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

Lund, Michael B.; Rodriguez, Joseph E.; Zhou, George; Gaudi, B. Scott; Stassun, Keivan G.; Johnson, Marshall C.; Bieryla, Allyson; Oelkers, Ryan J.; Stevens, Daniel J.; Collins, Karen A.; Penev, K.; Quinn, Samuel N.; Latham, David W.; Villanueva, Steven; Eastman, Jason D.; Kielkopf, John F.; Oberst, Thomas E.; Jensen, Eric L. N.; Cohen, David H.; Joner, M. D.; Stephens, Denise C.; Relles, Howard M.; Corfini, G.; Gregorio, J.; Zambelli, Roberto; Esquerdo, Gilbert A.; Calkins, M.; Berlind, P.; Ciardi, David R.; Dressing, Courtney D.; Patel, Rahul; Gagnon, Patrick; Gonzales, Erica J.; Beatty, Thomas G.; Siverd, Robert J.; Labadie-Bartz, Jonathan; Kuhn, Rudolf B.; Colón, Knicole D.; James, D. J.; Pepper, Joshua; Fulton, Benjamin J.; McLeod, Kim K.; Stockdale, C. J.; Novati, S. Calchi; DePoy, D. L.; Gould, Andrew; Marshall, J. L.; Trueblood, Mark; Trueblood, Patricia; Johnson, John Asher; Wright, Jason T.; McCrady, Nate; Wittenmyer, Robert A.; Johnson, Samson A.; Sergi, Anthony; Wilson, Maurice L.; Sliski, David H.

doi:10.3847/1538-3881/aa8f95

Cited by 99 publications

(60 citation statements)

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“…0 h m s = , decl.=+31°39′56 2 J2000.0). This is the same field that also yielded our other two most rapidly rotating planet hosts, KELT-9b ) and KELT-20b/ MASCARA-2b (Lund et al 2017;Talens et al 2017b), as well as KELT-8b (Fulton et al 2015). In the analysis of 6783 observations of HD 332124 obtained between 2007 May 29 and 2014 November 25 UT, we identified a candidate transit signal with a period of 3.612782 days and a depth of 1%; the target was given the KELT candidate ID of KC11C039077.…”

Section: Discoverymentioning

confidence: 90%

“…We show known transiting planets taken from the NASA Exoplanet Archive (https://exoplanetarchive. ipac.caltech.edu/), plus KELT-19Ab (Siverd et al 2018), KELT-20b/ MASCARA-2b (Lund et al 2017;Talens et al 2017b), and MASCARA-1b (Talens et al 2017a). The location of KELT-21b is marked.…”

Section: Discussionmentioning

confidence: 99%

“…KELT-21 is well above the Kraft break, where hot Jupiters tend to have a wide range of misalignments (Winn et al 2010). Although its well-aligned orbit is somewhat unusual in this context, some other hot Jupiters around hot stars are also aligned, such as KELT-7b (Zhou et al 2016a) and KELT-20b/MASCARA-2b (Lund et al 2017;Talens et al 2017b). Even for an isotropic distribution of misalignments, some systems should be aligned by chance.…”

Section: Spin-orbit Misalignmentmentioning

confidence: 99%

“…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%

“…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. As KELT was designed to target brighter stars ( V 8 1 1 < < ) than those in other transit surveys, hot, bright stars are overrepresented in its sample due to the larger volume probed.…”

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: Discoverymentioning

confidence: 90%

Section: Discussionmentioning

confidence: 99%

Section: Spin-orbit Misalignmentmentioning

confidence: 99%

Section: Spin-orbit Misalignmentmentioning

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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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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Future Exoplanet Research: XUV (EUV and X-Ray) Detection and Characterization

Branduardi‐Raymont

Dunn

Sciortino

2017

Handbook of Exoplanets

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This chapter gives an overview of the current status of XUV research in exoplanets and highlights the prospects of future observations. Fundamental questions about the formation and the physical and chemical evolution of exoplanets, particularly hot Jupiters, are addressed through the different lines of XUV research: these comprise XUV irradiation of planetary atmospheres by the host stars, and consequent mass loss and atmospheric evaporation; X-ray and UV transits in exoplanet systems; and Star-Planet Interactions, most often determined by magnetic and tidal forces. While no other UV instrumentation as powerful as that carried by the Hubble Space Telescope will be available for detailed studies in the foreseeable future, the discovery potential of future revolutionary X-ray observatories, such as ATHENA and Lynx, will provide accurate atmosphere characterization and will make strides towards establishing the physics of the interactions between exoplanets and their host stars.

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

Cited by 99 publications

References 100 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

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

Future Exoplanet Research: XUV (EUV and X-Ray) Detection and Characterization

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