KELT-19Ab: A P ∼ 4.6-day Hot Jupiter Transiting a Likely Am Star with a Distant Stellar Companion

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

doi:10.3847/1538-3881/aa9e4d

Cited by 69 publications

(71 citation statements)

References 73 publications

(92 reference statements)

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“…The first two of these are straightforward to measure; the latter is not, and we cannot measure this quantity for KELT-21 using our existing data. We can, however, set limits on ψ by making reasonable assumptions to limit I * , as we did in Siverd et al (2018) and Lund et al (2017). We follow Iorio (2011) by assuming that KELT-21 must be rotating at less than the break-up velocity, which must limit I * , since the equatorial velocity is v v I I sin sin eq * * = .…”

Section: Spin-orbit Misalignmentmentioning

confidence: 99%

“…Alternately, if only a single epoch of photometry is available, multicolor photometry can be used to check that the secondary is consistent with being at the same distance as the primary (e.g., Evans et al 2016). Finally, spectra can be used to determine whether the companion shares the systemic velocity of the primary (e.g., Siverd et al 2018). We, however, have only a single epoch of single-color photometry of the candidate companions found in Section 2.4, and the candidate companions are too faint to be detected in our spectra.…”

Section: Tablementioning

confidence: 99%

“…Indeed, more than half of the KELT planets discovered to date orbit stars above the Kraft break Pepper et al 2013;Collins et al 2014;Bieryla et al 2015;Zhou et al 2016b;Gaudi et al 2017;Lund et al 2017;McLeod et al 2017;Siverd et al 2018;Stevens et al 2017;Temple et al 2017), or, in the case of KELT-11, was above the Kraft break when it was on the main sequence . As discussed in Lund et al (2017), this is partially by design and Malmquist bias, and partially by accident.…”

Section: Introductionmentioning

confidence: 99%

“…In Kepler-13, the primary and secondary stars are of a similar mass while the tertiary star is much less massive, and the tertiary was discovered through RV observations of the secondary (Santerne et al 2012;Johnson et al 2014). Transit survey follow-up is typically biased against the latter type of system; visual binaries are often excluded from survey target lists, and the presence of multiple lines in a spectrum (especially if some of them are moving) is typically taken as reason to conclude that a planet candidate is a false positive, even if such a system could in fact host a planet (see Siverd et al 2018 for a recent case of a confirmed planet discovered in a binary stellar system with two sets of lines in the spectra). Planets in hierarchical triple systems are also of interest because their dynamics are richer than those of hot Jupiters in stellar binaries (e.g., Fang et al 2017;Hamers 2017); certain configurations could enhance the efficiency of hot Jupiter formation by high-eccentricity (Kozai-Lidov) migration (Hamers 2017).…”

Section: Introductionmentioning

confidence: 99%

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KELT-21b: A Hot Jupiter Transiting the Rapidly Rotating Metal-poor Late-A Primary of a Likely Hierarchical Triple System

Johnson

Rodriguez

Zhou

et al. 2018

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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=3.6127647±0.0000033 days and a radius of 1.586 0.040 0.039 -+ R J . We set an upper limit on the 1 planetary mass of M 3.91 P < M J at 3s 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 spinorbit misalignment of 5.6 1.91.7 . 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 K 6.39 0.06 S D =  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 ∼0.12 M ☉ , a projected mutual separation of ∼20 au, and a projected separation of ∼500 au from KELT-21. KELT-21b may be one of only a handful of known transiting planets in hierarchical triple stellar systems.

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Section: Spin-orbit Misalignmentmentioning

confidence: 99%

Section: Tablementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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KELT-21b: A Hot Jupiter Transiting the Rapidly Rotating Metal-poor Late-A Primary of a Likely Hierarchical Triple System

Johnson

Rodriguez

Zhou

et al. 2018

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“…We also note that the agreement between the SED and a single star spectral model rules out any blending against a bright background star. Line profiles measured from least-square deconvolutions can reveal close-companions with flux ratios of ∼ 1% (see Figure 5 of Siverd et al 2018). To search for fainter stellar blends, we inject and attempt to recover an additional stellar signal in the out-of-transit Magellan/MIKE line profiles.…”

Section: Blend Scenariosmentioning

confidence: 99%

HATS-70b: A 13 MJ Brown Dwarf Transiting an A Star*

Zhou¹,

Bakos²,

Bento³

et al. 2019

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We report the discovery of HATS-70b, a transiting brown dwarf at the deuterium burning limit. HATS-70b has a mass of M p = 12.9 +1.8 −1.6 M Jup and a radius of R p = 1.384 +0.079 −0.074 R Jup , residing in a close-in orbit with a period of 1.89 days. The host star is a M = 1.78 ± 0.12 M A star rotating at v sin I = 40.61 +0.32 −0.35 km s −1 , enabling us to characterize the spectroscopic transit of the brown dwarf via Doppler tomography. We find that HATS-70b, like other massive planets and brown dwarfs previously sampled, orbits in a low projected-obliquity orbit with λ = 8.9 +5.6 −4.5 • . The low obliquities of these systems is surprising given all brown dwarf and massive planets with obliquities measured orbit stars hotter than the Kraft break. This trend is tentatively inconsistent with dynamically chaotic migration for systems with massive companions, though the stronger tidal influence of these companions makes it difficult to draw conclusions on the primordial obliquity distribution of this population. We also introduce a modeling scheme for planets around rapidly rotating stars, accounting for the influence of gravity darkening on the derived stellar and planetary parameters. site is operated in conjunction with MPIA, and the station at Siding Spring Observatory (SSO) is operated jointly with ANU. This paper includes data gathered with the MPG 2.2 m and ESO 3.6 m telescopes at the ESO Observatory in La Silla. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile.

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KELT: The Kilodegree Extremely Little Telescope, a Survey for Exoplanets Transiting Bright, Hot Stars

Pepper¹,

Stassun²,

Gaudi³

2018

Handbook of Exoplanets

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The KELT project was originally designed as a small-aperture, wide-field photometric survey that would be optimally sensitive to planets transiting bright (V~8-10) stars. This magnitude range corresponded to the gap between the faint magnitude limit where radial velocity surveys were complete, and the bright magnitude limit for transiting planet hosts routinely found by dedicated ground-based transit surveys. Malmquist bias and other factors have also led the KELT survey to focus on discovering planets transiting relatively hot host stars as well. To date, the survey has discovered 22 transiting hot Jupiters, including some of the brightest transiting planet host stars known to date. Over half of these planets transit rapidly-rotating stars with Teff > 6250 K, which had been largely eschewed by both radial velocity and transit surveys, due to the challenge of obtaining precision radial velocities for such stars. The KELT survey has developed a protocol and specialized software for confirming transiting planets around stars rotating as rapidly as ~200 km/s. This chapter reviews KELT planet discoveries, describes their scientific value, and also briefly discusses the non-exoplanet science produced by the KELT project, especially long-timescale phenomena and preparations for the TESS mission.

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KELT-19Ab: A P ∼ 4.6-day Hot Jupiter Transiting a Likely Am Star with a Distant Stellar Companion

Cited by 69 publications

References 73 publications

KELT-21b: A Hot Jupiter Transiting the Rapidly Rotating Metal-poor Late-A Primary of a Likely Hierarchical Triple System

KELT-21b: A Hot Jupiter Transiting the Rapidly Rotating Metal-poor Late-A Primary of a Likely Hierarchical Triple System

HATS-70b: A 13 MJ Brown Dwarf Transiting an A Star*

KELT: The Kilodegree Extremely Little Telescope, a Survey for Exoplanets Transiting Bright, Hot Stars

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