HD 219666 b: a hot-Neptune from TESS Sector 1

Esposito, M.; Armstrong, David J.; Gandolfi, D.; Adibekyan, V.; Fridlund, M.; Santos, N. C.; Livingston, John H.; Delgado-Mena, E.; Fossati, L.; Lillo-Box, J.; Barragán, Oscar; Barrado, D.; Cubillos, Patricio; Cooke, Benjamin F.; Justesen, A. B.; Meru, Farzana; Díaz, R. F.; Dai, Fei; Nielsen, L. D.; Persson, C. M.; Wheatley, P. J.; Hatzes, A. P.; Eylen, Vincent Van; Musso, Maria; Alonso, R.; Beck, P. G.; Barros, S. C. C.; Bayliss, Daniel; Bonomo, A. S.; Bouchy, F.; Brown, D. J. A.; Bryant, Edward M.; Cabrera, J.; Cochran, William D.; Csizmadia, Sz.; Deeg, H. J.; Demangeon, O.; Deleuil, M.; Dumusque, X.; Eigmüller, Philipp; Endl, Michael; Erikson, A.; Faedi, F.; Figueira, P.; Fukui, A.; Grziwa, S.; Guenther, E. W.; Hidalgo, D.; Hjorth, María; Hirano, Teruyuki; Hojjatpanah, S.; Knudstrup, Emil; Korth, J.; Lam, K. W. F.; Leon, Jerome de; Lund, M. N.; Luque, R.; Mathur, S.; Montañés-Rodŕıguez, P.; Narita, Norio; Nespral, D.; Niraula, Prajwal; Nowak, G.; Osborn, H.; Πάλλη, Ε.; Pätzold, M.; Pollacco, D.; Prieto-Arranz, J.; Rauer, H.; Redfield, Seth; Ribas, I.; Sousa, S. G.; Smith, A. M. S.; Tala-Pinto, M.; Udry, S.; Winn, Joshua N.

doi:10.1051/0004-6361/201834853

Cited by 36 publications

(23 citation statements)

References 108 publications

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“…Exoplanet HD 219666b was discovered by Esposito et al (2019) using TESS data. It is a hot Neptune around a G7 star (mass 0.92 ± 0.03 M e , radius 1.03 ± 0.03 R e ) with a period of 6.04 days.…”

Section: Iterative Methods For Ld With Tess Light Curvesmentioning

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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Section: Iterative Methods For Ld With Tess Light Curvesmentioning

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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“…It will now move its observations to the north, continuing its full-sky survey. At the time of writing TESS has already successfully discovered and confirmed 29 new transiting planets (NASA Exoplanet Archive 1 , Akeson et al 2013) including π Mensae c Gandolfi et al 2018), HD 202772A b, (Wang et al 2019), LHS 3844 b (Vanderspek et al 2019) and HD 219666 b, (Esposito et al 2019).…”

Section: Introductionmentioning

confidence: 99%

An examination of the effect of the TESS extended mission on southern hemisphere monotransits

Cooke

Pollacco

2019

A&A

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Context. NASA recently announced an extended mission for TESS. As a result it is expected that the southern ecliptic hemisphere will be re-observed approximately two years after the initial survey. Aims. We aim to explore how TESS re-observing the southern ecliptic hemisphere will impact the number and distribution of monotransits discovered during the first year of observations. This simulation will be able to be scaled to any future TESS re-observations. Methods. We carry out an updated simulation of TESS detections in the southern ecliptic hemisphere. This simulation includes realistic Sector window-functions based on the first 11 sectors of SPOC 2 min SAP lightcurves. We then extend this simulation to cover the expected Year 4 of the mission when TESS will re-observe the southern ecliptic fields. For recovered monotransits we also look at the possibility of predicting the period based on the coverage in the TESS data. Results. We find an updated prediction of 339 monotransits from the TESS Year 1 southern ecliptic hemisphere, and that approximately 80% of these systems (266/339) will transit again in the Year 4 observations. The Year 4 observations will also contribute new monotransits not seen in Year 1, resulting in a total of 149 monotransits from the combined Year 1 and Year 4 data sets. We find that 75% (189/266) of recovered Year 1 monotransits will only transit once in the Year 4 data set. For these systems we will be able to constrain possible periods, but period aliasing due to the large time gap between Year 1 and Year 4 observations means that the true period will remain unknown without further spectroscopic or photometric follow-up.

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“…Kepler-1656 b, a dense sub-Saturn with a high eccentricity of e = 0.84 transiting a relatively bright (V = 11.6 mag) solar-type star, was recently reported by Brady et al (2018). Three sub-Saturns were discovered and characterised by the KESPRINT consortium, two of them in K2 campaign 3 (K2-60 b, Eigmüller et al 2017) and campaign 14 (HD 89345 b, aka K2-234 b, Van Eylen et al 2018;Yu et al 2018b), and HD 219666 b (Esposito et al 2019) in TESS Sector 1. One sub-Saturn, GJ 3470 b (Bonfils et al 2012), orbiting an M1.5 dwarf was not included by Petigura et al (2017), but we add it to the current sample, adopting the parameters from Awiphan et al (2016).…”

Section: Global Analysismentioning

confidence: 83%

K2-280 b – a low density warm sub-Saturn around a mildly evolved star

Nowak

Πάλλη

Deeg

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present an independent discovery and detailed characterisation of K2-280 b, a transiting low density warm sub-Saturn in a 19.9-day moderately eccentric orbit (e = $0.35_{-0.04}^{+0.05}$ ) from K2 campaign 7. A joint analysis of high precision HARPS, HARPS-N, and FIES radial velocity measurements and K2 photometric data indicates that K2-280 b has a radius of Rb = 7.50 ± 0.44 R⊕ and a mass of Mb = 37.1 ± 5.6 M⊕, yielding a mean density of ρb = $0.48 _{ - 0.10 } ^ { + 0.13 }$ g cm−3. The host star is a mildly evolved G7 star with an effective temperature of Teff = 5500 ± 100 K , a surface gravity of log g⋆ = 4.21 ± 0.05 (cgs), and an iron abundance of [Fe/H] = 0.33 ± 0.08 dex, and with an inferred mass of M⋆ = 1.03 ± 0.03 M⊙ and a radius of R⋆ = 1.28 ± 0.07 R⊙. We discuss the importance of K2-280 b for testing formation scenarios of sub-Saturn planets and the current sample of this intriguing group of planets that are absent in the Solar System.

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HD 219666 b: a hot-Neptune from TESS Sector 1

Cited by 36 publications

References 108 publications

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

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

An examination of the effect of the TESS extended mission on southern hemisphere monotransits

K2-280 b – a low density warm sub-Saturn around a mildly evolved star

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