TOI 122b and TOI 237b: Two Small Warm Planets Orbiting Inactive M Dwarfs Found by TESS

  title={TOI 122b and TOI 237b: Two Small Warm Planets Orbiting Inactive M Dwarfs Found by TESS},
  author={W. C. Waalkes and Zachory K. Berta-Thompson and Karen A. Collins and Adina D. Feinstein and Benjamin M. Tofflemire and B{\'a}rbara Rojas-Ayala and Michele L. Silverstein and Elisabeth R. Newton and George R. Ricker and Roland K. Vanderspek and David W. Latham and Sara Seager and Joshua N. Winn and Jon M. Jenkins and Jessie L. Christiansen and Robert F. Goeke and Alan M. Levine and Hugh Osborn and Stephen Andrew Rinehart and Mark E. Rose and Eric B. Ting and Joseph D. Twicken and Khalid Barkaoui and Jacob L. Bean and C{\'e}sar Brice{\~n}o and David R. Ciardi and Kevin I. Collins and Dennis M. Conti and Tianjun Gan and Micha{\"e}l Gillon and G. Isopi and Emmanuel Jehin and Eric L. N. Jensen and John F. Kielkopf and Nicholas M. Law and Franco Mallia and Andrew W. Mann and Benjamin T. Montet and Francisco J. Pozuelos and Howard M. Relles and Jessica E. Libby-Roberts and Carl A. Ziegler},
  journal={arXiv: Earth and Planetary Astrophysics},
We report the discovery and validation of TOI 122b and TOI 237b, two warm planets transiting inactive M dwarfs observed by \textit{TESS}. Our analysis shows TOI 122b has a radius of 2.72$\pm$0.18 R$_\rm{e}$ and receives 8.8$\pm$1.0$\times$ Earth's bolometric insolation, and TOI 237b has a radius of 1.44$\pm$0.12 R$_\rm{e}$ and receives 3.7$\pm$0.5$\times$ Earth insolation, straddling the 6.7$\times$ Earth insolation that Mercury receives from the sun. This makes these two of the cooler planets… 
5 Citations
The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
We present the Transiting Exoplanet Survey Satellite (TESS) discovery of the LHS 1678 (TOI-696) exoplanet system, comprised of two approximately Earth-sized transiting planets and a likely
Characterization of 92 southern TESS candidate planet hosts and a new photometric [Fe/H] relation for cool dwarfs
We present the results of a medium resolution optical spectroscopic survey of 92 cool (3, 000 . Teff . 4, 500K) southern TESS candidate planet hosts, and describe our spectral fitting methodology
NEMESIS: Exoplanet Transit Survey of Nearby M-dwarfs in TESS FFIs. I.
In this work, we present an analysis of 33,054 M-dwarf stars, located within 100 parsecs, via the Transiting Exoplanet Survey Satellite (TESS) full-frame images (FFIs) of observed sectors 1–5. We
New Perspectives on the Exoplanet Radius Gap from a Mathematica Tool and Visualized Water Equation of State
Recent astronomical observations obtained with the Kepler and TESS missions and their related ground-based follow-ups revealed an abundance of exoplanets with a size intermediate between Earth and
The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars
Accurate stellar properties are essential for precise stellar astrophysics and exoplanetary science. In the M-dwarf regime, much effort has gone into defining empirical relations that can use readily


A super-Earth and two sub-Neptunes transiting the nearby and quiet M dwarf TOI-270
One of the primary goals of exoplanetary science is to detect small, temperate planets passing (transiting) in front of bright and quiet host stars. This enables the characterization of planetary
The cosmic shoreline: the evidence that escape determines which planets have atmospheres, and what this may mean for Proxima Centauri b
The planets of the Solar System divide neatly between those with atmospheres and those without when arranged by insolation ($I$) and escape velocity ($v_{\mathrm{esc}}$). The dividing line goes as $I
The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf
We report the Transiting Exoplanet Survey Satellite (TESS) discovery of three terrestrial-sized planets transiting L 98-59 (TOI-175, TIC 307210830) -- a bright M dwarf at a distance of 10.6 pc. Using
A Super-Earth and Sub-Neptune Transiting the Late-type M Dwarf LP 791-18
Planets occur most frequently around cool dwarfs, but only a handful of specific examples are known to orbit the latest-type M stars. Using TESS photometry, we report the discovery of two planets
Planets Around Low-Mass Stars (PALMS). IV. The Outer Architecture of M Dwarf Planetary Systems
We present results from a high-contrast adaptive optics imaging search for giant planets and brown dwarfs (>1 MJup) around 122 newly identified nearby (<40 pc) young M dwarfs. Half of our targets are
Predicted Number, Multiplicity, and Orbital Dynamics of TESS M-dwarf Exoplanets
  • S. Ballard
  • Physics, Geology
    The Astronomical Journal
  • 2019
We present a study of the M dwarf exoplanetary systems forthcoming from NASA's TESS mission. While the mission's footprint is too complex to be characterized by a single detection completeness, we
Planetary system around the nearby M dwarf GJ 357 including a transiting, hot, Earth-sized planet optimal for atmospheric characterization
We report the detection of a transiting Earth-size planet around GJ 357, a nearby M2.5 V star, using data from the Transiting Exoplanet Survey Satellite (TESS). GJ 357 b (TOI-562.01) is a transiting,
Characterization of the L 98-59 multi-planetary system with HARPS
Aims.L 98-59 (TIC 307210830, TOI-175) is a nearby M3 dwarf around which TESS revealed three small transiting planets (0.80, 1.35, 1.57 Earth radii) in a compact configuration with orbital periods
The Transiting Exoplanet Survey Satellite: Simulations of planet detections and astrophysical false positives
The Transiting Exoplanet Survey Satellite (TESS) is a NASA-sponsored Explorer mission that will perform a wide-field survey for planets that transit bright host stars. Here, we predict the properties
TESS Discovery of an Ultra-short-period Planet around the Nearby M Dwarf LHS 3844
Data from the newly commissioned Transiting Exoplanet Survey Satellite has revealed a "hot Earth" around LHS 3844, an M dwarf located 15 pc away. The planet has a radius of 1.303 ± 0.022 R⊕ and