@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}

}

@article{nielsen_three_2020,

title = {Three Short Period Jupiters from TESS},

author = {Nielsen, L. D. and Brahm, R. and Bouchy, F. and Espinoza, N. and Turner, O. and Rappaport, S. and Pearce, L. and Ricker, G. and Vanderspek, R. and Latham, D. W. and Seager, S. and Winn, J. N. and Jenkins, J. M. and Acton, J. S. and Bakos, G. and Barclay, T. and Barkaoui, K. and Bhatti, W. and Brice\~{n}o, C. and Bryant, E. M. and Burleigh, M. R. and Ciardi, D. R. and Collins, K. A. and Collins, K. I. and Cooke, B. F. and Csubry, Z. and Santos, L. A. dos and Eigm\"{u}ller, Ph and Fausnaugh, M. M. and Gan, T. and Gillon, M. and Goad, M. R. and Guerrero, N. and Hagelberg, J. and Hart, R. and Henning, T. and Huang, C. X. and Jehin, E. and Jenkins, J. S. and Jord\`{a}n, A. and Kielkopf, J. F. and Kossakowski, D. and Lavie, B. and Law, N. and Lendl, M. and de Leon, J. P. and Lovis, C. and Mann, A. W. and Marmier, M. and McCormac, J. and Mori, M. and Moyano, M. and Narita, N. and Osip, D. and Otegi, J. F. and Pepe, F. and Pozuelos, F. J. and Raynard, L. and Relles, H. M. and Sarkis, P. and Segransan, D. and Seidel, J. V. and Shporer, A. and Stalport, M. and Stockdale, C. and Suc, V. and Tamura, M. and Tan, T. G. and Tilbrook, R. H. and Ting, E. B. and Trifonov, T. and Udry, S. and Vanderburg, A. and Wheatley, P. J. and Wingham, G. and Zhan, Z. and Ziegler, C.},

url = {http://arxiv.org/abs/2003.05932},

year  = {2020},

date = {2020-01-01},

urldate = {2020-03-14},

journal = {arXiv:2003.05932 [astro-ph]},

abstract = {We report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V=11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 +/- 0.078 Mjup planet in a grazing transit configuration with impact parameter b = 1.17 +0.10/-0.08. As a result the radius is poorly constrained, 2.03 +0.61/-0.49 Rjup. We perform a full phase-curve analysis of the TESS data and detect both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass 1.18 +/- 0.13 Mjup and radius 1.29 +/- 0.02 Rjup. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V=12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V=12.4 G-type star. It has a mass of 0.79 +/- 0.06 Mjup and radius 1.09 +0.08/-0.05 Rjup. Despite having the longest orbital period (P=2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with Fe/H ranging from 0.18 - 0.24.},

note = {arXiv: 2003.05932},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{armstrong_remnant_2020,

title = {A remnant planetary core in the hot Neptunian desert},

author = {Armstrong, David J. and Lopez, Th\'{e}o A. and Adibekyan, Vardan and Booth, Richard A. and Bryant, Edward M. and Collins, Karen A. and Emsenhuber, Alexandre and Huang, Chelsea X. and King, George W. and Lillo-box, Jorge and Lissauer, Jack J. and Matthews, Elisabeth C. and Mousis, Olivier and Nielsen, Louise D. and Osborn, Hugh and Otegi, Jon and Santos, Nuno C. and Sousa, S\'{e}rgio G. and Stassun, Keivan G. and Veras, Dimitri and Ziegler, Carl and Acton, Jack S. and Almenara, Jose M. and Anderson, David R. and Barrado, David and Barros, Susana C. C. and Bayliss, Daniel and Belardi, Claudia and Bouchy, Francois and Briceno, C\'{e}sar and Brogi, Matteo and Brown, David J. A. and Burleigh, Matthew R. and Casewell, Sarah L. and Chaushev, Alexander and Ciardi, David R. and Collins, Kevin I. and Col\'{o}n, Knicole D. and Cooke, Benjamin F. and Crossfield, Ian J. M. and D\'{i}az, Rodrigo F. and Deleuil, Magali and Mena, Elisa Delgado and Demangeon, Olivier D. S. and Dorn, Caroline and Dumusque, Xavier and Eigmuller, Philipp and Fausnaugh, Michael and Figueira, Pedro and Gan, Tianjun and Gandhi, Siddharth and Gill, Samuel and Goad, Michael R. and Guenther, Maximilian N. and Helled, Ravit and Hojjatpanah, Saeed and Howell, Steve B. and Jackman, James and Jenkins, James S. and Jenkins, Jon M. and Jensen, Eric L. N. and Kennedy, Grant M. and Latham, David W. and Law, Nicholas and Lendl, Monika and Lozovsky, Michael and Mann, Andrew W. and Moyano, Maximiliano and McCormac, James and Meru, Farzana and Mordasini, Christoph and Osborn, Ares and Pollacco, Don and Queloz, Didier and Raynard, Liam and Ricker, George R. and Rowden, Pamela and Santerne, Alexandre and Schlieder, Joshua E. and Seager, S. and Sha, Lizhou and Tan, Thiam-Guan and Tilbrook, Rosanna H. and Ting, Eric and Udry, St\'{e}phane and Vanderspek, Roland and Watson, Christopher A. and West, Richard G. and Wilson, Paul A. and Winn, Joshua N. and Wheatley, Peter and Villasenor, Jesus Noel and Vines, Jose I. and Zhan, Zhuchang},

url = {http://arxiv.org/abs/2003.10314},

year  = {2020},

date = {2020-01-01},

urldate = {2020-04-11},

journal = {arXiv:2003.10314 [astro-ph]},

abstract = {The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to major uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary pathways provide a new route to understanding planetary interiors. We present the discovery of TOI-849b, the remnant core of a giant planet, with a radius smaller than Neptune but an anomalously high mass $M_p=40.8textasciicircum+2.4_-2.5M_textbackslashoplus$ and density of $5.5textbackslashpm0.8$gcm$textasciicircum-3$, similar to the Earth. Interior structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than $3.9textasciicircum+0.8_-0.9$% of the total mass of the planet. TOI-849b transits a late G type star (T$_textbackslashrm mag=11.5$) with an orbital period of 18.4 hours, leading to an equilibrium temperature of 1800K. The planet's mass is larger than the theoretical threshold mass for runaway gas accretion. As such, the planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it avoided substantial gas accretion, perhaps through gap opening or late formation. Photoevaporation rates cannot provide the mass loss required to reduce a Jupiter-like gas giant, but can remove a few $M_textbackslashoplus$ hydrogen and helium envelope on timescales of several Gyr, implying that any remaining atmosphere is likely to be enriched by water or other volatiles from the planetary interior. TOI-849b represents a unique case where material from the primordial core is left over from formation and available to study.},

note = {arXiv: 2003.10314},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{huang_tess_2020,

title = {TESS spots a hot Jupiter with an inner transiting Neptune},

author = {Huang, Chelsea X. and Quinn, Samuel N. and Vanderburg, Andrew and Becker, Juliette and Rodriguez, Joseph E. and Pozuelos, Francisco J. and Gandolfi, Davide and Zhou, George and Mann, Andrew W. and Collins, Karen A. and Crossfield, Ian and Barkaoui, Khalid and Collins, Kevin I. and Fridlund, Malcolm and Gillon, Micha\"{e}l and Gonzales, Erica J. and G\"{u}nther, Maximilian N. and Henry, Todd J. and Howell, Steve B. and James, Hodari-Sadiki and Jao, Wei-Chun and Jehin, Emmanu\"{e}l and Jensen, Eric L. N. and Kane, Stephen R. and Lissauer, Jack J. and Matthews, Elisabeth and Matson, Rachel A. and Paredes, Leonardo A. and Schlieder, Joshua E. and Stassun, Keivan G. and Shporer, Avi and Sha, Lizhou and Tan, Thiam-Guan and Georgieva, Iskra and Mathur, Savita and Palle, Enric and Persson, Carina M. and Van Eylen, Vincent and Ricker, George R. and Vanderspek, Roland K. and Latham, David W. and Winn, Joshua N. and Seager, S. and Jenkins, Jon M. and Burke, Christopher J. and Goeke, Robert F. and Rinehart, Stephen and Rose, Mark E. and Ting, Eric B. and Torres, Guillermo and Wong, Ian},

url = {https://arxiv.org/abs/2003.10852v1},

doi = {10.3847/2041-8213/ab7302},

year  = {2020},

date = {2020-03-01},

urldate = {2020-04-11},

abstract = {Hot Jupiters are rarely accompanied by other planets within a factor of a few 

in orbital distance. Previously, only two such systems have been found. Here, 

we report the discovery of a third system using data from the Transiting 

Exoplanet Survey Satellite (TESS). The host star, TOI-1130, is an 11th 

magnitude K-dwarf in the Gaia G band. It has two transiting planets: a 

Neptune-sized planet ($3.65textbackslashpm 0.10$ $R_E$) with a 4.1-day period, and a hot 

Jupiter ($1.50textasciicircum+0.27_-0.22$ $R_J$) with an 8.4-day period. Precise 

radial-velocity observations show that the mass of the hot Jupiter is 

$0.974textasciicircum+0.043_-0.044$ $M_J$. For the inner Neptune, the data provide only 

an upper limit on the mass of 0.17 $M_J$ (3$σ$). Nevertheless, we are 

confident the inner planet is real, based on follow-up ground-based photometry 

and adaptive optics imaging that rule out other plausible sources of the TESS 

transit signal. The unusual planetary architecture of and the brightness of the 

host star make TOI-1130 a good test case for planet formation theories, and an 

attractive target for future spectroscopic observations.},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{hirao_ogle-2017-blg-0406_2020,

title = {OGLE-2017-BLG-0406: Spitzer Microlens Parallax Reveals Saturn-mass Planet orbiting M-dwarf Host in the Inner Galactic Disk},

author = {Hirao, Yuki and Bennett, David P. and Ryu, Yoon-Hyun and Koshimoto, Naoki and Udalski, Andrzej and Yee, Jennifer C. and Sumi, Takahiro and Bond, Ian A. and Shvartzvald, Yossi and Abe, Fumio and Barry, Richard K. and Bhattacharya, Aparna and Donachie, Martin and Fukui, Akihiko and Itow, Yoshitaka and Kondo, Iona and Li, Man Cheung Alex and Matsubara, Yutaka and Matsuo, Taro and Miyazaki, Shota and Muraki, Yasushi and Nagakane, Masayuki and Onishi, Kohji and Ranc, Clement and Rattenbury, Nicholas J. and Suematsu, Haruno and Shibai, Hiroshi and Sullivan, Denis J. and Suzuki, Daisuke and Tristram, Paul J. and Yonehara, Atsunori and Skowron, J. and Poleski, R. and Mroz, P. and Szymanski, M. K. and Soszynski, I. and Kozlowski, S. and Pietrukowicz, P. and Ulaczyk, K. and Rybicki, K. and Iwanek, P. and Albrow, Michael D. and Chung, Sun-Ju and Gould, Andrew and Han, Cheongho and Hwang, Kyu-Ha and Jung, Youn Kil and Shin, In-Gu and Zang, Weicheng and Cha, Sang-Mok and Kim, Dong-Jin and Kim, Hyoun-Woo and Kim, Seung-Lee and Lee, Chung-Uk and Lee, Dong-Joo and Lee, Yongseok and Park, Byeong-Gon and Pogge, Richard W. and Beichman, Charles A. and Bryden, Geoffery and Novati, Sebastiano Calchi and Carey, Sean and Gaudi, B. Scott and Henderson, Calen B. and Zhu, Wei and Bachelet, Etienne and Bolt, Greg and Christie, Grant and Hundertmark, Markus and Natusch, Tim and Maoz, Dan and McCormick, Jennie and Street, Rachel A. and Tan, Thiam-Guan and Tsapras, Yiannis and Jorgensen, U. G. and Dominik, M. and Bozza, V. and Skottfelt, J. and Snodgrass, C. and Ciceri, S. and Jaimes, R. Figuera and Evans, D. F. and Peixinho, N. and Hinse, T. C. and Burgdorf, M. J. and Southworth, J. and Rahvar, S. and Sajadian, S. and Rabus, M. and von Essen, C. and Fujii, Y. I. and Campbell-White, J. and Lowry, S. and Helling, C. and Mancini, L. and Haikala, L. and Kandori, Ryo},

url = {http://arxiv.org/abs/2004.09067},

year  = {2020},

date = {2020-01-01},

urldate = {2020-04-25},

journal = {arXiv:2004.09067 [astro-ph]},

abstract = {We report the discovery and analysis of the planetary microlensing event OGLE-2017-BLG-0406, which was observed both from the ground and by the $textbackslashit Spitzer$ satellite in a solar orbit. At high magnification, the anomaly in the light curve was densely observed by ground-based-survey and follow-up groups, and it was found to be explained by a planetary lens with a planet/host mass ratio of $q=7.0 textbackslashtimes 10textasciicircum-4$ from the light-curve modeling. The ground-only and $textbackslashit Spitzer$-"only" data each provide very strong one-dimensional (1-D) constraints on the 2-D microlens parallax vector $textbackslashbftextbackslashpi_textbackslashrm E$. When combined, these yield a precise measurement of $textbackslashbftextbackslashpi_textbackslashrm E$, and so of the masses of the host $M_textbackslashrm host=0.56textbackslashpm0.07textbackslash,M_textbackslashodot$ and planet $M_textbackslashrm planet = 0.41 textbackslashpm 0.05textbackslash,M_textbackslashrm Jup$. The system lies at a distance $D_textbackslashrm L=5.2 textbackslashpm 0.5 textbackslash textbackslashrm kpc$ from the Sun toward the Galactic bulge, and the host is more likely to be a dusk population star according to the kinematics of the lens. The projected separation of the planet from the host is $a_textbackslashperp = 3.5 textbackslashpm 0.3 textbackslash textbackslashrm au$, i.e., just over twice the snow line. The Galactic-disk kinematics are established in part from a precise measurement of the source proper motion based on OGLE-IV data. By contrast, the $textbackslashit Gaia$ proper-motion measurement of the source suffers from a catastrophic $10textbackslash,textbackslashsigma$ error.},

note = {arXiv: 2004.09067},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{jordan_hats-37ab_2020,

title = {HATS-37Ab and HATS-38b: Two Transiting Hot Neptunes in the Desert},

author = {Jord\'{a}n, A. and Bakos, G. \'{A} and Bayliss, D. and Bento, J. and Bhatti, W. and Brahm, R. and Csubry, Z. and Espinoza, N. and Hartman, J. D. and Henning, Th and Mancini, L. and Penev, K. and Rabus, M. and Sarkis, P. and Suc, V. and de Val-Borro, M. and Zhou, G. and Butler, R. P. and Teske, J. and Crane, J. and Shectman, S. and Tan, T. G. and Thompson, I. and Wallace, J. J. and L\'{a}z\'{a}r, J. and Papp, I. and S\'{a}ri, P.},

url = {http://arxiv.org/abs/2007.07135},

year  = {2020},

date = {2020-01-01},

urldate = {2020-07-19},

journal = {arXiv:2007.07135 [astro-ph]},

abstract = {We report the discovery of two transiting Neptunes by the HATSouth survey. The planet HATS-37Ab has a mass of 0.099 +- 0.042 M_J (31.5 +- 13.4 M_earth) and a radius of 0.606 +- 0.016 R_J, and is on a P = 4.3315 days orbit around a V = 12.266 mag, 0.843 M_sun star with a radius of 0.877 R_sun. We also present evidence that the star HATS-37A has an unresolved stellar companion HATS-37B, with a photometrically estimated mass of 0.654 M_sun.The planet HATS-38b has a mass of 0.074 +- 0.011 M_J (23.5 +- 3.5 M_earth) and a radius of 0.614 +- 0.017 R_J, and is on a P = 4.3750 days orbit around a V = 12.411 mag, 0.890 M_sun star with a radius of 1.105 R_sun. Both systems appear to be old, with isochrone-based ages of 11.46 +0.79-1.45 Gyr, and 11.89 +- 0.60 Gyr, respectively. Both HATS-37Ab and HATS-38b lie in the Neptune desert and are thus examples of a population with a low occurrence rate. They are also among the lowest mass planets found from ground-based wide-field surveys to date.},

note = {arXiv: 2007.07135},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{borkovits_compact_2020,

title = {The Compact Triply Eclipsing Triple Star TIC 209409435 Discovered with TESS},

author = {Borkovits, T. and Rappaport, S. A. and Tan, T. G. and Gagliano, R. and Jacobs, T. and Huang, X. and Mitnyan, T. and Hambsch, F.-J. and Kaye, T. and Maxted, P. F. L. and P\'{a}l, A. and Schmitt, A. R.},

url = {http://arxiv.org/abs/2006.10449},

doi = {10.1093/mnras/staa1817},

issn = {0035-8711, 1365-2966},

year  = {2020},

date = {2020-01-01},

urldate = {2020-07-19},

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

volume = {496},

number = {4},

pages = {4624--4636},

abstract = {We report the discovery in $TESS$ Sectors 3 and 4 of a compact triply eclipsing triple star system. TIC 209409435 is a previously unknown eclipsing binary with a period of 5.717 days, and the presence of a third star in an outer eccentric orbit of 121.872 day period was found from two sets of third-body eclipses and from eclipse timing variations. The latter exhibit signatures of strong 3rd-body perturbations. After the discovery, we obtained follow-up ground-based photometric observations of several binary eclipses as well as another of the third-body eclipses. We carried out comprehensive analyses, including the simultaneous photodynamical modelling of $TESS$ and ground-based lightcurves (including both archival WASP data, and our own follow-up measurements), as well as eclipse timing variation curves. Also, we have included in the simultaneous fits multiple star spectral energy distribution data and theoretical PARSEC stellar isochrones. We find that the inner binary consists of near twin stars of mass 0.90 $M_textbackslashodot$ and radius 0.88 $R_textbackslashodot$. The third star is just 9% more massive and 18% larger in radius. The inner binary has a rather small eccentricity while the outer orbit has $e = 0.40$. The inner binary and outer orbit have inclination angles within 0.1$textasciicircumtextbackslashcirc$ and 0.2$textasciicircumtextbackslashcirc$ of 90$textasciicircumtextbackslashcirc$, respectively. The mutual inclination angle is $textbackslashlesssim 1/4textasciicircumtextbackslashcirc$. All of these results were obtained without radial velocity observations.},

note = {arXiv: 2006.10449},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{burt_toi-824_2020,

title = {TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert},

author = {Burt, Jennifer A. and Nielsen, Louise D. and Quinn, Samuel N. and Mamajek, Eric E. and Matthews, Elisabeth C. and Zhou, George and Seidel, Julia V. and Huang, Chelsea X. and Lopez, Eric and Soto, Maritza and Otegi, Jon and Stassun, Keivan G. and Kreidberg, Laura and Collins, Karen A. and Eastman, Jason D. and Rodriguez, Joseph E. and Halverson, Samuel P. and Teske, Johanna K. and Wang, Sharon X. and Butler, R. Paul and Bouchy, Fran\c{c}ois and Dumusque, Xavier and Segransen, Damien and Shectman, Stephen A. and Crane, Jeffrey D. and Feng, Fabo and Montet, Benjamin T. and Feinstein, Adina D. and Beletski, Yuri and Flowers, Erin and G{textbackslash}{"u}nther, Maximilian N. and Daylan, Tansu and Collins, Kevin I. and Conti, Dennis M. and Gan, Tianjun and Jensen, Eric L. N. and Kielkopf, John F. and Tan, Thiam Guan and Helled, Ravit and Dorn, Caroline and Haldemann, Jonas and Lissauer, Jack J. and Ricker, George R. and Vanderspek, Roland and Latham, David W. and Seager, S. and Winn, Joshua N. and Jenkins, Jon M. and Twicken, Joseph D. and Smith, Jeffrey C. and Tenenbaum, Peter and Cartwright, Scott and Barclay, Thomas and Pepper, Joshua and Esquerdo, Gilbert and Fong, William},

url = {http://arxiv.org/abs/2008.11732},

year  = {2020},

date = {2020-01-01},

urldate = {2020-08-29},

journal = {arXiv:2008.11732 [astro-ph]},

abstract = {We report the detection of a transiting hot Neptune exoplanet orbiting TOI-824 (SCR J1448-5735), a nearby (d = 64 pc) K4V star, using data from the textbackslashtextitTransiting Exoplanet Survey Satellite (TESS). The newly discovered planet has a radius, $R_textbackslashrmp$ = 2.93 $textbackslashpm$ 0.20 R$_textbackslashoplus$, and an orbital period of 1.393 days. Radial velocity measurements using the Planet Finder Spectrograph (PFS) and the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph confirm the existence of the planet and we estimate its mass to be $M_textbackslashrmp$ = 18.47 $textbackslashpm$ 1.84 M$_textbackslashoplus$. The planet's mean density is $textbackslashrho_textbackslashrmp$ = 4.03$textasciicircum+0.98_-0.78$ g cm$textasciicircum-3$ making it more than twice as dense as Neptune. TOI-824 b's high equilibrium temperature makes the planet likely to have a cloud free atmosphere, and thus an excellent candidate for follow up atmospheric studies. The detectability of TOI-824 b's atmosphere from both ground and space is promising and could lead to the detailed characterization of the most irradiated, small planet at the edge of the hot Neptune desert that has retained its atmosphere to date.},

note = {arXiv: 2008.11732},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{cunningham_kelt-tess_2020,

title = {A KELT-TESS Eclipsing Binary in a Young Triple System Associated with a "Stellar String" Theia 301},

author = {Cunningham, Joni-Marie Clark and Felix, Dax L. and Dixon, Don M. and Stassun, Keivan G. and Siverd, Robert J. and Zhou, George and tan, Thiam-Guan and James, David and Kuhn, Rudolf B. and Kounkel, Marina},

url = {http://arxiv.org/abs/2009.03872},

year  = {2020},

date = {2020-01-01},

urldate = {2020-09-09},

journal = {arXiv:2009.03872 [astro-ph]},

abstract = {HD 54236 is a nearby, wide common-proper-motion visual pair that has been previously identified as likely being very young by virtue of strong X-ray emission and lithium absorption. Here we report the discovery that the brighter member of the wide pair, HDtextasciitilde54236A, is itself an eclipsing binary (EB), comprising two near-equal solar-mass stars on a 2.4 d orbit. It represents a potentially valuable opportunity to expand the number of benchmark-grade EBs at young stellar ages. Using new observations of Ca2H\&K emission and lithium absorption in the wide K-dwarf companion, HD 54236B, we obtain a robust age estimate of 225 +/- 50 Myr for the system. This age estimate and Gaia proper motions show HD 54236 is associated with Theiatextasciitilde301, a newly discovered local "stellar string", which itself may be related to the AB Dor moving group through shared stellar members. Applying this age estimate to ABtextasciitildeDor itself alleviates reported tension between observation and theory that arises for the luminosity of the 90M_Jup star/brown dwarf AB Dor C when younger age estimates are used.},

note = {arXiv: 2009.03872},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{weiss_tess-keck_2020,

title = {The TESS-Keck Survey II: Masses of Three Sub-Neptunes Transiting the Galactic Thick-Disk Star TOI-561},

author = {Weiss, Lauren M. and Dai, Fei and Huber, Daniel and Brewer, John and Collins, Karen A. and Ciardi, David R. and Matthews, Elisabeth C. and Ziegler, Carl and Howell, Steve B. and Batalha, Natalie M. and Crossfield, Ian J. M. and Dressing, Courtney and Fulton, Benjamin and Howard, Andrew W. and Isaacson, Howard and Kane, Stephen R. and Petigura, Erik A. and Robertson, Paul and Roy, Arpita and Rubenzahl, Ryan A. and Claytor, Zachary R. and Stassun, Keivan G. and Chontos, Ashley and Giacalone, Steven and Dalba, Paul A. and Mocnik, Teo and Hill, Michelle L. and Beard, Corey and Murphy, Joseph M. Akana and Rosenthal, Lee J. and Behmard, Aida and van Zandt, Judah and Lubin, Jack and Kosiarek, Molly R. and Lund, Michael B. and Christiansen, Jessie L. and Matson, Rachel A. and Beichman, Charles A. and Schlieder, Joshua E. and Gonzales, Erica J. and Brice\~{n}o, C\'{e}sar and Law, Nicholas and Mann, Andrew W. and Collins, Kevin I. and Evans, Phil and Fukui, Akihiko and Jensen, Eric L. N. and Murgas, Felipe and Narita, Norio and Palle, Enric and Parviainen, Hannu and Schwarz, Richard P. and Tan, Thiam-Guan and Jenkins, Jon and Ricker, George and Winn, Joshua N.},

url = {http://arxiv.org/abs/2009.03071},

year  = {2020},

date = {2020-01-01},

urldate = {2020-09-09},

journal = {arXiv:2009.03071 [astro-ph]},

abstract = {We report the discovery of TOI-561, a multiplanet system containing an ultra-short period planet (USP), based on photometry from the NASA TESS Mission and ground-based follow-up. This bright ($V=10.2$) star hosts three small transiting planets: TOI-561 b (TOI-561.02},

note = {arXiv: 2009.03071},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{luque_planetary_2020,

title = {A planetary system with two transiting mini-Neptunes near the radius valley transition around the bright M dwarf TOI-776},

author = {Luque, R. and Serrano, L. M. and Molaverdikhani, K. and Nixon, M. C. and Livingston, J. H. and Guenther, E. W. and Pall\'{e}, E. and Madhusudhan, N. and Nowak, G. and Korth, J. and Cochran, W. D. and Hirano, T. and Chaturvedi, P. and Goffo, E. and Albrecht, S. and Barrag\'{a}n, O. and Brice\~{n}o, C. and Cabrera, J. and Charbonneau, D. and Cloutier, R. and Collins, K. A. and Collins, K. I. and Col\'{o}n, K. D. and Crossfield, I. J. M. and Csizmadia, Sz and Dai, F. and Deeg, H. J. and Esposito, M. and Fridlund, M. and Gandolfi, D. and Georgieva, I. and Glidden, A. and Goeke, R. F. and Grziwa, S. and Hatzes, A. P. and Henze, C. E. and Howell, S. B. and Irwin, J. and Jenkins, J. M. and Jensen, E. L. N. and K\'{a}bath, P. and Kidwell Jr., R. C. and Kielkopf, J. F. and Knudstrup, E. and Lam, K. W. F. and Latham, D. W. and Lissauer, J. J. and Mann, A. W. and Matthews, E. C. and Mireles, I. and Narita, N. and Paegert, M. and Persson, C. M. and Redfield, S. and Ricker, G. R. and Rodler, F. and Schlieder, J. E. and Scott, N. J. and Seager, S. and \v{S}ubjak, J. and Tan, T. G. and Ting, E. B. and Vanderspek, R. and Van Eylen, V. and Winn, J. N. and Ziegler, C.},

url = {http://arxiv.org/abs/2009.08338},

year  = {2020},

date = {2020-01-01},

urldate = {2020-09-20},

journal = {arXiv:2009.08338 [astro-ph]},

abstract = {We report the discovery and characterization of two transiting planets around the bright M1 V star LP 961-53 (TOI-776},

note = {arXiv: 2009.08338},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{brahm_toi-481_2020,

title = {TOI-481 b \& TOI-892 b: Two long period hot Jupiters from the Transiting Exoplanet Survey Satellite},

author = {Brahm, Rafael and Nielsen, Louise D. and Wittenmyer, Robert A. and Wang, Songhu and Rodriguez, Joseph E. and Espinoza, N\'{e}stor and Jones, Mat\'{i}as I. and Jord\'{a}n, Andr\'{e}s and Henning, Thomas and Hobson, Melissa and Kossakowski, Diana and Rojas, Felipe and Sarkis, Paula and Schlecker, Martin and Trifonov, Trifon and Shahaf, Sahar and Ricker, George and Vanderspek, Roland and Latham, David W. and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Addison, Brett C. and Bakos, G\'{a}sp\'{a}r \'{A} and Bhatti, Waqas and Bayliss, Daniel and Berlind, Perry and Bieryla, Allyson and Bouchy, Francois and Bowler, Brendan P. and Brice\~{n}o, C\'{e}sar and Brown, Timothy M. and Bryant, Edward M. and Caldwell, Douglas A. and Charbonneau, David and Collins, Karen A. and Davis, Allen B. and Esquerdo, Gilbert A. and Fulton, Benjamin J. and Guerrero, Natalia M. and Henze, Christopher E. and Hogan, Aleisha and Horner, Jonathan and Huang, Chelsea X. and Irwin, Jonathan and Kane, Stephen R. and Kielkopf, John and Mann, Andrew W. and Mazeh, Tsevi and McCormac, James and McCully, Curtis and Mengel, Matthew W. and Mireles, Ismael and Okumura, Jack and Plavchan, Peter and Quinn, Samuel N. and Rabus, Markus and Saesen, Sophie and Schlieder, Joshua E. and Segransan, Damien and Shiao, Bernie and Shporer, Avi and Siverd, Robert J. and Stassun, Keivan G. and Suc, Vincent and Tan, Thiam-Guan and Torres, Pascal and Tinney, Chris G. and Udry, Stephane and Vanzi, Leonardo and Vezie, Michael and Vines, Jose I. and Vuckovic, Maja and Wright, Duncan J. and Yahalomi, Daniel A. and Zapata, Abner and Zhang, Hui and Ziegler, Carl},

url = {http://arxiv.org/abs/2009.08881},

year  = {2020},

date = {2020-01-01},

urldate = {2020-09-21},

journal = {arXiv:2009.08881 [astro-ph]},

abstract = {We present the discovery of two new 10-day period giant planets from the Transiting Exoplanet Survey Satellite ($TESS$) mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481 b and TOI-892 b have similar radii ($0.99textbackslashpm0.01$ $textbackslashrm R_J$ and $1.07textbackslashpm0.02$ $textbackslashrm R_J$, respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses ($1.53textbackslashpm0.03$ $textbackslashrm M_J$ versus $0.95textbackslashpm0.07$ $textbackslashrm M_J$, respectively). Both planets orbit metal-rich stars ([Fe/H]= $+0.26textbackslashpm 0.05$ dex and [Fe/H] = $+0.24 textbackslashpm 0.05$ dex, for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a $textbackslashrm M_textbackslashstar$ = $1.14textbackslashpm0.02$ $textbackslashrm M_textbackslashodot$, $textbackslashrm R_textbackslashstar$ = $1.66textbackslashpm0.02$ $textbackslashrm R_textbackslashodot$ G-type star ($T_textbackslashrm eff$ = $5735 textbackslashpm 72$ K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892, on the other hand, is a F-type dwarf star ($T_textbackslashrm eff$ = $6261 textbackslashpm 80$ K), which has a mass of $textbackslashrm M_textbackslashstar$ = $1.28textbackslashpm0.03$ $textbackslashrm M_textbackslashodot$, and a radius of $textbackslashrm R_textbackslashstar$ = $1.39textbackslashpm0.02$ $textbackslashrm R_textbackslashodot$. TOI-481 b and TOI-892 b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.},

note = {arXiv: 2009.08881},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{sha_toi-954_2020,

title = {TOI-954 b and EPIC 246193072 b: Short-Period Saturn-Mass Planets that Test Whether Irradiation Leads to Inflation},

author = {Sha, Lizhou and Huang, Chelsea X. and Shporer, Avi and Rodriguez, Joseph E. and Vanderburg, Andrew and Brahm, Rafael and Hagelberg, Janis and Matthews, Elisabeth C. and Ziegler, Carl and Livingston, John H. and Stassun, Keivan G. and Wright, Duncan J. and Crane, Jeffrey D. and Espinoza, N\'{e}stor and Bouchy, Fran\c{c}ois and Bakos, G\'{a}sp\'{a}r \'{A} and Collins, Karen A. and Zhou, George and Bieryla, Allyson and Hartman, Joel D. and Wittenmyer, Robert A. and Nielsen, Louise D. and Plavchan, Peter and Bayliss, Daniel and Sarkis, Paula and Tan, Thiam-Guan and Cloutier, Ryan and Mancini, Luigi and Jord\'{a}n, Andr\'{e}s and Wang, Sharon and Henning, Thomas and Narita, Norio and Penev, Kaloyan and Teske, Johanna K. and Kane, Stephen R. and Mann, Andrew W. and Addison, Brett C. and Tamura, Motohide and Horner, Jonathan and Barbieri, Mauro and Burt, Jennifer A. and D\'{i}az, Mat\'{i}as R. and Crossfield, Ian J. M. and Dragomir, Diana and Drass, Holger and Feinstein, Adina D. and Zhang, Hui and Hart, Rhodes and Kielkopf, John F. and Jensen, Eric L. N. and Montet, Benjamin T. and Ottoni, Ga\"{e}l and Schwarz, Richard P. and Rojas, Felipe and Nespral, David Lopez Fdez and Torres, Pascal and Mengel, Matthew W. and Udry, St\'{e}phane and Zapata, Abner and Snoddy, Erin and Okumura, Jack and Ricker, George R. and Vanderspek, Roland K. and Latham, David W. and Winn, Joshua N. and Seager, Sara and Jenkins, Jon M. and Col\'{o}n, Knicole D. and Henze, Christopher E. and Krishnamurthy, Akshata and Ting, Eric B. and Vezie, Michael and Villanueva, Steven},

url = {http://arxiv.org/abs/2010.14436},

year  = {2020},

date = {2020-01-01},

urldate = {2020-10-31},

journal = {arXiv:2010.14436 [astro-ph]},

abstract = {We report the discovery of two short-period Saturn-mass planets, one transiting the G subgiant TOI-954 (TIC 44792534, $ V = 10.343 $, $ T = 9.78 $) observed in TESS Sectors 4 \& 5, and one transiting the G dwarf EPIC 246193072 ($ V = 12.70 $, $ K = 10.67 $) observed in K2 Campaigns 12 \& 19. We confirm and characterize these two planets with a variety of ground-based archival and follow-up observations, including photometry, reconnaissance spectroscopy, precise radial velocity, and high-resolution imaging. Combining all available data, we find that TOI-954 b has a radius of $0.852_-0.062textasciicircum+0.053 textbackslash, R_textbackslashmathrmJ$ and a mass of $0.174_-0.017textasciicircum+0.018 textbackslash, M_textbackslashmathrmJ$ and is in a 3.68 d orbit, while EPIC 246193072 b has a radius of $0.774_-0.024textasciicircum+0.026 textbackslash, R_textbackslashmathrmJ$ and a mass of $0.260_-0.022textasciicircum+0.020 textbackslash, M_textbackslashmathrmJ$ and is in a 12.46 d orbit. As TOI-954 b is 30 times more irradiated than EPIC 246193072 b but is more or less of the same size, these two planets provide an opportunity to test whether irradiation leads to inflation of Saturn-mass planets and contribute to future comparative studies that explore Saturn-mass planets at contrasting points in their lifetimes.},

note = {arXiv: 2010.14436},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{teske_magellan-tess_2020,

title = {The Magellan-TESS Survey I: Survey Description and Mid-Survey Results},

author = {Teske, Johanna and Wang, Sharon Xuesong and Wolfgang, Angie and Gan, Tianjun and Plotnykov, Mykhaylo and Armstrong, David J. and Butler, R. Paul and Cale, Bryson and Crane, Jeffrey D. and Howard, Ward and Jensen, Eric L. N. and Law, Nicholas and Shectman, Stephen A. and Plavchan, Peter and Valencia, Diana and Vanderburg, Andrew and Ricker, George and Vanderspek, Roland and Latham, Dave W. and Seager, Sara and Winn, Joshua W. and Jenkins, Jon M. and Adibekyan, Vardan and Barrado, David and Barros, Susana C. C. and Brown, David J. A. and Bryant, Edward M. and Burt, Jennifer and Caldwell, Douglas A. and Charbonneau, David and Cloutier, Ryan and Collins, Karen A. and Collins, Kevin I. and Colon, Nicole D. and Conti, Dennis M. and Demangeon, Olivier D. S. and Eastman, Jason D. and Elmufti, Mohammed and Feng, Fabo and Flowers, Erin and Guerrero, Natalia M. and Hojjatpanah, Saeed and Irwin, Jonathan M. and Isopi, Giovanni and Lillo-Box, Jorge and Mallia, Franco and Massey, Bob and Mori, Mayuko and Mullally, Susan E. and Narita, Norio and Nishiumi, Taku and Osborn, Ares and Paegert, Martin and de Leon, Jerome Pitogo and Quinn, Samuel N. and Reefe, Michael and Schwarz, Richard P. and Shporer, Avi and Soubkiou, Abderahmane and Sousa, S\'{e}rgio G. and Stockdale, Chris and Str\om, Paul A. and Tan, Thiam-Guan and Tenenbaum, Peter and Wheatley, Peter J. and Wittrock, Justin and Yahalomi, Daniel A. and Zohrabi, Farzaneh and Zouhair, Benkhaldoun},

url = {http://arxiv.org/abs/2011.11560},

year  = {2020},

date = {2020-01-01},

urldate = {2020-11-25},

journal = {arXiv:2011.11560 [astro-ph]},

abstract = {One of the most significant revelations from Kepler is that roughly one-third of Sun-like stars host planets which orbit their stars within 100 days and are between the size of Earth and Neptune. How do these super-Earth and sub-Neptune planets form, what are they made of, and do they represent a continuous population or naturally divide into separate groups? Measuring their masses and thus bulk densities can help address these questions of their origin and composition. To that end, we began the Magellan-TESS Survey (MTS), which uses Magellan II/PFS to obtain radial velocity (RV) masses of 30 transiting exoplanets discovered by TESS and develops an analysis framework that connects observed planet distributions to underlying populations. In the past, RV measurements of small planets have been challenging to obtain due to the faintness and low RV semi-amplitudes of most Kepler systems, and challenging to interpret due to the potential biases in the existing ensemble of small planet masses from non-algorithmic decisions for target selection and observation plans. The MTS attempts to minimize these biases by focusing on bright TESS targets and employing a quantitative selection function and multi-year observing strategy. In this paper, we (1) describe the motivation and survey strategy behind the MTS, (2) present our first catalog of planet mass and density constraints for 25 TESS Objects of Interest (TOIs; 20 in our population analysis sample, five that are members of the same systems), and (3) employ a hierarchical Bayesian model to produce preliminary constraints on the mass-radius (M-R) relation. We find qualitative agreement with prior mass-radius relations but some quantitative differences (abridged). The the results of this work can inform more detailed studies of individual systems and offer a framework that can be applied to future RV surveys with the goal of population inferences.},

note = {arXiv: 2011.11560},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{zhou_two_2020,

title = {Two young planetary systems around field stars with ages between 20-320 Myr from TESS},

author = {Zhou, George and Quinn, Samuel N. and Irwin, Jonathan and Huang, Chelsea X. and Collins, Karen A. and Bouma, Luke G. and Khan, Lamisha and Landrigan, Anaka and Vanderburg, Andrew M. and Rodriguez, Joseph E. and Latham, David W. and Torres, Guillermo and Douglas, Stephanie T. and Bieryla, Allyson and Esquerdo, Gilbert A. and Berlind, Perry and Calkins, Michael L. and Buchhave, Lars A. and Charbonneau, David and Collins, Kevin I. and Kielkopf, John F. and Jensen, Eric L. N. and Tan, Thiam-Guan and Hart, Rhodes and Carter, Brad and Stockdale, Christopher and Ziegler, Carl and Law, Nicholas and Mann, Andrew W. and Howell, Steve B. and Matson, Rachel A. and Scott, Nicholas J. and Furlan, Elise and White, Russel J. and Hellier, Coel and Anderson, David R. and West, Richard G. and Ricker, George and Vanderspek, Roland and Seager, Sara and Jenkins, Jon M. and Winn, Joshua N. and Mireles, Ismael and Rowden, Pamela and Yahalomi, Daniel A. and Wohler, Bill and Brasseur, Clara E. and Daylan, Tansu and Colo\'{n}, Knicole D.},

url = {http://arxiv.org/abs/2011.13349},

year  = {2020},

date = {2020-01-01},

urldate = {2020-12-03},

journal = {arXiv:2011.13349 [astro-ph]},

abstract = {Planets around young stars trace the early evolution of planetary systems. We report the discovery and validation of two planetary systems with ages $textbackslashlesssim 300$ Myr from observations by the Transiting Exoplanet Survey Satellite. TOI-251 is a 40-320 Myr old G star hosting a 2.74 +0.18/-0.18 REarth mini-Neptune with a 4.94 day period. TOI-942 is a 20-160 Myr old K star hosting a system of inflated Neptune-sized planets, with TOI-942b orbiting with a period of 4.32 days, with a radius of 4.81 +0.20/-0.20 REarth, and TOI-942c orbiting in a period of 10.16 days with a radius of 5.79 +0.19/-0.18 REarth. Though we cannot place either host star into a known stellar association or cluster, we can estimate their ages via their photometric and spectroscopic properties. Both stars exhibit significant photometric variability due to spot modulation, with measured rotation periods of $textbackslashsim 3.5$ days. These stars also exhibit significant chromospheric activity, with age estimates from the chromospheric calcium emission lines and X-ray fluxes matching that estimated from gyrochronology. Both stars also exhibit significant lithium absorption, similar in equivalent width to well-characterized young cluster members. TESS has the potential to deliver a population of young planet-bearing field stars, contributing significantly to tracing the properties of planets as a function of their age.},

note = {arXiv: 2011.13349},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{giacalone_vetting_2020,

title = {Vetting of 384 TESS Objects of Interest with TRICERATOPS and Statistical Validation of 12 Planet Candidates},

author = {Giacalone, Steven and Dressing, Courtney D. and Jensen, Eric L. N. and Collins, Karen A. and Ricker, George R. and Vanderspek, Roland and Seager, S. and Winn, Joshua N. and Jenkins, Jon M. and Barclay, Thomas and Barkaoui, Khalid and Cadieux, Charles and Charbonneau, David and Collins, Kevin I. and Conti, Dennis M. and Doyon, Rene and Evans, Phil and Ghachoui, Mourad and Gillon, Michael and Guerrero, Natalia M. and Hart, Rhodes and Jehin, Emmanuel and Kielkopf, John F. and McLean, Brian and Murgas, Felipe and Palle, Enric and Parviainen, Hannu and Pozuelos, Francisco J. and Relles, Howard M. and Shporer, Avi and Socia, Quentin and Stockdale, Chris and Tan, Thiam-Guan and Torres, Guillermo and Twicken, Joseph D. and Waalkes, William C. and Waite, Ian A.},

url = {http://arxiv.org/abs/2002.00691},

year  = {2020},

date = {2020-01-01},

urldate = {2020-12-06},

journal = {arXiv:2002.00691 [astro-ph]},

abstract = {We present TRICERATOPS, a new Bayesian tool that can be used to vet and validate TESS Objects of Interest (TOIs). We test the tool on 68 TOIs that have been previously confirmed as planets or rejected as astrophysical false positives. By looking in the false positive probability (FPP) -- nearby false positive probability (NFPP) plane, we define criteria that TOIs must meet to be classified as validated planets (FPP textless 0.015 and NFPP textless 10textasciicircum-3), likely planets (FPP textless 0.5 and NFPP textless 10textasciicircum-3), and likely nearby false positives (NFPP textgreater 10textasciicircum-1). We apply this procedure on 384 unclassified TOIs and statistically validate 12, classify 125 as likely planets, and classify 52 as likely nearby false positives. Of the 12 statistically validated planets, 9 are newly validated. TRICERATOPS is currently the only TESS vetting and validation tool that models transits from nearby contaminant stars in addition to the target star. We therefore encourage use of this tool to prioritize follow-up observations that confirm bona fide planets and identify false positives originating from nearby stars.},

note = {arXiv: 2002.00691},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{johns_kelt-23b:_2019,

title = {KELT-23b: A Hot Jupiter Transiting a Near-Solar Twin Close to the TESS and JWST Continuous Viewing Zones},

author = {Johns, Daniel and Reed, Phillip and Rodriguez, Joseph and Pepper, Joshua and Stassun, Keivan and Penev, Kaloyan and Gaudi, B. Scott and Labadie-Bartz, Jonathan and Fulton, Benjamin and Quinn, Samuel and Eastman, Jason and Ciardi, David and Hirsch, Lea and Stevens, Daniel and Stevens, Catherine and Oberst, Thomas and Cohen, David and Jensen, Eric and Benni, Paul and Villanueva, Steven and Murawski, Gabriel and Bieryla, Allyson and Latham, David and Vanaverbeke, Siegfried and Dubois, Franky and Rau, Steve and Logie, Ludwig and Rauenzahn, Ryan and Wittenmyer, Robert and Zambelli, Roberto and Bayliss, Daniel and Beatty, Thomas and Collins, Karen and Colon, Knicole and Curtis, Ivan and Evans, Phil and Gregorio, Joao and James, David and DePoy, Darren and Johnson, Marshall and Joner, Michael and Kasper, David and Kielkopf, John and Kuhn, Rudolf and Lund, Michael and Manner, Mark and Marshall, Jennifer and McLeod, Kim and Penny, Matthew and Relles, Howard M. and Siverd, Robert and Stephens, Denise and Stockdale, Chris and Tan, Thiam-Guan and Trueblood, Mark and Trueblood, Patricia and Yao, Xinyu},

url = {http://arxiv.org/abs/1903.00031},

year  = {2019},

date = {2019-01-01},

urldate = {2019-03-15},

journal = {arXiv:1903.00031 [astro-ph]},

abstract = {We announce the discovery of KELT-23b, a hot Jupiter transiting the relatively bright ($V=10.3$) star BD+66 911 (TYC 4187-996-1), and characterize the system using follow-up photometry and spectroscopy. A global fit to the system yields $T_eff=5900textbackslashpm49 K$, $M_*=0.945textasciicircum+0.060_-0.054 M_textbackslashodot$, $R_*=0.995textbackslashpm0.015 R_textbackslashodot$, $L_*=1.082textasciicircum+0.051_-0.048 L_textbackslashodot$, log$g_*=4.418textasciicircum+0.026_-0.025$ (cgs), and $textbackslashleft[textbackslashrm Fe/textbackslashrm Htextbackslashright]=-0.105textbackslashpm49$. KELT-23b is a hot Jupiter with mass $M_P=0.938textasciicircum+0.045_-0.042 M_textbackslashrm J$, radius $R_P=1.322textbackslashpm0.025 R_textbackslashrm J$, and density $textbackslashrho_P=0.504textasciicircum+0.038_-0.035$ g cm$textasciicircum-3$. Intense insolation flux from the star has likely caused KELT-23b to become inflated. The time of inferior conjunction is $T_0=2458149.40776textbackslashpm0.00091textasciitildetextbackslashrm BJD_TDB$ and the orbital period is $P=2.255353textasciicircum+0.000031_-0.000030$ days. Due to strong tidal interactions, the planet is likely to spiral into its host within roughly a Gyr. This system has one of the highest positive ecliptic latitudes of all transiting planet hosts known to date, placing it near the Transiting Planet Survey Satellite and James Webb Space Telescope continuous viewing zones. Thus we expect it to be an excellent candidate for long-term monitoring and follow-up with these facilities.},

note = {arXiv: 1903.00031},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{osborn_pds_2019,

title = {The PDS 110 observing campaign - photometric and spectroscopic observations reveal eclipses are aperiodic},

author = {Osborn, Hugh P. and Kenworthy, Matthew and Rodriguez, Joseph E. and de Mooij, Ernst J. W. and Kennedy, Grant M. and Relles, Howard and Gomez, Edward and Hippke, Michael and Banfi, Massimo and Barbieri, Lorenzo and Becker, Igor and Benni, Paul and Berlind, Perry and Bieryla, Allyson and Bonnoli, Giacomo and Boussier, Hubert and Brincat, Stephen and Briol, John and Burleigh, Matthew and Butterley, Tim and Calkins, Michael L. and Chote, Paul and Ciceri, Simona and Deldem, Marc and Dhillon, Vik S. and Dose, Eric and Dubois, Frank and Dvorak, Shawn and Esquerdo, Gilbert A. and Evans, Daniel and Berangez, Stephane Ferratfiat Dagot and Fossey, Stephen and G\"{u}enther, Maximilian N. and Hall, John and Hambsch, Josch and Casas, Enrique Herrero and Hills, Kevin and James, Robert and Kafka, Stella and Killestein, Thomas L. and Kotnik, Clifford and Latham, David W. and Lemay, Damien and Lewin, Pablo and Littlefair, Stuart and Lopresti, Claudio and Mallonn, Matthias and Mancini, Luigi and Marchini, Alessandro and McCormac, James J. and Murawski, Gabriel and Myers, Gordon and Papini, Ricardo and Popov, Velimir and Quadri, Ulisse and Quinn, Samuel N. and Raynard, Liam and Rizzuti, Luca and Roa, James and Robertson, Jeff and Salvaggio, Fabio and Scholz, Alexander and Sfair, Rafael and Smith, Alexis M. S. and Southworth, John and Tan, T. G. and Vanaverbeke, Sigfried and Waagen, Elizabeth O. and Watson, Christopher and West, Richard and Wheatley, P. J. and Wilson, Richard W. and Winter, Othon C. and Zhou, George},

url = {http://arxiv.org/abs/1901.07981},

doi = {10.1093/mnras/stz283},

issn = {0035-8711, 1365-2966},

year  = {2019},

date = {2019-01-01},

urldate = {2019-03-15},

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

volume = {485},

number = {2},

pages = {1614--1625},

abstract = {PDS 110 is a young disk-hosting star in the Orion OB1A association. Two dimming events of similar depth and duration were seen in 2008 (WASP) and 2011 (KELT), consistent with an object in a closed periodic orbit. In this paper we present data from a ground-based observing campaign designed to measure the star both photometrically and spectroscopically during the time of predicted eclipse in September 2017. Despite high-quality photometry, the predicted eclipse did not occur, although coherent structure is present suggesting variable amounts of stellar flux or dust obscuration. We also searched for RV oscillations caused by any hypothetical companion and can rule out close binaries to 0.1 $M_textbackslashodot$. A search of Sonneberg plate archive data also enabled us to extend the photometric baseline of this star back more than 50 years, and similarly does not re-detect any deep eclipses. Taken together, they suggest that the eclipses seen in WASP and KELT photometry were due to aperiodic events. It would seem that PDS 110 undergoes stochastic dimmings that are shallower and shorter-duration than those of UX Ori variables, but may have a similar mechanism.},

note = {arXiv: 1901.07981},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{zhou_two_2019,

title = {Two new HATNet hot Jupiters around A stars, and the first glimpse at the occurrence rate of hot Jupiters from TESS},

author = {Zhou, G. and Huang, C. and Bakos, G. and Hartman, J. and Latham, D. and Quinn, S. and Collins, K. and Winn, J. and Kovacs, G. and Csubry, Z. and Bhatti, W. and Penev, K. and Bieryla, A. and Esquerdo, G. and Berlind, P. and Calkins, M. and de Val-Borro, M. and Noyes, R. and L\'{a}z\'{a}r, J. and Papp, I. and Sari, P. and Kovacs, T. and Buchhave, Lars A. and Szklen\'{a}r, T. and Beky, B. and Johnson, M. and Stassun, K. and Shporer, A. and Wong, I. and Espinoza, N. and Bayliss, D. and Howell, S. and Hellier, C. and Anderson, D. and West, R. and Brown, D. and Schanche, N. and Barkaoui, K. and Pozuelos, F. and Gillon, M. and Jehin, E. and Benkhaldoun, Z. and Daassou, A. and Ricker, G. and Vanderspek, R. and Seager, S. and Jenkins, J. and Lissauer, J. and Collins, K. and Gan, T. and Hart, R. and Horne, K. and Kielkopf, J. and Nielsen, L. and Nishiumi, T. and Narita, N. and Palle, E. and Relles, H. and Sefako, R. and Tan, T. and Davies, M. and Goeke, Robert F. and Guerrero, N. and Haworth, K. and Villanueva, S.},

url = {http://arxiv.org/abs/1906.00462},

year  = {2019},

date = {2019-01-01},

urldate = {2019-06-12},

journal = {arXiv:1906.00462 [astro-ph]},

abstract = {Wide field surveys for transiting planets are well suited to searching diverse stellar populations, enabling a better understanding of the link between the properties of planets and their parent stars. We report the discovery of HAT-P-69 b (TOI 625.01) and HAT-P-70 b (TOI 624.01), two new hot Jupiters around A stars from the HATNet survey which have also been observed by the Transiting Exoplanet Survey Satellite (TESS). HAT-P-69 b has a mass of 3.73 (+0.61/-0.59) Mjup and a radius of 1.626 (+0.032/-0.025) Rjup, and is in a prograde 4.79-day orbit around a star of mass 1.698+/-0.025 Msun and radius 1.854 (+0.043/-0.022) Rsun. HAT-P-70 b has a radius of 1.87 (+0.15/-0.10) Rjup and a mass constraint of textless6.78 (3sigma) Mjup, and is in a retrograde 2.74-day orbit around a star of mass 1.890 (+0.010/-0.013) Msun and radius 1.858 (+0.119/-0.091) Rsun. We use the confirmation of these planets around relatively massive stars as an opportunity to explore the occurrence rate of hot Jupiters as a function of stellar mass. We define a sample of 47,126 main-sequence stars brighter than Tmag=10 that yields 31 giant planet candidates, including 18 confirmed planets, 3 candidates, and 10 false positives. We find a net hot Jupiter occurrence rate of 0.45+/-0.10% within this sample, consistent with the rate measured by Kepler for FGK stars. When divided into stellar mass bins, we find the occurrence rate to be 0.71+/-0.31% G stars, 0.43+/-0.15% for F stars, and 0.32+/-0.12% for A stars. Thus, at this point, we cannot discern any statistically significant trend in the occurrence of hot Jupiters with stellar mass.},

note = {arXiv: 1906.00462},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{rodriguez_kelt-24b:_2019,

title = {KELT-24b: A 5M$_textbackslashrm J$ Planet on a 5.6 day Well-Aligned Orbit around the Young V=8.3 F-star HD 93148},

author = {Rodriguez, Joseph E. and Eastman, Jason D. and Zhou, George and Quinn, Samuel N. and Beatty, Thomas G. and Penev, Kaloyan and Johnson, Marshall C. and Cargile, Phillip A. and Latham, David W. and Bieryla, Allyson and Collins, Karen A. and Dressing, Courtney D. and Ciardi, David R. and Relles, Howard M. and Murawski, Gabriel and Nishiumi, Taku and Yonehara, Atsunori and Lund, Michael B. and Stevens, Daniel J. and Stassun, Keivan G. and Gaudi, B. Scott and Col\'{o}n, Knicole D. and Pepper, Joshua and Narita, Norio and Awiphan, Supachai and Chuanraksasat, Pongpichit and Benni, Paul and Ishimaru, Ryo and Yoshida, Fumi and Zambelli, Roberto and Garrison, Lehman H. and Wilson, Maurice L. and Cornachione, Matthew A. and Wang, Sharon X. and Labadie-Bartz, Jonathan and Rodr\'{i}guez, Romy and Siverd, Robert J. and Yao, Xinyu and Bayliss, Daniel and Berlind, Perry and Calkins, Michael L. and Christiansen, Jessie L. and Cohen, David H. and Conti, Dennis M. and Curtis, Ivan A. and Depoy, D. L. and Esquerdo, Gilbert A. and Evans, Phil and Feliz, Dax and Fulton, Benjamin J. and Gregorio, Joao and Holoien, Thomas W. S. and James, David J. and Jayasinghe, Tharindu and Jang-Condell, Hannah and Jensen, Eric L. N. and Johnson, John A. and Joner, Michael D. and Kielkopf, John F. and Kuhn, Rudolf B. and Manner, Mark and Marshall, Jennifer L. and McLeod, Kim K. and McCrady, Nate and Oberst, Thomas E. and Oelkers, Ryan J. and Penny, Matthew T. and Reed, Phillip A. and Sliski, David H. and Shappee, B. J. and Stephens, Denise C. and Stockdale, Chris and Tan, Thiam-Guan and Trueblood, Mark and Trueblood, Pat and Villanueva Jr., Steven and Wittenmyer, Robert A. and Wright, Jason T.},

url = {http://arxiv.org/abs/1906.03276},

year  = {2019},

date = {2019-06-01},

urldate = {2019-06-12},

journal = {arXiv:1906.03276 [astro-ph]},

abstract = {We present the discovery of KELT-24 b, a massive hot Jupiter orbiting a bright (V=8.3 mag},

note = {arXiv: 1906.03276},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{mancini_highly_2019,

title = {The highly inflated giant planet WASP-174b},

author = {Mancini, L. and Sarkis, P. and Henning, Th and Bakos, G. A. and Bayliss, D. and Bento, J. and Bhatti, W. and Brahm, R. and Csubry, Z. and Espinoza, N. and Hartman, J. and Jordan, A. and Penev, K. and Rabus, M. and Suc, V. and de Val-Borro, M. and Zhou, G. and Chen, G. and Damasso, M. and Southworth, J. and Tan, T. G.},

url = {http://arxiv.org/abs/1909.08674},

year  = {2019},

date = {2019-01-01},

urldate = {2019-09-20},

journal = {arXiv:1909.08674 [astro-ph]},

abstract = {The transiting exoplanetary system WASP-174 was reported to be composed by a main-sequence F star (V=11.8 mag) and a giant planet, WASP-174b (orbital period 4.23 days). However only an upper limit was placed on the planet mass (textless1.3 Mj), and a highly uncertain planetary radius (0.7-1.7 Rj) was determined. We aim to better characterise both the star and the planet and precisely measure their orbital and physical parameters. In order to constrain the mass of the planet, we obtained new measurements of the radial velocity of the star and joined them with those from the discovery paper. Photometric data from the HATSouth survey and new multi-band, high-quality (precision reached up to 0.37textasciitildemmag) photometric follow-up observations of transit events were acquired and analysed for getting accurate photometric parameters. We fit the model to all the observations, including data from the TESS space telescope, in two different modes: incorporating the stellar isochrones into the fit, and using an empirical method to get the stellar parameters. The two modes resulted to be consistent with each other to within 2 sigma. We confirm the grazing nature of the WASP-174b transits with a confidence level greater than 5 sigma, which is also corroborated by simultaneously observing the transit through four optical bands and noting how the transit depth changes due to the limb-darkening effect. We estimate that textasciitilde76% of the disk of the planet actually eclipses the parent star at mid-transit of its transit events. We find that WASP-174b is a highly-inflated hot giant planet with a mass of 0.330 Mj and a radius of 1.435 Rj, and is therefore a good target for transmission-spectroscopy observations. With a density of 0.135 g/cmtextasciicircum3, it is amongst the lowest-density planets ever discovered with precisely measured mass and radius.},

note = {arXiv: 1909.08674},

keywords = {},

pubstate = {published},

tppubtype = {article}

}