Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES‐2

Sozzetti, A.; Torres, Guillermo; Charbonneau, David; Latham, David W.; Holman, Matthew J.; Winn, Joshua N.; Laird, John B.; O’Donovan, Francis T.

doi:10.1086/519214

Cited by 315 publications

(397 citation statements)

References 96 publications

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“…With this stellar density, combined with the effective temperature and metallicity from the spectroscopic analysis, the surface gravity can be determined through isochrone fitting (see e.g. Sozzetti et al 2007). As presented in Mortier et al (in prep.…”

Section: Fgk Stars With Transiting Planetsmentioning

confidence: 99%

“…difference), the derived effective temperature and metallicity values are only ∼250 K and ∼0.10 dex higher, respectively, than the adopted solar values. As such, the temperatures and metallicities derived with our adopted spectroscopic method can be used as reference values even if the derived spectroscopic surface gravities differ from those derived using the transit light curve (and the stellar density; see Sozzetti et al 2007). A more detailed discussion of this issue will be presented in Mortier et al (in prep.…”

Section: Fgk Stars With Transiting Planetsmentioning

confidence: 99%

See 1 more Smart Citation

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

Santos

Sousa

Mortier

et al. 2013

A&A

293

255

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Context. Thanks to the importance that the star-planet relation has to our understanding of the planet formation process, the precise determination of stellar parameters for the ever increasing number of discovered extra-solar planets is of great relevance. Furthermore, precise stellar parameters are needed to fully characterize the planet properties. It is thus important to continue the efforts to determine, in the most uniform way possible, the parameters for stars with planets as new discoveries are announced. Aims. In this paper we present new precise atmospheric parameters for a sample of 48 stars with planets. We then take the opportunity to present a new catalogue of stellar parameters for FGK and M stars with planets detected by radial velocity, transit, and astrometry programs. Methods. Stellar atmospheric parameters and masses for the 48 stars were derived assuming local thermodynamic equilibrium (LTE) and using high-resolution and high signal-to-noise spectra. The methodology used is based on the measurement of equivalent widths for a list of iron lines and making use of iron ionization and excitation equilibrium principles. For the catalogue, and whenever possible, we used parameters derived in previous works published by our team, using well-defined methodologies for the derivation of stellar atmospheric parameters. This set of parameters amounts to over 65% of all planet host stars known, including more than 90% of all stars with planets discovered through radial velocity surveys. For the remaining targets, stellar parameters were collected from the literature. Results. The stellar parameters for the 48 stars are presented and compared with previously determined literature values. For the catalogue, we compile values for the effective temperature, surface gravity, metallicity, and stellar mass for almost all the planet host stars listed in the Extrasolar Planets Encyclopaedia. This data will be updated on a continuous basis. The compiled catalogue is available online. The data can be used for statistical studies of the star-planet correlation, as well as for the derivation of consistent properties for known planets.

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Section: Fgk Stars With Transiting Planetsmentioning

confidence: 99%

Section: Fgk Stars With Transiting Planetsmentioning

confidence: 99%

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

Santos

Sousa

Mortier

et al. 2013

A&A

293

255

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“…This analytic light curve was calculated with the stellar and planetary parameters given by Holman et al (2007) and Sozzetti et al (2007). To get the best fit we compare the analytic light curve with the observed light curve until the χ 2 is minimal.…”

Section: Determination Of the Midtransit Timementioning

confidence: 99%

“…The planet orbits the nearby 11th magnitude G0 V main-sequence dwarf GSC 03549-02811 every ∼2.5 days. From high-resolution spectra, Sozzetti et al (2007) derived accurate values of the stellar atmospheric parameters of the TrES-2 parent star such as effective temperature, surface gravity and metallicity. With the help of detailed analysis of high precision z-band photometry and light curve modeling of the 1.4% deep transit by the Transit Light Curve (TLC) Project ), estimates of the planetary parameters could also be determined.…”

Section: Introductionmentioning

confidence: 99%

Planetary transit observations at the University Observatory Jena: TrES‐2

Raetz¹,

Mugrauer²,

Schmidt³

et al. 2009

Astron Nachr

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We report on observations of several transit events of the transiting planet TrES-2 obtained with the Cassegrain-TeleskopKamera at the University Observatory Jena. Between March 2007 and November 2008 ten different transits and almost a complete orbital period were observed. Overall, in 40 nights of observation 4291 exposures (in total 71.52 h of observation) of the TrES-2 parent star were taken. With the transit timings for TrES-2 from the 34 events published by the TrESnetwork, the Transit Light Curve project and the Exoplanet Transit Database plus our own ten transits, we find that the orbital period is P = (2.470614 ± 0.000001) d, a slight change by ∼ 0.6 s compared to the previously published period. We present new ephemeris for this transiting planet. Furthermore, we found a second dip after the transit which could either be due to a blended variable star or occultation of a second star or even an additional object in the system. Our observations will be useful for future investigations of timing variations caused by additional perturbing planets and/or stellar spots and/or moons.

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“…However, stellar activity in late-type main-sequence stars induces photometric modulations and apparent radial velocity variations which may hamper the detection of Earth-like planets and the measurement of system parameters, such as the orbital semimajor axis of a planet, the transit depth and so on, which hence biases the inference of radius and mass of both planet and host star, and the characterization of planetary atmospheric properties (Sozzetti et al 2007;Enoch et al 2010;Oshagh et al 2015). Special variations in the spot distribution and the ratio between unperturbed and spotted areas across the stellar surface can modify the mid-transit times when fitted with a normal, symmetric transiting model, due to spot crossing events (Oshagh et al 2013b;Daassou et al 2014), which possibly mimic the TTV signals induced by gravitational perturbations of other planets.…”

Section: Introductionmentioning

confidence: 99%

Refined System Parameters and TTV Study of Transiting Exoplanetary System Hat-P-20

Sun

Wang

et al. 2016

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We report new photometric observations of the transiting exoplanetary system HAT-P-20, obtained using CCD cameras at Yunnan Observatories and Ho Koon Nature Education cum Astronomical Centre, China, from 2010 to 2013, and Observatori Ca l'Ou, Sant Marti Sesgueioles, Spain, from 2013 to 2015. The observed data are corrected for systematic errors according to the coarse de-correlation and SYSREM algorithms, so as to enhance the signal of the transit events. In order to consistently model the star spots and transits of this exoplanetary system, we develop a highly efficient tool STMT based on the analytic models of Mandel & Agol and Montalto et al. The physical parameters of HAT-P-20 are refined by homogeneously analyzing our new data, the radial velocity data, and the earlier photometric data in the literature with the Markov chain Monte Carlo technique. New radii and masses of both host star and planet are larger than those in the discovery paper due to the discrepancy of the radius among K-dwarfs between predicted values by standard stellar models and empirical calibration from observations. Through the analysis of all available mid-transit times calculated with the normal model and spotted model, we conclude that the periodic transit timing variations in these transit events revealed by employing the normal model are probably induced by spot crossing events. From the analysis of the distribution of occulted spots by HAT-P20b, we constrain the misaligned architecture between the planetary orbit and the spin of the host star.

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Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES‐2

Cited by 315 publications

References 96 publications

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

Planetary transit observations at the University Observatory Jena: TrES‐2

Refined System Parameters and TTV Study of Transiting Exoplanetary System Hat-P-20

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