TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26

Prša, Andrej; Kochoska, A.; Conroy, Kyle E.; Eisner, Nora L.; Hey, Daniel R.; IJspeert, L.; Kruse, Ethan; Fleming, Scott W.; Johnston, C.; Kristiansen, Martti H.; LaCourse, Daryll; Mortensen, Danielle; Pepper, Joshua; Stassun, Keivan G.; Torres, Guillermo; Abdul-Masih, M.; Chakraborty, Joheen; Gagliano, R.; Guo, Zhao; Hambleton, Kelly; Hong, Kyeongsoo; Jacobs, Thomas L.; Jones, David; Kostov, Veselin B.; Lee, Jae Woo; Omohundro, Mark; Orosz, Jerome A.; Page, Emma J.; Powell, Brian P.; Rappaport, S.; Reed, Phill; Schnittman, Jeremy D.; Schwengeler, Hans Martin; Shporer, Avi; Terentev, Ivan A.; Vanderburg, Andrew; Welsh, William F.; Caldwell, Douglas A.; Doty, J.; Jenkins, Jon M.; Latham, David W.; Ricker, G.; Seager, Sara; Schlieder, Joshua E.; Shiao, Bernie; Vanderspek, R.; Winn, Joshua N.

doi:10.3847/1538-4365/ac324a

Cited by 79 publications

(61 citation statements)

References 122 publications

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“…From this diagram, it can be seen that the expected features of an equal-mass binary main sequence and increasing binary fraction with mass are present in both catalogs. (Prša et al 2022). Eclipsing binaries from both catalogs have excess RV noise that meets our threshold in ∼ 70% of stars compared to the "field" rate of ∼ 20%.…”

Section: Location On the Hertzsprung Russell Diagrammentioning

confidence: 79%

“…Indeed, we find that for the 331 EBs in the Kepler EB catalog crossmatch (containing 2922 sources) that we have at least 3 RV transits for (Kirk et al 2016), 73.8% exceed the p < 0.001 threshold. For the 458 EBs in the TESS EB catalog crossmatch (containing 4584 sources) (Prša et al 2022) we recover 73.1% as binaries.…”

Section: Validation Against Catalogs Of Known Binariesmentioning

confidence: 83%

“…The intersection of this line with the CDFs is the proportion of the sample that are flagged as binaries. Right: Identical plot for the TESS Community Target List and Villanova TESS Eclipsing binary catalog(Prša et al 2022). Eclipsing binaries from both catalogs have excess RV noise that meets our threshold in ∼ 70% of stars compared to the "field" rate of ∼ 20%.…”

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confidence: 99%

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paired: A Statistical Framework for Determining Stellar Binarity with Gaia RVs. I. Planet Hosting Binaries

Chance¹,

Foreman-Mackey²,

Ballard³

et al. 2022

Preprint

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The effect of stellar multiplicity on the formation and evolution of planetary systems is complex. At a demographic level, campaigns with both high-resolution imaging and radial velocity observations indicate that planet formation is strongly disrupted by close binaries, while being relatively unaffected by wide companions. However, the magnitude and distance-limited nature of those tools mean that large ranges of mass ratios and separations remain largely unexplored. The Early Data Release 3 (EDR3) from the Gaia Mission includes radial velocity measurements of over 6.5 million targets, which we employ to explore the effect of binary companions within a statistical framework called paired. These companions present as a source of excess radial velocity noise in the Gaia catalog, when compared to the typical noise for stars of similar spectral type and magnitude. Within this framework, we examine the evidence for stellar multiplicity among the stars surveyed by NASA's Kepler and TESS missions. We use radial velocity errors published in Gaia EDR3 to estimate the probability of an unresolved stellar companion for a large subset of the Kepler and TESS Input Catalog stars, where possible benchmarking our inferred radial velocity semi-amplitudes against the those from ground-based radial velocity surveys. We determine that we are typically sensitive out to several AU and mass ratios > 0.1, dependent upon the stellar magnitude. We aim for paired to be a useful community tool for the exploration of the effects of binarity on planets at a population level, and for efficient identification of false-positive transit candidates.

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Section: Location On the Hertzsprung Russell Diagrammentioning

confidence: 79%

Section: Validation Against Catalogs Of Known Binariesmentioning

confidence: 83%

mentioning

confidence: 99%

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paired: A Statistical Framework for Determining Stellar Binarity with Gaia RVs. I. Planet Hosting Binaries

Chance¹,

Foreman-Mackey²,

Ballard³

et al. 2022

Preprint

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“…There are several ways to expand upon our work in the future. The recently published TESS Eclipsing Binary Catalog (Prša et al 2022) provides an opportunity to expand our analysis to a much larger data set. The recently released Gaia Data Release 3 will include Gaia time-series photometry for eclipsing binaries (Gaia Collaboration et al 2019).…”

Section: Discussionmentioning

confidence: 99%

Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect

Knote

Caballero-Nieves

Gokhale

et al. 2022

ApJS

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The O’Connell effect—the presence of unequal maxima in eclipsing binaries—remains an unsolved riddle in the study of close binary systems. The Kepler space telescope produced high-precision photometry of nearly 3000 eclipsing binary systems, providing a unique opportunity to study the O’Connell effect in a large sample and in greater detail than in previous studies. We have characterized the observational properties—including temperature, luminosity, and eclipse depth—of a set of 212 systems (7.3% of Kepler eclipsing binaries) that display a maxima flux difference of at least 1%, representing the largest sample of O’Connell effect systems yet studied. We explored how these characteristics correlate with each other to help understand the O’Connell effect’s underlying causes. We also describe some system classes with peculiar light-curve features aside from the O’Connell effect (∼24% of our sample), including temporal variation and asymmetric minima. We found that the O’Connell effect size’s correlations with period and temperature are inconsistent with Kouzuma's starspot study. Up to 20% of systems display the parabolic eclipse timing variation signal expected for binaries undergoing mass transfer. Most systems displaying the O’Connell effect have the brighter maximum following the primary eclipse, suggesting a fundamental link between which maximum is brighter and the O’Connell effect’s physical causes. Most importantly, we find that the O’Connell effect occurs exclusively in systems where the components are close enough to significantly affect each other, suggesting that the interaction between the components is ultimately responsible for causing the O’Connell effect.

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“…Although the primary focus by the VSG initially was directed towards exoplanet detections, signals from EBs can resemble that of planets, making a vast collection of EBs a natural byproduct (Schmitt et al 2016). This has resulted in large catalogues for Kepler (Kirk et al 2016), K2 (LaCourse et al (2015, Armstrong et al (2015)) and TESS (Prša et al 2022). Also, LaCourse and Jacobs (2018) presented a catalogue of single eclipses found in K2 C0-C14.…”

Section: Eclipsing Binariesmentioning

confidence: 99%

The Visual Survey Group: A Decade of Hunting Exoplanets and Unusual Stellar Events with Space-Based Telescopes

Kristiansen,

Rappaport,

Vanderburg

et al. 2022

Preprint

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This article presents the history of the Visual Survey Group (VSG) -a Professional-Amateur (Pro-Am) collaboration within the field of astronomy working on data from several space missions (Kepler, K2 and TESS). This paper covers the formation of the VSG, its survey-methods including the most common tools used and its discoveries made over the past decade. So far, the group has visually surveyed nearly 10 million light curves and authored 69 peer-reviewed papers which mainly focus on exoplanets and discoveries involving multistellar systems found using the transit method. The preferred manual search-method carried out by the VSG has revealed its strength by detecting numerous substellar objects which were overlooked or discarded by automated search programs, uncovering some of the most rare stars in our galaxy, and leading to several serendipitous discoveries of unprecedented astrophysical phenomena. The main purpose of the VSG is to assist in the exploration of our local Universe, and we therefore advocate continued crowd-sourced examination of time-domain data sets, and invite other research teams to reach out in order to establish collaborating projects.

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TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26

Cited by 79 publications

References 122 publications

paired: A Statistical Framework for Determining Stellar Binarity with Gaia RVs. I. Planet Hosting Binaries

paired: A Statistical Framework for Determining Stellar Binarity with Gaia RVs. I. Planet Hosting Binaries

Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect

The Visual Survey Group: A Decade of Hunting Exoplanets and Unusual Stellar Events with Space-Based Telescopes

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