TKS III: A Stellar Obliquity Measurement of TOI-1726 c
Fei Dai, Arpita Roy, Benjamin Fulton, Paul Robertson, Lea Hirsch, Howard Isaacson, Simon Albrecht, Andrew W. Mann, Martti H. Kristiansen, Natalie M. Batalha, Co… 展开作者
Fei Dai, Arpita Roy, Benjamin Fulton, Paul Robertson, Lea Hirsch, Howard Isaacson, Simon Albrecht, Andrew W. Mann, Martti H. Kristiansen, Natalie M. Batalha, Corey Beard, Aida Behmard, Ashley Chontos, Ian J. M. Crossfield, Paul A. Dalba, y Courtney Dressing, Steven Giacalone, Michelle Hill, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Mocnik, Joseph M. Akana Murphy, Erik A. Petigura, Lee Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Lauren M. Weiss, Judah Van Zandt, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Douglas A. Caldwell, David Charbonneau, Tansu Daylan, Maximilian N. Günther, Edward Morgan, Samuel N. Quinn, Mark E. Rose, Jeffrey C. Smith
We report the measurement of a spectroscopic transit of TOI-1726 c, one of two planets transiting a G-type star with $V$ = 6.9 in the Ursa Major Moving Group ($\sim$400 Myr). With a precise age constraint from cluster membership, TOI-1726 provides a great opportunity to test various obliquity excitation scenarios that operate on different timescales. By modeling the Rossiter-McLaughlin (RM) effect, we derived a sky-projected obliquity of $-1^{+35}_{-32}~^{\circ}$. This result rules out a polar/retrograde orbit; and is consistent with an aligned orbit for planet c. Considering the previously reported, similarly prograde RM measurement of planet b and the transiting nature of both planets, TOI-1726 tentatively conforms to the overall picture that compact multi-transiting planetary systems tend to have coplanar, likely aligned orbits. TOI-1726 is also a great atmospheric target for understanding differential atmospheric loss of sub-Neptune planets (planet b 2.2 $R_\oplus$ and c 2.7 $R_\oplus$ both likely underwent photoevaporation). The coplanar geometry points to a dynamically cold history of the system that simplifies any future modeling of atmospheric escape.
TOI-2076 b is a sub-Neptune-sized planet ($R= 2.39 \pm 0.10 {R_\oplus}$) that transits a young ($204 \pm 50 {MYr}$) bright ($V = 9.2$) K-dwarf hosting a system of three transiting planets. Using spectroscopic observations with the NEID spectrograph on the WIYN 3.5 m Telescope, we model the Rossiter-McLaughlin effect of TOI-2076 b, and derive a sky-projected obliquity of $λ=-3_{-15}^{+16\:\circ}$. Using the size of the star ($R=0.775 \pm0.015 {R_\odot}$), and the stellar rotation period ($P_{\mathrm{rot}}=7.27\pm0.23$ days), we estimate an obliquity of $ψ=18_{-9}^{+10\:\circ}$ ($ψ< 34^\circ$ at…
Mapping the orbital obliquity distribution of young planets is one avenue towards understanding mechanisms that sculpt the architectures of planetary systems. TOI-942 is a young field star, with an age of ~60 Myr, hosting a planetary system consisting of two transiting Neptune-sized planets in 4.3- and 10.1-day period orbits. We observed the spectroscopic transits of the inner Neptune TOI-942b to determine its projected orbital obliquity angle. Through two partial transits, we find the planet to be in a prograde orbit, with a projected obliquity angle of |lambda| = 1/+41-33 deg. In addition, i…
Close-in gas giants present a surprising range of stellar obliquity, the angle between a planet's orbital axis and its host star's spin axis. It is unclear whether the obliquities reflect the planets' dynamical history (e.g., aligned for in situ formation or disk migration versus misaligned for high-eccentricity tidal migration) or whether other mechanisms (e.g., primordial misalignment or planet-star interactions) are more important in sculpting the obliquity distribution. Here we present the stellar obliquity measurement of TOI-1268 (TIC-142394656, $V_{\rm mag} {\sim} 10.9$), a young K-type …
TOI-1259Ab: A Warm Jupiter Orbiting a K-dwarf White-Dwarf Binary is on a Well-aligned Orbit
University of Amsterdam（阿姆斯特丹大学）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Millennium Institute for Astrophysics（天体物理学千年研究所）；Vanderbilt University（范德堡大学）；Tufts University（塔夫茨大学）；The Pennsylvania State University（宾夕法尼亚州立大学）；Princeton University（普林斯顿大学）；University of Pennsylvania（宾夕法尼亚大学）
Understanding eccentric temperate giants: an in-depth study of the architecture and stellar obliquity of the TOI-2134 system
University of Birmingham（伯明翰大学）；Université de Liège（列日大学）；Flatiron Institute（平顿研究所）；Max Planck Institut für Astronomie（马克斯·普朗克天文学研究所）；University of Warwick（华威大学）
Ultra-hot Jupiters are defined as giant planets with equilibrium temperatures larger than 2000 K. Most of them are found orbiting bright A-F type stars, making them extremely suitable objects to study their atmospheres using high-resolution spectroscopy. Recent studies show a variety of atoms and molecules detected in the atmospheres of this type of planets. Here we present our analysis of the newly discovered ultra-hot Jupiter TOI-1431b/MASCARA-5b, using two transit observations with the HARPS-N spectrograph and one transit observation with the EXPRES spectrograph. Analysis of the Rossiter-Mc…
A dozen short-period detached binaries are known to host transiting circumbinary planets. In all circumbinary systems so far, the planetary and binary orbits are aligned within a couple of degrees. However, the obliquity of the primary star, which is an important tracer of their formation, evolution, and tidal history, has only been measured in one circumbinary system until now. EBLM J0608-59/TOI-1338 is a low-mass eclipsing binary system with a recently discovered circumbinary planet identified by TESS. Here, we perform high-resolution spectroscopy during primary eclipse to measure the projec…
The 35-Myr old infant planet TOI-837 b has a mildly misaligned orbit
Centro di Ateneo di Studi e Attività Spaziali “G. Colombo” – Università degli Studi di Padova（帕多瓦大学太空研究与活动中心“G. Colombo”）；INAF – Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Dipartimento di Fisica e Astronomia “Galileo Galilei”, Università di Padova（帕多瓦大学伽利略·伽利雷物理与天文学系）；Dipartimento di Fisica e Astronomia, Università di Padova（帕多瓦大学物理与天文学系）；INAF – Osservatorio Astrofisico di Catania（意大利国家天体物理研究所卡塔尼亚天文台）；INAF – Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；INAF – Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；INAF – Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）
Spin-Orbit Alignment of Two Neptune-size Planets Younger than 500 Myr: TOI-560 b and TOI-5082 b
Institute for Astronomy, University of Hawaii（夏威夷大学天文研究所）；Department of Astronomy, California Institute of Technology（加州理工学院天文学系）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Department of Astronomy, University of California Berkeley（加州大学伯克利分校天文学系）；Center for Computational Astrophysics, Flatiron Institute（西蒙斯基金会平顿研究所计算天体物理中心）；Korea Astronomy and Space Science Institute（韩国天文与空间科学研究院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Department of Astronomy, Indiana University（印第安纳大学天文学系）
The KPF-SLOPE Survey - Small, Compact Multi-Planet Systems Appear Spin-Orbit Aligned
California Institute of Technology（加州理工学院）；University of Hawai‘i（夏威夷大学）；Flatiron Institute（平顿研究所）；University of California Berkeley（加州大学伯克利分校）；University of Sydney（悉尼大学）
TOI-640 b is a hot, puffy Jupiter with a mass of $0.57 \pm 0.02$ M$_{\rm J}$ and radius of $1.72 \pm 0.05$ R$_{\rm J}$, orbiting a slightly evolved F-type star with a separation of $6.33^{+0.07}_{-0.06}$ R$_\star$. Through spectroscopic in-transit observations made with the HARPS spectrograph, we measured the Rossiter-McLaughlin effect, analysing both in-transit radial velocities and the distortion of the stellar spectral lines. From these observations, we find the host star to have a projected obliquity of $λ=184\pm3^\circ$. From the TESS light curve, we measured the stellar rotation period, …
HARPS-N Reveals a Well-aligned Orbit for the Highly Eccentric Warm Jupiter TOI-4127 b
The University of New Mexico（新墨西哥大学）；Instituto de Astrofísica de Canarias (IAC)（加那利天体物理研究所）；Universidad de La Laguna (ULL)（拉帕鲁纳大学）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；INAF – Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）
We present the discovery of two nearly identically-sized sub-Neptune transiting planets orbiting HD 63935, a bright ($V=8.6$ mag), sun-like ($T_{eff}=5560K$) star at 49 pc. TESS identified the first planet, HD 63935 b (TOI-509.01), in Sectors 7 and 34. We identified the second signal (HD 63935 c) in Keck HIRES and Lick APF radial velocity data as part of our followup campaign. It was subsequently confirmed with TESS photometry in Sector 34 as TOI-509.02. Our analysis of the photometric and radial velocity data yields a robust detection of both planets with periods of $9.0600 \pm 0.007$ and $21…
An Aligned Very-Low-Mass Star Orbiting an M dwarf and Obliquity Patterns Across Giant Planets, Brown Dwarfs, and Binary Stars
Westlake University（西湖大学）；Université de Montréal（蒙特利尔大学）；Observatoire du Mont-Mégantic, Université de Montréal（蒙特利尔大学马格尼克天文台）；Université de Genève（日内瓦大学）；Observatoire de Genève, Département d’Astronomie, Université de Genève（日内瓦大学天文学系日内瓦天文台）
CHIANTE I: Obliquity Measurements of Four High-Priority Ariel Targets in Binaries
Lowell Observatory（洛厄尔天文台）；Yale University（耶鲁大学）；University of Michigan（密歇根大学）；Flatiron Institute, Simons Foundation（平托研究所，西蒙斯基金会）；San Francisco State University（旧金山州立大学）；Northern Arizona University（北亚利桑那大学）；McDonald Observatory, University of Texas at Austin（麦克唐纳天文台，德克萨斯大学奥斯汀分校）
We confirm the planetary nature of two gas giants discovered by TESS to transit M dwarfs. TOI-3714 ($V=15.24,~J=11.74$) is an M2 dwarf hosting a hot Jupiter ($M_p=0.70 \pm 0.03~\mathrm{M_J}$ and $R_p=1.01 \pm 0.03~\mathrm{R_J}$) on an orbital period of $2.154849 \pm 0.000001$ days with a resolved white dwarf companion. TOI-3629 ($V=14.63,~J=11.42$) is an M1 dwarf hosting a hot Jupiter ($M_p=0.26 \pm 0.02~\mathrm{M_J}$ and $R_p=0.74 \pm 0.02~\mathrm{R_J}$) on an orbital period of $3.936551_{-0.000006}^{+0.000005}$ days. We characterize each transiting companion using a combination of ground-bas…
We report the discovery of TOI 837b and its validation as a transiting planet. We characterize the system using data from the NASA TESS mission, the ESA Gaia mission, ground-based photometry from El Sauce and ASTEP400, and spectroscopy from CHIRON, FEROS, and Veloce. We find that TOI 837 is a $T=9.9$ mag G0/F9 dwarf in the southern open cluster IC 2602. The star and planet are therefore $35^{+11}_{-5}$ million years old. Combining the transit photometry with a prior on the stellar parameters derived from the cluster color-magnitude diagram, we find that the planet has an orbital period of $8.3…
We report the confirmation and characterisation of TOI-1820~b, TOI-2025~b, and TOI-2158~b, three Jupiter-sized planets on short-period orbits around G-type stars detected by TESS. Through our ground-based efforts using the FIES and Tull spectrographs, we have confirmed these planets and characterised their orbits, and find periods of around $4.9$~d, $8.9$~d, and $8.6$~d for TOI-1820~b, TOI-2025~b, and TOI-2158~b, respectively. The sizes of the planets range from 0.96 to 1.14 Jupiter radii, and their masses are in the range from 0.8 to 4.4 Jupiter masses. For two of the systems, namely TOI-2025…
We report the discovery of a $M=67\pm2~\mathrm{M_J}$ brown dwarf transiting the early M dwarf TOI-2119 on an eccentric orbit ($e=0.3362 \pm 0.0005$) at an orbital period of $7.200861 \pm 0.000005$ days. We confirm the brown dwarf nature of the transiting companion using a combination of ground-based and space-based photometry and high-precision velocimetry from the Habitable-zone Planet Finder. Detection of the secondary eclipse with TESS photometry enables a precise determination of the eccentricity and reveals the brown dwarf has a brightness temperature of $2100\pm80$ K, a value which is co…
A tidally detached super Neptune on a strongly misaligned retrograde orbit
Centro di Ateneo di Studi e Attività Spaziali “G. Colombo” – Università degli Studi di Padova（帕多瓦大学太空研究与活动中心“G. Colombo”）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Dipartimento di Fisica e Astronomia “Galileo Galilei”, Università di Padova（帕多瓦大学伽利略·伽利雷物理与天文学系）；INAF - Osservatorio Astrofisico di Catania（意大利国家天体物理研究所卡塔尼亚天文台）；Dipartimento di Fisica e Astronomia, Università di Padova（帕多瓦大学物理与天文学系）；INAF - Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Fundación Galileo Galilei-INAF（伽利略·伽利雷基金会-INAF）；INAF - Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）
Princeton University（普林斯顿大学）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Millennium Institute for Astrophysics（天体物理学千年研究所）；Universidad Adolfo Ibáñez（阿道夫·伊巴涅斯大学）；Indiana University（印第安纳大学）；Data Observatory Foundation（数据观测基金会）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）
