A Catalog of Short Period Spectroscopic and Eclipsing Binaries Identified from the LAMOST and PTF Surveys

Yang, Fan; Long, R. J.; Shan, Su-Su; Zhang, Bo; Guo, Rui; Bai, Yu; Bai, Zhong-Rui; Cui, Kaiming; Wang, Song; Liu, Jifeng

doi:10.3847/1538-4365/ab9b77

Cited by 23 publications

(24 citation statements)

References 55 publications

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“…Such large period bias would cause significant TESS timing offsets when compared to ephemeris prediction and thereby are flagged. The fold-and-check method has been well utilized in period searching researches (Schwarzenberg-Czerny 1989;Yang et al 2020b;.…”

Section: Tess Transit Timing Validationmentioning

confidence: 99%

TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties

Shan¹,

Yang²,

Lu³

et al. 2021

Preprint

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A precise transit ephemeris serves as the premise for follow-up exoplanet observations. The transit timing variation (TTV) as an important scientific output potentially reveals planetary orbital evolution. We compare transit timings of 262 hot Jupiters from TESS with the archival ephemeris and find 31 of them having significant TESS timing offsets, among which WASP-161b shows the most significant offset of -203.7±4.1 minutes. The median value of these offsets is 17.8 minutes, equivalent to 3.4 σ. We evaluate the timing precision of TESS Objects of Interest (TOI) which provides the TESS timings in this work. The evaluation is applied by deriving TESS transit timing from a self-generated pipeline. We refine and update the previous ephemeris, based on precise timing (uncertainty within 1 minute) and a long timing baseline (∼ 10 years). Our refined ephemeris gives the transit timing at a median precision of 1.11 minutes until 2025 and 1.86 minutes until 2030. All the targets with timing offset larger than 10σ present earlier timings than the prediction, which cannot be due to underestimated ephemeris uncertainty, apsidal precision, or Rømer effect as those effects should be unsigned. We regard the timing offsets mainly originating from the underestimated ephemeris uncertainty. For some particular targets, timing offsets are due to tidal dissipation. We find a tentative TTV of XO-3b (timing offset > 10 σ) yielding a period derivative of 5.8±0.9×10 −9 . The TTV may be explained by tidal dissipation. Our result provides direct observational support for the tidal dissipation of XO-3b, reported in previous work.

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Section: Tess Transit Timing Validationmentioning

confidence: 99%

TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties

Shan¹,

Yang²,

Lu³

et al. 2021

Preprint

Self Cite

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“…WASP-161b has a well-measured ephemeris for transits. This enables us to apply a simple but effective detrending algorithm based on the ephemeris (Yang et al 2020). We extract the light curve centered at the transit midpoint time.…”

Section: Light Curves Derived From Tess Photometrymentioning

confidence: 99%

An Empirical Bayesian Approach to Limb Darkening in Modeling WASP-121b Transit Light Curves

Yang

Long

Liu

et al. 2021

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We present a novel, iterative method using an empirical Bayesian approach for modeling the limb-darkened WASP-121b transit from the TESS light curve. Our method is motivated by the need to improve R p /R * estimates for exoplanet atmosphere modeling and is particularly effective with the limb-darkening (LD) quadratic law requiring no prior central value from stellar atmospheric models. With the nonlinear LD law, the method has all the advantages of not needing atmospheric models but does not converge. The iterative method gives a different R p /R * for WASP-121b at a significance level of 1σ when compared with existing noniterative methods. To assess the origins and implications of this difference, we generate and analyze light curves with known values of the LD coefficients (LDCs). We find that noniterative modeling with LDC priors from stellar atmospheric models results in an inconsistent R p /R * at a 1.5σ level when the known LDC values are the same as those previously found when modeling real data by the iterative method. In contrast, the LDC values from the iterative modeling yield the correct value of R p /R * to within 0.25σ. For more general cases with different known inputs, Monte Carlo simulations show that the iterative method obtains unbiased LDCs and correct R p /R * to within a significance level of 0.3σ. Biased LDC priors can cause biased LDC posteriors and lead to bias in the R p /R * of up to 0.82%, 2.5σ for the quadratic law and 0.32%, 1.0σ for the nonlinear law. Our improvement in R p /R * estimation is important when analyzing exoplanet atmospheres.

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“…separate out CB from other types of eclipsing binaries (mainly the Algol and Beta Lyrae types; for example in Rucinski 1997a,b;Selam 2004;Derekas et al 2007;Lee et al 2014;Muraveva et al 2014;Nedoroščík et al 2015;Yang et al 2020) or to classify CB against different types of variable stars in time-series surveys (for example, see Pojmanski 2002;Eyer & Blake 2005;Debosscher et al 2007;Hoffman et al 2009;Kim et al 2014;Masci et al 2014;Jayasinghe et al 2019). In this work, a 4 th -order Fourier expansion (Derekas et al 2007;Deb & Singh 2011;Dey et al 2015;Chen et al 2018) in the following form was adopted to fit the folded ZTF light curves for the CB listed in Table 4:…”

Section: Light Curves Fitting With Fourier Expansionmentioning

confidence: 99%

Zwicky Transient Facility and Globular Clusters: the Period–Luminosity and Period–Luminosity–Color Relations for Late-type Contact Binaries

Ngeow

Liao

Bellm

et al. 2021

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In this work, we aimed to derive the gri-band period-luminosity (PL) and period-luminosity-color (PLC) relations for late-type contact binaries, for the first time, located in the globular clusters, using the homogeneous light curves collected by the Zwicky Transient Factory (ZTF). We started with 79 contact binaries in 15 globular clusters, and retained 30 contact binaries in 10 globular clusters that have adequate number of data points in the ZTF light curves and unaffected by blending. Magnitudes at mean and maximum light of these contact binaries were determined using a fourth-order Fourier expansion, while extinction corrections were done using the Bayerstar2019 3D reddening map together with adopting the homogeneous distances to their host globular clusters. After removing early-type and "anomaly" contact binaries, our derived gri-band PL and period-Wesenheit (PW) relations exhibit a much larger dispersion with large errors on the fitted coefficients. Nevertheless, the gr-band PL and PW relations based on this small sample of contact binaries in globular clusters were consistent with those based on a larger sample of nearby contact binaries. Good agreements of the PL and PW relations suggested both samples of contact binaries in the local Solar neighborhood and in the distant globular clusters can be combined and used to derive and calibrate the PL, PW and PLC relations. The final derived gr-band PL, PW and PLC relations were much improved than those based on the limited sample of contact binaries in the globular clusters.

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A Catalog of Short Period Spectroscopic and Eclipsing Binaries Identified from the LAMOST and PTF Surveys

Cited by 23 publications

References 55 publications

TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties

TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties

An Empirical Bayesian Approach to Limb Darkening in Modeling WASP-121b Transit Light Curves

Zwicky Transient Facility and Globular Clusters: the Period–Luminosity and Period–Luminosity–Color Relations for Late-type Contact Binaries

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