JWST COMPASS: A NIRSpec G395H Transmission Spectrum of Radius Valley-Dweller TOI-260 b
Earth and Planets Laboratory, Carnegie Institution for Science（卡内基科学研究所地球与行星实验室）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics and Astronomy, University of New Mexico（新墨西哥大学物理与天文系）；The Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；Eureka Scientific, Inc.（尤里卡科学公司）；NASA Ames Research Center（NASA艾姆斯研究中心）；School of Physics, University of Bristol（布里斯托尔大学物理学院）
Annabella Meech, Peter Gao, Nicole L. Wallack, Mercedes López-Morales, Dominic Oddo, Johanna Teske, Diana Dragomir, Angie Wolfgang, Nicholas Wogan, Hannah R. Wa… 展开作者
Annabella Meech, Peter Gao, Nicole L. Wallack, Mercedes López-Morales, Dominic Oddo, Johanna Teske, Diana Dragomir, Angie Wolfgang, Nicholas Wogan, Hannah R. Wakeford, Sarah E. Moran, James Kirk, Tyler A. Gordon, Anna Gagnebin, Natasha E. Batalha, Natalie M. Batalha, Lili Alderson, Munazza K. Alam, Artyom Aguichine
备注：
29 pages, 20 figures. Accepted for publication in AJ
We present a JWST/NIRSpec G395H transmission spectrum of TOI-260 b, a $T_\mathrm{eq}\sim 490$ K, $R_\mathrm{p} = 1.76\,R_\oplus$ planet. The transmission spectrum is derived by combining two transit observations, collected as part of the JWST COMPASS program. We achieved the same median transit depth precision of 37 ppm in both visits, and a median precision of 26 ppm when combining the spectroscopic light curves from the two visits. Implementing a 30-pixel-wide ($R\sim 200$) spectroscopic binning scheme, we find that the transmission spectrum is mostly featureless, with a possible feature around 3.17 $μ$m. We assess the significance of any features in the transmission spectrum with a suite of non-parametric models, which confirm the presence of a potential feature in the NRS1 bandpass and an offset between the NRS1 and NRS2 detectors. To investigate the atmospheric composition of TOI-260 b, we run a series of PLATON retrievals. We do not detect any clear molecular signatures, but the combined data from the two visits are sufficient to constrain the atmospheric metallicity to greater than $200\times$ solar, assuming no opaque deck $\lesssim2.5$ mbar. We also investigate causes of the potential feature near 3.17 $μ$m; while we find some compatible gaseous species and cannot fully discard an astrophysical origin, we suspect a systematics origin due to the variance in strength and position of the feature. Overall, this look at TOI-260 b adds to the small sample of radius-valley planets, which already seem to show a diversity in their atmospheric compositions. Determining the true nature of these enigmatic planets will require a larger telescope time investment.
The Hot Neptune Initiative (HONEI) III. An ultra-hot super Neptune orbiting the metal-rich subgiant star TOI-5646: the largest host for a desert dweller
University of Rome “Tor Vergata”（罗马第二大学）；INAF – Turin Astrophysical Observatory（意大利国家天体物理研究所都灵天文台）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；University of Bern（伯尔尼大学）；Leiden University（莱顿大学）；INAF – Astronomical Observatory of Rome（意大利国家天体物理研究所罗马天文台）
JWST NIRSpec G395H Transmission Spectra of Two Similar Sub-Neptunes in the TOI-125 System
Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Oxford（牛津大学）；Cavendish Laboratory, JJ Thomson Avenue, Cambridge CB3 0HE, UK（剑桥大学卡文迪许实验室）；University of California San Diego（加利福尼亚大学圣地亚哥分校）
JWST NIRSpec finds no clear signs of an atmosphere on TOI-1685 b
University of Oxford（牛津大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Bern（伯尔尼大学）；Ludwig Maximilian University（慕尼黑大学）；ARTORG Center for Biomedical Engineering Research, University of Bern（伯尔尼大学ARTORG生物医学工程研究中心）；University College London（伦敦大学学院）；University of Warwick（华威大学）；Johns Hopkins University（约翰斯·霍普金斯大学）
Transmission Spectrum of the Benchmark Temperate Exo-Neptune TOI-1231 b
School of Physics and Astronomy, Cardiff University（卡迪夫大学物理与天文学学院）；Institute of Astronomy, University of Cambridge（剑桥大学天文研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Space Science Institute（空间科学研究所）
Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；The Pennsylvania State University（宾夕法尼亚州立大学）；The University of Chicago（芝加哥大学）；Arizona State University（亚利桑那州立大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Carnegie Institution for Science（卡内基科学机构）
Magma ocean interactions can explain JWST observations of the sub-Neptune TOI-270 d
School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Department of Astronomy, University of Maryland（马里兰大学天文学系）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Astronomy & Astrophysics, University of Chicago（芝加哥大学天文学与天体物理学系）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Earth and Planets Laboratory, Carnegie Institution for Science（卡内基科学学会地球与行星实验室）
GEMS JWST: Transmission spectroscopy of TOI-5205b reveals significant stellar contamination and a metal-poor atmosphere
NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Johns Hopkins APL（约翰斯·霍普金斯大学应用物理实验室）；University of California, Riverside（加州大学河滨分校）；University of Zürich（苏黎世大学）；Carnegie Science（卡内基科学研究所）
GEMS JWST: A sub-Solar metallicity atmosphere for giant planet TOI-5293Ab orbiting a rapidly changing M-dwarf
Carnegie Science（卡内基科学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Johns Hopkins APL（约翰斯·霍普金斯大学应用物理实验室）；University of Maryland, College Park（马里兰大学帕克分校）；University of Zürich（苏黎世大学）
JWST COMPASS: NIRSpec/G395H Transmission Observations of the Sub-Neptune HD 15337 c
Carnegie Institution for Science（卡内基科学研究所）；California Institute of Technology（加州理工学院）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Space Telescope Science Institute（太空望远镜科学研究所）；Cornell University（康奈尔大学）；NASA Ames Research Center（美国国家航空航天局艾姆斯研究中心）
A Panchromatic JWST Spectrum of a Giant Starspot on the Fully Convective M-dwarf TOI-3884
University of Colorado Boulder（科罗拉多大学博尔德分校）；Flatiron Institute（平顿研究所）；Massachusetts Institute of Technology（麻省理工学院）；Michigan State University（密歇根州立大学）；Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité（巴黎天文台，PSL大学，法国国家科学研究中心，索邦大学，巴黎西岱大学）；Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS（波尔多天体物理学实验室，波尔多大学，法国国家科学研究中心）；Hobart and William Smith Colleges（霍巴特和威廉史密斯学院）；The Pennsylvania State University（宾夕法尼亚州立大学）；University of Tampa（坦帕大学）；Arizona State University（亚利桑那州立大学）；University of Birmingham（伯明翰大学）；Université de Liège（列日大学）；Instituto de Astrofísica de Canarias (IAC)（加那利群岛天体物理研究所）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Carnegie Institution for Science（卡内基科学机构）；Tata Institute of Fundamental Research（塔塔基础研究所）
Diversity in the haziness and chemistry of temperate sub-Neptunes
University of California, Los Angeles（加州大学洛杉矶分校）；University of Oxford（牛津大学）；University of Chicago（芝加哥大学）；McGill University（麦吉尔大学）；University of Waterloo（滑铁卢大学）；NRC Herzberg Astronomy and Astrophysics（国家研究委员会赫茨伯格天文学和天体物理学研究所）；University of Victoria（维多利亚大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Cornell University（康奈尔大学）；University of Michigan（密歇根大学）；University of St Andrews（圣安德鲁斯大学）
Evidence for LP 890-9d via Transit Timing Variations
Johns Hopkins Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）；Johns Hopkins University（约翰斯·霍普金斯大学）；University of Bristol（布里斯托大学）；Nevada Center for Astrophysics, University of Nevada, Las Vegas（内华达大学拉斯维加斯分校天体物理学中心）；Department of Physics and Astronomy, University of Nevada, Las Vegas（内华达大学拉斯维加斯分校物理与天文系）；Astronomy Department and Virtual Planetary Laboratory, University of Washington（华盛顿大学天文学系与虚拟行星实验室）
