@article{vines_ngts-31b_2025,

title = {NGTS-31b and NGTS-32b: two inflated hot Jupiters orbiting subgiant stars},

author = {Jose I Vines and James S Jenkins and David R Anderson and Douglas R Alves and Maximiliano Moyano and Jack S Acton and Ioannis Apergis and Khalid Barkaoui and Daniel Bayliss and Francois Bouchy and Edward M Bryant and Matthew R Burleigh and Sarah L Casewell and Jessie L Christiansen and Karen A Collins and Philipp Eigm\"{u}ller and Ben Falk and Samuel Gill and Edward Gillen and Michael R Goad and Maximilian N G\"{u}nther and Beth A Henderson and Alicia Kendall and Monika Lendl and James McCormac and Louise D Nielsen and Ares Osborn and Gavin Ramsay and George R Ricker and Pamela Rowden and Alexander Rudat and Suman Saha and Sara Seager and Alexis M S Smith and Thiam-Guan Tan and Rosanna H Tilbrook and St\'{e}phane Udry and Richard West and Peter J Wheatley and Joshua N Winn and Tafadzwa Zivave},

url = {https://doi.org/10.1093/mnras/stae2616},

doi = {10.1093/mnras/stae2616},

issn = {0035-8711},

year  = {2025},

date = {2025-01-01},

urldate = {2025-01-28},

journal = {Monthly Notices of the Royal Astronomical Society},

volume = {536},

number = {3},

pages = {2011\textendash2024},

abstract = {We present the discoveries of NGTS-31b(= TOI-2721), and NGTS-32b, two hot Jupiters from the Next Generation Transit Survey (NGTS) transiting slightly evolved stars. The orbital periods, radii, and masses are 4.16 and 3.31 d, 1.61 and 1.42 $R_J$, and 1.12 and 0.57 $M_J$, respectively. Both planets have an incident stellar flux significantly above the threshold where inflation occurs, with both planets showing signs of inflation. These planets have widely different equilibrium temperatures than other hot Jupiters of similar mass and radius, with NGTS-31b having a significantly lower temperature, and NGTS-32b being hotter. This dichotomy raises the question of how prevalent the roles of other inflation mechanisms are in the radius anomaly phenomena and will help further constrain different inflationary models.},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{cointepas_toi-663_2024,

title = {TOI-663: A newly discovered multi-planet system with three transiting mini-Neptunes orbiting an early M star},

author = {M. Cointepas and F. Bouchy and J. M. Almenara and X. Bonfils and N. Astudillo-Defru and H. Knierim and M. Stalport and L. Mignon and N. Grieves and J. Bean and M. Brady and J. Burt and B. L. Canto Martins and K. A. Collins and K. I. Collins and X. Delfosse and J. R. de Medeiros and B. -O. Demory and C. Dorn and T. Forveille and A. Fukui and T. Gan and Y. G\'{o}mez Maqueo Chew and S. Halverson and R. Helled and I. Helm and T. Hirano and K. Horne and S. B. Howell and K. Isogai and D. Kasper and K. Kawauchi and J. H. Livingston and B. Massey and R. A. Matson and F. Murgas and N. Narita and E. Palle and H. M. Relles and L. Sabin and N. Schanche and R. P. Schwarz and A. Seifahrt and A. Shporer and G. Stefansson and J. Sturmer and M. Tamura and T. -G. Tan and J. D. Twicken and N. Watanabe and R. D. Wells and F. P. Wilkin and G. R. Ricker and S. Seager and J. N. Winn and J. M. Jenkins},

url = {https://www.aanda.org/articles/aa/abs/2024/05/aa46899-23/aa46899-23.html},

doi = {10.1051/0004-6361/202346899},

issn = {0004-6361, 1432-0746},

year  = {2024},

date = {2024-05-01},

urldate = {2024-06-12},

journal = {A\&A},

volume = {685},

pages = {A19},

abstract = {We present the detection of three exoplanets orbiting the early M dwarf TOI-663 (TIC 54962195; \textit{V\<i/\> = 13.7 mag, \textit{J\<i/\> = 10.4 mag, \textit{R\<i/\>_{★\<sub/\> = 0.512 ± 0.015 \textit{R\<i/\>_{⊙\<sub/\>, \textit{M\<i/\>_{★\<sub/\> = 0.514 ± 0.012 \textit{M\<i/\>_{⊙\<sub/\>, \textit{d\<i/\> = 64 pc). TOI-663 b, c, and d, with respective radii of 2.27 ± 0.10 \textit{R\<i/\>_{⊕\<sub/\>, 2.26 ± 0.10 \textit{R\<i/\>_{⊕\<sub/\>, and 1.92 ± 0.13 \textit{R\<i/\>_{⊕\<sub/\> and masses of 4.45 ± 0.65 \textit{M\<i/\>_{⊕\<sub/\>, 3.65 ± 0.97 \textit{M\<i/\>_{⊕\<sub/\>, and \<5.2 \textit{M\<i/\>_{⊕\<sub/\> at 99%, are located just above the radius valley that separates rocky and volatile-rich exoplanets. The planet candidates are identified in two TESS sectors and are validated with ground-based photometric follow-up, precise radial-velocity measurements, and high-resolution imaging. We used the software package juliet to jointly model the photometric and radial-velocity datasets, with Gaussian processes applied to correct for systematics. The three planets discovered in the TOI-663 system are low-mass mini-Neptunes with radii significantly larger than those of rocky analogs, implying that volatiles, such as water, must predominate. In addition to this internal structure analysis, we also performed a dynamical analysis that confirmed the stability of the system. The three exoplanets in the TOI-663 system, similarly to other sub-Neptunes orbiting M dwarfs, have been found to have lower densities than planets of similar sizes orbiting stars of different spectral types.},

note = {Publisher: EDP Sciences},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{castro-gonzalez_toi-5005_2024,

title = {TOI-5005 b: A super-Neptune in the savanna near the ridge},

author = {A. Castro-Gonz\'{a}lez and J. Lillo-Box and D. J. Armstrong and L. Acu\~{n}a and A. Aguichine and V. Bourrier and S. Gandhi and S. G. Sousa and E. Delgado-Mena and A. Moya and V. Adibekyan and A. C. M. Correia and D. Barrado and M. Damasso and J. N. Winn and N. C. Santos and K. Barkaoui and S. C. C. Barros and Z. Benkhaldoun and F. Bouchy and C. Brice\~{n}o and D. A. Caldwell and K. A. Collins and Z. Essack and M. Ghachoui and M. Gillon and R. Hounsell and E. Jehin and J. M. Jenkins and M. A. F. Keniger and N. Law and A. W. Mann and L. D. Nielsen and F. J. Pozuelos and N. Schanche and S. Seager and T. -G. Tan and M. Timmermans and J. Villase\~{n}or and C. N. Watkins and C. Ziegler},

url = {http://arxiv.org/abs/2409.18129},

doi = {10.1051/0004-6361/202451656},

issn = {0004-6361, 1432-0746},

year  = {2024},

date = {2024-11-01},

urldate = {2025-01-28},

journal = {A\&A},

volume = {691},

pages = {A233},

abstract = {The Neptunian desert and savanna have been recently found to be separated by a ridge, an overdensity of planets in the $textbackslashsimeq$3-5 days period range. These features are thought to be shaped by dynamical and atmospheric processes. However, their relative roles are not yet well understood. We intend to confirm and characterise the super-Neptune TESS candidate TOI-5005.01, which orbits a moderately bright (V = 11.8) solar-type star (G2 V) with an orbital period of 6.3 days. We confirm TOI-5005 b to be a transiting super-Neptune with a radius of $R_textbackslashrm p$ = $6.25textbackslashpm 0.24$ $textbackslashrm R_textbackslashrm textbackslashoplus$ ($R_textbackslashrm p$ = $0.558textbackslashpm 0.021$ $textbackslashrm R_textbackslashrm J$) and a mass of $M_textbackslashrm p$ = $32.7textbackslashpm 5.9$ $textbackslashrm M_textbackslashoplus$ ($M_textbackslashrm p$ = $0.103textbackslashpm 0.018$ $textbackslashrm M_textbackslashrm J$), which corresponds to a mean density of $textbackslashrho_textbackslashrm p$ = $0.74 textbackslashpm 0.16$ $textbackslashrm g textbackslash, cmˆ-3$. Our internal structure modelling indicates that the overall metal mass fraction is well constrained to a value slightly lower than that of Neptune and Uranus ($Z_textbackslashrm planet$ = $0.76ˆ+0.04_-0.11$). We also estimated the present-day atmospheric mass-loss rate of TOI-5005 b but found contrasting predictions depending on the choice of photoevaporation model. At a population level, we find statistical evidence ($p$-value = $0.0092ˆ+0.0184_-0.0066$) that planets in the savanna such as TOI-5005 b tend to show lower densities than planets in the ridge, with a dividing line around 1 $textbackslashrm g textbackslash, cmˆ-3$, which supports the hypothesis of different evolutionary pathways populating both regimes. TOI-5005 b is located in a key region of the period-radius space to study the transition between the Neptunian ridge and the savanna. It orbits the brightest star of all such planets, which makes it a target of interest for atmospheric and orbital architecture observations that will bring a clearer picture of its overall evolution.},

note = {arXiv:2409.18129 [astro-ph]},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{wu_first_2024,

title = {First Resolution of Microlensed Images of a Binary-Lens Event},

author = {Zexuan Wu and Subo Dong and A. M\'{e}rand and Christopher S. Kochanek and Przemek Mr\'{o}z and Jinyi Shangguan and Grant Christie and Thiam-Guan Tan and Thomas Bensby and Joss Bland-Hawthorn and Sven Buder and Frank Eisenhauer and Andrew P. Gould and Janez Kos and Tim Natusch and Sanjib Sharma and Andrzej Udalski and J. Woillez and David A. H. Buckley and I. B. Thompson and Karim Abd El Dayem and Anthony Berdeu and Jean-Philippe Berger and Guillaume Bourdarot and Wolfgang Brandner and Richard I. Davies and Denis Defr\`{e}re and Catherine Dougados and Antonia Drescher and Andreas Eckart and Maximilian Fabricius and Helmut Feuchtgruber and Natascha M. F\"{o}rster Schreiber and Paulo Garcia and Reinhard Genzel and Stefan Gillessen and Gernot Hei\ssel and Sebastian H\"{o}nig and Mathis Houlle and Pierre Kervella and Laura Kreidberg and Sylvestre Lacour and Olivier Lai and Romain Laugier and Jean-Baptiste Le Bouquin and James Leftley and Bruno Lopez and Dieter Lutz and Felix Mang and Florentin Millour and Miguel Montarg\`{e}s and Hugo Nowacki and Mathias Nowak and Thomas Ott and Thibaut Paumard and Karine Perraut and Guy Perrin and Romain Petrov and Pierre-Olivier Petrucci and Nicolas Pourre and Sebastian Rabien and Diogo C. Ribeiro and Sylvie Robbe-Dubois and Matteo Sadun Bordoni and Daryl Santos and Jonas Sauter and Jules Scigliuto and Taro T. Shimizu and Christian Straubmeier and Eckhard Sturm and Matthias Subroweit and Calvin Sykes and Linda Tacconi and Fr\'{e}d\'{e}ric Vincent and Felix Widmann},

url = {http://arxiv.org/abs/2409.13015},

doi = {10.3847/1538-4357/ad90b9},

issn = {0004-637X, 1538-4357},

year  = {2024},

date = {2024-12-01},

urldate = {2025-01-28},

journal = {ApJ},

volume = {977},

number = {2},

pages = {229},

abstract = {We resolve the multiple images of the binary-lens microlensing event ASASSN-22av using the GRAVITY instrument of the Very Large Telescope Interferometer (VLTI). The light curves show weak binary-lens perturbations, complicating the analysis, but the joint modeling with the VLTI data breaks several degeneracies, arriving at a strongly favored solution. Thanks to precise measurements of angular Einstein radius textbackslashtheta_E = 0.724 +/- 0.002 mas and microlens parallax, we determine that the lens system consists of two M dwarfs with masses of M_1 = 0.258 +/- 0.008 M_sun and M_2 = 0.130 +/- 0.007 M_sun, a projected separation of r_textbackslashperp = 6.83 +/- 0.31 au and a distance of D_L = 2.29 +/- 0.08 kpc. The successful VLTI observations of ASASSN-22av open up a new path for studying intermediate-separation (i.e., a few astronomical units) stellar-mass binaries, including those containing dark compact objects such as neutron stars and stellar-mass black holes.},

note = {arXiv:2409.13015 [astro-ph]},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{mantovan_inflated_2024,

title = {The inflated, eccentric warm Jupiter TOI-4914 b orbiting a metal-poor star, and the hot Jupiters TOI-2714 b and TOI-2981 b},

author = {G. Mantovan and T. G. Wilson and L. Borsato and T. Zingales and K. Biazzo and D. Nardiello and L. Malavolta and S. Desidera and F. Marzari and A. Collier Cameron and V. Nascimbeni and F. Z. Majidi and M. Montalto and G. Piotto and K. G. Stassun and J. N. Winn and J. M. Jenkins and L. Mignon and A. Bieryla and D. W. Latham and K. Barkaoui and K. A. Collins and P. Evans and M. M. Fausnaugh and V. Granata and V. Kostov and A. W. Mann and F. J. Pozuelos and D. J. Radford and H. M. Relles and P. Rowden and S. Seager and T. -G. Tan and M. Timmermans and C. N. Watkins},

url = {http://arxiv.org/abs/2409.07520},

doi = {10.1051/0004-6361/202451841},

issn = {0004-6361, 1432-0746},

year  = {2024},

date = {2024-11-01},

urldate = {2025-01-28},

journal = {A\&A},

volume = {691},

pages = {A67},

abstract = {Recent observations of giant planets have revealed unexpected bulk densities. Hot Jupiters, in particular, appear larger than expected for their masses compared to planetary evolution models, while warm Jupiters seem denser than expected. These differences are often attributed to the influence of the stellar incident flux, but could they also result from different planet formation processes? Is there a trend linking the planetary density to the chemical composition of the host star? In this work we present the confirmation of three giant planets in orbit around solar analogue stars. TOI-2714 b ($P textbackslashsimeq 2.5$ d, $R_textbackslashrm p textbackslashsimeq 1.22 R_textbackslashrm J$, $M_textbackslashrm p = 0.72 M_textbackslashrm J$) and TOI-2981 b ($P textbackslashsimeq 3.6$ d, $R_textbackslashrm p textbackslashsimeq 1.2 R_textbackslashrm J$, $M_textbackslashrm p = 2 M_textbackslashrm J$) are hot Jupiters on nearly circular orbits, while TOI-4914 b ($P textbackslashsimeq 10.6$ d, $R_textbackslashrm p textbackslashsimeq 1.15 R_textbackslashrm J$, $M_textbackslashrm p = 0.72 M_textbackslashrm J$) is a warm Jupiter with a significant eccentricity ($e = 0.41 textbackslashpm 0.02$) that orbits a star more metal-poor ([Fe/H]$textasciitilde= -0.13$) than most of the stars known to host giant planets. Our radial velocity (RV) follow-up with the HARPS spectrograph allows us to detect their Keplerian signals at high significance (7, 30, and 23$textbackslashsigma$, respectively) and to place a strong constraint on the eccentricity of TOI-4914 b (18$textbackslashsigma$). TOI-4914 b, with its large radius and low insolation flux ($F_textbackslashstar \< 2 textbackslashtimes 10ˆ8textasciitildetextbackslashrm ergtextasciitildesˆ-1textasciitildecmˆ-2$), appears to be more inflated than what is supported by current theoretical models for giant planets. Moreover, it does not conform to the previously noted trend that warm giant planets orbiting metal-poor stars have low eccentricities. This study thus provides insights into the diverse orbital characteristics and formation processes of giant exoplanets, in particular the role of stellar metallicity in the evolution of planetary systems.},

note = {arXiv:2409.07520 [astro-ph]},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{saunders_tess_2024,

title = {TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence},

author = {Nicholas Saunders and Samuel K. Grunblatt and Ashley Chontos and Fei Dai and Daniel Huber and Jingwen Zhang and Gudmundur Stefansson and Jennifer L. van Saders and Joshua N. Winn and Daniel Hey and Andrew W. Howard and Benjamin Fulton and Howard Isaacson and Corey Beard and Steven Giacalone and Judah van Zandt and Joseph M. Akana Murphey and Malena Rice and Sarah Blunt and Emma Turtelboom and Paul A. Dalba and Jack Lubin and Casey Brinkman and Emma M. Louden and Emma Page and Cristilyn N. Watkins and Karen A. Collins and Chris Stockdale and Thiam-Guan Tan and Richard P. Schwarz and Bob Massey and Steve B. Howell and Andrew Vanderburg and George R. Ricker and Jon M. Jenkins and Sara Seager and Jessie L. Christiansen and Tansu Daylan and Ben Falk and Max Brodheim and Steven R. Gibson and Grant M. Hill and Bradford Holden and Aaron Householder and Stephen Kaye and Russ R. Laher and Kyle Lanclos and Erik A. Petigura and Arpita Roy and Ryan A. Rubenzahl and Christian Schwab and Abby P. Shaum and Martin M. Sirk and Christopher L. Smith and Josh Walawender and Sherry Yeh},

url = {http://arxiv.org/abs/2407.21650},

doi = {10.3847/1538-3881/ad543b},

issn = {0004-6256, 1538-3881},

year  = {2024},

date = {2024-08-01},

urldate = {2025-01-28},

journal = {AJ},

volume = {168},

number = {2},

pages = {81},

abstract = {The degree of alignment between a star's spin axis and the orbital plane of its planets (the stellar obliquity) is related to interesting and poorly understood processes that occur during planet formation and evolution. Hot Jupiters orbiting hot stars ($textbackslashgtrsim$6250 K) display a wide range of obliquities, while similar planets orbiting cool stars are preferentially aligned. Tidal dissipation is expected to be more rapid in stars with thick convective envelopes, potentially explaining this trend. Evolved stars provide an opportunity to test the damping hypothesis, particularly stars that were hot on the main sequence and have since cooled and developed deep convective envelopes. We present the first systematic study of the obliquities of hot Jupiters orbiting subgiants that recently developed convective envelopes using Rossiter-McLaughlin observations. Our sample includes two newly discovered systems in the Giants Transiting Giants Survey (TOI-6029 b, TOI-4379 b). We find that the orbits of hot Jupiters orbiting subgiants that have cooled below $textbackslashsim$6250 K are aligned or nearly aligned with the spin-axis of their host stars, indicating rapid tidal realignment after the emergence of a stellar convective envelope. We place an upper limit for the timescale of realignment for hot Jupiters orbiting subgiants at $textbackslashsim$500 Myr. Comparison with a simplified tidal evolution model shows that obliquity damping needs to be $textbackslashsim$4 orders of magnitude more efficient than orbital period decay to damp the obliquity without destroying the planet, which is consistent with recent predictions for tidal dissipation from inertial waves excited by hot Jupiters on misaligned orbits.},

note = {arXiv:2407.21650 [astro-ph]},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{korth_toi-1130_2023,

title = {TOI-1130: A photodynamical analysis of a hot Jupiter in resonance with an inner low-mass planet},

author = {J. Korth and D. Gandolfi and J. \v{S}ubjak and S. Howard and S. Ataiee and K. A. Collins and S. N. Quinn and A. J. Mustill and T. Guillot and N. Lodieu and A. M. S. Smith and M. Esposito and F. Rodler and A. Muresan and L. Abe and S. H. Albrecht and A. Alqasim and K. Barkaoui and P. G. Beck and C. J. Burke and R. P. Butler and D. M. Conti and K. I. Collins and J. D. Crane and F. Dai and H. J. Deeg and P. Evans and S. Grziwa and A. P. Hatzes and T. Hirano and K. Horne and C. X. Huang and J. M. Jenkins and P. Kab\'{a}th and J. F. Kielkopf and E. Knudstrup and D. W. Latham and J. Livingston and R. Luque and S. Mathur and F. Murgas and H. L. M. Osborne and E. Pall\'{e} and C. M. Persson and J. E. Rodriguez and M. Rose and P. Rowden and R. P. Schwarz and S. Seager and L. M. Serrano and L. Sha and S. A. Shectman and A. Shporer and G. Srdoc and C. Stockdale and T. G. Tan and J. K. Teske and V. Van Eylen and A. Vanderburg and R. Vanderspek and S. X. Wang and J. N. Winn},

url = {http://arxiv.org/abs/2305.15565},

doi = {10.1051/0004-6361/202244617},

issn = {0004-6361, 1432-0746},

year  = {2023},

date = {2023-07-01},

urldate = {2023-10-07},

journal = {A\&A},

volume = {675},

pages = {A115},

abstract = {The TOI-1130 is a known planetary system around a K-dwarf consisting of a gas giant planet, TOI-1130 c, on an 8.4-day orbit, accompanied by an inner Neptune-sized planet, TOI-1130 b, with an orbital period of 4.1 days. We collected precise radial velocity (RV) measurements of TOI-1130 with the HARPS and PFS spectrographs as part of our ongoing RV follow-up program. We perform a photodynamical modeling of the HARPS and PFS RVs, and transit photometry from the Transiting Exoplanet Survey Satellite (TESS) and the TESS Follow-up Observing Program. We determine the planet masses and radii of TOI-1130 b and TOI-1130 c to be Mb = 19.28 $textbackslashpm$ 0.97 M$_textbackslashoplus$ and Rb = 3.56 $textbackslashpm$ 0.13 R$_textbackslashoplus$, and Mc = 325.59 $textbackslashpm$ 5.59 M$_textbackslashoplus$ and Rc = 13.32+1.55-1.41 R$_textbackslashoplus$, respectively. We spectroscopically confirm TOI-1130 b that was previously only validated. We find that the two planets orbit with small eccentricities in a 2:1 resonant configuration. This is the first known system with a hot Jupiter and an inner lower mass planet locked in a mean-motion resonance. TOI-1130 belongs to the small yet increasing population of hot Jupiters with an inner low-mass planet that challenges the pathway for hot Jupiter formation. We also detect a linear RV trend possibly due to the presence of an outer massive companion.},

note = {arXiv:2305.15565 [astro-ph]},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{georgieva_toi-733_2023,

title = {TOI-733 b: a planet in the small-planet radius valley orbiting a Sun-like star},

author = {Iskra Y. Georgieva and Carina M. Persson and Elisa Goffo and Lorena Acu\~{n}a and Artyom Aguichine and Luisa M. Serrano and Kristine W. F. Lam and Davide Gandolfi and Karen A. Collins and Steven B. Howell and Fei Dai and Malcolm Fridlund and Judith Korth and Magali Deleuil and Oscar Barrag\'{a}n and William D. Cochran and Szil\'{a}rd Csizmadia and Hans J. Deeg and Eike Guenther and Artie P. Hatzes and Jon M. Jenkins and John Livingston and Rafael Luque and Olivier Mousis and Hannah L. M. Osborne and Enric Palle and Seth Redfield and Vincent Van Eylen and Joseph D. Twicken and Joshua N. Winn and Ahlam Alqasim and Kevin I. Collins and Crystal L. Gnilka and David W. Latham and Hannah M. Lewis and Howard M. Relles and George R. Ricker and Pamela Rowden and Sara Seager and Avi Shporer and Thiam-Guan Tan and Andrew Vanderburg and Roland Vanderspek},

url = {http://arxiv.org/abs/2304.06655},

doi = {10.1051/0004-6361/202345961},

issn = {0004-6361, 1432-0746},

year  = {2023},

date = {2023-06-01},

urldate = {2023-10-07},

journal = {A\&A},

volume = {674},

pages = {A117},

abstract = {We report the discovery of a hot ($T_textbackslashrm eq$ $textbackslashapprox$ 1055 K) planet in the small planet radius valley transiting the Sun-like star TOI-733, as part of the KESPRINT follow-up program of TESS planets carried out with the HARPS spectrograph. TESS photometry from sectors 9 and 36 yields an orbital period of $P_textbackslashrm orb$ = $4.884765 _ - 2.4e-5  textasciicircum  + 1.9e-5 $ days and a radius of $R_textbackslashmathrmp$ = $1.992 _ - 0.090  textasciicircum  + 0.085 $ $R_textbackslashoplus$. Multi-dimensional Gaussian process modelling of the radial velocity measurements from HARPS and activity indicators, gives a semi-amplitude of $K$ = $2.23 textbackslashpm 0.26 $ m s$textasciicircum-1$, translating into a planet mass of $M_textbackslashmathrmp$ = $5.72 _ - 0.68  textasciicircum  + 0.70 $ $M_textbackslashoplus$. These parameters imply that the planet is of moderate density ($textbackslashrho_textbackslashmathrmp$ = $3.98 _ - 0.66  textasciicircum  + 0.77 $ g cm$textasciicircum-3$) and place it in the transition region between rocky and volatile-rich planets with H/He-dominated envelopes on the mass-radius diagram. Combining these with stellar parameters and abundances, we calculate planet interior and atmosphere models, which in turn suggest that TOI-733 b has a volatile-enriched, most likely secondary outer envelope, and may represent a highly irradiated ocean world - one of only a few such planets around G-type stars that are well-characterised.},

note = {arXiv:2304.06655 [astro-ph]},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{mistry_vatest_2023,

title = {VaTEST II: Statistical Validation of 11 TESS-Detected Exoplanets Orbiting K-type Stars},

author = {Priyashkumar Mistry and Kamlesh Pathak and Aniket Prasad and Georgios Lekkas and Surendra Bhattarai and Sarvesh Gharat and Mousam Maity and Dhruv Kumar and Karen A. Collins and Richard P. Schwarz and Christopher R. Mann and Elise Furlan and Steve B. Howell and David Ciardi and Allyson Bieryla and Elisabeth C. Matthews and Erica Gonzales and Carl Ziegler and Ian Crossfield and Steven Giacalone and Thiam-Guan Tan and Phil Evans and Krzysztof G. Helminiak and Kevin I. Collins and Norio Narita and Akihiko Fukui and Francisco J. Pozuelos and Courtney Dressing and Abderahmane Soubkiou and Zouhair Benkhaldoun and Joshua E. Schlieder and Olga Suarez and Khalid Barkaoui and Enric Palle and Felipe Murgas and Gregor Srdoc and Maria V. Goliguzova and Ivan A. Strakhov and Crystal Gnilka and Kathryn Lester and Colin Littlefield and Nic Scott and Rachel Matson and Michael Gillon and Emmanuel Jehin and Mathilde Timmermans and Mourad Ghachoui and Lyu Abe and Philippe Bendjoya and Tristan Guillot and Amaury H. M. J. Triaud},

url = {http://arxiv.org/abs/2301.09865},

doi = {10.3847/1538-3881/acd548},

issn = {0004-6256, 1538-3881},

year  = {2023},

date = {2023-07-01},

urldate = {2023-10-07},

journal = {AJ},

volume = {166},

number = {1},

pages = {9},

abstract = {NASA's Transiting Exoplanet Survey Satellite (TESS) is an all-sky survey mission designed to find transiting exoplanets orbiting nearby bright stars. It has identified more than 329 transiting exoplanets, and almost 6,000 candidates remain unvalidated. In this manuscript, we discuss the findings from the ongoing VaTEST (Validation of Transiting Exoplanets using Statistical Tools) project, which aims to validate new exoplanets for further characterization. We validated 11 new exoplanets by examining the light curves of 24 candidates using the LATTE and TESS-Plot tools and computing the False Positive Probabilities using the statistical validation tool TRICERATOPS. These include planets suitable for atmospheric characterization using transmission spectroscopy (TOI-2194b), emission spectroscopy (TOI-3082b and TOI-5704b) and for both transmission and emission spectroscopy (TOI-672b, TOI- 1694b, and TOI-2443b); One super-Earth (TOI-2194b) orbiting a bright (V = 8.42 mag), metal-poor ([Fe/H] = -0.3720 $textbackslashpm$ 0.1) star; one short-period Neptune-like planet (TOI-5704) in the Hot Neptune Desert. In total, we validated 1 super-Earth, 7 sub-Neptunes, 1 Neptune-like, and 2 sub-Saturn or super-Neptune-like exoplanets. Additionally, we identify five likely planet candidates (TOI-323, TOI- 1180, TOI-2200, TOI-2408 and TOI-3913) which can be further studied to establish their planetary nature.},

note = {arXiv:2301.09865 [astro-ph]},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{christian_possible_2022,

title = {A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions},

author = {Sam Christian and Andrew Vanderburg and Juliette Becker and Daniel A. Yahalomi and Logan Pearce and George Zhou and Karen A. Collins and Adam L. Kraus and Keivan G. Stassun and Zoe Beurs and George R. Ricker and Roland K. Vanderspek and David W. Latham and Joshua N. Winn and S. Seager and Jon M. Jenkins and Lyu Abe and Karim Agabi and Pedro J. Amado and David Baker and Khalid Barkaoui and Zouhair Benkhaldoun and Paul Benni and John Berberian and Perry Berlind and Allyson Bieryla and Emma Esparza-Borges and Michael Bowen and Peyton Brown and Lars A. Buchhave and Christopher J. Burke and Marco Buttu and Charles Cadieux and Douglas A. Caldwell and David Charbonneau and Nikita Chazov and Sudhish Chimaladinne and Kevin I. Collins and Deven Combs and Dennis M. Conti and Nicolas Crouzet and Jerome P. Leon and Shila Deljookorani and Brendan Diamond and Ren\'{e} Doyon and Diana Dragomir and Georgina Dransfield and Zahra Essack and Phil Evans and Akihiko Fukui and Tianjun Gan and Gilbert A. Esquerdo and Micha\"{e}l Gillon and Eric Girardin and Pere Guerra and Tristan Guillot and Eleanor Kate K. Habich and Andreea Henriksen and Nora Hoch and Keisuke I. Isogai and Emmanu\"{e}l Jehin and Eric L. N. Jensen and Marshall C. Johnson and John H. Livingston and John F. Kielkopf and Kingsley Kim and Kiyoe Kawauchi and Vadim Krushinsky and Veronica Kunzle and Didier Laloum and Dominic Leger and Pablo Lewin and Franco Mallia and Bob Massey and Mayuko Mori and Kim K. McLeod and Djamel M\'{e}karnia and Ismael Mireles and Nikolay Mishevskiy and Motohide Tamura and Felipe Murgas and Norio Narita and Ramon Naves and Peter Nelson and Hugh P. Osborn and Enric Palle and Hannu Parviainen and Peter Plavchan and Francisco J. Pozuelos and Markus Rabus and Howard M. Relles and Cristina Rodr\'{i}guez L\'{o}pez and Samuel N. Quinn and Francois-Xavier Schmider and Joshua E. Schlieder and Richard P. Schwarz and Avi Shporer and Laurie Sibbald and Gregor Srdoc and Caitlin Stibbards and Hannah Stickler and Olga Suarez and Chris Stockdale and Thiam-Guan Tan and Yuka Terada and Amaury Triaud and Rene Tronsgaard and William C. Waalkes and Gavin Wang and Noriharu Watanabe and Marie-Sainte Wenceslas and Geof Wingham and Justin Wittrock and Carl Ziegler},

url = {http://arxiv.org/abs/2202.00042},

year  = {2022},

date = {2022-01-01},

urldate = {2022-02-12},

journal = {arXiv:2202.00042 [astro-ph]},

abstract = {Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 AU) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia EDR3 and the TESS mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there is statistically significant difference in the inclination distribution of wide-binary systems with transiting planets compared to a control sample, with the probability that the two distributions are the same being 0.0037. This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 AU. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion on the protoplanetary disk is the most promising explanation.},

note = {arXiv: 2202.00042},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{giacalone_validation_2022,

title = {Validation of 13 Hot and Potentially Terrestrial TESS Planets},

author = {Steven Giacalone and Courtney D. Dressing and Christina Hedges and Veselin B. Kostov and Karen A. Collins and Eric L. N. Jensen and Daniel A. Yahalomi and Allyson Bieryla and David R. Ciardi and Steve B. Howell and Jorge Lillo-Box and Khalid Barkaoui and Jennifer G. Winters and Elisabeth Matthews and John H. Livingston and Samuel N. Quinn and Boris S. Safonov and Charles Cadieux and E. Furlan and Ian J. M. Crossfield and Avi M. Mandell and Emily A. Gilbert and Ethan Kruse and Elisa V. Quintana and George R. Ricker and S. Seager and Joshua N. Winn and Jon M. Jenkins and Britt Duffy Adkins and David Baker and Thomas Barclay and David Barrado and Natalie M. Batalha and Alexander A. Belinski and Zouhair Benkhaldoun and Lars A. Buchhave and Luca Cacciapuoti and Ashley Chontos and Jessie L. Christiansen and Ryan Cloutier and Kevin I. Collins and Dennis M. Conti and Neil Cutting and Scott Dixon and Ren\'{e} Doyon and Mohammed El Mufti and Emma Esparza-Borges and Zahra Essack and Akihiko Fukui and Tianjun Gan and Kaz Gary and Mourad Ghachoui and Micha\"{e}l Gillon and Eric Girardin and Ana Glidden and Erica J. Gonzales and Pere Guerra and Elliott P. Horch and Krzysztof G. Helminiak and Andrew W. Howard and Daniel Huber and Jonathan M. Irwin and Giovanni Isopi and Emmanu\"{e}l Jehin and Taiki Kagetani and Stephen R. Kane and Kiyoe Kawauchi and John F. Kielkopf and Pablo Lewin and Lindy Luker and Michael B. Lund and Franco Mallia and Shude Mao and Bob Massey and Rachel A. Matson and Ismael Mireles and Mayuko Mori and Felipe Murgas and Norio Narita and Tanner O`Dwyer and Erik A. Petigura and Alex S. Polanski and Francisco J. Pozuelos and Enric Palle and Hannu Parviainen and Peter P. Plavchan and Howard M. Relles and Paul Robertson and Mark E. Rose and Pamela Rowden and Arpita Roy and Arjun B. Savel and Joshua E. Schlieder and Chloe Schnaible and Richard P. Schwarz and Ramatholo Sefako and Aleksandra Selezneva and Brett Skinner and Chris Stockdale and Ivan A. Strakhov and Thiam-Guan Tan and Guillermo Torres and Ren\'{e} Tronsgaard and Joseph D. Twicken and David Vermilion and Ian A. Waite and Bradley Walter and Gavin Wang and Carl Ziegler and Yujie Zou},

url = {http://arxiv.org/abs/2201.12661},

doi = {10.3847/1538-3881/ac4334},

year  = {2022},

date = {2022-01-01},

urldate = {2022-02-12},

journal = {arXiv:2201.12661 [astro-ph]},

abstract = {The James Webb Space Telescope (JWST) will be able to probe the atmospheres and surface properties of hot, terrestrial planets via emission spectroscopy. We identify 18 potentially terrestrial planet candidates detected by the Transiting Exoplanet Survey Satellite (TESS) that would make ideal targets for these observations. These planet candidates cover a broad range of planet radii ($R_textbackslashrm p textbackslashsim 0.6 - 2.0 R_textbackslashoplus$) and orbit stars of various magnitudes ($K_s = 5.78 - 10.78$, $V = 8.4 - 15.69$) and effective temperatures ($T_textbackslashrm eff textbackslashsim 3000 - 6000$ K). We use ground-based observations collected through the TESS Follow-up Observing Program (TFOP) and two vetting tools -- DAVE and TRICERATOPS -- to assess the reliabilities of these candidates as planets. We validate 13 planets: TOI-206 b, TOI-500 b, TOI-544 b, TOI-833 b, TOI-1075 b, TOI-1411 b, TOI-1442 b, TOI-1693 b, TOI-1860 b, TOI-2260 b, TOI-2411 b, TOI-2427 b, and TOI-2445 b. Seven of these planets (TOI-206 b, TOI-500 b, TOI-1075 b, TOI-1442 b, TOI-2260 b, TOI-2411 b, and TOI-2445 b) are ultra-short-period planets. TOI-1860 is the youngest ($133 textbackslashpm 26$ Myr) solar twin with a known planet to date. TOI-2260 is a young ($321 textbackslashpm 96$ Myr) G dwarf that is among the most metal-rich ([Fe/H] = $0.22 textbackslashpm 0.06$ dex) stars to host an ultra-short-period planet. With an estimated equilibrium temperature of $textbackslashsim 2600$ K, TOI-2260 b is also the fourth hottest known planet with $R_textbackslashrm p textless 2 textbackslash, R_textbackslashoplus$.},

note = {arXiv: 2201.12661},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{wittrock_transit_2022,

title = {Transit Timing Variations for AU Microscopii b \& c},

author = {Justin M. Wittrock and Stefan Dreizler and Michael A. Reefe and Brett M. Morris and Peter P. Plavchan and Patrick J. Lowrance and Brice-Olivier Demory and James G. Ingalls and Emily A. Gilbert and Thomas Barclay and Bryson L. Cale and Karen A. Collins and Kevin I. Collins and Ian J. M. Crossfield and Diana Dragomir and Jason D. Eastman and Mohammed El Mufti and Dax Feliz and Jonathan Gagne and Eric Gaidos and Peter Gao and Claire S. Geneser and Leslie Hebb and Christopher E. Henze and Keith D. Horne and Jon M. Jenkins and Eric L. N. Jensen and Stephen R. Kane and Laurel Kaye and Eder Martioli and Teresa A. Monsue and Enric Palle and Elisa V. Quintana and Don J. Radford and Veronica Roccatagliata and Joshua E. Schlieder and Richard P. Schwarz and Avi Shporer and Keivan G. Stassun and Christopher Stockdale and Thiam-Guan Tan and Angelle M. Tanner and Andrew Vanderburg and Laura D. Vega and Songhu Wang},

url = {http://arxiv.org/abs/2202.05813},

year  = {2022},

date = {2022-02-01},

urldate = {2022-02-18},

journal = {arXiv:2202.05813 [astro-ph]},

abstract = {We explore the transit timing variations (TTVs) of the young (22 Myr) nearby AU Mic planetary system. For AU Mic b, we introduce three Spitzer (4.5 $textbackslashmu$m) transits, five TESS transits, 11 LCO transits, one PEST transit, one Brierfield transit, and two transit timing measurements from Rossiter-McLaughlin observations; for textbackslashaumic c, we introduce three textbackslashtess Cycle transits. We present two independent TTV analyses. First, we use EXOFASTv2 to jointly model the Spitzer and ground-based transits and to obtain the midpoint transit times. We then construct an O-C diagram and model the TTVs with Exo-Striker. Second, we reproduce our results with an independent photodynamical analysis. We recover a TTV mass for AU Mic c of 10.8$textasciicircum+2.3_-2.2$ M$_E$. We compare the TTV-derived constraints to a recent radial-velocity (RV) mass determination. We also observe excess TTVs that do not appear to be consistent with the dynamical interactions of b and c alone, and do not appear to be due to spots or flares. Thus, we present a hypothetical non-transiting "middle-d" candidate exoplanet that is consistent with the observed TTVs, the candidate RV signal, and would establish the AU Mic system as a compact resonant multi-planet chain in a 4:6:9 period commensurability. These results demonstrate that the AU Mic planetary system is dynamically interacting producing detectable TTVs, and the implied orbital dynamics may inform the formation mechanisms for this young system. We recommend future RV and TTV observations of AU Mic b and c to further constrain the masses and to confirm the existence of possible additional planet(s).},

note = {arXiv: 2202.05813},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{almenara_gj_2022,

title = {GJ 3090 b: one of the most favourable mini-Neptune for atmospheric characterisation},

author = {J. M. Almenara and X. Bonfils and J. F. Otegi and O. Attia and M. Turbet and N. Astudillo-Defru and K. A. Collins and A. S. Polanski and V. Bourrier and C. Hellier and C. Ziegler and F. Bouchy and C. Brice\~{n}o and D. Charbonneau and M. Cointepas and K. I. Collins and I. Crossfield and X. Delfosse and R. F. D\'{i}az and C. Dorn and J. P. Doty and T. Forveille and G. Gaisn\'{e} and T. Gan and R. Helled and K. Hesse and J. M. Jenkins and E. L. N. Jensen and D. W. Latham and N. Law and A. W. Mann and S. Mao and B. McLean and F. Murgas and G. Myers and S. Seager and A. Shporer and T. G. Tan and J. D. Twicken and J. Winn},

url = {http://arxiv.org/abs/2207.14121},

doi = {10.1051/0004-6361/202243975},

issn = {0004-6361, 1432-0746},

year  = {2022},

date = {2022-09-01},

urldate = {2022-11-04},

journal = {A\&A},

volume = {665},

pages = {A91},

abstract = {We report the detection of GJ 3090 b (TOI-177.01), a mini-Neptune on a 2.9-day orbit transiting a bright (K = 7.3 mag) M2 dwarf located at 22 pc. The planet was identified by the Transiting Exoplanet Survey Satellite and was confirmed with the High Accuracy Radial velocity Planet Searcher radial velocities. Seeing-limited photometry and speckle imaging rule out nearby eclipsing binaries. Additional transits were observed with the LCOGT, Spitzer, and ExTrA telescopes. We characterise the star to have a mass of 0.519 $textbackslashpm$ 0.013 M$_textbackslashodot$ and a radius of 0.516 $textbackslashpm$ 0.016 R$_textbackslashodot$. We modelled the transit light curves and radial velocity measurements and obtained a planetary mass of 3.34 $textbackslashpm$ 0.72 M$_textbackslashoplus$, a radius of 2.13 $textbackslashpm$ 0.11 R$_textbackslashoplus$, and a mean density of 1.89$textasciicircum+0.52_-0.45$ g/cm$textasciicircum3$. The low density of the planet implies the presence of volatiles, and its radius and insolation place it immediately above the radius valley at the lower end of the mini-Neptune cluster. A coupled atmospheric and dynamical evolution analysis of the planet is inconsistent with a pure H-He atmosphere and favours a heavy mean molecular weight atmosphere. The transmission spectroscopy metric of 221$textasciicircum+66_-46$ means that GJ 3090 b is the second or third most favourable mini-Neptune after GJ 1214 b whose atmosphere may be characterised. At almost half the mass of GJ 1214 b, GJ 3090 b is an excellent probe of the edge of the transition between super-Earths and mini-Neptunes. We identify an additional signal in the radial velocity data that we attribute to a planet candidate with an orbital period of 13 days and a mass of 17.1$textasciicircum+8.9_-3.2$ M$_textbackslashoplus$, whose transits are not detected.},

note = {arXiv:2207.14121 [astro-ph]},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{rodriguez_tess_2021,

title = {TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full Frame Images},

author = {Rodriguez, Joseph E. and Quinn, Samuel N. and Zhou, George and Vanderburg, Andrew and Nielsen, Louise D. and Wittenmyer, Robert A. and Brahm, Rafael and Reed, Phillip A. and Huang, Chelsea X. and Vach, Sydney and Ciardi, David R. and Oelkers, Ryan J. and Stassun, Keivan G. and Hellier, Coel and Gaudi, B. Scott and Eastman, Jason D. and Collins, Karen A. and Bieryla, Allyson and Christian, Sam and Latham, David W. and Wright, Duncan J. and Matthews, Elisabeth and Gonzales, Erica J. and Ziegler, Carl and Dressing, Courtney D. and Howell, Steve B. and Tan, Thiam-Guan and Wittrock, Justin and Plavchan, Peter and McLeod, Kim K. and Baker, David and Wang, Gavin and Radford, Don and Schwarz, Richard P. and Esposito, Massimiliano and Ricker, George R. and Vanderspek, Roland K. and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Addison, Brett and Anderson, D. R. and Barclay, Thomas and Beatty, Thomas G. and Berlind, Perry and Bouchy, Francois and Bowen, Michael and Bowler, Brendan P. and Brasseur, C. E. and Brice\~{n}o, C\'{e}sar and Calkins, Michael L. and Chaturvedi, Priyanka and Chaverot, Guillaume and Chimaladinne, Sudhish and Christiansen, Jessie L. and Collins, Kevin and Crossfield, Ian J. M. and Eastridge, Kevin and Espinoza, N'estor and Esquerdo, Gilbert A. and Feliz, Dax and Fenske, Tyler and Fong, William and Gan, Tianjun and Gill, Holden and Gordon, Lindsey and Granados, Alex and Grieves, Nolan and Guenther, Eike W. and Guerrero, Natalia and Henning, Thomas and Henze, Christopher E. and Hesse, Katharine and Hobson, Melissa J. and Horner, Jonathan and James, David J. and Jensen, Eric L. N. and Jimenez, Mary and Jord\'{a}n, Andr\'{e}s and Kane, Stephen R. and Kielkopf, John and Kim, Kingsley and Kuhn, Rudolf B. and Latouf, Natasha and Law, Nicholas M. and Levine, Alan M. and Lund, Michael B. and Mann, Andrew W. and Mao, Shude and Matson, Rachel A. and McDermott, Scott and Mengel, Matthew W. and Mink, Jessica and Newman, Patrick and O'Dwyer, Tanner and Okumura, Jack and Palle, Enric and Pepper, Joshua and Quintana, Elisa V. and Sarkis, Paula and Savel, Arjun and Schlieder, Joshua E. and Schnaible, Chloe and Shporer, Avi and Sefako, Ramotholo and Seidel, Julia and Siverd, Robert J. and Skinner, Brett and Stalport, Manu and Stevens, Daniel J. and Stibbard, Caitlin and Tinney, C. G. and West, R. G. and Yahalomi, Daniel A. and Zhang, Hui},

url = {http://arxiv.org/abs/2101.01726},

year  = {2021},

date = {2021-01-01},

urldate = {2021-01-09},

journal = {arXiv:2101.01726 [astro-ph]},

abstract = {We present the discovery and characterization of five hot and warm Jupiters -- TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960) -- based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the $TESS$ Follow-up Observing Program (TFOP) Working Group. The planets are all Jovian size (R$_textbackslashrm P$ = 1.01-1.77 R$_textbackslashrm J$) and have masses that range from 0.85 to 6.33 M$_textbackslashrm J$. The host stars of these systems have F and G spectral types (5595 $textbackslashle$ T$_textbackslashrm eff$ $textbackslashle$ 6460 K) and are all relatively bright (9 $textlessVtextless$ 10.8, 8.2 $textlessKtextless$ 9.3) making them well-suited for future detailed characterization efforts. Three of the systems in our sample (TOI-640 b, TOI-1333 b, and TOI-1601 b) orbit subgiant host stars (log g$_*$ $textless$4.1). TOI-640 b is one of only three known hot Jupiters to have a highly inflated radius (R$_textbackslashrm P$ textgreater 1.7R$_textbackslashrm J$, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive hot Jupiter discovered to date by $TESS$ with a measured mass of $6.31textasciicircum+0.28_-0.30$ M$_textbackslashrm J$ and a statistically significant, non-zero orbital eccentricity of e = $0.074textasciicircum+0.021_-0.022$. This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-Solar analogue. NASA's $TESS$ mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals.},

note = {arXiv: 2101.01726},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{powell_tic_2021,

title = {TIC 168789840: A Sextuply-Eclipsing Sextuple Star System},

author = {Powell, Brian P. and Kostov, Veselin B. and Rappaport, Saul A. and Borkovits, Tamas and Zasche, Petr and Tokovinin, Andrei and Kruse, Ethan and Latham, David W. and Montet, Benjamin T. and Jensen, Eric L. N. and Jayaraman, Rahul and Collins, Karen A. and Masek, Martin and Hellier, Coel and Evans, Phil and Tan, Thiam-Guan and Schlieder, Joshua E. and Torres, Guillermo and Smale, Alan P. and Friedman, Adam H. and Barclay, Thomas and Gagliano, Robert and Quintana, Elisa V. and Jacobs, Thomas L. and Gilbert, Emily A. and Kristiansen, Martti H. and Colon, Knicole D. and LaCourse, Daryll M. and Olmschenk, Greg and Omohundro, Mark and Schnittman, Jeremy D. and Schwengeler, Hans M. and Barry, Richard K. and Terentev, Ivan A. and Boyd, Patricia and Schmitt, Allan R. and Quinn, Samuel N. and Vanderburg, Andrew and Palle, Enric and Armstrong, James and Ricker, George R. and Vanderspek, Roland and Seager, S. and Winn, Joshua N. and Jenkins, Jon M. and Caldwell, Douglas A. and Wohler, Bill and Shiao, Bernie and Burke, Christopher J. and Daylan, Tansu and Villasenor, Joel},

url = {http://arxiv.org/abs/2101.03433},

year  = {2021},

date = {2021-01-01},

urldate = {2021-01-12},

journal = {arXiv:2101.03433 [astro-ph]},

abstract = {We report the discovery of a sextuply-eclipsing sextuple star system from TESS data, TIC 168789840, also known as TYC 7037-89-1, the first known sextuple system consisting of three eclipsing binaries. The target was observed in Sectors 4 and 5 during Cycle 1, with lightcurves extracted from TESS Full Frame Image data. It was also previously observed by the WASP survey and ASAS-SN. The system consists of three gravitationally-bound eclipsing binaries in a hierarchical structure of an inner quadruple system with an outer binary subsystem. Follow-up observations from several different observatories were conducted as a means of determining additional parameters. The system was resolved by speckle interferometry with a 0."42 separation between the inner quadruple and outer binary, inferring an estimated outer period of textasciitilde2 kyr. It was determined that the fainter of the two resolved components is an 8.217 day eclipsing binary, which orbits the inner quadruple that contains two eclipsing binaries with periods of 1.570 days and 1.306 days. MCMC analysis of the stellar parameters has shown that the three binaries of TIC 168789840 are "triplets", as each binary is quite similar to the others in terms of mass, radius, and Teff. As a consequence of its rare composition, structure, and orientation, this object can provide important new insight into the formation, dynamics, and evolution of multiple star systems. Future observations could reveal if the intermediate and outer orbital planes are all aligned with the planes of the three inner eclipsing binaries.},

note = {arXiv: 2101.03433},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{ikwut-ukwa_two_2021,

title = {Two Massive Jupiters in Eccentric Orbits from the TESS Full Frame Images},

author = {Ikwut-Ukwa, Mma and Rodriguez, Joseph E. and Quinn, Samuel N. and Zhou, George and Vanderburg, Andrew and Ali, Asma and Bunten, Katya and Gaudi, B. Scott and Latham, David W. and Howell, Steve B. and Huang, Chelsea X. and Bieryla, Allyson and Collins, Karen A. and Carmichael, Theron W. and Rabus, Markus and Eastman, Jason D. and Collins, Kevin I. and Tan, Thiam-Guan and Schwarz, Richard P. and Myers, Gordon and Stockdale, Chris and Kielkopf, John F. and Radford, Don J. and Oelkers, Ryan J. and Jenkins, Jon M. and Ricker, George R. and Seager, Sara and Vanderspek, Roland K. and Winn, Joshua N. and Burt, Jennifer and Butler, R. Paul and Calkins, Michael L. and Crane, Jeffrey D. and Gnilka, Crystal L. and Esquerdo, Gilbert A. and Fong, Wlliam and Kreidberg, Laura and Mink, Jessica and Rodriguez, David R. and Schlieder, Joshua E. and Schectman, Stephen and Shporer, Avi and Teske, Johanna and Ting, Eric B. and Villasenor, Jesus Noel and Yahalomi, Daniel A.},

url = {http://arxiv.org/abs/2102.02222},

year  = {2021},

date = {2021-01-01},

urldate = {2021-02-05},

journal = {arXiv:2102.02222 [astro-ph]},

abstract = {We report the discovery of two short-period massive giant planets from NASA's Transiting Exoplanet Survey Satellite (TESS). Both systems, TOI-558 (TIC 207110080) and TOI-559 (TIC 209459275), were identified from the 30-minute cadence Full Frame Images and confirmed using ground-based photometric and spectroscopic follow-up observations from TESS's Follow-up Observing Program Working Group. We find that TOI-558 b, which transits an F-dwarf ($M_textbackslashstar=1.349textasciicircum+0.064_-0.065textbackslash M_textbackslashodot$, $R_textbackslashstar=1.496textasciicircum+0.042_-0.040textbackslash R_textbackslashodot$, $T_eff=6466textasciicircum+95_-93$ K, age $1.79textasciicircum+0.91_-0.73$ Gyr) with an orbital period of 14.574 days, has a mass of $3.61textbackslashpm0.15textbackslash M_J$, a radius of $1.086textasciicircum+0.041_-0.038textbackslash R_J$, and an eccentric (e=$0.300textasciicircum+0.022_-0.020$) orbit. TOI-559 b transits a G-dwarf ($M_textbackslashstar=1.026textbackslashpm0.057textbackslash M_textbackslashodot$, $R_textbackslashstar=1.233textasciicircum+0.028_-0.026textbackslash R_textbackslashodot$, $T_eff=5925textasciicircum+85_-76$ K, age $1.79textasciicircum+0.91_-0.73$ Gyr) in an eccentric (e=$0.151textbackslashpm0.011$) 6.984-day orbit with a mass of $6.01textasciicircum+0.24_-0.23textbackslash M_J$ and a radius of $1.091textasciicircum+0.028_-0.025textbackslash R_J$. Our spectroscopic follow-up also reveals a long-term radial velocity trend for TOI-559, indicating a long-period companion. The statistically significant orbital eccentricity measured for each system suggests that these planets migrated to their current location through dynamical interactions. Interestingly, both planets are also massive ($textgreater3textbackslash M_J$), adding to the population of massive hot Jupiters identified by TESS. Prompted by these new detections of high-mass planets, we analyzed the known mass distribution of hot Jupiters but find no significant evidence for multiple populations. TESS should provide a near magnitude-limited sample of transiting hot Jupiters, allowing for future detailed population studies.},

note = {arXiv: 2102.02222},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{newton_tess_2021,

title = {TESS Hunt for Young and Maturing Exoplanets (THYME) IV: Three small planets orbiting a 120 Myr-old star in the Pisces--Eridanus stream},

author = {Newton, Elisabeth R. and Mann, Andrew W. and Kraus, Adam L. and Livingston, John H. and Vanderburg, Andrew and Curtis, Jason L. and Thao, Pa Chia and Hawkins, Keith and Wood, Mackenna L. and Rizzuto, Aaron C. and Soubkiou, Abderahmane and Tofflemire, Benjamin M. and Zhou, George and Crossfield, Ian J. M. and Pearce, Logan A. and Collins, Karen A. and Conti, Dennis M. and Tan, Thiam-Guan and Villeneuva, Steven and Spencer, Alton and Dragomir, Diana and Quinn, Samuel N. and Jensen, Eric L. N. and Collins, Kevin I. and Stockdale, Chris and Cloutier, Ryan and Hellier, Coel and Benkhaldoun, Zouhair and Ziegler, Carl and Brice\~{n}o, C\'{e}sar and Law, Nicholas and Benneke, Bj\"{o}rn and Christiansen, Jessie L. and Gorjian, Varoujan and Kane, Stephen R. and Kreidberg, Laura and Morales, Farisa Y. and Werner, Michael W. and Twicken, Joseph D. and Levine, Alan M. and Ciardi, David R. and Guerrero, Natalia M. and Hesse, Katharine and Quintana, Elisa V. and Shiao, Bernie and Smith, Jeffrey C. and Torres, Guillermo and Ricker, George R. and Vanderspek, Roland and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Latham, David W.},

url = {http://arxiv.org/abs/2102.06049},

doi = {10.3847/1538-3881/abccc6},

issn = {1538-3881},

year  = {2021},

date = {2021-01-01},

urldate = {2021-02-12},

journal = {AJ},

volume = {161},

number = {2},

pages = {65},

abstract = {Young exoplanets can offer insight into the evolution of planetary atmospheres, compositions, and architectures. We present the discovery of the young planetary system TOI 451 (TIC 257605131, Gaia DR2 4844691297067063424). TOI 451 is a member of the 120-Myr-old Pisces--Eridanus stream (Psc--Eri). We confirm membership in the stream with its kinematics, its lithium abundance, and the rotation and UV excesses of both TOI 451 and its wide binary companion, TOI 451 B (itself likely an M dwarf binary). We identified three candidate planets transiting in the TESS data and followed up the signals with photometry from Spitzer and ground-based telescopes. The system comprises three validated planets at periods of 1.9, 9.2 and 16 days, with radii of 1.9, 3.1, and 4.1 Earth radii, respectively. The host star is near-solar mass with V=11.0 and H=9.3 and displays an infrared excess indicative of a debris disk. The planets offer excellent prospects for transmission spectroscopy with HST and JWST, providing the opportunity to study planetary atmospheres that may still be in the process of evolving.},

note = {arXiv: 2102.06049},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{zang_earth-mass_2021,

title = {An Earth-mass Planet in a Time of Covid-19: KMT-2020-BLG-0414Lb},

author = {Zang, Weicheng and Han, Cheongho and Kondo, Iona and Yee, Jennifer C. and Lee, Chung-Uk and Gould, Andrew and Mao, Shude and de Almeida, Leandro and Shvartzvald, Yossi and Zhang, Xiangyu and Albrow, Michael D. and Chung, Sun-Ju and Hwang, Kyu-Ha and Jung, Youn Kil and Ryu, Yoon-Hyun and Shin, In-Gu and Cha, Sang-Mok and Kim, Dong-Jin and Kim, Hyoun-Woo and Kim, Seung-Lee and Lee, Dong-Joo and Lee, Yongseok and Park, Byeong-Gon and Pogge, Richard W. and Drummond, John and Tan, Thiam-Guan and J\'{u}nior, Jos\'{e} Dias do Nascimento and Maoz, Dan and Penny, Matthew T. and Zhu, Wei and Bond, Ian A. and Abe, Fumio and Barry, Richard and Bennett, David P. and Bhattacharya, Aparna and Donachie, Martin and Fujii, Hirosane and Fukui, Akihiko and Hirao, Yuki and Itow, Yoshitaka and Kirikawa, Rintaro and Koshimoto, Naoki and Li, Man Cheung Alex and Matsubara, Yutaka and Muraki, Yasushi and Miyazaki, Shota and Ranc, Cl\'{e}ment and Rattenbury, Nicholas J. and Satoh, Yuki and Shoji, Hikaru and Sumi, Takahiro and Suzuki, Daisuke and Tanaka, Yuzuru and Tristram, Paul J. and Yamawaki, Tsubasa and Yonehara, Atsunori and Petric, Andreea and Burdullis, Todd and Fouqu\'{e}, Pascal},

url = {http://arxiv.org/abs/2103.01896},

year  = {2021},

date = {2021-01-01},

urldate = {2021-03-04},

journal = {arXiv:2103.01896 [astro-ph]},

abstract = {We report the discovery of KMT-2020-BLG-0414Lb, with a planet-to-host mass ratio $q_2 = 0.9$--$1.2 textbackslashtimes 10textasciicircum-5 = 3$--$4textasciitildeq_textbackslashoplus$ at $1textbackslashsigma$, which is the lowest mass-ratio microlensing planet to date. Together with two other recent discoveries ($4 textbackslashlesssim q/q_textbackslashoplus textbackslashlesssim 6$), it fills out the previous empty sector at the bottom of the triangular $(textbackslashlog s, textbackslashlog q)$ diagram, where $s$ is the planet-host separation in units of the angular Einstein radius $textbackslashtheta_textbackslashrm E$. Hence, these discoveries call into question the existence, or at least the strength, of the break in the mass-ratio function that was previously suggested to account for the paucity of very low-$q$ planets. Due to the extreme magnification of the event, $A_textbackslashrm maxtextbackslashsim 1450$ for the underlying single-lens event, its light curve revealed a second companion with $q_3 textbackslashsim 0.05$ and $textbartextbackslashlog s_3textbar textbackslashsim 1$, i.e., a factor $textbackslashsim 10$ closer to or farther from the host in projection. The measurements of the microlens parallax $textbackslashpi_textbackslashrm E$ and the angular Einstein radius $textbackslashtheta_textbackslashrm E$ allow estimates of the host, planet, and second companion masses, $(M_1, M_2, M_3) textbackslashsim (0.3M_textbackslashodot, 1.0M_textbackslashoplus, 17M_J)$, the planet and second companion projected separations, $(a_textbackslashperp,2, a_textbackslashperp,3) textbackslashsim (1.5, 0.15textasciitildetextbackslashrm ortextasciitilde15)$textasciitildeau, and system distance $D_textbackslashrm L textbackslashsim 1$ kpc. The lens could account for most or all of the blended light ($I textbackslashsim 19.3$) and so can be studied immediately with high-resolution photometric and spectroscopic observations that can further clarify the nature of the system. The planet was found as part of a new program of high-cadence follow-up observations of high-magnification events. The detection of this planet, despite the considerable difficulties imposed by Covid-19 (two KMT sites and OGLE were shut down), illustrates the potential utility of this program.},

note = {arXiv: 2103.01896},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{desidera_sphere_2021,

title = {The SPHERE infrared survey for exoplanets (SHINE)- I Sample definition and target characterization},

author = {Desidera, S. and Chauvin, G. and Bonavita, M. and Messina, S. and LeCoroller, H. and Schmidt, T. and Gratton, R. and Lazzoni, C. and Meyer, M. and Schlieder, J. and Cheetham, A. and Hagelberg, J. and Bonnefoy, M. and Feldt, M. and Lagrange, A.-M. and Langlois, M. and Vigan, A. and Tan, T. G. and Hambsch, F.-J. and Millward, M. and Alcala, J. and Benatti, S. and Brandner, W. and Carson, J. and Covino, E. and Delorme, P. and D'Orazi, V. and Janson, M. and Rigliaco, E. and Beuzit, J.-L. and Biller, B. and Boccaletti, A. and Dominik, C. and Cantalloube, F. and Fontaniv, C. and Galicher, R. and Henning, Th and Lagadec, E. and Ligi, R. and Maire, A.-L. and Menard, F. and Mesa, D. and Muller, A. and Samland, M. and Schmid, H. M. and Sissa, E. and Turatto, M. and Udry, S. and Asensio-Torres, A. Zurlo R. and Kopytova, T. and Rickman, E. and Abe, L. and Antichi, J. and Baruffolo, A. and Baudoz, P. and Baudrand, J. and Blanchard, P. and Bazzon, A. and Buey, T. and Carbillet, M. and Carle, M. and Charton, J. and Cascone, E. and Claudi, R. and Costille, A. and Deboulbe, A. and De Caprio, V. and Dohlen, K. and Fantinel, D. and Feautrier, P. and Fusco, T. and Gigan, P. and Giro, E. and Gisler, D. and Gluck, L. and Hubin, N. and Hugot, E. and Jaquet, M. and Kasper, M. and Madec, F. and Magnard, Y. and Martinez, P. and Maurel, D. and Mignant, D. Le and Moller-Nilsson, O. and Llored, M. and Moulin, T. and Origne, A. and Pavlov, A. and Perret, D. and Petit, C. and Pragt, J. and Puget, P. and Rabou, P. and Ramon, J. and Rigal, F. and Rochat, S. and Roelfsema, R. and Rousset, G. and Roux, A. and Salasnich, B. and Sauvage, J.-F. and Sevin, A. and Soenke, C. and Stadler, E. and Suarez, M. and Weber, L. and Wildi, F.},

url = {http://arxiv.org/abs/2103.04366},

year  = {2021},

date = {2021-01-01},

urldate = {2021-03-10},

journal = {arXiv:2103.04366 [astro-ph]},

abstract = {Large surveys with new-generation high-contrast imaging instruments are needed to derive the frequency and properties of exoplanet populations with separations from $textbackslashsim$5 to 300 AU. A careful assessment of the stellar properties is crucial for a proper understanding of when, where, and how frequently planets form, and how they evolve. The sensitivity of detection limits to stellar age makes this a key parameter for direct imaging surveys. We describe the SpHere INfrared survey for Exoplanets (SHINE), the largest direct imaging planet-search campaign initiated at the VLT in 2015 in the context of the SPHERE Guaranteed Time Observations of the SPHERE consortium. In this first paper we present the selection and the properties of the complete sample of stars surveyed with SHINE, focusing on the targets observed during the first phase of the survey (from February 2015 to February 2017). This early sample composed of 150 stars is used to perform a preliminary statistical analysis of the SHINE data, deferred to two companion papers presenting the survey performance, main discoveries, and the preliminary statistical constraints set by SHINE. Based on a large database collecting the stellar properties of all young nearby stars in the solar vicinity (including kinematics, membership to moving groups, isochrones, lithium abundance, rotation, and activity), we selected the original sample of 800 stars that were ranked in order of priority according to their sensitivity for planet detection in direct imaging with SPHERE. The properties of the stars that are part of the early statistical sample were revisited, including for instance measurements from the GAIA Data Release 2.},

note = {arXiv: 2103.04366},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{trifonov_nearby_2021,

title = {A nearby transiting rocky exoplanet that is suitable for atmospheric investigation},

author = {Trifonov, T. and Caballero, J. A. and Morales, J. C. and Seifahrt, A. and Ribas, I. and Reiners, A. and Bean, J. L. and Luque, R. and Parviainen, H. and Pall\'{e}, E. and Stock, S. and Zechmeister, M. and Amado, P. J. and Anglada-Escud\'{e}3, G. and Azzaro, M. and Barclay, T. and B\'{e}jar, V. J. S. and Bluhm, P. and Casasayas-Barris, N. and Cifuentes, C. and Collins, K. A. and Collins, K. I. and Cort\'{e}s-Contreras, M. and de Leon, J. and Dreizler, S. and Dressing, C. D. and Esparza-Borges, E. and Espinoza, N. and Fausnaugh, M. and Fukui, A. and Hatzes, A. P. and Hellier, C. and Henning, Th and Henze, C. E. and Herrero, E. and Jeffers, S. V. and Jenkins, J. M. and Jensen, E. L. N. and Kaminski, A. and Kasper, D. and Kossakowski, D. and K\"{u}rster, M. and Lafarga, M. and Latham, D. W. and Mann, A. W. and Molaverdikhani, K. and Montes, D. and Montet, B. T. and Murgas, F. and Narita, N. and Oshagh, M. and Passegger, V. M. and Pollacco, D. and Quinn, S. N. and Quirrenbach, A. and Ricker, G. R. and L\'{o}pez, C. Rodr\'{i}guez and Sanz-Forcada, J. and Schwarz, R. P. and Schweitzer, A. and Seager, S. and Shporer, A. and Stangret, M. and St\"{u}rmer, J. and Tan, T. G. and Tenenbaum, P. and Twicken, J. D. and Vanderspek, R. and Winn, J. N.},

url = {http://arxiv.org/abs/2103.04950},

doi = {10.1126/science.abd7645},

issn = {0036-8075, 1095-9203},

year  = {2021},

date = {2021-01-01},

urldate = {2021-03-10},

journal = {Science},

volume = {371},

number = {6533},

pages = {1038--1041},

abstract = {Spectroscopy of transiting exoplanets can be used to investigate their atmospheric properties and habitability. Combining radial velocity (RV) and transit data provides additional information on exoplanet physical properties. We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is 2.81 Earth masses and 1.31 Earth radii, with uncertainties of 5%, as determined from RV data and photometric light curves. The host star is at a distance of textasciitilde8.1 parsecs, has a J-band magnitude of textasciitilde7.2, and is observable from both hemispheres of Earth. On the basis of these properties and the planet's short orbital period and high equilibrium temperature, we show that this terrestrial planet is suitable for emission and transit spectroscopy.},

note = {arXiv: 2103.04950},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{dong_warm_2021,

title = {Warm Jupiters in TESS Full-Frame Images: A Catalog and Observed Eccentricity Distribution for Year 1},

author = {Dong, Jiayin and Huang, Chelsea X. and Dawson, Rebekah I. and Foreman-Mackey, Daniel and Collins, Karen A. and Quinn, Samuel N. and Lissauer, Jack J. and Beatty, Thomas G. and Quarles, Billy and Sha, Lizhou and Shporer, Avi and Guo, Zhao and Kane, Stephen R. and Abe, Lyu and Barkaoui, Khalid and Benkhaldoun, Zouhair and Brahm, Rafael A. and Bouchy, Francois and Carmichael, Theron W. and Collins, Kevin I. and Conti, Dennis M. and Crouzet, Nicolas and Dransfield, Georgina and Evans, Phil and Gan, Tianjun and Ghachoui, Mourad and Gillon, Michael and Grieves, Nolan and Guillot, Tristan and Hellier, Coel and Jehin, Emmanuel and Jensen, Eric L. and Jordan, Andres and Kamler, Jacob and Kielkopf, John and Mekarnia, Djamel and Nielsen, Louise D. and Pozuelos, Francisco J. and Radford, Don J. and Schmider, Francois-Xavier and Schwarz, Richard P. and Stockdale, Chris and Tan, Thiam-Guan and Timmermans, Mathilde and Triaud, Amaury H. and Wang, Gavin and Ricker, George R. and Vanderspek, Roland and Latham, David W. and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Mireles, Ismael and Yahalomi, Daniel and Morgan, Edward H. and Vezie, Michael and Quintana, Elisa V. and Rose, Mark E. and Smith, Jeffrey C. and Shiao, Bernie},

url = {http://arxiv.org/abs/2104.01970},

year  = {2021},

date = {2021-01-01},

urldate = {2021-04-19},

journal = {arXiv:2104.01970 [astro-ph]},

abstract = {Warm Jupiters -- defined here as planets larger than 6 Earth radii with orbital periods of 8--200 days -- are a key missing piece in our understanding of how planetary systems form and evolve. It is currently debated whether Warm Jupiters form in situ, undergo disk or high eccentricity tidal migration, or have a mixture of origin channels. These different classes of origin channels lead to different expectations for Warm Jupiters' properties, which are currently difficult to evaluate due to the small sample size. We take advantage of the textbackslashTESS survey and systematically search for Warm Jupiter candidates around main-sequence host stars brighter than the textbackslashTESS-band magnitude of 12 in the Full-Frame Images in Year 1 of the textbackslashTESS Prime Mission data. We introduce a catalog of 55 Warm Jupiter candidates, including 19 candidates that were not originally released as textbackslashTESS Objects of Interest (TOIs) by the textbackslashTESS team. We fit their textbackslashTESS light curves, characterize their eccentricities and transit-timing variations (TTVs), and prioritize a list for ground-based follow-up and textbackslashTESS Extended Mission observations. Using hierarchical Bayesian modeling, we find the preliminary eccentricity distributions of our Warm-Jupiter-candidate catalog using a Beta distribution, a Rayleigh distribution, and a two-component Gaussian distribution as the functional forms of the eccentricity distribution. Additional follow-up observations will be required to clean the sample of false positives for a full statistical study, derive the orbital solutions to break the eccentricity degeneracy, and provide mass measurements.},

note = {arXiv: 2104.01970},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{bryant_transit_2021,

title = {A transit timing variation observed for the long-period extremely low density exoplanet HIP 41378f},

author = {Bryant, Edward M. and Bayliss, Daniel and Santerne, Alexandre and Wheatley, Peter J. and Nascimbeni, Valerio and Ducrot, Elsa and Burdanov, Artem and Acton, Jack S. and Alves, Douglas R. and Anderson, David R. and Armstrong, David J. and Awiphan, Supachai and Cooke, Benjamin F. and Burleigh, Matthew R. and Casewell, Sarah L. and Delrez, Laetitia and Demory, Brice-Olivier and Eigm\"{u}ller, Philipp and Fukui, Akihiko and Gan, Tianjun and Gill, Samuel and Gillon, Michael and Goad, Michael R. and Tan, Thiam-Guan and G\"{u}nther, Maximilian N. and Hardee, Bronwen and Henderson, Beth A. and Jehin, Emmanuel and Jenkins, James S. and Kosiarek, Molly and Lendl, Monika and Moyano, Maximiliano and Murray, Catriona A. and Narita, Norio and Niraula, Prajwal and Odden, Caroline E. and Palle, Enric and Parviainen, Hannu and Pedersen, Peter P. and Pozuelos, Francisco J. and Rackham, Benjamin V. and Sebastian, Daniel and Stockdale, Chris and Tilbrook, Rosanna H. and Thompson, Samantha J. and Triaud, Amaury H. M. J. and Udry, St\'{e}phane and Vines, Jose I. and West, Richard G. and de Wit, Julien},

url = {http://arxiv.org/abs/2104.03159},

year  = {2021},

date = {2021-04-01},

urldate = {2021-04-19},

journal = {arXiv:2104.03159 [astro-ph]},

abstract = {HIP 41378 f is a temperate $9.2textbackslashpm0.1 R_textbackslashoplus$ planet with period of 542.08 days and an extremely low density of $0.09textbackslashpm0.02$ g cm$textasciicircum-3$. It transits the bright star HIP 41378 (V=8.93), making it an exciting target for atmospheric characterization including transmission spectroscopy. HIP 41378 was monitored photometrically between the dates of 2019 November 19 and November 28. We detected a transit of HIP 41378 f with NGTS, just the third transit ever detected for this planet, which confirms the orbital period. This is also the first ground-based detection of a transit of HIP 41378 f. Additional ground-based photometry was also obtained and used to constrain the time of the transit. The transit was measured to occur 1.50 hours earlier than predicted. We use an analytic transit timing variation (TTV) model to show the observed TTV can be explained by interactions between HIP 41378 e and HIP 41378 f. Using our TTV model, we predict the epochs of future transits of HIP 41378 f, with derived transit centres of T$_C,4 = 2459355.087textasciicircum+0.031_-0.022$ (May 2021) and T$_C,5 = 2459897.078textasciicircum+0.114_-0.060$ (Nov 2022).},

note = {arXiv: 2104.03159},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{grieves_populating_2021,

title = {Populating the brown dwarf and stellar boundary: Five stars with transiting companions near the hydrogen-burning mass limit},

author = {Grieves, Nolan and Bouchy, Fran\c{c}ois and Lendl, Monika and Carmichael, Theron and Mireles, Ismael and Shporer, Avi and McLeod, Kim K. and Collins, Karen A. and Brahm, Rafael and Stassun, Keivan G. and Gill, Sam and Bouma, Luke G. and Guillot, Tristan and Cointepas, Marion and Santos, Leonardo A. Dos and Casewell, Sarah L. and Jenkins, Jon M. and Henning, Thomas and Nielsen, Louise D. and Psaridi, Angelica and Udry, St\'{e}phane and S\'{e}gransan, Damien and Eastman, Jason D. and Zhou, George and Abe, Lyu and Agabi, Abelkrim and Charbonneau, David and Collins, Kevin I. and Colon, Knicole D. and Crouzet, Nicolas and Dransfield, Georgina and Evans, Phil and Goeke, Robert F. and Hart, Rhodes and Irwin, Jonathan M. and Jensen, Eric L. N. and Jord\'{a}n, Andr\'{e}s and Kielkopf, John F. and Latham, David W. and Marie-Sainte, Wenceslas and M\'{e}karnia, Djamel and Nelson, Peter and Quinn, Samuel N. and Radford, Don J. and Rodriguez, David R. and Rowden, Pamela and Schmider, Fran\c{c}ois-Xavier and Schwarz, Richard P. and Smith, Jeffrey C. and Stockdale, Chris and Suarez, Olga and Tan, Thiam-Guan and Triaud, Amaury H. M. J. and Waalkes, William and Wingham, Geof},

url = {http://arxiv.org/abs/2107.03480},

year  = {2021},

date = {2021-01-01},

urldate = {2021-07-09},

journal = {arXiv:2107.03480 [astro-ph]},

abstract = {We report the discovery of five transiting companions near the hydrogen-burning mass limit in close orbits around main sequence stars originally identified by the Transiting Exoplanet Survey Satellite (TESS) as TESS Objects of Interest (TOIs): TOI-148, TOI-587, TOI-681, TOI-746, and TOI-1213. Using TESS and ground-based photometry as well as radial velocities from the CORALIE, CHIRON, TRES, and FEROS spectrographs, we found the companions have orbital periods between 4.8 and 27.2 days, masses between 77 and 98 $textbackslashmathrmM_Jup$, and radii between 0.81 and 1.66 $textbackslashmathrmR_Jup$. These targets have masses near the uncertain lower limit of hydrogen core fusion ($textbackslashsim$73-96 $textbackslashmathrmM_Jup$), which separates brown dwarfs and low-mass stars. We constrained young ages for TOI-587 (0.2 $textbackslashpm$ 0.1 Gyr) and TOI-681 (0.17 $textbackslashpm$ 0.03 Gyr) and found them to have relatively larger radii compared to other transiting companions of a similar mass. Conversely we estimated older ages for TOI-148 and TOI-746 and found them to have relatively smaller companion radii. With an effective temperature of 9800 $textbackslashpm$ 200 K, TOI-587 is the hottest known main-sequence star to host a transiting brown dwarf or very low-mass star. We found evidence of spin-orbit synchronization for TOI-148 and TOI-746 as well as tidal circularization for TOI-148. These companions add to the population of brown dwarfs and very low-mass stars with well measured parameters ideal to test formation models of these rare objects, the origin of the brown dwarf desert, and the distinction between brown dwarfs and hydrogen-burning main sequence stars.},

note = {arXiv: 2107.03480},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{osborn_toi-431hip_2021,

title = {TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet},

author = {Osborn, Ares and Armstrong, David J. and Cale, Bryson and Brahm, Rafael and Wittenmyer, Robert A. and Dai, Fei and Crossfield, Ian J. M. and Bryant, Edward M. and Adibekyan, Vardan and Cloutier, Ryan and Collins, Karen A. and Mena, E. Delgado and Fridlund, Malcolm and Hellier, Coel and Howell, Steve B. and King, George W. and Lillo-Box, Jorge and Otegi, Jon and Sousa, S. and Stassun, Keivan G. and Matthews, Elisabeth C. and Ziegler, Carl and Ricker, George and Vanderspek, Roland and Latham, David W. and Seager, S. and Winn, Joshua N. and Jenkins, Jon M. and Acton, Jack S. and Addison, Brett C. and Anderson, David R. and Ballard, Sarah and Barrado, David and Barros, Susana C. C. and Batalha, Natalie and Bayliss, Daniel and Barclay, Thomas and Benneke, Bj\"{o}rn and Berberian Jr., John and Bouchy, Francois and Bowler, Brendan P. and Brice\~{n}o, C\'{e}sar and Burke, Christopher J. and Burleigh, Matthew R. and Casewell, Sarah L. and Ciardi, David and Collins, Kevin I. and Cooke, Benjamin F. and Demangeon, Olivier D. S. and D\'{i}az, Rodrigo F. and Dorn, C. and Dragomir, Diana and Dressing, Courtney and Dumusque, Xavier and Espinoza, N\'{e}stor and Figueira, P. and Fulton, Benjamin and Furlan, E. and Gaidos, E. and Geneser, C. and Gill, Samuel and Goad, Michael R. and Gonzales, Erica J. and Gorjian, Varoujan and G\"{u}nther, Maximilian N. and Helled, Ravit and Henderson, Beth A. and Henning, Thomas and Hogan, Aleisha and Hojjatpanah, Saeed and Horner, Jonathan and Howard, Andrew W. and Hoyer, Sergio and Huber, Dan and Isaacson, Howard and Jenkins, James S. and Jensen, Eric L. N. and Jord\'{a}n, Andr\'{e}s and Kane, Stephen R. and Kidwell Jr., Richard C. and Kielkopf, John and Law, Nicholas and Lendl, Monika and Lund, M. and Matson, Rachel A. and Mann, Andrew W. and McCormac, James and Mengel, Matthew W. and Morales, Farisa Y. and Nielsen, Louise D. and Okumura, Jack and Osborn, Hugh P. and Petigura, Erik A. and Plavchan, Peter and Pollacco, Don and Quintana, Elisa V. and Raynard, Liam and Robertson, Paul and Rose, Mark E. and Roy, Arpita and Reefe, Michael and Santerne, Alexandre and Santos, Nuno C. and Sarkis, Paula and Schlieder, J. and Schwarz, Richard P. and Scott, Nicholas J. and Shporer, Avi and Smith, A. M. S. and Stibbard, C. and Stockdale, Chris and Str\om, Paul A. and Twicken, Joseph D. and Tan, Thiam-Guan and Tanner, A. and Teske, J. and Tilbrook, Rosanna H. and Tinney, C. G. and Udry, Stephane and Villase\~{n}or, Jesus Noel and Vines, Jose I. and Wang, Sharon X. and Weiss, Lauren M. and West, Richard G. and Wheatley, Peter J. and Wright, Duncan J. and Zhang, Hui and Zohrabi, F.},

url = {http://arxiv.org/abs/2108.02310},

year  = {2021},

date = {2021-01-01},

urldate = {2021-08-16},

journal = {arXiv:2108.02310 [astro-ph]},

abstract = {We present the bright (V$_mag = 9.12$), multi-planet system TOI-431, characterised with photometry and radial velocities. We estimate the stellar rotation period to be $30.5 textbackslashpm 0.7$ days using archival photometry and radial velocities. TOI-431b is a super-Earth with a period of 0.49 days, a radius of 1.28 $textbackslashpm$ 0.04 R$_textbackslashoplus$, a mass of $3.07 textbackslashpm 0.35$ M$_textbackslashoplus$, and a density of $8.0 textbackslashpm 1.0$ g cm$textasciicircum-3$; TOI-431d is a sub-Neptune with a period of 12.46 days, a radius of $3.29 textbackslashpm 0.09$ R$_textbackslashoplus$, a mass of $9.90textasciicircum+1.53_-1.49$ M$_textbackslashoplus$, and a density of $1.36 textbackslashpm 0.25$ g cm$textasciicircum-3$. We find a third planet, TOI-431c, in the HARPS radial velocity data, but it is not seen to transit in the TESS light curves. It has an $M textbackslashsin i$ of $2.83textasciicircum+0.41_-0.34$ M$_textbackslashoplus$, and a period of 4.85 days. TOI-431d likely has an extended atmosphere and is one of the most well-suited TESS discoveries for atmospheric characterisation, while the super-Earth TOI-431b may be a stripped core. These planets straddle the radius gap, presenting an interesting case-study for atmospheric evolution, and TOI-431b is a prime TESS discovery for the study of rocky planet phase curves.},

note = {arXiv: 2108.02310},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{silverstein_lhs_2021,

title = {The LHS 1678 System: Two Earth-Sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc},

author = {Silverstein, Michele L. and Schlieder, Joshua E. and Barclay, Thomas and Hord, Benjamin J. and Jao, Wei-Chun and Vrijmoet, Eliot Halley and Henry, Todd J. and Cloutier, Ryan and Kostov, Veselin B. and Kruse, Ethan and Winters, Jennifer G. and Irwin, Jonathan M. and Kane, Stephen R. and Stassun, Keivan G. and Huang, Chelsea and Kunimoto, Michelle and Tey, Evan and Vanderburg, Andrew and Astudillo-Defru, Nicola and Bonfils, Xavier and Brasseur, C. E. and Charbonneau, David and Ciardi, David R. and Collins, Karen A. and Collins, Kevin I. and Conti, Dennis M. and Crossfield, Ian J. M. and Daylan, Tansu and Doty, John P. and Dressing, Courtney D. and Gilbert, Emily A. and Horne, Keith and Jenkins, Jon M. and Latham, David W. and Mann, Andrew W. and Matthews, Elisabeth and Paredes, Leonardo A. and Quinn, Samuel N. and Ricker, George R. and Schwarz, Richard P. and Seager, Sara and Sefako, Ramotholo and Shporer, Avi and Smith, Jeffrey C. and Stockdale, Christopher and Tan, Thiam-Guan and Torres, Guillermo and Twicken, Joseph D. and Vanderspek, Roland and Wang, Gavin and Winn, Joshua N.},

url = {http://arxiv.org/abs/2110.12079},

year  = {2021},

date = {2021-01-01},

urldate = {2021-11-06},

journal = {arXiv:2110.12079 [astro-ph]},

abstract = {We present the TESS discovery of the LHS 1678 (TOI-696) exoplanet system, comprised of two approximately Earth-sized transiting planets and a likely astrometric brown dwarf orbiting a bright ($V_J$=12.5, $K_s$=8.3) M2 dwarf at 19.9 pc. The two TESS-detected planets are of radius 0.70$textbackslashpm$0.04 $R_textbackslashoplus$ and 0.98$textbackslashpm$0.06 $R_textbackslashoplus$ in 0.86-day and 3.69-day orbits, respectively. Both planets are validated and characterized via ground-based follow-up observations. HARPS RV monitoring yields 97.7 percentile mass upper limits of 0.35 $M_textbackslashoplus$ and 1.4 $M_textbackslashoplus$ for planets b and c, respectively. The astrometric companion detected by the CTIO/SMARTS 0.9m has an orbital period on the order of decades and is undetected by other means. Additional ground-based observations constrain the companion to being a high-mass brown dwarf or smaller. Each planet is of unique interest; the inner planet has an ultra-short period, and the outer planet is in the Venus zone. Both are promising targets for atmospheric characterization with the JWST and mass measurements via extreme-precision radial velocity. A third planet candidate of radius 0.9$textbackslashpm$0.1 $R_textbackslashoplus$ in a 4.97-day orbit is also identified in multi-Cycle TESS data for validation in future work. The host star is associated with an observed gap in the lower main sequence of the Hertzsprung-Russell diagram. This gap is tied to the transition from partially- to fully-convective interiors in M dwarfs, and the effect of the associated stellar astrophysics on exoplanet evolution is currently unknown. The culmination of these system properties makes LHS 1678 a unique, compelling playground for comparative exoplanet science and understanding the formation and evolution of small, short-period exoplanets orbiting low-mass stars.},

note = {arXiv: 2110.12079},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{barragan_young_2021,

title = {The young HD 73583 (TOI-560) planetary system: Two 10-M$_textbackslashoplus$ mini-Neptunes transiting a 750-Myr-old, bright, and active K dwarf},

author = {Barrag\'{a}n, O. and Armstrong, D. J. and Gandolfi, D. and Carleo, I. and Vidotto, A. A. and D'Angelo, C. Villarreal and Oklop\v{c}i\'{c}, A. and Isaacson, H. and Oddo, D. and Collins, K. and Fridlund, M. and Sousa, S. G. and Persson, C. M. and Hellier, C. and Howell, S. and Howard, A. and Redfield, S. and Eisner, N. and Georgieva, I. Y. and Dragomir, D. and Bayliss, D. and Nielsen, L. D. and Klein, B. and Aigrain, S. and Zhang, M. and Teske, J. and Twicken, J. D. and Jenkins, J. and Esposito, M. and Van Eylen, V. and Rodler, F. and Adibekyan, V. and Alarcon, J. and Anderson, D. R. and Murphy, J. M. Akana and Barrado, D. and Barros, S. C. C. and Benneke, B. and Bouchy, F. and Bryant, E. M. and Butler, P. and Burt, J. and Cabrera, J. and Casewell, S. and Chaturvedi, P. and Cloutier, R. and Cochran, W. D. and Crane, J. and Crossfield, I. and Crouzet, N. and Collins, K. I. and Dai, F. and Deeg, H. J. and Deline, A. and Demangeon, O. D. S. and Dumusque, X. and Figueira, P. and Furlan, E. and Gnilka, C. and Goad, M. R. and Goffo, E. and Guti\'{e}rrez-Canales, F. and Hadjigeorghiou, A. and Hartman, Z. and Hatzes, A. P. and Harris, M. and Henderson, B. and Hirano, T. and Hojjatpanah, S. and Hoyer, S. and Kab\'{a}th, P. and Korth, J. and Lillo-Box, J. and Luque, R. and Marmier, M. and Mo\v{c}nik, T. and Muresan, A. and Murgas, F. and Nagel, E. and Osborne, H. L. M. and Osborn, A. and Osborn, H. P. and Palle, E. and Raimbault, M. and Ricker, G. R. and Rubenzahl, R. A. and Stockdale, C. and Santos, N. C. and Scott, N. and Schwarz, R. P. and Shectman, S. and Raimbault, M. and Seager, S. and S\'{e}gransan, D. and Serrano, L. M. and Skarka, M. and Smith, A. M. S. and \v{S}ubjak, J. and Tan, T. G. and Udry, S. and Watson, C. and Wheatley, P. J. and West, R. and Winn, J. N. and Wang, S. X. and Wolfgang, A. and Ziegler, C.},

url = {http://arxiv.org/abs/2110.13069},

year  = {2021},

date = {2021-01-01},

urldate = {2021-11-06},

journal = {arXiv:2110.13069 [astro-ph]},

abstract = {We present the discovery and characterisation of two transiting planets discovered by TESS in the light curves of the young and bright (V=9.67) star HD 73583 (TOI-560). We perform an intensive spectroscopic and photometric space- and ground-based follow-up in order to confirm and characterise the system. We found that HD 73583 is a young (750 Myr) active star with a rotational period of $12.1$ d and a mass and radius of $ 0.71 M_textbackslashodot$ and $0.66 R_textbackslashodot$, respectively. HD 73583 b ($P_textbackslashrm b=$ $6.4$d) has a mass and radius of $10 M_textbackslashoplus$ and $2.83 textbackslashpm 0.10 R_textbackslashoplus$, respectively, that gives a density of $2.43 textbackslashrm gtextbackslash,cmtextasciicircum-3$. HD 73583 c ($P_textbackslashrm c= 18.9$ d) has a mass and radius of $9.6 M_textbackslashoplus$ and $2.37 R_textbackslashoplus$, respectively, this translates to a density of $3.97 textbackslashrm gtextbackslash,cmtextasciicircum-3$. Both planets are consistent with worlds made of a solid core surrounded by a thick envelope. Because of their youth and host star brightness, they both are excellent candidates to perform transmission spectroscopy studies and search for mass-loss signatures. We expect atmospheric mass-loss rates of $2.4 textbackslashtimes 10textasciicircum10textbackslash,textbackslashrm gtextbackslash,stextasciicircum-1$ and $5.4 textbackslashtimes 10textasciicircum9textbackslash,textbackslashrm gtextbackslash,stextasciicircum-1$ for HD73583 b and c, respectively. We expect that the detection of evaporating signatures on H and He would be challenging, but doable with present and future instruments.},

note = {arXiv: 2110.13069},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{mufti_toi_2021,

title = {TOI 560 : Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS and HIRES RVs},

author = {Mufti, Mohammed El and Plavchan, Peter P. and Isaacson, Howard and Cale, Bryson L. and Feliz, Dax L. and Reefe, Michael A. and Hellier, Coel and Stassun, Keivan and Eastman, Jason and Polanski, Alex and Crossfield, Ian J. M. and Gaidos, Eric and Kostov, Veselin and Villasenor, Joel and Schlieder, Joshua E. and Bouma, Luke G. and Collins, Kevin I. and Wittrock, Justin M. and Zohrabi, Farzaneh and Lee, Rena A. and Sohani, Ahmad and Berberian, John and Vermilion, David and Newman, Patrick and Geneser, Claire and Tanner, Angelle and Batalha, Natalie M. and Dressing, Courtney and Fulton, Benjamin and Howard, Andrew W. and Huber, Daniel and Kane, Stephen R. and Petigura, Erik A. and Robertson, Paul and Roy, Arpita and Weiss, Lauren M. and Behmard, Aida and Beard, Corey and Chontos, Ashley and Dai, Fei and Dalba, Paul A. and Fetherolf, Tara and Giacalone, Steven and Hill, Michelle L. and Hirsch, Lea A. and Holcomb, Rae and Lubin, Jack and Mayo, Andrew and Movcnik, Teo and Murphy, Joseph M. Akana and Rosenthal, Lee J. and Rubenzahl, Ryan A. and Scarsdale, Nicholas and Stockdale, Christopher and Collins, Karen and Cloutier, Ryan and Relles, Howard and Tan, Thiam-Guan and Scott, Nicholas J. and Hartman, Zach and Matthews, Elisabeth and Ciardi, David and Gonzales, Erica and Matson, Rachel A. and Beichman, Charles and Furlan, E. and Gnilka, Crystal L. and Howell, Steve B. and Ziegler, Carl and Briceno, Cesar and Law, Nicholas and Mann, Andrew W. and Rabus, Markus and Johnson, Marshall C. and Christiansen, Jessie and Kreidberg, Laura and Werner, Michael W. and Berardo, David Anthony and Deming, Drake and Gorjian, Varoujan and Morales, Farisa Y. and Benneke, Bj\"{o}rn and Dragomir, Diana and Wittenmyer, Robert A. and Ballard, Sarah and Bowler, Brendan P. and Horner, Jonathan and Kielkopf, John and Liu, Huigen and Shporer, Avi and Tinney, C. G. and Zhang, Hui and Wright, Duncan J. and Addison, Brett C. and Mengel, Matthew W. and Okumura, Jack},

url = {http://arxiv.org/abs/2112.13448},

year  = {2021},

date = {2021-01-01},

urldate = {2021-12-29},

journal = {arXiv:2112.13448 [astro-ph]},

abstract = {We validate the presence of a two-planet system orbiting the 0.2--1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, $P = 6.397438 textbackslashpm 0.000037$ days, $e=0.294textasciicircum0.13_0.062$) initially discovered in the Sector 8 textbackslashtesstextbackslash mission observations, and a transiting mini-Neptune (TOI 560 c, $P = 18.8779 textbackslashpm 0.0016$ days) discovered in the Sector 34 observations, in a rare 1:3 orbital resonance. We utilize photometric data from textbackslashtesstextbackslash, textbackslashtextitSpitzer, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets and vet false positive scenarios. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published PFS RVs from Magellan Observatory. We place upper limits on the masses of both planets of $textless$2.1 and $textless$4.1 M$_Nep$ for b and c, respectively. We apply a Gaussian Processes (GP) model to the textbackslashtesstextbackslash light curves to place priors on a chromatic radial velocity GP model to constrain the stellar activity of the TOI 560 host star. TOI 560 is a nearby moderately young multi-planet system with two planets suitable for atmospheric characterization with James Webb Space Telescope (JWST) and other upcoming missions. In particular, it will undergo six transit pairs separated by $textless$6 hours before June 2027.},

note = {arXiv: 2112.13448},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{2021MNRAS.tmp.3215Kb,

title = {Transit Timings Variations in the three-planet system: TOI-270},

author = {Laurel Kaye and Shreyas Vissapragada and Maximilian N. G\"{u}nther and Suzanne Aigrain and Thomas Mikal-Evans and Eric L. N. Jensen and Hannu Parvianinen and Francisco J. Pozuelos and Lyu Abe and Jack S. Acton and Abdelkrim Agabi and Douglas R. Alves and David R. Anderson and David J. Armstrong and Khalid Barkaoui and Oscar Barrag\'{a}n and Bj\"{o}rn Benneke and Patricia T. Boyd and Rafael Brahm and Ivan Bruni and Edward M. Bryant and Matthew R. Burleigh and Sarah L. Casewell and David Ciardi and Ryan Cloutier and Karen A. Collins and Kevin I. Collins and Dennis M. Conti and Ian J. M. Crossfield and Nicolas Crouzet and Tansu Daylan and Diana Dragomir and Georgina Dransfield and Daniel Fabrycky and Michael Fausnaugh and G\'{a}bor F\"{u}\"{u}r\'{e}sz and Tianjun Gan and Samuel Gill and Micha"el Gillon and Michael R. Goad and Varoujan Gorjian and Michael Greklek-McKeon and Natalia Guerrero and Tristan Guillot and Emmanu"el Jehin and J. S. Jenkins and Monika Lendl and Jacob Kamler and Stephen R. Kane and John F. Kielkopf and Michelle Kunimoto and Wenceslas Marie-Sainte and James McCormac and Djamel M\'{e}karnia and Farisa Y. Morales and Maximiliano Moyano and Enric Palle and Vivien Parmentier and Howard M. Relles and Fran\c{c}ois-Xavier Schmider and Richard P. Schwarz and S. Seager and Alexis M. S. Smith and Thiam-Guan Tan and Jake Taylor and Amaury H. M. J. Triaud and Joseph D. Twicken and Stephane Udry and J. I. Vines and Gavin Wang and Peter J. Wheatley and Joshua N. Winn},

doi = {10.1093/mnras/stab3483},

year  = {2021},

date = {2021-12-01},

journal = {Monthly Notices of the RAS},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{addison_toi-257b_2020,

title = {TOI-257b (HD 19916b): A Warm sub-Saturn on a Moderately Eccentric Orbit Around an Evolved F-type Star},

author = {Addison, Brett C. and Wright, Duncan J. and Nicholson, Belinda A. and Cale, Bryson and Mocnik, Teo and Huber, Daniel and Plavchan, Peter and Wittenmyer, Robert A. and Vanderburg, Andrew and Chaplin, William J. and Chontos, Ashley and Clark, Jake T. and Eastman, Jason D. and Ziegler, Carl and Brahm, Rafael and Carter, Bradley D. and Clerte, Mathieu and Espinoza, N\'{e}stor and Horner, Jonathan and Bentley, John and Kane, Stephen R. and Kielkopf, John F. and Laychock, Emilie and Mengel, Matthew W. and Okumura, Jack and Stassun, Keivan G. and Bedding, Timothy R. and Bowler, Brendan P. and Burnelis, Andrius and Collins, Michaela and Crossfield, Ian and Davis, Allen B. and Evensberget, Dag and Heitzmann, Alexis and Howell, Steve B. and Law, Nicholas and Mann, Andrew W. and Marsden, Stephen and O'Connor, James and Shporer, Avi and Stevens, Catherine and Tinney, C. G. and Tylor, Christopher and Wang, Songhu and Zhang, Hui and Henning, Thomas and Kossakowski, Diana and Ricker, George and Sarkis, Paula and Vanderspek, Roland and Latham, David W. and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Mireles, Ismael and Rowden, Pam and Pepper, Joshua and Daylan, Tansu and Schlieder, Joshua E. and Collins, Karen A. and Collins, Kevin I. and Tan, Thiam-Guan and Ball, Warrick H. and Basu, Sarbani and Buzasi, Derek L. and Campante, Tiago L. and Corsaro, Enrico and Gonz\'{a}lez-Cuesta, Luc\'{i}a and Davies, Guy R. and a, Rafael {textasciitilde}A {textasciitilde}Garc\'{i} and Guo, Zhao and Handberg, Rasmus and Hekker, Saskia and Hey, Daniel R. and Kallinger, Thomas and Kawaler, Steven D. and Kayhan, Cenk and Kuszlewicz, James S. and Lund, Mikkel N. and Lyttle, Alexander and Mathur, Savita and Miglio, Andrea and Mosser, Benoit and Nielsen, Martin B. and Serenelli, Aldo M. and Aguirre, Victor Silva and Themessl, Nathalie},

url = {http://arxiv.org/abs/2001.07345},

year  = {2020},

date = {2020-01-01},

urldate = {2020-02-06},

journal = {arXiv:2001.07345 [astro-ph]},

abstract = {We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by TESS and confirmed to be of planetary origin based on radial-velocity observations with the Minerva-Australis telescope array. An analysis of the TESS photometry, the Minerva-Australis, FEROS, and HARPS radial velocities, and the asteroseismic data of the stellar oscillations reveals that TOI-257b has a mass of $M_P=0.134textasciicircum+0.023_-0.022$$textbackslashrmM_J$ ($42.6textasciicircum+7.3_-7.0$$textbackslashrmM_textbackslashoplus$), a radius of $R_P=0.626textasciicircum+0.013_-0.012$$textbackslashrmR_J$ ($7.02textasciicircum+0.15_-0.13$$textbackslashrmR_textbackslashoplus$), and an orbit with eccentricity $0.242textasciicircum+0.040_-0.065$ and period $18.38827textbackslashpm0.00072$$textbackslashrmdays$. TOI-257b orbits a bright ($textbackslashmathrmV=7.570$mag) somewhat evolved late F-type star with $M_*=1.390textbackslashpm0.046$$textbackslashrmM_textbackslashodot$, $R_*=1.888textbackslashpm0.033$$textbackslashrmR_textbackslashodot$, $T_textbackslashrm eff=6075textbackslashpm90$$textbackslashrmK$, and $vtextbackslashsini=11.3textbackslashpm0.5$km/s. Additionally, we statistically validate a second non-transiting sub-Saturn mass planet on a $textbackslashsim71$day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars that have been characterized with asteroseismology. Warm sub-Saturns are rare in the known sample of exoplanets, and thus the discovery of TOI-257b is important in the context of future work studying the formation and migration history of similar planetary systems.},

note = {arXiv: 2001.07345},

keywords = {},

pubstate = {published},

tppubtype = {article}

}