet archive in the K2 Table of Candidates. Our analysis marks 676 of these as planet candidates and 96 as false positives. All confirmed planets pass our vetting tests. 60 of our false positives are new identifications -- effectively doubling the overall number of astrophysical signals mimicking planetary transits in K2 data. Most of the targets listed as false positives in our catalog either show prominent secondary eclipses, transit depths suggesting a stellar companion instead of a planet, or significant photocenter shifts during transit. We packaged our tools into the open-source, automated vetting pipeline DAVE (Discovery and Vetting of Exoplanets) designed to streamline follow-up efforts by reducing the time and resources wasted observing targets that are likely false positives. DAVE will also be a valuable tool for analyzing planet candidates from NASA's TESS mission, where several guest-investigator programs will provide independent lightcurve sets -- and likely many more from the community. We are currently testing DAVE on recently-released TESS planet candidates and will present our results in a follow-up paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.07459v1-abstract-full').style.display = 'none'; document.getElementById('1901.07459v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">43 pages, 23 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/1901.01643">arXiv:1901.01643</a> <span> [<a href="https://arxiv.org/pdf/1901.01643">pdf</a>, <a href="https://arxiv.org/format/1901.01643">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab1488">10.3847/1538-3881/ab1488 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Hot Saturn Orbiting An Oscillating Late Subgiant Discovered by TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">Daniel Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">William J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Chontos%2C+A">Ashley Chontos</a>, <a href="/search/astro-ph?searchtype=author&query=Kjeldsen%2C+H">Hans Kjeldsen</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">Joergen Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">Timothy R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Ball%2C+W">Warrick Ball</a>, <a href="/search/astro-ph?searchtype=author&query=Brahm%2C+R">Rafael Brahm</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">Nestor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Jordan%2C+A">Andres Jordan</a>, <a href="/search/astro-ph?searchtype=author&query=Sarkis%2C+P">Paula Sarkis</a>, <a href="/search/astro-ph?searchtype=author&query=Knudstrup%2C+E">Emil Knudstrup</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">Simon Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Grundahl%2C+F">Frank Grundahl</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M+F">Mads Fredslund Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+P+L">Pere L. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Crossfield%2C+I">Ian Crossfield</a>, <a href="/search/astro-ph?searchtype=author&query=Fulton%2C+B">Benjamin Fulton</a>, <a href="/search/astro-ph?searchtype=author&query=Howard%2C+A+W">Andrew W. Howard</a>, <a href="/search/astro-ph?searchtype=author&query=Isaacson%2C+H+T">Howard T. Isaacson</a>, <a href="/search/astro-ph?searchtype=author&query=Weiss%2C+L+M">Lauren M. Weiss</a>, <a href="/search/astro-ph?searchtype=author&query=Handberg%2C+R">Rasmus Handberg</a>, <a href="/search/astro-ph?searchtype=author&query=Lund%2C+M+N">Mikkel N. Lund</a>, <a href="/search/astro-ph?searchtype=author&query=Serenelli%2C+A+M">Aldo M. Serenelli</a> , et al. (117 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="1901.01643v2-abstract-short" style="display: inline;"> We present the discovery of TOI-197.01, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. TOI-197 (HIP116158) is a bright (V=8.2 mag), spectroscopically classified subgiant which oscillates with an average frequency of about 430 muHz and displays a clear signature of mixed modes. The oscillation ampli… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.01643v2-abstract-full').style.display = 'inline'; document.getElementById('1901.01643v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.01643v2-abstract-full" style="display: none;"> We present the discovery of TOI-197.01, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. TOI-197 (HIP116158) is a bright (V=8.2 mag), spectroscopically classified subgiant which oscillates with an average frequency of about 430 muHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2-minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (2.943+/-0.064 Rsun), mass (1.212 +/- 0.074 Msun) and age (4.9+/-1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a "hot Saturn" (9.17+/-0.33 Rearth) with an orbital period of ~14.3 days, irradiance of 343+/-24 Fearth, moderate mass (60.5 +/- 5.7 Mearth) and density (0.431+/-0.062 gcc). The properties of TOI-197.01 show that the host-star metallicity - planet mass correlation found in sub-Saturns (4-8 Rearth) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ~15%, TOI-197.01 is one of the best characterized Saturn-sized planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.01643v2-abstract-full').style.display = 'none'; document.getElementById('1901.01643v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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 (excluding author list and references), 9 figures, 4 tables, accepted for publication in AJ. An electronic version of Table 3 is available as an ancillary file (sidebar on the right)</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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