The KELT Follow-up Network and Transit False-positive Catalog: Pre-vetted False Positives for TESS

Collins, Karen A.; Collins, Kevin I.; Pepper, Joshua; Labadie-Bartz, Jonathan; Stassun, Keivan G.; Gaudi, B. Scott; Bayliss, D.; Bento, J.; Colón, Knicole D.; Feliz, Dax L.; James, D. J.; Johnson, Marshall C.; Kuhn, Rudolf B.; Lund, Michael B.; Penny, Matthew T.; Rodriguez, Joseph E.; Siverd, Robert J.; Stevens, Daniel J.; Yao, Xinyu; Zhou, George; Akshay, Mundra; Aldi, G. F.; Ashcraft, Cliff; Awiphan, S.; Baştürk, Özgür; Baker, David; Beatty, Thomas G.; Benni, Paul; Berlind, P.; Berriman, G. Bruce; Berta-Thompson, Zachory K.; Bieryla, Allyson; Bozza, V.; Novati, S. Calchi; Calkins, M.; Cann, Jenna M.; Ciardi, David R.; Clark, Ian; Cochran, William D.; Cohen, David H.; Conti, Dennis M.; Crepp, Justin R.; Curtis, Ivan A.; D’Ago, G.; Diazeguigure, Kenny A.; Dressing, Courtney D.; Dubois, Franky; Ellingson, E.; Ellis, Tyler G.; Esquerdo, Gilbert A.; Evans, P.; Friedli, Alison J.; Fukui, A.; Fulton, Benjamin J.; Gonzales, Erica J.; Good, J. C.; Gregorio, J.; Gumusayak, Tolga; Hancock, Daniel A.; Harada, Caleb K.; Hart, Rhodes; Hintz, E. G.; Jang‐Condell, Hannah; Jeffery, Elizabeth; Jensen, Eric L. N.; Jofré, E.; Joner, M. D.; Kar, Aman; Kasper, David; Keten, Burak; Kielkopf, John F.; Komonjinda, S.; Kotnik, C.; Latham, David W.; Leuquire, Jacob D.; Lewis, Tiffany R.; Logie, Ludwig; Lowther, S.; MacQueen, Phillip J.; Martin, Trevor; Mawet, Dimitri; McLeod, Kim K.; Murawski, Gabriel; Narita, Norio; Nordhausen, Jim; Oberst, Thomas E.; Odden, Caroline; Panka, Peter A.; Petrucci, R.; Plavchan, Peter; Quinn, Samuel N.; Rau, Steve; Reed, Phillip A.; Relles, Howard M.; Renaud, Joe P.; Scarpetta, G.; Sorber, Rebecca L.; Spencer, Alex D.; Spencer, M.; Stephens, Denise C.; Stockdale, Chris; Tan, T. G.; Trueblood, Mark; Trueblood, Patricia; Vanaverbeke, Sigfried; Villanueva, Steven; Warner, Elizabeth; West, M.; Yalçınkaya, Selçuk; Yeigh, Rex R.; Zambelli, Roberto

doi:10.3847/1538-3881/aae582

Cited by 60 publications

(47 citation statements)

References 46 publications

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“…To examine the effect of the metallicity on the stellar radius, a large sample of empirical radii and homogeneous metallicity measurements is desirable. The detection of hundreds of low-mass eclipsing binary stars as false positives in searches for transiting exoplanets Collins et al 2018) will permit robust statistical studies to determine the physical properties of such objects. We expect that the number of measurements of masses and radii of very-low-mass stars will substantially increase as results from the recently launched TESS mission (Ricker et al 2014) are becoming available.…”

Section: Resultsmentioning

confidence: 99%

The EBLM Project

Boetticher

Triaud

Queloz

et al. 2019

A&A

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Measurements of the physical properties of stars at the lower end of the main sequence are scarce. In this context we report masses, radii and surface gravities of ten very-low-mass stars in eclipsing binary systems, with orbital periods of the order of several days. The objects probe the stellar mass-radius relation in the fully convective regime, M 0.35 M , down to the hydrogen burning mass-limit, M HB ∼ 0.07 M . The stars were detected by the WASP survey for transiting extra-solar planets, as low-mass, eclipsing companions orbiting more massive, F-and G-type host stars. We use eclipse observations of the host stars, performed with the TRAPPIST, Leonhard Euler and SPECULOOS telescopes, and radial velocities of the host stars obtained with the CORALIE spectrograph, to determine the physical properties of the low-mass companions. Surface gravities of the low-mass companions are derived from the eclipse and orbital parameters of each system. Spectroscopic measurements of the host star effective temperature and metallicity are used to infer the host star mass and age from stellar evolution models for solar-type stars. Masses and radii of the low-mass companions are then derived from the eclipse and orbital parameters of the binary systems. The objects are compared to stellar evolution models for low-mass stars, to test for an effect of the stellar metallicity and orbital period on the radius of low-mass stars in close binary systems. Measurements are found to be in good agreement with stellar evolution models; a systematic inflation of the radius of low-mass stars with respect to model predictions is limited to 1.6 ± 1.2%, in the fully convective low-mass regime. The sample of ten objects indicates a scaling of the radius of low-mass stars with the host star metallicity. No correlation between stellar radii and the orbital periods of the binary systems is determined. A combined analysis with thirteen comparable objects from the literature is consistent with this result.Article published by EDP Sciences A150, page 1 of 18 A&A 625, A150 (2019)

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Section: Resultsmentioning

confidence: 99%

The EBLM Project

Boetticher

Triaud

Queloz

et al. 2019

A&A

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“…This is because eclipsing binaries may mimic transit-like signals in photometric survey data. False positive rates are especially worse for ground-based surveys (e.g., more than 98% for the recent KELT survey 12 ), and still not negligible even for a space-based survey like Kepler 13 . This is also true for the upcoming TESS mission, and the false positive rate is predicted as 30-70% 14 depending on the galactic latitude.…”

Section: Introductionmentioning

confidence: 99%

MuSCAT2: four-color simultaneous camera for the 1.52-m Telescopio Carlos Sánchez

Narita

Fukui

Kusakabe

et al. 2018

J. Astron. Telesc. Instrum. Syst.

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We report the development of a 4-color simultaneous camera for the 1.52 m Telescopio Carlos Sánchez (TCS) in the Teide Observatory, Canaries, Spain. The new instrument, named MuSCAT2, has a capability of 4-color simultaneous imaging in g (400-550 nm), r (550-700 nm), i (700-820 nm), and z s (820-920 nm) bands. MuSCAT2 equips four 1024×1024 pixel CCDs, having a field of view of 7.4×7.4 arcmin 2 with a pixel scale of 0.44 arcsec per pixel. The principal purpose of MuSCAT2 is to perform high-precision multi-color exoplanet transit photometry. We have demonstrated photometric precisions of 0.057%, 0.050%, 0.060%, and 0.076% as root-mean-square residuals of 60 s binning in g, r, i and z s bands, respectively, for a G0 V star WASP-12 (V = 11.57 ± 0.16). MuSCAT2 has started science operations since January 2018, with over 250 telescope nights per year. MuSCAT2 is expected to become a reference tool for exoplanet transit observations, and will substantially contribute to the follow-up of the TESS and PLATO space missions.

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“…Part of the KELT strategy for discovering transiting exoplanets involves an algorithm that pre-selects potential exoplanet candidates from reduced light curves for all sources identified in a given field (Collins et al 2018). HD 62658 was one such source identified in this way.…”

Section: Keltmentioning

confidence: 99%

MOBSTER – III. HD 62658: a magnetic Bp star in an eclipsing binary with a non-magnetic ‘identical twin’

Shultz

Johnston

Labadie-Bartz

et al. 2019

Monthly Notices of the Royal Astronomical Society

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HD 62658 (B9p V) is a little-studied chemically peculiar star. Light curves obtained by the Kilodegree Extremely Little Telescope (KELT) and Transiting Exoplanet Survey Satellite (TESS) show clear eclipses with a period of about 4.75 d, as well as out-of-eclipse brightness modulation with the same 4.75 d period, consistent with synchronized rotational modulation of surface chemical spots. High-resolution ESPaDOnS circular spectropolarimetry shows a clear Zeeman signature in the line profile of the primary; there is no indication of a magnetic field in the secondary. PHOEBE modelling of the light curve and radial velocities indicates that the two components have almost identical masses of about 3 M ⊙ . The primary's longitudinal magnetic field B z varies between about +100 and −250 G, suggesting a surface magnetic dipole strength B d = 850 G. Bayesian analysis of the Stokes V profiles indicates B d = 650 G for the primary and B d < 110 G for the secondary. The primary's line profiles are highly variable, consistent with the hypothesis that the out-of-eclipse brightness modulation is a consequence of rotational modulation of that star's chemical spots. We also detect a residual signal in the light curve after removal of the orbital and rotational modulations, which might be pulsational in origin; this could be consistent with the weak line profile variability of the secondary. This system represents an excellent opportunity to examine the consequences of magnetic fields for stellar structure via comparison of two stars that are essentially identical with the exception that one is magnetic. The existence of such a system furthermore suggests that purely environmental explanations for the origin of fossil magnetic fields are incomplete.

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The KELT Follow-up Network and Transit False-positive Catalog: Pre-vetted False Positives for TESS

Cited by 60 publications

References 46 publications

The EBLM Project

The EBLM Project

MuSCAT2: four-color simultaneous camera for the 1.52-m Telescopio Carlos Sánchez

MOBSTER – III. HD 62658: a magnetic Bp star in an eclipsing binary with a non-magnetic ‘identical twin’

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