KELT-11b: A Highly Inflated Sub-Saturn Exoplanet Transiting the V = 8 Subgiant HD 93396

Pepper, Joshua; Rodriguez, Joseph E.; Collins, Karen A.; Johnson, John Asher; Fulton, Benjamin J.; Howard, Andrew W.; Beatty, Thomas G.; Stassun, Keivan G.; Isaacson, Howard; Colón, Knicole D.; Lund, Michael B.; Kuhn, Rudolf B.; Siverd, Robert J.; Gaudi, B. Scott; Tan, T. G.; Curtis, Ivan A.; Stockdale, C. J.; Mawet, Dimitri; Bottom, Michael; James, D. J.; Zhou, George; Bayliss, Daniel; Cargile, Phillip A.; Bieryla, Allyson; Penev, K.; Latham, David W.; Labadie-Bartz, Jonathan; Kielkopf, John F.; Eastman, Jason D.; Oberst, Thomas E.; Jensen, Eric L. N.; Nelson, Peter; Sliski, David H.; Wittenmyer, Robert A.; McCrady, Nate; Wright, Jason T.; Relles, Howard M.; Stevens, Daniel J.; Joner, M. D.; Hintz, E. G.

doi:10.3847/1538-3881/aa6572

Cited by 68 publications

(50 citation statements)

References 82 publications

(103 reference statements)

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“…The spacecraft's four year primary mission, together with its more recent K2 program extension (Howell et al 2014), confirmed the existence of over 2500 planets 1 , including many that resemble nothing found in the solar system. This incredible diversity includes the so-called 'hot Jupiters' and 'hot Neptunes' (e.g., Mayor & Queloz 1995;Charbonneau et al 2000;Gillon et al 2007;Bakos et al 2010;Bayliss et al 2013), planets moving on extremely eccentric orbits (e.g., Jones et al 2006;Wittenmyer et al 2017), planets with densities greater than iron and even osmium (e.g., Deleuil et al 2008;Dumusque et al 2014;Johns et al 2018), or comparable to styrofoam (e.g., Faedi et al 2011;Welsh et al 2015;Pepper et al 2017). Perhaps most surprisingly, Kepler revealed that planets between the size of Earth and Neptune ("super-Earths" or "mini-Neptunes") are incredibly common, despite the fact that no analog exists in the solar system (e.g., Charbonneau et al 2009; Barragán et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Minerva-Australis. I. Design, Commissioning, and First Photometric Results

Addison

Wright

Wittenmyer

et al. 2019

PASP

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100

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The MINERVA-Australis telescope array is a facility dedicated to the follow-up, confirmation, characterization, and mass measurement of planets orbiting bright stars discovered by the Transiting Exoplanet Survey Satellite (TESS) -a category in which it is almost unique in the Southern Hemisphere. It is located at the University of Southern Queensland's Mount Kent Observatory near Toowoomba, Australia. Its flexible design enables multiple 0.7 m robotic telescopes to be used both in combination, and independently, for high-resolution spectroscopy and precision photometry of TESS transit planet candidates.MINERVA-Australis also enables complementary studies of exoplanet spin-orbit alignments via Doppler observations of the Rossiter-McLaughlin effect, radial velocity searches for nontransiting planets, planet searches using transit timing variations, and ephemeris refinement for TESS planets. In this first paper, we describe the design, photometric instrumentation, software, and science goals of MINERVA-Australis, and note key differences from its Northern Hemisphere counterpart, the MINERVA array. We use recent transit observations of four PASP 3 planets, WASP-2b, WASP-44b, WASP-45b, and HD 189733b, to demonstrate the photometric capabilities of MINERVA-Australis.

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Section: Introductionmentioning

confidence: 99%

Minerva-Australis. I. Design, Commissioning, and First Photometric Results

Addison

Wright

Wittenmyer

et al. 2019

PASP

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100

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“…KELT observations have surveyed more than 70% of the celestial sphere, down to a limiting magnitude near V ∼ 13, with a baseline of 9 yrs using KELT North (hereafter, KELT-N) and 5 yrs using KELT South (hereafter, KELT-S). Initially deployed to detect exoplanet transits around bright (V < 10) stars, the survey has contributed discoveries to supernovae (Siverd et al 2015), the monitoring of Be Stars (Labadie-Bartz et al 2017), eclipses of stars by disks (Rodriguez et al 2013), gyrochronology of young stars (Cargile et al 2014), pre-identification of young variable objects to be observed by K2 (Rodriguez et al 2017a,b;Ansdell et al 2017), more than 21 confirmed transiting planets (with 19 in press Pepper et al 2013;Collins et al 2014;Bieryla et al 2015;Fulton et al 2015;Eastman et al 2016;Kuhn et al 2016;Rodriguez et al 2016c;Zhou et al 2016;Gaudi et al 2017;McLeod et al 2017;Oberst et al 2017;Pepper et al 2017;Stevens et al 2017;Temple et al 2017;Lund et al 2017;Siverd et al 2017)) and 1 short period, transiting brown dwarf .…”

Section: Introductionmentioning

confidence: 99%

Variability Properties of Four Million Sources in the TESS Input Catalog Observed with the Kilodegree Extremely Little Telescope Survey

Oelkers

Rodriguez

Stassun

et al. 2017

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102

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The Kilodegree Extremely Little Telescope (KELT) has been surveying more than 70% of the celestial sphere for nearly a decade. While the primary science goal of the survey is the discovery of transiting, large-radii planets around bright host stars, the survey has collected more than 10 6 images, with a typical cadence between 10 − 30 minutes, for more than 4 million sources with apparent visual magnitudes in the approximate range 7 < V < 13. Here we provide a catalog of 52,741 objects showing significant large-amplitude fluctuations likely caused by stellar variability and 62,229 objects identified with likely stellar rotation periods. The detected variability ranges in rms-amplitude from 3 mmag to 2.3 mag, and the detected periods range from ∼0.1 days to 2000 days. We provide variability upper limits for all other ∼4 million sources. These upper limits are principally a function of stellar brightness, but we achieve typical 1σ sensitivity on 30-minute timescales down to ∼5 mmag at V ∼ 8, and down to ∼43 mmag at V ∼ 13. We have matched our catalog to the TESS Input catalog and the AAVSO Variable Star Index to precipitate the follow up and classification of each source. The catalog is maintained as a living database on the Filtergraph visualization portal at the URL https://filtergraph.com/kelt_vars.

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“…In recent years, several papers have provided multiple lines of evidence showing that the initial spectroscopic estimates of the masses of the "Retired A Stars" were likely generally slightly overestimated and the uncertainties in their masses likely underestimated. Indeed, it appears that the majority of the members of the "Retired A Star" sample that have accurate mass measurements (via astroseismology or transits; Johnson et al 2014;Pepper et al 2017;Campante et al 2017;North et al 2017;Stassun et al 2017;Stello et al 2017) appear to actually be "Retired F Stars," i.e., more massive than the solar-type stars that dominated early RV surveys (and are therefore more massive than the Kraft break), but less massive than a zero-age main-sequence (ZAMS) A star. In retrospect, this fact should not be very surprising, as the average age of the Galactic thin disk (whose stars dominate the local solar neighborhood) is 7.4 8.2 Gyr - (Kilic et al 2017), corresponding to the hydrogen-fusing lifetime of a ZAMS late F star.…”

Section: Introductionmentioning

confidence: 99%

KELT-20b: A Giant Planet with a Period of P ∼ 3.5 days Transiting the V ∼ 7.6 Early A Star HD 185603

Lund

Rodriguez

Zhou

et al. 2017

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We report the discovery of KELT-20b, a hot Jupiter transiting a V 7.6 early A star, HD 185603, with an orbital period of P 3.47  days. Archival and follow-up photometry, Gaia parallax, radial velocities, Doppler tomography, and AO imaging were used to confirm the planetary nature of KELT-20b and characterize the system. From global modeling we infer that KELT-20 is a rapidly rotating ) . We place a 3s upper limit of M 3.5 J on the mass of the planet. Doppler tomographic 1 measurements indicate that the planetary orbit normal is well aligned with the projected spin axis of the star ( 3 . 4 2 . 1 l =    ). The inclination of the star is constrained to I 24 . 4 155 . 6 *  < <  , implying a three-dimensional spin-orbit alignment of 1 . 3 69 . 8 y  < <  . KELT-20b receives an insolation flux of 8 10 erg s cm 9 1 2´--, implying an equilibrium temperature of of ∼2250 K, assuming zero albedo and complete heat redistribution. Due to the high stellar T eff , KELT-20b also receives an ultraviolet (wavelength d 91.2  nm) insolation flux of 9.1 10 erg s cm 4 1 2´--, possibly indicating significant atmospheric ablation. Together with WASP-33, Kepler-13 A, HAT-P-57, KELT-17, and KELT-9, KELT-20 is the sixth A star host of a transiting giant planet, and the thirdbrightest host (in V ) of a transiting planet.

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KELT-11b: A Highly Inflated Sub-Saturn Exoplanet Transiting the V = 8 Subgiant HD 93396

Cited by 68 publications

References 82 publications

Minerva-Australis. I. Design, Commissioning, and First Photometric Results

Minerva-Australis. I. Design, Commissioning, and First Photometric Results

Variability Properties of Four Million Sources in the TESS Input Catalog Observed with the Kilodegree Extremely Little Telescope Survey

KELT-20b: A Giant Planet with a Period of P ∼ 3.5 days Transiting the V ∼ 7.6 Early A Star HD 185603

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