@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}

}

@article{petrucci_discarding_2019,

title = {Discarding orbital decay in WASP-19b after one decade of transit observations},

author = {Petrucci, R. and Jofr\'{e}, E. and Chew, Y. G\'{o}mez Maqueo and Hinse, T. C. and Ma\v{s}ek, M. and Tan, T.-G. and G\'{o}mez, M.},

url = {http://arxiv.org/abs/1910.11930},

year  = {2019},

date = {2019-01-01},

urldate = {2019-10-29},

journal = {arXiv:1910.11930 [astro-ph]},

abstract = {We present a empirical study of orbital decay for the exoplanet WASP-19b, based on mid-time measurements of 74 complete transits (12 newly obtained by our team and 62 from the literature), covering a 10-year baseline. A linear ephemeris best represents the mid-transit times as a function of epoch. Thus, we detect no evidence of the shortening of WASP-19b's orbital period and establish an upper limit of its steady changing rate, $textbackslashdotP=-2.294$ ms $yrtextasciicircum-1$, and a lower limit for the modified tidal quality factor $Q'_textbackslashstar = (1.23 textbackslashpm 0.231) textbackslashtimes 10textasciicircum6$. Both are in agreement with previous works. This is the first estimation of $Q'_textbackslashstar$ directly derived from the mid-times of WASP-19b obtained through homogeneously analyzed transit measurements. Additionally, we do not detect periodic variations in the transit timings within the measured uncertainties in the mid-times of transit. We are therefore able to discard the existence of planetary companions in the system down to a few $M_textbackslashmathrmtextbackslashoplus$ in the first order mean-motion resonances 1:2 and 2:1 with WASP-19b, in the most conservative case of circular orbits. Finally, we measure the empirical $Q'_textbackslashstar$ values of 15 exoplanet host stars which suggest that stars with $T_textbackslashmathrmeff$ $textbackslashlesssim$ 5600K dissipate tidal energy more efficiently than hotter stars. This tentative trend needs to be confirmed with a larger sample of empirically measured $Q'_textbackslashstar$.},

note = {arXiv: 1910.11930},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{diaz_toi-132_2019,

title = {TOI-132 b: A short-period planet in the Neptune desert transiting a $V=11.3$ G-type star},

author = {D\'{i}az, Mat\'{i}as R. and Jenkins, James S. and Gandolfi, Davide and Lopez, Eric D. and Soto, Maritza G. and Cort\'{e}s-Zuleta, P\'{i}a and Berdi\~{n}as, Zaira M. and Stassun, Keivan G. and Collins, Karen A. and Vines, Jos\'{e} I. and Ziegler, Carl and Fridlund, Malcolm and Jensen, Eric J. N. and Murgas, Felipe and Santerne, Alexandre and Wilson, Paul A. and Esposito, Massimiliano and Hatzes, Artie P. and Johnson, Marshall C. and Lam, Kristine W. F. and Livingston, John H. and Van Eylen, Vincent and Narita, Norio and Brice\~{n}o, C\'{e}sar and Collins, Kevin I. and Csizmadia, Szilard and Fausnaugh, Michael and Gan, Tianjun and Georgieva, Iska and Glidden, Ana and Jenkins, Jon M. and Latham, David W. and Law, Nicholas M. and Mann, Andrew W. and Mathur, Savita and Mireles, Ismael and Morris, Robert and Pall\'{e}, Enric and Persson, Carina M. and Rinehart, Stephen and Rose, Mark E. and Seager, Sara and Smith, Jeffrey C. and Tan, Thiam-Guan and Tokovinin, Andrei and Vanderburg, Andrew and Vanderspek, Roland and Yahalomi, Daniel A.},

url = {http://arxiv.org/abs/1911.02012},

year  = {2019},

date = {2019-01-01},

urldate = {2019-11-11},

journal = {arXiv:1911.02012 [astro-ph]},

abstract = {The Neptune desert is a feature seen in the radius-mass-period plane, whereby a notable dearth of short period, Neptune-like planets is found. Here we report the textbackslashtesstextbackslash, discovery of a new short-period planet in the Neptune desert, orbiting the G-type dwarf TYCtextbackslash,8003-1117-1 (TOI-132). textbackslashit TESS photometry shows transit-like dips at the level of $textbackslashsim$1400 ppm occurring every $textbackslashsim$2.11 days. High-precision radial velocity follow-up with HARPS confirmed the planetary nature of the transit signal and provided a semi-amplitude radial velocity variation of $textbackslashsim$11.5 m s$textasciicircum-1$, which, when combined with the stellar mass of $0.97textbackslashpm0.06$ $M_textbackslashodot$, provides a planetary mass of 22.83$textasciicircum+1.81_-1.80$ $M_textbackslashoplus$. Modeling the textbackslashit TESS high-quality light curve returns a planet radius of 3.43$textasciicircum+0.13_-0.14$ $R_textbackslashoplus$, and therefore the planet bulk density is found to be 3.11$textasciicircum+0.44_-0.450$ g cm$textasciicircum-3$. Planet structure models suggest that the bulk of the planet mass is in the form of a rocky core, with an atmospheric mass fraction of 4.3$textasciicircum+1.2_-2.3$textbackslash%. TOI-132 b is a textbackslashit TESS Level 1 Science Requirement candidate, and therefore priority follow-up will allow the search for additional planets in the system, whilst helping to constrain low-mass planet formation and evolution models, particularly valuable for better understanding the Neptune desert.},

note = {arXiv: 1911.02012},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{2019NatAs.tmp..420G,

title = {A super-Earth and two sub-Neptunes transiting the nearby and quiet M dwarf TOI-270},

author = {{G{"u}nther}, Maximilian N. and {Pozuelos}, Francisco J. and 

 {Dittmann}, Jason A. and {Dragomir}, Diana and {Kane}, Stephen R. and 

 {Daylan}, Tansu and {Feinstein}, Adina D. and {Huang}, Chelsea X. and 

 {Morton}, Timothy D. and {Bonfanti}, Andrea and {Bouma}, L.~G. and 

 {Burt}, Jennifer and {Collins}, Karen A. and {Lissauer}, Jack J. and 

 {Matthews}, Elisabeth and {Montet}, Benjamin T. and {Vand 

 erburg}, Andrew and {Wang}, Songhu and {Winters}, Jennifer G. and 

 {Ricker}, George R. and {Vanderspek}, Roland K. and {Latham}, David W. and 

 {Seager}, Sara and {Winn}, Joshua N. and {Jenkins}, Jon M. and 

 {Armstrong}, James D. and {Barkaoui}, Khalid and {Batalha}, Natalie and 

 {Bean}, Jacob L. and {Caldwell}, Douglas A. and {Ciardi}, David R. and 

 {Collins}, Kevin I. and {Crossfield}, Ian and {Fausnaugh}, Michael and 

 {Furesz}, Gabor and {Gan}, Tianjun and {Gillon}, Micha{"e}l and 

 {Guerrero}, Natalia and {Horne}, Keith and {Howell}, Steve B. and {Ireland 

 }, Michael and {Isopi}, Giovanni and {Jehin}, Emmanu{"e}l and 

 {Kielkopf}, John F. and {Lepine}, Sebastien and {Mallia}, Franco and 

 {Matson}, Rachel A. and {Myers}, Gordon and {Palle}, Enric and 

 {Quinn}, Samuel N. and {Relles}, Howard M. and 

 {Rojas-Ayala}, B{'a}rbara and {Schlieder}, Joshua and 

 {Sefako}, Ramotholo and {Shporer}, Avi and {Su{'a}rez}, Juan C. and 

 {Tan}, Thiam-Guan and {Ting}, Eric B. and {Twicken}, Joseph D. and 

 {Waite}, Ian A.},

doi = {10.1038/s41550-019-0845-5},

year  = {2019},

date = {2019-07-01},

journal = {Nature Astronomy},

pages = {420},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{martinez_kelt-25b_2019,

title = {KELT-25b and KELT-26b: A Hot Jupiter and a Substellar Companion Transiting Young A-stars Observed by TESS},

author = {Mart\'{i}nez, Romy Rodr\'{i}guez and Gaudi, B. Scott and Rodriguez, Joseph E. and Zhou, George and Labadie-Bartz, Jonathan and Quinn, Samuel N. and Penev, Kaloyan Minev and Tan, Thiam-Guan and Latham, David W. and Paredes, Leonardo A. and Kielkopf, John and Addison, Brett C. and Wright, Duncan J. and Teske, Johanna K. and Howell, Steve B. and Ciardi, David R. and Ziegler, Carl and Stassun, Keivan G. and Johnson, Marshall C. and Eastman, Jason D. and Siverd, Robert J. and Beatty, Thomas G. and Bouma, Luke G. and Pepper, Joshua and Lund, Michael B. and Villanueva, Steven and Stevens, Daniel J. and Jensen, Eric L. N. and Kilby, Coleman and Cohen, David H. and Bayliss, Daniel and Bieryla, Allyson and Cargile, Phillip A. and Collins, Karen A. and Conti, Dennis M. and Colon, Knicole D. and Curtis, Ivan A. and DePoy, Darren L. and Evans, Phil A. and Feliz, Dax and Gregorio, Joao and Rothenberg, Jason and James, David J. and Penny, Matthew T. and Reed, Phillip A. and Relles, Howard M. and Stephens, Denise C. and Joner, Michael D. and Kuhn, Rudolf B. and Stockdale, Chris and Trueblood, Mark and Trueblood, Patricia and Yao, Xinyu and Zambelli, Roberto and Vanderspek, Roland and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Henry, Todd J. and James, Hodari-Sadiki and Jao, Wei-Chun and Wang, Sharon X. and Butler, R. Paul and Crane, Jeffrey D. and Thompson, Ian B. and Schectman, Stephen and Wittenmyer, Robert A. and Bedding, Timothy R. and Okumura, Jack and Plavchan, Peter and Bowler, Brendan P. and Horner, Jonathan and Kane, Stephen R. and Mengel, Matthew W. and Morton, Timothy D. and Tinney, C. G. and Zhang, Hui and Scott, Nicholas J. and Matson, Rachel A. and Everett, Mark E. and Tokovinin, Andrei and Mann, Andrew W. and Dragomir, Diana and Guenther, Maximilian N. and Ting, Eric B. and Fausnaugh, Michael and Glidden, Ana and Quintana, Elisa V. and Manner, Mark and Marshall, Jennifer L. and McLeod, Kim K. and Khakpash, Somayeh},

url = {http://arxiv.org/abs/1912.01017},

year  = {2019},

date = {2019-01-01},

urldate = {2019-12-17},

journal = {arXiv:1912.01017 [astro-ph]},

abstract = {We present the discoveries of KELT-25b (TIC 65412605, TOI-626.01) and KELT-26b (TIC 160708862, TOI-1337.01), two transiting companions orbiting relatively bright, early A-stars. The transit signals were initially detected by the KELT survey, and subsequently confirmed by textbackslashtextitTESS photometry. KELT-25b is on a 4.40-day orbit around the V = 9.66 star CD-24 5016 ($T_textbackslashrm eff = 8280textasciicircum+440_-180$ K, $M_textbackslashstar$ = $2.18textasciicircum+0.12_-0.11$ $M_textbackslashodot$), while KELT-26b is on a 3.34-day orbit around the V = 9.95 star HD 134004 ($T_textbackslashrm eff$ =$8640textasciicircum+500_-240$ K, $M_textbackslashstar$ = $1.93textasciicircum+0.14_-0.16$ $M_textbackslashodot$), which is likely an Am star. We have confirmed the sub-stellar nature of both companions through detailed characterization of each system using ground-based and textbackslashtextitTESS photometry, radial velocity measurements, Doppler Tomography, and high-resolution imaging. For KELT-25, we determine a companion radius of $R_textbackslashrm P$ = $1.64textasciicircum+0.039_-0.043$ $R_textbackslashrm J$, and a 3-sigma upper limit on the companion's mass of $textbackslashsim64textasciitildeM_textbackslashrm J$. For KELT-26b, we infer a planetary mass and radius of $M_textbackslashrm P$ = $1.41textasciicircum+0.43_-0.51$ $M_textbackslashrm J$ and $R_textbackslashrm P$ = $1.940textasciicircum+0.060_-0.058$ $R_textbackslashrm J$. From Doppler Tomographic observations, we find KELT-26b to reside in a highly misaligned orbit. This conclusion is weakly corroborated by a subtle asymmetry in the transit light curve from the textbackslashtextitTESS data. KELT-25b appears to be in a well-aligned, prograde orbit, and the system is likely a member of a cluster or moving group.},

note = {arXiv: 1912.01017},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{shporer_gj_2019,

title = {GJ 1252 b: A 1.2 $R_textbackslashoplus$ planet transiting an M-dwarf at 20.4 pc},

author = {Shporer, Avi and Collins, Karen A. and Astudillo-Defru, Nicola and Irwin, Jonathan and Bonfils, Xavier and Collins, Kevin I. and Matthews, Elisabeth and Winters, Jennifer G. and Anderson, David R. and Armstrong, James D. and Charbonneau, David and Cloutier, Ryan and Daylan, Tansu and Gan, Tianjun and G\"{u}nther, Maximilian N. and Hellier, Coel and Horne, Keith and Huang, Chelsea X. and Jensen, Eric L. N. and Kielkopf, John and Sefako, Ramotholo and Stassun, Keivan G. and Tan, Thiam-Guan and Vanderburg, Andrew and Ricker, George R. and Latham, David W. and Vanderspek, Roland and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Colon, Knicole and Dressing, Courtney D. and L\'{e}pine, S\'{e}bastien and Muirhead, Philip S. and Rose, Mark E. and Twicken, Joseph D. and Villasenor, Jesus Noel},

url = {http://arxiv.org/abs/1912.05556},

year  = {2019},

date = {2019-01-01},

urldate = {2019-12-17},

journal = {arXiv:1912.05556 [astro-ph]},

abstract = {We report the discovery of GJ 1252 b, a planet with a radius of 1.193 $textbackslashpm$ 0.074 $R_textbackslashoplus$ and an orbital period of 0.52 days around an M3-type star (0.381 $textbackslashpm$ 0.019 $M_textbackslashodot$, 0.391 $textbackslashpm$ 0.020 $R_textbackslashodot$) located 20.4 pc away. We use TESS data, ground-based photometry and spectroscopy, Gaia astrometry, and high angular resolution imaging to show that the transit signal seen in the TESS data must originate from a transiting planet. We do so by ruling out all false positive scenarios that attempt to explain the transit signal as originating from an eclipsing stellar binary. Precise Doppler monitoring also leads to a tentative mass measurement of 2.09 $textbackslashpm$ 0.56 $M_textbackslashoplus$. The host star proximity, brightness ($V$ = 12.19 mag, $K$ = 7.92 mag), low stellar activity, and the system's short orbital period make this planet an attractive target for detailed characterization.},

note = {arXiv: 1912.05556},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{davis_toi_2019,

title = {TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESS},

author = {Davis, Allen B. and Wang, Songhu and Jones, Matias and Eastman, Jason D. and G\"{u}nther, Maximilian N. and Stassun, Keivan G. and Addison, Brett C. and Collins, Karen A. and Quinn, Samuel N. and Latham, David W. and Trifonov, Trifon and Shahaf, Sahar and Mazeh, Tsevi and Kane, Stephen R. and Wang, Xian-Yu and Tan, Thiam-Guan and Tokovinin, Andrei and Ziegler, Carl and Tronsgaard, Ren\'{e} and Millholland, Sarah and Cruz, Bryndis and Berlind, Perry and Calkins, Michael L. and Esquerdo, Gilbert A. and Collins, Kevin I. and Conti, Dennis M. and Evans, Phil and Lewin, Pablo and Radford, Don J. and Paredes, Leonardo A. and Henry, Todd J. and James, Hodari-Sadiki and Law, Nicholas M. and Mann, Andrew W. and Brice\~{n}o, C\'{e}sar and Ricker, George R. and Vanderspek, Roland and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Krishnamurthy, Akshata and Batalha, Natalie M. and Burt, Jennifer and Col\'{o}n, Knicole D. and Dynes, Scott and Caldwell, Douglas A. and Morris, Robert and Henze, Christopher E. and Fischer, Debra A.},

url = {http://arxiv.org/abs/1912.10186},

year  = {2019},

date = {2019-01-01},

urldate = {2019-12-24},

journal = {arXiv:1912.10186 [astro-ph]},

abstract = {We report the discovery and confirmation of two new hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS): TOI 564 b and TOI 905 b. The transits of these two planets were initially observed by TESS with orbital periods of 1.651 d and 3.739 d, respectively. We conducted follow-up observations of each system from the ground, including photometry in multiple filters, speckle interferometry, and radial velocity measurements. For TOI 564 b, our global fitting revealed a classical hot Jupiter with a mass of $1.463textasciicircum+0.10_-0.096textbackslash M_J$ and a radius of $1.02textasciicircum+0.71_-0.29textbackslash R_J$. TOI 905 b is a classical hot Jupiter as well, with a mass of $0.667textasciicircum+0.042_-0.041textbackslash M_J$ and radius of $1.171textasciicircum+0.053_-0.051textbackslash R_J$. Both planets orbit Sun-like, moderately bright, mid-G dwarf stars with V textasciitilde 11. While TOI 905 b fully transits its star, we found that TOI 564 b has a very high transit impact parameter of $0.994textasciicircum+0.083_-0.049$, making it one of only textasciitilde20 known systems to exhibit a grazing transit and one of the brightest host stars among them. TOI 564 b is therefore one of the most attractive systems to search for additional non-transiting, smaller planets by exploiting the sensitivity of grazing transits to small changes in inclination and transit duration over the time scale of several years.},

note = {arXiv: 1912.10186},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{zhou_occultations_2018,

title = {Occultations from an active accretion disk in a 72 day detached post-Algol system detected by K2},

author = {Zhou, G. and Rappaport, S. and Nelson, L. and Huang, C. X. and Senhadji, A. and Rodriguez, J. E. and Vanderburg, A. and Quinn, S. and Johnson, C. I. and Latham, D. W. and Torres, G. and Gary, B. L. and Tan, T. G. and Johnson, M. C. and Burt, J. and Kristiansen, M. H. and Jacobs, T. L. and LaCourse, D. and Schwengeler, H. M. and Terentev, I. and Bieryla, A. and Esquerdo, G. A. and Berlind, P. and Calkins, M. L. and Bento, J. and Cochran, W. D. and Karjalainen, M. and Hatzes, A. P. and Karjalainen, R. and Holden, B. and Butler, R. P.},

url = {http://arxiv.org/abs/1801.06188},

year  = {2018},

date = {2018-01-01},

urldate = {2018-02-12},

journal = {arXiv:1801.06188 [astro-ph]},

abstract = {Disks in binary systems can cause exotic eclipsing events. MWC 882 (BD-22 4376, EPIC 225300403) is such a disk-eclipsing system identified from observations during Campaign 11 of the K2 mission. We propose that MWC 882 is a post-Algol system with a B7 donor star of mass $0.542textbackslashpm0.053textbackslash,M_textbackslashodot$ in a 72 day period orbit around an A0 accreting star of mass $3.24textbackslashpm0.29textbackslash,M_textbackslashodot$. The $59.9textbackslashpm6.2textbackslash,R_textbackslashodot$ disk around the accreting star occults the donor star once every orbit, inducing 19 day long, 7% deep eclipses identified by K2, and subsequently found in pre-discovery ASAS and ASAS-SN observations. We coordinated a campaign of photometric and spectroscopic observations for MWC 882 to measure the dynamical masses of the components and to monitor the system during eclipse. We found the photometric eclipse to be gray to $textbackslashapprox 1$%. We found the primary star exhibits spectroscopic signatures of active accretion, and observed gas absorption features from the disk during eclipse. We suggest MWC 882 initially consisted of a $textbackslashapprox 3.6textbackslash,M_textbackslashodot$ donor star transferring mass via Roche lobe overflow to a $textbackslashapprox 2.1textbackslash,M_textbackslashodot$ accretor in a $textbackslashapprox 7$ day initial orbit. Through angular momentum conservation, the donor star is pushed outward during mass transfer to its current orbit of 72 days. The observed state of the system corresponds with the donor star having left the Red Giant Branch textasciitilde0.3 Myr ago, terminating active mass transfer. The present disk is expected to be short-lived ($10textasciicircum2$ years) without an active feeding mechanism, presenting a challenge to this model.},

note = {arXiv: 1801.06188},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{labadie-bartz_kelt-22ab:_2018,

title = {KELT-22Ab: A Massive Hot Jupiter Transiting a Near Solar Twin},

author = {Labadie-Bartz, Jonathan and Rodriguez, Joseph E. and Stassun, Keivan G. and Ciardi, David R. and Johnson, Marshall C. and Gaudi, B. Scott and Penev, Kaloyan M. and Bieryla, Allyson and Latham, David W. and Pepper, Joshua and Collins, Karen A. and Evans, Phil and Relles, Howard M. and Siverd, Robert J. and Bento, Joao and Yao, Xinyu and Stockdale, Chris and Tan, Thiam-Guan and Zhou, George and Colon, Knicole D. and Eastman, Jason D. and Albrow, Michael D. and Malpas, Amber and Bayliss, Daniel and Beatty, Thomas G. and Bozza, Valerio and Cohen, David H. and Curtis, Ivan A. and DePoy, Darren L. and Feliz, Dax and Fulton, Benjamin J. and Gregorio, Joao and James, David and Jang-Condell, Hannah and Jensen, Eric L. and Johnson, John A. and Johnson, Samson A. and Joner, Michael D. and Kielkopf, John and Kuhn, Rudolf B. and Lund, Michael B. and Manner, Mark and Marshall, Jennifer L. and McCrady, Nate and McLeod, Kim K. and Oberst, Thomas E. and Penny, Matthew T. and Pogge, Rick and Reed, Phillip A. and Sliski, David H. and Stephens, Denise C. and Stevens, Daniel J. and Trueblood, Mark and Trueblood, Patricia and Villanueva Jr., Steven and Wittenmyer, Robert A. and Wright, Jason T. and Zambelli, Roberto and Berlind, Perry and Calkins, Michael L. and Esquerdo, Gilbert A.},

url = {http://arxiv.org/abs/1803.07559},

year  = {2018},

date = {2018-01-01},

urldate = {2018-04-11},

journal = {arXiv:1803.07559 [astro-ph]},

abstract = {We present the discovery of KELT-22Ab, a hot Jupiter from the KELT-South survey. KELT-22Ab transits the moderately bright ($Vtextbackslashsim 11.1$) Sun-like G2V star TYC 7518-468-1. The planet has an orbital period of $P = 1.3866529 textbackslashpm 0.0000027 $ days, a radius of $R_P = 1.285_-0.071textasciicircum+0.12textasciitildeR_J$, and a relatively large mass of $M_P = 3.47_-0.14textasciicircum+0.15textasciitilde M_J$. The star has $R_textbackslashstar = 1.099_-0.046textasciicircum+0.079textasciitilde R_textbackslashodot$, $M_textbackslashstar = 1.092_-0.041textasciicircum+0.045textasciitilde M_textbackslashodot$, $T_textbackslashrm efftextbackslash, = 5767_-49textasciicircum+50textasciitilde$ K, $textbackslashlogg_textbackslashstar = 4.393_-0.060textasciicircum+0.039textasciitilde$ (cgs), and [m/H] = $+0.259_-0.083textasciicircum+0.085textasciitilde$, and thus, other than its slightly super-solar metallicity, appears to be a near solar twin. Surprisingly, KELT-22A exhibits kinematics and a Galactic orbit that are somewhat atypical for thin disk stars. Nevertheless, the star is rotating quite rapidly for its estimated age, shows evidence of chromospheric activity, and is somewhat metal rich. Imaging reveals a slightly fainter companion to KELT-22A that is likely bound, with a projected separation of 6textbackslasharcsec ($textbackslashsim$1400 AU). In addition to the orbital motion caused by the transiting planet, we detect a possible linear trend in the radial velocity of KELT-22A suggesting the presence of another relatively nearby body that is perhaps non-stellar. KELT-22Ab is highly irradiated (as a consequence of the small semi-major axis of $a/R_textbackslashstar = 4.97$), and is mildly inflated. At such small separations, tidal forces become significant. The configuration of this system is optimal for measuring the rate of tidal dissipation within the host star. Our models predict that, due to tidal forces, the semi-major axis of KELT-22Ab is decreasing rapidly, and is thus predicted to spiral into the star within the next Gyr.},

note = {arXiv: 1803.07559},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{bento_hats-39b_2018,

title = {HATS-39b, HATS-40b, HATS-41b, and HATS-42b: Three Inflated Hot Jupiters and a Super-Jupiter Transiting F Stars},

author = {Bento, J. and Hartman, J. D. and Bakos, G. A. and Bhatti, W. and Csubry, Z. and Penev, K. and Bayliss, D. and de Val-Borro, M. and Zhou, G. and Brahm, R. and Espinoza, N. and Rabus, M. and Jordan, A. and Suc, V. and Ciceri, S. and Sarkis, P. and Henning, T. and Mancini, L. and Tinney, C. G. and Wright, D. J. and Durkan, S. and Tan, T. G. and Lazar, J. and Papp, I. and Sari, P.},

url = {http://arxiv.org/abs/1804.01623},

doi = {10.1093/mnras/sty726},

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

year  = {2018},

date = {2018-01-01},

urldate = {2018-04-11},

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

abstract = {We report the discovery of four transiting hot Jupiters from the HATSouth survey: HATS-39b, HATS-40b, HATS41b and HATS-42b. These discoveries add to the growing number of transiting planets orbiting moderately bright (12.5 textless V textless 13.7) F dwarf stars on short (2-5 day) periods. The planets have similar radii, ranging from 1.33(+0.29/-0.20) R_J for HATS-41b to 1.58(+0.16/-0.12) R_J for HATS-40b. Their masses and bulk densities, however, span more than an order of magnitude. HATS-39b has a mass of 0.63 +/- 0.13 M_J, and an inflated radius of 1.57 +/- 0.12 R_J, making it a good target for future transmission spectroscopic studies. HATS-41b is a very massive 9.7 +/- 1.6 M_J planet and one of only a few hot Jupiters found to date with a mass over 5 M_J. This planet orbits the highest metallicity star ([Fe/H] = 0.470 +/- 0.010) known to host a transiting planet and is also likely on an eccentric orbit. The high mass, coupled with a relatively young age (1.34 +0.31/-0.51 Gyr) for the host star, are factors that may explain why this planet's orbit has not yet circularised.},

note = {arXiv: 1804.01623},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{collins_kelt_2018,

title = {The KELT Follow-Up Network and Transit False Positive Catalog: Pre-vetted False Positives for TESS},

author = {Collins, Karen A. and Collins, Kevin I. and Pepper, Joshua and Labadie-Bartz, Jonathan and Stassun, Keivan and Gaudi, B. Scott and Bayliss, Daniel and Bento, Joao and Col\'{o}n, Knicole D. and Feliz, Dax and James, David and Johnson, Marshall C. and Kuhn, Rudolf B. and Lund, Michael B. and Penny, Matthew T. and Rodriguez, Joseph E. and Siverd, Robert J. and Stevens, Daniel J. and Yao, Xinyu and Zhou, George and Akshay, Mundra and Aldi, Giulio F. and Ashcraft, Cliff and Awiphan, Supachai and Ba\c{s}t\"{u}rk, \"{O}zg\"{u}r and Baker, David and Beatty, Thomas G. and Benni, Paul and Berlind, Perry and Berriman, G. Bruce and Berta-Thompson, Zach and Bieryla, Allyson and Bozza, Valerio and Novati, Sebastiano Calchi and Calkins, Michael L. and Cann, Jenna M. and Ciardi, David R. and Clark, Ian R. and Cochran, William D. and Cohen, David H. and Conti, Dennis and Crepp, Justin R. and Curtis, Ivan A. and D'Ago, Giuseppe and Diazeguigure, Kenny A. and Dressing, Courtney D. and Dubois, Franky and Ellingson, Erica and Ellis, Tyler G. and Esquerdo, Gilbert A. and Evans, Phil and Friedli, Alison and Fukui, Akihiko and Fulton, Benjamin J. and Gonzales, Erica J. and Good, John C. and Gregorio, Joao and Gumusayak, Tolga and Hancock, Daniel A. and Harada, Caleb K. and Hart, Rhodes and Hintz, Eric G. and Jang-Condell, Hannah and Jeffery, Elizabeth J. and Jensen, Eric L. N. and Jofr\'{e}, Emiliano and Joner, Michael D. and Kar, Aman and Kasper, David H. and Keten, Burak and Kielkopf, John F. and Komonjinda, Siramas and Kotnik, Cliff and Latham, David W. and Leuquire, Jacob and Lewis, Tiffany R. and Logie, Ludwig and Lowther, Simon J. and MacQueen, Phillip J. and Martin, Trevor J. and Mawet, Dimitri and McLeod, Kim K. and Murawski, Gabriel and Narita, Norio and Nordhausen, Jim and Oberst, Thomas E. and Odden, Caroline and Panka, Peter A. and Petrucci, Romina and Plavchan, Peter and Quinn, Samuel N. and Rau, Steve and Reed, Phillip A. and Relles, Howard and Renaud, Joe P. and Scarpetta, Gaetano and Sorber, Rebecca L. and Spencer, Alex D. and Spencer, Michelle and Stephens, Denise C. and Stockdale, Chris and Tan, Thiam-Guan and Trueblood, Mark and Trueblood, Patricia and Vanaverbeke, Siegfried and Villanueva Jr., Steven and Warner, Elizabeth M. and West, Mary Lou and Yal\c{c}ınkaya, Sel\c{c}uk and Yeigh, Rex and Zambelli, Roberto},

url = {http://arxiv.org/abs/1803.01869},

year  = {2018},

date = {2018-01-01},

urldate = {2018-04-11},

journal = {arXiv:1803.01869 [astro-ph]},

abstract = {The Kilodegree Extremely Little Telescope (KELT) project has been conducting a photometric survey for transiting planets orbiting bright stars for over ten years. The KELT images have a pixel scale of textasciitilde23 arsec per pixel (similar to TESS) and a large point spread function, and the KELT reduction pipeline uses a weighted photometric aperture with radius 3 arcmin. At this angular scale, multiple stars are typically blended in the photometric apertures. In order to identify false positives and confirm transiting exoplanets, we have assembled a follow-up network (KELT-FUN) to conduct imaging with higher spatial resolution, cadence, and photometric precision than the KELT telescopes, as well as spectroscopic observations of the candidate host stars. The KELT-FUN team has followed-up over 1,600 planet candidates since 2011, resulting in more than 20 planet discoveries. We present an all-sky catalog of 1,081 bright stars (6textlessVtextless13) that show transit-like features in the KELT light curves. These stars were originally identified as planet candidates, but were subsequently determined to be astrophysical false positives (FPs) after photometric and/or spectroscopic follow-up observations. The remaining textasciitilde500 retired planet candidates have been classified as false alarms (instrumental or systematic noise). The KELT-FUN team continues to pursue KELT and other planet candidates and will eventually follow up certain classes of TESS candidates. The KELT FP catalog will help minimize the duplication of follow-up observations by current and future transit surveys such as TESS.},

note = {arXiv: 1803.01869},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{borkovits_epic_2018,

title = {EPIC 219217635: A Doubly Eclipsing Quadruple System Containing an Evolved Binary},

author = {Borkovits, T. and Albrecht, S. and Rappaport, S. and Nelson, L. and Vanderburg, A. and Gary, B. L. and Tan, T. G. and Justesen, A. B. and Kristiansen, M. H. and Jacobs, T. L. and LaCourse, D. and Ngo, H. and Wallack, N. and Ruane, G. and Mawet, D. and Howell, S. B. and Tronsgaard, R.},

url = {http://arxiv.org/abs/1805.09693},

doi = {10.1093/mnras/sty1386},

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

year  = {2018},

date = {2018-01-01},

urldate = {2018-06-18},

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

abstract = {We have discovered a doubly eclipsing, bound, quadruple star system in the field of K2 Campaign 7. EPIC 219217635 is a stellar image with $Kp = 12.7$ that contains an eclipsing binary (`EB') with $P_A = 3.59470$ d and a second EB with $P_B = 0.61825$ d. We have obtained followup radial-velocity (`RV') spectroscopy observations, adaptive optics imaging, as well as ground-based photometric observations. From our analysis of all the observations, we derive good estimates for a number of the system parameters. We conclude that (1) both binaries are bound in a quadruple star system; (2) a linear trend to the RV curve of binary A is found over a 2-year interval, corresponding to an acceleration, $textbackslashdot textbackslashgamma = 0.0024 textbackslashpm 0.0007$ cm s$textasciicircum-2$; (3) small irregular variations are seen in the eclipse-timing variations (`ETVs') detected over the same interval; (4) the orbital separation of the quadruple system is probably in the range of 8-25 AU; and (5) the orbital planes of the two binaries must be inclined with respect to each other by at least 25$textasciicircumtextbackslashcirc$. In addition, we find that binary B is evolved, and the cooler and currently less massive star has transferred much of its envelope to the currently more massive star. We have also demonstrated that the system is sufficiently bright that the eclipses can be followed using small ground-based telescopes, and that this system may be profitably studied over the next decade when the outer orbit of the quadruple is expected to manifest itself in the ETV and/or RV curves.},

note = {arXiv: 1805.09693},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{shvartzvald_$spitzer$_2018,

title = {$Spitzer$ Microlensing Parallax for OGLE-2017-BLG-0896 Reveals a Counter-Rotating Low-Mass Brown Dwarf},

author = {Shvartzvald, Yossi and Yee, Jennifer C. and Skowron, Jan and Lee, Chung-Uk and Udalski, Andrzej and Novati, Sebastiano Calchi and Bozza, Valerio and Beichman, Charles A. and Bryden, Geoffery and Carey, Sean and Gaudi, B. Scott and Henderson, Calen B. and Zhu, Wei and Bachelet, Etienne and Bolt, Greg and Christie, Grant and Maoz, Dan and Natusch, Tim and Pogge, Richard W. and Street, Rachel A. and Tan, Thiam-Guan and Tsapras, Yiannis and Pietrukowicz, Pawe\l and Soszy\'{n}ski, Igor and Szyma\'{n}ski, Micha\l K. and Mr\'{o}z, Przemek and Poleski, Radoslaw and Koz\lowski, Szymon and Ulaczyk, Krzysztof and Pawlak, Micha\l and Rybicki, Krzysztof A. and Iwanek, Patryk and Albrow, Michael D. and Cha, Sang-Mok and Chung, Sun-Ju and Gould, Andrew and Han, Cheongho and Hwang, Kyu-Ha and Jung, Youn Kil and Kim, Dong-Jin and Kim, Hyoun-Woo and Kim, Seung-Lee and Lee, Dong-Joo and Lee, Yongseok and Park, Byeong-Gon and Ryu, Yoon-Hyun and Shin, In-Gu and Zang, Weicheng and Dominik, Martin and Helling, Christiane and Hundertmark, Markus and J\orgensen, Uffe G. and Longa-Pe\~{n}a, Penelope and Lowry, Stephen and Sajadian, Sedighe and Burgdorf, Martin J. and Campbell-White, Justyn and Ciceri, Simona and Evans, Daniel F. and Fujii, Yuri I. and Hinse, Tobias C. and Rahvar, Sohrab and Rabus, Markus and Skottfelt, Jesper and Snodgrass, Colin and Southworth, John},

url = {http://arxiv.org/abs/1805.08778},

year  = {2018},

date = {2018-01-01},

urldate = {2018-06-18},

journal = {arXiv:1805.08778 [astro-ph]},

abstract = {The kinematics of isolated brown dwarfs in the Galaxy, beyond the solar neighborhood, is virtually unknown. Microlensing has the potential to probe this hidden population, as it can measure both the mass and five of the six phase-space coordinates (all except the radial velocity) even of a dark isolated lens. However, the measurements of both the microlens parallax and finite-source effects are needed in order to recover the full information. Here, we combine $Spitzer$ satellite parallax measurement with the ground-based light curve, which exhibits strong finite-source effects, of event OGLE-2017-BLG-0896. We find that the lens is a $textbackslashsim$19$M_J$ isolated brown dwarf. This is the lowest isolated-object mass measurement to date, only slightly above the common definition of a free-floating planet. The brown dwarf is located at $textbackslashsim$4 kpc toward the Galactic bulge, but with proper motion in the opposite direction of disk stars, possibly moving in the Galactic plane. While it is possibly a halo brown dwarf, it might also represent a different, unknown population.},

note = {arXiv: 1805.08778},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{sarkis_hats-59bc:_2018,

title = {HATS-59b,c: A Transiting Hot Jupiter and a Cold Massive Giant Planet Around a Sun-Like Star},

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

url = {http://arxiv.org/abs/1805.05925},

year  = {2018},

date = {2018-01-01},

urldate = {2018-06-18},

journal = {arXiv:1805.05925 [astro-ph]},

abstract = {We report the first discovery of a multi-planetary system by the HATSouth network, HATS-59b,c, a planetary system with an inner transiting hot Jupiter and an outer cold massive giant planet, which was detected via radial velocity. The inner transiting planet, HATS-59b, is on an eccentric orbit with $e = 0.129textbackslashpm0.049$, orbiting a $V=13.951textbackslashpm0.030$ mag solar-like star ($M_* = 1.038textbackslashpm0.039 M_textbackslashodot$, and $R_* = 1.036textbackslashpm0.067 R_textbackslashodot$) with a period of $5.416077textbackslashpm0.000017$ days. The outer companion, HATS-59c is on a circular orbit with $ m textbackslashsin i = 12.8textbackslashpm1.1 M_textbackslashmathrmJ$, and a period of $1422textbackslashpm14$ days. The inner planet has a mass of $0.806textbackslashpm0.069 M_textbackslashmathrmJ$ and a radius of $1.126textbackslashpm0.077 M_textbackslashmathrmJ$, yielding a density of $0.70textbackslashpm0.16 textbackslashrm gtextbackslash,cmtextasciicircum-3$. Unlike most of the planetary systems that include only a single hot Jupiter, HATS-59b,c includes, in addition to the transiting hot Jupiter, a massive outer companion. The architecture of this system is valuable for understanding planet migration.},

note = {arXiv: 1805.05925},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{bennett_planetary_2018,

title = {A Planetary Microlensing Event with an Unusually Red Source Star: MOA-2011-BLG-291},

author = {Bennett, David P. and Udalski, Andrzej and Bond, Ian A. and Suzuki, Daisuke and Ryu, Yoon-Hyun and Abe, Fumio and Barry, Richard K. and Bhattacharya, Aparna and Donachie, Martin and Fukui, Akihiko and Hirao, Yuki and Kawasaki, Kohei and Kondo, Iona and Koshimoto, Naoki and Li, Man Cheung Alex and Matsubara, Yutaka and Miyazaki, Shota and Muraki, Yasushi and Nagakane, Masayuki and Ohnishi, Koji and Ranc, Cl\'{e}ment and Rattenbury, Nicholas J. and Suematsu, Haruno and Sumi, Takahiro and Tristram, Paul J. and Yonehara, Atsunori and Szyma\'{n}ski, Micha\l K. and Soszy\'{n}ski, Igor and Wyrzykowski, \Lukasz and Ulaczyk, Krzysztof and Poleski, Radek and Koz\lowski, Szymon and Pietrukowicz, Pawe\l and Skowron, Jan and Shvartzvald, Yossi and Maoz, Dan and Kaspi, Shai and Friedmann, Matan and Batista, Virginie and DePoy, Darren and Dong, Subo and Gaudi, B. Scott and Gould, Andrew and Pogge, Cheongho Han Richard W. and Tan, Thiam-Guan and Yee, Jennifer C.},

url = {http://arxiv.org/abs/1806.06106},

year  = {2018},

date = {2018-01-01},

urldate = {2018-07-13},

journal = {arXiv:1806.06106 [astro-ph]},

abstract = {We present the analysis of planetary microlensing event MOA-2011-BLG-291, which has a mass ratio of $q=(3.8textbackslashpm0.7)textbackslashtimes10textasciicircum-4$ and a source star that is redder (or brighter) than the bulge main sequence. This event is located at a low Galactic latitude in the survey area that is currently planned for NASA's WFIRST exoplanet microlensing survey. This unusual color for a microlensed source star implies that we cannot assume that the source star is in the Galactic bulge. The favored interpretation is that the source star is a lower main sequence star at a distance of $D_S=4.9textbackslashpm1.3textbackslash,$kpc in the Galactic disk. However, the source could also be a turn-off star on the far side of the bulge or a sub-giant in the far side of the Galactic disk if it experiences significantly more reddening than the bulge red clump stars. However, these possibilities have only a small effect on our mass estimates for the host star and planet. We find host star and planet masses of $M_textbackslashrm host =0.15textasciicircum+0.27_-0.10M_textbackslashodot$ and $m_p=18textasciicircum+34_-12M_textbackslashoplus$ from a Bayesian analysis with a standard Galactic model under the assumption that the planet hosting probability does not depend on the host mass or distance. However, if we attempt to measure the host and planet masses with host star brightness measurements from high angular resolution follow-up imaging, the implied masses will be sensitive to the host star distance. The WFIRST exoplanet microlensing survey is expected to use this method to determine the masses for many of the planetary systems that it discovers, so this issue has important design implications for the WFIRST exoplanet microlensing survey.},

note = {arXiv: 1806.06106},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{hartman_hats-60b_2018,

title = {HATS-60b - HATS-69b: Ten Transiting Planets From HATSouth},

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

url = {http://arxiv.org/abs/1809.01048},

year  = {2018},

date = {2018-01-01},

urldate = {2018-09-05},

journal = {arXiv:1809.01048 [astro-ph]},

abstract = {We report the discovery of ten transiting extrasolar planets by the HATSouth survey. The planets range in mass from the Super-Neptune HATS-62b, with $M_p textless 0.191 M_J$, to the Super-Jupiter HATS-66b, with $M_p = 5.47 M_J$, and in size from the Saturn HATS-69b, with $R_p = 0.94 R_J$, to the inflated Jupiter HATS-67b, with $R_p = 1.69 R_J$. The planets have orbital periods between 1.6092 days (HATS-67b) and 7.8180 days (HATS-61b). The hosts are dwarf stars with masses ranging from $0.89 M_textbackslashodot$ (HATS-69) to $1.56 M_textbackslashodot$ (HATS-64), and have apparent magnitudes between $V = 12.276 textbackslashpm 0.020$ mag (HATS-68) and $V = 14.095 textbackslashpm 0.030$ mag (HATS-66). The Super-Neptune HATS-62b is the least massive planet discovered to date with a radius larger than Jupiter. Based largely on the Gaia DR2 distances and broad-band photometry, we identify three systems (HATS-62, -64, and -65) as having possible unresolved binary star companions. We discuss in detail our methods for incorporating the Gaia DR2 observations into our modeling of the system parameters, and into our blend analysis procedures.},

note = {arXiv: 1809.01048},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{ment_second_2018,

title = {A second planet with an Earth-like composition orbiting the nearby M dwarf LHS 1140},

author = {Ment, Kristo and Dittmann, Jason A. and Astudillo-Defru, Nicola and Charbonneau, David and Irwin, Jonathan and Bonfils, Xavier and Murgas, Felipe and Almenara, Jose-Manuel and Forveille, Thierry and Agol, Eric and Ballard, Sarah and Berta-Thompson, Zachory K. and Bouchy, Fran\c{c}ois and Cloutier, Ryan and Delfosse, Xavier and Doyon, Ren\'{e} and Dressing, Courtney D. and Esquerdo, Gilbert A. and Haywood, Rapha\"{e}lle D. and Kipping, David M. and Latham, David W. and Lovis, Christophe and Newton, Elisabeth R. and Pepe, Francesco and Rodriguez, Joseph E. and Santos, Nuno C. and Tan, Thiam-Guan and Udry, Stephane and Winters, Jennifer G. and W\"{u}nsche, Ana\"{e}l},

url = {http://arxiv.org/abs/1808.00485},

year  = {2018},

date = {2018-01-01},

urldate = {2018-09-05},

journal = {arXiv:1808.00485 [astro-ph]},

abstract = {LHS 1140 is a nearby mid-M dwarf known to host a temperate rocky super-Earth (LHS 1140 b) on a 24.737-day orbit. Based on photometric observations by MEarth and Spitzer as well as Doppler spectroscopy from HARPS, we report the discovery of an additional transiting rocky companion (LHS 1140 c) with a mass of $1.81textbackslashpm0.39textasciitildetextbackslashrm M_Earth$ and a radius of $1.282textbackslashpm0.024textasciitildetextbackslashrm R_Earth$ on a tighter, 3.77795-day orbit. We also obtain more precise estimates of the mass and radius of LHS 1140 b to be $6.98textbackslashpm0.98textasciitildetextbackslashrm M_Earth$ and $1.727textbackslashpm0.032textasciitildetextbackslashrm R_Earth$. The mean densities of planets b and c are $7.5textbackslashpm1.0textasciitildetextbackslashrmg/cmtextasciicircum3$ and $4.7textbackslashpm1.1textasciitildetextbackslashrmg/cmtextasciicircum3$, respectively, both consistent with the Earth's ratio of iron to magnesium silicate. The orbital eccentricities of LHS 1140 b and c are consistent with circular orbits and constrained to be below 0.06 and 0.31, respectively, with 90% confidence. Because the orbits of the two planets are co-planar and because we know from previous analyses of Kepler data that compact systems of small planets orbiting M dwarfs are commonplace, a search for more transiting planets in the LHS 1140 system could be fruitful. LHS 1140 c is one of the few known nearby terrestrial planets whose atmosphere could be studied with the upcoming James Webb Space Telescope.},

note = {arXiv: 1808.00485},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{borkovits_photodynamical_2018,

title = {Photodynamical analysis of the triply eclipsing hierarchical triple system EPIC 249432662},

author = {Borkovits, T. and Rappaport, S. and Kaye, T. and Isaacson, H. and Vanderburg, A. and Howard, A. W. and Kristiansen, M. H. and Omohundro, M. R. and Schwengeler, H. M. and Terentev, I. A. and Shporer, A. and Relles, H. and Villanueva Jr., S. and Tan, T. G. and Col\'{o}n, K. D. and Blex, J. and Haas, M. and Cochran, W. and Endl, M.},

url = {http://arxiv.org/abs/1809.04366},

year  = {2018},

date = {2018-01-01},

urldate = {2018-09-13},

journal = {arXiv:1809.04366 [astro-ph]},

abstract = {Using Campaign 15 data from the K2 mission, we have discovered a triply-eclipsing triple star system: EPIC 249432662. The inner eclipsing binary system has a period of 8.23 days, with shallow $textbackslashsim$3% eclipses. During the entire 80-day campaign, there is also a single eclipse event of a third-body in the system that reaches a depth of nearly 50% and has a total duration of 1.7 days, longer than for any previously known third-body eclipse involving unevolved stars. The binary eclipses exhibit clear eclipse timing variations. A combination of photodynamical modeling of the lightcurve, as well as seven follow-up radial velocity measurements, has led to a prediction of the subsequent eclipses of the third star with a period of 188 days. A campaign of follow-up ground-based photometry was able to capture the subsequent pair of third-body events as well as two further 8-day eclipses. A combined photo-spectro-dynamical analysis then leads to the determination of many of the system parameters. The 8-day binary consists of a pair of M stars, while most of the system light is from a K star around which the pair of M stars orbits.},

note = {arXiv: 1809.04366},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{mentel_constraining_2018,

title = {Constraining the period of the ringed secondary companion to the young star J1407 with photographic plates},

author = {Mentel, R. T. and Kenworthy, M. A. and Cameron, D. A. and Scott, E. L. and Mellon, S. N. and Hudec, R. and Birkby, J. L. and Mamajek, E. E. and Schrimpf, A. and Reichart, D. E. and Haislip, J. B. and Kouprianov, V. V. and Hambsch, F.-J. and Tan, T.-G. and Hills, K. and Grindlay, J. E.},

url = {http://arxiv.org/abs/1810.05171},

doi = {10.1051/0004-6361/201834004},

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

year  = {2018},

date = {2018-01-01},

urldate = {2018-12-04},

journal = {Astronomy \& Astrophysics},

volume = {619},

pages = {A157},

abstract = {Context. The 16 Myr old star 1SWASP J140747.93-394542.6 (V1400 Cen) underwent a series of complex eclipses in May 2007, interpreted as the transit of a giant Hill sphere filling debris ring system around a secondary companion, J1407b. No other eclipses have since been detected, although other measurements have constrained but not uniquely determined the orbital period of J1407b. Finding another eclipse towards J1407 will help determine the orbital period of the system, the geometry of the proposed ring system and enable planning of further observations to characterize the material within these putative rings. Aims. We carry out a search for other eclipses in photometric data of J1407 with the aim of constraining the orbital period of J1407b. Methods. We present photometry from archival photographic plates from the Harvard DASCH survey, and Bamberg and Sonneberg Observatories, in order to place additional constraints on the orbital period of J1407b by searching for other dimming and eclipse events. Using a visual inspection of all 387 plates and a period-folding algorithm we performed a search for other eclipses in these data sets. Results. We find no other deep eclipses in the data spanning from 1890 to 1990, nor in recent time-series photometry from 2012-2018. Conclusions. We rule out a large fraction of putative orbital periods for J1407b from 5 to 20 years. These limits are still marginally consistent with a large Hill sphere filling ring system surrounding a brown dwarf companion in a bound elliptical orbit about J1407. Issues with the stability of any rings combined with the lack of detection of another eclipse, suggests that J1407b may not be bound to J1407.},

note = {arXiv: 1810.05171},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{espinoza_hats-54b-hats-58ab:_2018,

title = {HATS-54b-HATS-58Ab: five new transiting hot Jupiters including one with a possible temperate companion},

author = {Espinoza, N\'{e}stor and Hartman, Joel D. and Bakos, Gaspar \'{A} and Henning, Thomas and Bayliss, Daniel and Bento, Joao and Bhatti, Waqas and Brahm, Rafael and Csubry, Zoltan and Suc, Vincent and Jord\'{a}n, Andr\'{e}s and Mancini, Luigi and Tan, T. G. and Penev, Kaloyan and Rabus, Markus and Sarkis, Paula and de Val-Borro, Miguel and Durkan, Stephen and Lazar, Josef and Papp, Istvan and Sari, Pal},

url = {http://arxiv.org/abs/1812.07668},

year  = {2018},

date = {2018-01-01},

urldate = {2018-12-22},

journal = {arXiv:1812.07668 [astro-ph]},

abstract = {We report the discovery by the HATSouth project of 5 new transiting hot Jupiters (HATS-54b through HATS-58Ab). HATS-54b, HATS-55b and HATS-58Ab are prototypical short period ($P = 2.5-4.2$ days, $R_ptextbackslashsim1.1-1.2$ $R_J$) hot-Jupiters that span effective temperatures from 1350 K to 1750 K, putting them in the proposed region of maximum radius inflation efficiency. The HATS-58 system is composed of two stars, HATS-58A and HATS-58B, which are detected thanks to Gaia DR2 data and which we account for in the joint modelling of the available data --- with this, we are led to conclude that the hot jupiter orbits the brighter HATS-58A star. HATS-57b is a short-period (2.35-day) massive (3.15 $M_J$) 1.14 $R_J$, dense ($2.65textbackslashpm0.21$ g cm$textasciicircum-3$) hot-Jupiter, orbiting a very active star ($2textbackslash%$ peak-to-peak flux variability). Finally, HATS-56b is a short period (4.32-day) highly inflated hot-Jupiter (1.7 $R_J$, 0.6 $M_J$), which is an excellent target for future atmospheric follow-up, especially considering the relatively bright nature ($V=11.6$) of its F dwarf host star. This latter exoplanet has another very interesting feature: the radial velocities show a significant quadratic trend. If we interpret this quadratic trend as arising from the pull of an additional planet in the system, we obtain a period of $P_c = 815textasciicircum+253_-143$ days for the possible planet HATS-56c, and a minimum mass of $M_ctextbackslashsin i_c = 5.11 textbackslashpm 0.94$ $M_J$. The candidate planet HATS-56c would have a zero-albedo equilibrium temperature of $T_textbackslashtextrmeq=332textbackslashpm 50$ K, and thus would be orbiting close to the habitable zone of HATS-56. Further radial-velocity follow-up, especially over the next two years, is needed to confirm the nature of HATS-56c.},

note = {arXiv: 1812.07668},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{mcleod_kelt-18b:_2017,

title = {KELT-18b: Puffy Planet, Hot Host, Probably Perturbed},

author = {McLeod, Kim K. and Rodriguez, Joseph E. and Oelkers, Ryan J. and Collins, Karen A. and Bieryla, Allyson and Fulton, Benjamin J. and Stassun, Keivan G. and Gaudi, B. Scott and Penev, Kaloyan and Stevens, Daniel J. and Col\'{o}n, Knicole D. and Pepper, Joshua and Narita, Norio and Tsuguru, Ryu and Fukui, Akihiko and Reed, Phillip A. and Tirrell, Bethany and Visgaitis, Tiffany and Kielkopf, John F. and Cohen, David H. and Jensen, Eric L. N. and Gregorio, Joao and Ba\c{s}t\"{u}rk, \"{O}zg\"{u}r and Oberst, Thomas E. and Melton, Casey and Kempton, Eliza M.-R. and Baldridge, Andrew and Zhao, Y. Sunny and Zambelli, Roberto and Latham, David W. and Esquerdo, Gilbert A. and Berlind, Perry and Calkins, Michael L. and Howard, Andrew W. and Isaacson, Howard and Weiss, Lauren M. and Beatty, Thomas G. and Eastman, Jason D. and Penny, Matthew T. and Siverd, Robert J. and Lund, Michael B. and Labadie-Bartz, Jonathan and Zhao, G. and Curtis, Ivan A. and Joner, Michael D. and Manner, Mark and Relles, Howard and Scarpetta, Gaetano and Stephens, Denise C. and Stockdale, Chris and Tan, T. G. and DePoy, D. L. and Marshall, Jennifer L. and Pogge, Richard W. and Trueblood, Mark and Trueblood, Patricia},

url = {http://arxiv.org/abs/1702.01657},

year  = {2017},

date = {2017-02-01},

urldate = {2017-02-20},

journal = {arXiv:1702.01657 [astro-ph]},

abstract = {We report the discovery of KELT-18b, a transiting hot Jupiter in a 2.87d orbit around the bright (V=10.1), hot, F4V star BD+60 1538 (TYC 3865-1173-1). We present follow-up photometry, spectroscopy, and adaptive optics imaging that allow a detailed characterization of the system. Our preferred model fits yield a host stellar temperature of 6670+/-120 K and a mass of 1.524+/-0.069 Msun, situating it as one of only a handful of known transiting planets with hosts that are as hot, massive, and bright. The planet has a mass of 1.18+/-0.11 Mjup, a radius of 1.57+/-0.04 Rjup, and a density of 0.377+/-0.040 g/cmtextasciicircum3, making it one of the most inflated planets known around a hot star. We argue that KELT-18b's high temperature, low surface gravity, and hot, bright host make it an excellent candidate for observations aimed at atmospheric characterization. We also present evidence for a bound stellar companion at a projected separation of textasciitilde1100 AU, and speculate that it may have contributed to the strong misalignment we suspect between KELT-18's spin axis and its planet's orbital axis. The inferior conjunction time is 2457542.524998 +/-0.000416 (BJD_TDB) and the orbital period is 2.8717510 +/- 0.0000029 days. We encourage Rossiter-McLaughlin measurements in the near future to confirm the suspected spin-orbit misalignment of this system.},

note = {arXiv: 1702.01657},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{dittmann_temperate_2017,

title = {A temperate rocky super-Earth transiting a nearby cool star},

author = {Dittmann, Jason A. and Irwin, Jonathan M. and Charbonneau, David and Bonfils, Xavier and Astudillo-Defru, Nicola and Haywood, Rapha\"{e}lle D. and Berta-Thompson, Zachory K. and Newton, Elisabeth R. and Rodriguez, Joseph E. and Winters, Jennifer G. and Tan, Thiam-Guan and Almenara, Jose-Manuel and Bouchy, Fran\c{c}ois and Delfosse, Xavier and Forveille, Thierry and Lovis, Christophe and Murgas, Felipe and Pepe, Francesco and Santos, Nuno C. and Udry, Stephane and W\"{u}nsche, Ana\"{e}l and Esquerdo, Gilbert A. and Latham, David W. and Dressing, Courtney D.},

url = {http://arxiv.org/abs/1704.05556},

doi = {10.1038/nature22055},

issn = {0028-0836, 1476-4687},

year  = {2017},

date = {2017-01-01},

urldate = {2017-04-21},

journal = {Nature},

volume = {544},

number = {7650},

pages = {333--336},

abstract = {M dwarf stars, which have masses less than 60 per cent that of the Sun, make up 75 per cent of the population of the stars in the Galaxy [1]. The atmospheres of orbiting Earth-sized planets are observationally accessible via transmission spectroscopy when the planets pass in front of these stars [2,3]. Statistical results suggest that the nearest transiting Earth-sized planet in the liquid-water, habitable zone of an M dwarf star is probably around 10.5 parsecs away [4]. A temperate planet has been discovered orbiting Proxima Centauri, the closest M dwarf [5], but it probably does not transit and its true mass is unknown. Seven Earth-sized planets transit the very low-mass star TRAPPIST-1, which is 12 parsecs away [6,7], but their masses and, particularly, their densities are poorly constrained. Here we report observations of LHS 1140b, a planet with a radius of 1.4 Earth radii transiting a small, cool star (LHS 1140) 12 parsecs away. We measure the mass of the planet to be 6.6 times that of Earth, consistent with a rocky bulk composition. LHS 1140b receives an insolation of 0.46 times that of Earth, placing it within the liquid-water, habitable zone [8]. With 90 per cent confidence, we place an upper limit on the orbital eccentricity of 0.29. The circular orbit is unlikely to be the result of tides and therefore was probably present at formation. Given its large surface gravity and cool insolation, the planet may have retained its atmosphere despite the greater luminosity (compared to the present-day) of its host star in its youth [9,10]. Because LHS 1140 is nearby, telescopes currently under construction might be able to search for specific atmospheric gases in the future [2,3].},

note = {arXiv: 1704.05556},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{temple_wasp-167b/kelt-13b:_2017,

title = {WASP-167b/KELT-13b: Joint discovery of a hot Jupiter transiting a rapidly-rotating F1V star},

author = {Temple, L. Y. and Hellier, C. and Albrow, M. D. and Anderson, D. R. and Bayliss, D. and Beatty, T. G. and Bieryla, A. and Brown, D. J. A. and Cargile, P. A. and Cameron, A. Collier and Collins, K. A. and Col\'{o}n, K. D. and Curtis, I. A. and D'Ago, G. and Delrez, L. and Eastman, J. and Gaudi, B. S. and Gillon, M. and Gregorio, J. and James, D. and Jehin, E. and Joner, M. D. and Kielkopf, J. F. and Kuhn, R. B. and Labadie-Bartz, J. and Latham, D. W. and Lendl, M. and Lund, M. B. and Malpas, A. L. and Maxted, P. F. L. and Myers, G. and Oberst, T. E. and Pepe, F. and Pepper, J. and Pollacco, D. and Queloz, D. and Rodriguez, J. E. and S\'{e}gransan, D. and Siverd, R. J. and Smalley, B. and Stassun, K. G. and Stevens, D. J. and Stockdale, C. and Tan, T. G. and Triaud, A. H. M. J. and Udry, S. and Villanueva Jr, S. and West, R. G. and Zhou, G.},

url = {http://arxiv.org/abs/1704.07771},

year  = {2017},

date = {2017-01-01},

urldate = {2017-04-28},

journal = {arXiv:1704.07771 [astro-ph]},

abstract = {We report the joint WASP/KELT discovery of WASP-167b/KELT-13b, a transiting hot Jupiter with a 2.02-d orbit around a $V$ = 10.5, F1V star with [Fe/H] = 0.1 $textbackslashpm$ 0.1. The 1.5 R$_textbackslashrm Jup$ planet was confirmed by Doppler tomography of the stellar line profiles during transit. We place a limit of $textless$ 8 M$_textbackslashrm Jup$ on its mass. The planet is in a retrograde orbit with a sky-projected spin-orbit angle of $textbackslashlambda = -165textasciicircumtextbackslashcirc textbackslashpm 5textasciicircumtextbackslashcirc$. This is in agreement with the known tendency for orbits around hotter stars to be more likely to be misaligned. WASP-167/KELT-13 is one of the few systems where the stellar rotation period is less than the planetary orbital period. We find evidence of non-radial stellar pulsations in the host star, making it a $textbackslashdelta$-Scuti or $textbackslashgamma$-Dor variable. The similarity to WASP-33, a previously known hot-Jupiter host with pulsations, adds to the suggestion that close-in planets might be able to excite stellar pulsations.},

note = {arXiv: 1704.07771},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{bayliss_hats-36b_2017,

title = {HATS-36b and 24 other transiting/eclipsing systems from the HATSouth - K2 Campaign 7 program},

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

url = {http://arxiv.org/abs/1706.03858},

year  = {2017},

date = {2017-01-01},

urldate = {2017-06-14},

journal = {arXiv:1706.03858 [astro-ph]},

abstract = {We report on the result of a campaign to monitor 25 HATSouth candidates using the K2 space telescope during Campaign 7 of the K2 mission. We discover HATS-36b (EPIC 215969174b), a hot Jupiter with a mass of 2.79$textbackslashpm$0.40 M$_J$ and a radius of 1.263$textbackslashpm$0.045 R$_J$ which transits a solar-type G0V star (V=14.386) in a 4.1752d period. We also refine the properties of three previously discovered HATSouth transiting planets (HATS-9b, HATS-11b, and HATS-12b) and search the K2 data for TTVs and additional transiting planets in these systems. In addition we also report on a further three systems that remain as Jupiter-radius transiting exoplanet candidates. These candidates do not have determined masses, however pass all of our other vetting observations. Finally we report on the 18 candidates which we are now able to classify as eclipsing binary or blended eclipsing binary systems based on a combination of the HATSouth data, the K2 data, and follow-up ground-based photometry and spectroscopy. These range in periods from 0.7 days to 16.7 days, and down to 1.5 mmag in eclipse depths. Our results show the power of combining ground-based imaging and spectroscopy with higher precision space-based photometry, and serve as an illustration as to what will be possible when combining ground-based observations with TESS data.},

note = {arXiv: 1706.03858},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{gaudi_giant_2017,

title = {A giant planet undergoing extreme-ultraviolet irradiation by its hot massive-star host},

author = {Gaudi, B. Scott and Stassun, Keivan G. and Collins, Karen A. and Beatty, Thomas G. and Zhou, George and Latham, David W. and Bieryla, Allyson and Eastman, Jason D. and Siverd, Robert J. and Crepp, Justin R. and Gonzales, Erica J. and Stevens, Daniel J. and Buchhave, Lars A. and Pepper, Joshua and Johnson, Marshall C. and Colon, Knicole D. and Jensen, Eric L. N. and Rodriguez, Joseph E. and Bozza, Valerio and Novati, Sebastiano Calchi and D’Ago, Giuseppe and Dumont, Mary T. and Ellis, Tyler and Gaillard, Clement and Jang-Condell, Hannah and Kasper, David H. and Fukui, Akihiko and Gregorio, Joao and Ito, Ayaka and Kielkopf, John F. and Manner, Mark and Matt, Kyle and Narita, Norio and Oberst, Thomas E. and Reed, Phillip A. and Scarpetta, Gaetano and Stephens, Denice C. and Yeigh, Rex R. and Zambelli, Roberto and Fulton, B. J. and Howard, Andrew W. and James, David J. and Penny, Matthew and Bayliss, Daniel and Curtis, Ivan A. and DePoy, D. L. and Esquerdo, Gilbert A. and Gould, Andrew and Joner, Michael D. and Kuhn, Rudolf B. and Labadie-Bartz, Jonathan and Lund, Michael B. and Marshall, Jennifer L. and McLeod, Kim K. and Pogge, Richard W. and Relles, Howard and Stockdale, Christopher and Tan, T. G. and Trueblood, Mark and Trueblood, Patricia},

url = {https://www.nature.com/nature/journal/vaop/ncurrent/full/nature22392.html},

doi = {10.1038/nature22392},

issn = {0028-0836},

year  = {2017},

date = {2017-06-01},

urldate = {2017-06-14},

journal = {Nature},

volume = {advance online publication},

abstract = {The amount of ultraviolet irradiation and ablation experienced by a planet depends strongly on the temperature of its host star. Of the thousands of extrasolar planets now known, only six have been found that transit hot, A-type stars (with temperatures of 7,300\textendash10,000 kelvin), and no planets are known to transit the even hotter B-type stars. For example, WASP-33 is an A-type star with a temperature of about 7,430 kelvin, which hosts the hottest known transiting planet, WASP-33b (ref. 1); the planet is itself as hot as a red dwarf star of type M (ref. 2). WASP-33b displays a large heat differential between its dayside and nightside, and is highly inflated\textendashtraits that have been linked to high insolation. However, even at the temperature of its dayside, its atmosphere probably resembles the molecule-dominated atmospheres of other planets and, given the level of ultraviolet irradiation it experiences, its atmosphere is unlikely to be substantially ablated over the lifetime of its star. Here we report observations of the bright star HD 195689 (also known as KELT-9), which reveal a close-in (orbital period of about 1.48 days) transiting giant planet, KELT-9b. At approximately 10,170 kelvin, the host star is at the dividing line between stars of type A and B, and we measure the dayside temperature of KELT-9b to be about 4,600 kelvin. This is as hot as stars of stellar type K4 (ref. 5). The molecules in K stars are entirely dissociated, and so the primary sources of opacity in the dayside atmosphere of KELT-9b are probably atomic metals. Furthermore, KELT-9b receives 700 times more extreme-ultraviolet radiation (that is, with wavelengths shorter than 91.2 nanometres) than WASP-33b, leading to a predicted range of mass-loss rates that could leave the planet largely stripped of its envelope during the main-sequence lifetime of the host star.},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{siverd_kelt-19ab:_2017,

title = {KELT-19Ab: A Ptextasciitilde4.6 Day Hot Jupiter Transiting a Likely Am Star with a Distant Stellar Companion},

author = {Siverd, Robert J. and Collins, Karen A. and Zhou, George and Gaudi, B. Scott and Stassun, Keivan G. and Johnson, Marshall C. and Quinn, Samuel N. and Bieryla, Allyson and Latham, David W. and Ciardi, David R. and Rodriguez, Joseph E. and Penev, Kaloyan and Pinsonneault, Marc and Pepper, Joshua and Eastman, Jason D. and Relles, Howard and Kielkopf, John F. and Gregorio, Joao and Oberst, Thomas E. and Aldi, Giulio Francesco and Esquerdo, Gilbert A. and Calkins, Michael L. and Berlind, Perry and Dressing, Courtney and Patel, Rahul and Stevens, Daniel J. and Beatty, Thomas G. and Lund, Michael B. and Labadie-Bartz, Jonathan and Kuhn, Rudolf B. and Colon, Knicole D. and James, David and Yao, Xinyu and Jensen, Eric L. N. and Cohen, David H. and McLeod, Kim K. and Penny, Matthew T. and Joner, Michael D. and Stephens, Denise C. and Villanueva Jr., Steven and Zambelli, Roberto and Stockdale, Christopher and Evans, Phil and Tan, Thiam-Guan and Curtis, Ivan A. and Reed, Phillip A. and Trueblood, Mark and Trueblood, Patricia},

url = {http://arxiv.org/abs/1709.07010},

year  = {2017},

date = {2017-01-01},

urldate = {2017-09-22},

journal = {arXiv:1709.07010 [astro-ph]},

abstract = {We present the discovery of the giant planet KELT-19Ab, which transits the moderately bright ($V textbackslashsim 9.9$) A8V star TYC 764-1494-1. We confirm the planetary nature of the companion via a combination of low-precision radial velocities, which limit the mass to $M_textbackslashrm P textless 4.1textbackslash,M_textbackslashrm J$ ($3textbackslashsigma$), and a clear Doppler tomography signal, which indicates a retrograde projected spin-orbit misalignment of $textbackslashlambda = -179.7textasciicircum+3.7_-3.8$ degrees. Global modeling indicates that the $T_textbackslashrm eff =7500 textbackslashpm 110textbackslash,textbackslashrm K$ host star has $M_* = 1.62textasciicircum+0.25_-0.20textbackslash,M_textbackslashodot$ and $R_* = 1.83 textbackslashpm 0.10textbackslash,R_textbackslashodot$. The planet has a radius of $R_textbackslashrm P=1.91 textbackslashpm 0.11textbackslash,R_textbackslashrm J$ and receives a stellar insolation flux of $textbackslashsim 3.2textbackslashtimes 10textasciicircum9textbackslash,textbackslashrmtextbackslash,ergtextbackslash,stextasciicircum-1textbackslash,cmtextasciicircum-2$, leading to an inferred equilibrium temperature of $T_textbackslashrm eq textbackslashsim 1935textbackslash,textbackslashrm K$ assuming zero albedo and complete heat redistribution. With a $vtextbackslashsinI_*=84.8textbackslashpm 2.0textbackslash,textbackslashrm kmtextbackslash,stextasciicircum-1$, the host star is rapidly-rotating. Interestingly, its $vtextbackslashsinI_*$ is relatively low compared to other stars with similar effective temperatures, and it appears to be enhanced in metallic species such as strontium but deficient in others such as calcium, suggesting that it is likely an Am star. KELT-19A would be the first definitive detection of an Am host of a transiting planet of which we are aware. Adaptive optics observations of the system reveal the existence of a companion with late G9V/early K1V spectral type at a projected separation of $textbackslashapprox 160textbackslash, textbackslashmathrmAU$. Radial velocity measurements indicate that this companion is bound. Most Am stars are known to have stellar companions, which are often invoked to explain the relatively slow rotation of the primary. In this case, the stellar companion is unlikely to have caused the tidal braking of the primary.},

note = {arXiv: 1709.07010},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{johnson_kelt-21b:_2017,

title = {KELT-21b: A Hot Jupiter Transiting the Rapidly-Rotating Metal-Poor Late-A Primary of a Likely Hierarchical Triple System},

author = {Johnson, Marshall C. and Rodriguez, Joseph E. and Zhou, George and Gonzales, Erica J. and Cargile, Phillip A. and Crepp, Justin R. and Penev, Kaloyan and Stassun, Keivan G. and Gaudi, B. Scott and Col\'{o}n, Knicole D. and Stevens, Daniel J. and Strassmeier, Klaus G. and Ilyin, Ilya and Collins, Karen A. and Kielkopf, John F. and Oberst, Thomas E. and Maritch, Luke and Reed, Phillip A. and Gregorio, Joao and Bozza, Valerio and Novati, Sebastiano Calchi and D'Ago, Giuseppe and Scarpetta, Gaetano and Zambelli, Roberto and Latham, David W. and Bieryla, Allyson and Cochran, William D. and Endl, Michael and Tayar, Jamie and Serenelli, Aldo and Aguirre, Victor Silva and Clarke, Seth P. and Martinez, Maria and Spencer, Michelle and Trump, Jason and Joner, Michael D. and Bugg, Adam G. and Hintz, Eric G. and Stephens, Denise C. and Arredondo, Anicia and Benzaid, Anissa and Yazdi, Sormeh and McLeod, Kim K. and Jensen, Eric L. N. and Hancock, Daniel A. and Sorber, Rebecca L. and Kasper, David H. and Jang-Condell, Hannah and Beatty, Thomas G. and Carroll, Thorsten and Eastman, Jason and James, David and Kuhn, Rudolf B. and Labadie-Bartz, Jonathan and Lund, Michael B. and Mallonn, Matthias and Pepper, Joshua and Siverd, Robert J. and Yao, Xinyu and Cohen, David H. and Curtis, Ivan A. and DePoy, D. L. and Fulton, Benjamin J. and Penny, Matthew T. and Relles, Howard and Stockdale, Christopher and Tan, Thiam-Guan and Villanueva Jr, Steven},

url = {http://arxiv.org/abs/1712.03241},

year  = {2017},

date = {2017-01-01},

urldate = {2018-01-02},

journal = {arXiv:1712.03241 [astro-ph]},

abstract = {We present the discovery of KELT-21b, a hot Jupiter transiting the $V=10.5$ A8V star HD 332124. The planet has an orbital period of $P=3.6127647textbackslashpm0.0000033$ days and a radius of $1.586_-0.040textasciicircum+0.039$ $R_J$. We set an upper limit on the planetary mass of $M_Ptextless3.91$ $M_J$ at $3textbackslashsigma$ confidence. We confirmed the planetary nature of the transiting companion using this mass limit and Doppler tomographic observations to verify that the companion transits HD 332124. These data also demonstrate that the planetary orbit is well-aligned with the stellar spin, with a sky-projected spin-orbit misalignment of $textbackslashlambda=-5.6_-1.9textasciicircum+1.7 textbackslashcirc$. The star has $T_textbackslashmathrmeff=7598_-84textasciicircum+81$ K, $M_*=1.458_-0.028textasciicircum+0.029$ $M_textbackslashodot$, $R_*=1.638textbackslashpm0.034$ $R_textbackslashodot$, and $vtextbackslashsin I_*=146$ km s$textasciicircum-1$, the highest projected rotation velocity of any star known to host a transiting hot Jupiter. The star also appears to be somewhat metal-poor and $textbackslashalpha$-enhanced, with [Fe/H]$=-0.405_-0.033textasciicircum+0.032$ and [$textbackslashalpha$/Fe]$=0.145 textbackslashpm 0.053$; these abundances are unusual, but not extraordinary, for a young star with thin-disk kinematics like KELT-21. High-resolution imaging observations revealed the presence of a pair of stellar companions to KELT-21, located at a separation of 1.2" and with a combined contrast of $textbackslashDelta K_S=6.39 textbackslashpm 0.06$ with respect to the primary. Although these companions are most likely physically associated with KELT-21, we cannot confirm this with our current data. If associated, the candidate companions KELT-21 B and C would each have masses of $textbackslashsim0.12$ $M_textbackslashodot$, a projected mutual separation of $textbackslashsim20$ AU, and a projected separation of $textbackslashsim500$ AU from KELT-21. KELT-21b may be one of only a handful of known transiting planets in hierarchical triple stellar systems.},

note = {arXiv: 1712.03241},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{henning_hats-50b_2017,

title = {HATS-50b through HATS-53b: four transiting hot Jupiters orbiting G-type stars discovered by the HATSouth survey},

author = {Henning, Th and Mancini, L. and Sarkis, P. and Bakos, G. A. and Hartman, J. D. and Bayliss, D. and Bento, J. and Bhatti, W. and Brahm, R. and Ciceri, S. and Csubry, Z. and de Val-Borro, M. and Espinoza, N. and Fulton, B. J. and Howard, A. W. and Isaacson, H. T. and Jordan, A. and Marcy, G. W. and Penev, K. and Rabus, M. and Suc, V. and Tan, T. G. and Tinney, C. G. and Wright, D. J. and Zhou, G. and Durkan, S. and Lazar, J. and Papp, I. and Sari, P.},

url = {http://arxiv.org/abs/1712.04324},

year  = {2017},

date = {2017-01-01},

urldate = {2018-01-02},

journal = {arXiv:1712.04324 [astro-ph]},

abstract = {We report the discovery of four close-in transiting exoplanets, HATS-50 through HATS-53, discovered using the HATSouth three-continent network of homogeneous and automated telescopes. These new exoplanets belong to the class of hot Jupiters and orbit G-type dwarf stars, with brightness in the range V=12.5-14.0 mag. While HATS-53 has many physical characteristics similar to the Sun, the other three stars appear to be metal rich, larger and more massive. Three of the new exoplanets, namely HATS-50, HATS-51 and HATS-53, have low density and similar orbital period. Instead, HATS-52 is more dense and has a shorter orbital period. It also receives an intensive radiation from its parent star and, consequently, presents a high equilibrium temperature. HATS-50 shows a marginal additional transit feature consistent with an ultra-short period hot super Neptune, which will be able to be confirmed with TESS photometry.},

note = {arXiv: 1712.04324},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{messina_age_2016,

title = {On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association},

author = {Messina, S. and Santallo, R. and Tan, T. G. and Elliott, P. and Feiden, G. A. and Buccino, A. and Mauas, P. and Petrucci, R. and Jofre', E.},

url = {http://arxiv.org/abs/1612.04597},

year  = {2016},

date = {2016-01-01},

urldate = {2016-12-24},

journal = {arXiv:1612.04597 [astro-ph]},

abstract = {There are a variety of different techniques available to estimate the ages of pre-main-sequence stars. Components of physical pairs, thanks to their strict coevality and the mass difference, such as the binary system analysed in this paper, are best suited to test the effectiveness of these different techniques. We consider the system WW Psa + TX Psa whose membership of the 25-Myr beta Pictoris association has been well established by earlier works. We investigate which age dating technique provides the best agreement between the age of the system and that of the association. We have photometrically monitored WW Psa and TX Psa and measured their rotation periods as P = 2.37d and P = 1.086d, respectively. We have retrieved from the literature their Li equivalent widths and measured their effective temperatures and luminosities. We investigate whether the ages of these stars derived using three independent techniques are consistent with the age of the beta Pictoris association. We find that the rotation periods and the Li contents of both stars are consistent with the distribution of other bona fide members of the cluster. On the contrary, the isochronal fitting provides similar ages for both stars, but a factor of about four younger than the quoted age of the association, or about 30% younger when the effects of magnetic fields are included. We explore the origin of the discrepant age inferred from isochronal fitting, including the possibilities that either the two components may be unresolved binaries or that the basic stellar parameters of both components are altered by enhanced magnetic activity. The latter is found to be the more reasonable cause, suggesting that age estimates based on the Li content is more reliable than isochronal fitting for pre-main-sequence stars with pronounced magnetic activity.},

note = {arXiv: 1612.04597},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{messina_beta_2016,

title = {The beta Pictoris association: Catalog of photometric rotational periods of low-mass members and candidate members},

author = {Messina, S. and Millward, M. and Buccino, A. and Zhang, L. and Medhi, B. J. and Jofre', E. and Petrucci, R. and Pi, Q. and Hambsch, F.-J. and Kehusmaa, P. and Harlingten, C. and Artemenko, S. and Curtis, I. and Hentunen, V.-P. and Malo, L. and Mauas, P. and Monard, B. and Serrano, M. Muro and Naves, R. and Santallo, R. and Savuskin, A. and Tan, T. G.},

url = {http://arxiv.org/abs/1612.04591},

doi = {10.1051/0004-6361/201629152},

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

year  = {2016},

date = {2016-01-01},

urldate = {2016-12-24},

journal = {Astronomy \& Astrophysics},

abstract = {We intended to compile the most complete catalog of bona fide members and candidate members of the beta Pictoris association, and to measure their rotation periods and basic properties from our own observations, public archives, and exploring the literature. We carried out a multi-observatories campaign to get our own photometric time series and collected all archived public photometric data time series for the stars in our catalog. Each time series was analyzed with the Lomb-Scargle and CLEAN periodograms to search for the stellar rotation periods. We complemented the measured rotational properties with detailed information on multiplicity, membership, and projected rotational velocity available in the literature and discussed star by star. We measured the rotation periods of 112 out of 117 among bona fide members and candidate members of the beta Pictoris association and, whenever possible, we also measured the luminosity, radius, and inclination of the stellar rotation axis. This represents to date the largest catalog of rotation periods of any young loose stellar association. We provided an extensive catalog of rotation periods together with other relevant basic properties useful to explore a number of open issues, such as the causes of spread of rotation periods among coeval stars, evolution of angular momentum, and lithium-rotation connection.},

note = {arXiv: 1612.04591},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{stevens_kelt-12b:_2016,

title = {KELT-12b: A $P textbackslashsim 5$ Day, Highly Inflated Hot Jupiter Transiting a Mildly Evolved Hot Star},

author = {Stevens, Daniel J. and Collins, Karen A. and Gaudi, B. Scott and Beatty, Thomas G. and Siverd, Robert J. and Bieryla, Allyson and Fulton, Benjamin J. and Crepp, Justin R. and Gonzales, Erica J. and Coker, Carl T. and Penev, Kaloyan and Stassun, Keivan G. and Jensen, Eric L. N. and Howard, Andrew W. and Latham, David W. and Rodriguez, Joseph E. and Zambelli, Roberto and Bozza, Valerio and Reed, Phillip A. and Gregorio, Joao and Buchhave, Lars A. and Penny, Matthew T. and Pepper, Joshua and Berlind, Perry and Novati, Sebastiano Calchi and Calkins, Michael L. and D'Ago, Giuseppe and Eastman, Jason D. and Bayliss, D. and Col\'{o}n, Knicole D. and Curtis, Ivan A. and DePoy, D. L. and Esquerdo, Gilbert A. and Gould, Andrew and Joner, Michael D. and Kielkopf, John F. and Labadie-Bartz, Jonathan and Lund, Michael B. and Manner, Mark and Marshall, Jennifer L. and McLeod, Kim K. and Oberst, Thomas E. and Pogge, Richard W. and Scarpetta, Gaetano and Stephens, Denise C. and Stockdale, Christopher and Tan, T. G. and Trueblood, Mark and Trueblood, Patricia},

url = {http://arxiv.org/abs/1608.04714},

year  = {2016},

date = {2016-01-01},

urldate = {2016-12-24},

journal = {arXiv:1608.04714 [astro-ph]},

abstract = {We report the discovery of KELT-12b, a highly inflated Jupiter-mass planet transiting a mildly evolved host star. We identified the initial transit signal in the KELT-North survey data and established the planetary nature of the companion through precise follow-up photometry, high-resolution spectroscopy, precise radial velocity measurements, and high-resolution adaptive optics imaging. Our preferred best-fit model indicates that the $V = 10.64$ host, TYC 2619-1057-1, has $T_textbackslashrm eff = 6278 textbackslashpm 51$ K, $textbackslashlogg_textbackslashstar = 3.89textasciicircum+0.054_-0.051$, and [Fe/H] = $0.19textasciicircum+0.083_-0.085$, with an inferred mass $M_textbackslashstar = 1.59textasciicircum+0.071_-0.091 M_textbackslashodot$ and radius $R_textbackslashstar = 2.37 textbackslashpm 0.18 R_textbackslashodot$. The planetary companion has $M_textbackslashrm P = 0.95 textbackslashpm 0.14 M_textbackslashrm J$, $R_textbackslashrm P = 1.79textasciicircum+0.18_-0.17 R_textbackslashrm J$, $textbackslashlogg_textbackslashrm P = 2.87textasciicircum+0.097_-0.098$, and density $textbackslashrho_textbackslashrm P = 0.21textasciicircum+0.075_-0.054$ g cm$textasciicircum-3$, making it one of the most inflated giant planets known. The time of inferior conjunction in $textbackslashrm BJD_TDB$ is $2457088.692055 textbackslashpm 0.0009$ and the period is $P = 5.0316144 textbackslashpm 0.0000306$ days. Despite the relatively large separation of $textbackslashsim0.07$ AU implied by its $textbackslashsim 5.03$-day orbital period, KELT-12b receives significant flux of $2.93textasciicircum+0.33_-0.30 textbackslashtimes 10textasciicircum9$ erg s$textasciicircum-1$ cm$textasciicircum-2$ from its host. We compare the radii and insolations of transiting gas-giant planets around hot ($T_textbackslashrm eff textbackslashgeq 6250$ K) and cool stars, noting that the observed paucity of known transiting giants around hot stars with low insolation is likely due to selection effects. We underscore the significance of long-term ground-based monitoring of hot stars and space-based targeting of hot stars with the Transiting Exoplanet Survey Satellite (TESS) to search for inflated giants in longer-period orbits.},

note = {arXiv: 1608.04714},

keywords = {},

pubstate = {published},

tppubtype = {article}

}